muse & alma

MUSE & ALMA

Françoise CombesObservatoire de Paris

Toulouse, 19 March 2009

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Capacities of ALMA

50 x 12m, bases from 200m to 14km, 3mm to 0.3mm(factor ~6 in surface with respect to IRAM-PdB)4 frequency bands at the beginning84-116 GHz, 211-275 GHz, 275-370 GHz, 602-720 GHzLarge bandwidth of 8GHz/polar

Spatial resolution, up to 10mas, Spectral resolution up to R=108

Dynamical range from 128x128 to 8192x8192 pixels

Small field of view: from 1arcmin (3mm) to 6 arsec (0.3mm)Possibility of mosaics

Early Science? Debated In 2012-3: Full Operation

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Main privilege of the mm/submm domainNegative K-correction: example of Arp 220

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K-correction for the CO linesSimple Model of a starburst ~ ULIRG

Very high molecular masses 1010 - 1011 MoHigh temperatures of dust: 30-50K up to 100K (or 200K)

Very small sizes: below 1kpc (300pc disks)In these conditions, the average column density is around 1024cm-2

and the dust becomes optically thick at λ < 150μ

Two components, both with low filling factor

1-the dense and hot component: star forming cores 106cm-3, 90K2-each embedded in a cloud 104cm-3, 30K

Individual velocity dispersion of 10km/sEmbedded in the rotational gradient of the galaxy, 300km/s

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LVG Model results

With the two-component models, At 30 and 90KTdust

6 - Tbg6 = cste

No negative K-correction

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Detecting galaxies at high redshiftwith ALMA // MUSE

For high z galaxies, go to low frequencies z=6 CO(7-6) at 3mm

At 3mm (115GHz), field of 1 arcmin x 1 arcminMost frequently 300x 300 = 90 000 pixels/spectra

Bandwidth 2x 8GHz ~ 16%, or ~50 000km/sPossibility to have several lines from the Rotational ladder of CO, or other molecules..

@z =6, the spacing between CO lines is of 16 GHz.With 2 tunings, one obtains a « redshift-machine »

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Complementarity Optical / Submm

Many submm sources(0.85mm, 1.2mm) have no optical counterparts

Multi-wavelengthstudies are fundamental

MUSE/VLT +JWST+ELT-40m+ALMA

Abell 1835 (Ivison et al 2000)

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Zoo of star-forming galaxies at high z

SDF

SDF

MAHOROBA-11

z=6 sampleby Dow-Hygelund07

LBG, LAE @ z> 5LBG, LAE @ z> 5

ERO, DRG, BzK, SMGERO, DRG, BzK, SMG ･･･････ ･･･････ z<5z<5

Different selection criteria,Different selection criteria,

LAE by the Lya line, LAE by the Lya line,

no continuum in generalno continuum in general

LBG, through continuum, LBG, through continuum,

weak linesweak lines

Should have some overlap,Should have some overlap,

although LAE less massive?although LAE less massive?

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Star formation rate in LBGs

SFE ~140 Mo/Lo

LCO & gas mass7 times higher than cB58

z=2.73

8 o'clock arcAllam et al 2007

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SMGs: Submillimeter GalaxiesStar formation efficiency LIR/L’CO vs z

6 SMGs not detected in CO

Greve et al 2005

40- 200 Myr SB phaseSFR ~700 Mo/yrMore efficient than ULIRGs

Mergers without bulges?

Total masses ~0.6 M*

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Ly-alpha Blobs LABs at z~3 detected in submm

Large SFR 103 Mo/yr, Might be different sources, SB or AGNcD in clusters? Cooling Flows?Superwinds? Radio sources?

Geach et al 2005, 2007

SB Av=3 AGN

X-ray

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Z=3 ULIRGs easy to detect with ALMA

nH2= 106cm-3

nH2= 105cm-3

nH2= 104cm-3

nH2= 103cm-3

M(H2) =6 1010Mo, N(H2) = 3.5 1024 cm-2, CO/H2 ~10-4

T=60K

SKA

ALMA

Size = 1kpc

Influence of density

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Predictions for LBG at z~3: ALMA 24h, 0.1"

Greve & Sommer-Larsen 2008 rms=10 Jy/beam (2-3 )

CO(4-3)

Jykm/s

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Low efficiency of star formation

In BzK galaxies, much more CO emission detected than expectedMassive galaxies, CO sizes 10kpc? L(FIR) ~1012 LoNormal SFR, M(H2) ~ 2 10 10 Mo ~2 Gyr Much larger population of gas rich galaxies at high z

Daddi et al 2008

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SMG versus UV/optical galaxiesBouché et al 2007SMG are very concentrated

But UV galaxies not(High extinction)

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Star formation rate (Schmidt law)Bouché et al 2007More efficient at high gas?

