GALAXY EVOLUTION

OPTICAL AND IR SURVEYS

Lucia PozzettiINAFOsservatorio Astronomico di Bologna

PEOPLE INVOLVED IN BOLOGNA

INAF-OAB: Bardelli, Cappi, Ciliegi, Gruppioni, Merighi, Mignoli, Pozzetti, Zamorani, Zucca, Post-doc: Lanzoni, (McCracken), PozziINAF-IRA: Bondi, Lari, Vettolani, ZanichelliUniBo: Marano, Gregorini, Post-doc: Bolzonella, 2

students

Funds (>2000): 2 ASI 3 Cofin Inaf CNRk€ 30 + 9 53 + 110 + 87 15.5 93

Publications since 1998 (2000) o 79 (64) Refereed + 10 in press (5 more than 50 citations, 2 more than 100)o ~100 (~80) Conference + Invited

GALAXY EVOLUTIONDeep optical to Far-IR surveys

to trace galaxy evolution and formation:

o Star Formation History (SFH) o Epoch of Mass Assembly o High-z galaxies (EROs, LBGs)

Stellar Mass Density (Dickinson et al. 2003)

Star Formation History (Madau, Pozzetti, Dickinson 1998)

Expertise:

Data: Optical/Far-IR data & spectral analysis (e.g. Lari Method for ISO)Analysis: Luminosity + Mass Function, SFH Spectral evolutionary models and Photometric redshift (e.g HyperZ)

Modeling: Hierarchical, PLE, Fundamental Plane

International Commitees (OAB): ESO- panel OPC, TNG-TAC, ESO Survey working group

Telescopes used: ESO (1.5m,2.2m,3.6m,NTT,VLT); ISO; CFHT, 2dF, VLA, public: HST, Chandra

MAIN PROJECTS AND SURVEYS

o ELAIS (European Large Area ISO

Survey)

o K20 (Large Programme VLT: K<20 redshift

survey)

o VVDS (VIMOS-VLT Deep Survey)

THE ELAIS MID-IR SURVEYTHE ELAIS MID-IR SURVEYTHE ELAIS MID-IR SURVEYTHE ELAIS MID-IR SURVEY

Gruppioni, Ciliegi, Pozzi, Zamorani (INAF-OAB), Gruppioni, Ciliegi, Pozzi, Zamorani (INAF-OAB), Lari (INAF-IRA)Lari (INAF-IRA), Franceschini (UniPd), Franceschini (UniPd)LaFranca, Matute (UniRm3LaFranca, Matute (UniRm3))

Gruppioni, Ciliegi, Pozzi, Zamorani (INAF-OAB), Gruppioni, Ciliegi, Pozzi, Zamorani (INAF-OAB), Lari (INAF-IRA)Lari (INAF-IRA), Franceschini (UniPd), Franceschini (UniPd)LaFranca, Matute (UniRm3LaFranca, Matute (UniRm3))

ITALIAN ITALIAN COLLABORATORS:COLLABORATORS:

ITALIAN ITALIAN COLLABORATORS:COLLABORATORS:

OTHER COLLABORATORS:OTHER COLLABORATORS:OTHER COLLABORATORS:OTHER COLLABORATORS:

ELAIS Consortium ELAIS Consortium (9 (9 European institutes, originally,European institutes, originally, 32 32 at the momentat the moment))ELAIS Consortium ELAIS Consortium (9 (9 European institutes, originally,European institutes, originally, 32 32 at the momentat the moment))

EEuropean uropean LLarge arge AArea rea IISO SO SSurveyurvey (P.I. Rowan-(P.I. Rowan-Robinson):Robinson): the largest Open Time project with the largest Open Time project with ISO ISO satellite (375h)satellite (375h)::12 deg12 deg22 ((88 in the North and in the North and 44 in the in the South) South) observed at observed at 15 & 90 15 & 90 mm with with ISO-CAM & ISO-CAM & PHOTPHOT

EEuropean uropean LLarge arge AArea rea IISO SO SSurveyurvey (P.I. Rowan-(P.I. Rowan-Robinson):Robinson): the largest Open Time project with the largest Open Time project with ISO ISO satellite (375h)satellite (375h)::12 deg12 deg22 ((88 in the North and in the North and 44 in the in the South) South) observed at observed at 15 & 90 15 & 90 mm with with ISO-CAM & ISO-CAM & PHOTPHOT

