ROXA : a new multi-frequency large sample of blazars selected with SDSS and 2dF optical spectroscopy

Astronomy & Astrophysics manuscript no. ROXA˙astroph c© ESO 2008February 5, 2008

ROXA: a new multi-frequency selected large sample of blazarswith SDSS and 2dF optical spectroscopy

Sara Turriziani1,2, Elisabetta Cavazzuti2,3 and Paolo Giommi2,3

1 Universita degli studi di Roma, Tor Vergata, Dip. Fisica, via della ricerca scientifica 1, 00133 Roma, Italy.2 ASI Science Data Center, ASDC c/o ESRIN, via G. Galilei 00044 Frascati, Italy.3 Agenzia Spaziale Italiana, Unita Osservazione dell’Universo, viale Liegi 26 00198 Roma, Italy

Received ....; Accepted ....

ABSTRACT

Context. Although Blazars are a small fraction of the overall AGN population they are expected to be the dominant population of extragalacticsources in the hard X-ray and gamma-ray bands and have been shown to be the largest contaminant of CMB fluctuation maps. So far the numberof known blazars is of the order of several hundreds, but the forthcoming AGILE, GLAST and Planck space observatories will detect severalthousand of objects of this type.Aims. In preparation for these missions it is necessary to identify new samples of blazars to study their multi-frequency characteristics andstatistical properties.Methods. We compiled a sample of objects with blazar-like properties via a cross-correlation between large radio (NVSS, ATCAPMN) and X-ray surveys (RASS) using the SDSS-DR4 and 2dF survey data to spectroscopically identify our candidates and test the validity of the selectionmethod.Results. We present the Radio - Optical - X-ray catalog built at ASDC (ROXA), a list of 816 objects among which 510 are confirmed blazars.Only 19% of the candidates turned out to be certainly non-blazars demonstrating the high efficiency of our selection method.Conclusions. Our catalog includes 173 new blazar identifications, or about 10% of all presently known blazars. The relatively high fluxthreshold in the X-ray energy band (given by the RASS survey) preferentially selects objects with high fx/ fr ratio leading to the discovery ofnew High Energy Peaked BL Lac (HBLs). Our catalog therefore includes many new potential targets for GeV-TeV observations.

Key words. galaxies: active – galaxies: Blazar: BL Lacertae surveys:

1. Introduction

Blazars are the rarest (∼ 5%) and most extreme type of ActiveGalactive Nuclei (AGN) known. Historically, the classificationof AGN has been largely based on observational characteristicsleading to the proliferation of different classes of objects. Allsources of this type, however, can be seen as part of a generalparadigm in which AGN are divided into Thermal EmissionDominated (TED) AGN, where the emitted radiation is mostlygenerated through the accretion process onto a super-massiveblack hole, and Non-Thermal Emission Dominated (NTED)AGN, where the observed emission is mostly non-thermal andis generated in a jet of material moving away from the nucleusat relativistic speeds (e.g. Giommi & Colafrancesco 2006).Within this framework blazars are the small subset of NTEDAGN in which the jet is closely aligned to the line of sightcausing their emission to be strongly amplified by relativisticeffects (as originally proposed by Blandford & Rees 1978).

We recognize a source as a blazar if it shows the propertiesusually associated to aligned beamed emission such as strong

Send offprint requests to: S. Turriziani, [email protected]

and rapidly variable emission in all energy bands, from radioto GeV, sometimes TeV energies, core dominated radio emis-sion with flat radio spectral index, superluminal motion of ra-dio compact regions, the presence of one sided jets (a jet onthe other side is thought to exist, but with emission that is de-amplified by relativistic effects) and high brightness tempera-tures (Tb ∼ 1011 − 1018K), close to or above the Compton limit(Tb ≈ 1012).

Sources that initially show only some of these properties,in later observations often also show the others, strengtheningthe hypothesis that these are basically equivalent and insep-arable features related to the same underlying physical process.

Blazars include BL Lacertae objects (BL Lacs) where weobserve a non-thermal optical continuum with no or very weakemission lines, and Flat Spectrum Radio Quasars (FSRQs)which exhibit both strong narrow and broad emission lines.Furthermore, BL Lacs can be distinguished by the peak of thesynchrotron emission in their Spectral Energy Distributions(SEDs). Objects with synchrotron peak at low energy (typi-cally in the Infra-Red) are generally found in radio surveys

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2 Turriziani et al.: ROXA MultiFrequecy Blazar Sample

and are called LBLs (Low Energy Peaked BL Lacs), whereasthe rarer objects with synchrotron peak in the UV/X-ray bandare called HBLs (High Energy Peaked BL Lacs) and aremainly selected in the X-ray band, where the maximum oftheir synchrotron power is emitted (e.g. Padovani & Giommi1995).

