CaltechAUTHORS
Published February 2022 | Version Submitted + Published
Journal Article Open

Why do black holes trace bulges (& central surface densities), instead of galaxies as a whole?

Creators

  • 1. ROR icon California Institute of Technology
  • 2. ROR icon Northwestern University
  • 3. ROR icon University of Connecticut

Abstract

Previous studies of fueling black holes in galactic nuclei have argued (on scales ∼0.01−1000pc) accretion is dynamical with inflow rates M˙∼ηM_(gas)/t_(dyn) in terms of gas mass M_(gas), dynamical time t_(dyn), and some η. But these models generally neglected expulsion of gas by stellar feedback, or considered extremely high densities where expulsion is inefficient. Studies of star formation, however, have shown on sub-kpc scales the expulsion efficiency f_(wind) = M_(ejected)/M_(total) scales with the gravitational acceleration as (1−f_(wind))/f_(wind)∼a¯_(grav)/⟨p˙/m∗⟩∼Σ_(eff)/Σ_(crit) where a¯_(grav) ≡ GM_(tot)(

Additional Information

© 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2021 No v ember 25. Received 2021 October 26; in original form 2021 March 15. Published: 29 November 2021. We thank Jessie Christiansen, Michael Fall, Peter Mitchell, Guang Yang, and our anonymous referee for a number of helpful suggestions and insightful comments. Support for PFH was provided by NSF Research Grants 1911233 & 20009234, NSF CAREER grant 1455342, NASA grants 80NSSC18K0562, HST-AR-15800.001-A. SW is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST2001905. CAFG was supported by NSF through grants AST-1715216 and CAREER award AST-1652522; by NASA through grant 17-ATP17-0067; by STScI through grant HST-AR-16124.001-A; and by the Research Corporation for Science Advancement through a Cottrell Scholar Award and a Scialog Award. Numerical calculations were run on the Caltech compute cluster 'Wheeler,' allocations FTA-Hopkins supported by the NSF and TACC, and NASA HEC SMD-16-7592. Data Availability Statement: The data supporting the plots within this article are available on reasonable request to the corresponding author. A public version of the GIZMO code is available at http://www.tapir.caltech.edu/~phopkins/Site/GIZMO.html.

Attached Files

Published - stab3458.pdf

Submitted - 2103.10444.pdf

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2103.10444.pdf

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Additional details

Identifiers

Eprint ID
108528
Resolver ID
CaltechAUTHORS:20210323-124505549

Related works

Describes
https://arxiv.org/abs/2103.10444 (URL)
http://www.tapir.caltech.edu/~phopkins/Site/GIZMO.html (URL)

Funding

NSF
AST-1911233
NSF
20009234
NSF
AST-1455342
NASA
80NSSC18K0562
NASA
HST-AR-15800.001-A
NSF
AST-2001905
NSF
AST-1715216
NSF
AST-1652522
NASA
17-ATP17-0067
NASA
HST-AR-16124.001-A
Cottrell Scholar of Research Corporation
Scialog Fellow of Research Corporation
NASA
SMD-16-7592

Dates

Created
2021-03-23
Created from EPrint's datestamp field
Updated
2022-01-24
Created from EPrint's last_modified field

Caltech Custom Metadata

Caltech groups
Astronomy Department , TAPIR