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D. B. Sanders Institute for Astronomy, University of Hawaii

The Dusty and Molecular Universe: A prelude to HERSCHEL and ALMA, 27-29 Oct, 2004, Paris. Starbursts and ULIRGs. Gas-Rich Mergers and the origin of nuclear starbursts and AGN. D. B. Sanders Institute for Astronomy, University of Hawaii. OUTLINE. IR Galaxies: SEDs, LF (vs.z)

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D. B. Sanders Institute for Astronomy, University of Hawaii

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  1. The Dusty and Molecular Universe: A prelude to HERSCHEL and ALMA, 27-29 Oct, 2004, Paris Starbursts and ULIRGs Gas-Rich Mergers and the origin of nuclear starbursts and AGN D. B. Sanders Institute for Astronomy, University of Hawaii

  2. OUTLINE • IR Galaxies: SEDs, LF (vs.z) • Origin & Evolution of LIGs/ULIGs • ULIGs: Superstarbursts and AGN • ULIGs and QSOs IRAS - ISO - SCUBA - MAMBO (1984) (1996) (1997) (1999) z <0.3 z < 1.5z < 5-6 ? SIRTF+AstroF - Herschel - ALMA (2003) (2006) (2008) (2010) z = 0-10?

  3. Two IRAS All-Sky Surveys: IRAS Revised Bright Galaxy Sample(RBGS:S60>5.24Jy) 638 Galaxies IRAS 1-Jy ULIG Sample(1-Jy:S60>1.0Jy,Lir > 1012 Lsun) 118 Galaxies

  4. Radio-to-UV SEDs of IRAS Selected Galaxies 638 Galaxies: f((60m) > 5 Jy 118 ULIGs: f((60m) > 1 Jy “Infrared Galaxies”  (f)IR / (f)opt > 1

  5. Galaxy Luminosity Functions slope = -1 LFIR high luminosity tail:   L-2.35  (z)  (1+z)5-8  3.5  (z <0.2) ~ 0.008 deg-2

  6. The Hubble Deep Field (The opt/UV view) The FIR/submm view SCUBA 850m

  7. kindly provided by Helmut Dannerbauer

  8. ULIGs at High Redshift ULIGs @ z ~ 2 – 4 f850 ~ 1 – 10 mJy m K ~ 20 – 24 m I ~ 24 – 30 m B ~ 26 – 33

  9. Galaxy Luminosity Functions slope= -1 Z ~2.4 Z=0.80 Z=0.40 Z=0.13 Z=0.045

  10. The “Star Formation Rate” versus Redshift

  11. The Origin and Evolution of Luminous Infrared Galaxies Strong Interactions/Mergers of Molecular Gas-rich Disks

  12. IRAS RBGS Optical Images of LIGs Log LIR = 11.66 - 11.99 Ishida, ApJL (2003) Log LIR = 11.10 - 11.48

  13. IRAS RBGS Optical Images of LIGs Ishida, ApJL (2003) Log LIR = 11.49 - 11.99

  14. IRAS RBGS Conclusion: In the range log(Lir/Lo) = 11.6 - 12.0, LIGs are in the final stages of merging, with a typical “pre-merger” time of tm < 3 x 108 years

  15. IRAS RBGS Optical Images Log LIR = 12.00 - 12.51 Ishida, ApJL (2003)

  16. IRAS RBGS Nuclear Separation vs. Lir

  17. IRAS RBGS Conclusion: At log(Lir/Lo) > 12.0, > 40% of ULIGs have merged and the remainder will merge within a time of tm < 108 years

  18. SummaryProperties of IRAS RBGS+1Jy ULIG samplesLog(LIR/Lsun) = 11.40 - 12.70 • Sources are predominantly strongly interacting/merging spiral pairs •  MK Tot ~ 2 LK* • MK pair ratio < 3:1 • LIR pair ratio < 5:1 • Pairs are predominantly late type spirals (Sb, Sc) • Both components are molecular gas rich (MH2 ~ 109 - 10Msun) •  pair separation  as  pair LIR   • ( Evidence for buildup of dense nuclear gas concentrations ) • ( Evidence for creation of luminous Seyfert 1 nuclei) • ( Evidence for S + S  E )

