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Population census, a case study & how to find more

Active intermediate-mass black holes (M BH <10 6 M sun ). Population census, a case study & how to find more. M ó nica Valencia-S. I. Physikalisches Institut. Universität zu Köln.

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Population census, a case study & how to find more

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  1. Active intermediate-mass black holes (MBH<106 Msun) Population census, a case study & how to find more Mónica Valencia-S. I. Physikalisches Institut. Universität zu Köln In collaboration with: A. Eckart, J. Zuther, C. Iserlohe, M. Garcia-Marin, A. Zensus, S. Smajic, M. Vitale, G. Busch, S. Fisher, L. Moser, M. Bremer, C. Straubmeier

  2. Over-classification vs. Unification SDSS J092600+442736 z=0.187. (c) SDSS NGC 6240. (c) NASA, CXC, MIT, STSc I, C. Canizares, and M. Nowak Cen A .(c) NASA, CXC, CfA, R.Kraft+, MPIfR, ESO, WFI, APEX, A.Weis+ HE0450-2958 HE1239-2426 (c) NASA,ESA, F. Courbin, and P. Magain Galactic Center. (c) NASA,CXC,MIT, F.Baganoff+

  3. Unification? NLR BLR Torus BH Accretion Disk Geometrical Unification of Active Galactic Nuclei (AGN) Low obscuration Broad Lines (10 000 km/s)+Narrow Lines (100 km/s) Type 1 Type 2 Obscuration (NH >1022 cm-2) Narrow Lines (100 km/s) Composed illustration. Originals (c) NASA/CXC/M.Weiss, K..Meisenheimer

  4. Unification parameter 2? Lbol/LEdd ~0.1 (BL AGN) Lbol/LEdd ~10-2.5 (no BLR) UV signature of SS disk “Big Blue Bump” High Accretion rate Thin disk BBB Broad lines Radio quietness QSOs Seyferts NLSy1s Advection Dominated / Radiatively Inefficient Accretion Flow Low Accretion rate Thick disk (ADAF/RIAF) No BBB No Broad lines Radio loudness FR I sources LINERs LLAGNs Trump + 2011. see also Nicastro 200, Elitzur &Ho 2009

  5. IRAS 01072+4954 in brief Low-luminosity AGN (LLAGN) Starburst galaxy: ~5 Msun/yr Pseudo-bulge <--Secular evolution Unobscured Sy2: LX(2-10keV)= 1041.5 erg/s NH < 4.0 x 1020 cm-2 Low-mass black hole: MBH ~ 105Msun High accretion rate: Lbol~1042.5erg/s, m~0.2 FWHMbroad lines~500 km/s LBT/LUCI. Infrared: K-band. Courtesy: J. Zuther IRAS 01072+4954 No Broad lines in optical, no FeII GEMINI/NIFS 3’’x3’’ Field-Of-View

  6. Unification parameter 2? Lbol/LEdd ~0.1 (BL AGN) Lbol/LEdd ~10-2.5 (no BLR) High Accretion rate Thin disk BBB Broad lines Radio quietness QSOs Seyferts NLSy1s Low Accretion rate Thick disk (ADAF/RIAF) No BBB No Broad lines Radio loudness FR I sources LINERs LLAGNs Trump + 2011. see also Nicastro 200, Elitzur &Ho 2009

  7. Brγλ 2.164 μm F(Brγ) = 1.0 x 10-16 erg s-1 cm-2 FWHM(Brγ) = 420 km/s S/N~2.8 IRAS 01072+4954 BH Accretion: Lbol/LEdd~0.2 M ~ 4.4 x 10-4 Msun/yr Broad Line Region: rBLR ~ 1 light-day ≈ 105 RS F(Hα) = (1.7 - 4.8) x 10-14 erg s-1 cm-2 FWHM(Hα) = 430 – 600 km/s F(Brγ) ≈ F(Hα) / 100

  8. Unification parameter 2? Lbol/LEdd ~0.1 (BL AGN) Lbol/LEdd ~10-2.5 (no BLR) BL AGN Stern & Laor 2012 LINER 1s Trump + 2011. see also Nicastro 200, Elitzur &Ho 2009 Younes+ 2012

  9. Unification parameter 3? Sy1 Sy2 Singh+,2011 TrueSy2 candidates Laor,2003 IMBH & NLSy1 Dewegan+,2008 Low Mass Sy2 Carol+,2009 LEdd

  10. Unification parameter 3? Sy1 Sy2 Singh+,2011 TrueSy2 candidates Laor,2003 IMBH & NLSy1 Dewegan+,2008 Low Mass Sy2 Carol+,2009 IRAS01072

  11. Unification parameter 3? Radio Loud NLSy1 Foschini (2013)

  12. Unification parameter 3? Radio Loud NLSy1 Foschini (2013) Jet (radio) vs. disk luminosity in BHs Foschini (2012) IRAS01072

  13. Why are IMBHs important?

  14. Why to study IMBHs? IMBHs are the connection between SMBHs and stellar BHs

  15. Why to study IMBHs? IMBHs are the connection between SMBHs and stellar BHs IMBHs are fundamental to probe models of SMBH seeds Greene 2012

  16. Why to study IMBHs? IMBHs are the connection between SMBHs and stellar BHs IMBHs are fundamental to probe models of SMBH seeds IMBHs are the most active population of BHs in the local universe (dowinsizing) IMBHs seem to be in an early stage of evolution, therefore they can help on understanding how BHs grow

  17. Why to study IMBHs? IMBHs are the connection between SMBHs and stellar BHs IMBHs are fundamental to probe models of SMBH seeds IMBHs are the most active population of BHs in the local universe (dowinsizing) IMBHs seem to be in an early stage of evolution, therefore they can help on understanding how BHs grow IMBHs seem to reside in young galaxies (starbursts), therefore they are important to recognize the nature of the star formation – AGN relation IMBHs seem to prefer spiral galaxies with bars or pseudobulges, therefore they might probe a different type of BH fueling IMBHs show signatures that might allow to probe the metal enrichment of the BLR in AGNs

  18. How many IMBHs have been detected? Extracted from: Hubble Ultra Deep Field. (c) NASA/ESA/S. Beckwith(STScI) and The HUDF Team.

