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Title: Massive galaxy formation back to cosmic reionization: the other half of galaxy formation


1
Massive galaxy formation back to cosmic
reionization the other half of galaxy
formation Chris Carilli (NRAO) Illinois, STScI,
March, 2009
  • Intro concepts, telescopes, techniques
  • Massive galaxy and SMBH formation within 1 Gyr of
    the Big Bang gas, dust, and star formation in
    quasar host galaxies at z6
  • sBzK galaxies the dawn of downsizing during
    the epoch galaxy assembly (z 2)
  • Future probing normal galaxy formation with the
    next generation telescopes
  • Collaborators Ran Wang, M. Pannella, Walter,
    Daddi, Menten, Cox, Bertoldi, Omont, Strauss,
    Fan, Wagg, Riechers, Neri

2
Star formation rate density vs. redshift
epoch of galaxy assembly
50 of present day stellar mass produced between
z1 to 3 (Marchesini et al. 2009)
3
Star formation rate density vs. redshift as a
function of FIR luminosity
FIR lt 1011 Lo SFRlt 30 Mo/yr
1011 to 12
1012 Lo SFR gt 300 Mo/yr
Le Floch et al. 2005
4
Star formation as function of galaxy stellar
mass specific star formation rates SFR/M
active star formation
tH-1
red and dead
Downsizing
Zheng
  • Massive galaxies form most of their stars at
    high z

5
Old, massive galaxies at high redshift zform gt
9? Wiklind et al., Mobasher et al. 2007
M 2e11 Mo, z5.2, age 1Gyr
6
Star formation history of Universe optical
limitations
  • Dust obscuration rest frame UV needs
    substantial dust-correction, missing earliest,
    most intense epochs of star formation
  • Only stars and star formation not (cold) gas gt
    missing the other half of the problem fuel for
    galaxy formation

7
Wilson et al.
Radio astronomy unveiling the cold, obscured
universe
  • mm continuum thermal emission from warm dust
    star formation
  • (sub)mm lines molecular gas, fine structure ISM
    cooling lines
  • (short) cm lines low order molecular
    transitions, dynamics
  • cm continuum synchrotron emission star
    formation, AGN

HST / OVRO CO
cm/mm rich in line continuum diagnostics
8
Powerful suite of existing cm/mm facilites
pushing back to first galaxies
30 field at 250 GHz, rms lt 0.3 mJy
Very Large Array 30 field at 1.4 GHz rmslt
10uJy, 1 res High res imaging at 20 to 50
GHz rms lt 0.1 mJy, res lt 0.2
Plateau de Bure Interferometer High res imaging
at 90 to 230 GHz rms lt 0.1mJy, res lt 0.5
9
M82 radio-FIR SED All mechanisms ? massive star
formation rate
Thermal dust 20 -- 70K
Synchrotron
Radio-FIR
Free-Free
SFR (Mo/yr) 3e-10 LFIR (Lo/yr) SFR (Mo/yr)
6e-29 L1.4 (erg/s/Hz)
10
Massive galaxy and SMBH formation at z6 gas,
dust, and star formation in quasar hosts
  • Why quasar hosts?
  • Spectroscopic redshifts
  • Extreme (massive) systems
  • MB lt -26 gt
  • Lbol gt 1e14 Lo
  • MBH gt 1e9 Mo
  • Rapidly increasing samples
  • zgt5 gt 100
  • zgt6 gt 20


Fan 2005
11
0.9um
Gunn-Peterson effect toward z6 SDSS QSOs
  • Pushing into the tail-end of cosmic reionization
    gt sets benchmark for first luminous structure
    formation
  • GP effect gt study of first light is restricted
    to ?obs gt 1um


Fan 05
12
Magorrian, Tremaine, Gebhardt, Merritt
Quasar host galaxies MBH -- Mbulge relation
MBH0.002 Mbulge
  • All low z spheroidal galaxies have central SMBH
  • Causal connection between SMBH and spheroidal
    galaxy formation
  • Luminous high z QSOs have massive host galaxies
    (1e12 Mo)

13
MAMBO 250 GHz surveys of zgt2 QSOs
HyLIRG
1e13 Lo
2.4mJy
  • 1/3 of luminous QSOs have S250 gt 2 mJy,
    independent of redshift from z1.5 to 6.4
  • LFIR 1e13 Lo 0.1 Lbol Dust heating by
    starburst or AGN?