But Xsmaller byfactor 2-4

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Do SMG actually trace massive haloes?

In the GOODS-N field, cluster of RG and SMG at z=1.99The strongest known association of SMG (Chapman et al 2008)Overdensity of 10. But only 2 in UV-selected galaxies Only a mild overdensity, experiencing brief and strong starburst

fieldHighly active merger periodsin modest mass structures

Merger bias

Herschel and ALMA couldprobe a large range ofenvironments

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Prediction of SFR-density reversal

From Elbaz et al 2007 SFR correl with Massand more massive galaxiesin clusters ?

But at z=1,SFR/M* increases with gal

SFR/M*

gal

Only 30% of the SF is due to mergers

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Evolution of Clusters, z=0.4-1

The LIRGs of the cluster CL0024+16, detected by Spitzer at 24 are detected in CO 0.5-1 x 1010 Mo ( SFR ~60Mo/yr) (or x 6 if normal CO/H2 conversion)

Geach et al 2009

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Mergers w or w/o black holes

Narayanan et al 06

With BH without With BH without

Gyr

Kkm/s

z=230"=235kpcCO(1-0)

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APM08279+5255 z=3.9 lensed QSO Influence of AGN feedback on CO emission?

This object is one of the brightest in the sky, and has been observedwith mm and cm telescopes (amplification factor ~50)CO(1-0) to CO(11-10) detectedRecent 0.3" resolution CO(1-0) mapping with VLA (Riechers + 2008)

Previously believed to be extended, CO emission is in 2 peaks,Co-spatial with optical/NIR, may be less amplified than thought (4?)

CO is in a circumnuclear disk of 550 pc radius, inclined by 25°Mgas ~1.3 1011 MoMBH = 2.3 1010Mo, bulge 10x less massive than the MBH- relation

No hint of the influence of the AGN feedback…

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APM08279+5255, Riechers et al 08

VLA __

GBT ---

Keck NIRC HST Chandra

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Excitation in high-z starbursts

Weiss et al 2007

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z> 7 sources: ALMA CO discovery space

Walter & Carilli 2007

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Cloverleaf

CII/LFIR ~0.06%,10 times less than locally

CII detected inJ1148 QSO at IRAM

Other lines CII 158m, CI, NII…CI/H2 ~10-5

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Molecular surveys

TODAY

ALMA prediction

TOMOROW

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Mapping large-scale structures & the environment of SMGs

COSMOS: overdensitiesz=0.25-1.05

With APEX, survey @870muCOSMOS 2deg2 to rms=2mJy: 300-600 sources with S/N>420x20 armin2 at the confusion level, 0.5-07mJy: 200-400 sources

Deeper with SCUBA-2 @450mu, CCAT 200/350mu (25m)

ALMA rms=50Jy N (>0.2mJy) = 60 000/deg2, 870mu FoV 19"1h 1 armin2: 20sources1yr = 1sqdegCertainly several smaller regions

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Molecular Absorptions

Chemistry @highzVariations of cst

~ 30-100 timesmore sourceswith ALMA?

Combes & Wiklind 1998

Up to now, only 5 systems: PKS1413, B3 1504 (self-abs)B0218, PKS1830, PMN J0134 (OH): gravit lenses+ local: CenA, 3C293 (0.045), 4C 31.04 (0.06)

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Cooling flows

Salome et al 2006, 2008Perseus A, nearby

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Conclusions •ALMA deep field in continuum: N(S), SFR (z) and SFH

•the CO lines will be intensively observed at high z with ALMA efficiency of star formation (z), and the kinematics, Mdyn

Now: 4 objects CO-detected at z~4-6: Mdyn ~ Mgas Now: 4 objects CO-detected at z~4-6: Mdyn ~ Mgas Mdyn ~ 20-30 MBH [vs. ~700 today]Mdyn ~ 20-30 MBH [vs. ~700 today]

Evolution with redshift or change toward high-mass end?Evolution with redshift or change toward high-mass end? black holes in QSOs may form before bulk of stellar bodyblack holes in QSOs may form before bulk of stellar body (Riechers, Carilli, et al 2009)

If CO not excited, either CII, or go to GBT, EVLA to detectthe low-J CO lines

•Dark matter as a function of redshift: study of individual galaxies with MUSE+JWST + ELT + ALMAand statistical studies, with Tully-Fisher relation