Journal of Double Star Observations V5, No4GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System in Process of Dissociation F. M. Rica and R. Benavides 406

Vol. 12 No. 4 April 22, 2016 Page Journal of Double Star Observations

Journal of

Double Star Observations

April 22, 2016

Astronomical Association of Queensland Program of Measurements of Seven Southern Multiple Stars Graeme Jenkinson

308

Astronomical Association of Queensland Program of Measurement of Nine Neglected Southern Multiple Stars Graeme Jenkinson

313

Results of 194 Double Stars Measurements from Astrometric CCD Observations at the Nikolaev Observatory (Ukraine) Daniil Bodryagin, Larisa Bondarchuk, and Nadiia Maigurova

320

Jonckheere Double Star Photometry – Part II: Delphinus Wilfried R.A. Knapp

327

Double Star Measurements for December 2013 Frank Smith

338

Photometry of Faint and Wide Doubles in Vulpecula Wilfried R.A. Knapp and Chris Thuemen

347

Jonckheere Double Star Photometry – Part III: Lyra, Equuleus, and Eridanus Wilfried R.A. Knapp

351

STT Doubles with Large ΔM – Part IV: Ophiuchus and Hercules Wilfried R.A. Knapp and John Nanson

361

Measurements with Reticle Micrometer Performed by a New Double Stars Observing Group from Poland Marcin Biskupski, Natalia Banacka, Justyna Cupryjak, Małgorzata Malinowska, Kamil Bujel, Zdzisław Kołtek, Jarosław Mazur, Marcin Muskała, Łukasz Płotkowski, Barłomiej Prowans, and Paweł Szkaplewicz

374

CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs:The Autumn 2015 Observing Program at Brilliant Sky Observatory, Part 1 Richard W. Harshaw

376

CCD Measurements of 8 Double Stars With Binary Nature: The Autumn 2015 Observing Program at Brilliant Sky Observatory, Part 2 Richard W. Harshaw

388

CCD Measurements of 141 Proper Motion Stars: The Autumn 2015 Observing Program at the Brilliant Sky Observatory, Part 3 Richard W. Harshaw

394

Measurements of Multi-star Systems LEO 5 and MKT 13 Faisal AlZaben, Allen Priest, Stephen Priest, Rex Qiu, Grady Boyce, and Pat Boyce

400

GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System in Process of Dissociation F. M. Rica and R. Benavides

406

Meeting Announcement: Opportunities for Student Astronomical Research in Southern California San Diego, California, June 12, 2016 414

Meeting Announcement: Small Telescope Research Communities of Practice American Astronomical Society’s 228th Meeting (Meeting in a Meeting Special Session), San Diego, CA, June 13/14

415

Meeting Announcement: Society for Astronomical Sciences 2016 Symposium Ontario California, June 16 - 18, 2016 417

Inside this issue:

Vol. 12 No. 4 April 22, 2016 Page 308 Journal of Double Star Observations

Introduction

These latest results are part of an ongoing program commenced in 2008 by the Double Star Section of the Astronomical Association of Queensland. The target stars were selected from the Washington Double Star Catalog (WDSC) and were observed in Queensland from a latitude of approximately 27° S.

Method

Once obtained with the equipment described above, the images were analyzed using the astrometric double star program REDUC (Losse, 2008). Approximately 10 stacked images of each target were taken per night for seven nights and the results averaged to obtain measures of separation and position angle with suffi-cient confidence.

Full details of the method are given in Napier-Munn and Jenkinson (2009). Some recent work on the errors inherent in the method is described in Napier-Munn and Jenkinson (2014). The images were obtained using a Meade DSI CCD camera in conjunction with an

equatorially mounted 150mm F8 refractor. For each target pair, either a 2x or 5x barlow lens was used as required. As proficiency has grown in the use of this equipment with the 150mm refractor, close doubles with considerable magnitude difference between the components have been successfully measured.

Results

For all of the systems the WDSC information is first reproduced, showing the epoch 2000 position, magnitudes, separation, PA, and the last recorded meas-urement. The new measurements are then given in tabu-lar form (Tables 2 - 8), including the mean and stand-ard deviation and 95% confidence limits. Any uncer-tainties between the images and the last recorded meas-urements are discussed. Finally a conclusion is given as to whether any movement of the component stars has occurred in PA or separation, based on the P-value for the t-test comparing the new mean values with the cata-loged value (P < 0.05 is considered as evidence of change).

Astronomical Association of Queensland Program of Measurements of Seven Southern Multiple Stars

Graeme Jenkinson

Astronomical Association of Queensland. [email protected]

Abstract: This paper presents the results of a mid-2014 program of the Astronomical Associa-tion of Queensland of photographic measurements of seven southern multiple stars. The images were obtained using a Meade DSI CCD camera in conjunction with an equatorially mounted 150mm F8 refractor. For each target pair, either a 2x or 5x barlow lens was used as required. Image processing was carried out using Losse’s REDUC software.

System

Last listed measure New measure

Comment PA º Sep. " Epoch PA º Sep. " Epoch*

B2350 Libra 202.0 9.3 1999 203.70 9.34 2014.335 Slow movement

HO554A-B Oph. 359.0 9.8 1904 355.89 9.59 2014.502 Definite change in PA

HO554A-C Oph 350.0 35.3 1999 350.08 35.94 2014.502 Possible increase in sep.

I 428 Circinus 315.0 11.0 2000 314.77 11.13 2014.330 No probable movement

I 1282 Scorpius 248.0 12.1 1998 251.39 12.70 2014.461 Definite change in PA

SEE114A-B Antlia 298.0 47.3 1999 298.57 52.58 2014.239 Changes since 1st measure

SEE234 Lupus 38.0 13.0 1999 37.04 13.33 2014.384 Little change

Table 1. Summary of Measurements of Seven Multiple Stars

* Epochs of new measures given in Besselian years as the average of the observations making up the measure.

mailto:[email protected]


… Measurements of Seven Southern Multiple Stars

The mean 95% confidence intervals for the new measures were ± 0º.305 in PA and ± 0².082 in separa-tion. The results are presented in Table 1.

Acknowledgements

This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Ob-servatory.

References

Losse F., Reduc software, V4.5.1. http://www.astrosurf.com/hfosaf/uk/tdownload.htm

Napier-Munn, T. J. and Jenkinson, G. 2009, "Mea-surement of Some Neglected Southern Multiple Stars in Pavo", Webb Society Double Star Section Circular 17, 6-12.

Napier-Munn, T.J. and Jenkinson, G., 2014, "Analysis of Errors in the Measurement of Double Stars Us-ing Imaging and the Reduc Software", Journal of Double Star Observations, 10, 193-198.

Argyle, Bob, 2004, Observing and Measuring Visual Double Stars, Springer

HO554A-C

Ophiuchus

RA. 17 01.2 DEC. -29.41 Last Measure 1999

MAG. 9.13 & 11.59 PA. 350.0° SEP. 35.3"

Date No. images PA° Sep"

27 June 2014 10 350.26 35.960

29 June 2014 10 350.20 35.893

30 June 2014 10 349.87 35.880

2 July 2014 10 349.73 36.003

3 July 2014 10 350.17 35.925

5 July 2014 10 350.12 35.972

8 July 2014 10 350.21 35.940

Mean 350.080 35.939

Standard dev. 0.200 0.044

95% CI +/- 0.185 0.040

P(t) movement 0.000 0.000

COMMENTS: A small increase in separation may have occurred in the

last 15 years.

Table 3. Measurements of HO 554 AC

B2350

Libra

RA. 15 09.9 DEC. -23 59 Last Measure 1999

MAG. 6.8 & 12.5 PA. 202.0° SEP. 9.3"


19 Apr 2014 10 204.26 9.248

21 Apr 2014 10 203.13 9.352

23 Apr 2014 10 203.90 9.489

25 Apr 2014 10 203.80 9.376

03 May 2014 10 203.76 9.396

21 May 2014 10 203.75 9.340

24 May 2014 10 203.31 9.156

Mean 203.701 9.337


95% CI +/- 0.347 0.099


COMMENTS: Slow changes evident since the first measures in 1953 of

201° and 10.3"

Table 2. Measurements of B 2350



Table 4. Measurements of I 428

I 428

Circinus


MAG. 5.8 & 11.6 PA. 315.0° SEP. 11.0"


18 Apr 2014 10 314.63 11.194

19 Apr 2014 10 314.60 11.097

21 Apr 2014 10 314.80 11.143

23 Apr 2014 10 314.86 11.041

25 Apr 2014 10 314.93 11.121

01 May 2014 10 314.43 11.071

17 May 2014 10 315.13 11.262

Mean 314.769 11.133


95% CI +/- 0.216 0.070


COMMENTS: No probable movement in the last 14 years.

I 1282

Scorpius


MAG. 6.03 & 13.0 PA. 248.0° SEP. 12.1"


25 May 2014 10 251.51 12.966

18 June 2014 10 251.50 12.794

22 June 2014 10 251.35 12.592

25 June 2014 10 251.72 12.713

26 June 2014 10 251.82 12.728

27 June 2014 10 250.89 12.489

29 June 2014 10 250.96 12.611

Mean 251.393 12.699


95% CI +/- 0.328 0.144


COMMENTS: Definite movement in PA, small increase in separation pos-

sible.

Table 5. Measurements of I 1282



Table 6. Measurements of SEE 114 AB

SEE114 A-B

Antlia


MAG. 6.0 & 12.8 PA. 298.0° SEP. 47.3"


28 Feb 2014 10 298.67 52.616

7 Mar 2014 10 298.55 52.632

13 Mar 2014 10 298.51 52.682

29 Mar 2014 10 298.72 52.500

30 Mar 2014 10 298.52 52.610

31 Mar 2014 10 298.50 52.502

18 April 2014 10 298.51 52.543

Mean 298.569 52.584


95% CI +/- 0.082 0.064


COMMENTS: Considerable increase in separation since the first measure

of 23.6" in 1897. Position angle has also increased from 283° at that

time.

SEE234

LUPUS


MAG. 6.1 & 12.5 PA. 38.0° SEP. 13.0"


25 Apr 2014 10 36.65 13.361

3 May 2014 10 37.90 13.319

21 May 2014 10 36.51 13.208

24 May 2014 10 36.87 13.463

25 May 2014 10 36.77 13.363

26 May 2014 10 37.55 13.251

7 June 2014 10 37.06 13.335

Mean 37.044 13.329

Standard devia-

tion 0.506 0.083

95% CI +/- 0.468 0.076


COMMENTS: Very slow changes since the first measure in 1897 of 31°

and 14.0"

Table 7. Measurements of SEE 234



Table 8. Measurements of HO 554 AB

HO554A-B

Ophiuchus


MAG. 7.9 & 12.9 PA. 359.0° SEP. 9.8"


27 June 2014 10 355.95 9.586

29 June 2014 10 356.39 9.545

30 June 2014 10 355.34 9.410

2 July 2014 10 355.43 9.648

3 July 2014 10 355.29 9.645

5 July 2014 10 356.67 9.634

8 July 2014 10 356.17 9.649

Mean 355.891 9.588

Standard devia-

tion 0.550 0.088

95% CI +/- 0.509 0.081


COMMENTS: Definite movement in PA and negligible change in separation

in the last 110 years.


Introduction

These latest results are a continuation of the Astro-nomical Association of Queensland’s program of meas-uring neglected southern multiple stars. Observed from an approximate latitude of 27°S, target stars were se-lected from the WDSC that met the criteria of a mini-mum of fifteen years since the last measure and prefer-ably with very few previous observations.

Method

All images were obtained using a Meade DSI 2 CCD camera coupled to an equatorially mounted 400mm F4.5 Newtonian reflector. Separations and position angles were measured using the software program REDUC (Losse), which is specifically designed to measure double stars, using appropri-ate images of the target pairs together with images of calibration pairs of known separation and PA; Argyle’s list of calibration pairs was used for this purpose (Argyle, 2004). For this optical/camera (Sony ICX429 752x582 pixel sensor) combination a FOV of approximately 0.2° was calculated using Argyle’s list. The use of REDUC requires input of the image scale of the particular camera/scope combination. By using the same information from the calibration pairs, the image scale mean can be calculated over a number of nights. In this case 10 images themselves consisting of 10 stacked images per night over 7 nights provided the necessary in-formation to calculate the mean. Using this optical

assembly to image calibration pairs Beta Tucanae, Theta Serpens, and Omicron Capricorni, raw im-age scales varied from 0.940 to 0.978, with a mean figure of 0.96260" per pixel. This figure is then used in REDUC for all the target star reductions. The imaging and reduction methods were de-scribed in detail in Napier-Munn & Jenkinson 2009.

In order to obtain statistically viable results, the DSI software is used to stack a minimum of 10 in-dividual good quality images as they are acquired, to generate one image for measuring. About 10 such images are obtained per pair per night, plus 3 trailed images with the tracking switched off in order to calibrate the E-W axis in the images. The REDUC software is then used to generate a single average measure for the 10 images. This process is repeated on 6-7 separate nights, generating mean separations and position angles together with standard deviations from which a confidence inter-val for the measurement can be calculated and a decision made as to whether there has been a sta-tistically significant change in PA or separation.

Results

The results are presented below, in order of increas-ing RA. For each system, the current WDSC infor-mation is first reproduced, including the epoch 2000 position, magnitudes (if known), PA, separation, and year of last measure. The new measures are then given

Astronomical Association of Queensland Program of Measurement of Nine Neglected Southern Multiple Stars

Graeme Jenkinson

Astronomical Association of Queensland E-mail: [email protected]

Abstract: Through the fir st half of 2015 measurements were completed for the following nine southern multiple stars as listed in the Washington Double Star Catalog. Using a 400mm F4.5 Newtonian reflector fitted with a Meade DSI 2 camera and software programme Astro-Planner V2.1 (Rodman) the obtained images were analyzed using Losse’s REDUC software.


… Measurement of Nine Neglected Southern Multiple Stars

in tabular form, including the date of measurement, mean, standard deviation, and 95% confidence limits

(from the formula st/√n, where t is the value of t for a

2-sided probability level (in this case = 0.05), s is the sample standard deviation, and n is the number of observations). An example of a relevant image used in the measures is included.

A conclusion is then given as to whether the pair has moved or not. This is based on judicious interpre-tation of three criteria in terms of both PA and separa-tion:

1. t-tests for a single sample mean comparing the new mean PA and separation values with the single

values given in the WDSC; P 0.05 was taken as evi-dence of movement (that is, the new mean is signifi-cantly different to the single value reported in the WDSC, with 95% or more confidence).

2. Whether the last measure as recorded in the WDSC lies within the 95% confidence interval of our new measure (suggesting no movement) or not (suggesting movement).

3. The absolute size of the change; a statistically significant change that is very small is still very small and may not be of practical significance.

Note that in a separate paper (Napier-Munn & Jen-kinson 2014) we have shown that the uncertainty in PA increases with decrease in separation, and the uncer-tainty in separation increases with increase in separa-tion, for reasons discussed in that paper. ‘Uncertainty’ here is defined as the standard deviation of repeated

measures. The mean 95% confidence intervals for the new

measures were ± 0.589° in PA and ± 0.134" in separa-tion. The results are given in Table 1.

Details of each measure are given in Tables 2 through 10 with examples of the measured images.

Acknowledgements

This research has made use of the Washington Double Star Catalogue maintained at the U.S. Naval Observatory.

References

Losse F., Reduc software, V4.5.1. http://www.astrosurf.com/hfosaf/uk/tdownload.htm

Napier-Munn, T. J. and Jenkinson, G. 2009,"Measurement of Some Neglected Southern Multiple Stars in Pavo", Webb Society Double Star Section Circular 17, 6-12.

Napier-Munn T.J. and Jenkinson, G. 2014, "Analysis of Errors in the Measurement of Double Stars Us-ing Imaging and the Reduc Software", Journal of Double Star Observations, 10, 193-198.

Argyle, Bob, 2004, Observing and Measuring Visual Double Stars, Springer

System

Last listed measure New measure

Comment

PA º Sep. " Epoch PA º Sep. " Epoch*

BU1419BC Puppis 300.0 7.8 1903 297.08 8.00 2015.083 Possible small PA change

SEE98 Puppis 67.0 5.9 1928 66.35 5.08 2015.043 Little evident movement

B2659 Pyxis 265.0 8.0 1932 172.79 18.61 2015.099 Large apparent movement

B2263 Vela 315.0 7.0 1932 21.63 12.38 2015.099 Considerable movement

CPO327 Centaurus 321.0 7.6 1930 324.34 6.55 2015.178 Movement

RST3746AB Cen 317.0 16.0 1944 325.97 14.81 2015.178 Clear movement

ARA1790 Corvus 184.0 11.3 1922 151.60 47.63 2015.303 Questionable Sep. change

RSS370 Lupus 148.0 7.2 1976 149.64 7.52 2015.308 Possible small PA

RSS386 TrA 270.0 10.3 1974 14.63 10.31 2015.308 Questionable PA change

* Epochs of new measures given in Besselian years as the average of the observations making up the measure.

Table 1. Summary of Measurements of Nine Multiple Stars.



Table 2. Measurements of BU 1419 BC.

Table 3. Measurements of HO 554 AC.

BU1419BC

Puppis


MAG. 7.55 &

13.0 PA. 300.0° SEP. 7.8"


16 January 2015 11 298.440 8.034

17 January 2015 10 297.130 8.113

30 January 2015 10 295.310 7.915

31 January 2015 9 298.250 7.777

6 February 2015 11 296.550 8.125

14 February 2015 10 297.380 8.131

15 February 2015 10 296.520 7.924

Mean 297.083 8.003


95% CI +/- 1.002 0.125


COMMENTS: Possible slight movement in PA over the last 112 years.

SEE98

Puppis


MAG. 6.7 & 12.7 PA. 67° SEP. 5.9"


6 January 2015 10 66.540 5.125

7 January 2015 10 66.380 5.134

8 January 2015 10 67.220 5.275

16 January 2015 10 66.750 5.612

17 January 2015 10 65.690 4.835

30 January2015 10 65.620 4.789

31 January 2015 10 66.220 4.787

Mean 66.346 5.080


95% CI +/- 0.526 0.282


COMMENTS:Little movement evident since 1929.



Table 4. Measurements of B 2659.

Table 5. Measurements of B 2263.

B2659

Pyxis


MAG. 7.7 &

13.2 PA. 265.0° SEP. 8.0"


17 January 2015 10 172.440 18.464

30 January 2015 10 172.940 18.639

31 January 2015 11 172.270 18.564

6 February 2015 10 173.220 18.625

14 February 2015 10 172.700 18.746

23 February 2015 10 173.020 18.607

24 February 2015 10 172.910 18.612

Mean 172.786 18.608


95% CI +/- 0.310 0.078


COMMENTS: Large apparent movement in both axes since the only

previous measurement in 1932 warrants further investigation.

B2263

Vela

RA. 11 03.2 DEC. -51 00 Last Measure

1932

MAG. 7.8 & 13.0 PA. 315.0° SEP. 7.0"


17 January 2015 10 21.660 12.232

30 January 2015 10 21.870 12.184

6 February 2015 10 21.000 12.407

14 February 2015 10 21.040 12.346

21 February 2015 10 23.330 12.143

23 February 2015 10 22.330 12.594

24 February 2015 9 21.880 12.497

Mean 21.630 12.377


95% CI +/- 0.547 0.164


COMMENTS: Poor seeing on 21 February 2015 – results deleted from

calculation of mean. Considerable movement apparent since the

only previous measure in 1932.



Table 6. Measurements of CPO 327.

Table 7. Measurements of RST 3746 AB.

CPO327

Centaurus


MAG. 8.0 & 12.8 PA. 321.0° SEP. 7.6"


21 February

2015 10 324.540 6.245

27 February

2015 10 325.720 6.348

7 March 2015 10 322.320 6.667

12 March 2015 10 323.680 6.532

14 March 2015 10 323.980 6.538

17 March 2015 10 325.640 6.710

19 March 2015 10 324.500 6.796

Mean 324.340 6.548


95% CI +/- 1.088 0.183


COMMENTS: Increase in PA and decrease in separation appear con-

sistent with the two previous measures in 1902 and 1930.

RST3746AB

CENTAURUS


MAG. 3.12 & 11.5 PA. 317.0° SEP. 16.0"


21 February 2015 10 326.260 14.684

27 February 2015 10 326.310 14.882

7 March 2015 10 325.880 14.774

12 March 2015 10 325.650 14.998

13 March 2015 10 326.020 14.510

14 March 2015 10 325.830 15.163

17 March 2015 10 325.830 14.640

Mean 325.969 14.807


95% CI +/- 0.224 0.207


COMMENTS: Changes in PA & separation consistent with two previ-

ous measures in 1937 & 1944.



Table 8. Measurements of ARA 1790.

Table 9. Measurements of RSS 370.

ARA 1790

Corvus


MAG. 8.8 & 11.1 PA. 184.0° SEP. 11.3"


16 April 2015 10 151.660 47.566

17 April 2015 10 151.720 47.724

22 April 2015 10 151.680 47.550

24 April 2015 10 151.680 47.479

26 April 2015 10 151.150 47.511

28 April 2015 10 151.510 47.773

29 April 2015 10 151.790 47.781

Mean 151.599 47.626


95% CI +/- 0.199 0.119


COMMENTS:Large increase in separation over 93 years. Change in

PA relative to separation change seems viable.

RSS 370

Lupus


MAG. 8.64 & -- PA. 148.0° SEP. 7.2"


14 April 2015 11 150.100 7.498

17 April 2015 10 150.230 7.520

18 April 2015 10 149.740 7.559

24 April 2015 10 151.040 7.587

26 April 2015 10 149.240 7.504

04 May 2015 10 148.840 7.615

05 May 2015 10 148.290 7.394

Mean 149.640 7.525


95% CI +/- 0.857 0.067


COMMENTS: Possible small increase in PA since the only previous

measure in 1976.



Table 10. Measurements of RSS 386.

RSS 386

Triangulum Aust.


MAG. 8.6 & 12.0 PA. 270° SEP. 10.3"


16 April 2015 10 14.460 10.246

17 April 2015 10 14.330 10.388

18 April 2015 10 13.590 10.285

24 April 2015 10 15.140 10.159

04 May 2015 10 14.870 10.378

05 May 2015 10 15.400 10.319

08 May 2015 10 14.610 10.364

Mean 14.629 10.306


95% CI +/- 0.549 0.077


COMMENTS: No change in separation makes large change in PA ques-

tionable over the last 41 years.


Instruments

These observations were carried out in Nikolaev Astronomical Observatory subordinated to Ministry of Education and Science of Ukraine. The observatory is located at an altitude of 52 m above sea level, the geo-graphic coordinates are longitude 31o 58´ E, and lati-tude 46o 58´ N [1]. The observations were made at the mobile multi-channel automatic telescope (Mobitel, Figure 1), which was created in the RI NAO. The main telescope is a Maksutov telescope (D = 500 mm, F = 3000 mm), that is equipped with an Alta U9000 CCD camera from Apogee Imaging Systems. The CCD has a sensor array of 3056 by 3056 pixels, and each pixel is 12 microns square which allows us to obtain imaging with scale 0.83"/pixel and FOV = 42.6´×42.6´ in drift scan mode. That system enables us to obtain a sufficient number of reference stars for astrometric re-duction in the UCAC4 catalog. For most stars the mean FWHM is less than 3".

Program and Processing

For the observational program, we selected WDS catalog [2] objects which are most appropriate to be observed by our telescope in the expected time frame (the full time of exposure is 85 s at the equator). For the main selection criteria we used a magnitude limit of 17

and a separation bigger than two FWHM. We also measured other WDS doubles from the observation vol-ume, which appeared in the imaged field.

All raw frames were processed using Astrometrica

[3] software. The star positions were obtained using reference stars from UCAC4 catalog [4]. Equatorial coordinates were calculated for all objects in the field of view. The mean number of observations per star was about 8. The coordinates in right ascension and declina-tion at mean observational epoch were averaged. Then we cross-matched our positional data with WDS cata-log and other astronomical catalogs for calculating the primary and secondary components proper motions and

Results of 194 Double Stars Measurements from Astrometric CCD Observations

at the Nikolaev Observatory (Ukraine)

Daniil Bodryagin, Larisa Bondarchuk, and Nadiia Maigurova

Research Institute "Nikolaev Astronomical Observatory", Nikolaev, Ukraine

[email protected]

Abstract: This paper presents the results of double stars measurements from CCD observations at the 50-cm telescope of the Nikolaev Observatory. The accurate positions at current epoch and proper motions were obtained for 194 WDS pairs. The position angles and separations were measured using REDUC software. The measures standard errors were 0.05" for separations and 0.2° for position angles.

Figure 1: The mobile multi-channel automatic telescope (Mobitel)


Results of 194 Double Stars Measurements from Astrometric CCD Observations at the Nikolaev ...

selecting all WDS doubles which appeared in the im-aged field.

Measurement

The measurements of doubles were made with RE-DUC software [5]. For calibration, we used previously determined exact values of orientation angle and image inclination regarding the celestial equator from astro-metric reductions. Position angle (Theta), separation (Rho), and their standard deviations were measured for each WDS double. The relationship between the stand-ard error of the positional angle and separation meas-urements versus the separation are shown in Figure 2.

Summary of the measurements is presented in Ta-ble 1. The table data set also includes estimation of magnitude difference between components made by REDUC software, date of observation, and number of observations for each WDS object.

References

1. http://www.mao.nikolaev.ua/

2. Mason B.D. et al: 2001, Astron. J., 122, 3466

3. http://www.astrometrica.at/

4. Zacharias N. et al: 2013, Astron. J., 145, 44Z

5. http://www.astrosurf.com/hfosaf/index.htm

Figure 2. Standard errors in positional angle (left) and separation vs separation.

http://www.mao.nikolaev.ua/

http://www.astrometrica.at/

http://www.astrosurf.com/hfosaf/index.htm



WDS no mag* Theta Std_Theta Rho Std_Rho Y M D N

00109+1705 5.82 98.1 1.5 13.46 0.27 2014 9 15 5

00146+2508 0.17 229.3 0.7 8.04 0.21 2014 10 11 9

00152+2454 1.38 159.6 0.2 31.27 0.15 2014 10 11 10

00197+1951 0.18 262.5 0.2 52.83 0.07 2014 10 9 10

00320+2509 1.32 228.9 0.2 38.10 0.12 2014 10 12 10

00374-0714 2.11 50.3 0.4 35.75 0.19 2014 10 11 9

00509+1215 2.82 95.6 1.1 24.36 0.43 2014 10 9 5

00541+1247 0.39 251.5 0.3 14.55 0.15 2014 10 1 10

00599+1400 2.54 158.5 0.2 45.74 0.21 2014 10 12 10

01116+0446 0.55 357.69 0.03 163.16 0.17 2014 10 6 8

01242+1254 0.03 217.1 0.1 28.58 0.30 2014 10 19 10

01493+1808 2.45 24.0 0.8 21.09 0.12 2014 10 14 10

01496+1741 4.17 343.9 0.2 24.30 0.13 2014 10 14 4

01598+1543 0.79 327.1 0.2 75.65 0.17 2014 10 19 10

02154+1126 0.98 162.7 0.3 43.19 0.31 2014 10 19 10

02476+1706 0.36 329.1 0.6 26.20 0.21 2014 10 19 10

02595+2440 0.59 210.5 0.4 13.73 0.12 2014 9 17 10

03134-0852 3.69 150.7 1.4 33.08 1.24 2014 10 19 10

03214+0803 1.01 84.5 1.2 4.31 1.23 2014 9 17 10

03216+0821 2.8 248.8 0.6 17.19 0.14 2014 9 17 10

03299+2417 3.48 13.5 0.2 26.17 0.37 2014 10 19 9

03308+2511 2.15 309.6 0.2 17.08 0.07 2014 9 19 5

03311+2437 1.55 50.5 0.1 14.47 0.08 2014 9 19 6

03308+2451 0.28 96.4 0.4 14.14 0.06 2014 9 19 5

03426+2430 0.59 344.5 2.2 3.54 0.71 2014 9 17 10

03435+2424 3.04 270.0 0.2 56.12 0.13 2014 9 17 10

03572-0706 2.13 104.4 0.2 65.73 0.06 2014 9 19 3

04026+1230 1.43 122.4 0.2 52.18 0.20 2014 9 14 7

04029+1228 1.25 339.7 0.2 39.78 0.18 2014 9 14 7

09225-0454 2.17 238.1 2.3 8.06 0.19 2014 3 18 10

09228-0516 3.37 309.9 0.3 33.64 0.22 2014 3 18 10

13040+2249 0.12 196.0 0.2 53.50 0.22 2014 3 21 9

13334+0636 1.92 78.2 0.1 165.13 0.22 2014 3 21 10

14491+0720 2.83 42.3 0.3 28.37 0.07 2013 4 29 10

16144+2740 0.04 39.7 0.2 38.08 0.03 2013 4 29 10

16244+3250 1.38 287.4 1.0 10.09 0.17 2013 5 25 10

16255+1944 0.14 339.8 0.5 7.87 0.09 2013 6 11 10

17018+1746 0.24 106.8 0.1 117.23 0.08 2013 5 27 10

17037+1336 0.0 116.55 0.01 304.94 0.03 2014 3 31 10

17126+1609 0.48 200.2 2.8 7.45 0.24 2013 6 19 10

17427+2459 0.08 123.9 1.5 6.44 0.12 2013 5 20 10

17512+2946 0.67 146.9 0.8 7.61 0.20 2013 7 11 10

17599+0435 0.41 359.7 0.2 26.98 0.11 2014 7 26 10

Table 1. Results of measurements of the 194 doubles stars using REDUC software.

Table 1 continues on next page.




18048+1253 0.56 277.1 0.4 18.62 0.13 2014 7 26 10

18057+1253 0.88 271.5 0.6 10.95 0.09 2014 7 26 10

18328+0633 1.05 58.3 0.6 12.16 0.09 2013 6 11 10

18331+0649 0.24 342.7 1.0 7.76 0.06 2013 6 11 10

18490+2405 0.81 273.4 1.0 9.58 0.15 2013 6 11 10

18491+2405 1.31 255.6 1.0 8.76 0.19 2013 6 11 10

18493+2411 0.9 106.5 1.3 7.47 0.26 2013 6 11 10

18499+2403 0.26 176.0 0.3 15.46 0.11 2013 6 11 9

18502+2414 0.88 169.5 0.5 8.90 0.11 2013 6 11 10

19328+1219 0.62 31.4 0.2 41.92 0.11 2013 7 9 10

19329+1223 1.54 148.7 0.1 112.96 0.14 2013 7 9 10

19332+1241 0.93 58.60 0.03 293.43 0.09 2013 7 9 10

19333+1248 0.49 193.9 0.1 37.64 0.05 2013 7 9 10

19338+1247 0.38 4.90 0.04 87.30 0.11 2013 7 9 5

19461+0131 0.51 257.1 0.4 10.38 0.07 2013 7 9 10

19503+1148 1.19 68.3 0.1 73.84 0.17 2013 6 11 10

19511+1140 1.34 237.84 0.04 140.99 0.12 2013 6 11 10

19568+2516 1.94 322.3 0.3 10.84 0.13 2013 6 19 6

20029+1328 0.36 56.56 0.02 80.40 0.14 2013 6 19 3

20030+1328 0.48 169.7 0.2 56.61 0.16 2013 6 19 3

20033+1354 0.82 40.31 0.05 47.94 0.08 2013 6 19 3

20033+1347 2.02 140.85 0.03 117.17 0.05 2013 6 19 3

20221+0331 2.56 217.4 0.5 20.51 0.13 2013 6 11 10

20253+0355 1.51 87.0 0.3 20.53 0.08 2013 6 11 10

20305+2411 0.45 220.0 0.2 20.56 0.10 2013 6 11 10

20305+2358 1.31 140.9 0.4 19.05 0.07 2013 6 11 10

20306+2417 0.79 228.9 0.3 17.91 0.13 2013 6 11 10

20306+2406 0.16 59.3 0.1 16.16 0.12 2013 6 11 10

20308+2416 0.27 248.5 0.3 22.51 0.14 2013 6 11 10

20308+2404 1.26 227.0 0.9 8.33 0.29 2013 6 11 10

20311+2429 0.15 281.8 0.4 13.17 0.11 2013 6 11 10

20313+2406 0.97 245.3 0.3 11.81 0.11 2013 6 11 6

20359+2331 0.87 292.8 0.4 17.90 0.10 2014 9 19 8

20359+2327 1.07 152.1 0.6 18.42 0.11 2014 9 19 8

20365+2334 2.35 56.6 0.2 18.28 0.10 2014 9 19 8

20365+2327 1.04 226.6 0.3 17.10 0.08 2014 9 19 8

20366+2342 0.25 22.5 0.8 6.75 0.20 2014 9 19 8

20367+2328 1.6 24.9 0.3 19.9 0.08 2014 9 19 8

20367+2327 0.61 300.7 0.6 8.23 0.20 2014 9 19 8

20367+2319 1.12 240.6 2.7 5.27 0.24 2014 9 19 9

20367+2316 2.48 331.8 0.8 7.87 0.09 2014 9 19 9

20368+2324 1.02 76.3 0.4 15.01 0.12 2014 9 19 9

20369+2330 0.93 326.3 0.3 17.29 0.16 2014 9 19 8

20369+2325 1.69 268.2 0.5 17.94 0.12 2014 9 19 9

20363+2321 0.82 134.1 0.3 21.57 0.19 2014 9 19 9

Table 1 (continued). Results of measurements of the 194 doubles stars using REDUC software.





20397+1415 0.97 147.1 0.3 32.54 0.13 2013 6 11 10

20397+1406 1.57 285.6 1.8 6.46 0.58 2013 6 11 10

20401+2509 2.07 288.9 0.4 10.36 0.11 2014 8 30 10

20401+2458 0.34 24.1 1.1 16.11 0.30 2014 8 30 9

20401+2450 0.4 34.5 1.6 5.63 0.22 2014 8 30 10

20412+2448 1.54 139.2 0.2 15.47 0.13 2014 8 30 10

20415+2459 1.42 197.7 0.6 8.83 0.10 2014 8 30 10

20417+2449 0.72 35.7 0.7 8.40 0.10 2014 8 30 9

20417+2437 2.99 94.1 0.6 8.37 0.10 2014 8 30 8

20401+2516 0.51 339.6 0.3 21.87 0.13 2014 9 17 10

20401+2513 1.1 296.1 0.2 18.58 0.05 2014 9 17 10

20408+2521 1.54 232.6 0.4 16.89 0.13 2014 9 17 10

20408+2505 3.2 302.7 0.3 18.68 0.06 2014 9 17 10

20413+2513 2.06 244.9 0.5 13.26 0.13 2014 9 17 10

20478+1109 0.64 58.3 0.2 48.63 0.09 2013 8 8 10

20487+2517 1.31 78.3 0.7 14.63 0.13 2014 8 20 10

20491+2509 0.09 101.1 0.6 8.81 0.18 2014 8 20 10

20492+2504 0.78 68.2 1.5 3.93 0.08 2014 8 20 10

20492+2510 1.2 355.6 1.8 5.98 0.10 2014 8 20 10

20495+2516 1.38 80.2 1.0 8.58 0.09 2014 8 20 10

20497+2507 1.42 276.1 0.8 9.61 0.16 2014 8 20 10

20497+2526 0.1 336.3 0.3 14.64 0.10 2014 8 20 10

20499+2454 0.41 53.8 0.7 9.69 0.14 2014 8 20 10

20499+2456 1.04 235.2 1.1 8.27 0.22 2014 8 20 10

20499+2508 0.22 341.7 1.5 4.55 0.16 2014 8 20 10

20499+2510 1.49 19.5 0.2 12.23 0.14 2014 8 20 10

20500+2508 0.89 253.9 0.7 12.48 0.19 2014 8 20 10

20501+2512 3.11 341.6 0.5 16.14 0.13 2014 8 20 10

20503+2507 2.78 83.9 0.4 10.72 0.10 2014 8 20 10

20543+2441 0.99 201.8 0.7 9.14 0.14 2014 9 2 11

20573+1434 0.68 60.9 0.2 72.94 0.12 2014 9 19 9

20580+1426 0.58 339.3 0.2 14.31 0.12 2014 9 19 10

21017+2516 0.59 167.3 0.8 6.79 0.07 2014 9 17 10

21024+2518 0.54 124.5 0.3 21.44 0.09 2014 9 17 10

21026+2515 0.47 353.4 0.4 16.86 0.15 2014 9 17 10

21027+2508 0.58 25.4 0.6 10.04 0.12 2014 9 17 10

21020+2515 0.83 312.0 0.2 18.30 0.12 2014 9 17 10

21057+2412 0.17 245.9 0.1 16.03 0.27 2014 8 30 3

21060+1443 0.34 137.3 0.1 68.31 0.08 2013 11 1 8

21060+2406 3.08 188.2 0.6 11.00 0.08 2014 8 30 10

21062+2346 0.51 76.4 0.4 15.19 0.09 2014 8 30 10

21065+2332 0.02 190.3 2.3 4.89 0.46 2014 8 30 10

21066+2347 2.17 223.1 0.4 20.09 0.09 2014 8 30 10

21068+2400 0.08 169.0 0.7 12.25 0.14 2014 8 30 10

21069+0458 4.61 271.4 0.1 53.01 0.08 2013 8 8 10






21070+1500 0.42 317.4 0.1 38.13 0.08 2013 11 1 8

21071+2332 0.29 86.1 0.4 11.48 0.08 2014 8 30 10

21101+2516 1.77 249.9 0.5 12.14 0.10 2014 8 20 10

21104+2512 0.75 247.0 1.7 5.38 0.09 2014 8 20 10

21105+2452 1.0 190.8 1.4 6.17 0.17 2014 8 20 10

21107+2512 0.36 138.9 0.5 13.93 0.14 2014 8 20 10

21108+2445 2.44 58.7 0.4 14.52 0.10 2014 8 20 10

21108+2452 0.63 145.0 1.0 8.11 0.08 2014 8 20 10

21110+2448 0.59 84.5 0.8 11.83 0.10 2014 8 20 10

21110+2519 2.13 194.0 0.3 13.83 0.06 2014 8 20 10

21185+2454 1.99 31.9 0.8 9.13 0.12 2014 8 28 10

21189+2504 1.24 166.3 0.2 16.87 0.11 2014 8 28 10

21194+2513 0.12 53.7 0.6 9.87 0.11 2014 8 28 9

21198+2435 0.81 85.2 1.2 5.85 0.32 2014 8 28 6

21200+2440 1.04 267.3 0.6 11.44 0.09 2014 8 28 9

21223+1111 0.9 191.1 1.3 4.16 0.25 2014 10 12 9

21227+1101 1.45 336.1 0.1 96.62 0.14 2014 10 12 10

21229+2346 0.09 192.2 0.4 13.84 0.13 2014 9 17 10

21240+2352 0.61 240.7 1.2 7.16 0.19 2014 9 17 10

21233+2401 1.02 49.3 0.5 12.71 0.08 2014 9 17 10

21282+1519 2.32 174.2 0.6 11.11 0.18 2013 8 8 10

21314+2451 2.68 127.0 0.4 17.23 0.12 2014 8 10 8

21315+2503 1.25 18.4 1.1 8.83 0.09 2014 8 20 10

21326+2522 1.11 66.4 0.2 36.63 0.11 2014 8 20 10

21329+2509 2.35 192.0 0.6 14.57 0.08 2014 8 20 10

21447+2402 1.99 298.4 0.8 7.06 0.10 2014 9 17 6

21462+2353** 0.23 128.6 0.8 8.13 0.19 2014 9 17 6

21462+2353** 0.99 212.2 0.5 19.65 0.11 2014 9 17 6

21455+2349 0.11 39.4 0.3 12.76 0.07 2014 9 17 10

21449+1040 0.22 55.0 0.9 7.89 0.09 2014 8 30 9

21528+2458 0.09 178.3 0.7 10.38 0.16 2014 8 20 10

21529+2525 0.03 11.9 0.3 23.47 0.14 2014 8 20 10

21534+2447 1.26 100.1 0.3 9.91 0.12 2014 8 20 10

21536+2516 1.57 322.9 0.3 18.07 0.17 2014 8 20 10

21539+2446 1.17 359.9 0.5 15.52 0.15 2014 8 20 10

21545+1615 1.49 20.2 1.1 8.44 0.11 2013 8 8 9

22010+2439 2.14 19.9 0.6 14.15 0.05 2014 8 28 10

22010+2453 0.09 178.8 0.5 12.25 0.14 2014 8 28 10

22016+2421 0.59 135.9 0.9 7.78 0.12 2014 8 28 10

22017+2446 0.85 78.0 0.5 13.82 0.11 2014 8 28 10

22021+2422 0.64 255.5 1.3 4.82 0.42 2014 8 28 10

22024+2420 0.7 65.0 0.5 7.40 0.10 2014 8 28 9

22138+2408 2.03 248.3 0.5 14.51 0.17 2014 8 20 10

22146+2342 0.2 28.5 0.4 16.94 0.08 2014 8 20 10

22312+0253 1.24 168.0 0.2 20.44 0.10 2014 8 30 10


Table 1 concludes on next page.




