Studying the gas, dust, and star formation in the first galaxies at cm and mm wavelengths Chris...
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![Page 1: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/1.jpg)
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
![Page 2: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/2.jpg)
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
![Page 3: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/3.jpg)
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…
![Page 4: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/4.jpg)
• 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
![Page 5: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/5.jpg)
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
![Page 6: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/6.jpg)
• 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
![Page 7: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/7.jpg)
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
![Page 8: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/8.jpg)
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
+
![Page 9: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/9.jpg)
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
![Page 10: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/10.jpg)
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
![Page 11: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/11.jpg)
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?
![Page 12: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/12.jpg)
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
![Page 13: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/13.jpg)
[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
![Page 14: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/14.jpg)
[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
![Page 15: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/15.jpg)
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
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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
![Page 17: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/17.jpg)
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
![Page 18: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/18.jpg)
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.
![Page 19: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/19.jpg)
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)
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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.
![Page 21: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/21.jpg)
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
![Page 22: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/22.jpg)
(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
![Page 23: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/23.jpg)
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
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AOS Technical Building
Array operations center at 5000m
Japanese antennas at 3000m
![Page 25: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/25.jpg)
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
![Page 26: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/26.jpg)
ESO
END
![Page 27: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/27.jpg)
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?
![Page 28: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/28.jpg)
• 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”
![Page 29: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/29.jpg)
• 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
![Page 30: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/30.jpg)
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)
![Page 31: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/31.jpg)
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?
![Page 32: 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.](https://reader030.fdocuments.in/reader030/viewer/2022032612/56649f045503460f94c17d9f/html5/thumbnails/32.jpg)
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
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1.4 GHz vs. Stellar Mass
Stacking detections ~ 2 to 9 +/- 0.2 uJy
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1.4 GHz vs. B-z
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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
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1.4GHz vs. BAB