  19. Population census From optical observations SDSS DR7 Stern & Laor 2011: 106<MBH<109.5 10-3<Lbol/LEdd<1 SDSS DR4 Dong+2012: 8x104<MBH<2x106  3% are LINER 1 3% host an AGN 3% host an AGN

  20. Population census From optical observations SDSS DR7 Stern & Laor 2011: 106<MBH<109.5 10-3<Lbol/LEdd<1 SDSS DR4 Dong+2012: 8x104<MBH<2x106  3% are LINER 1 3% host an AGN 3% host an AGN From X-rays: Desroches & Ho 2009, Ghosh+ 2008 M*,gal<1010Msun20% - 25 % Lx >2.3x1038 erg/s

  21. Population census From optical observations From multiwavelength campaigns Foschini 2011: From 76 NLSy1  46 radio loud  30 radio quiet From 49 RLNLSy1  12 γ-emitters SDSS DR7 Stern & Laor 2011: 106<MBH<109.5 10-3<Lbol/LEdd<1 SDSS DR4 Dong+2012: 8x104<MBH<2x106  3% are LINER 1 3% host an AGN 3% host an AGN From X-rays: ~ 310 low-mass BH (z<0.35) Desroches & Ho 2009, Ghosh+ 2008 M*,gal<1010Msun20% - 25 % Lx >2.3x1038 erg/s

  22. How to find more IMBHs?

  23. How to find more? From optical observations Problems: - Obscuration - Dilution of the AGN by the stellar continuum LAGN,B Lbol/LEdd (M*,gal / Lgal,B) B Lhost,B 0.1 (Msun/Lsun) T B/T : ratio stellar mass of the bulge to total stellar mass = NGC 4395. (c) Cord Scholz LAGN/Lhost (Sa) ~ 45 LAGN/Lhost (Sc) ~ 7 For maximal accreting BHs:

  24. How to find more? MBH M*,bulge ~ 0.001 LAGN Lhost α MBH From optical observations Problems: - Obscuration - Dilution of the AGN by the stellar continuum LAGN,B Lbol/LEdd (M*,gal / Lgal,B) B Lhost,B 0.1 (Msun/Lsun) T B/T : ratio stellar mass of the bulge to total stellar mass =

  25. How to find more? MBH – M*,bulgerelation log (MBH) = -1.0 (MK + 22.5) + 7.55 Valencia-S+ 2012 IRAS 01072 Graham+2012 IRAS 01072

  26. How to find more? MBH – LK,bulgerelation log (MBH) = -1.0 (MK + 22.5) + 7.55 Valencia-S+ (Jun.) 2012 IRAS 01072 log (MBH) = -1.09 (MK + 22.5) + 7.39 Graham & Scott (Dec.) 2012

  27. How to find more? MBH M*,bulge MBH M*,bulge ~ 0.001 ~ 10-5 – 10-4 From optical observations Problems: - Obscuration - Dilution of the AGN by the stellar continuum LAGN,B Lbol/LEdd (M*,gal / Lgal,B) B Lhost,B 0.1 (Msun/Lsun) T = For MBH > 7x107 Msun: For IMBHs with 105 Msun < MBH < 106 Msun:

  28. How to find more? From X-ray observations A max. accreting BH with MBH=105 Msun: LEdd = 1043 erg/s  LX(2-10kev) ~ 1042 erg/s

  29. How to find more? From X-ray observations A max. accreting BH with MBH=105 Msun: Like IRAS 01072 (z=0.0236): MBH~105 Msun Lbol/LEdd ~ 0.2 FX(2-10keV)=3.1 x 10-13 erg s-1 cm-2 Chandra (~ 25 ks) LEdd = 1043 erg/s  LX(2-10kev) ~ 1042 erg/s Sensitivity limit Chandra (2-10keV): FX~ 10-15 erg s-1 cm-2 (~ 20ks)  not detectable z > 0.2

  30. How to find more? From X-ray observations A max. accreting BH with MBH=105 Msun: Like IRAS 01072 (z=0.0236): MBH~105 Msun Lbol/LEdd ~ 0.2 FX(2-10keV)=3.1 x 10-13 erg s-1 cm-2 Chandra (~ 25 ks) LEdd = 1043 erg/s  LX(2-10kev) ~ 1042 erg/s Sensitivity limit Chandra (2-10keV): FX~ 10-15 erg s-1 cm-2 (~ 20ks)  not detectable z > 0.2 IMBHs: 105 Msun < MBH < 106 Msun Dong+2013 42/49 detections (S/N>3) z < 0.08 (D < 350 Mpc) FX(2-10keV) > 10-14 erg s-1 cm-2

  31. How to find more? LX(AGN)min ~ 1040 erg/s Artist impression. (c)ESO/ L.Casada From X-ray observations Stellar BH with MBH~ 10 Msun: LEdd = 1039 erg/s  LX(2-10kev) ~ 1038 erg/s Threshold on the Eddington ratio of IMBHs: For MBH = 105 Msun Lbol/LEdd ~ 0.001

  32. There is still some hope From Infrared observations Volume-weighted space density of active SMBH in the local Universe Goulding+ 2010

  33. Thanks!

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