In this paper we discuss a large sample of candidate blazarsthat we have assembled using a multi-frequency selection tech-nique based on the NVSS (Condon et al. 1998), ATCAPMN(ATCA catalogue of compact PMN sources in Tasker (2000),RASS (Voges et al. 1999; Voges et al. 2000) and GSC2 (Lasker1995; McLean et al. 2000) catalogs.

We have assessed the quality of the sample using a sub-sample of 816 objects for which data from Sloan Digital SkySurvey - Data Release 4 (SDSS-DR4; Adelman-McCarthyet al. 2006), 2dF Galaxy Redshift Survey (2dFGRS; Collesset al. 2001) and 2dF QSO Survey (2dFQSO; Shanks et al. 2000)are available.

We refer to our final list of 816 sources as the ROXA cata-log, which stands for Radio Optical X-ray ASDC catalog.

We have built ROXA as a complement to the work ofSowards-Emmerd et al. (2003, 2004, 2005) as we share theirgoal of significantly enlarging the existing blazar catalogsin order to understand blazars statistical properties and toselect interesting objects for upcoming high energy astronomymissions like AGILE, and GLAST. Sowards-Emmerd et al.(2005), with a single-band approach, selected flat-spectrumradio sources and then used optical telescopes for spectro-scopic follow-up observations, whereas in this work we use amulti-frequency approach that requires no additional telescopetime. Moreover, the selection of radio sources results mostly inthe discovery of LBL sources whereas our flux limits, whichare mostly driven by the relatively shallow X-ray sensitivityof the RASS survey, favor objects such as HBL since theyemit the maximum of their synchrotron emission near orwithin the X-ray band. This bias towards HBL sources isstrengthened by the Ultra-Violet excess requirement in theSDSS spectroscopical target selection (Richards et al. 2002).The presence of HBLs allows ROXA to contribute with newtargets for GeV/TeV observations.

ROXA is also an augmentation of Collinge et al. (2005)who searched for extragalatic quasi-featurless objects in theSecond Data Release of Sloan Digital Sky Survey (SDSS-DR2;Abazajian et al. 2004) with low proper motion in USNO-BCatalog (Monet et al. 2003) to built a BL Lac candidate sam-ple. However, further information in other bands is requiredto confirm classifications therefore we used a multifrequencyselection algorithm to build the candidate blazar sample and,although radio and X-ray selections could introduce biases,the high efficiency of the selection method allowed us to findmany new blazars.

The blazar selection algorithm is described in Section 2.In section 3 we focus on optical counterpart investigation andsource classification criteria. Finally, we discuss our results

and present our future projects in Section 4.

Throughout the paper we assume a cosmology with param-eters in agreement with the results of Wilkinson MicrowaveAnisotropy Probe (WMAP; Bennett et al. 2003): H0=70 kms−1 Mpc−1, ΩM=0.3, ΩΛ=0.7 (Spergel et al. 2003).

2. The selection method

For the definition of our sample we relied on the availability oflarge catalogs of astronomical objects combined with on-lineservices offering simple access to finding charts and magnitudeestimates.

The method is similar to that used for the DXRBS (Landtet al. 2001; Padovani et al. 2006) and the Sedentary Survey(Giommi et al. 1999, 2005) and consists in three steps:

1. a first cross-correlation between radio and X-ray surveys(the NRAO VLA Sky Survey (NVSS; Condon et al. 1998),ATCAPMN (ATCA catalogue of compact PMN sources inTasker (2000)) and ROSAT All Sky Survey (RASS; Vogeset al. 1999; Voges et al. 2000)).

2. For each radio/X-ray match, optical magnitudes were re-trieved from the Guide Star Catalog (GSC2; Lasker 1995;McLean et al. 2000)

3. For all radio/optical/X-ray matches we calculated the X-rayto optical (αox ) and radio to optical (αro ) spectral slopesand took only sources with αox and αro values within theblazar area (for more detail see e.g. Perlman et al. 1998;Giommi et al. 1999; Landt et al. 2001; Padovani et al.2006).

