Optical Variability Properties of High Luminosity AGN Classes CS

55 Pages·2004·2.98 MB·English

J.Astrophys.Astr. (2004) 25,1–55
OpticalVariabilityPropertiesofHighLuminosityAGNClasses
C.S.Stalin1;2;3,Gopal-Krishna2,RamSagar1 &PaulJ.Wiita4
1AryabhattaResearchInstituteofObservationalSciences(ARIES),ManoraPeak
Nainital263129,India.
2NationalCentreforRadioAstrophysics,TIFR,PuneUniversityCampus,Pune411007,India.
3LaboratoiredePhysiqueCorpusculaireetCosmolgie,CollegedeFrance,11pl.Marcelin
Berthelot,F-75231,ParisCedex5,France.
4DepartmentofPhysics&Astronomy,MSC8R0314,GeorgiaStateUniversity,Atlanta,
Georgia30303-3088,USA.
Received2003June24;accepted2004June22
Abstract. We present the results of a comparative study of the intra-
night optical variability (INOV) characteristics of radio-loud and radio-
quietquasars,whichinvolvesasystematicintra-nightopticalmonitoringof
sevensetsofhighluminosityAGNscoveringtheredshiftrangez’0:2to
z ’2:2.Thesample,matchedintheopticalluminosity–redshift.MB−z/
plane, consists of seven radio-quiet quasars (RQQs), eight radio lobe-
dominatedquasars(LDQs),fiveradiocore-dominatedquasars(CDQs)and
sixBLLacobjects(BLs).SystematicCCDobservations,aidedbyacare-
ful data analysis procedure, have allowed us to detect INOV with ampli-
tudesaslowasabout1%.Presentobservationscoveratotalof113nights
(720hours)withonlyasinglequasarmonitoredascontinuouslyaspossi-
bleonagivennight.Consideringthecasesofonlyunambiguousdetections
ofINOVwehaveestimateddutycycles(DCs)of17%,12%,20%and61%
forRQQs,LDQs,CDQs,andBLs,respectively.Themuchloweramplitude
andDCofINOVshownbyRQQscomparedtoBLsmaybeunderstoodin
terms of their having optical synchrotron jets which are modestly misdi-
rectedfromus.Fromourfairlyextensivedataset,nogeneraltrendofacor-
relationbetweentheINOVamplitudeandtheapparentopticalbrightnessof
thequasarisnoticed.ThissuggeststhatthephysicalmechanismsofINOV
andlongtermopticalvariability(LTOV)donothaveaone-to-onerelation-
shipanddifferentfactorsareinvolved.Also,theabsenceofaclearnegative
correlationbetweentheINOVandLTOVcharacteristicsofblazarsofour
samplepointstowardaninconspicuouscontributionofaccretiondiskfluc-
tuationstotheobservedINOV.TheINOVdutycycleoftheAGNsobserved
in this program suggests that INOV is associated predominantly with the
highly polarized optical emission components. We also report new VLA
imagingoftwoRQQs.1029C329&1252C020/inoursamplewhichhas
yieldeda5GHzdetectioninoneofthem.1252C020IS ’1mJy/.
5GHz
Keywords. Galaxies:active—galaxies:jets—galaxies:photometry—
quasars:general.
1
2 C.S.Stalinetal.
1. Introduction
Thequestionofwhyonlyasmallfractionofquasarsareradio-loudhasbeendebatedfor
almostfortyyears.Variousargumentshavebeenputforwardtoexplainthisapparent
radio-loud/radio-quietdichotomy.Althoughtheexistenceofthedichotomyhaseven
been questioned (e.g., Goldschmidt et al. 1999; White et al. 2000), a recent careful
analysisofthetrickyselectioneffectsindicatesthatitmaybereal(Ivezicetal.2002).
It has been argued recently that the radio emission correlates with the mass of the
nuclear black hole (e.g., Dunlop et al. 2003 and references therein); however, this
assertionhasbeenquestioned(Ho2002;Woo&Urry2002).McLure&Dunlop(2001)
stressthepossibleimportanceofaccretionrateandchangesinaccretionmodetothis
dichotomy.
