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GALAXY EVOLUTION OPTICAL AND IR SURVEYS Lucia Pozzetti INAF Osservatorio Astronomico di Bologna.

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Presentation on theme: "GALAXY EVOLUTION OPTICAL AND IR SURVEYS Lucia Pozzetti INAF Osservatorio Astronomico di Bologna."— Presentation transcript:

1 GALAXY EVOLUTION OPTICAL AND IR SURVEYS Lucia Pozzetti INAF Osservatorio Astronomico di Bologna

2 PEOPLE INVOLVED IN BOLOGNA INAF-OAB: Bardelli, Cappi, Ciliegi, Gruppioni, Merighi, Mignoli, Pozzetti, Zamorani, Zucca, Post-doc: Lanzoni, (McCracken), Pozzi INAF-IRA: Bondi, Lari, Vettolani, Zanichelli UniBo: Marano, Gregorini, Post-doc: Bolzonella, 2 students Funds (>2000): 2 ASI 3 Cofin Inaf CNR k 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

3 GALAXY EVOLUTION Deep 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)

4 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

5 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)

6 THE ELAIS MID-IR SURVEY Gruppioni, Ciliegi, Pozzi, Zamorani (INAF-OAB), Lari (INAF-IRA), Franceschini (UniPd) LaFranca, Matute (UniRm3 ) Gruppioni, Ciliegi, Pozzi, Zamorani (INAF-OAB), Lari (INAF-IRA), Franceschini (UniPd) LaFranca, Matute (UniRm3 ) ITALIAN COLLABORATORS: OTHER COLLABORATORS: ELAIS Consortium (9 European institutes, originally, 32 at the moment ) ELAIS Consortium (9 European institutes, originally, 32 at the moment ) European Large Area ISO Survey (P.I. Rowan-Robinson): the largest Open Time project with ISO satellite (375h): 12 deg 2 ( 8 in the North and 4 in the South) observed at 15 & 90 m with ISO-CAM & PHOT European Large Area ISO Survey (P.I. Rowan-Robinson): the largest Open Time project with ISO satellite (375h): 12 deg 2 ( 8 in the North and 4 in the South) observed at 15 & 90 m with ISO-CAM & PHOT

7 ELAIS-S1 (4 deg 2 ): Catalogue of 462 source 90% (100%) complete at 2 (3) mJy: 320 extragalactic objects (Lari, Pozzi, Gruppioni et al., 2001,MNRAS,325,1173) Source Counts in the range mJy: strong evolution for starburst galaxies (Gruppioni, Lari, Pozzi et al. 2002, MNRAS, 335,831)

8 Photometric IDs (80% R<23) [12n ESO+1.5m] Spectroscopic IDs (75% R<21.5 ~250 objs ) [2dF(2n) + ESO (15n)] (La Franca, Gruppioni et al., 2003, AJ, submitt.) Photometric IDs (80% R<23) [12n ESO+1.5m] Spectroscopic IDs (75% R<21.5 ~250 objs ) [2dF(2n) + ESO (15n)] (La Franca, Gruppioni et al., 2003, AJ, submitt.) ELAIS-S1 First derivation of 15- m Luminosity Function of Star-forming galaxies: strong evolution both in luminosity (1+z) 3.5 and density (1+z) 3.8 (Pozzi, Gruppioni et al., 2003, ApJ, submitted) First derivation of 15- m Luminosity Function of Star-forming galaxies: strong evolution both in luminosity (1+z) 3.5 and density (1+z) 3.8 (Pozzi, Gruppioni et al., 2003, ApJ, submitted) redshift

9 K20 REDSHIFT SURVEY P.I. A. Cimatti (INAF-OAA) K20 team: Pozzetti, Mignoli, Zamorani (INAF-OAB), Daddi, Renzini, DOdorico, 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 objects o Area: 52 arcmin^2 on 2 fields (CDFS+Q0055) o UBVRIzJKs multi-band imaging [public + 45h NTT+VLT] 92% redshift completeness Highest spectroscopic redshift completeness in the NIR

10 Scientific objectives Advantages of a K-selected sample: o Less dust extinction o 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

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

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

13 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 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)

14 VVDS SURVEY P.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 10 6 objects (McCracken et al. 03) o GTO Programme: 50 nights VLT+VIMOS o deep survey I AB <24: ~25,000 z, wide I AB <22.5: ~50,000 z 29 nights (21 clear) in 2002 ~21,000 spectra + 5 half nights in december deep VLA (~60h at 1.4Ghz) on 1 deg^2 (Bondi, Ciliegi et al. 03)

15 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~1.5 Complementary to wide local survey, like SDSS and 2dF in competition with DEIMOS-DEEP2 (P.I. M. Davis) at Keck Scientific results from the spectroscopic survey are still a few months ahead

16 Future Projects Legacy 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)

17 GRAZIE Provided by Lara


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