22335+1519 0.48 263.0 1.2 42.30 0.24 2014 10 19 10

22351+0346 2.1 289.31 0.04 369.81 0.13 2014 8 20 9

22428+2947 1.06 276.6 0.3 25.45 0.12 2014 8 28 10

22429+2958 0.79 52.4 0.3 28.49 0.12 2014 8 28 10

22430+2944 0.43 124.3 0.5 13.63 0.13 2014 8 28 10

22432+2941 0.63 283.9 0.5 18.06 0.11 2014 8 28 10

22439+2938 0.07 227.7 0.7 9.12 0.13 2014 8 28 10

22441+2940 1.46 149.9 0.2 23.85 0.10 2014 8 28 10

22443+2957 0.27 218.5 0.2 24.58 0.10 2014 8 28 10

22481+2444 0.74 38.9 0.1 41.25 0.15 2014 9 17 6

22482+2434 0.08 195.7 0.4 11.84 0.08 2014 9 17 10

22578+1833 0.62 80.8 0.5 16.85 0.08 2014 10 14 8

22574+1827 0.11 183.9 0.1 111.56 0.09 2014 10 14 9

23232-0839 2.02 94.4 0.7 157.30 0.13 2014 10 19 10

23527-0328 3.47 1.6 0.7 6.04 0.62 2014 10 14 4

23523-0341 1.9 178.6 0.1 277.12 0.10 2014 10 14 10

23533+0208 0.23 1.2 0.8 15.64 0.19 2013 11 1 4

Table 1 (conclusion). Results of measurements of the 194 doubles stars using REDUC software.

Notes: * all observations were obtained with filter close to Rc band;

** this star is triple and has two records in WDS; we measured both in the same order as in the catalog.


Jonckheere Double Star Photometry – Part II: Delphinus

Wilfried R.A. Knapp

Amateur visual double star astronomer Vienna, Austria

[email protected]

Abstract: If any double star discoverer is in urgent need of photometry then it is Jonckheere. There are over 3000 Jonckheere objects listed in the WDS catalog and a good part of them have magni-tudes which are obviously far too bright. To keep the workload manageable only one image per object is taken and photometry is done with a software allowing a simple point and click procedure – even a sin-gle measurement is better than the currently usually given estimation

Introduction

As follow up to the first report on J-objects in Cyg-nus (Knapp; Nanson 2016) I selected for this report all J-objects in Delphinus (Del) (plus ROE14AB in combi-nation with J563BC) given in Table 1 with all values based on WDS data as of April 2015.

Photometry

For each of the listed J-objects one single image was taken (in Bessel epoch 2015.683) with iTelescope iT24 with 3 second exposure time. The imaging ses-sions were not straight forward as in previous sessions in Cygnus, mostly due to uncooperative weather condi-tions. So, for several objects repeated imaging sessions were required and in a few cases I had to resort to an-other telescope location. In these cases, the different Bessel epochs and different scopes are indicated in the notes column. In all cases the initial plate solving was done by AAVSO VPhot and in the few cases with neg-ative VPhot result, but positive with MaxIm PinPoint. Each image was then once more plate solved with Astrometrica, using the UCAC4 catalog with ref-erence stars in the Vmag range of 10.5 to 14.5 giving not only RA/Dec coordinates but also photometry re-sults for all reference stars used including an average dVmag error. The J-objects were then located in the center of the image with a few exceptions, indicating that the given RA/Dec coordinates are usually correct with the exceptions suggesting position problems. Pho-tometry was then done using the Astrometrica proce-dure with point and click at the components delivering

Vmag measurements based on all reference stars used for plate solving. The only changing parameter was the aperture radius used for photometry aiming to keep it equal or at least near 1.5x FWHM. In cases with small-er separation the star disks touched or overlapped but, nevertheless individual photometry could be done though less reliable than with clearly separated disks. Several cases allowed only the measurement of the combined magnitude, but even in these cases it is pos-sible to make a well-founded estimate for the compo-

nents based on the initial observed m between the components based on the formula

according to Greaney 2012.

Summary

Table 2 shows, with few exceptions, quite large differences for the magnitudes compared with the WDS data, often even in cases where double digit val-ues suggest recent precise measurements. A few cases suggest errors in position, separation, and position an-gle, Several times the images suggest the non-existence of the objects in question.

References

Buchheim, Robert, 2008, "CCD Double-Star Measure-ments at Altimira Observatory in 2007", Journal of Double Star Observations, 4, 27-31.

1` 2102.5log 2.521 2.521

m mcombinedm




Greaney, Michael, 2012, "Some Useful Formulae" in R.W. Argyle, Observing and Measuring Visual Double Stars, 2nd Edition 2012, Chapter 25, Page 359, Springer.

Knapp, Wilfried and Nanson, John, 2016, "Jonckheere Double Star Photometry – Part I: Cyg", JDSO, 12, 168-179.

Acknowledgements

The following tools and resources have been used

for this research:

AAVSO APASS (via the UCAC4 catalog) AAVSO VPhot Aladin Sky Atlas v8.0

Astrometrica v4.8.2.405 AstroPlanner v2.2 iTelescope iT24 & iT27 MaxIm DL6 v6.08 SIMBAD, VizieR

WDS ID Name C RA Dec Sep M1 M2 PA

WDS20329+1142 J1 AB 20:32:52.760 +11:44:37.200 2.0 10.04 10.57 57

WDS20316+1150 J3 AB 20:31:33.391 +11:50:24.800 2.0 10.00 10.00 129

WDS20157+1003 J135 AB 20:15:43.430 +10:02:08.901 3.6 11.42 11.58 322

WDS20345+1138 J142 AB 20:34:25.910 +11:37:17.500 6.5 10.35 12.50 241

WDS20403+0349 J156 AB 20:40:20.583 +03:50:04.000 2.3 10.95 11.64 21

WDS20559+0835 J157 AB 20:55:51.537 +08:34:17.901 3.8 11.32 10.93 172

WDS20409+1738 J191 AB 20:40:52.162 +17:37:59.203 1.2 9.30 9.60 141

WDS20416+1058 J192 AB 20:42:36.580 +11:00:55.100 5.5 9.40 13.10 133

WDS20420+1821 J193 AB 20:42:02.550 +18:21:02.302 5.3 9.11 12.10 83

WDS20494+1124 J194 AB 20:49:23.528 +11:24:09.601 0.6 10.32 9.97 155

WDS20494+1124 J194 AB,C 20:49:23.528 +11:24:09.601 11.2 10.32 13.94 33

WDS20509+1907 J195 AB 20:50:53.568 +19:06:42.697 3.4 11.40 11.40 26

WDS21033+1655 J284 AB 21:03:12.192 +16:53:25.900 2.8 9.50 11.10 235

WDS20298+1712 J510 AB 20:29:45.690 +17:11:55.697 3.5 9.91 13.70 242

WDS20181+1555 J553 AB 20:18:06.692 +15:54:09.498 3.6 9.40 10.50 21

WDS20271+0948 J559 AB 20:27:06.862 +09:48:52.100 2.0 11.65 11.45 279

WDS20311+1248 J562 AB 20:31:07.271 +12:46:52.799 2.2 10.80 11.70 145

WDS20311+1648 ROE14 AB 20:31:03.178 +16:48:41.299 7.1 11.00 12.00 213

WDS20311+1648 J563 BC 20:31:02.691 +16:48:40.399 5.0 12.00 12.30 213

WDS20351+1533 J566 AB 20:35:09.952 +15:32:10.099 4.2 10.90 12.20 120

WDS20527+0527 J572 AB 20:52:39.400 +05:26:20.900 3.4 10.20 11.30 138

WDS20534+1921 J573 AB 20:53:18.532 +19:22:30.199 3.9 11.30 11.70 187

WDS20151+1143 J604 AB 20:15:05.438 +11:42:41.500 0.7 10.23 10.44 235

WDS20527+1726 J605 AC 20:52:44.069 +17:26:12.700 38.2 11.55 12.16 161

WDS20527+1726 J605 AB 20:52:44.069 +17:26:12.700 1.7 11.40 11.90 241

WDS20571+1801 J607 AB 20:57:05.297 +18:00:59.903 3.1 10.80 12.40 305

WDS20348+1857 J790 AB 20:34:54.001 +18:56:42.397 2.3 9.50 10.00 88

WDS21056+1749 J797 AB 21:05:37.301 +17:49:46.503 3.4 12.30 13.80 214

WDS20198+1203 J837 AB 20:19:52.010 +12:03:10.400 2.0 11.10 11.70 297

WDS20210+1028 J838 AB 20:21:00.667 +10:28:20.999 6.5 11.52 12.00 118

Table 1: WDS April 2015 values for the Jonckheere objects in Del sorted by designation number





WDS20235+1811 J839 AB 20:23:35.739 +18:10:40.901 1.9 11.50 11.70 350

WDS20249+1124 J840 AB 20:24:46.958 +11:23:38.599 3.8 9.50 10.50 51

WDS20249+1309 J841 AB 20:24:56.070 +13:08:58.000 0.2 10.50 11.50 274

WDS20249+1309 J841 AB.C 20:24:56.070 +13:08:58.000 8.4 10.10 10.50 82

WDS20250+1451 J842 AB 20:24:57.972 +14:51:16.501 4.2 10.04 12.10 179

WDS20314+2054 J844 AB 20:30:50.688 +20:53:41.603 4.1 12.20 12.80 118

WDS20434+1712 J845 AB 20:43:21.981 +17:12:28.499 4.0 11.99 12.20 224

WDS20541+1402 J846 AB 20:54:07.202 +14:02:13.000 3.3 10.80 11.14 157

WDS20396+1310 J912 AB 20:39:39.021 +13:09:45.400 1.8 10.00 10.00 125

WDS20385+1118 J1073 AB 20:38:25.577 +11:16:24.701 5.3 9.70 14.00 113

WDS20209+1332 J1173 AB 20:20:50.478 +13:31:04.600 3.7 10.41 13.70 83

WDS20157+0957 J1234 AB 20:15:42.778 +09:56:37.900 4.4 12.51 15.00 43

WDS20280+1244 J1241 AB 20:28:00.112 +12:44:08.100 1.1 10.33 12.30 168

WDS20386+1120 J1242 AB 20:38:30.871 +11:18:39.201 5.1 9.60 11.00 204

WDS20298+1154 J1243 AB 20:30:22.240 +11:54:28.999 3.2 10.80 10.80 121

WDS20146+1116 J1296 AB 20:14:28.497 +11:17:34.602 3.3 11.90 12.40 236

WDS20276+0745 J1297 AB 20:27:33.147 +07:44:07.799 1.2 11.23 11.27 14

WDS20554+0836 J1318 AB 20:55:23.570 +08:35:38.200 0.8 10.30 10.77 142

WDS20247+0302 J1342 AB 20:24:44.823 +03:05:03.200 2.7 9.40 11.50 307

WDS20270+1008 J1343 AB 20:27:01.891 +10:11:16.301 2.4 9.60 10.00 54

WDS20348+1121 J1344 AB 20:34:45.562 +11:20:14.199 2.3 9.10 11.50 103

WDS20438+1440 J1345 AB 20:43:47.751 +14:39:14.501 3.7 9.60 10.50 280

WDS20560+0837 J1346 AB 20:56:00.223 +08:35:46.100 2.4 13.20 13.20 327

WDS20260+1212 J1704 AB 20:26:02.949 +12:11:07.001 6.0 10.16 10.80 202

WDS20586+0723 J1715 AB 20:58:36.422 +07:23:15.399 5.2 11.61 13.00 125

WDS20593+1744 J1716 AB 20:59:15.210 +17:43:17.099 6.4 10.00 11.00 224

WDS20169+1303 J1879 AB 20:16:56.723 +13:02:42.601 10.9 11.83 11.95 233

WDS20169+1303 J1879 AC 20:16:56.723 +13:02:42.601 13.7 11.83 14.40 272

WDS20172+1304 J1880 AB 20:17:08.121 +13:04:32.001 13.5 11.23 13.30 246

WDS20303+0917 J1883 AB 20:30:08.851 +09:20:52.201 6.4 11.53 12.00 115

WDS20315+1448 J1884 AB 20:31:23.290 +14:50:01.400 8.6 9.80 9.80 131

WDS20315+1446 J1885 AB 20:31:24.148 +14:47:04.200 11.9 12.00 12.00 353

WDS20351+1413 J1887 AB 20:35:04.623 +14:13:40.799 5.5 11.68 11.70 280

WDS20439+1255 J1888 AB 20:43:49.688 +12:53:40.501 9.8 9.70 12.50 159

WDS20441+1258 J1889 AB 20:44:04.073 +12:31:48.799 4.8 14.30 14.30 15

WDS20485+1448 J1890 AB 20:48:29.901 +14:50:57.100 6.8 11.20 11.50 140

WDS20360+0411 J2192 AB 20:36:31.120 +04:15:22.100 4.9 9.90 12.50 17

WDS20305+1829 J2313 AB 20:30:30.178 +18:29:07.801 6.0 9.50 11.90 133

WDS20327+0453 J2314 AB 20:32:40.229 +04:52:49.300 4.9 10.60 11.60 70

WDS20327+0453 J2314 AC 20:32:40.229 +04:52:49.300 17.6 10.60 14.00 154

WDS20415+1611 J2319 AB 20:41:16.627 +16:12:44.999 7.0 9.80 12.00 188

WDS20488+0512 J2321 AB 20:48:50.727 +05:11:58.101 6.6 9.61 10.80 151

WDS20518+1736 J2325 AB 20:51:50.799 +17:36:17.401 5.3 11.60 13.70 260

WDS20230+0929 J2572 AB 20:23:08.260 +09:28:43.700 4.1 9.80 13.20 281

WDS20321+0330 J2573 AB 20:32:27.519 +03:29:17.300 4.0 12.50 12.80 150

Table 1 (continued): WDS April 2015 values for the Jonckheere objects in Del sorted by designation number





WDS20418+1404 J2575 AB 20:41:55.059 +14:05:23.400 0.7 9.70 13.00 311

WDS20393+1101 J2603 AB 20:39:18.160 +10:59:36.201 1.8 11.39 13.40 354

WDS20398+1927 J2604 AB 20:39:44.109 +19:26:07.502 2.0 12.12 12.10 142

WDS21058+1939 J2702 AB 21:05:43.851 +19:40:09.899 5.4 11.20 11.60 178

WDS20152+1357 J3066 AB 20:15:23.751 +14:00:30.401 4.5 11.00 11.50 334

WDS20152+1357 J3066 AC 20:15:23.751 +14:00:30.401 9.1 11.00 15.00 215

WDS20227+1345 J3079 AB 20:22:29.808 +13:45:35.300 7.6 12.90 13.30 139

WDS20227+2023 J3080 AB 20:22:46.940 +20:22:23.401 7.4 12.00 13.00 292

WDS20228+2023 J3081 AB 20:22:51.403 +20:22:15.999 6.3 10.00 11.00 0

WDS20229+1346 J3082 AB 20:23:07.148 +13:47:43.401 6.1 14.20 15.80 19

WDS20259+0902 J3084 AB 20:25:53.487 +09:02:12.701 5.8 12.03 12.90 88

WDS20263+1445 J3085 AB 20:26:15.488 +14:45:35.201 6.1 9.80 9.80 204

WDS20275+1514 J3087 AB 20:27:27.633 +15:13:46.000 5.6 10.50 11.60 328

WDS20293+1029 J3088 AB 20:29:20.690 +10:27:58.399 7.4 10.50 11.30 80

WDS20295+1033 J3089 AB 20:29:21.321 +10:31:41.301 4.6 11.60 12.30 316

WDS20314+2049 J3091 AB 20:31:34.228 +20:51:20.402 5.7 11.20 11.50 116

WDS20326+1024 J3092 AB 20:32:36.301 +10:23:49.902 5.3 12.10 12.60 335

WDS20334+1359 J3093 AB 20:33:25.012 +13:58:46.299 4.2 12.80 12.80 43

WDS20339+1915 J3094 AB 20:33:54.002 +19:14:56.299 7.4 11.10 14.80 22

WDS20363+1636 J3095 AB 20:36:07.760 +16:35:11.002 5.3 12.40 12.40 179

WDS20365+2044 J3096 AB 20:36:33.647 +20:43:53.100 21.9 10.50 12.60 2

WDS20365+2044 J3096 BC 20:36:33.880 +20:44:20.902 8.3 12.60 13.10 9

WDS20370+1420 J3098 AB 20:36:59.822 +14:21:15.300 4.9 12.60 13.10 303

WDS20378+1936 J3099 AB 20:37:26.869 +19:38:08.898 5.5 12.50 12.70 147

WDS20385+1848 J3102 AB 20:38:44.027 +18:49:32.097 6.2 11.60 12.10 97

WDS20393+2003 J3103 AB 20:39:30.499 +20:03:30.903 5.7 12.05 12.42 224

WDS20397+1406 J3104 AB 20:39:44.061 +14:06:00.698 6.3 9.90 11.20 286

WDS20416+1738 J3107 AB 20:41:23.013 +17:39:12.502 5.9 11.70 11.70 120

WDS20436+1537 J3108 AB 20:43:43.041 +15:38:59.501 6.2 11.00 12.50 197

WDS20433+1728 J3109 AB 20:43:20.107 +17:27:50.203 7.9 12.50 13.10 245

WDS20466+1532 J3110 AB 20:46:29.353 +15:31:51.501 6.7 11.20 11.50 222

WDS20509+1517 J3113 AB 20:51:01.663 +15:19:44.999 4.8 11.50 11.50 112

WDS20513+1647 J3115 AB 20:51:14.387 +16:46:12.798 7.2 12.16 15.20 318

WDS20522+1656 J3116 AB 20:52:09.600 +16:56:13.002 73.3 8.77 12.88 39

WDS20522+1656 J3116 BC 20:52:12.841 +16:57:09.897 5.9 13.30 14.80 139

WDS20585+1607 J3118 AB 20:58:30.880 +16:06:43.899 5.8 9.40 11.20 74

WDS21081+1857 J3125 AB 21:08:17.131 +18:57:53.801 4.7 12.40 13.60 258

WDS20285+0443 J3220 AB 20:28:18.933 +04:41:49.300 3.9 10.75 12.50 181

WDS20314+0701 J3221 AB 20:31:15.792 +06:59:14.300 3.8 10.00 11.60 166

WDS20487+0706 J3223 AB 20:48:44.561 +07:05:43.700 3.5 10.69 11.40 310

WDS20311+1247 J3244 AB 20:31:07.999 +12:45:59.000 4.6 11.38 12.90 160

WDS20519+1203 J3245 AB 20:51:51.877 +12:01:57.598 3.8 11.80 12.60 249

WDS20289+1022 J3263 AB 20:28:49.413 +10:23:15.099 7.1 11.30 12.10 55

WDS20292+1019 J3264 AB 20:29:10.829 +10:19:27.699 6.3 11.64 12.30 358

WDS20502+1246 J3277 AB 20:50:05.372 +12:42:41.500 4.1 10.70 12.50 327

WDS20555+1730 J3328 AB 20:55:28.239 +17:29:14.997 3.9 11.99 14.70 122

Table 1 (conclusion): WDS April 2015 values for the Jonckheere objects in Del sorted by designation number



WDS ID Name M1 WDS M1 new dM1 Err M1 M2 WDS M2 new dM2 Err M2 Notes

20329+1142 J1 AB 10.04 9.650 0.39 0.070 10.57 10.180 0.39 0.070 Overlapping star disks

- no separate photome-

try possible. Combined

magnitude 9.118 with

SNR 238.97 gives esti-

mated “M1 new” and “M2

new” values not con-

firming the current,

seemingly a bit too

faint, WDS values

20316+1150 J3 AB 10.00 11.946 -1.95 0.074 10.00 12.127 -2.13 0.074 Touching/overlapping

star disks

20157+1003 J135 AB 11.42 11.216 0.20 0.102 11.58 11.455 0.13 0.103 Touching star disks

20345+1138 J142 AB 10.35 10.285 0.06 0.080 12.50 12.523 -0.02 0.084

20403+0349 J156 AB 10.95 10.698 0.25 0.081 11.64 11.083 0.56 0.081 Touching/overlapping

star disks

20559+0835 J157 AB 11.32 11.484 -0.16 0.083 10.93 11.130 -0.20 0.082 Touching star disks

20409+1738 J191 AB 9.30 10.880 -1.58 0.140 9.60 11.180 -1.58 0.140 Overlapping star disks






new” values suggest-

ing much fainter mag-

nitudes than currently

WDS listed

20416+1058 J192 AB 9.40 11.381 -1.98 0.081 13.10 14.559 -1.46 0.158 Very low SNR <10 for

B.

20420+1821 J193 AB 9.11 8.976 0.13 0.080 12.10 11.675 0.42 0.083







new” values confirm-

ing rather well the

current WDS values

20494+1124 J194 AB.

C

10.32 9.325 1.00 0.090 13.94 14.005 -0.07 0.126 WDS gives here obvi-

ously M1 for A and not

AB combined. WDS value

for C well confirmed

20509+1907 J195 AB 11.40 12.365 -0.97 0.114 11.40 12.385 -0.98 0.115


20298+1712 J510 AB 9.91 9.829 0.08 0.090 13.70 13.052 0.65 0.106

20181+1555 J553 AB 9.40 10.641 -1.24 0.080 10.50 11.897 -1.40 0.082

20271+0948 J559 AB 11.65 11.350 0.30 0.088 11.45 11.248 0.20 0.089 Overlapping/Touching

star disks


20311+1648 ROE14 AB 11.00 11.457 -0.46 0.091 12.00 12.630 -0.63 0.094 ROE14 AB as "bonus"

20311+1648 J563 BC 12.00 12.630 -0.63 0.094 12.30 13.193 -0.89 0.097

20351+1533 J566 AB 10.90 10.126 0.77 0.130 12.20 11.252 0.95 0.131

20527+0527 J572 AB 10.20 9.927 0.27 0.120 11.30 11.446 -0.15 0.126 Touching star disks

20534+1921 J573 AB 11.30 11.766 -0.47 0.081 11.70 12.925 -1.23 0.086

Table 2. Bessel epoch 2015.683 (exceptions see notes column) photometry results for the J objects in Del. “M1 WDS” and “M2 WDS” are the WDS catalog values. “M1 new” stands for measured M1, “dM1” stands for delta between “M1 WDS” and “M1 new”. “M2 new” stands for measured M2, “dM2” stands for delta “M1 WDS” and “M1 new”. “Err M1” stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula .


2 210(2.5log (1 1/ ))magdV SNR











ing rather well the

current WDS values

20527+1726 J605 AC 11.55 11.665 -0.11 0.111 12.16 12.160 - 0.112 WDS values for A with

11.4 and 11.55 not

consistent

20527+1726 J605 AB 11.40 11.665 -0.26 0.111 11.90 11.982 -0.08 0.112 Overlapping star disks

20571+1801 J607 AB 10.80 10.714 0.09 0.130 12.40 12.440 -0.04 0.136 Touching star disks


21056+1749 J797 AB 12.30 12.053 0.25 0.101 13.80 13.259 0.54 0.106

20198+1203 J837 AB 11.10 10.848 0.25 0.100 11.70 11.905 -0.21 0.102 Overlapping/Touching

star disks

20210+1028 J838 AB 11.52 12.543 -1.02 0.093 12.00 12.579 -0.58 0.093

20235+1811 J839 AB 11.50 11.138 0.36 0.121 11.70 11.156 0.54 0.121 Overlapping/Touching

star disks

20249+1124 J840 AB 9.50 11.314 -1.81 0.081 10.50 12.835 -2.34 0.085








ing rather well the

current WDS values

20249+1309 J841 AB.C 10.10 10.045 0.05 0.100 10.50 10.664 -0.16 0.100

20250+1451 J842 AB 10.04 9.926 0.11 0.090 12.10 11.713 0.39 0.092

20314+2054 J844 AB 12.20 11.863 0.34 0.141 12.80 12.825 -0.02 0.146

20434+1712 J845 AB 11.99 12.658 -0.67 0.094 12.20 13.137 -0.94 0.100

20541+1402 J846 AB 10.80 10.622 0.18 0.071 11.14 11.060 0.08 0.071


20385+1118 J1073 AB 9.70 11.492 -1.79 0.081 14.00 14.170 -0.17 0.108 Low SNR <20 for B

20209+1332 J1173 AB 10.41 10.551 -0.14 0.071 13.70 12.164 1.54 0.079 Touching star disks

20157+0957 J1234 AB 12.51 11.892 0.62 0.095 15.00 13.392 1.61 0.137 Very low SNR <10 for B








ing rather the current

WDS values

20386+1120 J1242 AB 9.60 11.546 -1.95 0.113 11.00 12.538 -1.54 0.121

20298+1154 J1243 AB 10.80 12.608 -1.81 0.102 10.80 12.628 -1.83 0.102 iT27. Bessel epoch

2015.799

20146+1116 J1296 AB 11.90 12.619 -0.72 0.102 12.40 13.408 -1.01 0.106 iT27. Bessel epoch

2015.799

Table 2 (continued). Bessel epoch 2015.683 (exceptions see notes column) photometry results for the J objects in Del. ...












ing rather well the

current WDS values








ing rather well the

current WDS values

20247+0302 J1342 AB 9.40 12.090 -2.69 0.076 11.50 12.801 -1.30 0.072 Overlapping/Touching

star disks

20270+1008 J1343 AB 9.60 11.889 -2.29 0.121 10.00 12.039 -2.04 0.121 Overlapping/Touching

star disks. Bessel

epoch 2015.713

20348+1121 J1344 AB 9.10 10.646 -1.55 0.070 11.50 10.878 0.62 0.071 Overlapping/Touching

star disks. Bessel

epoch 2015.713

20438+1440 J1345 AB 9.60 11.712 -2.11 0.143 10.50 12.682 -2.18 0.151 Low SNR <20 for B

20560+0837 J1346 AB 13.20 12.477 0.72 0.102 13.20 12.524 0.68 0.102 iT27. Touching star

disks. Bessel epoch

2015.801

20260+1212 J1704 AB 10.16 10.320 -0.16 0.190 10.80 11.324 -0.52 0.191 Bessel epoch 2015.809

20586+0723 J1715 AB 11.61 12.232 -0.62 0.084 13.00 13.748 -0.75 0.124 Low SNR <20 for B

20593+1744 J1716 AB 10.00 11.781 -1.78 0.112 11.00 13.071 -2.07 0.122

20169+1303 J1879 AB 11.83 11.972 -0.14 0.095 11.95 12.811 -0.86 0.110 Low SNR <20 for B.

Bessel epoch 2015.809

20169+1303 J1879 AC 11.83 11.972 -0.14 0.095 14.40 13.959 0.44 0.165 Very low SNR <10 for

B. Bessel epoch

2015.809

20172+1304 J1880 AB 11.23 11.113 0.12 0.101 13.30 12.910 0.39 0.110

20303+0917 J1883 AB 11.53 11.665 -0.14 0.102 12.00 12.250 -0.25 0.103

20315+1448 J1884 AB 9.80 11.782 -1.98 0.152 9.80 12.355 -2.56 0.154

20315+1446 J1885 AB 12.00 13.283 -1.28 0.128 12.00 13.693 -1.69 0.136 Low SNR <20 for B

20351+1413 J1887 AB 11.68 11.934 -0.25 0.135 11.70 12.319 -0.62 0.139

20439+1255 J1888 AB 9.70 12.023 -2.32 0.092 12.50 13.897 -1.40 0.107 Low SNR <10 for B.


20441+1258 J1889 AB 14.30 14.386 -0.09 0.106 14.30 15.405 -1.11 0.198 Low SNR <20 for A and

very low SNR <10 for

B. Bessel epoch

2015.809

20485+1448 J1890 AB 11.20 11.670 -0.47 0.182 11.50 12.056 -0.56 0.183

20360+0411 J2192 AB 9.90 11.440 -1.54 0.051 12.50 12.882 -0.38 0.054 Bessel epoch 2015.713

20305+1829 J2313 AB 9.50 11.542 -2.04 0.122 11.90 13.209 -1.31 0.132 Low SNR <20 for B

20327+0453 J2314 AB 10.60 12.475 -1.88 0.113 11.60 12.800 -1.20 0.119 Low SNR <20 for B

20327+0453 J2314 AC 10.60 12.475 -1.88 0.052 14.00 No resolution, C

fainter than 14mag

20415+1611 J2319 AB 9.80 12.035 -2.24 0.102 12.00 13.711 -1.71 0.122

20488+0512 J2321 AB 9.61 9.700 -0.09 0.091 10.80 12.402 -1.60 0.097






20518+1736 J2325 AB 11.60 11.777 -0.18 0.142 13.70 13.254 0.45 0.151 Low SNR <20 for B.

Similar pair UCAC4-538

-140054/UCAC4-538-

140056 nearby

20230+0929 J2572 AB 9.80 12.206 -2.41 0.172 13.20 14.208 -1.01 0.213 Very low SNR<10 for B.

Image quality ques-

tionable

20321+0330 J2573 AB 12.50 12.945 -0.45 0.102 12.80 13.323 -0.52 0.117 Low SNR<20 for B

20418+1404 J2575 AB 9.70 13.00 Overlapping star disks




SNR 58.88 - questiona-

ble object, Bogus as-

sumed. If double at

all than A could be

not brighter than

11.8mag


- no trace of a sec-

ondary, no separate

photometry possible.

Combined magnitude

11.376 with SNR 52.42

- questionable object,

potential bogus


- no trace of a sec-

ondary, no separate


Combined magnitude

12.338 with SNR 21.91

- questionable object,

potential bogus

21058+1939 J2702 AB 11.20 11.038 0.16 0.081 11.60 11.268 0.33 0.082

20152+1357 J3066 AB 11.00 12.789 -1.79 0.106 11.50 13.641 -2.14 0.113

20152+1357 J3066 AC 11.00 12.789 -1.79 0.106 15.00 15.834 -0.83 0.345 Very low SNR<5 for C

20227+1345 J3079 AB 12.90 12.645 0.26 0.063 13.30 13.366 -0.07 0.067 Bessel epoch 2015.702

20227+2023 J3080 AB 12.00 12.058 -0.06 0.221 13.00 12.732 0.27 0.221 Large dVmag 0.22.


20228+2023 J3081 AB 10.00 12.111 -2.11 0.171 11.00 12.741 -1.74 0.172 Large dVmag 0.17.


20229+1346 J3082 AB 14.20 15.80 Most probably position

error. Only very faint

single star with

14.634mag and SNR

14.01 in the given po-

sition. But nearby

UCAC4-519-126369

20:23:07.099

+13:47:41.640

+14.264Vmag with com-

panion UCAC4-519-

126370 15.616mag model

fit, no Vmag. Bessel

epoch 2015.702

20259+0902 J3084 AB 12.03 13.208 -1.18 0.114 12.90 14.052 -1.15 0.127 Low SNR<20 for B. Bes-

sel epoch 2015.702

20263+1445 J3085 AB 9.80 11.608 -1.81 0.081 9.80 12.258 -2.46 0.082 Bessel epoch 2015.702






20275+1514 J3087 AB 10.50 11.928 -1.43 0.241 11.60 13.040 -1.44 0.245 Large dVmag 0.24.


20293+1029 J3088 AB 10.50 12.865 -2.37 0.181 11.30 13.033 -1.73 0.184 Low SNR<20 for A and

B. Bessel epoch

2015.702


very low SNR<5 for B.


20314+2049 J3091 AB 11.20 13.367 -2.17 0.226 11.50 13.407 -1.91 0.225 Bessel epoch 2015.702

20326+1024 J3092 AB 12.10 12.60 No resolution, no pho-

tometry possible. Both

components probably

much fainter than WDS

value. UCAC4-502-

130763 13.156fmag,

UCAC4-502-130762

13.652fmag. Given Vmag

12.705 for A seems

questionable, espe-

cially as the same

value is given for B

and similar bright

stars nearby are

listed with 13.764

Vmag. Bessel epoch

2015.702

20334+1359 J3093 AB 12.80 12.80 No resolution, no pho-

tometry possible. Both

components probably

much fainter than WDS

value. UCAC4-520-

130741 13.538fmag,

4UCAC4-520-130739

13.176fmag. Vmag

12.79mag for A seems

questionable, espe-

cially as similar

bright stars nearby

are listed with

14.240Vmag. Bessel

epoch 2015.702

20339+1915 J3094 AB 11.10 10.456 0.64 0.272 14.80 Companion too faint

for resolution, thus

rather confirming WDS

value. Image quality

questionable. Bessel

epoch 2015.702


B, image quality ques-

tionable. Bessel epoch

2015.702

20365+2044 J3096 AB 10.50 10.676 -0.18 0.171 12.60 12.825 -0.23 0.192 Low SNR<20 for B. Bes-

sel epoch 2015.702

20365+2044 J3096 BC 12.60 12.825 -0.23 0.192 13.10 Low SNR<20 for B, no

resolution for C, thus

probably much fainter

than 13.1mag. Ques-

tionable image quali-

ty. Bessel epoch

2015.702


B. Bessel epoch

2015.702






20378+1936 J3099 AB 12.50 13.012 -0.51 0.116 12.70 13.558 -0.86 0.121 Bessel epoch 2015.702

20385+1848 J3102 AB 11.60 11.678 -0.08 0.171 12.10 12.845 -0.75 0.173 Bessel epoch 2015.702

20393+2003 J3103 AB 12.05 10.494 1.56 0.170 12.42 12.618 -0.20 0.174 Bessel epoch 2015.702

20397+1406 J3104 AB 9.90 11.717 -1.82 0.111 11.20 13.103 -1.90 0.115 Bessel epoch 2015.702

20416+1738 J3107 AB 11.70 13.205 -1.51 0.132 11.70 13.295 -1.60 0.130 Bessel epoch 2015.702

20436+1537 J3108 AB 11.00 11.214 -0.21 0.101 12.50 12.133 0.37 0.102 Bessel epoch 2015.702

20433+1728 J3109 AB 12.50 12.577 -0.08 0.134 13.10 12.659 0.44 0.135 Bessel epoch 2015.702

20466+1532 J3110 AB 11.20 11.105 0.09 0.111 11.50 11.751 -0.25 0.112 Bessel epoch 2015.702

20509+1517 J3113 AB 11.50 12.829 -1.33 0.107 11.50 12.880 -1.38 0.106 Bessel epoch 2015.702

20513+1647 J3115 AB 12.16 11.714 0.45 0.104 15.20 13.673 1.53 0.128 Low SNR<20 for B. Bes-

sel epoch 2015.702

20522+1656 J3116 AB 8.77 8.687 0.08 0.080 12.88 13.155 -0.27 0.115 A too bright for reli-

able photometry, low

SNR<20 for B. Bessel

epoch 2015.702

20522+1656 J3116 BC 13.30 13.155 0.15 0.115 14.80 C too faint to be re-

solved, inconsistent

WDS data for B (12.88

vs 13.3mag). Bessel

epoch 2015.702

20585+1607 J3118 AB 9.40 9.607 -0.21 0.110 11.20 11.978 -0.78 0.113 Bessel epoch 2015.702

21081+1857 J3125 AB 12.40 12.490 -0.09 0.119 13.60 13.588 0.01 0.137 Low SNR<20 for B. Bes-

sel epoch 2015.702

20285+0443 J3220 AB 10.75 10.811 -0.06 0.102 12.50 11.972 0.53 0.111 Bessel epoch 2015.702


B. Bessel epoch

2015.702

20487+0706 J3223 AB 10.69 10.538 0.162 0.112 11.40 No resolution, not

even an elongation.

Probably WDS catalog

mismatch. Bessel epoch

2015.828


B. Same image as for

J562. Bessel epoch

2015.702


B. Bessel epoch

2015.828


very low SNR<10 B.



B. Bessel epoch

2015.828


B. Bessel epoch

2015.828

20555+1730 J3328 AB 11.99 11.740 0.25 0.133 14.70 13.037 1.66 0.181 Low SNR<20 for A and

very low SNR<10 B.


Table 2 (conclusion). Bessel epoch 2015.683 (exceptions see notes column) photometry results for the J objects in Del. ...

Table 2 notes on next page.



Notes regarding the notes column:

“iT27” indicates the use of telescope iT27 instead of iT24.

“Bessel epoch” indicates an epoch given different from 2015.683.

“Touching star disks” indicates that the rims of the star disks are touching and that the measurement results might be a bit less precise than with clearly separated star disks.

“Overlapping/Touching star disks” indicates that the star disks overlap to the degree of an elongation and that the measurement results is probably less precise than with clearly separated star disks.

“Overlapping star disks” indicates star disk overlap to the degree that photometry for the separated compo-nents was no longer possible and that it was neces-sary to resort to the measurement of the combined magnitude.

