Decade of pulsar Decade of pulsar observations in Pushchino observations in Pushchino

and Kalyazin Radio and Kalyazin Radio Astronomy observatoryAstronomy observatory..

V.A.Potapov, P.N.Lebedev Physical Institute of RAS, Pushchino Radio Astronomy Observatory, Pulsar Astrometry Dept.

The persons took part in this work.

• PRAO ASC LPI– Yu.Ilyasov; O.Doroshenko; V.Oreshko; A.Rodin;

M.Pshirkov, E.Zmeeva

• ASC LPI – M.Popov; V.Soglasnov

• KSRC NICT (Japan)– Yu.Hanado; M.Sekido; M.Imae; T.Kondo; S.Tekefuji

• MSU– N.Korotkova

Contents

• Pulsar timing at Kalyazin in 1997 - 2007.• Pulsar VLBI at Kalyazin.• Giant Pulses observations at Kalyzin and

Pushchino.

PULSAR TIMING AT KALYAZIN IN 1997 – 2007.

Historical overview

• 1995 – testing of 0.6 GHz pulsar timing system at 22 m radio-telescope (RT-22) in Pushchino.

• 1995 – 1996 – First timing observations at 0.6 GHz at Bear Lakes 64-m radio telescope

• 1997 – 2007 – Timing observations at 0.6 and 1.4 GHz in Kalyazin 64-m radio telescope (RT-64).

• 2007 - … - Elaboration of the new generation digital multi-frequency (0.6, 1.4, 1.6, 2.2 GHz) pulsar timing system for Kalyazin

Kalyazin 64-m radio telescope

Kalyazin 64-m radio telescope

Coordinates 57°13`22.8587 `` N.L.; 37° 54` 01.1533`` E.L.; h =178.079 m. Х=2731190.445; У=2126198.279 ; Z=5339535.645 m

Main reflector 64 m

Main reflector RMS 1.1 mm

Minimal wavelength 1.35 cm

Secondary reflector 6 m

Antenna efficiency 0.5 – 0.6

Receiving system Multi-frequency horn d=2m, l=6m

Polarizations RCP, LCP

Simultaneously used frequencies

0.6; 1.4; 2.3; 8.3 GHz or0.6; 1.7; 2.3; 4.8; 22 GHz

Guidance speed Fast - 1° / s; slow – 1.5` / s

RT-64 receivers (2007 yr. status)

System PR-0.6 PR-1.4 PR-2.2 PR-8.3

Freq. GHz 0.596-0.604 1.35-1.45 2,07-2,32 7.80-8.70

Heterodyne freq. GHz

562.0; 563.6 1590.0 2020,0 8080.0

Int. freq. MHz 38 175 230 300

T receiver, K 40 25 12 14

Antenna efficiency

0.53 0.5 0.55 0.3

“Analogue generation” Pulsar observation systems used in Kalyzin (till 2007).

1. AS-600/160: ~600 MHz; BW 2x3.2 MHz, (80x2x40KHz channels), τ=10 μs.

2. AS-1400/256: ~1400 MHz; 2x32 MHz (128x2x250 kHz) , τ<=4 μs.

3. AOP-1400: ~1400-1600 MHz; BW ~200 MHz (500x40kHz), τ<=4 μs.

AS-1400/256

AS-600/160

AOP-1400

AS-600/160, observer’s interface

AS-1400/256, observer’s interface

Data processing• Integration of pulsar profile and calculation

of topocentric TOAs: – kkfs1,2,3 packages (Doroshenko, Potapov, 1998-

2007)– iPulsar package with an extended possibility of

noise filtering in time/frequency domains (PA Dept., 2008)

• Barycentric TOAs and pulsar parameters calculations– TIMAPRv1,v2 (Doroshenko, Kopeikin, 1990-

2009)

Scientific goals

• Building ensemble PT and BPT scales.

• Investigation of the low-frequency noise in pulsar TOA residuals (search for the low-frequency gravitational waves background – GWB, in particular)

• Investigations of long-term ISM perturbations.

