Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES,...

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Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more leverage than looking at z~1 as their predicted abundance and properties (e.g. Passive vs. starbursting) are most critically dependent on theoretical model A Renzini, STScI, September 27, 2004 Fontana et al 2004

Transcript of Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES,...

Page 1: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Massive galaxies at z ~ 2 from K20+Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS )Looking at z~2 massive galaxies gives us more leverage than looking at z~1

✰ as their predicted abundance and properties (e.g. Passive vs. starbursting) are most critically dependent on theoretical model *assumptions, *algorithms and *parameters → allow to narrow down our model shopping list.

A Renzini, STScI, September 27, 2004

Fontana et al.2004

Page 2: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

The Local Mass Function (from the SDSS)

et al. (2003)

In the local universe:Among the MMGs the oldpassively evolving, early-type galaxies outnumber the starforming galaxies bymore than a factor ~10

Page 3: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

The High-z Tail in the K20 Sample

K<20 galaxies at z > 1.6:~ 0.0 predicted by SAMs32 observed in the the K20 sample

(apparent agreement with PLE models)

(old)SAM

PLE

Cimatti et al. 2002

Page 4: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

The Nature of the K<20, z>1.6 galaxies1. The Star-Forming Galaxies

Daddi et al. (2004)

Page 5: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

The K<20, z≈2 starforming galaxies Coadded spectra of 5 best

S/N galaxies (de Mello et al. 2004).

More stronglined than LBGsboth for ISM and photospheric absorptions➔ >~solar metallicity which along with:● M

*>1011M⊙

● SFR > ~ 100 M⊙/yr

● Strong clustering ➔

Likely progenitors of localellipticals and big bulges

Page 6: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

2. The Passively Evolving Galaxies

→ zF

> 2.5-3

Coadded VLT spectra ACS/GOODS

images

Cimatti et al. (Nature, July 8, 2004)

(The Highest redshift ellipticals)

Page 7: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

The MgUV

Feature: a key to hi-z

passive galaxiesFirst used by Dunlop/Spinrad et al '96; Cimatti et al '04; McCarthy et al. '04)

Page 8: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Passively Evolving galaxies (cont.)In red LBDS 53w091 (z=1.55) Blue=average of the 4 gals.

F5V

F2V

SDSS <z>=0.5

z=1 old EROs

Z=1 SF ERO

0.5 Gyr

1 Gyr 3Gyr

Page 9: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

The 4 galaxies in real colorGOODS ACS BViz images

Page 10: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Old galaxies at high redshift

In the K20/GOODS field (32 □)

Passive galaxies with R-K>6, z>1.5, K<20:

4 objects with zspec

3 objects with zphot

7 objects in total

In the currently “best” semi-analytic model(Somerville 2004): Mock catalog for a whole GOODS field (160 □):

Only one object with the samecharacteristics.

35 expected scaling from the K20

Page 11: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

The ACS/GOODS Morphologies 32 K20 galaxies at z>1.4 with deep z-band ACS imaging

S=Starforming ➔ mergers, starbursts

P=Passively evolving ➔ Elliptical and Bulge-dominated galaxies

Page 12: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Some Inferences (so far)● Massive (M*>1011M⊙) galaxies appear to be in place at z ~ 2 in much

greater number than predicted by most CDM Simulations

Models with strong SN/AGN feedback do better (Nagamine et al. 2001; Granato et al. 2004) [Anti-hierarchical galaxy assembly!]

While at z=0 most “most massive galaxies” are passively evolving, old ellipticals, by z~2 passive and active star-forming galaxies coexist in nearly equal number

☹ Limitations of the K20 survey: ✈ relatively small area (prone to cosmic variance) ✈ relatively shallow (K<20)

Page 13: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Post-K20: go wider, go deeper,focus on z~2

Daddi et al. (2004)

The BzK criterion forselecting BOTH starforming(reddening independent!) and passively evolving galaxies at 1.4<z<2.5

Calibrated on the K20, GOODS, and GDDSdatasets.

⇦K20/GOODS data only shown here.