2.1. The X-ray - radio cross correlation

The NVSS catalog of radio sources includes nearly two millionobjects above a flux limit of 2.5 mJy at 1.4GHz (Condon et al.1998), the ATCAPMN catalog includes 7178 objects and itis reasonibly complete down to ∼ 100 mJy (Tasker 2000)whereas the RASS X-ray catalog is a list of 124.735 objectsdetected during ROSAT All Sky Survey (Voges et al. 1999;Voges et al. 2000).As for the case of the Sedentary Survey (Giommi et al.1999) and the DXRBS (Padovani et al. 2006), we used theEXOSAT/BROWSE software to cross-correlate the NVSS andthe RASS catalogs. The cross-correlation used a radius of 1arcmin and resulted in 16.596 matches.We then restricted our sample to sources with Galactic latitude| b| > 20o finding 12.988 candidates. We kept only thosewith ∆rx < 2.5σrx, where σrx =

√σ2

x + σ2r is the total

(radio+X-ray) positional uncertainty and ∆rx is the actualdistance between the radio and X-ray positions. This resultedin 9663 entries.

We estimated the percentage of accidental spatial coin-cidences of unrelated objects by shifting the coordinates ofall the sources in one of the catalogs by a fixed amount andre-running the cross-correlation with the same parameters.

Turriziani et al.: ROXA MultiFrequecy Blazar Sample 3

This procedure led to the statistical estimation that only 1 - 2% could be spurious associations.

2.2. Blazar candidate selection

For each RASS-NVSS match we obtained the magnitudesof the optical candidate counterparts from the GSC2 catalog.When no GSC2 source was present within the few arc-secondspositional uncertainty of the NVSS radio source, we assumedthat the counterpart is fainter than Jmag=19.5, approximatelythe flux limit of GSC2 (McLean et al. 2000). In the very rarecases when more than one GSC2 object was present, the opti-cally brightest object was initially assumed to be the counter-part.

We used EXOSAT/BROWSE software to get 5 GHz fluxesvia a cross-correlation with several radio catalogs, such asNORTH6cm (Becker et al. 1991), GB6 (Gregory et al. 1996)and Parkes-MIT-NRAO (PMN; Griffith & Wright 1993). Forsources with no 5 GHz flux information we estimated it asF5Ghz = F1.4GHz × ( 20

6 )−αrm , where αrm is 0.25, the assumedaverage value for flat spectrum sources.

We corrected X-ray and optical fluxes for Galactic absorp-tion and the redshift-dependent K-correction. For sources withno redshift information we assumed a typical redshift equal tothe average value found in sources with the same X-ray to radioflux ratio ( fx/ fr ).

To build our candidate blazar sample we have calculatedthe optical to X-ray (αox ) and radio to optical (αro ) spectralslopes and selected objects with αro > 0.2 where most of theblazars are located in the αox -αro diagram (see e.g. Giommiet al. 1999, for details).

We relaxed the radio-loudness condition αro > 0.2 to αro >0.1 (where αro and αox are the usual effective spectral indicesdefined between the rest-frame frequencies of 5 GHz, 5000 Åand 1 keV) for objects which had no optical counterpart in theGSC2, since a lower limit on Jmag results in a lower limit onαro .

The selection process led to a sample of 7662 blazar can-didates. Fig. 1 shows the αro - αox diagram and Fig. 2 plots all7662 sources in Galactic coordinates. The non-uniform spacedistribution in this last plot reflects the sensitivity of the RASSsurvey, which was higher around the ecliptic coordinates, andthe higher radio flux limit (hence lower source density) of theATCAPMN catalog at declinations south of -40o.

3. Classification of optical counterparts usingSDSS and 2dF data

For all sources in our sample we used the SDSS on-line ser-vices (SkyServer-Radial search) to download SDSS measure-ments (right ascension, declination and u’ g’ r’ i’ z’ magni-tudes) of each optical object lying within 6 arcseconds fromeach NVSS radio position.

We found that 2.353 RASS+NVSS sources have SDSS-DR4 optical counterparts (including some multiple optical

Fig. 1. The αox – αro distribution for the whole sample of 7.662blazar candidates

Fig. 2. The Galactic coordinates of the 7662 blazar candidatesare plotted in Aitoff projection

counterparts, MOCs ).

We then used the SkyServer DR4 Spectroscopic Query(proximity with radius 10 arcseconds) and the DAS online ser-vices to acquire spectra. We used previous downloaded SDSSpositions to get spectral parameters and survey files for objectsclassified as galaxies, stars or ”unknown” in the SDSS standardproducts. We found 669 spectra among the 2353 SDSS opticalcounterparts.

In a similar way we searched for optical counterparts alsoin the 2dFGRS and in the 2dFQSO databases. This resulted inspectra and B j magnitude estimates for additional 199 objectsfrom 2dFGRS and for 94 from 2dFQSO (including MOCs).


