A Dependence of the Tidal Disruption Event Rate on Global Stellar Surface Mass Density and Stellar Velocity Dispersion

被引:77
作者
Graur, Or [1 ,2 ]
French, K. Decker [3 ,4 ]
Zahid, H. Jabran [1 ]
Guillochon, James [1 ]
Mandel, Kaisey S. [1 ,5 ,6 ,7 ]
Auchettl, Katie [8 ,9 ]
Zabludoff, Ann I. [3 ]
机构
[1] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA
[2] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA
[3] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA
[4] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA
[5] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England
[6] Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England
[7] Univ Cambridge, Stat Lab, DPMMS, Wilberforce Rd, Cambridge CB3 0WB, England
[8] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA
[9] Ohio State Univ, Dept Phys, 191 W Woodruff Ave, Columbus, OH 43210 USA
基金
美国国家科学基金会; 美国国家航空航天局;
关键词
black hole physics; galaxies: evolution; galaxies: nuclei; DIGITAL SKY SURVEY; X-RAY OUTBURST; ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; HIGH-Z GALAXIES; E+A GALAXIES; FOLLOW-UP; LUMINOSITY FUNCTIONS; QUIESCENT GALAXIES; NEARBY GALAXIES;
D O I
10.3847/1538-4357/aaa3fd
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The rate of tidal disruption events (TDEs), R-TDE, is predicted to depend on stellar conditions near the super-massive black hole (SMBH), which are on difficult-to-measure sub-parsec scales. We test whether R-TDE depends on kpc-scale global galaxy properties, which are observable. We concentrate on stellar surface mass density, Sigma M-*, and velocity dispersion, sigma(nu), which correlate with the stellar density and velocity dispersion of the stars around the SMBH. We consider 35 TDE candidates, with and without known X-ray emission. The hosts range from star-forming to quiescent to quiescent with strong Balmer absorption lines. The last (often with post-starburst spectra) are overrepresented in our sample by a factor of 35(-17)(+21) or 18(-7)(+8), depending on the strength of the H delta absorption line. For a subsample of hosts with homogeneous measurements, Sigma M-* = 10(9)-10(10) M-circle dot/kpc(2), higher on average than for a volume-weighted control sample of Sloan Digital Sky Survey galaxies with similar redshifts and stellar masses. This is because (1) most of the TDE hosts here are quiescent galaxies, which tend to have higher Sigma M-* than the star-forming galaxies that dominate the control, and (2) the star-forming hosts have higher average Sigma M-* than the star-forming control. There is also a weak suggestion that TDE hosts have lower sigma(nu) than for the quiescent control. Assuming that R-TDE infinity Sigma M-*(alpha) x sigma(beta)(nu), and applying a statistical model to the TDE hosts and control sample, we estimate (alpha) over cap = 0.9 +/- 0.2 and (beta) over cap = -1.0 +/- 0.6. This is broadly consistent with RTDE being tied to the dynamical relaxation of stars surrounding the SMBH.
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页数:19
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