Radio observations of massive galaxy and black hole formation in the early Universe

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Radio observations of massive galaxy and black
hole formation in the early Universe Chris
Carilli (NRAO) MPE, Garching, July 16, 2009

• Introductory remarks
• Massive galaxy and SMBH formation within 1 Gyr of
  Big Bang dust, gas, and star formation in quasar
  host galaxies at z6
• Future probing normal galaxy formation with the
  next generation telescopes
• Collaborators Ran Wang, Walter, Menten, Cox,
  Bertoldi, Omont, Strauss, Fan, Wagg, Riechers,
  Wagg, Neri

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SDSS J11485251 z6.42

• Why quasar hosts?
• Spectroscopic redshifts
• Extreme (massive) systems
• MBlt -26
• Lbolgt 1e14 Lo
• MBHgt 1e9 Mo
• Rapidly increasing samples
• zgt5 gt 100
• zgt6 gt20
• Note MBH derived from Ledd, MgII width, other
  eg. Kurk, Fan

Host galaxy CO 3-2 VLA
15.5kpc
3
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 ?obsgt 1um

Fan 05
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QSO host galaxies MBH -- Mbulge relation
Haaring Rix 2004
MBH0.0014 Mbulge

• Most (all?) low z spheroidal galaxies have SMBH
• Causal connection between SMBH and spheroidal
  galaxy formation
• Luminous high z QSOs have massive host galaxies
  (1e12 Mo)

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Massive galaxies form most of their stars
quickly, at high z specific star formation
rates SFR/M
active star formation
tH-1
red and dead
Downsizing
Zheng
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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)
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Plateau de Bure Interferometer High res imaging
at 90 to 230 GHz rms lt 0.1mJy, res lt 0.5
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

• Spectroscopic imaging of molecular gas, fuel for
  star formation in galaxies gas mass, ISM
  conditions, dynamics
• Fine structure lines dominant ISM gas coolant
• Dust synchrotron imaging cm-to-mm SEDs gt
  obscuration-free star formation rates, ISM
  conditions, AGN

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Dust and star formation MAMBO 250GHz surveys 1/3
of zgt2 quasars have S250gt 2mJy
HyLIRG

• Wang sample 33 zgt5.7 quasars (mostly SDSS)
• LFIR 0.3 to 1.3 x1013 Lo HyLIRG (47K, ß
  1.5)
• Mdust 1.5 to 5.5 x108Mo 10x MW (?125um 19
  cm2 g-1)

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• Dust formation at tunivlt1Gyr?
• AGB Winds 1.4e9yr gttuniv 0.87e9yr gt dust
  formation associated with high mass star
  formation? (Dwek, Shull, Nozawa)
• or smoking quasars dust formed in BLR winds
  (Elvis)
• Extinction toward z6.2 QSO and 6.3 GRBgt
  larger, silicate amorphous carbon dust grains
  formed in core collapse SNe vs. eg. graphite?

SMC, zlt4 quasars
Galactic
z6.2 quasar, GRB
Maiolino, Stratta
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Dust heating by starburst or AGN?
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Radio to near-IR SED

• FIR excess 47K dust
• Radio-FIR SED consistent with star forming galaxy

Elvis SED TD 1000K
TD 47 K
Radio-FIR correlation
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Radio-FIR correlation
SFR 400 to 2000 Mo/yr
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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
D
D
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Molecular gas fuel for star formation 8 CO
detections at z 6 with PdBI, VLA

• Mgas 0.7 to 3 x1010 Mo (a 0.8)
• Mgas/Mdust 20 to 70 starburst gals.

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High z quasar hosts vs. submm galaxies
SMG
QSO

• zmed(z6 QSO) 413 km s-1
• zmed(SMG) 565 km s-1
• Marginal evidence for ilt 30o in quasars?

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CO excitation ladder
?2
J1148 J1048
Dense, warm gas CO thermally excited to 6-5,
similar to starburst nucleus Tkgt 70 K nH2gt104
cm-3 Note VLA critical for low orders
NGC253
MW
MW
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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
• Need imaging!