“Low SNR <20” indicates that the measurement result might be a bit less precise than desired due to a low SNR value but this is already included in the calcula-tion of the error range estimation.

“Very low SNR <10” indicates that the measurement result is probably a bit less precise than desired due to a very low SNR value but this is already included in the calculation of the error range estimation.

“Image quality questionable” indicates a rather large average magnitude error for the reference stars used for plate solving either due to not this perfect weather conditions during imaging or may be erroneous Vmag values for the stars used for plate solving. But this is already included in the calculation of the error range estimation.

“too bright for reliable photometry” indicates a star far brighter than the for plate solving used range 10.5 to 14.5mag – despite this most such cases showed a reasonable measurement result anyway

In case of J3223 separation is calculated based on the RA/Dec coordinates of the components. This is done using the formulae provided by Buchheim, 2008.

Specifications of the used telescopes:

iT24: 610.mm CDK with 3962 mm focal length. Resolution 0.625 arcsec/pixel. V-filter. No transfor-mation coefficients available. Located in Auberry, Cali-fornia. Elevation 1405 m.

iT27: 700.mm CDK with 4531.mm focal length. CCD: FLI PL09000. Resolution 0.53 arcsec/pixel. V-filter. No B-V transformation coefficients available. Located in Siding Spring, Australia. Elevation 1122 m.


Introduction and Instrumentation

I have been imaging double stars for a number of years using the equipment at iTelescopes.

This series of measurements of visual doubles used the T21 telescope at the iTelescopes Observatory. The instrument is a Planewave 24inch (0.61m) Dall-Kirkham Astrograph with a focal length of approxi-mately 3962 mm. The CCD camera is a FLI-PL0900 with 12um square pixels. The field of view is 31.8 X 31.8 arc-mins. The resolution is 0.62 arc-sec/pixel.The OTA is mounted on a Planewave Ascension 200HR.

The instrument is capable of quickly and accurately slewing to a selected double star. The system takes about one minute to take short exposure and save the resulting image in a FITS format. Taking 5 to 6 expo-sures per double star allows 6 doubles to be imaged per hour. To maximize telescope time, the FITS images are stored on the iTelescopes server and are retrieved later to be analyzed by suitable software (in my case MPO Canopus).

Methods

Imaging was done by entering the coordinates of the double into the robotic telescope’s web interface. A test exposure was done and checked for centering and proper exposure. If all was well an exposure run of 5 to 7 images through a clear filter was done for each pair. Exposures typically ran about 10-15 seconds for 10-13 magnitude doubles. After the observing session was

completed, the images were retrieved from an ftp site provided by the iTelescope observatory. Some doubles appeared on more than one image and were measured more than 5 times.

Each image in the exposure sequence was exam-ined and any trailed or sub-par images were discarded. MPO Canopus was used to reduce the images (Warner, 2006). Any image that the software could not reach a plate solution was also discarded. Canopus produces an astronomic solution to the image based on the UCAC3 catalog (Zacharias et all.2010) . The software measures double stars using a subroutine built into Canopus. It also produces a great amount of information about the astrometric solution. All images were copied to archival CD-ROM material and are available by request from the author. Each starting and ending image was blinked—just in case.

Results

Table 1 shows the results for the 288 doubles meas-ured.

Discussion

POU1903. I report a new “C” component. See Notes following Table 1.

POU1912. I report a new “C” component. See Notes following Table 1.

I report that components of POU894, POU1470, POU1889, and POU 1920 have close doubles as one of their components. In each case, I measured to the

Double Star Measurements for December 2013

Frank Smith

20 Coburn Way Jaffrey, NH 03452

[email protected]

Abstract: I report 288 measurements of binary systems from 2013.911. The observations were con-ducted with the T24 robotic telescope located at the iTelescope Observatory, Auberry CA, USA (http://www.itelescope.net/). Discussion includes notes on a number of the observed doubles. Several new components of existing binaries were discovered. One new multiple star system is described. Infor-mation about instrumentation and methodology and results is included.



brighter of the two new components, which will be a little different than previous measures.

New System

I am aware that WDS does not need any more dou-bles, but I could not resist measuring a striking quadru-ple star located near SLE 766. As usual, Dr. Mason and Dr. Hartkopf have the final say in determining if the measure warrants inclusion in the WDS catalog. See image of this system in Figure 1.

“A” star is UCAC4 503-030116. Position 06:42:25.0975+10:26:56.715. APASS V mag 10.382. proper motion PA 8.4 DEC -17.2.

“B” Star is UCAC4 503-030113. 2MASS J mag 11.215. proper motion PA -1.8 DEC -42.4.

“C” star is UCAC4 503-030109. 2MASS J mag 11.332. “C” is also URAT1 503-6011053 proper mo-tion PA 0.9 DEC -2.4 .

“D” star is UCAC4 503-030108. 2MASS J mag 11.633. proper motion: PA 6.4 DEC -46.7. The “B” and “D” components have similar proper motions and could be a CPM pair.

Acknowledgements

“Thank you” to Dr. Mason and Dr. Hartkopf for being willing to work with amateurs and for answering data requests. “Thank you” also to my sister Gail Smith who proofread this article.

This article made use of the Washington Double Star Catalog maintained by the U.S. Naval Observato-ry.

This research made use of the VizierR Catalog Ac-cess Tool, CDS, Strasbourg, France. The original de-scription of the Vizier service was published in A&AS 143,2.

References

iTelecopes. http://www.itelescope.net/

Mason, B.D., 2006 “Requesting double star data from the US Naval Observatory”. JDSO. 2, 21-35.

UCAC3 Catalog (Zacharias, et al. 2010).

UCAC4 Catalog (Zacharias, et al. 2012).

Warner, Brian 2006. MPO Canopus, http://www.minorplanetobserver.com/MPOSoftware/MPOCanopus.htm.

Table 1 starts on next page. Figure 1. CCD image showing SLE766 and new doubles

http://www.itelescope.net/



WDS ID Discoverer RA DEC PA SEP Epoch No. PAsd SEPsd Notes

06036+2427 POU862 AB 0604.5 2427 168.6 9.62 2013.911 5 0.10 0.054

06036+2427 POU 863 AC 0604.5 2427 106.3 9.08 2013.911 5 0.28 0.107

06043+2439 POU 882 0604.5 2445 34.2 12.81 2013.911 7 1.00 0.707

06038+2416 POU 867 0604.7 2416 48.6 8.25 2013.911 5 0.74 0.088

06039+2418 POU 868 0604.8 2418 252.6 14.68 2013.911 5 0.32 0.085

06040+2425 POU 871 0604.9 2425 121.2 9.87 2013.911 5 0.31 0.065

06042+2424 POU 881 0605.1 2424 116.7 11.09 2013.911 5 0.29 0.073

06043+2422 POU 883 0605.2 2422 193.7 9.40 2013.911 5 0.34 0.021

06046+2438 POU 894 0605.5 2437 1.4 12.70 2013.911 5 0.07 0.036 1

06046+3644 ALI 315 0605.5 3643 262.2 11.12 2013.911 5 0.07 0.085

06048+2411 POU 898 0605.7 2411 358.7 11.69 2013.911 5 0.40 0.039

06048+2408 POU 900 0605.7 2408 222.0 8.54 2013.911 5 0.83 0.144

06048+2413 POU 897 0605.7 2412 327.6 13.56 2013.911 5 0.41 0.095

06048+2410 POU 899 0605.7 2409 302.6 8.68 2013.911 5 0.27 0.164

06050+2446 POU 903 0605.8 2446 110.0 13.88 2013.911 5 0.34 0.041

06052+2443 POU 908 0606.0 2411 72.5 8.18 2013.911 5 0.73 0.075

06052+2443 POU 910 0606.1 2442 27.5 14.62 2013.911 5 0.69 0.083 2

06053+2416 POU 914 0606.2 2416 228.8 14.88 2013.911 5 0.04 0.028

06055+1336 SLE 832 0606.2 1336 64.5 10.96 2013.911 5 0.89 0.099

06055+2439 POU 916 0606.4 2439 283.3 12.30 2013.911 5 0.11 0.020

06058+1326 SLE 833 AB 0606.6 1326 343.5 38.56 2013.911 5 0.28 0.066

06058+1326 SLE 833 AC 0606.6 1326 345.2 32.28 2013.911 5 0.20 0.248

06059+3632 ALI 316 0606.8 3632 243.9 13.71 2013.911 5 0.37 0.040

06277+2249 BTG 10 0628.7 2251 310.4 35.32 2013.911 2 0.12 0.105

06277+2249 BTG 10 AC 0628.7 2251 310.8 35.36 2013.911 3 0.18 0.137

06277+2249 J 1092 AB 0628.7 2251 226.5 6.28 2013.911 5 0.43 0.277

06280+2332 POU 1338 0628.8 2331 149.9 18.74 2013.911 5 0.21 0.074

06281+2320 POU 1340 0628.9 2320 11.2 16.07 2013.911 5 0.26 0.065

06283+2325 POU 1343 0629.1 2325 166.8 7.50 2013.911 5 0.29 0.175

06285+2307 POU 1345 0629.3 2307 180.8 16.63 2013.911 5 0.22 0.090

06288+2313 POU 1347 0629.6 2311 80.5 14.59 2013.911 5 0.07 0.075

06289+2322 POU 1350 0629.7 2321 157.2 15.78 2013.911 5 0.17 0.075

06291+2322 POU 1355-2 0629.9 2326 141.7 8.83 2013.911 5 0.50 0.076 3

06294+2311 POU 1360 0630.2 2311 41.5 15.41 2013.911 5 0.23 0.083

06293+2308 POU 1358 0630.2 2308 162.6 8.34 2013.911 5 0.38 0.078

06342+2257 POU 1463 0635.0 2257 223.1 21.85 2013.911 6 0.09 0.089

06342+2305 POU 1465 0635.0 2305 53.9 18.24 2013.911 6 0.10 0.092

06343+2311 POU 1470 0635.2 2310 268.9 14.76 2013.911 6 0.11 0.083 4

06344+2408 POU 1478 0635.2 2308 56.8 15.10 2013.911 6 0.34 0.087

06344+2314 POU 1476 0635.2 2314 80.1 15.48 2013.911 6 0.25 0.069

06345+2322 POU 1481 0635.3 2321 302.5 7.58 2013.911 6 0.38 0.325

06346+2318 POU 1489 0635.4 2318 169.1 12.35 2013.911 6 0.25 0.074

06347+2310 POU 1492 0635.5 2310 315.9 15.07 2013.911 6 0.14 0.037

06350+2302 POU 1508 AB 0635.8 2302 62.6 10.72 2013.911 6 0.43 0.088

Table 1. Reported Measurements from December 2013





06350+2302 POU 1509 AC 0635.8 2302 221.8 14.65 2013.911 6 0.26 0.069

06351+2258 POU 1523 0635.9 2257 283.8 16.64 2013.911 6 0.21 0.051

06353+2252 POU 1528 0636.1 2252 294.6 8.80 2013.911 6 0.03 0.036

06353+2258 POU 1530 0636.1 2257 42.3 14.76 2013.911 5 0.28 0.072

06356+2253 POU 1542 0636.4 2252 191.7 10.97 2013.911 5 0.38 0.019

06356+2319 POU 1546 0636.5 2319 243.1 9.47 2013.911 6 0.74 0.088

06357+2305 POU 1548 0636.5 2305 14.8 12.23 2013.911 6 0.41 0.074

06357+2258 POU 1556 AB 0636.6 2257 131.0 11.54 2013.911 5 0.17 0.034

06357+2258 POU 1557 AC 0636.6 2257 155.6 22.04 2013.911 5 0.19 0.065

06258+2259 POU 1563 0636.6 2259 233.1 11.35 2013.911 6 0.42 0.059

06358+2255 POU1564 0636.6 2254 298.5 14.13 2013.911 6 0.29 0.158 5

06359+2257 POU 1568 0636.7 2256 94.7 13.38 2013.911 6 0.11 0.058

06359+2306 POU 1573 0636.7 2305 300.2 8.76 2013.911 6 0.64 0.084

06361+2257 POU 1579 0636.9 2256 47.1 11.64 2013.911 6 0.47 0.091

06363+2300 POU 1592 0637.1 2300 146.0 16.94 2013.911 6 0.35 0.117

06364+2257 POU 1598 0637.2 2256 35.8 11.37 2013.911 6 0.35 0.057

06370+2320 POU 1640 0637.8 2319 144.0 15.65 2013.911 6 0.12 0.064

06371+2342 POU 1644 0637.9 2341 141.1 13.48 2013.911 7 0.08 0.052

06370+2329 POU 1645 0637.9 2328 331.8 9.36 2013.911 6 0.30 0.036

06371+2329 POU 1652 0638.0 2328 121.6 10.73 2013.911 6 0.26 0.056

06371+2328 POU 1648 0638.0 2327 58.1 6.00 2013.911 6 0.90 0.216

06372+2424 POU 1653 0638.1 2424 0.3 12.62 2013.911 5 0.12 0.043 6

06372+2426 POU 1654 0638.1 2425 129.8 13.09 2013.911 5 0.08 0.054

06373+2429 POU 1655 0638.2 2428 136.9 12.49 2013.911 5 0.13 0.022

06373+2430 POU 1657 0638.2 2430 263.4 12.19 2013.911 5 0.28 0.063

06373+2326 POU 1660 0638.2 2325 230.6 15.19 2013.911 6 0.12 0.034

06374+2325 POU 1666 0638.2 2324 27.0 7.07 2013.911 6 0.21 0.129

06375+2321 POU 1671 0638.3 2321 234.7 17.27 2013.911 6 0.11 0.016

06374+2443 POU 1662 0638.3 2442 234.5 13.89 2013.911 5 0.19 0.031

06375+2347 POU 1672 0638.4 2346 197.2 10.47 2013.911 6 0.31 0.055

06376+2337 POU 1679 0638.4 2336 216.0 14.06 2013.911 6 0.16 0.021

06375+2411 POU 1676 0638.4 2410 249.7 9.42 2013.911 11 0.21 0.032

06376+2429 POU 1681 AB 0638.5 2428 211.8 7.93 2013.911 5 0.23 0.123

06376+2429 POU 1682 AC 0638.5 2428 29.5 12.05 2013.911 5 0.21 0.021

06377+2353 POU 1688 AB 0638.6 2352 32.9 18.80 2013.911 6 0.12 0.018

06377+2353 POU 1689 AC 0638.6 2352 208.4 9.70 2013.911 6 0.21 0.075

06377+2353 POU 1690 AD 0638.6 2352 132.8 11.72 2013.911 6 0.07 0.062

06377+2439 POU 1691 0638.6 2438 133.1 11.34 2013.911 5 0.38 0.076

06377+2441 POU 1686 0638.6 2440 127.2 18.21 2013.911 5 0.17 0.039

06377+2421 POU 1692 0638.6 2420 77.6 9.85 2013.911 5 0.34 0.039

06379+2336 POU 1700 AB 0638.7 2335 33.5 22.56 2013.911 5 0.73 0.119

06378+2322 POU 1697 0638.7 2321 225.9 13.53 2013.911 6 0.16 0.049

06379+2413 POU 1701 0638.8 2412 252.6 12.63 2013.911 6 0.33 0.048

06381+2344 POU 1708 0638.9 2343 257.6 11.02 2013.911 6 0.24 0.030

06380+2425 POU 1707 0638.9 2425 327.7 17.64 2013.911 5 0.10 0.021

06382+2334 POU 1717 0639.0 2333 226.5 10.87 2013.911 6 0.35 0.032

06383+2323 POU1715 0639.0 2322 35.4 13.61 2013.911 6 0.24 0.036

06383+2410 POU 1716 0639.1 2409 247.6 8.51 2013.911 11 0.08 0.086

06382+2425 POU 1718 0639.2 2422 57.8 11.56 2013.911 5 0.19 0.057

06385+2329 POU1725 0639.3 2328 266.4 8.98 2013.911 6 0.17 0.049

06385+2337 POU 1724 0639.3 2336 1.6 11.54 2013.911 6 0.09 0.028

06386+2321 POU1726 0639.4 2320 3.5 9.46 2013.911 6 0.62 0.079

06386+2427 POU 1729 0639.4 2426 179.7 11.34 2013.911 5 0.11 0.043

06387+2344 POU 1734 0639.5 2343 296.5 13.18 2013.911 11 0.18 0.061

Table 1 (continued). Reported Measurements from December 2013





063872317 POU 1735 0639.5 2316 66.3 15.66 2013.911 6 0.16 0.031

06386+2426 POU 1730 0639.5 2425 32.1 13.13 2013.911 5 0.17 0.023

06387+2356 POU 1731 0639.5 2355 27.2 13.35 2013.911 6 0.13 0.048

06388+2304 POU 1740 0639.6 2303 185.1 7.52 2013.911 5 0.44 0.082

06388+2301 POU 1737 0639.6 2300 223.7 6.52 2013.911 5 0.23 0.090

06388+2350 POU 1739 0639.6 2349 216.2 9.03 2013.911 6 0.20 0.036

06389+2359 POU 1741-1 0639.7 2358 97.6 12.62 2013.911 6 0.37 0.047 7

06389+2359 POU 1741-2 0639.8 2358 108.8 11.93 2013.911 6 0.92 0.095 7

06389+2341 POU 1744 0639.7 2340 112.8 12.17 2013.911 11 0.51 0.031

06390+2446 POU 1746 0639.8 2445 33.9 9.17 2013.911 5 0.17 0.099

06389+2444 POU 1742 0639.8 2443 100.6 17.22 2013.911 5 0.15 0.025

06389+2448 POU 1743 0639.8 2447 109.8 17.28 2013.911 5 0.19 0.028

06390+2410 POU 1749 0639.8 2409 197.9 10.77 2013.911 11 0.30 0.098

06391+2405 POU 1757 AB 0639.9 2403 129.0 11.49 2013.911 11 0.19 0.039

06391+2405 POU 1758 AC 0639.9 2403 53.8 16.94 2013.911 11 0.17 0.043

06390+2453 POU 1750 0639.9 2452 298.7 12.20 2013.911 5 0.31 0.063

06392+2314 POU 1761 0640.0 2313 156.1 15.50 2013.911 6 0.13 0.023

06393+0357 BAL 2679 0640.0 0355 186.0 11.00 2013.911 5 0.03 0.051

06392+2307 POU 1765 0640.0 2306 293.3 7.95 2013.911 5 0.28 0.159

06393+2307 POU 1768 AB 0640.1 2306 331.0 9.39 2013.911 5 0.28 0.022

06393+2307 POU 1769 AC 0640.1 2306 62.9 15.98 2013.911 5 0.16 0.022

06392+2452 POU 1762 0640.1 2451 145.3 10.67 2013.911 5 0.31 0.054

06393+2340 POU 1767 0640.1 2338 277.2 14.60 2013.911 5 0.20 0.054

06394+2421 POU 1773 0640.2 2419 297.5 16.47 2013.911 6 0.29 0.068

06393+2409 POU 1771 0640.2 2408 261.1 14.92 2013.911 16 0.31 0.057

06394+2335 POU 1772 0640.2 2333 242.1 13.95 2013.911 5 0.21 0.042

06394+2318 POU 1774 0640.2 2317 218.4 11.08 2013.911 6 0.19 0.038

06396+0417 BAL 2681 0640.3 0416 295.4 11.07 2013.911 5 0.19 0.026

06403+2320 POU1825 0640.3 2326 31.7 16.21 2013.911 5 0.08 0.025

06395+2436 TOK 19 0640.4 2435 248.5 31.38 2013.911 3 0.27 0.110

06396+2333 POU 1779 AB 0640.4 2332 340.6 5.86 2013.911 5 0.18 0.359

06396+2333 POU 1780 AC 0640.4 2332 352.8 13.63 2013.911 5 0.26 0.118

06397+0410 BAL 2683 0640.4 0409 302.5 9.01 2013.911 5 0.13 0.053

06396+2338 POU 1781 0640.4 2337 256.7 11.88 2013.911 5 0.16 0.023

06395+2355 POU 1777 0640.4 2354 134.9 7.35 2013.911 5 0.64 0.133

06396+2340 POU 1782 0640.4 2339 13.5 13.88 2013.911 5 0.19 0.049

06397+0334 HJ 2329 0640.5 0333 87.2 17.37 2013.911 5 0.02 0.031

06397+2305 POU 1786 0640.5 2304 355.2 8.09 2013.911 5 0.61 0.104

06397+2321 POU 1788 0640.5 2321 259.6 10.90 2013.911 5 0.26 0.061

06396+2356 POU 1785 0640.5 2355 83.4 14.88 2013.911 5 0.51 0.065

06397+2323 POU 1789 0640.6 2322 56.4 9.75 2013.911 5 0.10 0.064

06397+2442 POU 1787 0640.6 2441 234.0 10.59 2013.911 10 0.23 0.054

06398+2259 POU 1791 0640.6 2257 141.2 8.07 2013.911 5 0.15 0.048

06398+0839 SLE 557 0640.6 0839 168.6 11.01 2013.911 5 0.21 0.062

06398+2439 POU 1790 0640.7 2438 72.1 12.64 2013.911 10 0.24 0.033

06398+2432 POU 1792 0640.7 2431 4.3 13.83 2013.911 5 0.20 0.028

06398+2434 POU 1794 0640.7 2432 15.0 10.94 2013.911 5 0.35 0.076

06399+2313 POU 1795 0640.7 2312 135.1 8.16 2013.911 5 0.32 0.019

06400+2317 POU 1799 0640.8 2316 304.3 11.36 2013.911 5 0.24 0.116

06400+2313 POU 1800 0640.8 2311 220.8 10.81 2013.911 5 0.43 0.038

06399+2431 POU 1796 0640.8 2429 301.1 15.08 2013.911 5 0.38 0.046

06403+2320 POU 1825 0640.8 2325 31.7 16.21 2013.911 5 0.08 0.025

06401+2410 POU 1806 AB 0640.9 2408 166.1 8.87 2013.911 5 0.43 0.043

06401+2410 POU 1807 AC 0640.9 2408 271.6 11.43 2013.911 5 0.25 0.124






06400+2414 POU 1802 AC 0640.9 2412 162.4 7.17 2013.911 5 0.56 0.152

06400+2343 POU 1803 0640.9 2342 244.3 11.95 2013.911 5 0.20 0.036

06401+2342 POU 1805 0640.9 2341 40.3 10.48 2013.911 10 0.32 0.077

06400+2404 POU 1804 0640.9 2403 344.0 7.49 2013.911 10 1.26 0.083

06401+2309 POU 1808 0640.9 2308 15.4 8.19 2013.911 5 0.31 0.053

06403+0332 HJ 2331 AB 0641.0 0332 293.5 26.92 2013.911 5 0.15 0.087

06403+0332 HJ 2331 AC 0641.0 0332 50.8 25.46 2013.911 5 0.15 0.031

06402+2332 POU 1813 0641.0 2331 322.0 13.91 2013.911 9 0.29 0.091

06402+2331 POU 1810 0641.0 2330 334.6 9.22 2013.911 10 0.19 0.046

06402+2304 POU 1811 0641.0 2303 110.7 9.15 2013.911 5 0.29 0.051

06402+2423 POU 1814 AB 0641.1 2422 17.6 7.09 2013.911 4 0.47 0.413

06402+2423 POU 1815 AC 0641.1 2422 55.9 13.27 2013.911 5 0.33 0.143

06403+2431 POU 1822 AC 0641.1 2430 55.8 13.22 2013.911 5 0.30 0.059

06404+0344 BAL 2184 0641.1 0343 204.8 16.65 2013.911 5 0.06 0.036

06402+2404 POU 1816 0641.1 2403 220.4 10.96 2013.911 10 0.30 0.040

06402+2431 POU 1812 0641.1 2430 151.7 10.60 2013.911 5 0.24 0.032

06402+2422 POU 1817 0641.1 2421 168.0 7.93 2013.911 7 0.29 0.094

06404+2301 POU 1831 AB 0641.2 2300 152.1 11.26 2013.911 5 0.23 0.028

06404+2301 POU 1832 AC 0641.2 2300 263.2 8.10 2013.911 5 0.49 0.092

06404+2331 POU 1826 AB 0641.2 2330 77.6 17.78 2013.911 11 0.30 0.058

06404+2331 POU 1827 AC 0641.2 2330 197.8 15.62 2013.911 11 0.44 0.072

06403+2428 POU 1820 0641.2 2427 1.5 10.40 2013.911 5 0.52 0.094

06405+2302 POU 1830 0641.2 2301 74.0 13.08 2013.911 5 0.35 0.102

06403+2421 POU 1824 0641.2 2420 323.2 16.62 2013.911 5 0.25 0.049

06406+0402 BAL 2687 0641.3 0402 164.3 18.08 2013.911 5 0.11 0.037

06404+2307 POU 1836 0641.3 2305 280.7 11.95 2013.911 5 0.14 0.093

06405+2438 POU 1837 AB 0641.4 2437 130.1 12.49 2013.911 5 0.22 0.038

06405+2438 POU 1838 AC 0641.4 2437 171.5 21.29 2013.911 5 0.10 0.057

06405+2424 POU 1834 0641.4 2422 200.1 12.57 2013.911 5 0.19 0.037

06405+2349 POU 1835 0641.4 2348 138.7 15.84 2013.911 10 0.17 0.039

06405+2413 POU 1839 0641.4 2412 280.9 12.22 2013.911 5 0.41 0.077

06405+2354 POU 1840 0641.4 2353 289.8 5.51 2013.911 9 0.74 0.521

06406+2411 POU 1841 0641.4 2410 8.6 6.66 2013.911 5 0.65 0.213

06406+2402 POU 1842 0641.4 2400 296.5 5.27 2013.911 9 0.59 0.298

06407+2315 POU 1847 0641.5 2313 335.7 11.19 2013.911 5 0.27 0.037

06406+2319 POU 1844 0641.5 2320 256.2 18.89 2013.911 5 0.10 0.040

06408+2357 POU 1848 AB 0641.6 2355 183.7 11.46 2013.911 9 0.25 0.034

06408+2357 POU 1849 AC 0641.6 2355 112.2 17.43 2013.911 9 0.17 0.072

06408+2424 POU 1851 0641.7 2423 233.5 11.90 2013.911 6 0.19 0.055

06409+2328 POU 1853 0641.7 2326 122.3 12.95 2013.911 5 0.19 0.028

06410+2418 POU 1854 0641.8 2418 204.2 8.28 2013.911 5 0.29 0.055

06411+2355 POU 1855 0641.9 2348 206.0 15.53 2013.911 10 0.21 0.046

06411+2415 POU 1856 0641.9 2414 313.9 12.73 2013.911 10 0.58 0.111

06411+2347 POU 1857 0641.9 2346 321.5 10.69 2013.911 10 0.20 0.087

06463+2425 POU 2002 0641.9 2449 273.5 7.89 2013.911 5 0.64 0.049

06411+2425 POU 1863 AC 0642.0 2425 229.4 11.55 2013.911 5 0.22 0.093

06412+2412 POU 1864 0642.0 2411 17.3 16.54 2013.911 5 0.21 0.051

06411+2416 POU 1861 0642.0 2415 224.5 10.00 2013.911 5 0.58 0.160

06411+2427 POU 1858 0642.0 2427 279.0 10.95 2013.911 5 0.40 0.068

06411+2354 POU 1859 0642.0 2354 111.1 10.96 2013.911 9 0.45 0.104

06411+2340 POU 1860 0642.0 2339 325.4 9.99 2013.911 10 0.21 0.049

06412+2356 POU 1867 AB 0642.1 2356 211.2 11.68 2013.911 10 0.36 0.059

06412+2356 POU 1868 AC 0642.1 2356 232.4 20.53 2013.911 10 0.11 0.060

06412+2454 POU 1865 0642.1 2449 171.0 14.11 2013.911 5 0.24 0.012






06412+2418 POU 1869 0642.1 2418 126.1 7.50 2013.911 5 1.13 0.096

06413+2412 POU 1870 0642.1 2412 111.4 12.00 2013.911 5 0.43 0.112

06465+2359 POU 2004 0642.1 2423 29.8 7.26 2013.911 5 0.69 0.046

06413+2408 POU 1873 0642.2 2408 160.1 15.94 2013.911 5 0.14 0.023

06413+2439 POU 1875 0642.2 2439 292.0 8.79 2013.911 5 0.19 0.034

06417+2359 POU 1894 0642.2 2358 221.9 10.96 2013.911 9 0.25 0.064

06466+2423 POU 2005 0642.2 2447 43.4 13.85 2013.911 5 0.52 0.044

06466+2431 POU 2006 0642.2 2455 335.1 5.35 2013.911 5 0.46 0.310

06414+2336 POU 1883 AB 0642.3 2335 25.7 17.31 2013.911 5 0.33 0.062

06414+2453 POU 1877 0642.3 2452 259.4 15.72 2013.911 5 0.22 0.069

06414+2337 POU 1881 0642.3 2336 328.2 12.24 2013.911 5 0.32 0.043

06415+2434 POU 1885 0642.3 2434 137.4 10.40 2013.911 5 0.37 0.069

06414+2415 POU 1882 0642.3 2450 48.3 11.99 2013.911 5 0.31 0.038 13

06415+2314 POU 1886 0642.3 2341 109.3 9.94 2013.911 5 0.16 0.050

06415+2421 POU 1889 0642.4 2420 140.3 15.86 2013.911 5 0.61 0.150 8

06415+2315 POU 1890 0642.4 2350 22.4 14.34 2013.911 5 0.28 0.031

06417+2411 POU 1893 0642.5 2411 67.3 10.60 2013.911 5 0.31 0.112

06417+2327 POU 1895 0642.6 2327 336.5 6.52 2013.911 5 0.80 0.315

06470+2405 POU 2010 0642.6 2429 264.7 12.44 2013.911 6 0.34 0.077

06418+2412 POU 1896 0642.6 2412 221.9 10.37 2013.911 5 0.41 0.051

06419+2406 POU 1903 AB 0642.7 2406 98.9 14.89 2013.911 5 0.28 0.035 9

06419+2406 POU 1903 AC 0642.7 2406 127.0 14.18 2013.911 5 0.11 0.033 9

06419+2444 POU 1902 0642.7 2443 132.3 11.67 2013.911 5 0.40 0.070 11

06418+2436 POU 1901 0642.7 2436 128.9 15.57 2013.911 5 0.13 0.039 12

06419+2416 POU 1905 0642.8 2415 30.7 13.07 2013.911 5 0.13 0.032

06419+2437 POU 1906 0642.8 2436 332.9 16.57 2013.911 5 0.26 0.095

06419+2438 POU 1907 0642.8 2438 47.5 18.74 2013.911 5 0.05 0.024

06742+2409 POU 2012 0642.8 2433 266.5 9.78 2013.911 5 0.13 0.009

06420+2402 POU 1908 0642.8 2401 262.1 14.80 2013.911 5 0.20 0.047

06421+2400 POU 1911 0642.9 2400 272.9 15.26 2013.911 5 0.22 0.029

06421+2329 POU 1915 0642.9 2329 140.2 6.33 2013.911 5 0.65 0.121

06421+2359 POU 1910 0642.9 2359 66.6 5.70 2013.911 5 0.23 0.201

06421+2441 POU 1912 BC 0643.0 2440 141.3 8.63 2013.911 5 0.03 0.015 10

06421+2441 POU 1912 AB 0643.0 2441 202.8 15.75 2013.911 5 0.19 0.019 10

06421+2441 POU 1912 AC 0643.0 2441 182.0 21.27 2013.911 5 0.17 0.033 10

06421+2420 POU 1913 0643.0 2420 208.0 16.66 2013.911 5 0.19 0.038

06422+2431 POU 1916 0643.0 2430 94.9 12.25 2013.911 5 0.38 0.061

06474+2413 POU 2013 0643.0 2437 350.3 11.02 2013.911 5 0.30 0.038

06421+2437 POU 1914 0643.0 2437 258.5 10.97 2013.911 5 0.08 0.014

06422+2448 POU 1917 0643.1 2448 225.0 12.33 2013.911 5 0.24 0.068

06423+2412 POU 1918 0643.1 2412 357.8 10.36 2013.911 5 0.39 0.064

06423+2355 POU 1919 0643.1 2355 229.8 6.86 2013.911 5 0.38 0.200

NEW AB 0643.2 1026 235.6 6.93 2013.911 5 0.55 0.157 14

NEW AC 0643.2 1026 278.1 12.40 2013.911 5 0.08 0.027 14

NEW AD 0643.2 1026 233.4 15.30 2013.911 5 0.18 0.036 14

06424+2423 POU 1921 0643.2 2422 107.7 10.76 2013.911 5 0.09 0.070

06424+2448 POU 1920 0643.2 2448 350.7 15.02 2013.911 5 0.11 0.080 11

06422+2431 POU 2016 0643.2 2425 333.1 11.11 2013.911 5 0.50 0.044

06424+2413 POU 1923 0643.3 2413 127.9 13.41 2013.911 6 0.13 0.018

06477+2357 POU 2018 0643.3 2421 211.2 11.39 2013.911 5 0.38 0.077

06478+2408 POU 2022 0643.4 2432 73.1 10.74 2013.911 5 0.06 0.016

06426+1034 SLE 766 0643.4 1033 192.6 11.04 2013.911 5 0.24 0.053

06478+2406 POU 2024 0643.4 2430 126.0 11.34 2013.911 5 0.23 0.026

06478+2427 POU 2021 0643.4 2451 32.4 10.90 2013.911 5 0.27 0.063





Notes:

1. POU894. "A" star is a close binary, see Figure 2.

2. POU610. "B" star faint. 3UCAC 23005118 has a listed V mag of 15.903.

3. POU 1355. I'm measuring 3UCAC 227-059131 06:29:05.68 +23:26:25.3 Mag 14.9 as the "A" star and 3UCAC 227-059127 06:29:06.09+23:26:18.7 Mag 14.74 as the "B" star.

4. POU1470. "B" star is a close double. See image. I'm measuring to the brighter component 3UCAC 227-062476 Mag 12.59. The other star is 3UCAC 227-062480. See Figure 3.

5. POU1546. I'm measuring 3UCAC 226-064744 06:46.76.7+22:55:06.7 Mag 14.6 as the "A"star. "B" is 3UCAC 226-064729 06:35:45.86+22:55:13.3 Mag 15.2

is the "B" star.

6. POU1653."A" star is much fainter in my CCD image. "A" 3UCAC 229-069631 V mag 14.365, "B" 3UCAC 229-069633 V mag 13.37.

7. POU1741.There are two pairs available. One matches the 1906 measure and one matches 1998 measure. POU1741-1. Measuring 3UCAC 228-068389 V mag 15.04 and 3UCAC 228-068382 V mag 14.81. POU1741-2. Measuring: star at 06:38:57.47+23:58:36.3 mag 17.37, 06:38:58.32+23:58:32.6 mag 16.41

8. POU1889. 'B" star is a close double. See Figure 4.

9. POU1903. New "C" star. See Figure 5. "C" is UCAC-4 4UC571-033128. "A" and "B" stars have large and simi-lar proper motions. Probable CPM pair.


06425+2438 POU 1925 0643.4 2437 152.0 17.66 2013.911 5 0.18 0.051

06428+2436 POU 1933 0643.5 2436 129.9 16.47 2013.911 5 0.32 0.071

06428+2427 POU 1930 0643.6 2426 222.8 13.61 2013.911 5 0.09 0.024

06481+2401 POU 2025 0643.7 2425 191.7 8.67 2013.911 5 0.50 0.054

06430+1020 SLE 767 0643.7 1019 61.5 19.41 2013.911 5 0.25 0.067

06429+2422 POU 1934 0643.7 2421 309.1 16.96 2013.911 5 0.15 0.079

06430+2436 POU 1938 0643.8 2435 107.2 11.19 2013.911 5 0.05 0.008

063431+2425 POU 1940 0643.9 2424 60.8 16.88 2013.911 5 0.14 0.022

06483+2405 POU 2027 0643.9 2429 227.6 14.92 2013.911 5 0.33 0.039

06430+2442 POU 1939 0643.9 2441 78.0 8.44 2013.911 5 0.30 0.062

06432+2430 POU 1948 0644.1 2430 27.3 16.17 2013.911 5 0.23 0.057

06434+2419 POU 1952 0644.2 2419 281.9 14.49 2013.911 5 0.30 0.098

06487+2359 POU 2032 0644.2 2424 194.9 8.38 2013.911 5 0.71 0.127

06433+2432 POU 1950 0644.2 2432 330.4 8.07 2013.911 5 0.36 0.028

06487+2403 POU 2033 0644.3 2427 167.3 13.89 2013.911 5 0.11 0.046

06435+2439 POU 1955 0644.3 2437 129.2 13.26 2013.911 5 0.14 0.039

06434+2418 POU 1953 0644.3 2418 76.4 9.21 2013.911 5 0.50 0.027

06436+2421 POU 1956 0644.4 2419 288.4 16.28 2013.911 5 0.04 0.007

06451+0251 BAL 1715 0645.8 0250 310.1 17.85 2013.911 5 0.27 0.080

06452+0306 BAL 2191 0645.9 0306 120.4 11.03 2013.911 5 0.22 0.048

06462+0256 BAL 2193 0647.1 0310 184.3 7.68 2013.911 6 0.36 0.118

06463+0247 BAL 1721 0647.1 0246 71.2 12.31 2013.911 5 0.15 0.090

06472+2346 POU 2011 0648.0 2344 208.6 7.87 2013.911 5 0.58 0.045

06481+2337 POU 2026 0648.9 2337 356.2 9.63 2013.911 5 0.48 0.037

06483+2337 POU 2029 0649.2 2337 91.6 12.99 2013.911 5 0.03 0.096

06490+2345 POU 2035 0649.8 2344 110.4 12.41 2013.911 5 0.16 0.095

Table 1 (conclusion). Reported Measurements from December 2013

Figure 2. POU894. "A" is a close double Figure 3. POU1470. "B" star is a close double



10. POU1912. Measuring new "C" star. See Figure 6. "C" is 3UCAC 230-070508 Mag 15.73.

11. POU1920. "A" star is a close double. See Figure 7.

12. POU1901. I'm measuring 3UCAC 230-070377 and 3UCAC 230-070384. "A" star is at 06:41:52.31+24:44:02.5

13. POU1882. Position seems wrong. I'm measuring 3UCAC 230-070172 and 3UCAC 230-070181. "A" is at 06:41:29.46+24:51:14.8.

14. New quadruple star. See "Discussion".

Illustration 4: POU1889 showing "B" star as a close double. Figure 5. POU1903 showing "B" and "C" components.

Figure 6. POU1912 showing new "C" component. Figure 7. POU1920. Measuring to brighter companion.