  19. LCO N=53 LHCN

  20. LIR/LHCN LHCN LCO LIR/LCO

  21. Log (LIR/Lsun) = 11.01 Int. Class = 3 Gao et al. Mirabel et al. Hibbard et al. Ponman et al.

  22. UGC 83038 = Mrk 231 Log (LIR/Lsun) = 12.57 Int. Class = 4 Sanders et al. Hutchings & Neff Scoville et al. Surace et al

  23. SummaryNuclear Molecular Gas Concentrations @ r < 700 pcGeneral Results for ULIGs • Mnuc/Mtot = 40 – 100 % • Mnuc = 1 – 3 x 1010Msun •   (H2) ~ 0.65 – 2 x 1010Msun •  n (H2)spherical ~ 130 – 400 cm-3 • => ffnuc ~ 1 (for a population of W3-like GMCs) •  N (H2)spherical~ 10 23.2 – 23.7 cm-2 OVRO Interferometer Bryant, Scoville et al. 1993-9

  24. Summary Optical Spectral Classification of LIGs+ULIGs Veilleux, Kim & Sanders (1998) KPNO 4m + UH 2.2m

  25. 1-D surface brightness radial profiles

  26. SummaryHost Properties of 1-Jy Sample of ULIGsLog(LIR/Lsun) > 12.0 • redshift range: 0.018 – 0.271 •  MK Tot ~ 2.7 LK* •  MR Tot ~ 2.5 LR* • ~ 1/3 are E (r1/4-law profile @ r ~ 1.5 – 6.0 kpc) • ~ 1/3 are E/Sp • ~ 1/3 are “amorphous/chaotic”

  27. Beyond the IRAS RBGS Sample … Question: What happens Next ?

  28. A Plausible Scenario … LIG ULIG QSO

  29. Evolution of Fine Structure in a “post-merger” simulation Barnes (2002)

  30. Evolution of the Luminosity Profile for a “Post-Merger” Remnant Barnes (2002) R = 27.5 mag arcsec-2 (kpc)

  31. Near-IR Imaging of PGQSOs with Gemini-North Hopuka’a AO System (Olivier Guyon 2002) PG 1411+442 40x40 kpc “Raw Image” (resolution ~0.12 arcsec) PSF-subtracted image ~24 magH arcsec-2 (3)

  32. NIR-AO Imaging of a Complete Sample of 38 PGQSOs Olivier Guyon, PhD Thesis, 2002 Raw (H-band) -psf - <radial profile> Gemini-N 8m

  33. NIR-AO Imaging of a Complete Sample of 38 PGQSOs Olivier Guyon, PhD Thesis, 2002 Raw (H-band) -psf- <radial profile> Mean Radio-to-Xray SED of PGQSOs

  34. Warped Disk ModelSanders, Phinney et al. (1989)

  35. PGQSOs typically have dominant spheroids + a moderate disk component (central bars, mini-spirals, …) • PGQSO hosts typically have faint tidal debris

  36. “SFR + MBH” versus Redshift

  37. Summary • Good evidence for S + S -> E merger sequence for ULIGs • Good evidence for creation of luminous Seyfert 1 nuclei in ULIGs • Confirmation of strong evolution with z in the ULIG population • ISOPHOT Deep Field sources consistent with LIG/ULIGs (z ≈ 0 -1.5) • ?? SCUBA Deep Field sources consistent with LIG/ULIGs (z ≈2 - 4)?? • [“SFR” vs. z ]opt+UV [“SFR” vs. z ]IRAS+ISO+SCUBA • High-z ULIGs may represent epoch of spheroid / MBH formation

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