Constraints on Broad Line Quasar Black Hole Masses, Eddington Ratios, and Lifetimes Brandon C. Kelly (CfA) Marianne Vestergaard (DARK, Denmark), Xiaohui Fan (Arizona), Philip Hopkins (Berkeley), Lars Hernquist (CfA), & Aneta Siemiginowska (CfA) 3/10/10 Brandon Kelly, [email protected]
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Constraints on Broad Line Quasar Black Hole Masses, Eddington Ratios, and Lifetimes
Constraints on Broad Line Quasar Black Hole Masses, Eddington Ratios, and Lifetimes. Brandon C. Kelly (CfA) Marianne Vestergaard (DARK, Denmark), Xiaohui Fan (Arizona), Philip Hopkins (Berkeley), Lars Hernquist (CfA), & Aneta Siemiginowska (CfA). Black Hole Growth and Galaxy Evolution. - PowerPoint PPT Presentation
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Constraints on Broad Line Quasar Black Hole Masses, Eddington
Ratios, and Lifetimes
Brandon C. Kelly (CfA)
Marianne Vestergaard (DARK, Denmark), Xiaohui Fan (Arizona), Philip Hopkins (Berkeley), Lars Hernquist
• Tight correlation between MBH and host galaxy bulge properties implies that supermassive black holes (SMBH) and galaxy evolution is linked (e.g., Merritt & Ferrarese 2001, Tremaine et al. 2002)
• Can be explained if black hole growth is self-regulated (e.g., Wyithe & Loeb 2003, Di Matteo et al. 2005)
• If growth is SR, then broad line phase for bright quasars occurs at end of growth
Black Solid: Our Estimated BHMFsGreen Solid: Best-fit BHMFDashed Black : Local BHMF for all SMBHs (Merloni & Heinz 2008)Red Solid: BHMF from Vestergaard et al.(2008)
• If SMBH growth is self-regulated, this should be representative of the most massive SMBH
• Consistent with maximum mass seen in cosmological simulations (Sijacki et al. 2009) and that expected from self-regulation arguments (Natarajan & Treister 2009)
• If SMBH growth is self-regulated, this should be representative of the most massive SMBH
• Consistent with maximum mass seen in cosmological simulations (Sijacki et al. 2009) and that expected from self-regulation arguments (Natarajan & Treister 2009)
Sijacki et all (2009)
Summary• First work to rigorously and self-consistently correct
for statistical uncertainty and incompleteness in the broad line quasar mass function
• BLQSO BHMF qualitatively in agreement with cosmological model of self-regulated black hole growth
• Most BL quasars are not accreting at or near L / Ledd
• SMBHs cannot experience all of their growth in a BL phase
• Maximum SMBH mass is ~ 1010 – 1011 MSUN
• Uncertainty in mass estimates may be ~ 0.2 dex, or correlated with luminosity
Standard value of 0.4 dex implies a mass estimate distribution that is too broad, implies:
- Statistical error is correlated with luminosity? (Shen & Kelly 2010)- Uncorrected radiation pressure? (Marconi et al. 2008)- Broad line mass estimates are meaningless at this L and z?
Standard value of 0.4 dex implies a mass estimate distribution that is too broad, implies:
- Statistical error is correlated with luminosity? (Shen & Kelly 2010)- Uncorrected radiation pressure? (Marconi et al. 2008)- Broad line mass estimates are meaningless at this L and z?
Future workFuture work
• Incorporate more flexible L / Ledd distribution• Investigate if error in mass estimates is correlated
with luminosity, and include in application to DR7 data set (Shen & Kelly, in prep)
• Apply technique to COSMOS and other multiwavelength data sets to better determine Eddington ratio distribution and BHMF (Kelly & Trump, et al.)
• Reverberation mapping of higher z and L sources to better determine uncertainties (Elvis and Trump, et al.)