3.1. Sources Classification

All candidates that had MOCs were associated to a single op-tical object through a visual inspection procedure using theNVSS, ESO and NED online services. For each source wecross-checked the optical (ESO and SuperCOSMOS Surveys)finding chart with the RASS and NVSS positions and with theposition in the FIRST catalog (R.L. et al. 1997) when available.In this way we were able to chose the best optical counterpartfor each blazar candidate. Moreover, we excluded those objectswith RASS source extent greater than 30 arcsec. We did notapply this condition to those detections with 20 or less photonssince in these cases the uncertainty in the estimation of X-rayextent is too large.

We built SEDs and analyzed optical spectra, with CaH&Kevaluation when needed, to classify each object (the equivalentwidth of emission lines in radio-loud AGN depends stronglyon the contribution from non-thermal jet emission, and,therefore, on the Ca H&K break value (Marcha et al. 1996;Scarpa & Falomo 1997)). Sources with SDSS magnitudeestimates, although not targeted for spectroscopy by SDSSpipelines, were kept in the sample only if already classified inthe literature as reported in NED.

SDSS and 2dF automated redshift estimation and spectralclassification proved to be unreliable for several BL Lacobjects because of the lack of emission lines. When possible,we re-calculated redshifts using the IRAF analysis package(Tody 1986, 1993).

We also defined a transition class for those objectsthat show properties in between two standard classifications.Regarding Radio Galaxies and BL Lacs we defined sources tobe :

– BL Lac if Lx > 1044 erg s−1 or CaH&K < 0.4 or both– Radio Galaxy if CaH&K > 0.4 AND Lx < 5 × 1043 erg s−1

– Radio Galaxy/BL Lac transition object if CaH&K > 0.4AND Lx between 5 × 1043 and 1044 erg s−1

Moreover we identified other transition classes for thoseobjects showing optical properties which are borderline fortheir standard classification. These are BL Lac/FSRQ transi-tion object and R.G./FSRQ transition object.

We re-calculated αro and αox parameters estimating Vmagas in the following:

– for SDSS objects: V = g’ - 0.55(g’ - r’) - 0.03– for 2dF objects: V = B j + 0.5– for object detected by both SDSS and 2dF we used SDSS

magnitudes.

Our final catalog ROXA includes 816 objects, 510 of whichare confirmed blazars (i.e. 62.5%). Of the remaining sources110 (or 13% of the total) are confirmed QSOs (by the SDSS or2dF optical spectra) but their radio spectral slope is currentlynot available and therefore they remain blazar candidates. Only19% of the candidates turned out to be definitely non-blazars.

Table 1 summarizes the statistics of our source classifica-tion. The complete catalog is reported in Table 2. The first

column of Table 1 contains source classification, the secondcolumn gives the number of previously known objects (thatis sources previously reported in the literature as blazars), thethird column gives the number of new objects (classified in thiswork for the first time), the fourth column gives the total num-ber of objects and the last column gives the percentage withrespect to the entire sample .

The label confirmed blazars includes BL LAC, FSRQ, BLLac/FSRQ transition object and BL Lac candidate.

The label “others“ is used to comprise several non-blazarsources, such as stars and variuos types of galaxies (Normal,Starburst and Seyfert).We point out that we identified 173 new blazars.

Fig. 3 reports the multi-band indexes distribution of ROXAconfirmed blazars.

Fig. 3. ROXA αro – αox distribution of the confirmed blazars.Symbols are as follows: ? – BL Lac, 4 – FSRQ, • – HFSRQ, ⊕– BL Lac/FSRQ, + – BL Lac candidate, x – HFSRQ candidate

4. Conclusions and future work

In this paper we presented the ROXA (Radio Optical X-rayASDC) catalog, a list of of 816 objects including 510 con-firmed blazars. This catalog has been extracted from a sampleof 7662 objects selected, through the cross matching procedurebetween the NVSS, ATCAPMN, RASS and the GSC2 catalog,to have properties similar to those of previously known blazarsin the αro -αox diagram.

We tested the selection method, also used in the DXRBSand in the Sedentary surveys, via a cross-correlation of the can-didate sample with the SDSS DR4 and 2dF surveys for whichoptical spectra are available. We analyzed SEDs and spectra to


Table 1. ROXA Catalog Statistic

Known objects new objects Total Sample %BL LAC 182 60 242 29.7%FSRQ 147 99 246 30.1%BL Lac/FSRQ transition obj. 1 7 8 1.0%BL LAC candidate 7 7 14 1.7%confirmed blazars 337 173 510 62.5%R.G./BL Lac transition obj. 0 24 24 3.0%R.G./FSRQ transition obj. 0 2 2 0.2%Radio Galaxies 24 8 32 3.9%SSRQ 59 43 102 12.5%QSO RL 60 50 110 13.5%Galaxies NELG 12 2 14 1.7%BLRG 2 0 2 0.2%others 18 2 20 2.5%Total 512 304 816 100%

classify the candidate blazars and we confirmed the validity ofthe selection algorithm.