Introduction

This paper identifies double star systems in Vulpec-ula that appear to have visual magnitudes that are in conflict with the data as published in the WDS. During the course of a long term project to image double stars accessible to backyard telescopes while employing a consistent imaging regime, from one location, the sheer volume of images has allowed the authors to identify with some certainty double star systems having compo-nent magnitudes that are clearly in conflict with the published data. After visually identifying these suspect systems, the authors consult the University of Stras-burg’s website, VizieR, to access the online digital sky survey catalogues to confirm the visual observations. The preliminary findings are listed below:

J 1303 - WDS mags. 9.8, 10.3. UCAC4 fmags 12.350 and 12.578; Vmag for “A” 12.086 but no value for "B". J 1303 actually belongs to Sagitta and somehow slipped into this list but we decided to keep it here to make use of the already existing photometry result. The image clearly shows, with the benefit of 4 additional field stars, that the WDS data is suspect (see Figure 1)

AG 247 – WDS mags. 9.02, 12 . UCAC4 provides fmags for A & B of 8.965 and 13.121 .Vmag for A only, 9.015. During our imaging run in Vulpecula, it became apparent, given the better seeing and transparency, our imaging setup was able to record

deeper, at least an additional magnitude, to reach beyond 12.5. In spite of this, our image contained only the smallest hint of the companion. We esti-mate “B” to be approaching magnitude 13. See Figure 2.

HJ 1504 – Chris Thuemen found what appeared to be clerical errors in the WDS data per April 2015 …position angles or magnitudes had been inter-changed…A for B and B for A, and sent Brian Ma-

Photometry of Faint and Wide Doubles in Vulpecula

Wilfried R.A. Knapp

Vienna, Austria [email protected]

Chris Thuemen

Double Star Imaging Project Pembroke, Ontario, Canada

[email protected]

Abstract: Images of several double stars in Vulpecula published on the “Double Star Imaging Project” Yahoo Group page suggest magnitude issues compared with the corresponding WDS catalog data per April 2015. Taking additional images with V-filter enabled photometry for these pairs, providing con-firming results.

Figure 1: J 1303





son/USNO an email to confirm this in the latter part of August 2015. This led to a change in the WDS data accordingly, including changes in the estimat-ed magnitudes for A, B, C to 7.1, 12.4, and 11.3.

A 264AB – WDS mags. of 8.20 and 13.00. There is conflicting data in the UCAC4 and NOMAD1 sur-veys. The image clearly shows something at the approximate location of the “B” component which tells us it has to be brighter than mag 13 with an estimation around 12.0. A careful review of the WDS records indicates there is is a second compo-nent, the “C” from MAD 7AC that is likely contrib-uting to the unexpected brightness at the “B” com-ponent location. A 264 is actually a multiple with six components including HDS 2720 Aa,Ab indi-cating A to be a close double itself. MAD 7 con-tains two entries in the WDS, MAD 7AC and BC. A star map (see Figure 3) based on the WDS data shows inconsistent positions for B and C. Using the WDS given positions for A and B for calculating separation and position angle with the formulae provided by Buchheim 2008 we get 3.1” and 285° PA means somewhat off from the listed values and for this reason we included MAD7 in our list. Also the coordinates for HDS2720 are somewhat ques-tionable – if A264A is a close double then HDS2720Aa cannot have identical coordinates.

HO 445 with WDS M1 9.8 and M2 10.9. The im-age is suggesting that the companion is dimmer than the WDS data. We estimate a magnitude in the order of 11.5

DAM 373 – was added to the list because it is in the same field of view as A 264 and WDS mags

with single digit precision suggested estimation instead of measurement. The WDS data indicates a DM of 2.2 but our image is suggesting the differ-ence to be negligible.

STF 2523CD a.k.a. KRU 8 – WDS mags of C and D are 7.10 & 14.20. The DSS2.F.POSSII image from Aladin very nicely shows the “D” component as a real bump on the southeast quadrant of the pri-mary “C” component. This is consistent with our new image in that the “D” component is quite obvi-ous and clearly separated from the primary. Com-ponent “D” is brighter than the mag. 12.804 (UCAC 4 # 556-091331) south southwest of the “C” star. We found no mag value for “D” from ei-ther UCAC4 or NOMAD1 data but we estimate the “D” component magnitude at ~11.9. A summary of the WDS April 2015 data is given in

Table 1. To investigate further our initial findings, we con-

cluded that the best approach would be to obtain new images suitable for photometry. These images were taken with an online 610mm f/6.5 CDK telescope hav-ing a resolution of 0.625 arcseconds per pixel and equipped with a V-filter, located in Auberry, California. Initial plate solving and stacking of 5 images each was done with AAVSO VPhot and plate solving of the stacked image was then repeated with Astrometrica with UCAC4 as reference star catalog. Photometry was completed with Astrometrica based on all plate solving using reference star Vmags. Only reference stars with magnitude between 10.5 and 14.5 were used because of the higher precision in this magnitude range, thus re-sults for stars significantly brighter are less reliable than

Figure 2. Image of AG 247 Figure 3. Star map of A 264 based on WDS coordinates.



ID Name RA Dec Sep PA M1 M2

WDS19157+1654 J 1303 AB Sge 19:15:42.819 +16:54:02.601 4.7 198 9.80 10.30

WDS20089+2520 AG 247 AB Vul 20:08:54.732 +25:20:12.403 39.0 30 9.02 12.00

WDS20225+2618 HJ 1504 AC Vul 20:22:32.589 +26:17:53.103 52.0 228 7.16 11.20

WDS19127+2435 A 264 AB Vul 19:12:42.437 +24:34:36.299 3.2 288 8.20 13.00

WDS19127+2435 A 264 DE Vul 19:12:44.250 +24:34:24.798 5.0 119 15.00 15.50

WDS19127+2435 A 264 AD Vul 19:12:42.437 +24:34:36.299 27.3 115 8.23 15.00

WDS19127+2435 MAD 7 AC Vul 19:12:42.437 +24:34:36.299 1.9 340 8.20 12.80

WDS19127+2435 MAD 7 BC Vul 19:12:42.218 +24:34:37.103 2.3 72 13.00 12.80

WDS19124+2435 HO 445 AB Vul 19:12:27.022 +24:35:29.102 5.4 243 9.80 10.90

WDS19126+2433 DAM 373 AB Vul 19:12:38.270 +24:32:37.297 8.7 123 12.00 14.20

WDS19268+2110 STF 2523

KRU 8 CD Vul 19:26:58.870 +21:06:22.997 10.5 138 7.10 14.20

Table 1: WDS 2015 April values for the objectsFurther Research

ID Name M1+ Err1 M2+ Err2 Date Notes

WDS19157+1654 J 1303 AB 12.677 0.07 13.042 0.07 2015.762

WDS20089+2520 AG 247 AB 9.987 0.06 12.942 0.06 2015.678 1

WDS20225+2618 HJ 1504 AB 6.981 0.08 12.304 0.08 2015.678 1

WDS20225+2618 HJ 1504 AC 6.981 0.08 11.218 0.08 2015.678 1

WDS19127+2435 A 264 AB 8.189 0.13 11.941 0.13 2015.678 1

WDS19127+2435 A 264 DE 15.021 0.22 15.423 0.30 2015.678 2

WDS19127+2435 A 264 AD 8.189 0.13 15.021 0.22 2015.678 3

WDS19127+2435 MAD 7 AC 8.189 0.13 - - 2015.678 4

WDS19127+2435 MAD 7 BC 11.941 0.13 - - 2015.678 5

WDS19124+2435 HO 445 AB 10.191 0.16 11.614 0.16 2015.678 1

WDS19126+2433 DAM 373 AB 13.918 0.15 14.480 0.17 2015.672 2

WDS19268+2110 STF2523

KRU 8 CD 6.402 0.17 12.818 0.18 2015.678 1

Table 2: Photometry and measurement results based on iTelescope iT24 images used with AAVSO VPhot

Notes:

1. A too bright for reliable photometry as the used UCAC4 reference stars were in the 12mag range

2. Very low SNR

3. A too bright for reliable photometry as the used UCAC4 reference stars were in the 12mag range. WDS mag for A not consistent (8.20 vs 8.23)

4. A too bright for reliable photometry as the used UCAC4 reference stars were in the 12mag range. No resolution for C, too close to the bright A component. Position C inconsistent from A and B

5. No resolution for C, too close to the bright A component. Position for MAD 7 B not consistent with A264 B



the results for star in the indicated magnitude range. The new values are included in Table 2. M+ is new measurement, Err is the error estimation calculated as

where SNR = Signal to noise ratio, dVmag = average Vmag error over all used reference stars (SNR and dVmag not listed due to space restrictions). Number of observations is 5 for all objects. Date given is the Bes-sel epoch of the observation.

Summary

With few exceptions the photometry results con-firmed the image based first impressions at least to some degree. In the Table 3 we give a summary per object.

References

Buchheim, Robert – 2008, CCD Double-Star Measure-ments at Altimira Observatory in 2007, Journal of Double Star Observations, Vol. 4 No. 1 Page 28

Acknowledgements

The following tools and resources have been used for this research:

Washington Double Star Catalog iTelescope AAVSO VPhot AAVSO APASS UCAC4 catalog via the University of Heidelberg

website Aladin Sky Atlas CDS, SIMBAD, VizieR, UCAC4,

Nomad, URAT1, GAIA 2MASS All Sky Catalog AstroPlanner Astrometrica

(Continued from page 348)

ID Name Notes

WDS19157+1654 J 1303 AB The components are about 3 mag fainter than listed but

delta_m remained similar to Jonckheere’s estimation

WDS20089+2520 AG 247 AB B is about 1 mag fainter than listed

WDS20225+2618 HJ 1504 AB

As already mentioned in the introduction the mag data

for B was changed meanwhile to 12.4 quite close to the

new measurement result of 12.304

WDS20225+2618 HJ 1504 AC

As already mentioned in the introduction the mag data

for C was changed meanwhile to 11.3 quite close to the

new measurement result of 11.218

WDS19127+2435 A 264 AB

B as suspected is more than 1 mag. brighter than

listed. Astrometry results based on Astrometrica:

19:12:42.517/+ 24:34:36.22 for A and 19:12:42.284/+

24:34:37.18 for B with average error 0.15/0.13 giving

3.320“ +/-0.198 separation and 286.806° +/-3.421 PA

rather confirm the current WDS Sep/PA data within the

given error range. Latest GAIA measurements with

19:12:42.448/+ 24:34:36.318 for A and 19:12:42.231/+

24:34:37.117 for B would give 3.066“ separation and

285.123° PA

WDS19127+2435 A 264 DE WDS mag for E 15.5 quite confirmed with 15.423

WDS19127+2435 A 264 AD WDS mag for D 15 quite confirmed with 15.041

WDS19127+2435 MAD 7 AC Position C could not be verified – A too bright and C

too close to be separated

WDS19127+2435 MAD 7 BC

Position for B measured with RA 19:12:42.284 with an

average error of 0.15 and Dec +24:34:37.18 with an av-

erage error of 0.13. With the given error range of our

tools we cannot decide if the A 264 or the MAD 7 data

should be corrected, it is only clear that the current

data does not match. Probably it would be best to ac-

cept the latest precise measurements from GAIA

WDS19124+2435 HO 445 AB Both components fainter than listed, especially B

WDS19126+2433 DAM 373 AB Both components fainter than listed, especially A

WDS19268+2110 KRU 8 CD D is about 1.5mag brighter than WDS listed

Table 3: Summary of results compared to WDS per April 2015. With a few exception WDS data changes are suggested

2 2102.5log (1 1/ )magErr dV SNR


1. Introduction

As follow up to the first two reports on J-objects in Cygnus (Knapp; Nanson 2016) and Delphinus (Knapp 2016) I selected for this report all J-objects in Lyra (Lyr), Equuleus (Equ), and Eridanus (Eri) given in the Tables 1 to 3 with all values based on WDS data as of April 2015.

2. Measurements

2.1 Photometry for the J-objects in Lyra For each of the listed J-objects one single image

was taken (in Bessel epoch 2015.713) with iTelescope iT24 with 3 second exposure time. The initial plate solving was done by AAVSO VPhot and in the few cases with negative VPhot result again but positive with MaxIm DL6/PinPoint. Each image was then once more plate solved with Astrometrica using the UCAC4 cata-log with reference stars in the Vmag range of 10.5 to 14.5 giving not only RA/Dec coordinates but also pho-tometry results for all reference stars used including an average dVmag error. The J-objects were then located in the center of the image (worked fine with few excep-tions indicating that the given RA/Dec coordinates are usually correct with the exceptions suggesting position problems) and photometry was then done using the As-trometrica procedure with point and click at the compo-nents delivering Vmag measurements based on all ref-erence stars used for plate solving. The only changing parameter was the aperture radius used for photometry aiming to keep it equal or at least near 1.5x FWHM. In cases with smaller separation the star disks touched or overlapped but allowed nevertheless individual pho-tometry even if less reliable than with clear separated

disks. J110 allowed only the measurement of the com-bined magnitude but even in this case it is then possible to make a well-founded estimation for the components

based on the initial observed m between the compo-nents based on the formula

according to Greaney 2012. Measurements of the J-objects in Lyra are given in

Table 4.

2.2 Photometry and Astrometry for the J-objects in Equ

Beginning with the J-objects in Equ, I decided to provide photometric results and astrometric measure-ments in the form of RA/Dec coordinates resulting from plate solving as well as separation and position angle calculated based on the RA/Dec coordinates of the components. This is done by using the spherical trigonometry formulas provided by Buchheim 2008.

Measurements of the J-objects in Equ are given in Table 5.

2.3 Photometry and Astrometry for the J-objects in Eri In Table 6, I again report photometric results and

astrometric measurements in the form of RA/Dec coor-dinates resulting from plate solving as well as separa-tion and position angle calculated based on the RA/Dec coordinates of the components. This is done by using the spherical trigonometry formulas provided by Buch-heim 2008.

Table 6 gives the measurements of the J-objects in Eri.

(Continued on page 360)

Jonckheere Double Star Photometry – Part III: Lyra, Equuleus, and Eridanus

Wilfried R.A. Knapp


Abstract: If any double star discoverer is in urgent need of photometry then it is Jonckheere. There are over 3000 Jonckheere objects listed in the WDS catalog and a good part of them have magnitudes which are obviously far too bright. To keep the workload manageable only one im-age per object is taken and photometry is done with a software allowing a simple point and click procedure – even a single measurement is better than the currently usually given estimation.

1` 2102.5log 2.521 2.521

m mcombinedm




WDS ID Name RA Dec Sep M1 M2 PA

18511+3524 J110 AB 18:51:06.099 +35:24:14.095 2.0 10.47 11.81 174

19018+3337 J112 AB 19:01:48.373 +33:37:16.501 25.4 6.39 13.30 178

18497+3223 J131 AB 18:49:41.470 +32:23:14.701 2.7 10.77 13.00 179

18386+2937 J525 AB 18:38:31.427 +29:37:06.997 3.1 9.20 9.40 69

18225+3130 J760 AB 18:22:28.757 +31:30:17.400 2.4 9.50 13.00 212

18274+3137 J761 AB 18:27:19.009 +31:36:35.803 3.7 9.60 11.20 180

18300+4033 J762 AB 18:30:01.387 +40:34:18.206 3.9 10.00 12.50 249

18301+4325 J763 AB 18:30:09.647 +43:26:30.106 1.8 9.70 9.70 309

18349+4053 J764 AB 18:34:53.410 +40:54:10.099 2.8 12.56 13.70 201

18494+3324 J765 AB 18:49:11.951 +33:25:51.105 2.3 12.30 12.50 333

19030+3729 J766 AB 19:02:56.942 +37:27:53.300 3.0 10.80 11.40 2

19030+3729 J766 AC 19:02:56.942 +37:27:53.300 16.7 10.80 12.10 176

19064+3750 J767 AB 19:06:29.987 +37:49:27.503 3.0 10.51 12.00 1

19064+3750 J767 AC 19:06:29.987 +37:49:27.503 7.9 10.51 13.00 181

19131+2946 J768 AB 19:13:05.571 +29:46:56.798 2.9 10.50 12.20 350

19203+2914 J769 AB 19:20:15.527 +29:12:01.500 3.7 9.70 9.90 207

19031+2757 J811 AB 19:03:08.340 +27:56:44.903 2.6 11.90 12.40 248

18381+3000 J1138 AB 18:38:00.693 +30:00:38.802 2.7 9.80 9.80 300

19075+2728 J1205 AB 19:07:25.667 +27:28:39.202 3.5 10.00 10.20 317

19117+2712 J1206 AB 19:11:37.632 +27:12:44.703 3.0 11.94 12.20 332

18491+2834 J1208 AB 18:49:09.932 +28:34:17.499 5.0 9.50 10.00 333

19045+3406 J1209 AB 19:04:25.079 +34:06:19.893 4.6 9.50 10.00 155

19115+2953 J1263 AB 19:11:31.418 +29:53:24.602 31.1 7.62 13.00 255

19115+2953 J1263 BC 19:11:28.699 +29:53:10.203 8.0 13.00 14.10 42

19047+2850 J2941 AB 19:04:46.441 +28:51:04.499 8.6 10.80 12.50 234

19056+2848 J2942 AB 19:05:40.549 +28:49:42.802 6.8 11.80 13.00 60

19079+3043 J2945 AC 19:07:48.567 +30:43:36.202 9.8 10.81 14.10 192

19068+3815 J3213 AB 19:06:51.500 +38:15:42.105 2.5 9.70 9.70 201

19145+2945 J3313 AB 19:14:31.738 +29:45:13.898 10.7 8.94 14.00 32

Table 1: WDS April 2015 values for the Jonckheere objects in Lyra sorted by designation number



Table 2: WDS April 2015 values for the Jonckheere objects in Equuleus sorted by designation number


21021+1016 J158 AB 21:02:08.863 +10:17:33.400 5.0 10.93 13.10 166

21086+0938 J159 AB 21:08:35.231 +09:37:46.301 4.0 10.30 11.30 247

21225+1057 J161 AB 21:22:28.071 +10:57:18.401 2.0 10.45 10.66 299

21124+0745 J576 AB 21:12:25.450 +07:45:06.101 2.3 10.10 10.60 236

20595+1113 J608 AB 20:59:27.721 +11:13:22.301 5.0 11.20 13.50 105

21091+0429 J848 AB 21:09:07.730 +04:28:57.100 2.6 10.23 13.00 145

20592+1129 J913 AB 20:59:09.882 +11:28:41.001 2.9 9.20 10.90 120

21242+0248 J914 AB 21:24:11.060 +02:46:59.600 1.9 11.11 11.11 0

21256+0248 J1039 AB 21:25:37.509 +02:47:43.900 4.3 9.60 10.50 332

21224+0953 J1356 AB 21:22:26.478 +09:52:36.200 7.7 12.00 12.40 178

21192+0339 J1721 AB 21:19:20.568 +03:40:56.800 3.8 11.10 13.80 275

21066+1137 J1781 AB 21:06:38.907 +11:36:55.802 7.8 9.40 11.00 117

21197+0537 J2341 AB 21:19:43.111 +05:37:11.900 7.3 11.90 11.90 349

21071+1042 J2576 AB 21:06:55.702 +10:29:50.099 6.1 12.00 13.00 59

21222+1114 J2605 AB 21:22:21.451 +11:13:50.800 1.9 11.55 13.30 222

Table 3: WDS April 2015 values for the Jonckheere objects in Eridanus sorted by designation number


04531-1039 J318 AB 04:53:10.249 -10:39:16.900 4.8 12.44 12.60 286

05043-0514 J319 AB 05:04:21.341 -05:12:59.700 3.3 11.05 12.10 233

04234-0634 J708 AB 04:23:23.471 -06:34:15.400 2.2 10.84 11.13 282

04297-0335 J709 AB 04:29:42.339 -03:34:40.600 1.2 10.72 10.86 87

04383-0243 J710 AB 04:38:19.390 -02:42:55.900 3.2 10.50 11.70 315

04584-0908 J1003 AB 04:58:26.311 -09:06:00.101 5.4 11.36 13.60 238

05088-0830 J1004 AB 05:08:49.960 -08:30:58.801 3.3 12.52 12.50 322

04302-0337 J1087 AB 04:30:12.760 -03:37:12.900 2.6 11.06 15.10 13

02475-0601 J1245 AB 02:47:29.960 -06:00:51.801 2.3 11.00 11.04 12

02501-0616 J1453 AB 02:50:07.000 -06:16:11.900 9.2 11.10 10.70 201

02501-0616 J1453 AC 02:50:07.000 -06:16:11.900 38.5 11.13 13.00 69

03032-0215 J1455 AB 03:03:07.460 -02:14:53.700 6.2 11.50 11.80 61

03175-1222 J1456 AB 03:17:30.390 -12:22:51.801 3.6 11.06 11.16 319

03361-0320 J1457 AB 03:36:04.420 -03:20:05.800 2.9 10.34 10.84 216

04220-0626 J1459 AB 04:21:59.820 -06:25:33.901 3.0 11.03 11.10 241



Table 4. Bessel epoch 2015.713 photometry results for the J objects in Lyr. “M1 WDS” and “M2 WDS” are the WDS catalog values. “M1 new” stands for measured M1, “dM1” stands for delta between “M1 WDS” and “M1 new”. “M2 new” stands for measured M2, “dM2” stands for delta “M1 WDS” and “M1 new”. “Err M1” stands for the estimated error range calcu-lated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2


18511+3524 J110 AB 10.47 10.710 -0.240 0.130 11.81 12.050 -0.240 0.130

Overlapping star

disks - no separate


Combined magnitude

10.436 with SNR

132.41 gives estimat-

ed “M1 new” and “M2


ing rather well the

current WDS values

19018+3337 J112 AB 6.39 6.504 -0.114 0.180 13.30 12.582 0.718 0.182 A too bright for re-

liable photometry

18497+3223 J131 AB 10.77 10.767 0.003 0.150 13.00 - - -

No resolution of B

suggests B being far

fainter than listed

18386+2937 J525 AB 9.20 11.162 -1.962 0.141 9.40 11.342 -1.942 0.141

18225+3130 J760 AB 9.50 11.524 -2.024 0.130 13.00 12.914 0.086 0.133

18274+3137 J761 AB 9.60 11.211 -1.611 0.140 11.20 12.801 -1.601 0.143

18300+4033 J762 AB 10.00 12.404 -2.404 0.082 12.50 13.643 -1.143 0.090

18301+4325 J763 AB 9.70 11.975 -2.275 0.076 9.70 12.250 -2.550 0.081 Touching/Overlapping

star disks

18349+4053 J764 AB 12.56 11.751 0.809 0.052 13.70 12.395 1.305 0.055

18494+3324 J765 AB 12.30 11.385 0.915 0.160 12.50 11.408 1.092 0.160 Touching star disks


19030+3729 J766 AC 10.80 11.718 -0.918 0.131 12.10 12.780 -0.680 0.132

19064+3750 J767 AB 10.51 11.587 -1.077 0.141 12.00 13.140 -1.140 0.146

19064+3750 J767 AC 10.51 11.587 -1.077 0.141 13.00 13.994 -0.994 0.150

19131+2946 J768 AB 10.50 12.356 -1.856 0.152 12.20 14.681 -2.481 0.174 SNR for B <20

19203+2914 J769 AB 9.70 11.603 -1.903 0.160 9.90 12.185 -2.285 0.161

19031+2757 J811 AB 11.90 11.699 0.201 0.151 12.40 12.973 -0.573 0.164 Touching star disks.

SNR for B <20


19075+2728 J1205 AB 10.00 12.094 -2.094 0.161 10.20 12.250 -2.050 0.162

19117+2712 J1206 AB 11.94 13.373 -1.433 0.174 12.20 13.479 -1.279 0.175

No double star at

this position. Nearby

A 19 11 46.012 +27 12

02.68 and B 19 11

45.900 +27 12 04.86

with dRA 0.14 and

dDec 0.15 giving Sep

2.643" with Err 0.205

and PA 325.573° with

Err 4.439

18491+2834 J1208 AB 9.50 11.538 -2.038 0.131 10.00 12.051 -2.051 0.131

Minor position issue:

A 18 49 14.783 +28 34

46.97 18 49 14.627

+28 34 51.17 with dRA

0.14 and dDec 0.15

giving Sep 4.676"

with Err 0.205 and PA

333.930° with Err

2.413

19045+3406 J1209 AB 9.50 11.529 -2.029 0.190 10.00 12.303 -2.303 0.191




Table 4 (conclusion). Bessel epoch 2015.713 photometry results for the J objects in Lyr. “M1 WDS” and “M2 WDS” are the WDS catalog values. “M1 new” stands for measured M1, “dM1” stands for delta between “M1 WDS” and “M1 new”. “M2 new” stands for measured M2, “dM2” stands for delta “M1 WDS” and “M1 new”. “Err M1” stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2


19115+2953 J1263 AB 7.62 7.466 0.154 0.140 13.00 12.917 0.083 0.142

A too bright for re-

liable measurement,

star disk looks elon-

gated, might be a

close double itself

19115+2953 J1263 BC 13.00 12.917 0.083 0.142 14.10 14.040 0.060 0.151 SNR for C <20

19047+2850 J2941 AB 10.80 12.361 -1.561 0.141 12.50 14.402 -1.902 0.150 SNR for B <20

19056+2848 J2942 AB 11.80 13.155 -1.355 0.152 13.00 14.433 -1.433 0.165 SNR for B <20

19079+3043 J2945 AC 10.81 10.616 0.194 0.150 14.10 13.685 0.415 0.156

Mag for HLM16 B meas-

ured with 12.340 with

SNR 51.98 (WDS lists

12.7mag)


“Touching star disks” indicates that the rims of the star disks are touching and that the measurement results might be a bit less precise than with clearly separated star disks

“Overlapping/Touching star disks” indicates that the star disks overlap to the degree of an elongation and that the meas-urement results is probably less precise than with clearly separated star disks

“Overlapping star disks” indicates star disk overlap to the degree that photometry for the separated components was no longer possible and that it was necessary to resort to the measurement of the combined magnitude

“Low SNR <20” indicates that the measurement result might be a bit less precise than desired due to a low SNR value but this is already included in the calculation of the error range estimation

“too bright for reliable photometry” indicates a star far brighter than the for plate solving used range 10.5 to 14.5mag – despite this most such cases showed a reasonable measurement result anyway

In case of questionable astrometric data separation and position angle is calculated based on the RA/Dec coordinates of the components. This is done using the formulas provided by Buchheim 2008

Specifications of the used telescope: T24: 610mm CDK with 3962mm focal length. Resolution 0.625 arcsec/pixel. V-filter. No transformation coefficients available. Located in Auberry, California. Elevation 1405m



Table 5. Bessel epoch 2015.837 astrometry and photometry results for the J objects in Equ plus BRT1355 as bonus. Number of observations is 1. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. Sep is separation calculated as SQRT(((RA2-RA1)*cos(Dec1))^2+(Dec2-Dec1)^2) in radians. Err Sep is the error estimation for Sep calculated as SQRT(dRA^2+dDec^2). The position angle PA is calculated as arctan((RA2-RA1)*cos(Dec1))/(Dec2-Dec1)) in radians and Err_PA is the error estimation for PA calculated as arctan(Err_Sep/Sep) in degrees as-suming the worst case that Err_Sep points in the right angle to the direction of the separation means perpendicular to the separation vector. “Err Mag” stands for the estimated error range calculated from the average delta Vmag over all refer-ence stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2)


Name RA Dec Sep Err Sep PA Err PA Mag Err Mag Notes

J 158

A 21 02 08.841 10 17 33.41

5.386 0.270 168.621 2.872

10.641 0.191 iT27 1x3s. SNR for

B<20 B 21 02 08.913 10 17 28.13 12.861 0.207

J 159

A 21 08 35.186 09 37 44.36

4.171 0.336 245.192 4.606

9.843 0.100

iT27 1x3s

B 21 08 34.930 09 37 42.61 11.652 0.104

J 161

A 21 22 28.149 10 57 17.73

2.488 0.236 289.735 5.420

10.163 0.091 iT27 1x3s. Touching/

Overlapping star

disks B 21 22 27.990 10 57 18.57 10.306 0.091

J 576

A 21 12 25.542 07 45 06.52

2.357 0.297 237.681 7.182

10.791 0.092 iT27 1x3s. Touching/

Overlapping star

disks B 21 12 25.408 07 45 05.26 10.844 0.092

J 608

A 20 59 27.719 11 13 22.35

5.003 0.304 112.567 3.479

10.965 0.102 iT27 1x3s. SNR for

B<10, barely to see B 20 59 28.033 11 13 20.43 14.233 0.227

J 848

A 21 09 07.719 04 28 56.66

2.806 0.348 140.646 7.074

9.982 0.081 iT27 1x3s. Touching/

Overlapping star

disks B 21 09 07.838 04 28 54.49 12.324 0.090

J 913

A 20 59 09.859 11 28 40.68

2.686 0.374 123.697 7.937

10.811 0.111 iT27 1x3s. Touching/

Overlapping star

disks B 20 59 10.011 11 28 39.19 12.485 0.121

J 914

A 21 24 11.162 02 46 59.33

2.040 0.311 0.842 8.671

10.800 0.071 iT27 1x3s. Touching/

Overlapping star

disks B 21 24 11.164 02 47 01.37 10.978 0.071

J 1039

A 21 25 37.490 02 47 41.91

4.722 0.291 343.598 3.523

12.160 0.073 iT27 1x3s. SNR for

B<20 B 21 25 37.401 02 47 46.44 14.117 0.093

J 1356 A 21 22 26.526 09 52 37.01

7.993 0.255 175.653 1.827 11.936 0.111

iT27 1x3s B 21 22 26.567 09 52 29.04 12.847 0.113

J 1721 A 21 19 20.592 03 40 56.73

3.161 0.205 272.357 3.714 11.248 0.061

iT27 1x3s B 21 19 20.381 03 40 56.86 12.587 0.066



Table 5 (conclusion). Bessel epoch 2015.837 astrometry and photometry results for the J objects in Equ plus BRT1355 as bo-nus. Number of observations is 1. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. Sep is separation calculated as SQRT(((RA2-RA1)*cos(Dec1))^2+(Dec2-Dec1)^2) in radians. Err Sep is the error estimation for Sep calculated as SQRT(dRA^2+dDec^2). The position angle PA is calculated as arctan((RA2-RA1)*cos(Dec1))/(Dec2-Dec1)) in radians and Err_PA is the error estimation for PA calculated as arctan(Err_Sep/Sep) in degrees assuming the worst case that Err_Sep points in the right angle to the direction of the separation means perpendicular to the separation vector. “Err Mag” stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2)


J 1781 A 21 06 38.930 11 36 54.99

7.499 0.355 116.447 2.711 10.718 0.101

iT27 1x3s B 21 06 39.387 11 36 51.65 12.405 0.103

J 2341 A 21 19 43.114 05 37 11.38

7.424 0.292 349.926 2.249 12.090 0.092

iT27 1x3s B 21 19 43.027 05 37 18.69 13.156 0.094

J 2576

A 21 06 55.769 10 29 50.38

5.393 0.382 57.973 4.050

14.453 0.127 iT27 1x3s. SNR for A

and B<20. No good

match with the origi-

nal Jonckheere 12/13

mags B 21 06 56.079 10 29 53.24 14.146 0.139

J 2605

A 21 22 21.445 11 13 50.63

2.055 0.318 226.301 8.802

12.333 0.088 iT27 1x3s. Touching/

Overlapping star

disks B 21 22 21.344 11 13 49.21 12.369 0.090

BRT1355

A 21 22 25.570 11 11 01.00

3.912 0.318 194.373 4.651

11.491 0.082 iT27 1x3s. Touching

star disks B 21 22 25.504 11 10 57.21 12.528 0.087


“iT27 1x3s” indicates that the given values base on one iT27 image with 3 seconds exposure time.


“Overlapping/Touching star disks” indicates that the star disks overlap to the degree of an elongation and that the meas-urement results is probably less precise than with clearly separated star disks.

“Overlapping star disks” indicates star disk overlap to the degree that photometry for the separated components was no longer possible and that it was necessary to resort to the measurement of the combined magnitude.

“Low SNR <20” indicates that the measurement result might be a bit less precise than desired due to a low SNR value but this is already included in the calculation of the error range estimation.

“too bright for reliable photometry” indicates a star far brighter than the range used in plate solving (mag. 10.5 to 14.5), despite this most such cases showed a reasonable measurement result anyway.

Specifications of the used telescope: iT27: 700mm CDK with 4531mm focal length. CCD: FLI PL09000. Resolution 0.53 arcsec/pixel. V-filter. No B-V transformation coefficients available. Located in Siding Spring, Australia. Elevation 1122m



Table 6. Bessel epoch 2015.966 astrometry and photometry results for the J objects in Eri. Number of observations is 1. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. Sep is separa-tion calculated as SQRT(((RA2-RA1)*cos(Dec1))^2+(Dec2-Dec1)^2) in radians. Err Sep is the error estimation for Sep cal-culated as SQRT(dRA^2+dDec^2). The position angle PA is calculated as arctan((RA2-RA1)*cos(Dec1))/(Dec2-Dec1)) in ra-dians and Err_PA is the error estimation for PA calculated as arctan(Err_Sep/Sep) in degrees assuming the worst case that Err_Sep points in the right angle to the direction of the separation means perpendicular to the separation vector. “Err Mag” stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2)



J 318

A 04 53 10.255 -10 39 17.09

4.816 0.219 286.031 2.607

11.319 0.061

iT27 1x3s

B 04 53 09.941 -10 39 15.76 11.738 0.061

J 319

A 05 04 21.336 -05 12 59.55

3.399 0.213 233.958 3.579

10.982 0.061

iT27 1x3s

B 05 04 21.152 -05 13 01.55 11.821 0.061

J 708

A 04 23 23.450 -06 34 15.70

2.279 0.248 286.045 6.199

10.596 0.062 iT27 1x3s. Touching/

Overlapping star

disks B 04 23 23.303 -06 34 15.07 10.836 0.061

J 709 04 29 42.350 -03 34 40.90 - 0.248 - - 10.245 0.051

iT27 1x3s. No resolu-

tion but elongation

according to the

listed WDS PA. Com-

bined magnitude

10.245 suggests

10.93/11.07mag for A/

B keeping the given

delta_m

J 710

A 04 38 19.368 -02 42 55.82

3.096 0.227 315.817 4.189

10.478 0.061 iT27 1x3s. Touching

star disks B 04 38 19.224 -02 42 53.60 11.706 0.066

J 1003

A 04 58 26.324 -09 06 00.31

5.536 0.262 236.317 2.707

11.287 0.061

iT27 1x3s

B 04 58 26.013 -09 06 03.38 13.151 0.063

J 1004

A 05 08 49.953 -08 30 58.89

3.233 0.233 320.371 4.130

12.305 0.062

iT27 1x3s

B 05 08 49.814 -08 30 56.40 12.402 0.062

J 1087

A 04 30 12.763 -03 37 13.78

2.965 0.361 16.723 6.935

11.047 0.101 iT27 1x3s. Touching/

Overlapping star

disks B 04 30 12.820 -03 37 10.94 13.149 0.109

J 1245

A 02 47 29.959 -06 00 52.63

2.642 0.304 20.149 6.568

10.402 0.076 iT27 1x3s. Touching/

Overlapping star

disks B 02 47 30.020 -06 00 50.15 10.615 0.083



Table 6 (conclusion). Bessel epoch 2015.966 astrometry and photometry results for the J objects in Eri. Number of observa-tions is 1. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. Sep is separation calculated as SQRT(((RA2-RA1)*cos(Dec1))^2+(Dec2-Dec1)^2) in radians. Err Sep is the error estimation for Sep calculated as SQRT(dRA^2+dDec^2). The position angle PA is calculated as arctan((RA2-RA1)*cos(Dec1))/(Dec2-Dec1)) in radians and Err_PA is the error estimation for PA calculated as arctan(Err_Sep/Sep) in degrees assuming the worst case that Err_Sep points in the right angle to the direction of the separation means perpendicular to the separation vec-tor. “Err Mag” stands for the estimated error range calculated from the average delta Vmag over all reference stars used in the image and the SNR value of the star with the formula SQRT(dVmag^2+(2.5*LOG10(1+1/SNR))^2)


J 1453

A 02 50 07.009 -06 16 12.02

9.500 0.336 200.296 2.027

10.977 0.092

iT27 1x3s

B 02 50 06.788 -06 16 20.93 11.287 0.092

J 1453

A 02 50 07.009 -06 16 12.02

38.360 0.336 68.096 0.502

10.977 0.092

iT27 1x3s

C 02 50 09.396 -06 15 57.71 12.974 0.101

J 1455

A 03 03 07.440 -02 14 54.05

6.257 0.178 63.008 1.630

11.577 0.080

iT27 1x3s

B 03 03 07.812 -02 14 51.21 11.941 0.081

J 1456

A 03 17 30.417 -12 22 51.62

3.890 0.311 325.603 4.577

11.098 0.101

iT27 1x3s

B 03 17 30.267 -12 22 48.41 11.014 0.101

J 1457

A 03 36 04.465 -03 20 04.95

3.277 0.318 220.809 5.548

10.104 0.131 iT27 1x3s. Touching

star disks B 03 36 04.322 -03 20 07.43 10.368 0.134

J 1459

A 04 22 00.001 -06 25 32.96

3.155 0.278 240.369 5.036

10.996 0.052 iT27 1x3s. Touching

star disks

B 04 21 59.817 -06 25 34.52 10.919 0.051


“iT27 1x3s” indicates that the given values base on one iT27 image with 3 seconds exposure time.


“Overlapping/Touching star disks” indicates that the star disks overlap to the degree of an elongation and that the meas-urement results are probably less precise than with clearly separated star disks.

“Overlapping star disks” indicates star disk overlap to the degree that photometry for the separated components was no longer possible and that it was necessary to resort to the measurement of the combined magnitude.

“Low SNR <20” indicates that the measurement result might be a bit less precise than desired due to a low SNR value but this is already included in the calculation of the error range estimation.

“too bright for reliable photometry” indicates a star far brighter than the for plate solving used range 10.5 to 14.5mag – despite this most such cases showed a reasonable measurement result anyway.

Specifications of the used telescope: -iT27: 700mm CDK with 4531mm focal length. CCD: FLI PL09000. Resolution 0.53 arcsec/pixel. V-filter. No B-V transformation coefficients available. Located in Siding Spring, Australia. Elevation 1122m



3. Summary

All result tables show, with some exceptions, quite large differences for the magnitudes compared with the WDS data often even in cases where double digit val-ues suggest recent precise measurements. But it is obvi-ous that the Jonckheere objects in more southern con-stellations have been visited rather often compared to the J-objects in the more northern constellations also with the effect of a far better data quality. A few cases suggest errors in position, separation, and position an-gle as the difference to the WDS data is larger than the given error estimation. In some cases the available equipment did not allow separate measurement due to heavily overlapping star disks. The measurement of the combined magnitude allowed an estimation of the com-

ponents on the basis of the given m using the formula provided by Greaney 2012.

