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From ULIRGs to QSOs

From ULIRGs to QSOs. XiaoYang, Xia Center for Astrophysics Tianjin Normal University Collaborators: H. Wu, Deng, Zou, Z. Zheng, Mao, X.Z. Zheng, Hao, Huo, Y. Gao, Wang,J.L, Tan. Outline. The morphology and environment of ULIRGs and LIRGs May give hint for high-z SMGs

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From ULIRGs to QSOs

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  1. From ULIRGs to QSOs XiaoYang, Xia Center for Astrophysics Tianjin Normal University Collaborators: H. Wu, Deng, Zou, Z. Zheng, Mao, X.Z. Zheng, Hao, Huo, Y. Gao, Wang,J.L, Tan

  2. Outline • The morphology and environment of ULIRGs and LIRGs May give hint for high-z SMGs • Infrared luminous QSOs may give hint on high-z submm loud QSOs Then the relation of ULIRGs with SMGs and IR QSOs with submm loud QSOs

  3. The morphology of ULIRGs • Based on 97 HST snapshot images, we find that all ULIRGs are interacting/merging galaxies and the fractions of single, double and multi-nucleus/nuclei are 43%, 39% and 18%, respectively • The AGN fraction is 80%, 65% to 36% from single, double and multi-nucleus/nuclei • QSOs and ellipticals appear at last stage of merger • Some ULIRGs have extended soft X-ray halo based on Chandra observations (e.g. NGC 6240, Mrk 273)

  4. Cui et al. 2002

  5. The morphology of ULIRGs • All ULIRGs are interacting/merging galaxies and the fractions of single, double and multi-nucleus/nuclei are 43%, 39% and 18%, respectively, based on 97 HST snapshot images. • The AGN fractions are 80% 65% 36% single double multi nucleus/nuclei (total AGN fraction is about 65%, similar as z=1-3 ULIRGs, but little less than 80% for SMGs) • QSOs and ellipticals appear at last stage of merger • Some ULIRGs have extended soft X-ray halo based on Chandra observations (e.g. NGC 6240, Mrk 273)

  6. Z. Zheng, et al. 1999

  7. The morphology of ULIRGs • Based on 97 HST snapshot images, we find that all ULIRGs are interacting/merging galaxies and the fractions of single, double and multi-nucleus/nuclei are 43%, 39% and 18%, respectively • The AGN fraction is 36%, 65% to 80% from single, double and multi-nucleus/nuclei • QSOs and ellipticals appear at last stage of merger • Some ULIRGs have extended soft X-ray halo based on Chandra observations (e.g. NGC 6240, Mrk 273)

  8. Huo et al. ApJ 2004

  9. Mrk273 108x80 kpc Xia et al. 2002

  10. NGC 6240 Huo et al. 2004

  11. ·· · Ellipticals Groups ULIRGs

  12. Not all local ULIRGs will be sub-L* ellipticals • Some ULIRGs may form from group and will be massive ellipticals • Such case could be more at higher-z

  13. This result is conflict with lower metallicity in center of ULIRGs based on optical analysis “we find that LIRGs and ULIRGs are underabundant by a factor of 2 on average” by Rupke et al.2008, ApJ, 674, 172

  14. Le Floc'h et al., 2006

  15. Morphology of LIRGs Wang, et al. 2006, ApJ, 649, 722 Based on SDSS DR2 159 images (R<15.9m and z<0.1)

  16. Barred spiral

  17. The morphology of LIRGs • The fractions of interacting/merging and normal spirals are 50% and 40%, respectively • 75% spirals are with strong bar

  18. Lir<4x10^11 Lsun

  19. Interacting/merging Spirals Wang et al. 2006, ApJ

  20. Infrared luminous QSOs QSOs with Lir>10^12Msun

  21. IR QSOs sample • QDOT IRAS galaxy sample(Lawrence et al. 1999) • 1 Jy ULIRGs sample(Kim & Sanders 1998) • IRAS-ROSAT cross-identification sample(Moran et al. 1996) • A sample of 31 IR QSOs (z<0.35)，takes a fraction of about 25% in local universe.

  22. Zheng, X.Z., 2002

  23. Zheng, 2002

  24. ● PG QSOs IR QSOs ○ Hao, et al. 2005

  25. BH mass of ULIRGs is 10^7-10^8Msun

  26. Samples by Spitzer IRS 19 IR QSOs Hao et al. 2005, 15 have both low & high –res obs. 35ULIRGs IRAS 1-Jy sample and Spitzer GTO #105 + High-resolution mid-IR data, Farrah et al. (2007) 20PG QSOs Spitzer GTO & GO #14, 3187 & 20142, with enough S/N, z<0.27 + PG QSOs from QUEST (Schweitzer et al. 2006)

  27. ③ The low resolution mid-infrared spectra of IR QSOs Cao, et al. 2008

  28. ③ Fine structure line [NeII] 12.81m  SFR indicator in QSOs

  29. ③

  30. ③

  31. ③ SFR/Mdot SFR/Mdot Feedback may play role to suppress both star formation and AGN Anti-correlated H blueshift

  32. High-z SMGs are scaled up of ULIRGs • Are high-z submm-loud QSOs are scaled up of IR QSOs? 30% high-z QSOs detected at submm

  33. High-z (sub)mm loud QSOs • Optically selected QSOs at redshift about 4 with 1.2mm observation, Omont et al. (2001) • Optically selected QSOs at redshift about 4 with 1.2mm observation, Carilli et al. (2001) • Optically selected QSOs at redshift about 2 with 1.2mm observation, Omont et al. (2003) • X-ray absorbed and submillimeter detected QSOs Stevens et al. (2005) • CO/HCN detected QSOs Carrilli et al. (2002, 2005)

  34. Carilli et al. 2007 Z=6 Z=6 Z=6 Hao, et al. 2008

  35. Molecular gas of IR QSOs(Xia, Gao, Hao, Omont,Leon, Ocana, Tan and Mao) Sample IR QSOs 20 observed at 2008 fall PG & HE QSOs 24 ULIRGs 36 SMG 12 submm-loud QSOs 15

  36. 15/20 IR QSOs detected by IRAM 30m

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