Onthetheoreticalside,twomainapproacheshavebeenputforwardtoexplainthis
dichotomy. In one scenario, the jets in RQQs are absent or inherently weak. Some
possiblemechanismsidentifythisdifferentiatingfactorwiththespinoftheblackhole
(Wilson&Colbert1995;Blandford2000),ormagneticconfigurations(Meier2002).
Wills (1996) suggested that all quasars launch jets but those aimed into a galactic
diskaredestroyedbyinteractionswiththedensegasandthusappearradio-quiet.An
extreme variant of this possibility is the hypothesis that the relativistic jets in RQQs
arelargelysnuffedoutbeforeescapingthenuclearregionitselfduetoheavyinverse
Comptonlosses(Kundt2002).Asaconsequence,jetsonradioemittingphysicalscales
arequenched,eventhoughtheymightemitsubstantialamountsofnon-thermaloptical
synchrotronemissiononmicro-arcsecondscales.Unfortunately,such(cid:22)arcsecscales
are beyond the reach of any existing imaging telescopes and the only way to probe
theirconditionsisthroughfluxvariabilityobservations.
Althoughintra-nightopticalvariability(INOV)or“microvariability”wasconvinc-
inglyestablishedforblazarsoveradecadeago(e.g.,Miller,Carini&Goodrich1989;
Carini, Noble & Miller 1998), the question of whether RQQs also show INOV has
remainedcontroversial(Gopal-Krishnaetal.1995,2000;Jang&Miller1995,1997;
Rabbette et al. 1998; de Diego et al. 1998; Romero et al. 1999; Carini et al. 1999).
Likewise,thecauseofINOVisstillamuchdebatedissue.However,forblazars(CDQs
and BL Lacs) which are believed to be dominated by non-thermal Doppler boosted
emission from jets (e.g., Blandford & Rees 1978), the occurrence of rapid intensity
variations in both the radio and optical bands is believed to be due to shocks propa-
gatingdowntheirrelativisticjets(e.g.,Marscher&Gear1985).Intra-nightvariability
in blazars may well arise from instabilities or turbulent fluctuations in the flow of
such jets (e.g., Hughes, Aller & Aller 1992; Marscher, Gear & Travis 1992). Alter-
nate models, which invoke accretion disk instabilities or perturbations (e.g., Man-
galam & Wiita 1993; for a review see Wiita 1996) may also explain INOV, partic-
ularly in RQQs, where any contribution from the jets, if they are at all present, is
weak.
WhileconclusiveevidenceforthepresenceofjetsinRQQsisfarfromclear,deep
VLAobservationshintatthepresenceofweakjetseveninRQQs(Kellermannetal.
1989;Miller,Rawlings&Saunders1993;Kellermannetal.1994;Papadopoulosetal.
1995; Kukula et al. 1998; Blundell & Beasley 1998; Blundell & Rawlings 2001).
The existence of incipient nuclear jets in RQQs have also been inferred from radio
spectralindexmeasurementsofopticallyselectedquasarsamples(Falcke,Patnaik&
Sherwood1996).IfindeedopticalsynchrotronjetsexisteveninRQQs,thenafairly
OpticalVariabilityinLuminousAGNs 3
robustsignatureofsuchun-imageable(becauseatthemicro-arcsecondscale)jetscan
comefromdetectionofINOVatthelevelexhibitedbytheirradioloudcounterparts,
namelytheLDQs.Topersuetheseissues,aprojecttosearchforINOVinthefourmajor
classesofpowerfulAGNswasinitiatedin1998asacollaborativeeffortbetweenthe
Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital and the
National Centre for Radio Astrophysics (NCRA), Pune. The present paper presents
thedetailedresultsofthisproject,partofwhichhasbeenpublishedelsewhere(Gopal-
Krishnaetal.2003,hereafterGSSW03;Stalinetal.2004,SGSW04;Sagaretal.2004,
SSGW04).
2. Selectionofthesample
AGNs in general, have very different observational characteristics including a huge
range in luminosity, redshift and power across the electromagnetic spectrum. Also,
the co-moving number density of quasars detected at a given absolute magnitude is
foundtoundergoarapidevolutionwithredshift(Schmidt&Green1983;Boyleetal.
