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Starburst galaxies at low and high redshift

Starburst galaxies at low and high redshift. ESO, Santiago April 2006. Credits. starbursts at high redshift Kirsten Kraiberg Knudsen (PhD October 2004) Tracy Webb (McGill University, Montreal) Lottie van Starkenburg (SINFONI) and the FIRES team: Marijn Franx Pieter van Dokkum (Yale)

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Starburst galaxies at low and high redshift

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  1. Starburst galaxies at low and high redshift ESO, Santiago April 2006

  2. Credits • starbursts at high redshift • Kirsten Kraiberg Knudsen (PhD October 2004) • Tracy Webb (McGill University, Montreal) • Lottie van Starkenburg (SINFONI) and the FIRES team: • Marijn Franx • Pieter van Dokkum (Yale) • Ivo Labbé (Carnegie) • Greg Rudnick (NOAO) • Hans-Walter Rix (MPIA) • Mariska Kriek • Natascha Förster Schreiber (MPE) • Alan Moorwood (ESO) • starbursts at low redshift • Leonie Snijders (VISIR) • Liesbeth Vermaas (SINFONI) • Kate Isaak (Cardiff) • Padelis Papadopoulos (ETH Zürich) Starburst galaxies at low and high redshift

  3. « The stellar systems are scattered through space as far as telescopes can penetrate. We find them smaller and fainter, in constantly increasing numbers, and we know that we are reaching out into space, until, with the faintest nebulae than can be detected with greatest telescopes, we arrive at the frontiers of the known Universe. » Edwin Hubble, The Realm of the Nebulae (1936) Starburst galaxies at low and high redshift

  4. What is a starburst galaxy? A starburst galaxy is a galaxy with such a high star formation rate that it will turn all of its gas into stars in tb << tHubble Milky Way: correction factor for mass return from stars  gradual buildup of disk Starburst galaxies at low and high redshift

  5. A luminous infrared galaxy: the Antennae • Crossing orbits give • gas concentration in • interaction zone • Intense obscured • star formation in • overlap region • Most intense star formation is obscured SCUBA 850 mm (Webb, Snijders & Van der Werf , in preparation) Starburst galaxies at low and high redshift

  6. Arp220 An ultraluminous infrared galaxy: Arp220 Starburst galaxies at low and high redshift

  7. Starformation in ULIRGs Arp220: correction factor for mass return from stars NB: tb few 108 yrs  merger timescale  dynamical timescale (crossing/rotation time)  free-fall time protogalaxy? Such high SFRs can build up an entire galaxy in t << tHubble relation to galaxy formation? Starburst galaxies at low and high redshift

  8. Simple-minded estimate of "maximum star formation rate" In the absence of external pressure, the maximum star formation rate occurs when a gas mass is turned into stars on the free-fall timescale.  initial starburst– rapid formation of bulk of the stellar population  formation of spheroids? Implication: high SFRs are found in the most massive galaxies Starburst galaxies at low and high redshift

  9. Do “maximum starburst” galaxies exist? ultraluminous IR galaxies (ULIRGs) maximum starbursts luminous IR galaxies (LIRGs) normal galaxies (Kennicutt 1998) Starburst galaxies at low and high redshift

  10. ULIRGs ULIRGs as “maximum starbursts” (cf., 30–50% for normal spirals) Starburst galaxies at low and high redshift

  11. LIR/LCO  SFR/MH2  SFE (Gao & Solomon 2001) LIR SFR Starformation efficiency • Starbursts cannot • be simply scaled up. • More intense starbursts are also more efficient with their fuel. Starburst galaxies at low and high redshift

  12. LIR/LCO  SFR/MH2  SFE (Gao & Solomon 2001) Role of dense gas LHCN/LCO mass fraction of dense gas • More dense gas means more efficient star formation. Starburst galaxies at low and high redshift

  13. NGC 4038/4039 detail NGC 4038/4039 Orion (M42) 30 Doradus Superstarclusters:does size matter? NGC4038/4039 cluster:  100 pc Orion:  1.5 pc Starburst galaxies at low and high redshift

  14. Superstarclusters: densities Starburst galaxies at low and high redshift

  15. contours: dust continuum [NeII] 12.8 m ESO/VLT VISIR (Snijders et al., in prep.) The Antennae with Spitzer and VISIR IRAC/Spitzer (Wang et al., 2004) Starburst galaxies at low and high redshift

