HLIRGS, An X-ray view
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HLIRGS, An X-ray view

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Talk about HLIRG for the international astrophysics spring school "Observing the X- and Gamma-Ray Sky", on April 2006, at the Institute of Scientific Studies, Cargese, Corsica (France). ...

Talk about HLIRG for the international astrophysics spring school "Observing the X- and Gamma-Ray Sky", on April 2006, at the Institute of Scientific Studies, Cargese, Corsica (France).

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  • LIRGs: población extragaláctica dominante para luminosidades IR >10^11Lsol, mayor densidad espacial que cualquier otra clase de galaxia de luminosidad bolometrica comparable ULIRGs: raros en el Universo local, pero existe una gran población a z > 1-3. Podrían dominar la formación estelar en el Universo. HLIRGs: exhiben tasas de formación estelar superiores a 1000 Msol/yr, y la mayoría parece que contienen un AGN

Transcript

  • 1. HYPER-LUMINOUS INFRARED GALAXIES An X-ray view Ángel Ruiz Camuñas F. Panessa, F. Carrera Cargèse – 7 April 2006
  • 2. HLIRGs: Introduction
    • LIRGs: L IR > 10 11 L 
      • ULIRGs: L IR > 10 12 L 
        • HLIRGs: L IR > 10 13 L 
  • 3. HLIRGs: Introduction
    • ~50 detected HLIRGs, ~100-200 estimated with 60  m flux >200 mJy over the whole sky.
    • Unique laboratories to investigate extremely high star formation ( ~1000 M  /yr ) and its conection to supermassive black holes.
    • Evolutionary conection: QSO  ULIRG  HLIRG
    • Cosmic X-ray and infrared background.
  • 4. HLIRGs: Introduction
    • Three hypothesis:
      • High-luminosity tail of the ULIRGs : starburst and/or AGN triggered by interactions and mergers.
      • Very young galaxies during their maximal star formation episode.
      • IR emission via other mechanism (different new class of object): e.g. transient IR luminous phase in the QSO evolution.
  • 5. HLIRGs: Samples
    • Sub-samples from Rowan-Robinson (2000):
      • Farrah et al. 2002:
        • Detected HLIRGs in FIR or submm surveys. Complete, homogeneous and unbiased to AGNs.
        • (8 sources with our own XMM data in the future)
      • XMM-sample:
        • All sources with public data in the XMM-Newton archive in December 2004, and redshift between ~0.3 y ~1.5. (9 sources, 2 from Farrah sample)
        • Previous results suggest that some sources could be highly obscured and no direct X-ray emission is detected: Compton-thick sources .
        • Franceschini et al. 2003: ULIRGs comparison sample .
  • 6. HLIRGs: Sample +10 41 32 00 26 06.5 0.575 Starburst IRAS F00235+1024 +45 40 36 12 08 58.0 1.158 QSO PG 1206+459 +70 31 33 16 34 28.9 1.334 QSO IRAS 16347+7037 +38 32 14 14 23 55.0 1.21 QSO IRAS F14218+3845 +64 20 36 18 21 57.3 0.297 QSO IRAS 18216+6418 +32 42 47 15 32 44.0 0.926 Seyfert 2 IRAS F15307+3252 +10 11 12 12 54 00.8 0.3 Seyfert 2 IRAS 12514+1027 +40 56 28 09 13 45.4 0.442 Seyfert 2 IRAS 09104+4109 -70 55 27 00 20 34.7 0.327 LINER IRAS 00182-7112 DEC RA z Type Source
  • 7. HLIRGs: Objectives
    • Determine the relative contribution of AGN and starburst emission to the bolometric luminosity and their interplay.
    • X-ray study contributes:
      • Search of “hard” (2-10 keV) non thermal emission (associated to AGN or HMXB from the starburst).
      • Search of “soft” (0.2-2 keV) emission using thermal models (probably associated to starburst): Thermal emission .
      • Search of absorption features and FeK emission lines.
  • 8. IRAS 00182-7112 IRAS 09104+4109 IRAS 12514+1027 PG 1206+459 IRAS F14218+3845 IRAS F15307+3252 IRAS 16347+7037 IRAS18216+6418
  • 9. HLIRGs: Spectral analysis TH: Thermal model NTH: No thermal model LINE: FeK emission line <42.4 <44.3 0.5 - IRAS F00235+1024 <44.0 45.1 0.6 NTH PG 1206+459 <43.8 44.6 0.6 NTH IRAS F14218+3845 45.1 45.6 0.49 ± 0.09 TH + NTH IRAS 18216+6418 45.7 46.0 1.53 ± 0.18 TH + NTH IRAS 16347+7037 <43.1 43.7 0.6 NTH IRAS F15307+3252 42.2 43.3 0.35 +0.17 -0.07 TH + NTH IRAS 12514+1027 <43.0 44.5 0.6 LINE + NTH IRAS 09104+4109 <41.9 44.8 0.6 LINE + NTH IRAS 00182-7112 Log L th Log L po kT Model Source Starburst LINER Seyfert 2 QSO
  • 10. HLIRGs: Discussion (I)
    • “ Mixed” sources.
    • Same tendency as AGN-dominated ULIRGs.
    Infrared luminosity 2-10 keV NTh luminosity
  • 11. HLIRGs: Discussion (II) AGN and starburst contribution using infrared SED Rowan-Robinson (2000) QSO X-ray / infrared luminosity ratio Elvis et al. (1994) IR X
  • 12. HLIRGs: Discussion (II) Relative contribution to the infrared emission from the AGN
    • Significative difference between X-ray and IR estimation.
    1 to 1 line Using XMM-Newton data and local quasar SED Using fits to the infrared SED
  • 13. HLIRGs: Discussion (II)
    • Two hypothesis:
      • AGN in HLIRGs have a different SED from a local QSO (Elvis et al. 1994).
      • Compton-thick sources.
    • Source by source analysis.
  • 14. HLIRGs: Discussion (III)
    • Only three sources with thermal emission.
    Franceschini et al. 2003 correlation 2-10 keV PL luminosity 0.5-10 keV thermal luminosity
  • 15. HLIRGs: Discussion (IV)
    • SFR evolution probably due to selection effects.
    • XR/IR ~constant with z -> AGN and SB physically conected.
    Redshift SFR L(0.5-10)/LIR IRAS sensitivity limit HLIRGs limit Elvis et al. 1994 ratio
  • 16. HLIRGs: Conclusion
    • Heterogeneous sources.
    • Thermal component detected only in three sources. Two of them can not be starburst.
    • “ Mixed ” AGN + starburst sources .
    • Local quasars SED not valid in three sources (intrinsic AGN infrared excess).
    • Absorption detected with XMM data only on two sources. Multi-wavelength analysis reveals five Compton-thick sources .
    • Estimating the AGN contribution is hard with X-ray observations only.
    • This results in detail will be publish in A. Ruiz et al. 2006 (in preparation).