SFR
1e3 Mo/yr
Index1.5
1e11 Mo
Mgas
FIR 1e10 Lo/yr gt tdep 3e8yr FIR 1e13 Lo/yr
gttdep 1e7yr
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114852 z6.42 VLA imaging at 0.15 resolution
CO3-2 VLA
IRAM
0.3
1 5.5kpc

• Size 6 kpc
• Double peaked, each 1kpc, M(H2) 5 x109 Mo
• TB 35 K starburst nuclei

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CO rotation curves QSO host galaxy dynamics at
high z
CO 2-1
23221944, z4.2 Molecular Einstein ring Riechers
et al. 2008
50 km/s channels
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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

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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
Perhaps black holes form first?
Riechers
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Mbh/Mdyn vs. inclination for z6 QSOs
Low z relation
All must be face-on ilt20o Need imaging!
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CII 158um search in zgt 6.2 quasars

• Dominant ISM gas cooling line
• Traces CNM and PDRs
• zgt4 gt FS lines observed in (sub)mmbands (zgt6.2
  gtBure)

• J11485251 z6.42
• SCII 10mJy, S250GHz 5mJy
• LCII 4x109 Lo(LNIIlt 0.1LCII )

• J16233112 z6.25
• SCII 3mJy
• S250GHzlt1mJy

Kundsen, Bertoldi, Walter, Maiolino
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Maximal star forming disk (Walter 2009)
1
PdBI, 0.25res

• CII size 1.5 kpc gt SFR/area 1000 Mo yr-1
  kpc-2
• Maximal starburst (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

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CII
zgt4

• CII/FIR decreases with LFIR lower gas
  heating efficiency due to charged dust grains gt
  luminous starbursts are still difficult to detect
  in C
• Normal star forming galaxies are not much harder
  to detect
• HyLIRGat zgt 4 no worse than ULIRG at low z gt
  lower metalicity?
• Dont pre-select on dust

Maiolino, Bertoldi, Knudsen,Iono, Wagg
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Summary of cm/mm detections at zgt5.7 33 quasars
J14253254 CO at z 5.9
J1048 z6.23 PdBI, VLA

• Only direct probe of host galaxies
• 11 in dust gtMdustgt 1e8 Mo Dust formation in
  SNe?
• 8 in CO gtMgasgt 1e10 Mo Fuel for star
  formation in galaxies
• 10 at 1.4 GHz continuum radio loud AGN fraction
  8
• Radio FIR SED gt SFR 1000 Mo/yr
• 2 in CII gt maximal star forming disk 1000
  Mo yr-1 kpc-2

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Building a giant elliptical galaxy SMBH at
tunivlt 1Gyr
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• Multi-scale simulation isolating most massive
  halo in 3Gpc3
• 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 et al.

• 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

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Pushing to normal galaxies during reionization,
eg. z5.7 Ly? galaxies in COSMOS
NB850nm
Murayama et al. 07

• SUBARU Ly???????SFR? 10 Mo/yr
• 100 sources in 2 deg-2 in ?z 5.7 /- 0.05

• Stacking analysis (100 LAEs)
• MAMBO S250lt 2mJy gt SFRlt300
• VLA S1.4lt 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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GBT limits on CO in zgt6 LAE
Wagg 2009
Even with strong lensing (4.5x) and optimistic a
(0.8) M(H2) lt 5x109 Mo gt still 2x MW gas
masses
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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)

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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
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J1148 in 24hrs with ALMA

• 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

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Key role for EVLA total gas masses from low
order CO
z6
CII
Not excited?
6-5
3-2
Dannerbauer et al. 2009
reionization
Normal galaxies may not have high order lines
excited, in particular for dense gas tracers like
HCN, HCO (critical densities gt 106 cm-3). EVLA
crucial for low order transitions gt total gas
mass
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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

• 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

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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
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• EVLA Status
• Antenna retrofits now gt 50 completed.
• Early science start in Q1 2010, using new
  correlator
• proposal deadline Oct 1, 2009 for shared-risk
  obs
• 2GHz BW
• 20 to 50 GHz complete
• 8 GHz correlator ready in late 2010
• Full receiver complement completed 2012.

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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

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END
ESO
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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?
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Comparison to low z quasar hosts
z6 quasars
IRAS selected
Stacked mm non-detections
PG quasars
Hao et al. 2005