14
Dust gt Gas
FIR 1e13 Lo SFR gt 1000 Mo/yr
MW
M(H2) gt 1010 Mo
Detect dust 1hr, CO in 10hr
15
Pushing into reionization Host galaxy of
J11485251 at z6.42
  • Highest redshift SDSS QSO (tuniv 870Myr)
  • Lbol 1e14 Lo
  • Black hole 3 x 109 Mo (Willot etal.)
  • Gunn Peterson trough (Fan etal.)

16
  • 114852 z6.42 Dust detection

MAMBO 250 GHz
3
S250 5.0 /- 0.6 mJy LFIR 1.2e13 Lo Mdust
7e8 Mo
  • Dust formation? (Dwek, Maiolino, Stratta,
    Shull, Nozawa)
  • AGB Winds 1.4e9yr gt tuniv 0.87e9yr
  • dust formation associated with high mass star
    formation?
  • Required yeild 0.1 and 1 Mo of dust per SNe
    (Dwek 2009)

17
114852 z6.42 Gas detection
VLA
CO3-2 VLA
IRAM
PdBI
1 5.5kpc
  • FWHM 305 km/s
  • z 6.419 /- 0.001
  • Mgas/Mdust 30 starburst galaxies)
  • Size 6 kpc
  • M(H2) 2e10 Mo

18
11485251 Radio to near-IR SED
TD 50 K
Elvis SED
Radio-FIR correlation
  • FIR excess 50K dust
  • Radio-FIR SED follows star forming galaxy
  • SFR 3000 Mo/yr

19

CO excitation ladder
?2
Dense, warm gas CO thermally excited to 6-5,
similar to starburst nucleus Tkin gt 70 K nH2 gt
1e4 cm-3 gt Conditions similar to GMC cores, but
over the inner few kpc
NGC253
MW
20
LFIR vs L(CO) integrated Kennicutt-Schmidt
law
  • Star formation efficiency(SFR/Mgas) increases
    with increasing SFR
  • Gas depletion timescale(Mgas/SFR) decreases with
    SFR ? in exponential galaxy formation models
    eg. Noeske 2008

1e3 Mo/yr
SFR
High-z QSO, submm gal tdep 1e7yr
Index1
tdep 3e8yr
1e11 Mo
High-z sources 10 -- 100 x Mgas of Milky Way
Index1.5
Mgas
Universal star formation law?
21
CO rotation curves quasar host galaxy dynamics
at high z
VLA CO 2-1
23221944, z4.2 Molecular Einstein ring
50 km/s channels
22
23221944 CO rotation curve lens inversion and
QSO host galaxy dynamics
Riechers 08
  • Galaxy dynamical mass (rlt3kpc) 4.4e10 Mo
  • M(H2) 1.7e10 Mo gt baryon dominated in inner
    few kpc
  • MBH 1.5e9 Mo (from MgII lines, Eddington)

23
Break-down of MBH -- Mbulge relation at very high
z Use CO rotation curves to get host galaxy
dynamical mass
  • Perhaps black holes form first?
  • Caveats
  • Inclination
  • Selected optical QSO
  • Non-rotational dynamics (eg. infall, hydro)
  • (see also Sheilds 06, Coppin 08)

High z QSO hosts Low z QSO hosts Other low z
galaxies
Riechers
24
Atomic fine structure lines CII 158um
  • Dominant ISM gas cooling line
  • Traces CNM and PDRs
  • zgt4 gt FS lines observed at high resolution in
    (sub)mm bands
  • J11485251 z6.42
  • LCII 4x109 Lo (LNII lt 0.1LCII )
  • SFR 6.5e-6 LCII 3000 Mo/yr

25
Maximal star forming disk (Walter 2009,
Nature)
1
PdBI, 0.25res
  • CII size 1.5 kpc gt SFR/area 1000 Mo yr-1
    kpc-2
  • Maximal starburst disk (Thompson, Quataert,
    Murray 2005)
  • Self-gravitating gas disk
  • Vertical disk support by radiation pressure on
    dust grains
  • Eddington limited SFR/area 1000 Mo yr-1 kpc-2
  • eg. Arp 220 on 100pc scale, Orion on 0.1pc scale