Long-term timing of millisecond pulsars at 600 MHz in 1997-2007

J0613-0200, J1012+5307, J1022+1001, J1640+2224, J1643-1224, J1713+0747, B1937+21, J2145-0750

Position of 8 Kalyazin millisecond pulsars (bold points) between about 40 millisecond pulsars with regular timing.

Pulsar time stability investigations, σz statistics

Sloped lines correspond to the energy density of GWB from the early Universe ( S(f) ~ 1/f ⁵ )

Pulsar time stability investigations, σz

statistics

Approaches to the ensemble PT, weighted average.

6 Kalyazin pulsars EPT synthesis. PTS package used (Pshirkov, Korotkova, 2010)

Approaches to the ensemble PT, weighted average.

6 Kalyazin pulsars EPT. Res weighing 30 days averaged.

Approaches to the ensemble PT, weighted average and Wiener filtering.

(Rodin, 2010)

Approaches to the ensemble PT, weighted average and Wiener filtering.

Dashed line - 6 pulsars, weighted average (residuals),Points – 3 pulsars, weighted average (residuals, J0613-02, J1640+22,J1713+07)Line – 6 pulsars, Wiener filtering (Rodin, 2011)

Approaches to BPT and ultra-low frequency GWB.

(Ilyasov, Kopeikin, Rodin, 1998)

• Pulsar time- PT•Binary pulsar time - BPT•Time terrestrial – TT•Barycentric time - BT

Approaches to BPT and ultra-low frequency GWB.

Ultra-low frequency GWB limiting.

(Kopeikin, 1997, Kopeikin & Potapov, 2004)

Summary on relic GWB energy density Ωgh² limiting using Kalyazin pulsar timing data.

• <= 10⁻⁷ in f ~ 6x10 ⁻⁹ Hz, straight σz

analysis (Potapov, 2004)

• ~ 10⁻⁸ in f ~ 6x10 ⁻⁹ Hz, using correlation functions of 6 pulsars TOAs with SSA “Caterpillar” method (Rodin, 2011)

• <= 4x10⁻⁴ in f ~ 10 ⁻¹¹ - 7.1x10⁻⁷ Hz (J1640+22 binary parameters analysis, Potapov, 2004)

Two frequency observations at of PSR B1937+21 – discovery of secular DM variation.

KK – Kalyazin (0.6 GHz) – Kashima (2.15 GHz) observations, KA – Kalyazin 0.6 – 1.4 GHz observations.d(DM)/dt= - 0.00114(1) pc ∙ cm⁻³ in 1984 – 2004 (Ilyasov et al. 2004)

Prospects for future timing in Kalyazin.

Digital FFT pulsar processors one module test at 1.4 GHz (BW = 50 MHz, 512 channels, 3 min integration), PSR B1937+21 and J1713+0747

160507_B1937+21_10 SNR=22.8

Время в миллисекундах10

Мощ

ност

ь

1.003

1.003

1.002

1.002

1.001

1.001

1

1

170507_J1713+0747_03 SNR=4.8

Время в миллисекундах43210

Мощ

ност

ь

1.001

1.001

1.001

1.001

1

1

1

1

1

1

1

Prospects for future timing in Kalyazin 2011 ~ .

• Digital FFT pulsar processors– 80 MHz BW in 256 chan. at 0.6 GHz with

τ<=3μs– Up to 200 MHz BW in 1024 chan. at 1.4 or 1.6

GHz with τ<=1μs– 200+ MHz BW in 1024 chan. at 2.2 GHz with

τ<=1μs

• Regular timing >~ 20 binary millisecond pulsars of northern hemisphere in about 1 session/(10-15) days in 2 – 3 frequencies.

PULSAR VLBI AT KALYAZIN

Kalyazin VLBI system (2007 yr.)

K-5 registrator

S2 registrator

Video converter 16 х 4 MHz

K-4 frequency synthesizer

16 1

Time service

Meteo

GPS 0,6 GHz 1,4 GHz 2,2 GHz

RT-64 receivers Phase calibr.