Our final catalog consists of ∼ 62.5% confirmed blazars, ∼13% QSO with no radio spectral information and of ∼ 19% ofsources that are surely non blazars. Since the ratio between flatand steep spectrum QSO is 254/102 (see tab. 1 ) the majorityof QSO with no radio spectral information is expected to beblazars. We can therefore conclude that our selection algorithmhas an efficiency of (∼ 70%). We also contributed several newblazar identifications finding 173 new blazars.

Our method for the construction of the ROXA catalog iscomplementary to the work of Sowards-Emmerd et al. (2005)and Collinge et al. (2005) as these authors used single-bandapproaches whereas we used a multi-frequency selection al-gorithm. Sowards-Emmerd et al. (2005) selected flat spectrumradio sources and then requested telescope time for follow-up spectroscopic observations whereas Collinge et al. (2005)searched for extragalatic quasi-featurless objects in SDSS-DR2with low proper motion in USNO-B Catalog to built a BLLac candidate sample. However further information in otherbands are required to confirm the classifications. Moreover,the selection of radio sources results in finding mostly LBLsby Sowards-Emmerd et al. (2005) whereas our algorithm havegreater chances of finding HBLs, because of our relatively highX-Ray flux limit that preferentially select objects in which themaximum of synchrotron power is emitted at high energy.

We share the goal with Sowards-Emmerd et al. (2005) tocreate as large as possible blazar catalogs to be used as targetsfor observations during the next planned new high energymissions (e.g. AGILE and GLAST).

We plan to request high frequency radio observations in or-der to measure the spectral slope of the 110 QSOs with ra-dio measurements at a single frequency and to better evaluatethe nuclear spectra of the 102 Steep Spectrum Radio Quasars(SSRQs) as their steep slopes could be due to extended radiocomponents.

In principle, by applying this selection method to the entiresky and not just to limited regions, we could build a much largersample suitable for the identification of foreground sources inCMB maps and in gamma-ray data. At present, the most suit-able optical data available are from the SDSS project. For thisreason we intend to update the ROXA catalog as new SDSSreleases become available.

Acknowledgements. We are grateful to Silvia Piranomonte for herhelp in the analysis of part of the optical spectra. This work ispartly based on data from the 2dF, SDSS, NVSS, ROSAT, GSC2,GB6, Parkes-MIT-NRAO (PMN), NORTH6cm catalogs and ser-vices. Additional data have been obtained from the NASA/IPACExtragalactic Database (NED) and from the ASI Science Data Center(ASDC).

Funding for the creation and distribution of the SDSS Archive hasbeen provided by the Alfred P. Sloan Foundation, the ParticipatingInstitutions, the National Aeronautics and Space Administration, theNational Science Foundation, the U.S. Department of Energy, theJapanese Monbukagakusho, and the Max Planck Society. The SDSSis managed by the Astrophysical Research Consortium (ARC) for theParticipating Institutions.

IRAF is distributed by the National Optical AstronomyObservatories, which are operated by the Association of Universitiesfor Research in Astronomy, Inc., under cooperative agreement withthe National Science Foundation

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mag

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.311

1.9

0.0

3.30

E-1

33.

98E

-12

2.45

E+

448.

31E

+32

FSR

Q*

RO

XA

J141

756.

5+25

4326

.10.

240.

022

.789

.70.

02.

70E

-11

4.07

E-1

04.

54E

+45

1.51

E+

32B

LL

acR

OX

AJ1

4175

8.6+

4051

59.6

0.38

0.0

21.2

253.

289

.02.

10E

-13

2.36

E-1

21.

06E

+44

1.28

E+

33SS

RQ

RO

XA

J141

858.

8+39

4638

.70.

470.

020

.226

0.4

0.0

3.00

E-1

31.

56E

-12

2.53

E+

442.

20E

+33

NE

LG

RO

XA

J141

908.

0+06

2834

.71.

440.

017

.261

00.9

0.0

6.70

E-1

21.

48E

-12

8.61

E+

467.

84E

+35

SSR

QR

OX

AJ1

4194

6.3+

4634

24.3

0.55

0.0

20.3

215.

380

.03.

00E

-13

3.75

E-1

23.

56E

+44

2.55

E+

33SS

RQ

RO

XA

J141

946.

5+54

2314

.71.

830.

019

.461

2.2

0.0

3.00

E-1

36.

62E

-13

6.98

E+

451.

42E

+35

FSR

QR

OX

AJ1

4194

6.6+

3821

48.3

0.15

0.0

15.8

788.

813

50.0

1.30

E-1

29.

