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The Black Hole Mass Function Derived from Local Spiral Galaxies

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The Black Hole Mass Function Derived from Local Spiral Galaxies PUBLISHED IN THE ASTROPHYSICAL JOURNAL, 789:124 (16PP),2014 JULY 10 Preprint typeset using LATEX style emulateapj v. 12/16/11 THE BLACK HOLE MASS FUNCTION DERIVED FROM LOCAL SPIRAL GALAXIES BENJAMIN L. DAVIS1 , JOEL C. BERRIER1,2,5,LUCAS JOHNS3,6 ,DOUGLAS W. SHIELDS1,2, MATTHEW T. HARTLEY2,DANIEL KENNEFICK1,2, JULIA KENNEFICK1,2, MARC S. SEIGAR1,4 , AND CLAUD H.S. LACY1,2 Published in The Astrophysical Journal, 789:124 (16pp), 2014 July 10 ABSTRACT We present our determination of the nuclear supermassive black hole mass (SMBH) function for spiral galax- ies in the local universe, established from a volume-limited sample consisting of a statistically complete col- lection of the brightest spiral galaxies in the southern (δ< 0◦) hemisphere. Our SMBH mass function agrees well at the high-mass end with previous values given in the literature. At the low-mass end, inconsistencies exist in previous works that still need to be resolved, but our work is more in line with expectations based on modeling of black hole evolution. This low-mass end of the spectrum is critical to our understanding of the mass function and evolution of black holes since the epoch of maximum quasar activity. A limiting luminos- ity (redshift-independent) distance, DL = 25.4 Mpc (z =0.00572) and a limiting absolute B-band magnitude, MB = −19.12 define the sample. These limits define a sample of 140 spiral galaxies, with 128 measurable pitch angles to establish the pitch angle distribution for this sample. This pitch angle distribution function may be useful in the study of the morphology of late-type galaxies. We then use an established relationship between the logarithmic spiral arm pitch angle and the mass of the central SMBH in a host galaxy in order to estimate the mass of the 128 respective SMBHs in this volume-limited sample. This result effectively gives us −1 the distribution of mass for SMBHs residing in spiral galaxies over a lookback time, tL 82.1 h67.77 Myr and 4 −3 3 ≤ contained within a comoving volume, VC =3.37 10 h67.77 Mpc . We estimate that the density of SMBHs × +6.55 4 3 −3 residing in spiral galaxies in the local universe is ρ =5.54−2.73 10 h67.77 M⊙ Mpc . Thus, our derived cos- Ω ×+5.14 −7 mological SMBH mass density for spiral galaxies is BH =4.35−2.15 10 h67.77. Assuming that black holes +0.023 3 h × Ω grow via baryonic accretion, we predict that 0.020−0.010 h67.77 of the universal baryonic inventory ( BH/ωb) is confined within nuclear SMBHs at the center of spiral galaxies. Subject headings: black hole physics — cosmology: miscellaneous — galaxies: evolution — galaxies: spiral 1. INTRODUCTION It is of particular interest to understand the low-mass end Strong evidence suggests that supermassive black holes of the BHMF in order to understand how the QLF of past (SMBHs) reside in the nuclei of most galaxies and that cor- epochs evolves into the BHMF of today (Shankar 2009). It relations exist between the mass of the SMBH and certain is now widely accepted that black holes in active galactic nu- properties of the host galaxy (Kormendy & Richstone 1995; clei (AGN) do not generally accrete at the Eddington limit Kormendy & Gebhardt 2001). It is therefore possible to con- (Shankar 2009). This is not a problem for the brightest and duct a census by studying the numerous observable galaxies most visible AGN, presumably powered by large black holes in our universe in order to estimate demographic informa- accreting at a considerable fraction of their Eddington limit. tion (i.e., mass) for the population of SMBHs in our universe. Smaller black holes cannot imitate this luminosity without ac- Following the discovery of quasars (Schmidt 1963) and the creting at super-Eddington rates. However, one cannot know early suspicion that their power sources were in fact SMBHs whether a relatively dim quasar contains a small black hole (Salpeter 1964; Lynden-Bell 1969), the study of quasar evo- accreting strongly or a larger black hole accreting at a rela- lution via quasar luminosity functions (QLFs) has resulted in tively low rate (a small fraction of its Eddington limit). It is notable successes in understanding the population of SMBHs therefore not easy to tell what the BHMF was for AGN in the arXiv:1405.5876v3 [astro-ph.GA] 16 Jan 2018 in the universe and their mass function. But, studies of the past, because it is non-trivial to count the number of lower- supermassive black hole mass function (BHMF) have left us mass black holes (those with masses in the range of less than with no clear consensus, especially at the low-mass end of the a