  16. Probing dense molecular gas molecular gas temperature of dense gas dense molecular gas Starburst galaxies at low and high redshift

  17. Dense gas in the ULIRG Mrk231 (Papadopoulos & Van der Werf 2001) Mrk231 CO 65 and 43 RxW/JCMT (Papadopoulos, Isaak & Van der Werf 2006) Starburst galaxies at low and high redshift

  18. Again: dense gas in Mrk231 Mrk231 CO 32 and 10HCN 43 RxB3/JCMT (Papadopoulos, Isaak & Van der Werf 2006) Starburst galaxies at low and high redshift

  19. Two phases of molecular gas • Combine these data with CO 10, 21 and 13CO 21 (upper limit): no model reproduces all CO lines: CO 43/65 and CO 10/21/32 probe different gas phases. diffuse phase: T  50—85 K and n  300—103 cm—3, dense phase: T  50—65 K and n  104 cm—3. • Total mass of molecular gas from CO: M  3.5∙1010 M (or up to a factor 4—5 lower). Mass of dense molecular gas from HCN: M  1.5—3.5∙1010 M. Almost all molecular gas in Mrk231 is dense. Starburst galaxies at low and high redshift

  20. ULIRGs and galaxy formation • Locally, ULIRGs are energetically unimportant: contribute only 2% of local bolometric energy density How important are ULIRGs at high z?  observe redshifted far-IR emission in submillimetre with JCMT/SCUBA • Local ULIRGs almost always have a hidden AGN: causal link with the extreme starburst? Are high-z ULIRGs the sites of the coeval formation of spheroids and supermassive black holes?  question for the coming decade Starburst galaxies at low and high redshift

  21. 1mm1mm1nm Microwave Background IR/Optical Background X-Ray Background Stars+BlackHoles AGN Big Bang Cosmic energy density (Puget et al. 1996, Hauser et al. 1998 Fixsen et al. 1998) Starburst galaxies at low and high redshift

  22. Is obscured star formation important? • Direct starlight: • Far-IR background: nIn = 1.7 . 10-5erg/s/cm2/sr nIn = 3.1 . 10-5erg/s/cm2/sr Obscured star formation dominates. Starburst galaxies at low and high redshift

  23. Submillimetre cosmology • Submm samples have high proportion of high-z galaxies • Galaxies up to z 10 detectable • Brightness-limited volume-limited • Luminosities without precise redshifts • Sources do not fade much from z=1 to 10 • Deeper surveys probe fainter galaxies, not higher z Largenegativek-correction: Starburst galaxies at low and high redshift

  24. Counts and backgrounds Resolved background at 850mm:  25% down to 2 mJy Connection to other populations at fainter flux levels. Lensing can probe these. Submm background comes from small number of (ultra)luminous galaxies Starburst galaxies at low and high redshift

  25. SCUBA/JCMT lensed galaxy survey • 12 gravitationally lensing clusters • 1 blank field (NTT Deep Field) • Survey area 72 arcmin2 • Deepest fields are confusion-limited (2 mJy) • 55 sources detected at 850 m Knudsen PhD thesis Van der Werf Starburst galaxies at low and high redshift

  26. Faint submillimetre source counts • Counts imply strong evolution • First time the faint submm population is substantially probed • Connection with optical population • Turnover in counts detected for the first time (Knudsen, Van der Werf & Kneib, in prep.) Starburst galaxies at low and high redshift

  27. Submillimetre source counts and evolution luminosity evolution: L (1+z)p density evolution: N (1+z)q Counts + background imply pure luminosity evolution proportional to (1+z)3 Starburst galaxies at low and high redshift

  28. Submm galaxies in the NTT Deep Field Not an ERO (?) ERO (Knudsen et al. in preparation) Starburst galaxies at low and high redshift

  29. FIRES: Faint Infrared Extragalactic Survey ISAAC/Antu HDF-S: Labbé et al., 2003 MS1054—03: Förster Schreiber et al., 2006 Starburst galaxies at low and high redshift

  30. Starburst galaxies at low and high redshift

  31. I814 Ks FIRES allows better mass selection the 6 most massive z 3 galaxies in the HDF-S • FIRES allows selection of high-z galaxies in the rest-frame V-band • much closer to a mass-selection than rest-frame UV • a new class of high-z galaxies: Distant Red Galaxies (DRGs) Starburst galaxies at low and high redshift