63E

-13

8.26

E+

435.

01E

+32

BL

Lac

RO

XA

J142

020.

5+46

2440

.71.

250.

019

.846

.834

.02.

00E

-13

5.88

E-1

21.

80E

+45

4.20

E+

33FS

RQ

*R

OX

AJ1

4210

5.9+

3855

22.6

0.49

0.0

18.6

86.3

0.0

4.60

E-1

37.

20E

-12

4.19

E+

447.

85E

+32

FSR

QR

OX

AJ1

4215

5.3+

3723

29.1

1.65

0.0

19.7

4.1

0.0

1.40

E-1

34.

61E

-11

2.51

E+

457.

34E

+32

QSO

RL

RO

XA

J142

230.

2+32

2310

.30.

690.

019

.140

5.3

0.0

8.70

E-1

32.

90E

-12

1.79

E+

458.

34E

+33

FSR

QR

OX

AJ1

4223

5.8-

0152

11.2

0.67

0.0

19.0

114.

20.

07.

60E

-13

8.99

E-1

21.

46E

+45

2.19

E+

33Q

SOR

L*

RO

XA

J142

238.

8+58

0155

.40.

000.

018

.213

.30.

02.

50E

-11

2.54

E-0

90.

00E

+00

0.00

E+

00B

LL

acR

OX

AJ1

4231

4.0+

5055

37.3

0.28

0.0

17.8

178.

423

2.0

5.90

E-1

22.

54E

-11

1.41

E+

454.

25E

+32

FSR

QR

OX

AJ1

4233

9.7+

0436

34.8

1.65

0.0

20.4

20.9

0.0

3.50

E-1

32.

26E

-11

6.29

E+

453.

76E

+33

QSO

RL

RO

XA

J142

345.

2+46

5057

.20.

550.

019

.020

.50.

03.

40E

-13

2.24

E-1

14.

16E

+44

2.51

E+

32FS

RQ

*R

OX

AJ1

4235

1.4+

4015

31.7

0.08

0.0

15.7

12.6

0.0

2.10

E-1

22.

25E

-10

3.49

E+

432.

09E

+30

0.47

Rad

ioG

alax

yR

OX

AJ1

4242

1.1+

3705

52.7

0.29

0.0

18.7

79.2

0.0

7.20

E-1

31.

23E

-11

1.92

E+

442.

11E

+32

0.49

BL

Lac

RO

XA

J142

422.

9+34

3356

.70.

580.

019

.810

.10.

01.

90E

-12

2.54

E-1

02.

56E

+45

1.36

E+

320.

08B

LL

acR

OX

AJ1

4244

7.3+

0239

51.9

0.05

0.0

15.0

11.7

0.0

1.10

E-1

21.

27E

-10

7.63

E+

428.

11E

+29

0.49

Rad

ioG

alax

yR

OX

AJ1

4245

5.4+

3615

35.9

0.00

0.0

18.0

91.2

0.0

3.40

E-1

35.

04E

-12

0.00

E+

000.

00E

+00

BL

Lac

RO

XA

J142

545.

8+00

2242

.70.

3318

.618

.970

.90.

07.

90E

-13

1.51

E-1

12.

76E

+44

2.48

E+

32Q

SOR

LR

OX

AJ1

4254

7.9+

5230

34.0

0.42

0.0

18.7

11.8

0.0

4.10

E-1

34.

69E

-11

2.60

E+

447.

47E

+31

QSO

RL

*R

OX

AJ1

4255

0.6+

2404

03.3

0.65

0.0

17.3

1559

.50.

01.

50E

-12

1.30

E-1

22.

71E

+45

2.81

E+

34SS

RQ

RO

XA

J142

651.

4+36

3853

.00.

500.

018

.83.

60.

04.

80E

-13

1.80

E-1

04.

65E

+44

3.49

E+

31Q

SOR

LR

OX

AJ1

4270

0.3+

2348

00.0

0.00

0.0

14.9

430.

20.

06.

90E

-12

2.17

E-1

10.

00E

+00

0.00

E+

00B

LL

acR

OX

AJ1

4274

5.7+

3908

32.0

0.17

0.0

19.1

7.4

0.0

2.30

E-1

34.

20E

-11

1.72

E+

435.

55E

+30

0.29

BL

Lac

*R

OX

AJ1

4283

2.6+

4240

24.7

0.13

0.0

16.8

58.9

0.0

5.30

E-1

11.

22E

-09

2.32

E+

452.

58E

+31

0.05

BL

Lac

RO

XA

J142

921.

7+54

0611

.13.

010.

020

.210

28.9

0.0

2.50

E-1

33.

28E

-13

1.95

E+

468.