million to ten million solar masses). However, if we counted spectrum. the number of local lower-mass black holes, the requirement that the BHMF from the quasar epochs evolve into the local 1 Arkansas Center for Space and Planetary Sciences, University of BHMF could significantly constrain the BHMF in the past, as Arkansas, 346 1/2 North Arkansas Avenue, Fayetteville, AR 72701, USA; well as determine a more complete local picture. Thus, one [email protected] should pay attention to late-type (spiral) galaxies, since a sig- 2 Department of Physics, University of Arkansas, 226 Physics Building, 835 West Dickson Street, Fayetteville, AR 72701, USA nificant fraction of these lower-mass black holes are found in 3 Department of Physics, Reed College, 3203 SE Woodstock Boulevard, such galaxies (our own Milky Way being an example). Portland, OR, 97202, USA Some indicators of SMBH mass such as the central stellar 4 Department of Physics and Astronomy, University of Arkansas at Little velocity dispersion (Gebhardt et al. 2000; Ferrarese & Merritt Rock, 2801 South University Avenue, Little Rock, AR 72204, USA 2000) or Sérsic index (Graham & Driver 2007) have been 5 Now at Department of Physics and Astronomy, Rutgers, The State Uni- versity of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854-8019, used to construct BHMFs for early-type galaxies (e.g., USA Grahametal. 2007). They have been used also to study 6 Now at Department of Physics, University of California, San Diego, La late-type galaxies, but not always with success because these Jolla, CA 92092, USA quantities are defined for the bulge component of galaxies, 2 Davis et al. measuring them in disk galaxies requires decomposition into theorem, i.e., separate components of the galactic bulge, disk, and bar. GMBulge σ2 , (2) Thus, we are currently handicapped in the study of the low- ≈ R mass end of the BHMF by the relative scarcity of infor- mation on the mass function of spiral galaxies. One ap- where G is the universal gravitational constant and R is the proach has been to use luminosity or other functions avail- radius of the bulge; and the nuclear SMBH mass is directly able for all galaxy types in a sample to produce a mass func- proportional to the velocity dispersion via the M–σ relation, tion based upon the relevant scaling relation (Salucci et al. i.e., M σα, (3) 1999; Aller & Richstone 2002; Shankar et al. 2004, 2009; ∝ Tundo et al. 2007). Our approach contrasts with this one by with α =4.8 0.5 (Ferrarese & Merritt 2000); it therefore fol- taking individual measurements of a quantity for each galaxy lows that the± mass (M) of the nuclear SMBH must be indi- individually in a carefully selected and complete local sample. rectly proportional to the pitch angle of its host galaxy’s spiral Recently, it has been shown that there is a strong correla- arms, i.e., − tion between SMBH mass and spiral arm pitch angle in disk M 10 (0.062±0.009)|P|, (4) galaxies (Seigar et al. 2008; Berrier et al. 2013). This corre- ∝ lation presents a number of potential advantages for the pur- as shown in Equation (6). poses of developing the BHMF at lower masses. First, there is Admittedly, galaxies are complex structures. However, evidence that it has lower scatter when applied to disk galax- a number of measurable features of disk galaxies are now ies than any of the other correlations that have been presented known to correlate with each other, even though they are mea- (Berrier et al. 2013). Second, the pitch angle is less prob- sured on very different length scales (e.g., σ, bulge luminos- lematically measured in disk galaxies than the other features, ity, Sérsic Index, and spiral arm pitch angle). Each of these which is likely the explanation for the lower scatter. It does quantities is influenced, or even determined, by the mass of not require any decomposition of the bulge, disk, or bar com- the central bulge of the disk galaxy, and this quantity in turn ponents besides a trivial exclusion of the central region of the seems to correlate quite well with the mass of the central black galaxy before the analysis (described below in §2.1). Finally, hole. The precise details of how this nexus of what we might it can be derived from imaging data alone, which is already call “traits” of the host galaxy correlate to the black hole mass available in high quality for many nearby galaxies. is still subject to debate (see for instance Läsker et al. (2014), It may be objected that the spiral arm structure of a disk which shows that central black hole may correlate equally galaxy spans tens of thousands of light years, many orders of well with total galaxy luminosity as with central bulge lumi- magnitude greater than the scale (some few light years) over nosity).
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