Special cases:

J131B in Lyr: No resolution, B probably fainter than +13mag

J1206 in Lyr: WDS gives here for unknown reasons a position slightly different from the WDS ID. The measured position is a better match with the WDS ID (assumed to be the original position given by Jonckheere) and is also confirmed by an elongation in the 2MASS image

J1208 in Lyr: Position error in WDS catalog by about 72 arcseconds. Measured position confirmed by UCAC4 catalog with 593-069152 and 593-069151

J2576 in Equ: No good match with the original Jonckheere 12/13 mag estimation. J2576 was not found at the given IDS position by Heintz accord-ing to his 1990 paper and the current precise WDS position seems to be given for a potential candidate with similar parameters for separation and position angle – but at the cost of a rather bad match of the estimated magnitudes compared with the measured 14.45/14.15mag regarding not only delta_m but also position of the primary. Measurement results confirmed by UCAC4 catalog objects 503-140424 and 503-140426. Unfortunately the star field around the given position does not offer another better matching candidate so we can either take what we have or declare J2576 as lost Jonckheere object.

Acknowledgements


AAVSO APASS (via the UCAC4 catalog)

AAVSO VPhot Aladin Sky Atlas v8.0 Astrometrica v4.8.2.405 AstroPlanner v2.2 iTelescope iT24 & iT27 MaxIm DL6 v6.08 SIMBAD, VizieR, UCAC4, URAT1, GAIA UCAC4 catalog via the University of Heidelberg

website and directly from USNO DVD

Washington Double Star Catalog

References


Greaney, Michael – 2012, "Some Useful Formulae" in R.W. Argyle, Observing and Measuring Visual Double Stars, 2nd Edition 2012, Chapter 25, Page 359

Heintz, W.D. – 1990, Observations of double stars and new pairs. XIV. Astrophysical Journal Supplement Series Vol. 74, p. 275-290

Knapp, Wilfried; Nanson, John – 2016, Jonckheere Double Star Photometry – Part I: Cyg, Journal of Double Star Observing, Vol. 12 No 2 pp. nn-mm

Knapp, Wilfried – 2016, Jonckheere Double Star Pho-tometry – Part II: Del, Journal of Double Star Ob-serving, Vol. 12 No 3 pp. nn-mm



1. Introduction

As follow up to our reports “STT Doubles with Large delta_M – Part I, II and III” we continued in the constellations of Ophiuchus (Oph) and Hercules (Her), which contained 9 objects from our list (see Table 1) conveniently located with reasonable altitude at the time of observation. All values are from the WDS data as of the end of 2014.

2. Further Research

Following the procedure for parts I, II, and III of our report we concluded again that the best approach would be to check historical data on all objects, observe

them visually with the target of comparing with the ex-isting data and obtain as many images as possible suita-ble for photometry.

2.1 Historical Research and Catalog Comparisons Of the nine stars in this survey, five of them have

notable aspects worth further investigation. Three main research sources were used for this section of the paper, the first of which was W.J. Hussey’s Micrometrical Observations of the Double Stars Discovered at Pulko-vo, published in 1901, which provided preliminary his-torical information on each of the stars. Hussey’s book includes his observations and measures of all the stars originally listed in Otto Wilhelm Struve’s 1845 Pulko-

STT Doubles with Large ΔM – Part IV: Ophiuchus and Hercules

Wilfried R.A. Knapp


John Nanson

Star Splitters Double Star Blog Manzanita, Oregon

[email protected]

Abstract: The results of visual double star observing sessions suggested a pattern for STT dou-

bles with large M of being harder to resolve than would be expected based on the WDS catalog data. It was felt this might be a problem with expectations on one hand, and on the other might be an indication of a need for new precise measurements, so we decided to take a closer look at a selected sample of STT doubles and do some research. We found that like in the other con-stellations covered so far (Gem, Leo, UMa, etc.) at least several of the selected objects in Ophiu-chus and Hercules show parameters quite different from the current WDS data.

Name Comp ID RA Dec Con Sep PA M1 M2 ΔM

STT 326 AB 17183+0931 17:18:15.811 +09:31:03.899 Oph 17.9 223 8.10 12.40 4.30

STT 342 AB 18073+0934 18:07:21.019 +09:33:49.199 Oph 24.8 298 3.73 14.00 10.27

STT 310 AB 16254+3755 16:25:25.459 +37:54:36.796 Her 3.0 226 8.40 11.00 2.60

STT 314 AB 16389+2028 16:38:51.498 +20:27:57.599 Her 3.8 234 8.80 11.70 2.90

STT 317 AB 16530+4424 16:52:57.219 +44:24:08.000 Her 24.8 200 8.21 12.00 3.79

STT 324 AB 17080+3112 17:08:00.700 +31:12:22.497 Her 3.5 220 6.60 11.10 4.50

STT 328 AB 17173+3306 17:17:19.568 +33:06:00.406 Her 4.2 59 4.80 10.20 5.40

STT 338 AC 17520+1520 17:51:58.462 +15:19:34.899 Her 32.8 201 7.21 13.60 6.39

STT 585 BP 16450+0605 16:44:57.961 +06:02:37.099 Her 77.4 3 10.4 13.10 2.70

Table 1. WDS 2014.96 values for the selected STT objects in Oph and Her





vo Catalog, as well as data beginning with the date of first measure and continuing through the following years up to 1900. That data, plus inclusion of the back-ground for the Pulkovo Catalog, makes Hussey’s book a valuable source of reference. Also consulted was S.W. Burnham’s A General Catalogue of Double Stars Within 121° of the North Pole, Part II, for information on STT 585. In addition, Bill Hartkopf of the USNO graciously supplied text files for STT 324, 326, 338, 342, and 585, as well as other information.

STT 317 (Her) stood out immediately as a star worth further investigation because of the very noticea-ble changes in position angle and separation of the AB pair. According to Hussey’s data (Hussey, 1910, p. 137), Johann Heinrich Mädler made the first measure-ments of STT 317 AB in 1843, which were 234.1° and 15.39". The most recent WDS data (dated 2013) at the time we made observations of STT 317 showed a posi-tion angle of 200° and a separation of 24.80". That considerable change in PA and separation is due to the two stars moving in opposite directions, which is shown in Figure 2. Also notable in the image is the high prop-er motion of the C component relative to A and B. However, there is less change between the first AC measures in 1874 (318.1° and 113.40") and the 2013 WDS measures (316° and 130.40") due to the two stars moving in similar directions.

STT 324 (Her) shows measurements changing from 213.6° and 3.8" in 1848 to 219.9° and 3.5" in 2000, the date of the most recent measures in the WDS. We requested the text file to see what changes had tak-en place in the 152 years between those two dates and

found almost all of the fourteen measures between 1867 and 2000 (Table 2) showed a position angle in the range of 219° to 221°. The separations are more errat-ic, ranging from a high of 4.05" in 1869 by Dembowski to a low of 3.5" in 2000. Hussey (1901, p. 139) shows the first measures of STT 324 in 1848 were made by Otto Struve, and he also shows a follow-up measure of 218.5° and 3.87" by Struve in 1853 which is not listed in the WDS text file. So in general, it appears the posi-tion angle of this pair has been rather consistently in the 220° range, while the separation has fluctuated some-what, averaging out to 3.79".

STT 326 (Oph) stood out because of a consistent change in position angle and separation, which is a re-sult of the two stars moving away from each other. The WDS proper motion numbers show the primary is moving east and south at a relatively slow rate of +027 -020, while the secondary is moving west and south at similar rate, -015 -021. When the 139 years of data of shown in the WDS is plotted, the consistent trend is very obvious, see Figure 2.

STT 342 (Oph) has a strange history which be-gan with Otto Struve’s 1841 observation of a compan-ion at an estimated distance of 1.5". He recorded eight additional observations (Figure 3) of what he identified as an eighth magnitude companion, several of which described it as “suspect.” (Hussey, 1901, pp. 144-45).


Figure 1. Proper Motion of STT 317 Components

Table 2. Data from WDS Text File for STT 324



Figure 2. STT 326 Measures from WDS Text File

Figure 3. Otto Struve's Observations of Close Companion of STT 342 (from Hussey, 1901, p. 145).



But as Hussey states, Struve also recorded another eight observations in which he failed to see the companion. Although other observers also reported measures be-tween 1845 and 1884, no one reported the sighting of the companion when using large refractors, specifically the 26 inch at the USNO and the 36 inch at Lick. Hus-sey, S.W. Burnham, and R.G. Aitken each used the 36 inch Lick Refractor with no success during the period 1889 to 1898, which seems to have effectively decided the matter.

Burnham credits Simon Newcomb with the first measure of the star now identified as B, which surpris-ingly didn’t occur until 1890, perhaps because of all the attention focused on the spurious close companion. The star now identified as C was discovered by John Herschel in 1827, which he cataloged as H 5943.

STT 585 (Her) is included here because of its anomalous numbering. When Otto Struve published his first Dorpat catalog in 1845, it ended at number 514. That catalog also was restricted to pairs with separa-tions of 16” or less for companions fainter than ninth magnitude. All of the components of STT 585 are well over that limit, and all are fainter than tenth magnitude. The pairs wider than 16” of separation were added to Struve’s appendix, which included a total of 254 stars.

So STT 585 stands out as being peculiarly num-bered, which is significant also because the first measures of it weren’t made until 1854. Research in Burnham’s 1906 General Catalog (Burnham, 1901, p. 725) shows STT 585 is referred to only as 41 Herculis, and a 1996 copy of the WDS shows the star and its components referred to only as STT, with no number attached. However, a look at a 2001 copy of the WDS found the system had been designated as STT 585. A request to Bill Hartkopf at the WDS for background on the numbering provided information that stars such as this, which were not numbered in the IDS catalog (the predecessor to the WDS), were later given designations by Brian Mason of the WDS.

2.2 Visual Observations Both Nanson and Knapp made visual observations

of the stars included in this report. Nanson used a 152 mm f/10 refractor and a 235 mm SCT, while Knapp utilized 140 mm and 185 mm refractors and a 235 mm SCT, as well as a masking device to evaluate what could be seen at lesser apertures.

STT 310 (Her): This was a difficult pair with a magnitude differential of 2.4 and a separation of 3“ ac-cording to the WDS data. Nanson observed it at the meridian with a six inch f/10 refractor and detected a definite elongation at 380x, and had a brief glimpse of a dot of light at the correct PA. Given the difficulty, he

estimated the secondary was slightly fainter than the WDS magnitude of 11.0. Knapp observed the second-ary at 200x in a 140 mm refractor and could still see it when the aperture was reduced to 110 mm, suggesting a magnitude slightly brighter than 11.0.

STT 314 (Her): Knapp observed this pair twice with a 185 mm refractor and resolved the secondary at 250x and 360x. He noticed a comparison star with a Vmag of 13.021 (UCAC4 553-056558) was a bit fainter than the secondary, but since he could still see the sec-ondary with averted vision when the aperture was re-duced to 130mm, he concluded the WDS magnitude of 11.7 was correct. Nanson used the same comparison star and concluded the secondary was just slightly brighter, but also felt the Vmag of 13.021 for the com-parison star was too faint. He estimated the secondary to be of about 12.5 magnitude, which was in line with the difficulty he had in resolving it.

STT 317 (Her): Nanson resolved the B compo-nent at 109x and 152x in the six inch refractor, and con-cluded it was definitely fainter than the WDS magni-tude of 12.0. It appeared to be slightly fainter than a 12.340 magnitude comparison star, suggesting the WDS magnitude is a bit too bright. Knapp resolved B in the 140 mm refractor with averted vision at a magni-fication of 280x, and could still detect it with the aper-ture reduced to 100 mm, which he concluded confirmed the WDS magnitude.

STT 324 (Her): Knapp resolved the secondary in a 185 mm refractor at 100x and could still detect it at 180x with the aperture reduced to 170 mm. Compari-son stars with Vmags of 11.635 and 11.812 appeared to be similar in brightness to the secondary, suggesting it’s slightly fainter than the WDS magnitude of 11.1. Nan-son attempted this pair twice with the six inch refractor, but seeing conditions were too poor each time to allow visual detection.

STT 326 (Oph): Nanson observed this pair once with a 235 mm SCT and resolved the secondary at 136x. It appeared to be similar in magnitude to a com-parison star with a Vmag of 12.660, suggesting the WDS magnitude of 12.4 for B is about right. Knapp observed STT 326 twice, catching a glimpse of it through a thin veil of clouds in the 140mm refractor at 180x, and during the next observation detected it at 40x in the 185 mm refractor, with confirmations at 100x, 180x, and 250x. He could still detect the secondary with averted vision when the aperture was reduced to 110mm, suggesting the secondary is brighter (about 11.8) than the WDS’s 12.4. A comparison star with a Vmag of 13.477 seemed somewhat fainter than the sec-ondary.

STT 328 (Her): Knapp resolved the secondary




at 140x and 200x in the 140 mm refractor, and could still detect it with the aperture reduced to 115 mm, which seems to confirm the WDS magnitude of 10.2. Nanson observed this pair twice with the six inch re-fractor, finding the secondary easier to resolve each

time than would be expected for a pair with a M of 5.4 and a separation of 4.2". No comparison stars were available, but based on both his experience and Knapp’s, it’s possible that either the separation is wider than 4.2" or the magnitude of the secondary is brighter than the WDS’s 10.2

STT 338 (Her): Using a 235 mm SCT at 196x Nanson found C was slightly fainter than a comparison star with a Vmag of 12.951, suggesting it may be a bit brighter than the WDS magnitude of 13.60. Knapp came to the same conclusion using a 185mm refractor at 180x, but found the limit aperture for resolution was 150 mm, which would seem to suggest a magnitude for C of 12.4. A second observation with the same refrac-tor resulted in a limiting aperture of 160 mm, which still suggests C is brighter than the WDS’s 13.60 mag-nitude.

STT 342 (Oph): Knapp was unable to resolve B using 140 mm and 180 mm refractors. C was resolved with the 185 mm refractor at 180x, but was more diffi-cult than expected based on the data. A comparison star with a Vmag of 11.934 was similar in brightness to C, suggesting the WDS magnitude for it of 11.48 is close. However, a limiting aperture for C of 130mm suggests C may be slightly fainter than 11.48. Nanson found B very difficult with a 235 mm SCT, but finally got a glimpse of it at 408x. Further attempts to see it failed, but based on the one observation, it’s likely that B is a bit brighter than the 14.0 magnitude listed for it in the WDS. Using the same comparison star for C that Knapp used, he also found the two to be similar in mag-nitude.

STT 585 (Her): Using a 235 mm SCT and two comparison stars, Nanson found P was obviously brighter than the WDS magnitude of 13.10, perhaps by as much as half a magnitude. Knapp observed P twice, resolving it at 100x in the 185mm refractor on the first observation. Based on a limiting aperture of 170 mm for P, he estimated its magnitude in the 12.5 to 12.6 range. A second observation with the 185 mm refractor resulted in a limiting aperture of 120 mm, again point-ing toward P being brighter than the WDS’s 13.

2.3 Photometry and Astrometry Results Several hundred images taken with iTelescope re-

mote telescopes were in a first step plate solved and stacked with AAVSO VPhot. The stacked images were then plate solved with Astrometrica with UCAC4 refer-ence stars with Vmags in the range 10.5 to 14.5mag.

The RA/Dec coordinates resulting from plate solving were used to calculate Sep and PA using the formula provided by R. Buchheim (2008). Photometry was also performed with Astrometrica based on the Vmags of the UCAC4 reference stars used for plate solving. The results are shown in Table 3.

3. Summary

Tables 4 and 5 below compare the final results of our research with the WDS data that was current at the time we began working on the group of stars in Oph and Her.

In Table 4 the results of our photometry have been averaged for each star. Because we’re aware that both the NOMAD-1 and the UCAC4 catalogs are frequently consulted when making WDS evaluations of magni-tudes changes, the data from those catalogs has also been included for each of the stars.

Red type has been used in Tables 4 and 5 to call attention to significant differences from the WDS data. With regard to Table 4, those magnitudes that differ by two tenths of a magnitude or more from the WDS val-ues have been highlighted. In Table 5 differences in separation in excess of two-tenths of an arc second are highlighted, as are all position angles which differ by more than a degree.

Subsequent to our measures, as a quality check for our astrometry results we turned to the URAT1 catalog for the most recent precise professional measurements available. We used its coordinates to calculate the Sep and PA for all objects in this report for which URAT1 data was available and compared these values with our results, which are shown below in Table 6.

With the exception of STT 585 BP, the Sep results are all within the given error range, so this comparison can be considered as confirmation for the reported re-sults. In the case of STT 585 BP, a rather high rate of proper motion for B (GAIA shows a PM of -219 -255) seems to be the cause of the discrepancy. We calculat-ed a 0.3” shift in position of B between the 2013.735 URAT1 data and the 2015.497 date of our measure.

With regard to the use of URAT1 as a quality check on our astrometry, we contacted Norbert Zacharias at the USNO, who was closely involved in the URAT1 project. He referred us to a paper on which he was lead author which contains this information: "URAT1 can serve as accurate reference star catalog before Gaia data become available. The position accuracy of URAT1 is about 4 times higher than for UCAC4 data at its faint end and the sky density of URAT1 is about 4 times larger than that of UCAC4, similar to the sky density of 2MASS." (Zacharias, 2015, p. 11).




STT 326 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date

2015 N Notes

A 17 18 15.842 09 31 03.51 18.038 0.233 223.934 0.741

8.036 0.120 519 5 iT11 stack 5x1s

B 17 18 14.996 09 30 50.52 12.190 0.127

A 17 18 15.863 09 31 03.35 18.143 0.234 224.004 0.740

7.979 0.110 478 2 iT24 stack 2x1s

B 17 18 15.011 09 30 50.30 12.034 0.113

A 17 18 15.844 09 31 03.33 18.170 0.234 224.182 0.739

7.934 0.110 476 5 iT24 stack 5x1s

B 17 18 14.988 09 30 50.30 11.983 0.114

A 17 18 15.845 09 31 03.49 18.029 0.163 223.766 0.517

8.013 0.060 511 5 iT24 stack 5x1s_2

B 17 18 15.002 09 30 50.47 12.088 0.064

A 17 18 15.849 09 31 03.52 18.099 0.156 223.814 0.492

7.999 0.090 522 5 iT24 stack 5x1s_3

B 17 18 15.002 09 30 50.46 12.039 0.093

A 17 18 15.853 09 31 03.53 18.187 0.276 223.419 0.869

8.074 0.151 516 5 iT24 stack 5x1s_4

B 17 18 15.008 09 30 50.32 12.143 0.155

A 17 18 15.848 09 31 03.57 18.077 0.198 223.880 0.629

7.993 0.080 524 5 iT24 stack 5x1s_5

B 17 18 15.001 09 30 50.54 12.071 0.085

A 17 18 15.849 09 31 03.471 18.106 0.217 223.857 0.688

8.004 0.107 507 32 Summary line

B 17 18 15.001 09 30 50.416 12.078 0.111

STT342 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date

2015 N Notes

A 18 07 20.934 09 33 51.60 24.941 0.270 295.965 0.621

4.658 0.131 519 4

iT24 stack 4x1s.

SNR for B <20 B 18 07 19.418 09 34 02.52 13.780 0.152

A 18 07 20.917 09 33 51.28 24.659 0.212 297.405 0.493

4.707 0.190 524 5

iT24 stack 5x1s.

SNR for B <20 B 18 07 19.437 09 34 02.63 14.003 0.211

A 18 07 20.943 09 33 51.36 25.129 0.184 297.055 0.419

5.021 0.140 511 5

iT24 stack

5x1s_2. SNR for B

<20 B 18 07 19.430 09 34 02.79 13.864 0.154

A 18 07 20.932 09 33 50.90 25.397 0.234 298.427 0.529

4.569 0.120 628 5 iT24 stack 5x3s

B 18 07 19.422 09 34 02.99 13.868 0.130

A 18 07 20.930 09 33 50.57 25.326 0.213 298.411 0.481

4.969 0.120 628 5 iT24 stack 5x6s

B 18 07 19.424 09 34 02.62 13.903 0.126

A 18 07 20.918 09 33 50.75 25.249 0.198 298.299 0.449

5.054 0.120 628 5 iT24 stack 5x9s

B 18 07 19.415 09 34 02.72 13.799 0.124

A 18 07 20.916 09 33 51.54 24.698 0.191 297.358 0.443

4.060 0.140 522 6

iT24 stack 6x1s.

SNR for B <20 B 18 07 19.433 09 34 02.89 13.822 0.157

A 18 07 20.927 09 33 51.143 25.055 0.216 297.565 0.495

4.720 0.139 566 35

SNR for B in some

images <20. A too

bright for relia-

ble photometry B 18 7 19.426 09 34 02.737 13.863 0.153

Table 3: Photometry and astrometry results for the selected STT objects in Oph and Her. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. Sep is separation calculated as SQRT(((RA2-RA1)*cos(Dec1))^2+(Dec2-Dec1)^2) in radians. Err_Sep is calculated as SQRT(dRA^2+dSep^2) with dRA and dDec as average RA and Dec plate solving errors. PA is calculated as arctan((RA2-RA1)*cos(Dec1))/(Dec2-Dec1)) in radi-ans depending on quadrant and Err_PA is the error estimation for PA calculated as arctan(Err_Sep/Sep) in degrees assum-ing the worst case that Err_Sep points in the right angle to the direction of the separation means perpendicular to the sepa-ration vector. Mag is the photometry result based on UCAC4 reference stars with Vmags between 10.5 and 14.5mag. Err_Mag is calculated as square root of (dVmag^2 + (2.5*Log10(1+1/SNR))^2) with dVmag as the average Vmag error over all used reference stars and SNR is the signal to noise ratio for the given star. Date is the Bessel epoch in 2015 and N is the number of images (usually with 1s exposure time) used for the reported values. iT in the Notes column indicates the tele-scope used with number of images and exposure time given. The average results over all used images are given in the line below the individual stacks in red and bold. The error esti-mation over all used images is calculated as root mean square over the individual Err values. The N column in the summary line gives the total number of images used and Date the average Bessel epoch.





2015 N Notes

A 16 25 25.445 37 54 36.33 2.936 0.150 222.629 2.925

8.230 0.080 467 5 iT24 stack 5x1s

B 16 25 25.277 37 54 34.17 11.123 0.085

A 16 25 25.445 37 54 36.31 3.064 0.184 221.634 3.444

8.215 0.070 522 5

iT24 stack

5x1s_2 B 16 25 25.273 37 54 34.02 11.081 0.074

A 16 25 25.446 37 54 36.22 3.432 0.184 222.257 3.066

8.209 0.080 516 5

iT24 stack

5x1s_3 B 16 25 25.251 37 54 33.68 11.325 0.084

A 16 25 25.445 37 54 36.37 3.209 0.163 221.869 2.904

8.209 0.070 525 5

iT24 stack

5x1s_4 B 16 25 25.264 37 54 33.98 11.066 0.073

A 16 25 25.445 37 54 36.307 3.160 0.171 222.094 3.095

8.216 0.075 507 20

Touching/

overlapping star

disks B 16 25 25.266 37 54 33.962 11.149 0.079


2015 N Notes

A 16 38 51.508 20 27 57.45 3.576 0.277 235.218 4.423

8.313 0.100 472 5 iT11 stack 5x1s

B 16 38 51.299 20 27 55.41 11.139 0.104

A 16 38 51.497 20 27 57.43 3.639 0.213 234.950 3.343

8.278 0.100 521 5 iT18 stack 5x1s

B 16 38 51.285 20 27 55.34 11.301 0.109

A 16 38 51.492 20 27 57.64 3.729 0.198 232.311 3.039

8.123 0.100 470 5 iT21 stack 5x1s

B 16 38 51.282 20 27 55.36 11.110 0.111

A 16 38 51.492 20 27 57.29 3.557 0.170 232.202 2.732

8.223 0.070 473 5 iT24 stack 5x1s

B 16 38 51.292 20 27 55.11 11.278 0.073

A 16 38 51.497 20 27 57.35 3.393 0.194 228.915 3.275

8.236 0.070 478 5 iT24 stack 5x1s_2

B 16 38 51.315 20 27 55.12 10.979 0.075

A 16 38 51.494 20 27 57.35 3.740 0.261 231.068 3.989

8.234 0.061 476 5 iT24 stack 5x1s_3

B 16 38 51.287 20 27 55.00 11.019 0.070

A 16 38 51.499 20 27 57.28 3.720 0.172 229.412 2.648

8.206 0.070 524 5 iT24 stack 5x1s_4

B 16 38 51.298 20 27 54.86 11.254 0.073

A 16 38 51.495 20 27 57.05 3.530 0.248 235.094 4.012

8.280 0.100 516 5 iT24 stack 5x1s_5

B 16 38 51.289 20 27 55.03 11.430 0.111

A 16 38 51.499 20 27 57.28 3.720 0.172 229.412 2.648

8.206 0.070 524 5 iT24 stack 5x1s_6

B 16 38 51.298 20 27 54.86 11.254 0.073

A 16 38 51.497 20 27 57.347 3.619 0.215 232.056 3.399

8.233 0.084 495 45 Summary line

B 16 38 51.294 20 27 55.121 11.196 0.091

Table 3 (continued). Photometry and astrometry results for the selected STT objects in Oph and Her. RA and Dec are the co-ordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. ...






STT 317 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes

A 16 52 57.208 44 24 09.33 24.713 0.355 199.744 0.823

7.900 0.070 530 4

iT21 stack 4x1s.

SNR B<20 B 16 52 56.429 44 23 46.07 12.677 0.103

A 16 52 57.196 44 24 09.67 24.808 0.141 200.349 0.327

8.030 0.070 476 3 iT24 stack 3x1s

B 16 52 56.391 44 23 46.41 12.517 0.078

A 16 52 57.187 44 24 09.81 24.852 0.178 200.154 0.410

7.757 0.060 467 5 iT24 stack 5x1s

B 16 52 56.388 44 23 46.48 12.471 0.068

A 16 52 57.189 44 24 09.83 24.925 0.164 200.276 0.377

7.822 0.050 473 5

iT24 stack

5x1s_2 B 16 52 56.383 44 23 46.45 12.472 0.057

A 16 52 57.200 44 24 09.60 24.760 0.149 200.444 0.344

7.769 0.070 511 5

iT24 stack

5x1s_3 B 16 52 56.393 44 23 46.40 12.499 0.076

A 16 52 57.195 44 24 09.60 24.713 0.163 200.485 0.377

7.850 0.060 522 5

iT24 stack

5x1s_4 B 16 52 56.388 44 23 46.45 12.501 0.067

A 16 52 57.194 44 24 09.63 24.741 0.163 200.460 0.377

7.852 0.080 516 5

iT24 stack

5x1s_5 B 16 52 56.387 44 23 46.45 12.484 0.087

A 16 52 57.196 44 24 09.639 24.787 0.200 200.273 0.462

7.854 0.066 499 32 Summary line

B 16 52 56.394 44 23 46.387 12.517 0.078


A 17 08 00.683 31 12 22.06 2.974 0.191 218.411 3.676

6.098 0.070 473 5

iT24 stack 5x1s.

Overlapping star

disks. SNR for

B<20 B 17 08 00.539 31 12 19.73 10.530 0.095

A 17 08 00.682 31 12 22.08 3.550 0.212 221.957 3.420

6.039 0.070 473 5

iT24 stack

5x1s_2. Overlap-

ping star disks.

SNR for B<20 B 17 08 00.497 31 12 19.44 10.883 0.095

A 17 08 00.691 31 12 21.72 3.669 0.177 227.256 2.761

5.953 0.090 478 5

iT24 stack

5x1s_3. Overlap-

ping star disks B 17 08 00.481 31 12 19.23 10.657 0.102

A 17 08 00.678 31 12 21.98 3.676 0.205 219.173 3.195

5.820 0.090 476 5

iT24 stack

5x1s_4. Overlap-

ping star disks B 17 08 00.497 31 12 19.13 10.039 0.102

A 17 08 00.685 31 12 22.11 3.786 0.200 218.081 3.024

6.130 0.080 511 5

iT24 stack

5x1s_5. Overlap-

ping star disks B 17 08 00.503 31 12 19.13 11.197 0.094

A 17 08 00.670 31 12 22.41 3.084 0.212 205.639 3.935

5.801 0.120 516 5

iT24 stack

5x1s_6. Overlap-

ping star disks B 17 08 00.566 31 12 19.63 10.180 0.127

A 17 08 00.683 31 12 22.21 3.612 0.184 217.395 2.922

6.076 0.080 525 5

iT24 stack

5x1s_7. Overlap-

ping star disks B 17 08 00.512 31 12 19.34 10.980 0.090

A 17 08 00.683 31 12 22.21 4.196 0.184 218.366 2.516

6.085 0.080 525 5

iT24 stack

5x1s_8. Overlap-

ping star disks B 17 08 00.480 31 12 18.92 11.523 0.089

A 17 08 00.682 31 12 22.097 3.552 0.196 218.535 3.161

6.000 0.086 497 40 Summary line

B 17 08 00.509 31 12 19.319 10.749 0.100





STF2127 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes

A 17 07 04.412 31 05 34.78 15.127 0.191 280.475 0.724

8.423 0.070 473 5 iT24 stack 5x1s

B 17 07 03.254 31 05 37.53 11.555 0.072

A 17 07 04.417 31 05 34.74 15.163 0.212 280.411 0.802

8.404 0.070 473 5

iT24 stack

5x1s_2 B 17 07 03.256 31 05 37.48 11.569 0.072

A 17 07 04.424 31 05 34.47 15.301 0.177 281.574 0.662

8.356 0.090 478 5

iT24 stack

5x1s_3 B 17 07 03.257 31 05 37.54 11.615 0.092

A 17 07 04.407 31 05 34.56 15.056 0.205 281.144 0.781

8.217 0.090 476 5

iT24 stack

5x1s_4 B 17 07 03.257 31 05 37.47 11.669 0.094

A 17 07 04.420 31 05 34.81 15.213 0.200 280.376 0.753

8.453 0.080 511 5

iT24 stack

5x1s_5 B 17 07 03.255 31 05 37.55 11.528 0.082

A 17 07 04.403 31 05 35.10 14.955 0.212 279.585 0.813

8.186 0.120 516 5

iT24 stack

5x1s_6 B 17 07 03.255 31 05 37.59 11.521 0.122

A 17 07 04.409 31 05 34.86 15.148 0.184 280.113 0.697

8.424 0.080 525 5

iT24 stack

5x1s_7 B 17 07 03.248 31 05 37.52 11.528 0.082

A 17 07 04.413 31 05 34.760 15.137 0.198 280.528 0.749

8.352 0.087 493 35 Summary line

B 17 07 03.255 31 05 37.526 11.569 0.089


A 17 17 19.563 33 06 00.05 4.549 0.184 57.708 2.321

4.808 0.070 470 4

iT24 stack 4x1s.

Overlapping star

disks. SNR for

B<20 B 17 17 19.869 33 06 02.48 10.328 0.112

A 17 17 19.559 33 06 00.36 4.694 0.219 61.082 2.675

4.848 0.080 473 5

iT24 stack 5x1s.

Overlapping star

disks, SNR for

B<20 B 17 17 19.886 33 06 02.63 10.461 0.117

A 17 17 19.565 33 06 00.38 4.533 0.214 57.730 2.703

4.837 0.080 478 5

iT24 stack

5x1s_2. Overlap-

ping star disks,

SNR for B<20 B 17 17 19.870 33 06 02.80 10.147 0.122

A 17 17 19.556 33 06 00.46 4.326 0.198 60.960 2.627

4.096 0.080 516 5

iT24 stack

5x1s_3. Overlap-

ping star disks,

SNR for B<20 B 17 17 19.857 33 06 02.56 10.118 0.097

A 17 17 19.563 33 06 00.42 4.508 0.163 59.469 2.068

4.810 0.080 522 5

iT24 stack

5x1s_4. Overlap-

ping star disks,

SNR for B<20 B 17 17 19.872 33 06 02.71 10.301 0.109

A 17 17 19.561 33 06 00.334 4.520 0.197 59.386 2.494

4.680 0.078 492 24 Summary line

B 17 17 19.871 33 06 02.636 10.271 0.112





STT338 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes

AB 17 51 58.466 15 19 35.28 32.525 0.250 202.077 0.440

6.363 0.150 472 5

iT11 stack 5x1s.

SNR for B<20 C 17 51 57.621 15 19 05.14 13.239 0.169

AB 17 51 58.470 15 19 34.96 32.617 0.262 202.148 0.460

6.309 0.090 521 4

iT18 stack 4x1s.

SNR for C<10 C 17 51 57.620 15 19 04.75 13.157 0.143

AB 17 51 58.461 15 19 34.91 32.648 0.184 202.236 0.323

5.985 0.140 470 5

iT21 stack 5x1s.

SNR for C<20 C 17 51 57.607 15 19 04.69 13.033 0.167

AB 17 51 58.461 15 19 35.15 32.789 0.191 202.053 0.334

6.091 0.080 473 5 iT24 stack 5x1s

C 17 51 57.610 15 19 04.76 13.022 0.088

AB 17 51 58.453 15 19 35.22 32.649 0.227 201.961 0.398

6.062 0.080 467 5

iT24 stack

5x1s_2 C 17 51 57.609 15 19 04.94 13.041 0.089

AB 17 51 58.451 15 19 35.02 32.270 0.226 202.094 0.402

6.005 0.080 478 5

iT24 stack

5x1s_3 C 17 51 57.612 15 19 05.12 12.988 0.089

AB 17 51 58.458 15 19 35.24 32.660 0.191 202.008 0.335

6.215 0.070 511 5

iT24 stack

5x1s_4 C 17 51 57.612 15 19 04.96 13.124 0.079

AB 17 51 58.449 15 19 35.30 32.885 0.226 201.388 0.394

6.101 0.090 516 5

iT24 stack

5x1s_5 C 17 51 57.620 15 19 04.68 13.176 0.099

AB 17 51 58.448 15 19 35.34 32.726 0.212 202.015 0.371

6.073 0.080 522 5

iT24 stack

5x1s_6 C 17 51 57.600 15 19 05.00 13.037 0.089

AB 17 51 58.457 15 19 35.158 32.641 0.220 201.997 0.387

6.134 0.099 492 44 Summary line

C 17 51 57.612 15 19 04.893 13.091 0.117

STT338 RA Dec Sep Err Sep PA Err PA Mag Err Mag Date N Notes

AB 17 51 58.466 15 19 35.28 96.303 0.250 246.786 0.149

6.363 0.150 472 5 iT11 stack 5x1s

D 17 51 52.348 15 18 57.32 11.834 0.154

AB 17 51 58.470 15 19 34.96 96.338 0.262 246.846 0.156

6.309 0.090 521 4 iT18 stack 4x1s

D 17 51 52.347 15 18 57.08 11.819 0.104

AB 17 51 58.461 15 19 34.91 96.291 0.184 246.847 0.109

5.985 0.140 530 5 iT21 stack 5x1s

D 17 51 52.341 15 18 57.05 11.110 0.148

AB 17 51 58.461 15 19 35.15 96.367 0.191 246.828 0.114

6.091 0.080 473 5 iT24 stack 5x1s

D 17 51 52.337 15 18 57.23 11.666 0.082

AB 17 51 58.453 15 19 35.22 96.288 0.227 246.762 0.135

6.062 0.080 467 5

iT24 stack

5x1s_2 D 17 51 52.337 15 18 57.23 11.650 0.082

AB 17 51 58.451 15 19 35.02 96.251 0.226 246.837 0.135

6.005 0.080 478 5

iT24 stack

5x1s_3 D 17 51 52.334 15 18 57.16 11.019 0.087

AB 17 51 58.458 15 19 35.24 96.328 0.191 246.773 0.114

6.215 0.070 511 5

iT24 stack

5x1s_4 D 17 51 52.339 15 18 57.25 11.660 0.072

AB 17 51 58.449 15 19 35.30 96.131 0.226 246.631 0.135

6.101 0.090 516 5

iT24 stack

5x1s_5 D 17 51 52.349 15 18 57.17 11.734 0.092

AB 17 51 58.448 15 19 35.34 96.329 0.212 246.728 0.126

6.073 0.080 522 5

iT24 stack

5x1s_6 D 17 51 52.331 15 18 57.28 11.633 0.082

AB 17 51 58.457 15 19 35.158 96.292 0.220 246.782 0.131

6.134 0.099 499 44 Summary line

D 17 51 52.34 15 18 57.197 11.569 0.104



Table 3 (conclusion). Photometry and astrometry results for the selected STT objects in Oph and Her. RA and Dec are the coordinates based on plate solving with UCAC4 reference stars in the 10.5 to 14.5mag range. ...


B 16 44 57.753 06 02 33.08 89.669 0.255 5.202 0.163

10.369 0.092 472 5

iT11 stack 5x1s.

SNR for P<20 P 16 44 58.298 06 04 02.38 12.940 0.113

B 16 44 57.734 06 02 33.16 89.754 0.228 5.092 0.146

10.321 0.113 515 2

iT18 stack 5x1s.

SNR for P<10 P 16 44 58.268 06 04 02.56 13.125 0.169

B 16 44 57.726 06 02 33.22 89.801 0.333 5.414 0.212

9.887 0.161 515 9

iT21 stack 5x1s.

SNR for P<20 P 16 44 58.294 06 04 02.62 12.544 0.174

B 16 44 57.733 06 02 33.14 89.624 0.177 5.233 0.113

10.272 0.160 473 5 iT24 stack 5x1s

P 16 44 58.281 06 04 02.39 12.742 0.163

B 16 44 57.731 06 02 33.19 89.640 0.205 5.280 0.131

10.259 0.081 467 5

iT24 stack

5x1s_2 P 16 44 58.284 06 04 02.45 12.783 0.086

B 16 44 57.735 06 02 33.24 89.565 0.177 5.246 0.113

10.263 0.071 476 5

iT24 stack

5x1s_3 P 16 44 58.284 06 04 02.43 12.749 0.081

B 16 44 57.733 06 02 33.11 89.666 0.205 5.250 0.131

10.275 0.071 511 5

iT24 stack

5x1s_4 P 16 44 58.283 06 04 02.40 12.763 0.076

B 16 44 57.741 06 02 32.98 89.615 0.248 5.243 0.159

10.326 0.121 516 5

iT24 stack

5x1s_5 P 16 44 58.290 06 04 02.22 12.876 0.126

B 16 44 57.736 06 02 33.10 89.929 0.227 5.263 0.144

10.303 0.120 524 5

iT24 stack

5x1s_6 P 16 44 58.289 06 04 02.65 12.838 0.125

B 16 44 57.736 06 02 33.136 89.696 0.233 5.247 0.149

10.253 0.115 497 46 Summary line

P 16 44 58.286 06 04 02.456 12.818 0.129

Specifications of the used telescopes:

iT11: 510mm CDK with 2280mm focal length. CCD: FLI ProLine PL11002M. Resolution 0.81 arcsec/pixel. B- and V-Filter. Transformation coefficients B-V available. Located in Mayhill, New Mexico. Elevation 2225m

iT18: 318mm CDK with 2541mm focal length. CCD: SBIG-STXL-6303E. Resolution 0.73 arcsec/pixel. V-filter. No transformation coefficients available. Located in Nerpio, Spain. Elevation 1650m

iT21: 431mm CDK with 1940mm focal length. CCD: FLI-PL6303E. Resolution 0.96 arcsec/pixel. V-filter. Transfor-mation coefficients V-R available, but not used. Located in Mayhill, New Mexico. Elevation 2225m

iT24: 610mm CDK with 3962mm focal length. CCD: FLI-PL09000. Resolution 0.62 arcsec/pixel. V-filter. No transfor-mation coefficients available. Located in Auberry, California. Elevation 1405m



Table 4. Photometry and Visual Results Compared to WDS

WDS

Mag

NOMAD-1

VMag

UCAC4

VMa

UCAC4

f. mag

Average of

Photometry

Measures

Results of Visual Observations

STT 326 B 12.40 12.060 - 12.307 12.078

Three observations: one concluded B was slightly

brighter, one that it was close to the WDS value,

and one that it was fainter.