04E

+35

FSR

QR

OX

AJ1

4311

0.3+

5118

32.5

0.46

0.0

20.5

17.5

0.0

2.00

E-1

31.

54E

-11

1.56

E+

441.

36E

+32

0.42

BL

Lac

*R

OX

AJ1

4324

4.4-

0059

15.1

1.03

0.0

17.5

132.

60.

07.

30E

-13

7.44

E-1

24.

06E

+45

7.38

E+

33Q

SOR

LR

OX

AJ1

4352

8.3+

5507

51.9

0.14

0.0

16.6

7.4

0.0

1.70

E-1

23.

10E

-10

8.90

E+

433.

87E

+30

0.47

R.G

./BL

Lac

*R

OX

AJ1

4355

0.1+

3632

35.5

0.01

0.0

13.5

4.0

0.0

2.50

E-1

38.

45E

-11

1.10

E+

411.

76E

+28

BL

Lac

cand

idat

e*R

OX

AJ1

4355

4.1+

3957

44.4

0.00

0.0

17.6

28.3

0.0

2.80

E-1

31.

34E

-11

0.00

E+

000.

00E

+00

Star


Tabl

e2:

cont

inue

d

Sour

cena

me

zB

jm

agg’

mag

Rad

ioflu

xR

adio

flux

X-r

ayflu

xf x/

f rL x

L rC

aH&

KC

lass

ifica

tiona

1.4

GH

z5

GH

zm

Jym

Jyer

gcm−

2s−

1er

gcm−

2s−

1Jy−

1er

gs−

1er

gs−

1H

z−1

RO

XA

J143

641.

8+02

2940

.40.

770.

017

.931

.70.

07.

60E

-13

3.24

E-1

12.

10E

+45

8.75

E+

32Q

SOR

LR

OX

AJ1

4365

7.7+

5639

24.8

0.00

0.0

18.6

21.4

0.0

2.70

E-1

21.

70E

-10

0.00

E+

000.

00E

+00

BL

Lac

RO

XA

J143

718.

1+36

1858

.81.

110.

019

.742

.50.

02.

10E

-13

6.68

E-1

21.

42E

+45

2.87

E+

33Q

SOR

LR

OX

AJ1

4372

7.0+

5045

38.9

0.78

0.0

17.6

58.0

23.0

7.30

E-1

33.

17E

-11

2.08

E+

451.

66E

+33

FSR

Q*

RO

XA

J143

748.

1-01

4710

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310.

015

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01.

70E

-12

4.35

E-1

11.

73E

+46

5.36

E+

33Q

SOR

LR

OX

AJ1

4375

6.4+

3519

36.9

0.54

0.0

18.3

98.0

0.0

3.10

E-1

34.

27E

-12

3.53

E+

441.

12E

+33

SSR

Q*

RO

XA

J143

917.

3+39

3242

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000.

016

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80E

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2.90

E-1

00.

00E

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0.00

E+

00B

LL

acR

OX

AJ1

4394

2.7+

5827

59.1

0.43

0.0

17.9

46.9

45.0

6.00

E-1

31.

33E

-11

3.91

E+

443.

06E

+32

FSR

Q*

RO

XA

J143

946.

9+49

5805

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170.

018

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1.7

198.

03.

00E

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1.52

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22.

53E

+43

9.42

E+

31B

LL

acca

ndid

ate

RO

XA

J144

003.

4+37

0727

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100.

016

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09.

90E

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8.63

E-1

12.

40E

+43

3.76

E+

300.

47R

adio

Gal

axy

RO

XA

J144

131.

9+60

1852

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540.

018

.392

.442

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50E

-13

1.07

E-1

15.

08E

+44

1.04

E+

33SS

RQ

*R

OX

AJ1

4420

5.8-

0248

03.0

0.32

19.9

20.0

3.9

0.0

8.40

E-1

32.

91E

-10

2.81

E+

441.

31E

+31

QSO

RL

RO

XA

J144

248.

1+12

0040

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160.

017

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01.

40E

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2.73

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01.

01E

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4.99

E+

31B

LL

acR

OX

AJ1

4451

6.8+

0039

34.2

0.31

0.0

22.7

8.4

0.0

1.40

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22.

25E

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4.23

E+

442.

54E

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0.42

BL

Lac

/FSR

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RO

XA

J144

632.

5+41

2729

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640.

020

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03.

10E

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9.50

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25.

36E

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7.63

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09B

LL

ac*

RO

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800.

4+36

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000.

017

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07.

50E

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2.79

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00.

00E

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0.00

E+

00B

LL

acR

OX

AJ1

4481

9.3+

4432

32.7

0.08

0.0

16.2

6.0

0.0

1.30

E-1

22.

