Studying the gas, dust, and star formation in the first galaxies at cm and mm wavelengths

Chris Carilli, KIAA-PKU reionization workshop, July 2008

QSO host galaxies at z ~ 6: massive galaxy and SMBH hole formation within 1Gyr of the Big Bang

Pushing to normal galaxies with ALMA and the EVLA

USA – Carilli, Wang, Wagg, Fan, Strauss

Euro – Walter, Bertoldi, Cox, Menten, Omont

Why QSO hosts?

Spectroscopic redshifts

Extreme (massive) systems

MB < -26 =>

Lbol > 1e14 Lo

MBH > 1e9 Mo

Rapidly increasing samples:

z>4: > 1000 known

z>5: 80

z>6: 15

Fan 05

QSO host galaxies – MBH -- Mbulge relation

Most (all?) low z spheroidal galaxies have SMBH: MBH=0.002 Mbulge

‘Causal connection between SMBH and spheroidal galaxy formation’

Luminous high z QSOs have massive host galaxies (1e12 Mo)

Magorrian, Tremaine, Gebhardt, Merritt…

• 1/3 of luminous QSOs have S250 > 2 mJy, independent of redshift from z=1.5 to 6.4

• LFIR ~ 1e13 Lo (HyLIRG) ~ 0.1 x Lbol: Dust heating by starburst or AGN?

MAMBO surveys of z>2 QSOs

1e13 Lo

2.4mJy

Dust => Gas: LFIR vs L’(CO)

non-linear => increasing SF eff (SFR/gas mass) with increasing SFR

Massive gas reservoirs > 1010 Mo > 10 x MW

Index=1.5

1e11 Mo

1e3 Mo/yr

z ~ 6 QSO hosts

Star formation rate

Gas Mass

• Highest redshift SDSS QSO (tuniv = 0.87Gyr)• Lbol = 1e14 Lo

• Black hole: ~3 x 109 Mo (Willot etal.)• Gunn Peterson trough (Fan etal.)

Pushing into reionization: QSO 1148+52 at z=6.4

1148+52 z=6.42: Dust detection

Dust formation?

• AGB Winds ≥ 1.4e9yr > tuniv = 0.87e9yr

=> dust formation associated with high mass star formation: Silicate gains (vs. eg. Graphite) formed in core collapse SNe (Maiolino 07)?

S250 = 5.0 +/- 0.6 mJy

LFIR = 1.2e13 Lo

Mdust =7e8 Mo

3’

MAMBO 250 GHz

1148+52 z=6.42: Gas detection

• FWHM = 305 km/s• z = 6.419 +/- 0.001

• Mgas/Mdust ~ 30 (~ starburst galaxies)

IRAM

VLA

1” ~ 5.5kpc

CO3-2 VLA

Size ~ 5.5 kpc

M(H2) ~ 2e10 Mo

‘Fuel for galaxy formation’

PdBI

+

1148+5251

Radio to near-IR SED TD = 50 K

FIR excess = 50K dust

Radio-FIR SED follows star forming galaxy

SFR ~ 3000 Mo/yr

Radio-FIR correlation

Elvis SED

Dense, warm gas: CO thermally excited to 6-5, similar to starburst nucleus

Tkin > 80 K

nH2 ~ 1e5 cm^-3

CO excitation ladder 2

NGC253

MW

Break-down of MBH -- Mbulge relation at very high z

Use CO rotation curves to get host galaxy dynamical mass

High z QSO hosts

Low z QSO hosts

Other low z galaxies

Riechers +

Perhaps black holes form first?

Atomic fine structure lines: [CII] 158um at z=6.4

Dominant ISM gas coolant = star formation tracer

z>4 => FS lines observed in (sub)mm bands

[CII] size ~ 6kpc ~ molecular gas => distributed star formation

SFR ~ 6.5e-6 L[CII] ~ 3000 Mo/yr

1”

[CII] + CO 3-2

[CII]

[NII]

IRAM 30m

Plateau de Bure

[CII] -- the good and the bad

[CII]/FIR decreases rapidly with LFIR (lower heating efficiency due to charged dust grains?) => luminous starbursts are still difficult to detect in C+

Normal star forming galaxies (eg. LAEs) are not much harder to detect!

J1623 z=6.25

Malhotra + 2000

[CII] in J1623+3111 at z = 6.25

FIR-weaker QSO Host

S250 < 1mJy => FIR < 3e12 Lo

=> Dust detection should not be a prerequisite for [CII] search

Bertoldi + 2008

Only direct probe of host galaxies

10 in dust => Mdust > 1e8 Mo

5 in CO => Mgas > 1e10 Mo

10 at 1.4 GHz continuum:

-- SFR > 1000 Mo/yr

-- Radio loud AGN fraction ~ 6%

2 in [CII] => SFR > 1000 Mo/yr

J1425+3254 CO at z = 5.9

Current Plateau de Bure is routinely detecting ~ 1mJy lines, and 0.1 mJy continuum at 90GHz!

Summary of cm/mm detections at z>5.7: 33 quasars

Building a giant elliptical galaxy + SMBH at tuniv < 1Gyr

Multi-scale simulation isolating most

massive halo in 3 Gpc^3 (co-mov)

Stellar mass ~ 1e12 Mo forms in series (7) of major, gas rich mergers from z~14, with SFR ~ 1e3 - 1e4 Mo/yr

SMBH of ~ 2e9 Mo forms via Eddington-limited accretion + mergers

Evolves into giant elliptical galaxy in massive cluster (3e15 Mo) by z=0

Generally consistent with ‘downsizing’

10.5

8.1

6.5

Li, Hernquist, Roberston..