26
CII
  • CII/FIR decreases rapidly with LFIR (lower
    heating efficiency due to charged dust grains?)
    gt luminous starbursts are still difficult to
    detect in C
  • Normal star forming galaxies (eg. LAEs) are not
    much harder to detect
  • Dont pre-select on dust

J1623 z6.25
J1148 z6.42
Bertoldi, Maiolino, Iono, Malhotra 2000
27
Summary host galaxies of 33 quasars at zgt5.7
  • cm/mm only direct probe of host galaxies
  • 11 in dust gt FIR 1013 Lo Mdust gt 1e8 Mo
    Dust formation in SNe?
  • 8 in CO gt Mgas gt 1010 Mo Fuel for star
    formation in galaxies
  • 10 at 1.4 GHz continuum SED gt SFR gt 1000 Mo/yr
  • 2 in CII gt maximal star forming disk 1000
    Mo yr-1 kpc-2

J14253254 CO at z 5.9
28
Building a giant elliptical galaxy SMBH at
tunivlt 1Gyr
10
  • Multi-scale simulation isolating most massive
    halo in 3 Gpc3
  • Stellar mass 1e12 Mo forms in series (7) of
    major, gas rich mergers from z14, with SFR ? 1e3
    Mo/yr
  • SMBH of 2e9 Mo forms via Eddington-limited
    accretion mergers
  • Evolves into giant elliptical galaxy in massive
    cluster (3e15 Mo) by z0

6.5
Li, Hernquist, Hopkins, Roberston..
  • Rapid enrichment of metals, dust in ISM (z gt 8)
  • Rare, extreme mass objects 100 SDSS z6 QSOs
    on entire sky
  • Integration times of hours to days to detect
    HyLIGRs

29
  • Cosmological deep fields COSMOS
  • Definitive study of galaxy and SMBG evolution
    vs. environmnent
  • ACS 600 orbits for 2deg2 to IAB 26
  • VLA, Spitzer, 11-band SUBARU, Galex,
    Chandra/XMM
  • Approaching SDSS in volume and resolution but at
    z gt 1
  • 2e6 galaxies from z 0 to 7

30
COSMOS VLA deep field
  • Full field at 1.4GHz
  • 1.5 resolution
  • rms 8 uJy/beam
  • 4000 sources (10xHUDF)

Mostly SF gal at z lt 1 AGN, or extreme starburst
at zgt1
31
sBzK galaxies normal star forming galaxies at
z 1.5 to 2.5
Daddi et al 2004
sBzK
Lowz gal
stars
  • near-IR selected KAB 23
  • M 1010 to 1011 Mo

32
sBzK galaxies normal star forming galaxies at
z 1.5 to 2.5
HST
  • Space density few x10-4 Mpc-3 30x SMG, 100x
    quasars
  • HST sizes 1 9kpc
  • Gas dynamics gt disk-like, not mergers (Genzel,
    Tacconi)

star forming
3.2
Daddi, McCracken
33
30,000 sBzK galaxies in Cosmos (Daddi,
McCracken)
30,000 z 2 sBzk SF gal
Early-type pBzK
zphot 1.3 to 2.6
other
34
VLA radio stacking 30,000 sBzK in Cosmos
  • ltSFRgt 96 Mo yr-1 FIR 3e11 Lo
  • VLA size 1 HST
  • SKA science before the SKA!

ltS1.4gt 8.8 /- 0.1 uJy
Pannella
35
Stacking in bins of 3000
1010 Mo
3x1011 Mo
  • SFR independent of blue magnitude
  • SFR increases with B-z gt dust extinction
    increases with SFR (or M)
  • SFR increases with stellar mass

36
Dawn of Downsizing SFR/M vs. M
  • SSFR constant with M, unlike zlt1gt
    pre-downsizing
  • zgt1.5 sBzK well above the red and dead galaxy
    line
  • UV dust correction f(SFR, M) factor 5 at
    2e10 Mo LBG (Shapely 01)