2000; Wisotzki 2000). Therefore, sample selection is crucial for studying INOV of
quasars. To avoid selection biases introduced by differences in luminosity and red-
shift,theobjectswereselectedsuchthatallobjectsinagivensethavesimilaroptical
magnitudes, in addition to having very similar redshifts; they are thus well matched
in the optical luminosity–redshift plane. Our sample, selected from the catalog of
Ve´ron-Cetty&Ve´ron(1998),consistsofsevensetsofAGNscoveringatotalredshift
range from z D 0:17 to z D 2:2. Each set was designed to consist of a radio-quiet
quasar(RQQ),aradiolobe-dominatedquasar(LDQ),aradiocore-dominatedquasar
(CDQ) and/or a BL Lac object (BL). These seven sets cover seven narrow redshift
intervals centered at z D 0:21, 0.26, 0.35, 0.43, 0.51, 0.95 and 1.92. However, it
was not possible to find seven complete sets that satisfied our other observationally
dictatedcriteria(sufficientlybrighttoallowdensetemporalsamplingandhavingsev-
eral suitable nearby comparison stars), so our entire sample actually consists of 26,
not 28, QSOs with the distribution of 7 RQQs, 8 LDQs, 5 CDQs and 6 BLs. The
slight unevenness in number is because the two QSOs 1308C326 and 1512C370
were initially selected as CDQs, but better radio data classified 1512 C 370 as an
LDQ (see SGSW04), while the blazar 1308 C 326 was found to be a BL Lac (see
SSGW04). Due to the paucity of BL Lacs at low z, one object .1215C303/ serves
as a member of both Sets 1 and 2, and none was available in the highest redshift
bin. The general properties of the objects monitored in this program are given in
Table1.
ThemagnituderangefortheQSOsinoursampleis−30:0<MB <−24:3(assum-
ingH D50kms−1Mpc−1;q D0).Thisimpliesthatwearedealingwithluminous
0 0
AGNs,whicharelegitimatelyclassifiedasQSOs,andinallcasestheunderlyinggalaxy
contaminationtotheluminosityoftheAGNis< 10%.Moreover,sincetheAGNof
thefourdifferenttypesaresimilarlydistributedinthez−MB plane,thisselectioncri-
terionminimisesselectionbiasessuchasK-corrections,evolutionaryeffectsandany
otherdifferenceslinkedtoredshiftandluminosity.Conservatively,wehaveincluded
in our sample only those RQQs for which the K-corrected ratio of 5GHz to 2500 Å
flux densities is less than 1 i.e., R(cid:3) < 1 (see Table 1) even though the usual crite-
rionusedtocallaQSOanRQQisR < 10.R D f.5GHz/=f.B/;Kellermannetal.
1989).
4 C.S.Stalinetal.
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OpticalVariabilityinLuminousAGNs 5
3. Radioobservationsandreductions
SinceradiofluxdatawerenotavailablefortwoofourQSOs(1252C020and1029C
329),inordertoascertaintheirradioclassification,wetookVLA1snapshotsat5GHz
in the BnC configuration, in a dual intermediate frequency mode with a total on-
sourceintegrationtimeof10minutes.Theresultingimages,madeusingtheCLEAN
algorithmwithintheAIPSsoftware,areshowninFig.1(rmsnoise(cid:24)50(cid:22)Jy).While
theQSO1252C020wasfoundbeassociatedwithanextendedweakradiosourceof
1(cid:6)0:1mJy,theotherQSO,1029C329,hasnoradiocounterpartdowntoa3-sigma
limitof0.15mJy.ThereforebothareproperlyclassifiedasRQQs,withR D0:52and
R <0:23,respectively.
1252+020 (Radio Quiet Quasar)
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Figure1. (Continued)
1TheVeryLargeArray(VLA)oftheNationalRadioAstronomyObservatoryisoperated
byAssociatedUniversities,Inc.underacooperativeagreementwiththeNationalScience
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6 C.S.Stalinetal.
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Figure1(a–b). VLA5GHztotalintensityimagesofthequasars1252C020(left)and1029C329
(right).Thesynthesisedbeamsareshownintheinsetboxes.