10

• Rapid enrichment of metals, dust in ISM (z > 8)

• Rare, extreme mass objects: ~ 100 SDSS z~6 QSOs on entire sky

• Integration times of hours to days to detect HyLIGRs

Pushing to ‘normal galaxies’ during reionization, eg. z=5.7 Ly galaxies in COSMOS

SUBARU: Ly ~ 10 Mo/yr

100 deg^-2 in z ~ 5.7 +/- 0.05

NB850nm

Murayama et al. 07

Pushing to ‘normal galaxies’ during reionization, eg. z=5.7 Ly galaxies in COSMOS

Stacking analysis (100 LAEs)

MAMBO: <S250> < 2mJy => SFR<300

VLA: <S1.4> < 2.5uJy => SFR<125

Still factor 10 away from SFR(Lya)

VLA Stacking analysis

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

What is EVLA? First steps to the SKA

Status•Antenna retrofits now 50% completed.•Early science in 2010, using new correlator.•Full receiver complement completed 2012.

By building on the existing infrastructure, multiply ten-fold the VLA’s observational capabilities, including 10x continuum sensitivity (1uJy), full frequency coverage (1 to 50 GHz), 80x BW (8GHz)

50 x 12m array

Atacama Compact Array 12x7m + 4x12m TP

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 -> order of magnitude, or more, improvement in all areas of (sub)mm astronomy, including resolution, sensitivity, and frequency coverage.

ALMA into reionization Spectral simulation of J1148+5251

Detect dust emission in 1sec (5) at 250 GHz

Detect [CII] in minutes

Detect multiple lines, molecules per band => detailed astrochemistry

Image dust and gas at sub-kpc resolution – gas dynamics

HCN

HCO+

CO

CCH

LAE, LBGs: ALMA will detect dust, molecular, and FS lines in 1 to 3 hours in normal galaxies at z ~ 6

(sub)mm: high order molecular lines. fine structure lines -- ISM physics, dynamics

cm telescopes: low order molecular transitions -- total gas mass, dense gas tracers

Pushing to normal galaxies: spectral lines

FS lines will be workhorse lines in the study of the first galaxies with ALMA.

Study of molecular gas in first galaxies will be done primarily with cm telescopes

cm: Star formation, AGN

(sub)mm Dust, molecular gas

Near-IR: Stars, ionized gas, AGN

Arp 220 vs z

Pushing to normal galaxies: continuum

A Panchromatic view of galaxy formation

AOS Technical Building

Array operations center at 5000m

Japanese antennas at 3000m

ESO

ALMA Status•Antennas, receivers, correlator fully prototyped, now in production: best (sub)mm receivers and antennas ever!•Site construction well under way: Observation Support Facility and Array Operations Site•North American ALMA Science Center (C’Ville): gearing up for science commissioning and early operations

•Timeline Q1 2007: First fringes at ATF (Socorro) Q1 2009: Three antenna array at AOS Q2 2010: First call for (early science) proposals Q4 2010: Start early science (16 antennas) Q4 2012: Full operations

ESO

END

Pushing uJy radio studies to z>2: Cosmos LBG, BzK, and LAE samples

Counterparts L1.4GHz

M82 (SFR~10)

Arp220 (SFR~100)

M87 (low lum AGN)

> 2.0e+31 erg/s/Hz 4e+29 4e+30 9e+31

• 8500 LBGs (U,B,V) identified, z~ 3, 4, 5• 100 LAE in NB850 filter z = 5.7• 30,000 BzK star forming galaxies z ~ 1.5 to 2• ‘normal’ galaxy population at high redshift?

• V-drop, z>4.5• S1.4 = 45 uJy • S230 = 5 ± 1.4 mJy• Keck spectrum => starburst

galaxy at z = 4.52• Most distant, spectroscopically

confirmed submm galaxy (the next most distant at z=3.6)

• Complex optical/IR morphology: varying extinction

QuickTime™ and aTIFF (LZW) decompressor

are needed to see this picture.

Figure 5 - A color image of J1000+0234 with radio contours

Ha + IR: high extinction

UV knot+ Lya

J1000+0234 -- V-drop+radio ID: most distant submm galaxy

Capak +

1”

• CO/radio continuum coincident with a dust-lane seen rest frame UV image

• Gass mass ~ 2e10 Mo= fuel for galaxy formation

• Massive galaxy forming from a merging system, SFR ~ 3000 Mo/yr

• Comparison to uv-derived SFR => uv extinction factor ~100

J1000+0234 -- V-drop+radio ID: most distant submm galaxy

VLA CO 2-1

VLA 1.4 GHz

ACS

LBG Stacking (SKA Science without the SKA)

• Find the average properties of our “non-detections” using stacking: reduces noise by ~ √N.

• Mean stacking: exclude 3, 4 sources: significantly affects results

• Median stacking does not require source exclusion, and is more robust calculation (see FIRST analysis by White et. al, 2006)

U-Dropouts (2.5 < z < 3.5)

Median Flux Density = 0.90+/-0.21 Jy

<SFRuv> ~ 17 Mo/yr

<SFRrad> ~ 31 Mo/yr

UV either extinction ~ factor 2 (vs. standard LBG factor 5)

or Radio-FIR correlation fails at high z?

BzK galaxies: Star forming galaxies at z~ 1.5 to 2 (Pannella et al)

Star forming galaxies with stellar masses ~ 1e10 to 1e11 Mo

SFR ~ 30 -- 50 Moyr

1.4 GHz vs. Stellar Mass

Stacking detections ~ 2 to 9 +/- 0.2 uJy

1.4 GHz vs. B-z

Specific star formation rate (= SFR/M*) vs. stellar mass: radio vs. UV data

Radio: no dust-bias => SSFR ~ constant w. M*

UV not corrected for dust: more massive SF galaxies with higher SFR are also more extincted

Radio SFR

UV SFR

1.4GHz vs. BAB