ELAIS-S1 (4 degELAIS-S1 (4 deg22))::Catalogue of 462 Catalogue of 462 source 90% (100%) source 90% (100%) complete at 2 (3) mJy:complete at 2 (3) mJy: 320 extragalactic 320 extragalactic objects objects (Lari, Pozzi, Gruppioni et (Lari, Pozzi, Gruppioni et al., al., 2001,MNRAS,325,1173)2001,MNRAS,325,1173)

Source Counts in the Source Counts in the range 0.5 - 100 mJy:range 0.5 - 100 mJy:strong evolution for strong evolution for starburst galaxiesstarburst galaxies(Gruppioni, Lari, Pozzi et (Gruppioni, Lari, Pozzi et al. 2002, MNRAS, 335,831)al. 2002, MNRAS, 335,831)

Photometric IDs Photometric IDs (80% R<23) (80% R<23) [12n [12n ESO+1.5m]ESO+1.5m]

Spectroscopic IDsSpectroscopic IDs(75% R<21.5 (75% R<21.5 ~250 ~250

objsobjs))[2dF(2n) + ESO (15n)][2dF(2n) + ESO (15n)](La Franca, Gruppioni et (La Franca, Gruppioni et

al., 2003, AJ, submitt.) al., 2003, AJ, submitt.)

Photometric IDs Photometric IDs (80% R<23) (80% R<23) [12n [12n ESO+1.5m]ESO+1.5m]

Spectroscopic IDsSpectroscopic IDs(75% R<21.5 (75% R<21.5 ~250 ~250

objsobjs))[2dF(2n) + ESO (15n)][2dF(2n) + ESO (15n)](La Franca, Gruppioni et (La Franca, Gruppioni et

al., 2003, AJ, submitt.) al., 2003, AJ, submitt.)

ELAIS-S1ELAIS-S1

FirstFirst derivation of 15- derivation of 15-m Luminosity m Luminosity Function of Star-Function of Star-forming galaxies: forming galaxies: strong evolutionstrong evolution both both ininluminosity (1+z)luminosity (1+z)3.5 3.5 andanddensity (1+z)density (1+z)3.83.8 (Pozzi, Gruppioni et al., (Pozzi, Gruppioni et al., 2003, ApJ, submitted)2003, ApJ, submitted)

FirstFirst derivation of 15- derivation of 15-m Luminosity m Luminosity Function of Star-Function of Star-forming galaxies: forming galaxies: strong evolutionstrong evolution both both ininluminosity (1+z)luminosity (1+z)3.5 3.5 andanddensity (1+z)density (1+z)3.83.8 (Pozzi, Gruppioni et al., (Pozzi, Gruppioni et al., 2003, ApJ, submitted)2003, ApJ, submitted)

redshift

K20 REDSHIFT SURVEYP.I. A. Cimatti (INAF-OAA)

K20 team: Pozzetti, Mignoli, Zamorani (INAF-OAB), Daddi, Renzini, D’Odorico, Gilmozzi, (ESO) Fontana, Giallongo, Menci, Poli (OARm), Saracco (OABr), Cristiani (OATs), Broadhurst (HUJ)o Large Programme: 17 nights VLT (MOS with FORS1 & FORS2 + ISAAC)o Ks<20 selected sample: ~550 objectso Area: 52 arcmin^2 on 2 fields (CDFS+Q0055)o UBVRIzJKs multi-band imaging [public + 45h

NTT+VLT]

92% redshift completenessHighest spectroscopic redshift completeness in

the NIR

Scientific objectives

Advantages of a K-selected sample:o Less dust extinctiono More sensitive to stellar mass

Objectives:o To test galaxy evolution models o To search massive old high-z (z>1)

ellipticals (EROs)o To probe the near-IR luminosity function

and stellar mass function up to z~2

o First spectroscopic sample of EROs:(Cimatti, Daddi et al. 02, Daddi et al. 02) :31% old ellipticals @ z~1 age>~3 Gyrs, zform>2 33% dusty starbursts 20% of SFD @ z~1

o Redshift distribution (Cimatti, Mignoli et al. 02, Cimatti, Pozzetti et al. 02):