STT 342 B 14.00 - - 13.711 13.863 One observation of B found it was slightly

brighter than the WDS value.

STT 310 B 11.00 - - - 11.149

Two observations: one found B slightly brighter,

one estimated it to be slightly fainter than the

WDS value.

STT 314 B 11.70 - - - 11.196 Two observations: one found the WDS magnitude to

be about right, one estimated B at 12.5.

STT 317 B 12.00 12.220 - 12.475 12.517

Two observations: one found the WDS magnitude to

be about right, the other concluded B was a bit

fainter than the WDS value.

STT 324 B 11.10 - - - 10.749 One observation suggested B was slightly fainter

than the WDS magnitude.

STF 2127 B 12.30 11.030 - 11.342 11.569 No visual observations made.

STT 328 B 10.20 - - - 10.271

One observation tended to confirm the WDS magni-

tude; the other felt B was either brighter than

the WDS magnitude or the separation was slightly

wider than the WDS value.

STT 338 C 13.60 13.80 - 12.746 13.091 Three observations indicated C was brighter than

the WDS value.

STT 338 D 10.60 11.950 11.671 11.289 11.569 No visual estimates made.

STT 585 P 13.10 11.960 12.799 12.812 12.818 Three observations, all indicating P was brighter

than the WDS magnitude.

WDS Coordinates WDS Sep WDS PA Astrometry

Coordinates

Astrometry

Sep Astrometry PA

STT 326 AB 17 18 15.81

+09 31 03.9 17.90" 223°

17 18 15.849

+09 31 03.471 18.106" 223.857°

STT 342 AB 18 07 21.02

+09 33 49.2 24.90" 298°

18 07 20.927

+09 33 51.143 25.055" 297.565°

STT 310 AB 16 25 25.46

+37 54 36.8 3.00" 226°

16 25 25.445

+37 54 36.307 3.160" 222.094°

STT 314 AB 16 38 51.50

+20 27 57.6 3.80" 234°

16 38 51.497

+20 27 57.347 3.619" 232.056°

STT 317 AB 16 52 57.22

+44 24 08.0 24.80" 200°

16 52 57.196

+44 24 09.639 24.787" 200.273°

STT 324 AB 17 08 00.70

+31 12 22.5 3.50" 220°

17 08 00.682

+31 12 22.097 3.552" 218.535°

STF 2127 AB 17 07 04.42

+31 05 35.1 14.80" 276°

17 07 04.413

+31 05 34.760 15.137" 280.528°

STT 328 AB 17 17 19.57

+33 06 00.4 4.20" 59°

17 17 19.561

+33 06 00.334 4.520" 59.386°

STT 338 AB-C 17 51 58.46

+15 19 34.9 32.80" 201°

17 51 58.457

+15 19 35.158 32.641" 201.997°

STT 338 AB-D 17 51 58.46

+15 19 34.9 95.60" 247°

17 51 58.457

+15 19 35.158 96.292" 246.782°

STT 585 BP** 16 44 57.96

+06 02 37.1 85.90" 3°

16 44 57.736

+06 02 33.136 89.696" 5.247°

Table 5. Astrometry Results Compared to WDS

** At the time we first pulled data from the WDS for STT 585 BP, it listed the 2001 (most recent) separation as 77.40”. However, a look at the text file for that pair of stars showed a separation of 85.858” for the 2001 measure. That error is now corrected in the current WDS listing of STT 585 BP.



References


Burnham, S.W. – 1906, A General Catalogue of Dou-ble Stars Within 120° of the North Pole, Part II. University of Chicago Press, Chicago

Greaney, Michael – 2012, "Some Useful Formulae" in R.W. Argyle, Observing and Measuring Visual Double Stars, 2nd Edition 2012, Chapter 25, Page 359

Hussey, W.J. – 1901, Micrometrical Observations of the Double Stars Discovered at Pulkowa Made with the Thirty-Six-Inch and Twelve-Inch Refractors of Lick Observatory, pp. 14-16. A.J. Johnston, Sacra-mento

Knapp, Wilfried; Nanson, John; Smith, Steven – 2015, STT Doubles with Large Delta_M – Part I: Gem, Journal of Double Star Observing, Vol. 11 No. 4 pp. 390-401.

Knapp, Wilfried; Nanson, John; Smith, Steven – 2016, STT Doubles with Large Delta_M – Part II: Leo and UMa, Journal of Double Star Observing, Vol. 12 No 2 pp. 110-126.

Knapp, Wilfried; Nanson, John – 2015, STT Doubles with Large Delta_M – Part III: Vir, Ser, CrB, Com and Boo, Journal of Double Star Observing, Vol. 12 No 2 pp. 127-141.

Zacharias, Norbert, et al – 2015, The First U.S. Naval Observatory Robotic Astrometric Telescope Cata-log (URAT1), The Astronomical Journal, Vol 150 , Issue 4 (August 19, 2015), pp. 1-12.

Acknowledgements

Our thanks to Bill Hartkopf at the USNO/WDS for his enthusiastic aid and advice.


Washington Double Star Catalog iTelescope

AAVSO VPhot AAVSO APASS UCAC4 catalog via the University of Heidelberg

website and directly from USNO DVD

Aladin Sky Atlas v8.0 SIMBAD, VizieR 2MASS All Sky Catalog URAT1 Survey

AstroPlanner v2.2 MaxIm DL6 v6.08 Astrometrica v4.8.2.405


Table 6. Astrometry Results Compared with URAT1 Coordinates

Object URAT1 Sep

iTelescope Sep

Err Sep

Within

Error

Range?

URAT1 PA iTelescope

PA Err PA

Within

Error

Range?

STT 326 AB 18.031" 18.106" 0.217 Yes 223.648° 223.857° 0.688 Yes

STT 342 AB 25.040" 25.055" 0.216 Yes 297.562° 297.565° 0.495 Yes

STT 317 AB 24.710" 24.787" 0.200 Yes 200.574° 200.273° 0.462 Yes

STF 2127 AB 15.219" 15.137" 0.198 Yes 280.579° 280.528° 0.749 Yes

STT 338 AB-C 32.588" 32.641" 0.220 Yes 202.149° 201.997° 0.387 Yes

STT 338 AB-D 96.349" 96.292° 0.220 Yes 246.862° 246.782° 0.131 Yes

STT 585 BP 89.254" 89.696° 0.233 No 5.033° 5.247° 0.149 No


Introduction

A new group of double stars observers has been informally founded as a part of the Polish Astronomy Amateur Association, division Szczecin. None of the observers had previous experience in double star as-tronomy, so it was clearly an educational program to learn how to use a reticle micrometer eyepiece and to spark an interest in double stars in general. The purpose was also to learn the basics before taking the next steps in the vast field of double star astronomy.

The program was based on the observing list gener-ated by Brian Mason from the USNO, previously re-quested by the first author. The list contained 54 stars with the following specifications:

RA: from 13h to 18h DEC: from 15o to 60 o Magnitudes: > 10 mag, no lower limit Separation: from 10'' to 80'' Last observation: 2005

The limits were mainly determined by the observa-

tory location close to the city center where the measure-ments were carried out. The telescope used was the Zeiss Coude-Refractor 150/2250 from the year 1980.

Method

Calibration was performed via the drift method and

led to value 9.253’’ for one division at the linear scale of the Celestron Micrometer Eyepiece. Measurements were carried out in two to five person groups at the time, with an exception of 1 night when only 1 person ran observations. Each person's position angle and sep-aration results were noted and averaged. Ten out of 20 observed stars was measured during two or more nights. In those cases Bessellian dates were averaged. For each system, the measurement errors were calculat-ed as a standard deviation of all results.

Results

Nineteen double stars were measured from May to September 2015, giving a total of 245 single observa-tions. The vast spread of errors is due to a few factors like poor telescope drive and lack of experience for the program participants. Table 1 gives the measurements and uncertainties.

Acknowledgements

Special thanks to people who made this program possible - Bob Argyle and Bruce MacEvoy for basic knowledge and patiently showing directions, also Brian Mason for great help with the observing list.

The authors are all amateur astronomers with a spe-cial interest in double stars and photometry. All partici-pants of the described program are members of the As-tronomy Amateur Association, Szczecin Division .

Measurements with Reticle Micrometer Performed by a New Double Stars Observing Group from Poland

Marcin Biskupski, Natalia Banacka, Justyna Cupryjak, Małgorzata Malinowska, Kamil Bujel, Zdzisław Kołtek, Jarosław Mazur, Marcin Muskała, Łukasz Płotkowski,

Barłomiej Prowans, and Paweł Szkaplewicz

Polish Astronomy Amateur Association Szczecin Divison, Poland

Email: [email protected]

Abstract: Measurements of 19 double stars using a reticle micrometer eyepiece are re-ported. The observational program was held in spring and summer of 2015 as an extended workshop for a new double stars observing group from Szczecin, Poland. The goal of the pro-gram was to learn how to measure position angle and separation using a reticle micrometer eye-piece.


Measurements with Reticle Micrometer Performed by a New Double Stars Observing Group from Poland

disc wds mags PA err SEP err date

HZG 8AC 11045+3814 6.04, 7.56 83.75 0.76 150.64 0.77 2015.368

HJL1062 11202+1707 7.92, 9.13 187 0 103.63 0 2015.390

HJL1065AC 11390+4109 8.11, 9.18 3.63 0.29 132.32 2.37 2015.553

ARG 101 11512+3322 6.27, 9.28 273.75 0.5 46.08 0.77 2015.390

STTA112AB 11545+1925 8.28, 8.49 36.75 0.35 73.79 0.33 2015.384

STFA 25AC 13135+6717 6.64, 8.89 223.38 0.18 105.02 1.31 2015.550

HJ 1231AC 13253+4028 8.67, 8.85 233.25 1.06 92.53 0 2015.550

STF1831AC 14161+5643 7.16, 6.73 221.69 0.74 112.19 0.33 2015.381

STF1830CE 14161+5643 6.73, 9.33 246.67 0.58 139.03 0.89 2015.384

ARY 42 15174+3022 9.3, 9.63 188.33 0.58 92.76 1.58 2015.409

STTA138BC 15201+6023 7.76, 9.28 48.81 0.49 91.6 0.59 2015.550

BAR 41CD 15520+4238 7.8, 9.7 51.5 0.58 66.62 0.76 2015.409

ARY 12 15599+6914 8.9, 8.95 248.38 0.48 124.22 0.89 2015.384

STFA 30BC 16362+5255 6.42, 5.5 16.86 0.43 91.47 0.4 2015.396

BU 953AB,D 16366+6948 8.04, 8.03 46.39 0.47 147.96 1.05 2015.507

POP1222AD 16448+3544 9.37, 8.91 7 0.61 158.5 0.41 2015.444

STTA151AB 17039+5314 7.93, 9.34 171.4 0.67 88.42 1 2015.537

S 689AB 17246+3913 7.48, 8.44 198.15 0.84 91.19 0.58 2015.529

STTA157AB 17407+3117 6.43, 7.92 106.2 0.69 118.28 0.83 2015.537

Table 1. Measurements of the Double Stars


The Observing Program

From October 23 to December 1, 2015, a vigorous program of measuring double stars with a Skyris 618C CCD camera was done at Brilliant Sky Observatory (Cave Creek, Arizona). Over 18 different nights, over 220 double stars were imaged and their FITS cubes re-duced using Plate Solve 3.47B. In this report, I describe the measurements of 66 pairs that are known rectilinear systems or showing signs of being such. These stars were chosen for two reasons: (1) to check the accuracy of my measurements, and (b) to add data to the valida-tion (or correction) of the ephemerides in the Fourth Catalog of Rectilinear Elements (Hartkopf, Mason, Oc-tober 2015).

Equipment Used

Brilliant Sky Observatory (so-named for the street on which it is located) is a roll-off roof structure that houses a Celestron C-11 SCT telescope mounted on a Celestron CGEM-DX GoTo mount controlled by a lap-top using TheSky 6.0. To keep the focal length as con-sistent as possible, a JMI digital motorized focus con-trol moves the primary mirror in extremely tiny incre-ments to bring star images to a sharp focus. The differ-ence in the readout spans about 20 counts between win-ter and summer (due to thermal expansion and contrac-tion of the entire optical train). Since a complete turn of the focus knob causes a change of 100 counts on the JMI digital readout, this corresponds to a mirror shift of approximately 0.16 mm, an insignificant effect on the system’s overall focal length, which in turn assures that the camera pixel scale remains constant for each ob-

serving session at a given focal ratio. The camera was calibrated as described in Harshaw (2015).

The Skyris 618C, being a color camera, is run in black and white mode using FireCapture software. FITS frames are sent to a 2 TB external USB hard drive and later compiled into FITS cubes and reduced with Plate Solve 3.47B software.

Plate Solve 3.47B was written by David Rowe of PlaneWave Instruments. Mr. Rowe is an ardent sup-porter of astronomers doing speckle interferometry and high-resolution CCD imaging of double stars. Plate Solve 3.47B has a number of powerful features and is still in development and not yet ready for general re-lease. The observer can calibrate the camera’s angle (orientation with respect to celestial north) with “drift” files of a bright stars. By capturing “drift” files of a ref-erence star (a bright star where one can use camera in-tegration times of 20ms or less, thus generating a large number of frames for the short transit across the cam-era’s chip), Plate Solve can compute the RMS line-of-best-fit of the star’s image and then accurately deter-mine celestial north (to within a tenth of a degree). I run ten drift files per observing run to drive down the stand-ard errors to an acceptable level.

Plate Solve also can use the same data in the drift file to compute the camera’s pixel scale, but I find that it takes many dozens of drifts to drive the standard error down to an acceptable level. This new feature is a great addition and makes the grating calibration method de-scribed by the author (Harshaw, 2015) and Cotterell (2015) unnecessary, thus saving an observer the ex-pense of making a grating and procuring an H Alpha filter.

CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs:The Autumn 2015 Observing Program at

Brilliant Sky Observatory, Part 1

Richard W. Harshaw Brilliant Sky Observatory, Cave Creek, AZ

[email protected]

Abstract: A set of 66 stars with known rectilinear solutions was observed with a CCD camera at f/30— 22 known rectilinear pairs, 18 strongly linear pairs and 26 possible linear pairs. Data reduction showed that all but one of the 22 rectilinear measurements fell within the estimated positions of the ephemerides as reported in the Fourth Catalog of Rectilinear Elements. The lone exception was only 0.040 arc seconds off the predicted value of rho. The other 44 cases show varying degrees of linearity, some probably being at the point of deriving a rectilinear solution.


CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs ...

In addition to that, Plate Solve can also compile the FITS images made at the telescope into FITS cubes, and then pre-process those cubes to reduce file size and greatly reduce processing time during reduction.

Procedure

For CCD measures, I find that taking 100 frames and then selecting the best 25% for signal to noise ratio yields 25 frames that Plate Solve can work with very nicely. I find that as a general rule, Plate Solve gives more accurate solutions than lucky imaging.

When measuring the autocorrelograms with Plate Solve, I take advantage of the fact that an autocorrelo-gram produces an image with axial symmetry. The au-tocorrelogram is not technically an “image” of the pair, but is instead a graphical representation of the pair’s power spectrum, a process covered in detail in the Plate Solve User’s Guide (Rowe, Genet, 2013; PDF copy available upon request). As such, one of the “images” of the companion star will be the true one (at the proper value of theta and rho) while the other will be its mirror image (same rho, 180° complement of theta). I always measure both companion “images” when doing reduc-tion. In a high-quality FITS cube, both measurements will be identical, of course (with the exception of the quadrant flip for the complementary image); in cubes of lesser quality, there may be very small differences in the two measurements. These are reported in the tables as two measurements, although only one FITS cube is being analyzed.

Figure 1 shows a noisy image—the integration time had to be run up to 1.05 seconds due to the faintness of

the stars (10.03 and 10.44 magnitudes respectively). Figure 2 shows the same image after processing to re-move noise. Note the small pink circle Plate Solve drew on the companion “image” at the 7 0’clock position. This indicates that Plate Solve thinks this is the com-panion star to be measured. (As it turns out in this case, this is in fact the location of the companion, the “image” at 1 o’clock being the complement produced by the symmetric solution of the Fourier transform.)

Plate Solve has a tool that allows the user to re-move the pink circle and manually select the other “image” to perform a measurement of the complement (or, in many cases, the actual companion as Plate Solve does not always correctly select the companion star since it does not have the measurement history availa-ble to it).

The largeness of the stars’ “images” is an indication of the usually poor seeing in Arizona. (Most nights while collecting data, the stars were forming images approximately 2 arc seconds across. Such is the price one pays for strong thermals rising off the desert floor. But the dry air also makes for exceptional transparency, which is why Arizona figures so prominently as the Continental United States’ premier observing location for deep sky objects.) Since fainter stars require longer integration times (or “shutter speeds”) in the camera, the roiling of the atmosphere produces a smudged out image.

Results Part 1: 22 Rectilinear Pairs Observed

In Table 1, I present the results of the measures of 22 pairs with known rectilinear solutions. In this table,

Figure 1. Unprocessed autocorrelogram of SMA 30.

Figure 2: SMA 30 after enhancement using Plate Solve 3.47B’s tools.



Notes:

1. The parallax for A is given as 5.64 mas (±1.42), while B shows 34.52 mas (±30.8). Clearly the parallax for B is meaningless. The uncertainty in the parallax of A (25.18%) makes it a poor guide to the star’s actual dis-tance, but the star could be 177 parsecs away. If at that distance, the minimum mean distance between the two stars would be 2,307 AU.

2. The parallaxes of this system are close (4.03 mas ±1.13 for A, 3.92 mas ±2.69 for B), yet the error esti-mates make these values virtually unusable as true distance indicators. Having said that, there is a likely chance that the two could be bound as both have a projected mean distance of 248 pc (A) or 255 pc (B). In either case, the minimum mean separation at present would be between 1,665 AU and 1,712 AU.

3. The parallax of A is known, and is 167.98 mas ±0.48. This implies a distance of 6 pc with a probable mini-mum mean separation of the two stars at present of 67 AU.

4. Curious parallax case. A has a parallax of 9.89 mas ±2.19, while B’s is negative and hence unusable. If the system is at the distance indicated by A, the two stars can be no closer at present than 1,235 AU.

5. The parallaxes in this case are unusable. The primary is shown to have a parallax of 10.01 mas ±3.60 (a 36% uncertainty, hence not reliable as a distance indicator),

while B’s parallax has an error estimate three times its value! If the system is truly at the distance suggested by A’s parallax (100 pc), the minimum separation of the two stars at present is 948 AU.

6. Although this pair has a rectilinear solution, the paral-laxes leave open the possibility they are physical. The given parallaxes are 15.60 mas ±0.96 and 16.52 mas ±0.72, suggesting the pair lies somewhere between 61 and 64 pc away. At this distance, the minimum separa-tion at present would be between 813 and 861 AU.

7. This pair shows only a parallax for the primary (3.54 mas ±0.74). The uncertainty of 21% puts this pair just off the uncertainty cutoff of 20%, but is close enough to let us conjecture the pair, if physical, could be 282 pc away with the stars lying some 4,641 AU apart.

8. A case of vastly different parallaxes, the primary show-ing 31.99 mas ±0.86, with the companion showing 15.02 mas ±6.12. Tossing out the companion’s value as too uncertain, a solution using the primary’s value suggests a distance of 31 pc with a minimum separa-tion of 457 AU. Given the fact that there is a very low probability that the parallaxes could actually have any overlap, and the system is almost certainly optical.

9. Only the primary has a parallax (-3.67 mas ± 1.94), so no safe conclusions about distance or separation can be drawn.

WDS Number Disc Comp Date Last Last Last

Year

Meas.

Made Meas Meas Resid Resid Note

00032+4508 HJ 1927 2015.836 72.8 9.83 2011 4 73.362 9.524 -0.562 0.306

00033+6053 HJ 1928 AB 2015.858 183.6 15.34 2010 2 183.096 15.231 0.504 0.109

00047+3416 STF3056 AB, C 2015.915 3.0 26.04 2012 6 3.859 26.034 -0.859 0.002 1

00047+3416 STF3056 AB, C 2015.836 3.0 26.04 2012 6 3.303 26.060 -0.303 -0.024

00272+4959 STF 30 AB 2015.849 314.2 13.20 2014 6 314.361 13.430 -0.161 -0.230 2

00305+2208 HJ 1027 2015.852 217.0 18.21 2010 2 217.809 18.458 -0.809 -0.248

00384+4059 STF 44 2015.852 273.9 12.72 2012 2 274.069 12.815 -0.169 -0.095

00413+5240 AG 299 2015.855 69.0 29.86 2010 2 68.882 30.410 0.118 -0.550

00444+7713 STF 50 2015.863 95.7 22.10 2007 4 96.621 22.489 -0.921 -0.385 3

00504+5038 BU 232 AB, C 2015.901 299.2 24.53 2010 6 299.991 24.444 -0.791 0.086 4

00584+5426 HJ 2003 2015.910 332.4 17.00 2010 6 332.145 16.843 0.255 0.157

00595+8341 STF 69 2015.855 32.5 28.59 2010 2 33.101 28.815 -0.601 -0.225

01207+4620 STF 112 AB 2015.852 336.5 19.17 2011 2 336.789 18.990 -0.289 0.180 5

01268+4908 ARG 50 2015.910 137.3 15.48 2010 6 135.768 15.182 1.532 0.298

01276+6429 STF 121 AB 2015.877 268.0 12.00 2012 6 267.824 12.001 0.176 -0.001

01352+8321 STF 118 2015.855 93.8 15.33 2010 2 93.741 15.522 0.059 -0.192

01374+5838 STT 33 AB 2015.855 77.5 26.64 2011 6 77.081 26.861 0.419 -0.221 6

01383+7235 HJ 2053 2015.904 36.3 33.03 2010 6 36.621 32.871 -0.321 0.159 7

01395+3216 SEI 19 2015.910 347.6 18.86 2011 6 348.405 18.698 -0.805 0.162

01459+7142 HJ 1089 AB 2015.904 89.2 26.34 2012 6 89.340 26.234 -0.140 0.106

01581+4123 S 404 AB 2015.882 82.7 28.90 2012 10 84.367 29.247 -1.667 -0.347 8

02407+6117 STF 284 AB 2015.904 190.4 6.82 2011 6 189.953 6.903 0.447 -0.083 9

Table 1: Measures on 22 Rectilinear Pairs



Last and Last are the last measures of and on record, the year of that measurement being given in the Last Year column. Meas. Made indicates how many measurements of that system I made (bearing in mind that I measured both the actual companion and its com-

plementary image). Meas and Meas are the values I obtained from my measurements, being the means of all

the measurements. Resid and Resid are residuals of the 2015 measurements compared to the last measure on record. The Note flag refers to notes that appear at the end of Table 1.

Table 2 presents the ephemerides and residuals for

these 22 pairs based on the values for and predicted in the Fourth Catalog of Rectilinear Elements. The mean of all the residuals for these 22 pairs was -0.099°

for and +0.044 arc sec for .

It is noteworthy that every pair measured yielded

and values that fell well within the uncertainty bars for each pair except for WDS 01489+7142 (HJ 1089),

where the value of fell just outside the upper limit from the ephemerides (0.040" over the limit).

Measures of Likely Linear Pairs

Analysis of the Measurement History With Excel Microsoft’s Excel spreadsheet program has a useful

tool for working with the Cartesian plots of a pair’s his-torical measurements. After plotting the data for a given pair, the mouse may be right-clicked on any data point which brings up a menu that has, among other options, the ability to insert a trend line. Selecting that option and asking for a linear trend helps identify data that may be emerging as a rectilinear case.

It is possible to ask Excel to display the R2 value (the RMS value of the line of best fit). A value of 1.00 indicates a perfect fit of all the data points to a line; a value of 0.00 indicates no pattern whatsoever exists. Values between 0.00 and 1.00 suggest varying degrees of the fit of the data to a straight line.

In my data plots, I sort linear cases into one of five classes, depending on the R2 value. Graphs with an R2 value of 0.80 and up are assigned to Class 1 (very strong linear tendency). Values between 0.60 and 0.79 are assigned Class 2; values between 0.40 and 0.59 Class 3; 0.20 to 0.39, Class 4; and all others Class 5.

However, it must be noted that Excel’s linear trend line function is a non-weighted function. All data points

WDS Number Disc Comp Meas Meas 2015 Err 2015 Err Resid Resid

00032+4508 HJ 1927 73.362 9.524 72.7 3.7 9.713 0.436 -0.662 0.189

00033+6053 HJ 1928 AB 183.096 15.231 183.2 1.8 15.700 2.174 0.104 0.469

00047+3416 STF3056 AB, C 3.859 26.034 3.1 2.5 25.982 1.120 -0.759 -0.052

00047+3416 STF3056 AB, C 3.303 26.060 3.1 2.5 25.982 1.120 -0.203 -0.078

00272+4959 STF 30 AB 314.361 13.430 314.6 1.4 13.370 0.322 0.239 -0.060

00305+2208 HJ 1027 217.809 18.458 217.8 3.0 19.083 0.967 -0.009 0.625

00384+4059 STF 44 274.069 12.815 273.9 0.9 12.719 0.490 -0.169 -0.096

00413+5240 AG 299 68.882 30.410 68.6 1.3 30.389 0.656 -0.282 -0.021

00444+7713 STF 50 96.621 22.489 96.2 3.2 22.339 0.736 -0.421 -0.150

00504+5038 BU 232 AB, C 299.991 24.444 298.9 3.7 24.610 1.633 -1.091 0.166

00584+5426 HJ 2003 332.145 16.843 331.8 1.5 17.071 0.346 -0.345 0.228

00595+8341 STF 69 33.101 28.815 32.7 0.6 28.858 0.322 -0.401 0.043

01207+4620 STF 112 AB 336.789 18.990 336.5 3.6 18.987 1.556 -0.289 -0.003

01268+4908 ARG 50 135.768 15.182 136.3 1.5 15.648 0.401 0.532 0.466

01276+6429 STF 121 AB 267.824 12.001 267.7 4.1 11.946 1.112 -0.124 -0.055

01352+8321 STF 118 93.741 15.522 93.9 1.7 15.493 0.472 0.159 -0.029

01374+5838 STT 33 AB 77.081 26.861 77.3 9.5 26.922 4.217 0.219 0.061

01383+7235 HJ 2053 36.621 32.871 36.2 0.5 32.984 0.286 -0.421 0.113

01395+3216 SEI 19 348.405 18.698 347.7 1.2 18.735 0.597 -0.705 0.037

01459+7142 HJ 1089 AB 89.340 26.234 89.0 0.3 26.568 0.141 -0.340 0.334

01581+4123 S 404 AB 84.367 29.247 83.9 1.7 29.008 1.315 -0.467 -0.239

02407+6117 STF 284 AB 189.953 6.903 190.3 8.8 6.911 2.134 0.347 0.008

Table 2: Ephemerides and Residuals for the Rectilinear Pairs



are given equal weight in determining the final fit of the line. In working with double stars this is not how we evaluate the historical data, of course. To be precise, each measurement must be assigned a weight based on a number of factors (see http://ad.usno.navy.mil/wds/orb6/orb6text.html#grading for more information). Hence, the Excel linear trend line function can serve as an indicator that a pair may be linear, but not as a defin-itive statement.

One must exercise caution when assigning a linear nature to a pair. There are two mitigating factors that can actually rule against linearity. These factors are (1) the number of measurements (some pairs have fewer than a dozen measurements), and (2) the total displace-ment of the companion over the history of the measure-ments (in some cases, the companion has only moved 3

arc seconds in nearly 200 years). When a pair has sig-

nificant change in over the years, it is more likely that the pair is linear. Even then, however, one must be careful that we are not observing a nearly edge-on orbit in which the companion is transiting in front of (or be-hind) the primary in its normal orbit. (A similar prob-lem exists with common proper motions, which will be covered in another paper.)

Results, Part 2: 18 Pairs That Are Showing Def-inite Rectilinear Motion

Having said all of that, I present Table 3, which shows 18 pairs that have high R2 values but for which no rectilinear solutions presently exist.



Year

Meas.

Made Meas Meas Resid Resid R2 Note

00042+4959 HJ 1931 2015.849 117.0 22.40 2014 2 117.491 22.843 -0.491 -0.443 n/a 10

00071+6309 ES 1934 AB 2015.915 70.4 6.77 2004 4 70.949 6.835 -0.549 -0.065 0.8787 11

00099+1125 HJ 1939 2015.915 168.7 31.09 2010 6 169.569 30.630 -0.869 0.460 0.9243 12

00099+7329 WFC 1 2015.877 36.5 6.42 2010 6 34.806 6.277 1.694 0.143 0.7922 13

00167+4104 FAB 2 AB 2015.852 308.8 12.17 2010 2 304.499 12.940 4.301 -0.770 0.9972 14

00287+5801 MLB 107 AB 2015.910 2.8 34.97 2011 6 3.219 34.443 -0.419 0.525 0.8825 15

00304+6059 STI 82 AB 2015.863 81.7 11.19 2011 2 84.524 11.122 -2.824 0.071 0.9508 16

00324+4455 HJ 1029 2015.852 289.1 14.80 2010 2 289.098 15.002 0.002 -0.202 0.9980 17

00395+6002 HJ 1042 2015.863 63.3 15.34 2014 2 63.690 15.349 -0.390 -0.009 0.7965 18

00458+4951 ES 446 2015.901 256.6 13.83 2007 6 257.022 13.846 -0.422 -0.016 0.8015 19

00552+3814 KU 71 2015.855 248.9 22.50 2013 2 248.311 22.328 0.589 0.172 0.8092 20

01107+8021 STF 89 2015.855 322.2 16.57 2006 2 319.640 16.803 2.560 -0.233 0.9287 21

01246+5311 ES 2583 2015.882 343.8 26.39 2011 10 345.133 25.949 -1.333 0.438 0.9129 22

01495+2842 STF 176 2015.915 330.5 23.70 2006 6 331.513 23.695 -1.013 0.005 0.9395 23

01594+5036 AG 302 2015.893 2.6 14.65 2010 6 3.134 14.595 -0.534 0.055 0.7978 24

02108+5624 ARG 7 2015.893 252.9 16.79 2009 6 252.945 16.930 -0.045 -0.140 0.8857 25

02124+7256 HJ 1107 2015.915 99.5 21.21 2012 6 98.805 21.126 0.695 0.084 0.9363 26

02481+3733 AG 51 2015.915 285.5 11.10 2010 6 284.654 11.256 0.846 -0.156 0.9183 27

Table 3. 18 Likely Rectilinear Pairs

http://ad.usno.navy.mil/wds/orb6/orb6text.html#grading

http://ad.usno.navy.mil/wds/orb6/orb6text.html#grading



Table 3 Notes:

10. It is ironic that the first pair in this table does not yield a linear trend line solution, as the data plots in almost a perfectly north-south line and Excel tries to draw the trend line horizontally! Nonetheless, the plot shows a nearly straight line with the companion moving in the

general direction of = 180°. Figure 3 is a plot of the measurements showing 2015.849 as the red box:

11. Figure 4 is the data plot for this pair, based on weighted measurements (more reliable than Excel’s equal weight line).

12. Figure 5 is a weighted plot of the data.

13. The WFC 1897.75 measurement should be heavily dis-counted as it plots well away from the rest of the data. (If it is included, the R2 value drops to 0.3863.) Figure 6 is the plot with WFC 1897.75 removed:

Figure 3: Data plot of WDS 00042+4959 showing strong linear nature in the motion of the companion.

Figure 4. Plot of WDS 00071+6309 AB.

Figure 5. Plot of WDS 00099+1125.

Figure 6. Plot of WDS 00099+7329 without WFC 1897.75.



14. Figure 7 is a data plot of WDS 00167_4104

15. Figure 8 is a plot of WDS 00287+5801 AB.

16. Only seven measures for this pair make classification a bit premature despite the high R2 value. See Figure 9.

17. A plot of this pair is shown in Figure 10.

Figure 7: Plot of WDS 00167_4104.

Figure 9: Plot of WDS 00304+6059 AB; premature classifi-cation may be the case here.

Figure 10: Plot of WDS 00324+4455.

Figure 8. Plot of WDS 00287+5801 AB.



18. Here is a plot (Figure 11) using weighted measurements:

19. Both CLL 1980 and TOB 1989.43 plot well away from the data (See Figure 12.) and, if included, drop the R2 value down to 0.0009. They should be given very little, if any, weight for analysis.

20. A plot of this pair is given in Figure 13.

21. Apparently EGB 1879.75 flipped the protractor on his micrometer as his data point plots well away from the historical trend. If we subtract his q from 360°, his data point falls right on the trend line. Figure 14 is a weighted plot of the data:


Figure 12: Plot of WDS 00458+4951 without CLL 1980 and TOB 1989.43.


Figure 14: Plot of WDS 01107+8021 with EGB 1879.75 cor-rected for quadrant flip.



22. This pair is plotted in Figure 15.

23. See Figure 16. CLL 1980.8 should be given no weight. It plots well away from the trend and its presence drops the R2 value from 0.9395 to 0.8084.

24. Figure 17 is a plot of this pair.

25. Figure 18 is a plot of this pair.


Figure 16. Plot of WDS 01495+2842 without CLL 1980.8.





26. John Herschel’s measurements are very poor and should be given a very low weight during analysis. The plot of this pair, without HJ 1828 and HJ 1831.83, is shown in Figure 19.

27. A plot of this pair is given in Figure 20.


Figure 19. Plot of WDS 02124+7256 without HJ 1828 and HJ 1831.83.

Results, Part 3: 26 Pairs That Are Showing Pos-sible Rectilinear Motion

In Table 4, I present the measurements on 26 pairs that show some possibility of rectilinear motion. These cases are very vague at this time, but these pairs de-serve extra attention by astrometrists in the years ahead to help determine their true nature.

In Table 4, Last , Last , and Last Year are the

year and latest recorded measures for and . Meas. Made shows how many measurements I made of the pair (using both the companion and its complement

image). Meas and Meas report my measurements of

the pair. Resid and Resid show the residuals of my measurement compared to the last measurement on rec-ord.

Discussion

The Autumn 2015 observing program at Brilliant

Sky Observatory produced many useful and accurate CCD measurements of 66 known (or possibly) rectilin-ear pairs. The measurements confirmed the accuracy of the ephemerides of the known pairs in all but one case, and that exception was marginal.

In addition, 18 cases were uncovered that are likely at or nearly at a solvable state for determining the recti-linear elements and producing ephemerides.

The utility and accuracy of Plate Solve 3.47B is well established by this observing program.

The ability of the Skyris to capture data on close and faint pairs was demonstrated by this program.

Recommended Future Observations

I plan to measure the same stars early in 2016 after their early evening positions make them easily ob-served on the west side of the meridian and then com-pare east-meridian measurements to west-meridian measurements to identify systemic errors (if any) and provide a second set of measures for these stars.





Table 4 Notes:

1. The plot shows a vague suggestion of sinusoidal mo-tion of the companion.

2. Just starting to show a linear trend.

3. HJ 1831.83 should be heavily discounted in the analy-sis.


5. HJ 2818.0 should be heavily discounted in the analysis.


7. FmY 2012.85 should be heavily discounted in the anal-ysis.





Year

Meas.


00059+1805 STF3060 AB 2015.904 133.6 3.35 2012 6 134.528 3.444 -0.928 -0.099 0.5181

00091+5938 ARG 1 AB 2015.836 329.0 25.94 2012 4 328.757 25.961 0.243 -0.021 1

00100+4623 STF 3 2015.904 80.9 4.95 2011 6 82.409 5.012 -1.509 -0.062 0.3247 2

00229+5420 ES 42 2015.882 206.1 7.26 2003 8 208.633 7.202 -2.533 0.059 0.6613

00253+3724 ES 1938 2015.910 8.4 7.14 2010 6 8.106 7.038 0.294 0.102 0.4393

00303+5624 STI1364 2015.852 6.7 14.64 2012 2 7.309 14.682 -0.609 -0.042 0.6164

00318+3658 STT 13 AB 2015.893 131.4 6.85 2011 6 132.211 6.762 -0.811 0.088

00403+2403 BU 1348 AC 2015.852 233.1 46.44 2011 2 53.128 46.516 -0.028 -0.076 0.0169

00444+3332 STF 54 2015.855 188.5 18.52 2010 2 188.426 18.301 0.074 0.223 0.3848

00505+7538 HJ 1997 2015.855 47.3 17.60 2014 2 47.273 17.598 0.027 0.002 0.6379

00538+5242 STF 70 AB 2015.915 247.7 8.04 2011 6 247.244 8.132 0.456 -0.092 0.6059

01134+7137 HJ 2022 2015.877 154.1 11.85 2012 6 154.406 11.929 -0.306 -0.079 0.6938 3

01147+4255 ARG 49 AC 2015.893 99.8 22.71 2003 6 102.929 23.489 -3.129 -0.779 0.6105

01245+3902 STTA 17 AB 2015.890 101.5 35.80 2014 10 101.141 35.376 0.359 0.424

01279+7807 HJ 2038 2015.855 358.1 26.20 2010 2 358.030 25.959 0.070 0.241 0.2585 4

01301+4131 HJ 1081 2015.893 318.1 8.89 2003 6 319.380 8.419 -1.280 0.471 0.3954 5

01317+6103 STF 128 2015.877 309.1 11.28 2007 10 310.169 11.360 -1.069 -0.077 .02492

01342+4800 STF 134 2015.910 354.6 11.11 2010 6 356.415 10.989 -1.815 0.121 0.7090

01344+5553 HJ 2047 2015.855 55.4 13.33 2005 2 56.702 13.320 -1.302 0.010 0.7453 6

01364+7909 STF 127 2015.855 190.4 23.71 2010 2 190.226 23.395 0.174 0.315 7

01393+3901 HJ 1087 2015.910 74.5 13.26 2014 6 75.072 13.077 -0.572 0.183 0.0472 8

01393+5257 STF 139 AB 2015.893 38.9 9.21 2011 5 39.117 9.212 -0.217 -0.002 0.3689 9

01456+7721 HJ 2065 2015.915 156.2 21.65 2012 4 155.737 21.320 0.463 0.330 0.7648

01523+3355 HU 805 AC 2015.910 257.2 14.82 2012 6 256.967 14.793 0.233 0.030 0.7155

02011+7358 STF 184 2015.863 14.9 17.03 2010 2 14.474 16.989 0.426 0.041 0.6478

02109+1341 STF 224 2015.915 243.5 6.00 2011 6 243.862 5.942 -0.362 0.058 0.5726 10

Table 4. 26 Possible Rectilinear Pairs



Acknowledgments

This research has made use of the Washington Double Star Catalog maintained at the U. S. Naval Ob-servatory. Use was also made of the VizieR service of the Centre de Données astronomiques de Strasbourg and the Hipparcos 2 Output Catalog, and the Fourth Catalog of Rectilinear Elements produced by the U. S. Naval Observatory.