1 Hz

5 MHz

GPS TEC-meter

8,3 GHz

Data General Data General Data GeneralData General

16 1

Amplifier of int. frequency

S2 Video converter

(DAS)

Coordinates and proper motion

detection on the base Kalyazin – Kashima (Japan)

Sekido et al., 1998

Coordinates and proper motion detection on the base Kalyazin - Kashima

Sekido et al., 1998

DE200 – ICRF frame connection.

Rotation axes Rodin, Sekido 2002 pulsar VLBI

(mas)

Bartel et al., 1985LLR and quasar VLBI observations(mas)

X -4±2 -2±2

Y -13±3 -12±3

Z -17±5 -6±3

VLBI observations of pulsars B0329+54, B0355+54, B0950+08, B1933+16, B2021+51 were used.

Prospects of Space-Earth pulsar VLBI in “RadioAstron” space radio telescope project.

• Kalyazin RT-64 will be used as a one of the Earth VLBI station.

• Space radio telescope with 10-m diameter and 300000 km in apogee may provide sub - 0.1 mas accuracy of point object coordinate in ICRF.

• In space RT – one Earth RT-64 configuration up to 22 pulsars with flux 13 < S < 1100 mJy may be observed at 1.6 GHz.

• In full configuration (Earth telescopes equivalent to the one 130 m diameter radio telescope) up to 56 pulsars with 7 < S < 1100 mJy.

• The launch is planned in the 3th decade of July 2011.

• As much as 3-4 pulsars are to be observed in the early observation program.

List of pulsars – candidates for the Space-Earth VLBI.

-------------------------------------------------------------------------------------------------------------------------# NAME PSRJ RAJ DECJ S1400 S/N Res Calibrator 1d (hms) (dms) (mJy) (mas) (rfc_2011a)

1 B0833-45 J0835-4510 08:35:20.6 -45:10:34.8 1100.00 1340.672 1.325374 1+1U2 B1713-40 J1717-4054 17:17:21 -40:54:38 54.00 80.35447 22.11376 13 B0736-40 J0738-4042 07:38:32.3 -40:42:40.9 80.00 58.76232 30.23942 1 4 B2020+28 J2022+2854 20:22:37.0 +28:54:23.1 38.00 48.46162 36.66644 25 B1556-44 J1559-4438 15:59:41.5 -44:38:45.9 40.00 46.88687 37.89811 16 B2016+28 J2018+2839 20:18:03.8 +28:39:54.2 30.00 41.14197 43.19014 17 B1642-03 J1645-0317 16:45:02.0 -03:17:58.3 21.00 39.99059 44.43322 18 B1929+10 J1932+1059 19:32:13.9 +10:59:32.4 36.00 39.61237 44.85835 19 B1749-28 J1752-2806 17:52:58.6 -28:06:37.3 18.00 30.15447 58.92846 1N10 B1240-64 J1243-6423 12:43:17.1 -64:23:23.8 13.00 21.13359 84.07916 111 B0628-28 J0630-2834 06:30:49.4 -28:34:42.7 23.00 20.28642 87.59385 112 B1054-62 J1056-6258 10:56:25.5 -62:58:47.6 21.00 18.90665 93.98259 113 B0823+26 J0826+2637 08:26:51.3 +26:37:23.7 10.00 17.89530 99.29751 1N14 B1449-64 J1453-6413 14:53:32.7 -64:13:15.5 14.00 16.47393 107.8626 115 B0904-74 J0904-7459 09:04:10.8 -74:59:42.8 14.00 15.87081 111.9607 116 B2045-16 J2048-1616 20:48:35.6 -16:16:44.5 13.00 15.80564 112.4212 117 B1804-08 J1807-0847 18:07:38.0 -08:47:43.2 15.00 14.56202 122.0251 118 B1742-30 J1745-3040 17:45:56.3 -30:40:23.5 13.00 14.21371 125.0126 1+1N19 B2111+46 J2113+4644 21:13:24.3 +46:44:08.7 19.00 13.39365 132.6660 120 B1237+25 J1239+2453 12:39:40.4 +24:53:49.2 10.00 13.06561 135.9964 1 21 B1737-30 J1740-3015 17:40:33.8 -30:15:43.5 6.40 12.45043 142.7252 1N22 B0538-75 J0536-7543 05:36:30.7 -75:43:56.7 13.00 12.24966 145.0554 1 23 B0450+55 J0454+5543 04:54:07.7 +55:43:41.4 13.00 12.16867 146.0209 124 B1508+55 J1509+5531 15:09:25.6 +55:31:32.3 8.00 11.60582 153.1043 125 B1358-63 J1401-6357 14:01:52.4 -63:57:45.5 6.20 11.29577 157.3060 126 B0818-13 J0820-1350 08:20:26.3 -13:50:55.8 7.00 11.29269 157.3478 1+1U27 B1857-26 J1900-2600 19:00:47.5 -26:00:43.8 13.00 10.70191 166.0371 3