Substantial population at high-z (32% at z>1) Underpredicted by hierarchical models

deficit

excess

o Near-IR Luminosity Function up to z~2 (Pozzetti, Cimatti, al. 03) : Mild luminosity evolution up to z~1.5Luminous red ellipticals fully in place up to z~1.5

mild evolution deficit

excess

o Stellar Mass Function up to z~2(Fontana, Pozzetti, al. 03, submitted) : Slow decrease (~50%) of mass density up to z~2

Most of current hierarchical merging models do not match the above results

deficit

K20 Follow-up K20 team + : Lanzoni (INAF-OAB), Vernet, diSerego Alighieri (OAA), Fasano, Pignatelli (OAPd), Cassata, Franceschini (UniPd), Fomalont, Kellerman (NRAO)

o Spectral analysis and evolution (Mignoli et al., Pozzetti et al., in prep.)

o X-ray analysis (public Chandra data): EROs (Brusa et al. 02), clustering (Gilli et al. 03)

o Morphological analysis from GOODS-ACS images Luminous starbursts/mergers @z~2-2.5: building blocks of massive spheroids ? (Daddi et al. 03) Morphologies of EROs (Cimatti et al. 03 ): ~40% early, 30%spiral, 30%

Irr.o High resolution spectroscopy (4 nights VLT+FORS2) Tully-Fisher (Vernet et al., in prep.), Fundamental-Plane (Cimatti et al. , Lanzoni et al. in prep), spectral population analysis (Pozzetti et al., in prep)o Radio observations (VLA-1.4 GHz) (Fomalont et al., in prep)

VVDS SURVEYP.I. Le Fevre (LAM) + Co P.I. Vettolani (INAF-IRA)consortium: Bardelli, Cappi, Ciliegi, Merighi, Pozzetti, Zamorani, Zucca,(McCracken) (INAF-OAB), Bondi, Vettolani, Zanichelli (INAF-IRA), Marano,Gregorini,Bolzonella,Bongiorno + 2 students (UniBo), + INAF-OABr, INAF-IASF, INAF-OANa, + LAM (Marsiglia), OMP (Tolosa)o Area: 4 fields 2x2 deg^2 o deep BVRI (CFHT) U (ESO+2.2m) JK (ESO+NTT) imaging Multicolor catalog 106 objects (McCracken et al. 03)

o GTO Programme: 50 nights VLT+VIMOSo deep survey IAB<24: ~25,000 z, wide IAB<22.5: ~50,000

z 29 nights (21 clear) in 2002 ~21,000 spectra+ 5 half nights in december 2003

+ deep VLA (~60h at 1.4Ghz) on 1 deg^2 (Bondi, Ciliegi et al. 03)

o Evolution of the optical luminosity function and star formation rate of various types of galaxies (ellipticals, star-forming galaxies etc.) in various density environments

o Evolution of the clustering properties o High-z galaxies (LBGs, EROs)

VVDS is the deepest and largest optical redshift survey to date to study galaxy evolution up to z~1.5Complementary to wide local survey, like SDSS and 2dFin competition with DEIMOS-DEEP2 (P.I. M. Davis) at Keck

Scientific results from the spectroscopic surveyare still a few months ahead

Future ProjectsLegacy Programs in which we are

involved:o SWIRE (Sirtf Wide-area Infrared Extragalactic Survey: 851h SIRTF: P.I. Lonsdale) + ESO (WFI + VIMOS + 150h SOFI) + ATCA (120h)

o GOODS (The Great Observatories Origins Deep Survey: 647h SIRTF: P.I. Dickinson) + HST + VLT

o COSMOS (590 orbits HST) + CFHT + Subaru + KPNO + VLT-VIMOS + XMM + VLA + SIRTF + GALEX

+IRAM

Other programs:o Massive Galaxies at z~2 (4n VIMOS + Subaru, P.I. Renzini)

o GMASS (Galaxy Mass Assembly: ESO-LP: 145h FORS2, P.I. Cimatti)

GRAZIE

Provided by Lara