Page 14: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Why the BzK criterion works

Daddi et al. (2004)

BC03 models with various ages, SF histories,and reddening:Nice agreement with theK20 empirical findings

SSPsCont. SF

SFR ~ e(-t/τ)z<1.4

Page 15: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

BzK- vs. LBG UGR-selected Galaxies A preliminary comparison: K20 BzK sample vs UGR sample (Steidel et al. 2004)

K20 BzK Objects (K<20)

<E(B-V)> > 0.3

<SFR> = ~ 200 M⊙/yr

~1 Object/□'

~1/3 of the BzK+UGR Star Formation Rate @ z=2

Misses objects with K>20

Misses Objects wit

/ y~ 1 /□Object '

~1/3 + of the BzK UGR Star

Formation Rate = 2@ z

Misses objects with>20K

UGR Objects (R<25)

E(B-V) < 0.3

<SFR> =~50 M⊙/yr

~9 objects/□'

~2/3 of the BzK+UGR Star Formation Rate @ z = 2

Misses highly reddened objects

~ 9 /□Objects '

~2/3 +of the BzK UGR Star FormationRate = 2@ z

Misses highly reddenedobjects

Page 16: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Going deeper: the GMASS projectVLT/FORS2 ultradeep spectroscopy (~30 hours integration per mask) overthe UDF/GOODS-South field. PI A. Cimatti, Co-Is as usualScheduled for September-November 2004.

(Also called the K21 project)

The selected targets on the BzK diagram

All targets with: K>20 (average 21.2)(4.5)

AB<23.5 (FromSpitzer/GOODS)

Perhaps the first Spitzer-selectedsample.

Page 17: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Going Deeper: the UDF+GRAPES* Sample

*Malhotra et al. 2004

Daddi et al. 2004 (in prep) Selecting candidate passively evolving galaxies at z>1.4 from theUDF field (Bz) & GOODS (K) withthe BzK plot. ACS/GRISM spectra from the GRAPES project.

GOODS

K20

UDF

Targets down to K=21.1

Page 18: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

ACS Cutouts & ACS/GRISM SpectraThe Mg

UV Feature as a

function of SSP ageand for Continous SF+ E(B-V)=1.2

Redshifts identified by the Mg

UV Feature

agree with photo-z's

Page 19: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

ACS&NICMOS Morphologies

n~1.0

n=2.9

n= 4.7

n=9.0

n=4.2

n=4.3merger?

N=8.2

Sersic index in z

Page 20: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Passive or Active?

Object #4950 @ z=1.55

Page 21: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Masses and Mass Densities

Typical (stellar) masses of these galaxies are ~ 0.5-2 1011M⊙

The 6 passively evolving galaxies at 1.4<z<2.0 with M* > ~10

11M⊙ correspond to 20-40% of

the number density of such galaxies at z=0.

Assuming ro = 10 Mpc for their correlation length the 1 range

becomes 10-80% (!) COSMIC VARIANCE dominates

BIGGER FIELDS ARE NEEDED!

Page 22: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Going Wider: BzK-selected galaxiesOver ~ 1000 □

ESO/SUBARU Collaboration: Cimatti, Daddi, Renzini, + Arimoto, Ikuta, Kong, Broadhurst, Pozzetti et al. Onodera, et al. K-band (<20.2) from NTT, Bz bands from SuprimeCam

Objects observed withVIMOS, February '04❍ Blue grism, R=200 Red grism, R=600

Reductions in progress

Page 23: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Work in ProgressTypical VIMOS/Blue grism spectra of BzK-selected galaxies (R=200)

Z = 1.822 B=23.6

Z=2.360 B=24.4 Z=1.565 B=24.3

Z=2.200 B=24.3

Page 24: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

GOODS, COSMOS, .....GOODS: 160 + 160 □' COSMOS: 2 □° ACS Equatorial Field Goal: ~90,000 redshifts w/ VLT/VIMOSGOODS-South: To be proposed ... + Magellan/IMACS~6000 redshifts from the VLT + whoever may like to join with other~2000 released, the rest next fall telescopes

COSMOS:

Mappinggalaxyevolutionas a functionof redshiftand LSSContextby 2006-07.

Page 25: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

COSMOS Targets BzK+UGR selected

Passive, z>1.4

Starforming, 1.4<z<2.5

Stars

Galaxies, z<1.4

Red, Blue, Black: (K)<0.22000; 20,000; 100,000(BzK-selected galaxies)

Yellow, Cyan: (K)>0.2~50,000 (UGR-selected, à la Steidel)

Yellow+Blue: VLT/VIMOS/LR-blueBlack: VLT/VIMOS/LR-Red

Red: Magellan/IMACS

Data: Bz (SUBARU), K (NOAO, IfA), U (CFHT)from B. Mobasher catalog

Page 26: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

COSMOS Targets

UGR

BzK

Bottom line: all selectioncriteria are +/- biased:the BzK+UGR selectionis the most un-biased criterion we were able toinvent.