93E

-10

2.00

E+

439.

22E

+29

QSO

RL

RO

XA

J144

837.

5+50

1448

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070.

019

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7.4

271.

02.

20E

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8.12

E-1

31.

37E

+45

4.47

E+

34SS

RQ

RO

XA

J144

850.

2+04

0219

.80.

870.

020

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1.3

381.

04.

70E

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1.23

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21.

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LL

ac*

RO

XA

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921.

4+63

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040.

014

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06.6

1053

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70E

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1.61

E-1

37.

01E

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1.24

E+

32N

EL

GR

OX

AJ1

4493

1.9+

2746

27.5

0.22

0.0

18.2

90.8

0.0

6.60

E-1

29.

82E

-11

9.88

E+

441.

36E

+32

BL

Lac

RO

XA

J145

002.

3+00

1629

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9618

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40E

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1.54

E-1

13.

47E

+45

5.15

E+

32FS

RQ

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OX

AJ1

4520

1.9+

5530

52.7

1.41

0.0

19.3

274.

511

5.0

2.30

E-1

32.

00E

-12

2.82

E+

453.

37E

+34

SSR

QR

OX

AJ1

4522

3.5+

4522

30.2

0.47

0.0

17.5

381.

90.

02.

50E

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8.85

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22.

06E

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3.14

E+

33St

arR

OX

AJ1

4542

7.1+

5124

33.6

0.00

0.0

18.2

178.

113

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6.70

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35.

04E

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0.00

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00E

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BL

Lac

RO

XA

J145

432.

2+29

5558

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580.

020

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1.3

0.0

8.10

E-1

31.

50E

-12

1.11

E+

451.

00E

+34

FSR

QR

OX

AJ1

4582

6.4+

4832

38.2

0.54

0.0

20.5

3.4

0.0

5.60

E-1

22.

23E

-09

6.51

E+

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95E

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BL

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RO

XA

J145

940.

0+41

1758

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180.

017

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9.6

55.0

2.00

E-1

33.

64E

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1.75

E+

431.

31E

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0.43

BL

Lac

*R

OX

AJ1

4594

8.5+

3141

12.5

0.64

0.0

21.6

6.4

0.0

2.40

E-1

35.

07E

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4.12

E+

441.

10E

+32

0.22

BL

Lac

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OX

AJ1

4595

8.3+

3337

01.8

0.64

0.0

16.7

15.7

0.0

1.50

E-1

21.

29E

-10

2.66

E+

452.

78E

+32

HFS

RQ

cand

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OX

AJ1

5002

7.1+

4508

58.9

1.20

0.0

18.1

142.

00.

04.

90E

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4.66

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24.

04E

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1.17

E+

34SS

RQ

RO

XA

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117.

8+54

5518

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340.

019

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7.7

74.0

6.70

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39.

05E

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2.57

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57E

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SSR

Q*

RO

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124.

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018

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03.

90E

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2.77

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14.

39E

+45

2.14

E+

33Q

SOR

LR

OX

AJ1

5022

6.7+

3947

31.7

0.56

0.0

21.2

434.

80.

03.

90E

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1.21

E-1

24.

92E

+44

5.48

E+

330.

42R

adio

Gal

axy

RO

XA

J150

653.

8+02

1904

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220.

019

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80.

06.

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25E

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1.25

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LL

ac*

RO

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5.42

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12.

52E

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3.25

E+

34FS

RQ

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OX

AJ1

5082

4.5+

5604

23.0

0.98

0.0

19.5

22.7

30.0

4.20

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31.

40E

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2.08

E+

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12E

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FSR

Q*

RO

XA

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842.

0+27

0918

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000.

019

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50E

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2.86

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00.

00E

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0.00

E+

00B

LL

acR

OX

AJ1

5094

7.8+

5556

17.1

0.00

0.0

18.1

31.5

44.0

8.80

E-1

32.

00E

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0.00

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00E

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BL

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017.

8+42

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490.

021

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0.0

2.70

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31.

40E

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34E

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NE

LG

RO

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142.

7+44

3043

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019

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1.6

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1.05

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16E

+34

SSR

QR

OX

AJ1

5143

6.6+

4450

03.9

0.57

0.0

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40.5

31.0

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3.95

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33E

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FSR

Q*

RO

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443.

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370.

016

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9.8

0.0

3.20

E-1

24.

37E

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1.51

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454.

68E

+33

SSR

QR

OX

AJ1

5151

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4755

08.9

0.91

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18.5

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Documents

ROXA : a new multi-frequency large sample of blazars selected with SDSS and 2dF optical spectroscopy