1.4GHz SSFR
z2.1
z1.5
5x
tH-1 (z1.8)
z0.3
UV SSFR
37
SSFR vs. z for fixed M 3e10 Mo
SFR 100 (t/3.4e9Gyr)-2.5 Factor 30 decrease
from z2.5 to 0
38
sBzK not extreme starbursts, but massive gas
reservoirs
Daddi 2008
  • 6 of 6 sBzK detected in CO with Bure
  • Gas mass gt 1010 Mo high z HyLIRG (SMG, QSO
    host)
  • but
  • SFR lt 10 HyLIRG
  • 5 arcmin-2 (vs 0.05 for SMGs)

39
FIR/LCO
SMG, QSO hosts
MW
Daddi
Dannerbauer
  • CO excitation Milky Way (but mass gt 10xMW)
  • FIR/LCO Milky Way
  • Gas depletion timescales gt few x108 yrs

40
Summary sBzK at z1.3 to 2.5 -- extreme gas rich
galaxies without hyper-starbursts
Genzel 08
  • Common Contribute 20 to cosmic SFR density
    at z 2
  • ltSFR1.4gt 96 Mo yr-1 (FIR few x1011Lo)
  • SSFR constant with M pre-downsizing
  • Gas masses gt 1010 Mo gt M
  • Gas depletion time gt few x108yrs
  • secular galaxy formation during the epoch of
    galaxy assembly (forming normal ellipticals or
    large spirals? Daddi , Genzel )

41
What is EVLA? First steps to the SKA-high
  • By building on the existing infrastructure,
    multiply ten-fold the VLAs observational
    capabilities, including
  • 10x continuum sensitivity (lt1uJy)
  • full frequency coverage (1 to 50 GHz)
  • 80x BW (8GHz)

42
What is ALMA? North American, European, Japanese,
and Chilean collaboration to build operate a
large millimeter/submm array at high altitude
site (5000m) in northern Chile -gt order of
magnitude, or more, improvement in all areas of
(sub)mm astronomy, including resolution,
sensitivity, and frequency coverage.
50 x 12m array
Atacama Compact Array 12x7m 4x12m TP
43
J1148 in 24hrs with ALMA
  • Detect dust emission in 1sec (5?) at 250 GHz
  • Detect CII in minutes
  • Detect multiple lines, molecules per band gt
    detailed astrochemistry
  • Image dust and gas at sub-kpc resolution gas
    dynamics, K-S
  • LAE, LBGs detect dust, molecular, and FS lines
    in 1 to 3 hrs

44
Pushing to normal galaxies spectral lines
Arp220 z5
cm telescopes low order molecular transitions --
total gas mass, dense gas tracers
(sub)mm high order molecular lines. fine
structure lines -- ISM physics, dynamics
1 sBzK CO detection in every EVLA 40-48 GHz
full synthesis 3 sBzK CO detections in every
ALMA 90-98 GHz full synthesis
45
Pushing to normal galaxies continuum A
Panchromatic view of 1st galaxy formation
Arp 220 vs z
cm Star formation, AGN
(sub)mm Dust, FSL, mol. gas
Near-IR Stars, ionized gas, AGN
46
  • EVLA Status
  • Antenna retrofits now 50 completed.
  • Early science start in Q4 2009, using new
    correlator proposal deadline June 1, 2009 for
    shared-risk obs!!
  • Full receiver complement completed 2012.

47
AOS Technical Building
  • Antennas, receivers, correlator in production
    best submm receivers and antennas ever!
  • Site construction well under way Observation
    Support Facility, Array Operations Site, antenna
    pads

Array operations center
Antenna commissioning in progress
  • North American ALMA Science Center (CVille)
    support early science Q4 2010, full ops Q4 2012

48
END
ESO
49
A new paradigm in galaxy formation cold mode
accretion or stream-fed galaxy formation (Keres,
Dekel)
  • Galaxies smoothly accrete gas at 100 Mo/yr
    onto disk from filamentary IGM (?Mcl/Mgal lt 0.1)
  • Generate giant star forming regions, which
    migrate inward over tH to form bulge
  • Terminates when gas supply is depleted, or
    shut-off by hot halo
  • Major unknown gas supply