The author thanks Dr. William H. Hartkopf of the U. S. Naval Observatory for reviewing the draft of this paper.

References

Cotterell, J. David 2015. Calibrating the Plate Scale of a 20 cm Telescope with a Multiple-Slit Diffraction Mask. JDSO Vol 11 No 4, 387-389. Viewable online at JDSO.org.

Harshaw, Richard 2015. Calibrating a CCD Camera for Speckle Interferometry. JDSO Vol 11 No 1s, 314-322.




From October 23 to December 1, 2015, a vigorous program of measuring double stars with a Skyris 618C CCD camera was done at Brilliant Sky Observatory (Cave Creek, Arizona). Over 18 different nights, over 220 double stars were imaged and their FITS cubes re-duced using Plate Solve 3.47B. This report focuses on 8 pairs that either have known orbits (one case), or are showing strong arc-like shapes of the plots of their measurements (four pairs), or are close pairs (three) best analyzed with speckle interferometry.

Equipment Used

The equipment used in this observing program is described in detail in Harshaw 2016. This includes the telescope (a C-11), the mount (CGEM-DX), camera (Celestron Skyris 618c), and data reduction software (Plate Solve 3.47B).

Procedure

When doing speckle interferometry, I select pairs that are no farther apart than 7 arc seconds and with both magnitudes being brighter than 8.50, since fainter stars require integration times of greater than 100ms. (The “rule of thumb” for speckle integration times says 50ms or less, which is considered by many to be about as long as one can image without smearing out the speckles created by the atmosphere. But this rule was established with large research-grade telescopes which

must look through many millions of Fried turbulence cells compared to a smaller telescope’s thousands of cells. A member of our speckle “community”, Clif Ash-craft of New Jersey, has been getting good speckle re-sults with integration times in the 100ms range.) The magnitude limit comes into play when one considers that when obtaining speckles, I use a Johnson-Cousins “R” filter to reduce atmospheric dispersion. This means that there are only a little over 180 pairs that can be an-alyzed with speckle using a Skyris 618C on a C-11.

For speckle, I obtain 1,000 FITS frames (which Plate Solve converts into a FITS cube for processing), and generally run 3 to 8 sets of frames.

The speckle procedure also requires obtaining 1,000 FITS frames of a single “deconvolution” star. The Fourier Transform that Plate Solve develops for the deconvolution star is then applied to the double star to enhance the clarity of the data and produce a high-quality autocorrelogram.

For CCD measures, I find that taking 100 frames and then selecting the best 25% for signal to noise ratio yields 25 frames that Plate Solve can work with very nicely. I find that as a general rule, Plate Solve gives more accurate solutions than lucky imaging.

For a description of my processing method, see Harshaw 2016.

Results, Part 1: One Grade 3 Orbit

First to report is the one pair with a known orbit

CCD Measurements of 8 Double Stars With Binary Nature The Autumn 2015 Observing Program

at Brilliant Sky Observatory, Part 2

Richard W. Harshaw

[email protected] Brilliant Sky Observatory, Cave Creek, AZ

Abstract: Results of CCD measures of five pairs are reported as well as three cases of speckle interfer-ometry. Results show that the Skyris 618 CCD camera and an 11-inch SCT can do serious and accurate double star astrometry


CCD Measurements of 8 Double Stars With Binary Nature ...

that was imaged during the Autumn 2015 observing season at Brilliant Sky Observatory. The results are shown in Table 1.

In Table 1, Last and Last are the measures of

and (respectively) in the year shown in Last Year. Meas. Made is the number of measurements made of

the autocorrelograms. Meas. and Meas. and Resid.

and Resid. are the measurements (and residuals) of the measurement made. With only six measures made of three FITS cubes, the standard error is of little value.

The PNG file for this pair from the U. S. Naval Ob-servatory is shown in Figure 1.

After obtaining the measurement history of this pair from the U. S. Naval Observatory, the past measure-ments were corrected for precession of the equinoxes and plotted in Cartesian coordinates using Microsoft’s Excel. The result of that plot, showing the 2015.855 measure, is the red box in Figure 2.

Results, Part 2: 4 Pairs That Show A Short Arc

Short arc binaries are pairs whose data plot is be-ginning to show an arc, the telltale sign that the pair is probably physically bound, as the arc is the projection of the orbital path on the plane of the sky.

However, do not interpret short arc to mean short period. In some cases, the arc may be revealing itself at periastron (or apastron) and the arc may be a small piece of a huge and highly inclined orbit.

But the arcing does suggest, no matter the orbital period that may someday be derived, that the pair is gravitationally bound. It may take centuries more of measurement to collect enough data to permit an orbital solution, but the existence of such pairs should warrant special attention by astrometrists in the future.

To determine a pair to be a short arc binary, it is necessary to obtain the measurement data from the U. S. Naval Observatory and then to enter the values of theta and rho into a spreadsheet that can then translate the values into X, Y coordinates, thus allowing the user to plot the data in Cartesian space. This is done by the simple mathematical conversions of

X = * sin(

Y = * cos()

In addition, we must adjust for the precession of the equinoxes to normalize the measurements for differ-ent epochs to the present day. All of this is done in an Excel program I wrote for the purpose of plotting the measurement histories.

Excel has a trend line function that can be invoked by right-clicking on any data point in the graph of the

measurements and selecting Insert Trend Line. This allows us to select a polynomial line that takes on the shape of an arc. We can also ask for the R2 value, a number that reflects the goodness of the fit of the data to the curve. However, Excel assigns equal weights to all the data points, which is not how we analyze histori-cal data in double star astrometrics. The higher the R2 value, the more likely it is that we are indeed seeing the emergence of a short arc and hence have a clue about the physical/binary nature of the pair. The lower the R2 value, the more scatter or noise in the data and the less likely we are looking at a true binary system.

The format of Table 2 is the same as Table 1 but with the addition of the R2 value column.

Results, Part 3: 3 Speckle Interferometry Pairs

In the autumn 2015 observing program at Brilliant Sky Observatory, three pairs were measured using speckle interferometry. This process has been docu-mented in Harshaw (2015).

All three speckle measurements were made at f/30 and consisted of pairs bright enough to image at inte-gration times of under 50ms and with separations of 7 arc seconds or less, using a Johnson-Cousins “R” filter.

(Two stars are borderline cases for . As a general rule, stars wider than 7 arc seconds will probably have their light passing through different isoplanatic patches, so true speckle interferometry is not usually reliable at these separations. However, exceptionally good seeing might extend the patch a bit.)

In all three pairs, the stars have common proper motion.

The data for the speckle measurements are in Table 3.

Discussion

The Autumn 2015 observing program at Brilliant Sky Observatory proved that speckle interferometry on close double stars can be done with amateur-class equipment and inexpensive CCD cameras.

The one known orbit pair that was measured showed results that are in good conformance with the ephemerides from the Sixth Catalog of Orbits of Visual Binary Stars.

The short arc binaries deserve special attention by astrometrists in the coming years.


Observations of the pairs featured in Table 2 would be a good investment of amateur observing time as we may be only a few measurements away from deriving





Year

Meas.


00089+6627 FAB 1 2015.858 178.9 14.65 2011 2 181.034 14.905 -2.134 -0.255 0.5461 2

00311+5648 ES 2 AB 2015.890 112.1 5.93 2012 8 112.686 5.854 -0.586 0.076 0.7661 3

00546+3910 STF 72 2015.855 172.5 23.03 2014 2 172.969 23.339 -0.469 -0.309 0.7203 4

01373+6344 MLB 383 AD 2015.877 165.6 31.96 2011 6 164.809 31.752 0.791 0.208 0.0478 5

Table 2: Short Arc Binaries

WDS Number Disc Comp Date Last Last Last Year Meas.

Made Meas Meas Resid Resid Notes

00491+5749 STF 60 AB 2015.855 324.3 12.78 2014 6 324.783 13.696 -0.483 -0.916 1

Table 1: Measure of WDS 00491+5749 (STF 60 AC)

Notes to Tables:

1. Using the Sixth Orbit Catalog ephemerides and extrapolating for 2015.855, the projected values for and are 323.642°

and 13.346". The residuals for the 2015.855 measurement are +1.141° and +0.353" . See Figures 1 and 2.

2. The trend line (Figure 3) is actually “reversed”—the concave side of the curve points away from the system’s center of mass. May not be a true short arc binary.

3. In this case, the trend line has the pair’s center of mass on the correct side of the curve. See Figure 4.

4. Parallaxes for both stars are known, but neither is reliable as a test for distance and physical separation of the two stars. The parallax values are 1.33 ±1.30 mas for the primary and 12.33 ±5.51 mas for the companion. See Figure 5.

5. See Figure 6 for a plot of WDS 01373+6344.

6. See Figure 7 for a plot of WDS 00499+2743, a speckle measurement.

7. See Figure 8 for a plot of WDS 01001+4443, a speckle measurement.

8. See Figure 9 for a plot of WDS 01535+1918 AB, a pair with several anomalous measurements.


Year

Meas.

Made Meas Meas Resid Resid Plot

00499+2743 STF 61 2015.855 115.0 4.50 2014 20 113.529 4.200 1.471 0.300 6

01001+4443 STF 79 2015.855 194.1 7.90 2013 10 192.327 7.842 1.773 0.058 7

01535+1918 STF 180 AB 2015.855 0.9 7.41 2014 10 359.704 7.362 -0.604 0.048 8

Table 3: Speckle Interferometry on Three Pairs

Figure 1: PNG plot of WDS 00401+5749. Figure 2: Plot of WDS 00491+5749 AB history showing the 2015.855 measurement (red box).



Figure 3: Plot of WDS 00089+6627, a curious case of a re-verse trend curve.

Figure 4: Plot of WDS 00311+5648 AB.

Figure 5. Plot of WDS 00546+3910. Figure 6: Plot of WDS 01373+6344 AD.



Figure 7. Plot of WDS 00499+2743, a speckle measurement.


Figure 9. Plot of WDS 01535+1918 AB, a pair with several

anomalous measurements.



an orbital solution.

Acknowledgments

This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Ob-servatory. Use was also made of the VizieR service of the Centre de Données astronomiques de Strasbourg and the Hipparcos 2 Output Catalog as well as the Sixth Catalog of Orbits of Visual Binary Stars (Hartkopf and Mason, June 2015).

References



Harshaw, Richard 2016. CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs. JDSO, in submission.



From October 23 to December 1, 2015, a vigorous program of measuring double stars with a Skyris 618C CCD camera was done at Brilliant Sky Observatory (Cave Creek, Arizona). Over 18 different nights, over 220 double stars were imaged and their FITS cubes re-duced using Plate Solve 3.47B. This report focuses on 141 pairs that share some degree of proper motion.

Equipment Used

The equipment used for this project is described in Harshaw 2016.

Procedure

See Harshaw 2016 for a complete description of the procedure used for these observations.

Results: 141 Pairs That Are Proper Motion Re-lated

This set of measurements deals with stars that share proper motion to some degree. I list three types of prop-er motion classes, based on the relative differences in the proper motions.

The proper motion of a star can be depicted as a vector. When the resultant of the two vectors is divided by the largest vector, the result will either be zero (or very near it) if the proper motions are identical, some-where between 20% and 60% of the resultant of the

vectors, or over 60% of the resultant. Pairs in the first category are classed as Common Proper Motion pairs, or CPM. Pairs in the second category are classed as Similar Proper Motion pairs (SPM), and those in the third category are classed as Different Proper Motion pairs (DPM).

Some examples might help illustrate the classifica-tion scheme.

Case 1 has two stars in which the proper mo-tion (PM) vectors of the stars are +027 +018 for the primary and +026 +018 for the companion. The result-ant is found by:

R = 1 mas

The largest vector is that of the primary, for which the value is

V = 31.6 mas

The ratio of the resultant to the largest vector is thus 1/31.6 = 3.2%. This is a CPM case.

Case 2 has a pair with PM of -026 +005 for the pri-

CCD Measurements of 141 Proper Motion Stars: The Autumn 2015 Observing Program at the

Brilliant Sky Observatory, Part 3

Richard W. Harshaw

[email protected] Brilliant Sky Observatory, Cave Creek, AZ

Abstract: The use of a Skyr is 618C camera on a Celestron C-11 SCT proved to be a reliable means of obtaining accurate data for double star astrometry. 141 systems were examined, with all but one result plotting within the scattered data from the historical measurements.


CCD Measurements of 141 Proper Motion Stars: The Autumn 2015 Observing Program ...

mary and -018 +009 for the companion. The resultant is 8.94 mas while the largest vector has a scalar value of 26.48 mas. The resultant is 33.7% of the scalar, so this is a SPM pair.

For Case 3, the primary has PM of +038 -076 with a companion of -010 +037. The resultant is 122.7 mas while the scalar for the largest vector is 85.0 mas. The ratio is 69.2%, so this would be a DPM case.

Common proper motion stars are a challenge for double star astrometry. First, they appear to be moving across the sky at the same angular rate. If they are at nearly the same distance (established by accurate paral-laxes, which are not always available for both stars of a double), they are probably physically related. If close enough to be gravitationally bound, they are probably a true binary (albeit one with an extremely long period). If too far for gravitational binding (and such binding would depend on the total system mass relative to the orbital velocity of the pair, as noted by Rica [2011]), then the pair probably shares a common origin— per-haps being ejected together from an open star cluster or stellar association.

It might also be the case that stars that show no sig-nificant displacement over two or three centuries could be in highly eccentric orbits whose plane is nearly on our line of sight and whose major axis is oriented more or less along our line of sight, and that we are viewing the motion of the companion along one of the longer sides of the orbit as it approaches (or recedes from) earth. In such cases, a star may show no significant an-gular displacement for thousands of years.

Finally, the two stars may not be related to each other at all. They just happen to share angular motion across the sky. If they are at greatly different distances, this implies that the more remote star has a higher abso-lute motion through space than the nearer star, but other than that, we cannot make any conclusions about the nature of the system, unless accurate parallaxes for both stars are known and the parallaxes place the stars at significantly different distances (too far apart for gravi-tational binding).

Discussion

All but one of 141 measurements plotted inside the region of all the historical measurement plots. Only one measurement plotted on the outer edge of the historical grouping (WDS 00142+4612).

The capabilities of the Skyris 618 and an 11-inch SCT to do accurate double star astrometry are well-established.


Four pairs appear to be physical and warrant extra attention: WDS 00528+5638, WDS 01057+2128, WDS

02053+6740 and WDS 02370+2439. Three pairs show an optical nature and could use

extra observations in the next few decades: WDS 00028+8017, WDS 00352+3650 and WDS 21543+1943.

Four pairs are starting to show what may be a linear trend. These are WDS 00029+7122, WDS 00052+3020, WDS 01420+5547 and WDS 01513+6451.

Acknowledgments

This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Ob-servatory. Use was also made of the VizieR service of the Centre de Données astronomiques de Strasbourg and the Hipparcos 2 Output Catalog.

References



Harshaw, Richard 2016. CCD Measurements of 66 Rectilinear and Probable Rectilinear Pairs. JDSO¸ in submission.

Rica, F. M. 2011. Determining the Nature of a Double Star: The Law of Conservation of Energy and the Orbital Velocity. JDSO Vol 7 No 4, 254-259.



WDS No. Disc Comp Date Last Last Last

Year

Meas.

Made Meas Meas Resid Resid Type Note

00004+6026 STI1248 2015.855 48.2 12.37 2011 2 48.021 12.254 0.179 0.114 CPM

00005+6713 HJ 1924 2015.858 225.1 8.20 2010 2 224.761 8.087 0.339 0.113 CPM

00020+2347 TVB 2 2015.849 292.2 28.07 2010 6 292.166 27.925 0.034 0.145 CPM

00026+6606 STF3053 AB 2015.833 70.0 14.30 2014 10 70.586 15.159 -0.586 -0.859 SPM

00027+5958 ARG 47 2015.833 290.0 9.90 2010 6 287.620 9.876 2.380 0.024 DPM

00028+8017 STF3051 2015.836 23.6 16.69 2010 6 22.827 16.768 0.773 -0.078 CPM 1

00029+7122 STF3052 2015.836 8.7 34.72 2010 6 8.294 34.649 0.406 0.071 SPM 2

00031+0816 STF3054 2015.836 180.0 34.70 2014 6 181.296 33.597 -1.296 1.103 CPM

00039+2759 HJ 1929 AB, C 2015.904 287.3 5.43 2011 6 288.115 5.138 -0.815 0.292 SPM

00040+6050 HJ 1930 2015.858 346.4 10.95 2011 2 346.404 10.810 -0.004 0.140 CPM

00042+2701 SMA 1 2015.852 161.3 13.12 2010 2 161.356 13.382 -0.056 -0.262 CPM

00043+4235 HJ 1932 AB 2015.882 306.5 7.11 2011 6 307.037 7.155 -0.537 -0.045 CPM

00052+3020 STF3058 2015.836 52.2 12.60 2012 6 51.267 12.616 0.933 -0.016 CPM 3

00068+5430 ES 611 2015.849 291.0 9.88 2003 2 289.970 10.367 1.030 -0.487 CPM

00078+5723 HJ 3241 2015.849 8.1 15.04 2014 4 7.976 14.974 0.124 0.066 CPM

00089+3713 STF 1 2015.836 286.7 9.65 2014 4 286.216 9.855 0.484 -0.205 SPM

00096+4758 ES 1126 2015.910 318.3 6.36 2008 6 317.634 6.056 0.666 0.304 SPM

00099+0827 STF 4 2015.904 276.1 5.20 2009 6 276.109 5.243 -0.009 -0.043 CPM

00099+3014 MLB 552 2015.882 190.0 8.20 2012 8 190.027 8.042 -0.027 0.158 DPM

00112+4419 ES 1406 AB 2015.890 331.5 9.35 2011 8 333.136 9.686 -1.636 -0.336 SPM

00114+5205 HJ 1004 AC 2015.890 314.8 25.10 2014 8 315.279 25.207 -0.479 -0.107 DPM 4

00115+2949 MLB 441 AB 2015.852 358.7 14.14 2012 2 358.670 14.138 0.030 0.002 CPM 5

00116-0305 STF 8 2015.836 291.8 7.99 2012 6 291.325 7.621 0.475 0.369 CPM

00129+6150 ES 1865 AB 2015.858 121.6 23.60 2012 3 123.289 23.712 -1.689 -0.112 DPM

00137+4934 STF 9 2015.849 164.5 20.19 2003 4 165.411 19.935 -0.911 0.255 CPM

00138+3612 BU 1341 AB 2015.910 319.0 20.51 2014 8 319.330 20.295 -0.330 0.215 CPM

00142+4612 ES 1195 2015.910 14.6 6.68 2002 6 12.856 6.788 1.744 -0.104 CPM 6

00148+6250 STF 10 AB 2015.849 176.0 17.60 2012 4 175.664 17.503 0.336 0.097

00150+0849 STF 12 2015.836 145.0 11.60 2014 8 147.190 11.527 -2.190 0.073 SPM

00152+7801 STF 11 2015.858 191.8 7.97 2010 6 191.522 8.220 0.278 -0.250 CPM

00160+4835 HJ 1009 AB 2015.852 27.9 16.79 2003 2 28.287 16.199 -0.387 0.591 SPM

00160+4835 HJ 1009 AC 2015.852 138.4 36.46 2002 2 137.085 36.108 1.315 0.352 SPM

00161+6006 HJ 1010 2015.858 117.8 20.40 2008 2 118.246 20.471 -0.446 -0.071 SPM

00162+2918 STF 17 AB 2015.849 30.0 26.90 2012 4 28.986 26.696 1.014 0.204 SPM 7

00167+5439 STF 16 2015.901 39.1 5.82 2003 6 40.618 5.869 -1.518 -0.049 SPM

00174+1631 STF 20 2015.849 233.4 11.88 2009 4 233.425 11.913 -0.025 -0.029 CPM

00174+3550 WEI 1 2015.904 286.6 5.28 2009 6 285.884 5.386 0.716 -0.106 CPM

00185+2608 STF 24 2015.904 247.0 5.10 2013 6 247.429 4.950 -0.429 0.150 SPM

00203+5412 HDS 44 2015.852 32.1 12.34 2009 4 37.636 12.312 -5.536 0.028 DPM

00214+6700 STF 26 AB, C 2015.858 114.4 13.33 2010 4 113.627 13.753 0.773 -0.424 CPM

00216+5543 STI1334 2015.910 235.4 6.61 2011 6 235.867 6.600 -0.467 0.010 SPM

00220+4213 HJ 1021 2015.910 246.2 6.15 2002 6 247.127 6.016 -0.927 0.135 SPM

00239+2930 STF 28 AB 2015.849 224.2 32.80 2013 6 223.919 32.786 0.281 0.014 CPM

00260+6647 HJ 1026 2015.863 192.1 12.35 2012 2 192.393 12.466 -0.293 -0.116 CPM

00261+3448 HJ 622 2015.852 130.9 19.86 2014 2 130.924 19.794 -0.024 0.066 CPM

Table 1. Measurements on 141 Proper Motion Pairs





Year

Meas.


00270+6430 MLB 277 2015.877 72.6 6.34 2011 6 73.272 6.709 -0.672 -0.369 ???

00271+6112 FOX 108 2015.863 26.8 7.58 2012 2 26.919 7.369 -0.119 0.211 SPM

00287+5700 STI1358 2015.852 302.6 14.32 2011 2 302.691 14.247 -0.091 0.074 SPM

00310+5539 ES 116 2015.882 256.0 7.41 2003 10 257.762 7.409 -1.762 0.001 DPM

00327+7807 STF 34 2015.863 339.4 5.79 2006 6 339.111 5.609 0.289 0.181 CPM

00329+3007 FOX 111 2015.852 26.5 23.22 2010 2 26.771 23.081 -0.271 0.139 SPM

00333+3731 ALI 249 2015.852 287.3 13.33 2005 2 287.398 13.023 -0.098 0.307 CPM 8

00350+5636 ES 3 2015.849 158.6 8.10 2012 4 158.769 7.921 -0.169 0.179 CPM

00352+3650 STF 40 AB 2015.849 312.1 11.64 2014 6 311.628 12.015 0.472 -0.375 SPM 9

00355+5841 STF 38 2015.852 144.4 16.89 2012 4 144.265 16.900 0.135 -0.010 SPM

00369+3343 H 5 17 AB 2015.890 173.5 35.60 2014 10 173.969 35.702 -0.469 -0.102 SPM

00400+5549 ES 936 2015.901 269.0 6.03 2011 6 270.994 7.886 -1.994 -1.856 CPM

00403+2403 STF 47 AB 2015.852 205.7 16.40 2011 2 205.464 16.560 0.236 -0.160 CPM

00403+4343 HJ 1044 2015.890 138.9 21.73 2005 8 139.389 21.560 -0.489 0.170 CPM

00430+4405 ES 1408 2015.901 262.5 7.90 2005 6 265.106 7.558 -2.606 0.342 CPM

00474+7239 STF 57 2015.863 197.9 6.29 2010 2 15.271 6.151 182.629 0.139 ???

00475+4214 ES 1488 2015.890 280.9 6.91 2004 8 282.638 6.810 -1.738 0.100 CPM

00495+5534 STI1437 2015.910 298.6 11.27 2011 2 298.641 11.093 -0.041 0.176 SPM

00503+3548 STF 62 2015.855 303.0 11.81 2012 2 303.010 11.757 -0.010 0.053 CPM

00514+7010 HJ 1999 2015.863 16.2 25.60 2010 2 16.153 25.312 0.047 0.288 CPM

00528+5638 BU 1 AD 2015.890 194.8 8.96 2012 6 196.763 8.896 -1.963 0.064 SPM

00528+5638 BU 1 CD 2015.890 133.0 3.10 2013 6 134.536 3.718 -1.536 -0.618 ??? 10

00536+6835 AG 8 2015.855 35.2 17.41 2010 2 34.923 17.387 0.277 0.023 CPM

00543+6903 AG 9 2015.863 70.6 6.49 2003 2 71.112 6.419 -0.512 0.070 SPM

00573+6020 ARG 3 2015.855 200.2 20.69 2014 2 199.991 20.677 0.209 0.013 CPM

00581+2655 STF 77 2015.855 118.0 10.37 2005 2 119.324 10.300 -1.324 0.070 CPM

00583+5659 STI1492 2015.882 315.9 14.55 2010 8 316.312 14.380 -0.412 0.172 DPM

01003+6717 HJ 1061 2015.877 103.6 13.17 2010 4 102.748 13.125 0.852 0.045 CPM

01027+4742 HJ 2010 2015.833 270.7 9.88 2011 8 270.428 9.899 0.272 -0.019 CPM

01032+6032 MLB 43 2015.858 297.7 7.53 2012 2 294.973 7.089 2.727 0.441 SPM

01057+2128 STF 88 AB 2015.833 159.0 29.69 2014 10 158.917 29.556 0.083 0.134 CPM 11

01058+0455 STF 90 AB 2015.833 83.4 32.88 2014 8 83.452 32.887 -0.052 -0.007 CPM 12

01101+5145 STT 23 AB 2015.852 190.9 14.32 2011 4 191.201 14.503 -0.301 -0.183 SPM

01103+1636 STF 94 AC 2015.852 280.8 20.24 2005 2 281.175 20.279 -0.375 -0.039 CPM

01107+6515 STI 194 2015.858 21.9 10.21 2011 2 20.387 10.636 1.513 -0.426 CPM

01129+3205 STF 98 AB 2015.833 248.0 20.00 2014 8 248.457 19.502 -0.457 0.498 CPM

01133+4426 HJ 2027 AB 2015.893 161.2 18.76 2003 6 160.789 18.203 0.411 0.557 CPM

01137+0735 STF 100 AB 2015.833 63.2 22.80 2012 10 62.971 22.752 0.229 0.048 CPM

01146+4102 AG 300 2015.882 44.8 6.58 2008 8 45.119 6.599 -0.319 -0.019 SPM

01147+4255 ARG 49 AB 2015.893 106.8 36.26 2003 6 105.753 35.328 1.047 0.932 DPM

01170+3828 STF 104 2015.852 321.6 13.33 2010 2 323.037 13.423 -1.437 -0.093 SPM

01172+6810 HJ 1075 2015.877 104.5 7.78 2010 6 103.365 7.797 1.135 -0.017 DPM

01178+4901 STF 102 AB, C 2015.882 223.8 10.08 2012 14 224.002 10.060 -0.202 0.020 CPM

01192+5821 STI1560 2015.893 324.4 13.90 2005 6 324.862 13.782 -0.462 0.118 CPM

01200+6355 STF 109 AB 2015.877 11.4 7.20 2012 4 8.911 7.254 2.489 -0.054 CPM

Table 1 (cointinued). Measurements on 141 Proper Motion Pairs





Year

Meas.


01283+5329 STF 123 AB 2015.852 162.1 16.30 2007 2 162.121 16.335 -0.021 -0.035 CPM

01326+5445 ES 2584 2015.890 196.3 15.70 2008 8 196.536 15.649 -0.236 0.051 CPM

01330+5340 HJ 2051 2015.910 75.3 23.15 2002 6 76.064 22.812 -0.764 0.342 DPM 13

01331+5416 ES 2585 2015.893 29.0 15.05 2006 6 29.782 15.037 -0.782 0.013 CPM

01332+6041 STF 131 AB 2015.877 147.7 13.35 2012 10 142.878 13.920 4.822 -0.570 CPM

01340+4559 ARG 5 2015.882 319.2 9.93 2006 8 319.825 9.930 -0.625 0.000 CPM

01348+5209 ES 759 2015.910 90.9 10.37 2008 6 92.037 10.260 -1.137 0.110 CPM

01348+6954 STF 130 2015.877 187.7 7.69 2003 10 187.098 7.608 0.602 0.081 CPM

01373+6714 HJ 1084 2015.877 358.3 15.56 2010 8 358.904 15.584 -0.604 -0.024 SPM

01409+4952 HU 531 AB, C 2015.890 280.2 6.11 2011 6 279.762 6.092 0.438 0.018 CPM

01420+5547 HJ 2066 2015.910 71.7 20.74 2005 6 72.016 20.677 -0.316 0.063 DPM 14

01431+3426 COU 668 AB 2015.910 41.0 25.36 2011 6 41.290 24.932 -0.290 0.428 SPM

01447+5607 ES 1772 AB 2015.915 107.5 24.67 2011 4 106.801 23.919 0.699 0.751 DPM

01460+6113 STF 151 2015.863 38.1 7.25 2011 2 38.015 6.814 0.085 0.436 CPM

01461+6114 STF 152 2015.863 106.3 9.28 2012 4 105.898 9.422 0.402 -0.142 SPM

01466+6116 STF 153 2015.863 69.1 7.84 2012 4 69.062 7.710 0.038 0.130 CPM

01467+3856 STF 157 AC 2015.890 115.6 12.50 2011 8 115.620 12.475 -0.020 0.025 SPM

01487+6150 HJ 1091 2015.863 151.9 28.28 2011 4 151.481 28.106 0.419 0.174 CPM

01487+7528 HJ 2075 AB 2015.863 230.8 30.73 2003 4 230.844 30.514 -0.044 0.219 CPM 15

01492+3404 STF 164 2015.890 95.4 9.81 2011 8 95.847 9.825 -0.447 -0.015 CPM 16

01493+6135 ES 1951 2015.863 158.6 6.41 2011 4 160.639 6.122 -2.039 0.288 SPM

01513+6451 STF 163 AB 2015.863 37.2 34.75 2012 4 37.073 34.167 0.127 0.583 CPM 17

01514+4329 HJ 2089 2015.890 306.1 29.07 2011 6 306.464 29.031 -0.364 0.039 CPM

01517+4549 ARG 51 2015.890 170.9 15.87 2011 6 171.825 15.839 -0.925 0.031 CPM

01527+5717 ARG 6 AB 2015.882 136.4 14.81 2003 8 136.135 14.913 0.265 -0.103 SPM

01545+5954 HDS 259 2015.893 211.8 16.79 2008 6 211.734 16.499 0.066 0.291 SPM

01561+3745 HJ 1097 2015.915 39.9 14.82 2011 3 39.796 14.645 0.104 0.175 CPM

01561+6035 AG 301 2015.863 262.3 8.60 2011 2 262.186 8.564 0.114 0.036 CPM

01567+3505 ES 2144 2015.915 143.4 6.33 2011 4 144.010 6.407 -0.610 -0.077 CPM

01595+6254 STF 188 2015.863 238.1 31.88 2011 4 237.860 31.827 0.240 0.053 SPM 18

02039+4220 STF 205 A, BC 2015.855 63.2 9.39 2013 10 61.952 9.708 1.248 -0.318 CPM

02042+5257 HJ 2104 2015.855 169.8 30.61 2003 2 168.411 30.161 1.389 0.449 SPM

02053+6740 STF 199 2015.863 22.2 35.80 2012 4 22.089 35.562 0.111 0.238 CPM 19

02078+5525 SMA 30 2015.915 327.8 11.13 2003 4 329.072 11.141 -1.272 -0.012 SPM

02091+4048 STF 215 2015.893 59.5 19.71 2011 6 60.031 19.584 -0.531 0.126 CPM

02091+4051 AG 32 AB 2015.915 99.8 21.40 2011 4 99.094 21.164 0.706 0.236 CPM 20

02094+4254 FOX 122 2015.915 5.0 17.38 2008 4 6.581 17.351 -1.581 0.029 SPM

02103+3322 STF 219 2015.855 184.6 11.40 2011 8 185.638 11.662 -1.038 -0.262 CPM 21

02109+3902 STF 222 2015.893 35.8 16.68 2013 10 36.515 16.603 -0.715 0.077 SPM

02124+3018 STF 227 2015.855 69.0 3.80 2012 10 67.422 3.871 1.578 -0.071 CPM

02149+5829 STF 230 2015.901 258.8 24.19 2011 6 259.189 23.788 -0.389 0.402 CPM

02172+3729 STF 238 AC 2015.915 355.8 10.93 2012 6 356.464 10.845 -0.664 0.085 DPM 22

02216+7212 HJ 2122 2015.904 140.1 31.51 2011 6 139.466 31.269 0.634 0.241 CPM 23

02236+7406 STF 241 2015.904 286.0 20.13 2011 6 285.018 19.989 0.982 0.141 DPM

02370+2439 STFA 5 AB 2015.849 275.0 38.00 2012 6 274.593 37.747 0.407 0.253 CPM 24

Table 1 (continued). Measurements on 141 Proper Motion Pairs




Notes:

1. The parallax of the primary is 6.72 mas ± 0.80, implying a distance of 148 pc and minimum separation of 1,241 AU. But the parallax for the companion is given as 11.46 mas ± 3.56, which is 31% of the parallax and hence not reliable as a true distance indicator. Howev-er, assuming this parallax is close to the real one, the companion would appear to be about 87 pc distant, or some 61 pc closer to earth than the companion. Proba-bly an optical system based on this.

2. Both stars have parallax values but the error estimates are too large to make them reliable as true distance indicators. However, a linear trend does appear to be forming in the data plot.

3. This pair may be starting to show a linear trend. The parallax for each star is known, but the error estimates are so large as to make the values unreliable as true distance indicators.

4. HJ 1828.0 should be given very little weight during analysis.

5. Both BAZ 1935.05 and WFC 1958.32 appear to have quadrant reversals.

6. I am not completely at ease with my measurement.

7. HJ 1828.1 should be discounted heavily during analy-sis.

8. High velocity pair.

9. Parallaxes of both stars are known, but only the prima-ry is reliable. It is given as 3.85 mas ±0.86, implying a distance of 260 pc. If both stars are at this distance, the minimum separation between the two is 1,600 AU. The parallax of the companion has an uncertainty of 70% of the parallax itself, so is not a reliable indicator. If the companion really is at the distance implied by its parallax (1.61 mas), it is some 260 pc farther away than the primary and thus the system would clearly be opti-cal.

10. Although the pair is shown as CPM, the parallaxes are nearly identical, being 11.86 mas ± 0.68 for the primary and 11.64 mas ± 0.68 for the companion. Using the mean of 11.73 mas, the system is thus 85 pc away and the stars are 512 AU apart. This system is most likely physical.

11. Like STF 88, this pair has nearly identical parallaxes (24.61 mas ± 0.76 and 23.28 mas ± 0.60). Using the mean of 23.95 mas, the pair is then about 42 pc away with the stars 686 AU apart at minimum. This pair is most likely physical.

12. Only the primary has a usable parallax (18.76 mas ± 2.76), which places it 53 pc away. If the pair is physical

(and given the companion parallax of 10.64 mas ± 10.93, this is not likely), the minimum separation would be 606 AU.

13. HJ 1831.88 should be assigned a minimal weight dur-ing analysis.

14. Starting to show a linear trend?

15. HJ 1831.84 should be given minimal weight during analysis.

16. Both Mad 1834.36 and WFD 1916.20 should be given very low weights during analysis.

17. A linear trend appears to be emerging. The parallax of the primary is given as 0.17 mas ± 0.063, a value which is on the verge of being unreliable. But assuming it is accurate, the distance to the primary is at least 5,880 pc away which would make the minimum separation of the two stars over 100,000 AU. This pair is probably optical.

18. HJ 1828 should be given minimal weight during analy-sis.

19. HJ 1828 should be given minimal weight during analy-sis. The parallax of both stars is known with good accu-racy and is almost identical. Using the mean of 7.41 mas, the distance to the system works out to 135 pc, making the stars at least 2,348 AU apart. The system is most probably physical.

20. Dob 1912.96 should be assigned a low weight during analysis.

21. The parallaxes of both stars are similar enough to sug-gest a physical system, but the uncertainty in the com-panion’s motion makes use of its parallax unreliable. Assuming the system to be at the distance suggested by the primary’s parallax, the pair is 160 pc with a mini-mum separation of 934 AU. But the uncertainty in the parallax of the primary means this analysis should be held with a healthy degree of skepticism.

22. HJ 1828 should be given minimal weight during analy-sis.

23. CLL 1980.8 appears to be a case of quadrant reversal.

24. This is a high proper motion pair, and given that the parallaxes are virtually identical (the mean being 24.24 mas), the distance to the system works out to 41 pc with the stars being at least 778 AU apart. Most likely a physical system.

25. Both stars have a parallax, but only the primary’s is reliable. Its value puts the primary at 103 pc with the pair being 1,143 AU apart. The parallax for the com-panion would imply a distance of 37 pc, so it is possible that this is an optical pair.


Year

Meas.


20585+1626 STF2738 AB 2015.816 254.0 14.80 2013 10 254.108 14.929 -0.108 -0.129 SPM

21105+2227 STF2769 AB 2015.816 299.2 18.14 2014 10 299.310 18.067 -0.110 0.073 CPM

21359+2622 HJ 1661 2015.816 84.6 11.93 2011 8 85.207 11.932 -0.607 -0.002 CPM

21390+5729 STF2816 AD 2015.808 338.4 19.80 2012 10 337.671 19.865 0.729 -0.065 CPM

21543+1943 STF2841 A, BC 2015.808 109.8 22.20 2014 10 108.235 22.200 1.565 0.000 CPM 25

22086+5917 STF2872 A, BC 2015.808 315.6 21.61 2014 10 314.825 21.528 0.775 0.082 CPM

Table 1 (conclusion). Measurements on 141 Proper Motion Pairs


Introduction

As a part of an educational course on double stars at the Army and Navy Academy in Carlsbad, Califor-nia, we obtained images for multi-star systems LEO 5 and MKT 13 in order to measure the relative positions and separations of these systems. Using the Washing-ton Double Star catalog (WDS), we chose star systems which would meet a set of criteria which would allow us to make good measurements with the equipment and tools available. These criteria included star systems with separations of 4 arc seconds or more, visual mag-nitude of 12 or brighter, and difference in visual magni-tude less than 3. Our team, shown in Figure 1, selected two candidate star systems which had not recently been measured.

Attempts were made to acquire images using an 11-inch Celestron Schmidt-Cassegrain telescope at Tierra Del Sol, near San Diego, California, but weather condi-tions prevented us from acquiring any useful images. We utilized the iTelescope network of remotely operat-ed telescopes to acquire CCD images of the candidate systems. We used the iTelescope T7 system located in Nerpio, Spain, which is a 17-inch CDK with a focal ratio of f/6.8, equipped with an SBIG STL11000M monochrome camera (Figure 2). The field of view is 28x42 arcminutes with 0.63 arcseconds per pixel scale. This telescope provided a large enough aperture to ac-quire high quality images of the 11th magnitude stars in one of the systems we chose. We chose to use a tele-scope in Spain because of the good weather available at the time of the observations.

