1 / 30

MUSE & ALMA

MUSE & ALMA. Françoise Combes Observatoire de Paris Toulouse, 19 March 2009. 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 beginning 84-116 GHz, 211-275 GHz, 275-370 GHz, 602-720 GHz

tex
Download Presentation

MUSE & ALMA

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. MUSE & ALMA Françoise Combes Observatoire de Paris Toulouse, 19 March 2009

  2. 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 beginning 84-116 GHz, 211-275 GHz, 275-370 GHz, 602-720 GHz Large 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

  3. Main privilege of the mm/submm domain Negative K-correction: example of Arp 220

  4. K-correction for the CO linesSimple Model of a starburst ~ ULIRG Very high molecular masses 1010 - 1011 Mo High 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, 90K 2-each embedded in a cloud 104cm-3, 30K Individual velocity dispersion of 10km/s Embedded in the rotational gradient of the galaxy, 300km/s

  5. LVG Model results With the two-component models, At 30 and 90K Tdust6 - Tbg6 = cste  No negative K-correction

  6. 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 arcmin Most frequently 300x 300 = 90 000 pixels/spectra Bandwidth 2x 8GHz ~ 16%, or ~50 000km/s Possibility 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 »

  7. Complementarity Optical / Submm Abell 1835 (Ivison et al 2000) Many submm sources (0.85mm, 1.2mm) have no optical counterparts Multi-wavelength studies are fundamental MUSE/VLT + JWST+ELT-40m +ALMA

  8. z=6 sample by Dow-Hygelund07 SDF SDF MAHOROBA-11 Zoo of star-forming galaxies at high z LBG, LAE @ z> 5 ERO, DRG, BzK, SMG･･･････ z<5 Different selection criteria, LAE by the Lya line, no continuum in general LBG, through continuum, weak lines Should have some overlap, although LAE less massive?

  9. Star formation rate in LBGs SFE ~140 Mo/Lo LCO & gas mass 7 times higher than cB58 z=2.73 8 o'clock arc Allam et al 2007

  10. SMGs: Submillimeter GalaxiesStar formation efficiency LIR/L’CO vs z Greve et al 2005 6 SMGs not detected in CO 40- 200 Myr SB phase SFR ~700 Mo/yr More efficient than ULIRGs Mergers without bulges? Total masses ~0.6 M*

  11. X-ray AGN SB Av=3 Ly-alpha Blobs LABs at z~3 detected in submm Large SFR 103 Mo/yr, Might be different sources, SB or AGN cD in clusters? Cooling Flows? Superwinds? Radio sources? Geach et al 2005, 2007

  12. T=60K Influence of density ALMA SKA Size = 1kpc Z=3 ULIRGs easy to detect with ALMA M(H2) =6 1010Mo, N(H2) = 3.5 1024 cm-2, CO/H2 ~10-4 nH2= 106cm-3 nH2= 105cm-3 nH2= 104cm-3 nH2= 103cm-3

  13. Predictions for LBG at z~3: ALMA 24h, 0.1" CO(4-3) mJykm/s Greve & Sommer-Larsen 2008 rms=10 mJy/beam (2-3 s)

  14. Low efficiency of star formation In BzK galaxies, much more CO emission detected than expected Massive galaxies, CO sizes 10kpc? L(FIR) ~1012 Lo Normal SFR, M(H2) ~ 2 10 10 Mo t ~2 Gyr  Much larger population of gas rich galaxies at high z Daddi et al 2008

  15. SMG versus UV/optical galaxies Bouché et al 2007 SMG are very concentrated But UV galaxies not (High extinction)

  16. Star formation rate (Schmidt law) Bouché et al 2007 More efficient at high Sgas? But X smaller by factor 2-4

  17. Do SMG actually trace massive haloes? In the GOODS-N field, cluster of RG and SMG at z=1.99 The 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 • Highly active merger periods • in modest mass structures • Merger bias Herschel and ALMA could probe a large range of environments field

  18. SFR/M* Sgal Prediction of SFR-density reversal Only 30% of the SF is due to mergers From Elbaz et al 2007 SFR correl with Mass and more massive galaxies in clusters ? But at z=1, SFR/M* increases with Sgal

  19. Evolution of Clusters, z=0.4-1 The LIRGs of the cluster CL0024+16, detected by Spitzer at 24 m 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

  20. Mergers w or w/o black holes With BH without With BH without Kkm/s z=2 30"= 235kpc CO(1-0) Gyr Narayanan et al 06

  21. APM08279+5255 z=3.9 lensed QSOInfluence of AGN feedback on CO emission? This object is one of the brightest in the sky, and has been observed with mm and cm telescopes (amplification factor ~50) CO(1-0) to CO(11-10) detected Recent 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 Mo MBH = 2.3 1010Mo, bulge 10x less massive than the MBH-s relation No hint of the influence of the AGN feedback…

  22. VLA__ GBT --- APM08279+5255, Riechers et al 08 Chandra Keck NIRC HST

  23. Excitation in high-z starbursts Weiss et al 2007

  24. z> 7 sources: ALMA CO discovery space Walter & Carilli 2007

  25. Other lines CII 158m, CI, NII… CI/H2 ~10-5 Cloverleaf CII/LFIR ~0.06%, 10 times less than locally CII detected in J1148 QSO at IRAM

  26. Molecular surveys TODAY TOMOROW ALMA prediction

  27. Mapping large-scale structures & the environment of SMGs With APEX, survey @870mu COSMOS 2deg2 to rms=2mJy: 300-600 sources with S/N>4 20x20 armin2 at the confusion level, 0.5-07mJy: 200-400 sources Deeper with SCUBA-2 @450mu, CCAT 200/350mu (25m) ALMA rms=50mJy N (>0.2mJy) = 60 000/deg2, 870mu FoV 19" 1h 1 armin2: 20sources 1yr = 1sqdeg Certainly several smaller regions COSMOS: overdensities z=0.25-1.05

  28. Molecular Absorptions 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) Chemistry @highz Variations of cst ~ 30-100 times more sources with ALMA? Combes & Wiklind 1998

  29. Cooling flows Perseus A, nearby Salome et al 2006, 2008

  30. 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 • Mdyn ~ 20-30 MBH [vs. ~700 today] • Evolution with redshift or change toward high-mass end? • black 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 detect the low-J CO lines • Dark matter as a function of redshift: study of individual galaxies • with MUSE+JWST + ELT + ALMA • and statistical studies, with Tully-Fisher relation

More Related