 

GIANT PULSES OBSERVATIONS AT KALYAZIN AND PUSHCHINO

List of pulsars with GP detected.

PSRJname

(Bname)

RA

hms

DEC

dms

P0

s

DM W50

ms

S1.4

mJy

1 2 3 4 5 6 7J0034-0721  00:34:08.86 -07:21:53.4 0.94295 11.38 56.7 11.0

J0218+4232 02:18:06.351 42:32:17.43 0.002323 61.25 * 0.9

J0534+2200 /B0531+21

05:34:31.973 22:00:52.06 0.033084 56.79 3,0 14.0

J0540-6919 05:40:11.16 -69:19:53.9 0.050498 146.5 18 0.024

J1115+5030 11:15:38.40 50:30:12.29 1.656439 9.19 16.6 3.0

J1752+2359 17:52:35.42 23:59:48.2 0.00305 19.8 0.15 0.18

J1939+2134/B1937+21

19:39:38.558 21:34:59.13 0.00155 71.0 0.06 10

J1959+2048 19:59:36.769 20:48:15.12 0.035112 29.1 0.03 0.4

MJy GP registration of Crab pulsar in Kalyazin using K-5 VLBI DAS.

F, GHz Spic , Jy N (per hour)

0.6 (0.3 1.0 ) 106 6 8

4.85 (1 2) 104 2 3

(Popov, Soglasnov, 2007)

GP registration for local time standard

synchronization.

GP of B0531+21 in Algonquin Park – Kalyazin VLBI observations in 2005. (S-2, 2.2 MHz)

CCF of GP observed on the base Algonquin Park – Kalyazin.Time delay determination accuracy ±5 ns.

GP registration for local time standard synchronization and astrometric pulsar VLBI.

CCF phase of 268 GPs of B0531+21 in Algonquin Park – Kalyazin VLBI. Phase ±0.5 Rad equiv. ± 2.5 ns

Structure function CCF phase vs time of observations. GP (upper) And calibration source DA193. Saturation of structure function corresponds to scintillation time at2.2 GHz

GP registration of Crab pulsar in Pushchino using K-5 VLBI DAS. (Dec. 2010 data)

The “Radioastron” VLBI session simulation 02 Feb. 2011.

• The main Goal – to make VLBI session in “Radioastron” mode.

• Sites: “Quasar” VLBI system of 3 34-m radiotelescopes (Svetloe, Badary, Zelenchuk), Medicina 32-m radiotelescope, Pushchino 22-m radiotelesope (Space RT simulation mode)

• Equipement: RDR and Mark-5 DAS.• Our particular goals: 1) to prove possibility of the

time synchronization of the on-board and Earth time standard using GP, 2) to test possibility of pulsars GP VLBI with “Radioastron”.

The “Radioastron” VLBI session simulation 02 Feb. 2011. Results of GP observations.

Crab GP with complex Microstructure. Simultaneously registered Crab GP

The “Radioastron” VLBI session simulation 02 Feb. 2011. TOA of GP delay between sites (correlation of

GPs in time domain).

SV – Svetloe, BD – Badary, ZK – Zelenchuk, PU - Pushchino

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