COSMOS PIs:ACS (Scoville), SUBARU (Taniguchi)CFHT (LeFevere)VLT (Lilly)Magellan (McCarthy)XMM (Hasinger)Galex (Rich)VLA (Schinnerer).................

Page 27: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

SUMMARY

Different CDM Models tuned to match some z=0 observable diverge widely by z=2.

By z=2 the massive galaxy mix is ~50-50 passive and starbursting

Current data favor an early build up of galactic spheroids, with the more massive ones completing their star formation ahead of the less massive ones (seemingly “anti-hierarchical”, “downsizing”)

Fully explored fields (< 100 □) are still dominated by cosmic variance. But ..................

Page 28: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

2005-2007 (~full) Mapping of Galaxy Evolution up to z = 6.7

GOODS, IDDS, GDDS, GMASS, GEMS, COMBO17, UDF, CDFS, SDF, DEEP2, VVDS, COSMOS, SWIRE, GALEX, DEIMOS, VIMOS, IMAX, MOIRCS, GMOS, ACS, SuPrime, CHANDRA, XMM, SPITZER, SCUBA, VLA, FORS2, ISAAC, NICMOS, .............................................................

END

Page 29: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.
Page 30: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Ellipticals in clusters and fieldlook much the same

Bernardi et al. (2003): ~9000ellipticals in the SDSS sample.

No appreciable trend of the stellar population content withlocal density.

“Field” ellipticals less than~1 Gyr younger than clusterellipticals.

Page 31: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Searching for the high-z Precursors ofthe MMGs at z=0

By and large, this is ~equivalent to searching for the precursors of ellipticalgalaxies.

@ z=1: Passively evolving “EROs” (R-K>5) in (almost) enough number

Beyond z=1:

■Up to which redshift passively evolving galaxies can be found?

■Given that the bulk of stars in ellipticals formed at z>~3: where are the ELLIPTICALS IN FORMATION?

Page 32: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Searching for High-z Massive Galaxies(the K20 Project, and Beyond)

1999: in absence of a better criterion, pick near-IR bright galaxies as best proxies to MMGs: i.e. Select for VLT spectroscopy K 20 galaxies ➔ the “K20 project” PI: A. Cimatti, Co-Is: E. Daddi, A. Fontana, L. Pozzetti, A. Renzini, G. Zamorani, T. Broadhurst, M. Mignoli, et al.

Deep VLT Spectroscopy of 546 K 20 objects, over two fields (52 □)

● Now 92% complete ( 95 % over the subfield included in the GOODS field)

Page 33: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

The Redshift Distribution of the K<20 Sample of Galaxies

Pure Luminosity Evolution (PLE) Models apparently do better than CDM (<2002)

Semianalytic Models (SAM)

(Cimatti et al. 2002)

PLE

SAM

SAM

Page 34: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

The Stellar Masses of K20 Galaxies

Stellar masses derived from either color (R-K) (MA)or SED (UBVRIzJHK) fits(BF) and the K magnitude.

● Old Passive (Early type)❍ Early + Emission line Photo-z onlyX Star forming

Page 35: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

The Evolution of the Galaxy Mass FunctionFontana et al. (2004)

□ BF Masses

∇ MA Masses

❍ zspec

only

Color code:

Bad fitPoor fit Fair fitGood fit

Menci et al '02, '04 Nagamine et al '01 Cole et al. '00; Granato et al. '04 (Salpeter IMF) (Gould IMF) Somerville et al. '04a, '04b (Kennicutt IMF)

Page 36: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Drory et al. (2004)

The K20 vs the Munics Mass Function up to z=1.2(Very nice agreement)

1 □o ; K<19.5;mostly photo-z's

Page 37: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

The Build Up of Stellar MassThrough Cosmic Time

⇧ is my preferred value fromthe fossil evidence (mass and formation redshift of local spheroids), i.e. >30% of the stellar mass done by z=3(Renzini 1998, 1999)

From Fontana et al. (2004)

Page 38: Massive galaxies at z ~ 2 from K20+ Preamble: (Cimatti, Daddi, Fontana, Arimoto, GOODS, GRAPES, COSMOS ) Looking at z~2 massive galaxies gives us more.

Baryon-to-star conversion as a function of galaxy mass

PLE

Available baryons from CDM

simulation assuming cosmic share (

b/

m)

Two Main Points:

There are enough massive DM halos to account for the massive galaxies we see (No fundamental failure of the DM paradigm). Strong mass dependence of the baryon-to-star conversion efficiency (many interesting ramifications ... ).