Cerverino Dekel
50
Summary sBzK at z1.3 to 2.5 -- extreme gas rich
galaxies without hyper-starbursts
When galaxies were young Mgas gt M
  • Common Contribute 20 to cosmic SFR density
    at z 2
  • ltSFR1.4gt 96 Mo yr-1 (FIR few x1011Lo)
  • SSFR constant with M pre-downsizing
  • Gas masses gt 1010 Mo gt M
  • Gas depletion time gt few x108yrs
  • gt secular galaxy formation during the epoch of
    galaxy assembly

sBzK
??
Low z ellipt
Major missing piece cool gas fuel for star
formation
51
Dust formation at tunivlt1Gyr Extinction toward
z6.2 quasar and 6.3 GRB starburst model gt
larger, silicate amorphous carbon dust grains
(vs. eg. graphite) formed in core collapse
SNe? Required yeild 0.1 and 1 Mo of dust per
SNe (Dwek 2009)
SMC, zlt4 quasars
Galactic
Starburst model
z6.2 quasar, 6.3 GRB
Stratta, Dwek, Maiolino, Shull, Nozawa, Dunne
52
Break-down of radio-FIR correlation inverse
Compton losses off CMB?
IC losses off CMB dominate synchrotron in nuclear
starbursts at zgt4
IC losses dominate in normal galaxies at zgt0.5
dEe/dt ? UB, U?
53
(No Transcript)
54
Anti-correlation of FIR luminosity and Lya EW
D
D
Dust gt Log EW lt 1.5 No dust gt Log EW gt 1.5
D
D
D
No D
D
D
D
55
FIR-detected star forming hosts
z6 FIR detected
IR-selected star forming hosts
Stacked non-detections
Optically selected, passive ellipticals
56
Higher Density Tracers HCN, HCO
HCO 1-0
HCN 1-0
z2.6
  • ncr gt 1e5 cm-3 (vs. ncr(CO) 103 cm-3)
  • Dense gas lines 5-10 fainter than CO

200uJy
57
HCN Dense gas directly associated with star
forming clouds
  • FIR -- HCN linear relation from GMCs to HyLIRGs
  • SFR per unit dense gas mass constant in all
    galaxies
  • Conclusions
  • CO traces all gas
  • HCN traces dense gas gt Counting star forming
    clouds
  • gt dense/total gas increases with SFR

Index 1
Gao , Wu
58
Kennicutt-Schmidt laws
  • CO-FIR lum FIR ? L(CO)1.5/-0.2
  • K-S law ? ? ?g1.4/-0.15
  • SFR ? ? / timescale
  • Low density gas tracers excited in all gas, such
    that timescale? FF time? ?-0.5 gt SFR ? ?1.5
  • High density gas tracers only excited in densest
    gas, such that all clouds have roughly same
    (critical) density gt timescale is same gt SFR ?
    ?1?cr0.5
  • Predicts departure from linearity for HCN/HCO in
    galaxies where mean density approaches critical
    density
  • gt HyLIRG at high z entire ISM ?cr

Krumholz Thompson
59
High z quasar hosts vs. Submm galaxies Gas mass
and line widths
QSO
SMG
  • Gas mass distribution similar ltMH2gt 3e10 Mo
  • ltVQSOgt 300 km s-1
  • ltVSMGgt 700 km s-1
  • gt Quasar hosts preferentially face-on lt?Igt
    13o

60
Dawn of Downsizing SFR/M vs. M
  • SSFR constant with M, unlike zlt1gt
    pre-downsizing
  • zgt1.5 sBzK well above the red and dead galaxy
    line
  • Extinction increases with SFR, M
  • UV dust correction f(SFR, M)
  • Factor 5 at 2e10 Mo ltLBGgt (Shapely 01)

5x
tH-1 (z1.8)
z0.3
61
Radio stacking pushing to normal galaxies
during reionization, eg. z5.7 Ly? galaxies
NB850nm
Murayama et al. 07
  • SUBARU Ly??????????? 10 Mo/yr
  • 100 sources in 2 deg-2 in ?z 5.7 /- 0.05
  • Stacking analysis (100 LAEs)
  • MAMBO S250 lt 2mJy gt SFRlt300
  • VLA S1.4 lt 2.5uJy gt SFRlt125

gt Need order magnitude improvement in
sensitivity at radio through submm wavelengths in
order to study earliest generation of normal
galaxies.
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