J/A+A/684/A202ivo://CDS.VizieR/J/A+A/684/A202doi:10.26093/cds/vizier.36840202CDSLambert S.Sol H.Pierron A.2024-11-29T20:01:51Z2024-04-25T08:22:01ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frquasarsinterferometryradio-sourcesvisible-astronomyWe investigated the location of the optical emission with respect to the parsec-scale radio structure and attempted to identify whether the optical centroid is coincident with the radio core or a radio component of the jet. We used optical Gaia DR3 and 8 GHz ICRF3 positions and a model fitting of 15 GHz imaging by the MOJAVE VLBA survey for 422 sources, mostly blazars. We searched for possible associations between optical centroids and radio components. We also compared the astrometric and photometric properties of each category, looked for trends between the various source parameters, and discussed possible biases. Sources can be separated into four categories based on whether their optical centroid (i) falls onto the radio core (category C), (ii) lies close to the base of the jet (category B), (iii) coincides with a radio component downstream in the jet (category J), or (iv) is not found to coincide with a detected radio component (category O). Due to a number of random and systematic errors, the number of sources falling into each category remains approximate but close to 32%, 36%, 22%, and 10%, respectively. The family of quasars, mostly flat spectrum radio quasars (FSRQs), clearly dominates the C and B categories, with their percentage decreasing from categories C to O. Conversely, the family of BL Lacs is spread over the four classes and dominates the category O. Radio galaxies are mainly in classes O and J, and the radio-loud narrow-line Seyfert 1 all belong to class C. An individual analysis of O sources shows that, despite the absence of a direct association with a specific radio component, the optical Gaia centroid is globally related to the radio VLBI jet structure. Our study shows that the spatial distribution of the optical counterparts seen by Gaia below the 0.2-arcsec scale around the radio cores appears in the vast majority of cases to be related to the AGN core or to its jet, with most of them located downstream in the jet. Those associated to the core also exhibit a bluer color index, suggesting a possible contribution of the accretion disk to the optical emission, while those associated to a radio knot in the jet appear redder and tend on average to be found in more polarized radio sources. Most BL Lacs have their optical emission coincident with the jet base or a knot in the jet, while sources with an optical emission on or close to the radio core are mostly FSRQs. Radio components associated with the optical centroid at the jet base or along the jet are mainly stationary or quasi-stationary features, with low apparent MOJAVE velocities. There are indications that the apparent proper motion of the Gaia centroids may be higher than the speed of the associated radio components, but the significance of this trend requires further investigation.2024A&A...684A.202Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/684/A202CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/620/A68 : Polarization of quasars (Hutsemekers+, 2018)J/ApJS/234/12 : MOJAVE XV. VLBA 15GHz obs. of AGN jets 1996-2016 (Lister+ 2018)J/ApJ/923/30 : MOJAVE XVIII. Bright radio-loud active AGNs (Lister+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/684/A202https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/684/A202http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/684/A202https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/684/A202https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/684/A202http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/684/A202GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/684/A202/table (Numerical quantities that allowed to built up the analyses and conclusions of the article)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/684/A202/table?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/684/A202/table?