  32. Rest-frame SEDs: Lyman break galaxies Starburst galaxies at low and high redshift

  33. Rest-frame SEDs: distant red galaxies (Förster Schreiber et al., 2004) Starburst galaxies at low and high redshift

  34. Selection of distant red galaxies (Franx et al., 2003) Starburst galaxies at low and high redshift

  35. DRGs are (mostly) star forming galaxies star formation rates > 100 M yr—1 (Van Dokkum et al., 2004) Starburst galaxies at low and high redshift

  36. SCUBA observations of MS1054–03 M1383 S850 = 5 mJy Starburst galaxies at low and high redshift

  37. Submm galaxies and DRGs • Lyman Break Galaxies have no detectable submm emission even after massive source stacking • Distant Red Galaxies are massive and have high SFRs • DRGs: 3 arcmin–2 for K<22.5 same source density as submm galaxies with >0.8 mJy at 850 m • 1 FIRES field observed with SCUBA: 1 DRG detected directly (5 mJy) • connection between sub-mJy submm galaxies and DRGs? Starburst galaxies at low and high redshift

  38. Stacking DRGs DRGs, EROs DRGs: S850 = 1.11  0.28 mJy (Knudsen et al., 2005) random positions Starburst galaxies at low and high redshift

  39. Breaking the confusion barrier: gravitational lenses A2218 Starburst galaxies at low and high redshift

  40. A2218: SCUBA 850 m Starburst galaxies at low and high redshift

  41. The submm triple behind A2218 Triple image, z=2.515 Magnification in total factor 40 Intrinsic 850 m flux: 0.8 mJy Redshifted H: strong star formation J–K=2.7: Distant Red Galaxy (Kneib et al., 2004a) Starburst galaxies at low and high redshift

  42. CO 3–2 detection of the submm triple (Sheth et al., 2004; Kneib et al., 2005b) Detected both at Owens Valley and Plateau de Bure CO line width  less massive than bright SMGs but comparable to DRGs Starburst galaxies at low and high redshift

  43. Conclusions and outlook: low z • Gas density is crucial in determining starburst properties; also related to depth of potential well? • Luminous starbursts tend to have both high L/M and high M • Molecular lines probe density/temperature structure • The future: SINFONI+LGS, APEX, HIFI/Herschel, ALMA Starburst galaxies at low and high redshift

  44. Conclusions and outlook: high z • Starbursts are a key process in galaxy evolution • We are looking back towards a strongly obscured universe, energetically dominated by dusty starbursts • DRGs are massive and have high SFRs; as a population they are at least as important as LBGs for cosmic mass budget and SFR • Connection between DRGs and faint submm galaxies • The future: SCUBA2, ALMA, HAWK-I, JWST, ELT Starburst galaxies at low and high redshift

  45. To coldly go…: SCUBA-2 • SCUBA-2 will bring rectangular array imaging to submm astronomy • 8 4032 sub-arrays – 4 at 850 m, 4 at 450 m • Mapping speed unequalled • Operational mid-2007 • Legacy programs defined: • Cosmological survey • Full Galactic plane survey • Full Gould’s Belt survey • Shallow “all-sky” survey • Unbiased debris disk survey Starburst galaxies at low and high redshift

  46. SCUBA-2 Cosmology Legacy Survey 1 deg2 field, will be mapped to confusion limit in 23 hours by SCUBA-2 at 850 m • 4 PIs: Dunlop, Halpern, Smail, Van der Werf • Large survey (20 deg2) at 850 m, deep survey at 450 m (0.5 deg2) • 450 m survey will resolve full submm background and detect all LIRGs in the survey area out to z=2 (ULIRGs out to z=4) • Connection with other populations: optical, near-IR, X-ray, radio,… • Time allocation 102 good nights (including 50% of the best weather until mid-2009) SCUBA-2 field-of-view Starburst galaxies at low and high redshift

  47. « We are, by definition, in the very center of the observable region. We know our immediate neighborhood rather intimately. With increasing distance, our knowledge fades, and fades rapidly. Eventually, we reach the dim boundary, the utmost limits of our Telescopes. There, we measure shadows, and we search among ghostly errors of measurement for landmarks that are scarcely more substantial. The search will continue. Not until the empirical resources are exhausted, need we pass on the dreamy realms of speculation. » Edwin Hubble, The Realm of the Nebulae (1936) Starburst galaxies at low and high redshift

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