We imaged both LEO 5 and MKT 13 on two differ-ent nights. On each night we acquired four images per system using a luminance filter and four images using a hydrogen alpha (Ha-7nm) filter. These two filters were chosen in order to ensure that we would have good measurements on the fainter stars while also ensuring that we would not have blooming problems on some of the brighter stars.

Star system LEO 5 is a triple system in the constel-lation Perseus. The AB pair of this system has not had reported observations since 2006, while the AC pair

Measurements of Multi-star Systems LEO 5 and MKT 13

Faisal AlZaben1, Allen Priest

1, Stephen Priest

1, Rex Qiu

1,

Grady Boyce2, and Pat Boyce

2

1. Army and Navy Academy, Carlsbad, California 2. Boyce Research Initiatives and Education Foundation

Abstract: We repor t measurements of the position angles and separations of two multi-star systems observed during the fall of 2015. Image data was obtained using an online 17-inch iTelescope system in Nerpio, Spain. Image data was analyzed using Maxim DL Pro 6 and Mira Pro x64 software tools at the Army and Navy Academy in Carlsbad, California. Our measure-ments of the LEO 5 system are consistent with historical data, although inconclusive as to the nature of the system. Our measurements and the historical data for the MKT 13 system show a consistent linearity in the position angle and separation.

Figure 1. Allen Priest, Stephen Priest, Faisal AlZaben, and Rex Qiu.



was last reported in 2012. The stars in the system are faint, all with visual magnitudes of about 11. The AB pair of stars in this system appear fairly close to one another with a visual separation of about 4.5 arc sec-onds. The AC pair has a separation of about 48 arc sec-onds.

Star system MKT 13 is a quintuple system in the constellation of Taurus. While there are five stars in this system, the Aa and Bb stars are each actually very close binary stars with separations of 0.1 arc seconds or less and too close for us to measure with our equip-ment. The AB pair of this system last reported observa-tions were in 2011. The AC pair was last reported in 2000. The WDS catalog reports that the A and B stars in the system have visual magnitudes of about 3.41 and 3.94 while the C star is fainter, measuring about 11.96 in magnitude. Because of the wide difference in bright-ness, we were unable to obtain measurements on the AC pair with the images we acquired. Thus, we fo-cused on measurements of the AB pair which have a visual separation of about 341 arcseconds.

Methods and Procedures

Each observation was scheduled via the iTelescope internet portal where we designated: RA & Dec coordi-nates, image time, number of images, date and time to acquire the image, and filters to be used. Once the im-ages were acquired, they were calibrated by the auto-mated iTelescope systems and made available to us

through an FTP server. The calibration procedure uti-lized dark frames, bias frames, and flat frames to cor-rect for anomalous effects of the optical system and camera used.

Pinpoint Astrometry, a plug-in for the popular Maxim DL software, was then used to obtain a plate solution for each image by locating a number of stars in the image and comparing their positions against the Fourth U.S. Naval Observatory CCD Astrograph Cata-logue (UCAC4). This procedure is crucial to determine the exact pixel scale and rotation angle of the image which are then used in determination of the star’s sepa-rations and angles. This information is placed into the FITS header for the image when saved. Even though all of our images were taken on the same telescope with the same camera, we performed this plate solving pro-cess on every image that we used to guarantee highest accuracy of our measurements. This process confirmed a pixel resolution of 0.63ʺ/pixel and a camera rotation angle of 272°.

Each WCS calibrated image was then opened with Mira Pro x64, a software product from Mirametrics, Inc. This software enables making many different pho-tometric measurements of the stars in the image includ-ing visual magnitude, absolute position in RA and Dec, and separation in arc seconds, and relative position an-gles. As we were initially unfamiliar with these star systems, it was also helpful to use star charting soft-ware such as The SkyX and Stellarium to verify the

Figure 2. T7 17-inch Planewave f/6.8 Corrected Dall-Kirkham (CDK) Astrograph in Spain.



appearance of the stars in our systems. These tools al-lowed us to visually identify the positions of the star pairs within the field of view of our images to quickly begin the process of measuring the stars’ separations.

Using the point and click Distance & Angle func-tion of Mira Pro x64, we measured the position angle and separation of the binary stars. When the first star is clicked upon, Mira calculates the centroid of the star and synchronizes the start of the measurement from that point. Releasing the mouse button on the second star allows the Mira software to locate that star’s centroid position and provide the desired measurement from these centroid positions. An example of this process is shown in Figure 3. The software calculates the centroid of each star based on the image data. In most cases, this provides a very accurate location for the star and minimizes the effects of noise. The parameters of this calculation can be adjusted if necessary to account for the size of the stars in the image. In some cases, where the star might be overexposed resulting in blooming, it is possible to disable this centroid measurement and use other methods of pinpointing a star’s location. For ex-ample, if there are diffraction spikes in the image, these can be used to locate the center of the star. However, for our images, this was not necessary, and we relied on the centroid measurement. Because this measurement is based on the brightness data for many pixels in the star image, it is possible for this centroid calculation to pinpoint a star’s location within a fraction of a pixel. This resulted in very accurate measurements even for the faintest stars.

After completion of the position angle and separa-tion measurements, the data were placed into an Excel spreadsheet to calculate the mean, standard deviation, and standard error of the mean for each binary star sys-tem. Once these were calculated, each measurement was compared to the data available in the Washington Double Star catalog (WDS). This comparison allowed us to confirm that the measurements are being made appropriately and that our data is in agreement with previously published data. If there had been an error in the processing, such as an incorrect image angle or pix-el scale, this error would show up in the comparison and let us know that there was a problem. In one case, early in the process of learning to use the Mira soft-ware, it was found that the FITS image was inverted due to an improper setting when opening the file. This gave double star angles which were obviously incorrect based on the historical measurements in the WDS. We were then able to go back to verify the mistake and to correct it.

Star System LEO 5 [WDS 02191+5422]

The AB pair required an additional effort to obtain accurate measurements because of the small ~4.5 arc second separation. Initially, this required adjustment of the contrast stretching of the image in order to identify the two stars. The default stretching performed by Mira Pro x64 caused the two stars to appear as a single star. By adjusting the amount of stretching, and viewing the image as a negative, it was fairly easy to view the 2 stars. Adjustment of the sample radius of the centroid calculation was necessary so that the centroid measure-ment accurately identified the 2 stars separately rather than combining them together as a single star.

Sixteen images were acquired of this system on 2 nights of observing, October 10th and 21st of 2015. An example image with the stars labeled is shown in Figure 4. Eight of these images were taken using the Ha filter and eight were taken with a luminance filter. Exposure times on the first observing night were varied from 60 seconds to 120 seconds. The Ha-filtered images taken on the first night were found to be under-exposed re-sulting in poor signal-to-noise ratio on 2 of the images. These 2 images were therefore discarded as no meas-urements could be obtained. On the second night of observations, the exposure times for the Ha-filtered im-ages were doubled and ranged from 120 to 240 sec-onds.

The mean, standard deviation, and the standard er-ror of the mean for the separation distance in arc sec-onds and the angle in degrees were calculated from these data as shown in Table 1. The date is the mean of


Figure 3. Example Position Angle and Separation measurement

procedure with Mira Pro.



Figure 4. Sample Image of LEO 5 with Stars Labeled.

WDS No. ID Date Obser-

vations PA Sep.

02191+5422 LEO 5AB 2015.79 14

Mean 338.53 4.18

Std Dev 1.075 0.333

Std Error 0.287 0.089

02191+5422 LEO 5AC 2015.79 14

Mean 10.07 47.95

Std Dev 0.095 0.073

Std Error 0.025 0.019

Figure 5. Graphical Representation of Historical Data Points for LEO 5 AB Pair.

Figure 6. Graphical Representation of Historical Data Points for LEO 5 AC Pair.

Table 1. Measured Data Results for LEO 5



the two observation dates.

Historical Data for LEO 5 We requested the historical data from the US Naval

Observatory. The data we received, along with our measured data, are shown graphically in Figures 5 and 6.

Discussion of Results for LEO 5 Our data agreed well with the historical data and

the calculated standard deviation indicates that our measurements were accurate. The historical trend of the measured data does not provide enough information to draw conclusions about whether these star pairs are physical doubles or not. A search of other databases did not yield any additional information about these stars.

Star System MKT13 [WDS 04287+1552]

This is a quintuple star system with each of the A and B stars being, themselves, binary pairs with known orbital data. The orbital parameters are available from the Sixth Catalog of Orbits of Visual Binary Stars. As mentioned earlier, the Aa pair and the Bb binary pairs are too close for us to separate using the observing

techniques we employed. In addition, while the A and B stars are very visible with magnitudes of 3.41 and 3.94, respectably, the C star in this system is much dim-mer with a magnitude of 11.96. Because of this large variation in visual magnitude, we were unable to meas-ure the separation and angle for the AC pair.

We were able to make 13 measurements from the images acquired. From these data, we calculated the mean, standard deviation, and the standard error of the mean for the separation distance in arc seconds and the position angle in degrees. These are shown in Table 2. The date observed is the mean of the two observation dates. There were seven and six observations on the first and second nights, respectively.

Historical Data for MKT 13 We requested the historical data from the US Naval

Observatory. The data we received are shown in Figure 7. Because of the large number of historical data points received (42), we chose to plot the angle and separation vs. observation date in order to look for trends in the data.

Discussion of Results for MKT 13 From the graphed data, there does appear to be a

trend in the position angle of this pair. A linear fit gives a trend of about 4.7 millidegrees per year with an


Figure 7. Graph of Historical Data Points for MKT 13 AB.

WDS No. ID Date Obser-

vations PA Sep.

04287+1552 MKT13AB 2015.79 13

Mean 346.72 337.97

Std Dev 0.435 3.033

Std Error 0.121 0.841

Table 2. Measured Data Results for MKT 13



R2 value of 0.54. The separation appears to be decreas-ing very slowly but a trend in this data is uncertain. A linear fit to the trend for the separation measures about 3.6 milliarcseconds per year with an R2 value of 0.04.

Acknowledgements

We would like to thank Russell Genet for his assis-tance and guidance which allowed us this opportunity to do research and for introducing our team to the study of binary stars. Additionally, we thank the Boyce Re-search Initiatives and Education Foundation (B.R.I.E.F.) for their instructional support and financial donation that allowed us to use the iTelescope robotic telescope system and the Maxim DL Pro 6 and Mira Pro x64 software tools. This research made extensive use of the Washington Double Star catalog maintained by the U.S. Naval Observatory.

References

Genet, R. M., Johnson, J. M., Buchheim, R., and Harshaw, R. 2015. Small Telescope Astronomical Research Handbook. In preparation.

Hartkopf, W.I. and Mason, B.D 2006, Sixth Catalog of Orbits of Visual Binary Stars. US Naval Observato-ry, Washington. http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/orb6

Mason, B. and Hartkopf, W. USNO CCD Astrograph Catalog (UCAC), March 2011. Astrometry Depart-ment, U.S. Naval Observatory. http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/ucac.

Mason, B. and Hartkopf, W. The Washington Double Star Catalog, October 2015. Astrometry Depart-ment, U.S. Naval Observatory. http://ad.usno.navy.mil/wds/wds.html.

Stelle Doppie Double Star Database Search Engine, http://stelledoppie.goaction.it

http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/orb6

http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/orb6

http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/ucac



http://ad.usno.navy.mil/wds/wds.html

http://ad.usno.navy.mil/wds/wds.html

http://stelledoppie.goaction.it


1. Introduction

The very wide binaries after formation are subject to dynamical process that causes their evolution. In environments with high or moderate stellar density, most pairs with separations of a few hundreds to a few thousands AU are disintegrated (that is, disrupted) within a few million years (Parker et al. 2009). In the stars field, outside of these high density environments, Galactic tides and weak interactions with passing stars disrupt binary stars with separations of a few times 10,000 AU on a time scale of about 10 Gyr (Heggie 1975; Weinberg et al. 1987).

Recently, astronomers discovered that stars of dis-rupted binaries don’t quickly leave the binary environ-ment but escaping stars drift apart with low relative velocity and remain within the Jaboci radius during millions or tens of millions of years.

In order to study the process of dissociation of very wide systems, Poveda et al. (2009) presented the very wide and nearby system GJ 282 AB–NLTT 18149 as the most interesting object in his very wide common

proper motion binary search. GJ 282 AB is a wide pair (~58 arcsec) composed by two red stars of 7.20 and 8.87 magnitudes at 14.2 pc of distance. The high com-mon proper motion, common radial velocity, and com-mon age strongly suggest a bound nature for AB.

NLTT 18149 (= Giclas 112-29) is a red dwarf star located at 1.09 deg (0.27 pc) of separation to GJ 282 AB. Its common distance, common age, common prop-er motion, common radial velocity to GJ 282 AB strongly suggest possible physical relation. Poveda et al. (2009) concluded that the system GJ 282 AB–NLTT 18149 is in the process of dynamical disintegration. The large physical separation of very wide binaries such as these is larger than the isolate stars formation regions. Astronomers think that these systems can only form during the dissolution phase of open clusters of low density (Kouwenhoven et al. 2010).

The main objective of this work is to confirm the bound status of GJ 282 AB and the dynamical disinte-gration status of GJ 282 AB–NLTT 18149.

The organization of this paper is as follows. In Sec-tion 2, we detail the characteristic of the AB pair, the

GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System in Process of

Dissociation

F. M. Rica

1, R. Benavides

2

1 Astronomical Federation of Extremadura, C/José Ruíz Azorín, 14, 4º D, Mérida E-06800, Spain

email: [email protected] 2 Astronomical Observatory of Posadas ( J53 MPC code), Posadas E-14730, Spain

Abstract: Very wide binar ies are interesting objects that shed light on the binary for -mation process and their dynamical evolution. Poveda et al. (2009) studied the possible physical relation of the near (14.2 pc) and wide (~58”) binary star GJ 282 AB and the extremely wide (1.09º; ~55,000 AU) companion, NLTT 18149, and they concluded that this very wide system is in the process of dynamical disintegration. In this work, we confirm the same conclusion but using a different method. We first study dynamically GJ 282 AB, confirmed that it is a bound system and then we determine possible orbital solutions. Later, we calculate the relative velocity of NLTT 18149 with respect to the GJ 282 AB’s center mass using their (U, V, W) galactocen-tric velocity. The relative velocity, V rel = 1.98 ± 0.16 km s-1, is much larger than the escape ve-

locity (0.25 ± 0.01 km s-1). Therefore, with a significance level of 11, we also conclude that this very wide system is in a process of dynamical disintegration.


GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System …

new astrometric measures performed, the dynamic study and the orbital calculation. In Section 3, we pre-sent the very wide component, the calculus of the char-acteristics of the mass center and the study of the possi-ble physical relation of C with respect to AB.

2. The Close System GJ 282 AB

S. van den Bergh in 1949 discovered, using the photographic technique with astrograph, two red stars with high common proper motions. This object was catalogued as GJ 282 AB, a wide pair (~58 arcsec, 825 UA) listed as WDS 07400-0336 AB ( = BGH 3 AB) in the Washington Double Star Catalog (hereafter WDS). It is composed of two young stars of 7.20 (K2V) and 8.87 (K6/7V) magnitudes at 14.2 pc of distance The high common proper motion, common radial velocity, and common age strongly suggest a bound nature for AB.

To confirm this bound status, we study the relative motion of B component with respect to A by weighted

linear fits using d/dt, d/dt, dx/dt, and dy/dt plots (see Figures 1 and 2). The WDS catalog lists 27 astrometric measures from 1890 to 2003 and was kindly provided by Brian Mason. We assign initial weights for astromet-ric measures using a data-weighting scheme and pro-cess based on Rica et al. (2012).

To confirm the bound status, we study the relative motion of B component with respect to A by weighted

linear fits using d/dt, d/dt, dx/dt, and dy/dt plots (see Figures 1 and 2). The WDS catalog lists 27 astrometric measures from 1890 to 2003 and was kindly provided by Brian Mason. We assign initial weights for astromet-ric measures using a data-weighting scheme and pro-cess based on Rica et al. (2012).

In this work, we add two more astrometric measures to the WDS for epochs 2010.5589 and 2014.131 using the catalogs WISE and URAT1 (Zacharias et al. 2015). In addition to this, Rafael Be-navides used a f/10 Celestron telescope of 0.3 m with a ASCOM QHY9 CCD camera, to take 5 CCD images of 0.6 seconds of exposition on 2015 February 8th. The telescope is located at the Posadas Observatory (Córdoba, Spain) with the MPC code J53. The pixel

size of the camera was of 5.4 m (0.86" in the focal plane). We use Astrometrica 4.8.2 for the calibration and astrometric process.

All the astrometric measures, with a time baseline of 125 years, are listed in Table 1. This table lists, from the left to right, the observational epoch, the position angle (2000 equinox), and distance as listed in WDS in the three first columns. The number of nights (N), the reference (as used in WDS), the aperture of the tele-scope (in meters), the observational technique (as listed

in WDS), the weights assigned to and , and the O – C residuals are also listed.

The United State Naval Observatory (USNO) per-

Figure 1. Historical position angle, of GJ 282 AB and its evo-lution with time. We determined a very significant change of +0.0090 ± 0.0004 deg yr-1

Figure 2. Historical distance, of GJ 282 AB and its evolution with time. We determined a change of -0.0021 ± 0.0005 arcsec yr-1.



Date º " N Ref. Ap Tec w w O-C° O-C"

1890.600 112.1 57.623 2 WFD1906b 0.2 T 0 9 1.10 -0.49

1893.200 111.0 57.963 1 WFC1998 0.3 Pa 20 22 -0.04 -0.14

1894.180 110.7 57.799 1 WFC1998 0.3 Pa 20 22 -0.35 -0.30

1903.500 111.8 59.240 4 WFD1940 0.2 T 3 0 0.62 1.16

1933.500 111.6 57.654 1 WFC1945b 0.1 Pa 20 22 0.00 -0.37

1946.000 112.2 58.200 1 Bgh1958 0.1 Pa 20 32 0.42 0.21

1968.650 112.1 57.943 4 WFC1992 0.2 Pa 79 86 0.01 -0.01

1970.235 112.1 57.943 1 USN1974 0.7 Po 6596 16020 0.00 0.00

1970.238 112.1 57.935 1 USN1974 0.7 Po 6596 16020 0.00 -0.01

1970.915 112.1 57.957 1 USN1974 0.7 Po 6596 16020 -0.01 0.01

1971.174 112.1 57.943 1 USN1974 0.7 Po 6596 16020 0.01 0.00

1971.185 112.1 57.947 1 USN1974 0.7 Po 6596 16020 0.00 0.00

1971.185 112.1 57.940 1 USN1974 0.7 Po 6596 16020 -0.01 0.00

1975.876 112.2 57.919 1 USN1978 0.7 Po 3298 8010 -0.02 -0.01

1975.876 112.2 57.917 1 USN1978 0.7 Po 6596 8010 -0.01 -0.02

1976.092 112.2 57.932 1 USN1978 0.7 Po 6596 16020 0.00 0.00

1976.155 112.2 57.946 1 USN1978 0.7 Po 6596 16020 -0.01 0.01

1976.155 112.2 57.928 1 USN1978 0.7 Po 6596 16020 0.00 0.00

1976.158 112.2 57.928 1 USN1978 0.7 Po 6596 16020 0.00 0.00

1976.158 112.2 57.933 1 USN1978 0.7 Po 6596 16020 0.01 0.00

1981.200 112.3 58.011 2 WFC1999 0.2 Pa 56 61 0.03 0.09

1985.960 112.6 58.105 4 WFC1994 0.2 Pa 79 86 0.26 0.19

1987.800 112.8 58.340 4 WFD1985 0.2 T 6 6 0.44 0.43

1991.850 112.5 57.920 1 TYC2002 0.3 Ht 79 86 0.08 0.02

1998.860 112.7 57.960 1 TMA2003 1.3 E2 99 108 0.18 0.07

2000.102 112.6 57.974 6 UC_2013b 0.2 Eu 40 43 0.07 0.09

2003.068 113.0 58.260 1 Arn2003e 0.2 Mg 3 2 0.43 0.38

2010.559 112.7 57.710 1 WISE 0.4 Hw 123 123 0.02 -0.15

2014.131 112.7 57.900 1 URAT1 0.2 E 1111 1111 0.01 0.05

2015.108 112.79 57.85 1 Benavides 0.3 C 400 400 0.12 0.00

Table 1. Astrometric data, weights and residuals for the linear trend of GJ 282 AB



formed a very accurate series (root mean square, RMS, of ~0.01º and ~0.01” for position angles and distances) of astrometric measures using the Alvan Clark 0.7 m refractor telescope. For the observing condition, the correction of relative astrometry for atmospheric refrac-tion is negligible for position angle (< 0.01º) but signif-icant (+0.02”) for the USNO distances. We correct for atmospheric refraction in the USNO distances.

Our dynamic study shows that the angular separa-tion decreases about 2.06 ± 0.51 mas yr-1 while the po-sition angle clearly increases 0.0090 ± 0.0004 deg yr-1. The total relative motion (9.3 ± 0.5 mas yr-1) has a sig-

nificance of 13, therefore we can reject the non-motion hypothesis. The positional, dynamical, and kin-ematical parameters for the linear fit are shown in Table 2. The RMS of this fit is 0.02º and 0.013” and the mean absolute, MA, 0.01º and 0.007”. The RMS gives the mean spread of the measures with respect to the mean.

And the MA gives the uncertainty of the near future ephemerids. The adopted values for the stellar masses are 0.80 and 0.65 solar mass.

The total relative velocity of B with respect to A is 0.67 ± 0.04 km s-1 much smaller than the upper limit of the escape velocity (1.74 ± 0.05 km s-1). By using the work of Winsberg et al. (1987) about dynamic evolu-tion, we can conclude that GJ 282 AB is immune to external perturbations (gravitational binding energy of -8.8 x 10-42 ergs) and that is a high common proper mo-tion, common distance, common age binary, composed by stars gravitationally bound.

We determined orbital solutions for GJ 282 AB using the method of orbital calculation presented by Hauser & Marcy (1999). This method only needs in-stant position (x, y, z) and velocity vectors (Vx, Vy, Vz) in addition to a parallax and stellar masses to obtain a family of orbits depending on z (the line-of-sight posi-tion of the component). The input parameters are those of Table 2. The only unknown input data is the z pa-rameter. We constrained the value of z following the procedure in Hauser & Marcy (1999) and one orbit for each value of z is obtained.

We study the empirical distribution of r (in arcsec-

ond) as a function of . For this task, we select about 300 grade 1-2 orbital solutions from the Sixth Catalog of Orbits of Visual Binary (Hartkopf & Mason 2003),

calculate the ephemerides for and r for different

epochs. The comparison between and r give us the distribution of r as a function of s. We see that the val-

ues for r/ are highly dependent on the orbital inclina-tion (see Figure 3). For highly-inclined orbits, the 3D effect is greater and therefore we could find r-values

much greater than . Figure 4 shows the cumulative distribution.

Table 3 shows same numbers (quartiles, percen-

tiles, mean, median, etc.) about the distribution of r/.

The median happens for r/= 1.11 (that is, 50% of pos-

sible orbital solutions have values of r/ from 1.0 to 1.11). If we center over the median, 50% of the orbital solutions ranges from 1.02 to 1.38 (from 1.00 to 1.38 for the 75% of the possible orbital solutions). Finally,

the 90% of possible orbital solutions have r/ ≤ 2.0 ap-proximately. Only the high-inclined orbits have greater


Mean Epoch 1990.000

(deg) for mean epoch 112.445 ± 0.007

(arcsec) for mean epoch 57.904 ± 0.009

x (AU) [East-West] +763 ± 14

y (AU) [North-South] -315 ± 6

d/dt (mas yr-1) -2.06 ± 0.51

d/dt (deg yr-1) +0.0090 ± 0.0004

dx/dt (mas yr-1) -5.31 ± 0.53

dy/dt (mas yr-1) -7.65 ± 0.41

Vx (km s-1) [East-West] -0.36 ± 0.04

Vy (AU) [North-South] -0.52 ± 0.03

Vz (km s-1), radial velocity -0.1 ± 0.2

Vtot (km s-1) 0.67 ± 0.04

Vesc_max (km s-1) 1.74 ± 0.05

Mass of A (Msun) 0.80 ± 0.05

Mass of B (Msun) 0.65 ± 0.05

Distance (pc) 14.3 ± 0.3

Table 2. Positional, Dynamical, and Kinematic Parame-ters for GJ 282 AB.

Name Mean Minimum Maximum Q10 Quartile1 Median Quartile3 Q90

r/ 1.40 1.00 17.14 1.00 1.02 1.11 1.38 1.96

Table 3. Statistics for the r/ Distribution



Figure 3. The relation of r/ with the orbital inclination (in degrees).

Figure 4. Cumulative distribution of r/s in AU (or r/ in arcseconds).



values. The maximum value is 17.14. Table 4 lists orbital solutions for different values of

the radius-vector (r) chosen in function of the empirical

distribution of r (in arcsecond) in function of . An or-bital solution for the minimum value of the radius-vector, r = s (that is z = 0 AU) is shown. In the 50th percentile of the distribution of r in function of s, r = 1.11s (z = ± 396 UA) and in the 75th percentile, r = 1.38s (z = ± 783 UA) two orbital solutions. Therefore, in this table is represented the 75% range of possible orbital solutions.

Figure 5 shows orbital solutions for the AB compo-nents calculated in this work. The thick black ellipse is the orbital solution for z = +396 UA (when r = 1.11 s, the median value) while the dash ellipse is for z = -396 UA. The legends in the inner box are self-explicative. The possible regions (“zone possible” in the inner box) of possible orbital solutions cover the 90% of the confi-dence interval for z parameter.

3. The Very Wide Companion NLTT 18149

Giclas 112-29 (= NLTT 18149) is a red dwarf (M1.5V) star located at 1.09 deg of separation to GJ 282 AB. Its common distance, common age, common proper motion, and common radial velocity to GJ 282 AB strongly suggest a possible physical relation: It is not listed in WDS. Poveda et al. (2009) concluded that the system GJ 282 AB–NLTT 18149 is in the process of dynamical disintegration. They determined that the perspective effect for the wide pair and the orbital mo-tion of GJ 282 AB cannot explain the large differ-ence in proper motion between GJ 282 and NLTT 18149.

In this work, we want to confirm the dynamical disintegration status of GJ 282 AB–NLTT 18149 by the

study of the relative velocity of NLTT 18149 with re-spect to the center of mass of GJ 282 AB (CMAB).

To determine the properties (AR and DEC, proper motion and radial velocity) for CMAB, we assign weights to the A and B members in function of the stel-lar masses, as in Kiselev, Romanenko & Gorynya (2009). The values for the weights are pA = 0.55 and pB = 0.45 for A and B components respectively. The adopted values for the stellar masses are 0.80 and 0.65 solar mass for A and B components.

In 1991.25, the CMAB has an offset of 23.42” East and 9.66” South to GJ 282 A. To obtain the (AR, DEC) coordinate for CMAB in this epoch, we use the Hippar-cos coordinate for GJ 282 A and the offset determined previously. For the proper motion and radial velocity of CMAB, we calculate the weighted mean of the values for A and B using the weights pA and pB. We assume that the CMAB is at the same distance that the A compo-nent.

The (U, V, W) galactocentric velocities were calcu-lated following the work of Przybylski (1962). We cal-culate the relative velocity of NLTT 18149 with respect to the CMAB from the difference of their (U, V, W) ve-locities:

The positional, kinematical, and dynamical data of the stellar components and the CMAB are listed in Table 5. The relative velocity (V rel) obtained using formula (1) is 1.98 ± 0.16 km s-1. We determined the errors us-ing a Monte Carlo approach with Gaussian errors for the input data.

From the Tycho-2, 2MASS and URAT1 AR and DEC coordinates of the three components, we deter-mine the relative position of C with respect to CMAB:



Table 4. Computed Orbital Parameters

2 2 2

rel

C CMab C CMab C CMab

V

U U V V W W

(1)

COMPUTED ORBITAL PARAMETERS FOR WDS 07400-0336 = BGH 3 AB

WITH r = s r = 1.11 s and r = 1.38 s

Parameter -783 AU -396 AU 0 AU +396 AU +783 AU

P (yr) 15000 10172 8493 10172 15000

T (yr) 9259 6728 5776 6365 8274

e 0.651 0.724 0.761 0.742 0.681

a (arcsec) 48.4 37.4 33.2 37.4 48.4

a (AU) 688.4 531.3 471.2 531.3 688.4

i (deg) 45.7 29.0 9.4 25.8 43.6

(deg) 72.8 60.6 355.9 270.2 260.0

(deg) -135.6 -127.8 -67.6 15.9 25.6

q (AU) 240.18 146.52 112.74 136.93 219.31



Figure 5 Orbital solutions for the AB components calculated in this work. The legends in the inner box are self-explanatory. The possible regions (“zone possible” in the inner box) of possible orbital solutions cover the 90% if the confidence interval for z parameter.

A Component B Component CMAB C Component

2000 for 1991.25 07h 39m 59.29s ... 07h 40m 00.85s 07 36 07.06

2000 for 1991.25 -03º 35' 48.6" ... -03º 35' 58.26" -03 06 36.6

(mas yr-1) 2) +71.7 ± 1.2 +66.8 ± 1.3 +69.5 ± 0.9 +36.3 ± 1.6

(mas yr-1) 2) -276.1 ± 1.3 -286.2 ± 1.4 -280.5 ± 1.0 -253.5 ± 0.8

Vrad (km s-1) 1) -21.8 ± 0.2 -22.0 ± 0.2 -21.9 ± 0.2 -22.7 ± 0.2

Parallax (mas) 3) 70.37 ± 0.64 ... 70.37 ± 0.64 70.55 ± 1.64

U (km s-1) ... ... +28.12 ± 0.15 +27.59 ± 0.15

V (km s-1) ... ... +0.13 ± 0.13 +1.28 ± 0.13

W (km s-1) ... ... -8.22 ± 0.03 -9.34 ± 0.03

1) Poveda et al. (2009); 2) Tycho-2 catalog; 3) Hipparcos

Table 5. Data for the Stellar Components and the CMAB



Tycho-2: 296.649 ± 0.001º and 3899.61 ± 04” (1991.78) 2MASS: 296.652 ± 0.001º and 3899.81 ± 0.08” (1998.865) URAT1: 296.650 ± 0.001º and 3899.88 ± 0.06” (2014.05)

The errors in the relative measures were determined

using the (AR, DEC) astrometry uncertainties listed in the Tycho-2, 2MASS and URAT1 catalogs. At the dis-tance of this system, the angular separation corresponds to a projected physical separation (s) of 55,345 UA (= 0.268 pc). So s is the lower limit of radius-vector (r) which allows us to calculate an upper limit for the es-cape velocity (V esc_max) of 0.25 ± 0.01 km s-1.

The binding energy for GJ 282 AB–NLTT 18149 is -2.0x1041 ergius and in the Fig. 15 and 16 of Close et al. (2007) we can see that there is no binary with such as low binding energy. And in his Fig. 17, our very wide system is located in the “field unstable” region. Wein-berg, Shapiro and Wasserman (1987) studied the dy-namical evolution and survival probability of very wide binaries. GJ 282 AB–NLTT 18149 has a binding ener-gy between the curves for ao = 0.063 pc (-2.7x1041 er-gius) and ao = 0.16 pc (-1.1x1041 ergius) in their Fig. 6, therefore the probability of survival at the age of the system (300-500 Myr) is about 80%.

But our result shows that V rel > Vesc_max with a sig-

nificance of nearly 11. Trigonometric parallax listed in Hipparcos catalog for the A and C components yield greater values for r and therefore smaller values for V esc reinforcing our conclusion. Our result confirms that GJ 282 AB–NLTT 18149 is in the process of gravitational

dissociation with significance of at least 11.

Acknowledgements

This publication makes use of data products from the Wide-field Infrared Survey Explorer (WSIE), which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aero-nautics and Space Administration.

This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Ob-servatory and the Simbad database operated at CDS,

Strasbourg, France.

References

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Gaidos E. et al., 2014, MNRAS, 443, 2561

Hartkopf W. I., Mason B. D., 2003, Sixth Catalog of Orbits of Visual Binary Stars, U.S. Naval Observa-tory, Washington, http://ad.usno.navy.mil/wds/orb6.html

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Zacharias, N. et al., 2015, AJ, 150, 101



Opportunities for Student Astronomical Research in Southern California Workshop on Sunday, June 12, 2016

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Meet and Greet -- 11:00 to 12:30

No host brunch gathering at the Fox Sports Grill at the Hilton

Meeting -- 12:30 to 5:00 in the Cobalt Room Here are some of our experienced speakers and the topics we will cover:

Dr. Russ Genet, past President of the Astronomy Society of the Pacific Bob Buchheim, President of the Society for Astronomical Sciences (SAS) Dr. John Kenney, Chair of the Astronomy and Physics Department of Concordia University and more to be announced at our website soon.

Overview of small telescope research opportunities for amateurs, professionals and students The Astronomy Research Seminar - its importance, history and future as a key STEM component The astronomy community and its connections to SAS, AAVSO, schools and universities How to publish your seminar student research through InStAR and Collins Foundation Press InStAR and BRIEF resources provided for schools, instructors and students nationwide Student experiences and outcomes - lessons learned and impact on their careers Expansion of the astronomy community, seminar, resources and research areas Q&A - How to start the seminar at your school and tailor it to your school's needs and programs

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Small Telescope Research Communities of Practice

American Astronomical Society’s 228th Meeting, Hilton Bayfront, San Diego, California Meeting-in-a-Meeting Special Sessions, Monday/Tuesday June 13/14, 2016 Discussions Moderator: Virginia Trimble, University of California, Irvine

Organizer: Russell Genet, California Polytechnic State University [email protected] (805) 438-3305

This Meeting-in-a-Meeting consists of three 90-minute special invited-talk sessions and a contributed poster session on a common topic: small telescope research communities of practice. Talks and posters in special sessions do not count against presenters as their regular meeting presentation.

Three 90-minute Oral Sessions

I. Pro-Am Communities of Practice Monday, 13 June,10:00am-11:30am

Communities of practice are natural, usually informal groups of people that work together. Experienced members teach new members the “ropes.” This vital human activity has been studied in depth by social learning theorists such as Etienne Wenger, whose 1998 book, Communities of Practice: Learning, Meaning, and Identity, defined the field. As Wenger suggested in his classic book, “Learning is a matter of engagement: it depends on opportunities to contribute actively to the practices of communities that we value and that value us, to integrate their enterprises into our understanding of the world, and to make creative use of their respective repertoires.” There are, in astronomy, many communities of practice. Some communities are centered on observing faint objects with large telescopes and analyzing the results. These communities, led by seasoned astronomers, include graduate students and post-docs who are learning the ropes. Other astronomical communities of practice are centered on observing brighter objects with smaller telescopes. These communities often stress professional-amateur (pro-am) cooperative research. They take advantage of the large number of smaller telescopes and ob-servers. Examples of such pro-am communities of practice include variable star observers (ably organized by the American Association of Variable Star Observers), and a wide range of pro-am research fostered by the Society for Astronomical Sciences

Speakers Russ Genet, California Polytechnic State University: Introduction to Pro-Am and Student-Centered Astronomical

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search

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For students who would like to become scientists, joining a community of practice early in their educa-tional career is beneficial. A number colleges and universities offer well-developed undergraduate astronomical research programs. There are also a number of summer research programs for undergraduate astronomy students, such as the NSF-sponsored Research Experience for Undergraduates (REU). High school students are also participating in organized, student-centered astronomical research programs. A good example is the now decade-long Astronomy Research Seminar offered by Cuesta College in San Luis Obispo, California. Well over 100 stu-dents, composed primarily of high school juniors and seniors, have been coauthors of several dozen published papers. Being published researchers has frequently boosted these students’ educational careers with admissions to choice schools, often with scholarships. This seminar was recently expanded to serve multiple schools with a vol-unteer assistant instructor at each school. The students meet regularly with their assistant instructor and also meet online with other teams and the seminar’s overall instructor. This seminar features a textbook, self-paced learning units, and a website sponsored by the Institute for Student Astronomical Research. Each team is required to plan a project, obtain observations (either locally or via a remote robotic telescope), analyze their data, write a paper, submit it for external review and publication, and present their results.


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Community College Students Pat Boyce and Grady Boyce, Boyce Research Initiative: High School Astronomical Research at the Army and

Navy Academy

Round-Table Discussion by the Speakers Moderator, Jolyon Johnson, University of Washington

III. Research Areas Suitable for Small Telescopes Tuesday, 14 June, 10:00am-11:30am

Advances in low cost but increasingly powerful instrumentation, computers, and software have greatly in-creased the capabilities of smaller telescopes. Close visual binary star astronomy provides a good example of how such advances have allowed observers, at very low cost, to obtain outstanding results. Visual double stars with separations below the seeing limit typically require speckle interferometry observations with high-speed, low-noise, electron-multiplying emCCD cameras costing well over $10,000. Recently, however, low-noise CMOS cameras (such as the ZWO ASI290MM) have become available which cost under $1000 and perform nearly as well. There are many other areas that are well suited to smaller telescope research, including time series photometry of eclipsing binaries, variable stars, exoplanet transits, and asteroids, not to mention asteroid and lunar occultations, as well as stellar polarimetry. Low resolution spectroscopy on smaller telescopes works well for both stellar spectral classifica-tion and following variable stars. These many research areas have not only benefited from camera and computer ad-vances, but increasingly from the automation of smaller telescopes and observatories.

Speakers David Rowe, PlaneWave Instruments: Advances in Small-Telescope Speckle Interferometry Dominic Ludovic, University of Iowa: A Low Cost Grism Spectrometer for Small Telescopes Virginia Trimble, University of California, Irvine: Second to Last Thoughts

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Special Small Telescope Research Communities of Practice Poster Session

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The SAS Program Committee invites you to participate in the Society for Astronomical Sciences’ 35th Annual Symposium. This is the premier annual conference devoted to small-telescope astronomical science.

The SAS Symposium brings together amateur astronomers who are engaged in scientific research, professional astronomers, and students for in-depth discussions of small-telescope research results. It is an excellent venue for highlighting results, discussing targets of observational campaigns, developing collaborations, and bringing to-gether the community of practice to share expertise and experience. You need not be an expert to benefit from participating in SAS: one goal of SAS is to provide a mentoring environment where you will learn how you can contribute to astronomical science.

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Documents

Journal of Double Star Observations V5, No4GJ 282 AB (WDS 07400-0336 AB = BGH 3 AB) and GICLAS 112-29: A Very Wide System in Process of Dissociation F. M. Rica and R. Benavides 406