4. Opticalobservationsanddatareductions
4.1 Theinstrument
The optical observations of the selected quasars were carried out using the 104cm
Sampurnanand telescope of the ARIES, Nainital. This is an RC system with a f/13
beam(Sagar1999).Thedetectorusedfortheobservationswasacryogenicallycooled
2048(cid:2)2048pixel2 CCD,exceptpriortoOctober1999,whenasmallerCCDofsize
1024(cid:2)1024pixel2 was used. In each CCD, a pixel corresponds to a square of 0.38
arcsecsize,coveringatotalskyareaofabout120(cid:2)120 inthecaseoflargerCCDand
about60(cid:2)60inthecaseofsmallerCCD.ToincreasetheS/Nratio,observationswere
carriedoutin2(cid:2)2binnedmode.Practicallyalltheobservationswerecarriedoutusing
Rfilter,exceptontwonights,wherequasi-simultaneousRandIfilterobservationswere
done.ThechoiceoftheRfilterinthisobservationalprogramisbecauseofitsbeing
atthemaximumresponseoftheCCDsystems;thusthetimeresolutionachievablefor
eachobjectismaximised.
OpticalVariabilityinLuminousAGNs 7
4.2 Observingstrategy
The main goal of this program was to obtain lengthy temporally dense data trains
for each object on each night it was observed, in order to be able to detect low level
intra-night variations at high S/N. The optical monitoring of blazars has shown that
theprobabilityofobservingINOVinagivennightisgreatlyenhancedbycontinuous
monitoringforatleast3to4hours(Carini1990).Accordingly,weattemptedtomonitor
eachobjectforaminimumof5hourspernight,withatimeresolutionoftheorderof
10minutes.However,onoccasionswhentheobjectwasinafaintstate,thesampling
timecouldbeupto30minutes.
Another important strategy was to center the field of view so as to cover as many
suitablecomparisonstarsaspossiblewithintheCCDframe.Foreachofourquasars
wecouldgetatleasttwo,butoftenmore,comparisonstarswithin1magnitudeofthe
quasar’s brightness in the frame. Several putative sources were eliminated from our
sampleiftheyhadnosuitablecomparisonstarsintheirvicinities.Theavailabilityof
multiple comparison stars allowed us to identify and discount any comparison star
whichitselfvariedduringagivennight,thusallowingreliabledifferentialphotometry
of the QSO. The positions and apparent B and R magnitudes of all the comparison
starsusedinourdifferentialphotometryaregiveninSGSW04andSSGW04andso
willnotberepeatedhere.Theentireprogrammeconsistsofobservationson113nights
fromOctober1998throughMay2002,addingupto720hoursofusefulobservations
(i.e.,6.4hours/nightonaverage).Alogoftheobservationsalongwiththebasicresults
aregiveninTable2.
4.3 Datareduction
Preliminary processing of the images as well as the photometry was done using the
IRAF2 software. The bias level of the CCD is determined from several bias frames
(generally more than seven) taken intermittently during our observations over the
night. A mean bias frame was formed using the task zerocombine in IRAF which
was then subtracted from all the image frames of the night. Care was also taken in
formingthemeanbiasframesuchthattheyarenotaffectedbycosmic-ray(CR)hits.
TheroutinestepofdarkframesubtractionwasnotperformedastheCCDsusedinthe
observationswerecryogenicallycooledto−120(cid:14)Catwhichtemperaturetheamount
of thermal charge is negligible for the exposure times of the present observations.
Flatfieldingwasdonebytakingseveraltwilightskyframeswhichwerethenmedian
combined to generate the flat field template which was then used to derive the final
frames; any errors in the flat field template were well within 0.1%. Finally CR hits
seen in the flat fielded target frames were removed using the facilities available in
MIDAS3.
2IRAFisdistributedbytheNationalOpticalAstronomyObservatories,whichisoperated
by the Association of Universities for Research in Astronomy, Inc. under co-operative
agreementwiththeNationalScienceFoundation.
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Contin Object(type)C2932QQ) C0937DQ) C5532DQ) C1942L) C4829QQ) −5007DQ)
( 0R 7L 9C 2B 7R 3L
2. 1( 0( 0( 0( 0( 0(
e
bl
Ta Setno.5. 6.