GAIA Galaxy Survey a multi-colour galaxy survey with GAIA

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rXiv:astro-ph/0110144v2 27 Oct 2001J.Phys.IVFrance1(2008)Pr1-1

c󰀃EDPSciences,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