GAIA Galaxy Survey a multi-colour galaxy survey with GAIA
- 格式:pdf
- 大小:145.82 KB
- 文档页数:6
a
rXiv:astro-ph/0110144v2 27 Oct 2001J.Phys.IVFrance1(2008)Pr1-1
cEDPSciences,LesUlis
GAIAGalaxySurvey:amulti-colourgalaxysurveywithGAIA
MattiaVaccari1
1DipartimentodiAstronomiaandCISAS“GiuseppeColombo”,Universit`adiPadova,Vicolodell’Osservatorio2,I-35122,Padova,Italy(e-mail:vaccari@pd.astro.it)
Abstract
TheperformanceexpectedfromagalaxysurveytobecarriedoutwithGAIA,theGAIAGalaxySurvey,isoutlined.Fromastatisticalmodelofgalaxynumberdensity,sizeandsurfacebrightnessdistribution,andfromdetailednumericalsimulationsbasedonrealimages,itisconservativelyestimatedthatGAIAwouldbeabletodetectandobserveabout3milliongalaxiesbrighterthanV≃17andtoprovidemulti-colourandmulti-epochbroad-bandphotometryofthesewithanend-of-missionangularresolutionof≃0.35arcsecandaphotometricaccuracyofsimeq0.2mag/arcsec2atµV=20mag/arcsec2.Thesubstantialscientificcaseforperformingsuchasurveyandtheadditionaleffortsrequiredintermsofmissionpreparation,operationsandtelemetryarealsodiscussed.
1INTRODUCTION
Sincetheverybeginningofthefeasibilitystudies,theGAIAmissiondesignwasdrivenby
theneedofdeterminingthepositionandthebrightnessofhugenumbersofstarswiththe
uttermostaccuracy.DuringtheConceptandTechnologtStudycompletedinJuly2000(see[9]
and[2]),however,itclearlyemergedthatsuchastar-drivenmissioncouldalsoprovide,several
socalledby-productswhichwouldsubstantiallyenrichitsalreadyimpressivescientificyield.In
particular,itwasrealizedthatthescientificcaseforGAIAimagingofhigh-surfacebrightness
skyregionssuchasthecentralregionsofnearbygalaxieswasdramatic.
Theissuesconnectedwiththisopportunityhavebeenaddressedinacertaindetailina
numberofstudies(see[10],[11],[8]and[12]),andsuchobservationswereincludedinthemission
baselinedesignasdescribedin[2]underthenameofGAIAGalaxySurvey.Inthispaperthe
currentideasontheimplementationofsuchasurveyandontheexpectedperformanceare
presented.
InSection2theoverallstrategyforgalaxydetectionandobservationwithGAIAisoutlined.
InSections3and4thedetectionandobservation,respectively,arediscussedingreaterdetail
andresultsofdedicatedstudiesarepresented.InSection5thesubstantialscientificcasefor
performingsuchasurveyisbrieflysketched,andinSection6theadditionaleffortsrequiredin
termsofmissionpreparation,operationsandtelemetryarediscussed.
Onlythemeasurementofrelativelylargeenhancementsofthesurfacebrightnesswithre-
specttotheskybackgroundisdiscussedhere,althoughitisbelievedthattherathersimilar
issueoftheobservationofGalacticNebulaecouldbeaddressedalongthesamelines.The
measurementofthesurfacebrightnessoftheskybackground,instead,callsforasubstantially
differentapproach,asdescribedin[6].Pr1-2JOURNALDEPHYSIQUEIV
2GALAXYDETECTIONANDOBSERVATIONWITHGAIA
Duringitsscientificoperations,theGAIAsatellitewillcontinuouslyspinaboutitssymmetry
axis,andthechargescontainedintheCCDpixelswillcorrespondinglybeshiftedalong-scanto
integratetheimageforalongerexposuretime,atechniqueknownasTime-DelayIntegration
(TDI).InordertolimittheCCDs’readingfrequencyandthecorrespondingreadnoiseand
telemetryrate,adedicatedCCDreadoutprocesswasdevised,consistingindetectingobjects
astheyenterthefieldofview,determiningtheirposition,magnitudeandsignal-to-noisera-
tio,and,ifthelatterexceedsacertainlimit,collectingdatafromregionsaroundsuchstars
only.Whilethisapproachwasthesubjectofdetailedstudiesasfaraspoint-likeobjectswere
concerned,leadingtothedefinitionoftheAstrotelescopes’focalplaneandtheCCDbinning
strategydescribede.g.in[5],theprocessofgalaxydetectionandobservationcalledfora
ratherdifferentapproachinordertoidentifyandmeasurefaintsurfacebrightnessvariations.
Asfirstsuggestedin[3],galaxiescouldbedetectedintheAstroSkyMapper(ASM)asan
averagesurfacebrightnesssignificantlyinexcessoverthelocalskybackgroundandobserved
indifferentcoloursintheBroadBandPhotometer(BBP).Thisobservingstrategypreventing
fromoptimallyobservingstarswheneveragalaxyisbeingobserved(whichishoweverlessthan
1%percentofthetime),itcouldbeimplementedinoneofthetwoAstrosonly.
Inordertofollowthisgeneralidea,onehadtooptimize:
•thesizeoftheareasoverwhichtheaveragesurfacebrightnessandthelocalskyback-
groundvaluesarecomputed.Itispresentlyenvisagedtodeterminetheformerthrough
trimmedmedianfilteringofASM1samplesof2×2pixelsandthelatteroverafew
degreesofscanwiththesamealgorithm.However,theexactmethodusedtodetermine
thelocalskybackgroundisnotofinterestforourpurposes,sincethereadnoiseisbyfar
thedominantnoisesource.
•thevalueforthedetectionareaandS/Nlimitsothatusefuldataaretransmittedto
thegroundwithoutbeingswampedinlessinterestingdatafromtheMilkyWayorthe
zodiacallight.Thelargerthedetectionarea,thefainterthedetectionlimitcanbefor
objectsofconstantsurfacebrightness,iftheerrorontheskybackgroundisnegligible.
Ontheotherhand,thedetectionareashouldbesmallenoughthatalargenumberof