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/684/A202/table?GETtext/xml+votable180.050000true1.488230838.33754140.0055555555555555566/18 60 110 514 532 579 674 700 893 911 968 1085 1154 1263 1342 1450 1509 1546 1622 1701-1702 1782 2122 2143 2214 2228 2280 2397 2414 2549 2710 2721 2836 3017 3024 3096 3309 3492 3675 3710 3712 3784 3820 3876 3882 3886 3951 3971 4027 4054 4285 4572 4685 4695 4770 4820 4964 4977 5139 5154 5353 5423 5448 5458 5460 5546 5597 5693 5767 5817 5848 6018 6088 6164 6252 6368 6496 6507 6641 6647 6777 6815 6822 6853 6888 6948 6963 6984 6996 7004 7045 7091 7129 7181 7226 7235 7371 7389 7446 7548 7570 7653 7745 7758 7857 7896 7969 8004 8031 8123 8177 8199 8220 8299 8466 8487 8515 8615 8699 8915 9003 9075 9248 9442 9460 9545 9570 9612 9629 9632-9633 9676 9688 9711 9714 9723 9998 10006 10163 10170 10249-10250 10352 10422 10501 10548 10681 10921 11153 11212 11242 11430 11522-11523 11529 11552 11631 11639-11640 11649 11715 11845 12047 12241 12323 12352 12466 12475 12580 12599 12604 12619 12625 12664 12896 13156 13230 13320 13352 13410 13447 13485 13496 13572 13582 13693 13729 13820 13927 14068 14338 14520 14608 14641 14737 14797 14842 14854 14858 15023 15067 15147 15211 15286 15490 15494 15916 15936 15969 16027 16049 16059 16093 16113 16184 16247 16272 16281 16298 16301 16355 16720 17184 17186 17351 17364 17414 17516 17541 17579 17857 17917 17927 18002 18005 18035 18037 18158 18214 18253 18378 18457 18506 18624 18661 18669 18718 18821 18907 19088 19101 19190 19271 19370 19373 19398 19487 19523 19567 19593 19622 19831 19878 20099 20224 20468 20836 20888 20920 20935 21121 21266 21358 21437 21564 21574 21758 21768 21793 21873 21924 21935 21960 21968 21972 22271 22363 22396 22501 22658 22894 22917 22950 23014-23015 23099 23121 23127 23323 23416 23691 23786 23897 24084 24123 24260 24444 24571 24775 24828 24845 25016 25196 25255 25302 25409 25503 25630 25649 25742 25818 25864 26083 26115 26131 26292 26303 26340 26363 26491 26550 26614 26898 26900 26966 27060 27124 27138 27243 27310 27417 27423 27765 28083 28139 28225 28249 28315 28339 28454 28479 28492 28517 29016-29017 29570 29620 29675 29714 29772 30012 30446 31190 31211 31391 31399 31430 31451 31461 31559 31599 31656 31663-31664 31773 31894 31930 31986 32311 32345 32660 32764 34675 35706 35786 36058 36090 36151 36188 36554 36602 36785 38763 40434 40479 40527 40730 40762 40766 40874 40885 42901 42980 44147 44247 44730 44805 44908 45011 46963-46964 48023 48123 48595 48610 48798 48846 48965 490719.939104355462015e-24 3.916500758235022e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/684/A202?format=asciiOpticalRadiodefaultJ/A+A/684/A202/tableNumerical quantities that allowed to built up the analyses and conclusions of the articlerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSimbadSimbad column added by the CDSmeta.ref.urlcharIERSIERS B1950 source name (HHMM+DDd)meta.id;meta.maincharDVGaia-ICRF3 vector lengthmaspos.angDistancefloatE_DVGaia-ICRF3 vector length errormasstat.error;stat.maxfloatthetaVGaia-ICRF3 vector position-angledegpos.posAng;pos.pmintE_thetaVGaia-ICRF3 vector position-angle errordegstat.error;stat.maxintDGGaia-MOJAVE core vector lengthmaspos.angDistancefloatE_DGGaia-MOJAVE core vector length errormasstat.error;stat.maxfloatthetaGGaia-MOJAVE core vector position-angledegpos.posAng;pos.pmintE_thetaGGaia-MOJAVE core vector position-angle errordegstat.error;stat.maxintMOJCOMP[0/57]? Identifier of MOJAVE component closest to Gaia (MCCG) following the numbering of Lister et al. (2021ApJ...923...30L, Cat. J/ApJ/923/30)meta.idintnullableDMMCCG-MOJAVE core vector lengthmaspos.angDistancefloatthetaMMCCG-MOJAVE core position-angledegpos.posAng;pos.pmcharDGMMCCG-Gaia vector lengthmaspos.angDistancefloatE_DGMMCCG-Gaia vector length errormasstat.error;stat.maxfloatthetaGMMCCG-Gaia vector position-angledegpos.posAng;pos.pmintE_thetaGMMCCG-Gaia vector position-angle errordegstat.error;stat.maxintNormDGGaia-MOJAVE core normalized separationpos.distancefloatNormDGMMCCG-Gaia normalized separationpos.distancefloatVG? Gaia proper motionmas/yrpos.pmfloatnullableE_VG? Gaia proper motion errormas/yrstat.error;stat.maxfloatnullablephiG? Gaia proper motion position-angledegpos.pmintnullableE_phiG? Gaia proper motion position-angle errordegstat.error;stat.maxintnullableVM? MCCG proper motionmas/yrpos.pmfloatnullableE_VM? MCCG proper motion errormas/yrstat.error;stat.maxfloatnullablephiM? MCCG proper motion position-angledegpos.pmintnullableE_phiM? MCCG proper motion position-angle errordegstat.error;stat.maxintnullableMOJFLUX? MCCG 15 GHz fluxJyphot.flux.density;em.radio.12-30GHzfloatnullableType[0/7]? Activity Type (NED Homogenized Classification) (1)src.classintnullablez? Redshift from NEDsrc.redshiftfloatnullableGmagGaia G magnitudemagphot.mag;em.optfloatOPol? Optical polarization from Hutsemekers et al. (2018A&A...620A..68H, Cat. J/A+A/620/A68)phys.polarizationfloatnullableRPol? Maximum of fractional radio polarization from Lister et al. (2018ApJS..234...12L, Cat. J/ApJS/234/12)phys.polarizationfloatnullableBP-RP? Gaia BP-RP colour indexmagphot.color;em.opt.B;em.opt.RfloatnullableRUWE? Gaia RUWEstat.errorfloatnullableVLBIStab? VLBI stability from geodetic time seriesmasstat.fit.paramfloatnullableCat[1/4] Category (1: C, 2: B, 3: J, 4: O)meta.codeint_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.main