249 research outputs found
A Tidal Disruption Flare in Abell 1689 from an Archival X-ray Survey of Galaxy Clusters
Theory suggests that a star making a close passage by a supermassive black
hole at the center of a galaxy can under most circumstances be expected to emit
a giant flare of radiation as it is disrupted and a portion of the resulting
stream of shock-heated stellar debris falls back onto the black hole itself. We
examine the first results of an ongoing archival survey of galaxy clusters
using Chandra and XMM-selected data, and report a likely tidal disruption flare
from SDSS J131122.15-012345.6 in Abell 1689. The flare is observed to vary by a
factor of >30 over at least 2 years, to have maximum L_X(0.3-3.0 keV)> 5 x
10^{42} erg s^{-1} and to emit as a blackbody with kT~0.12 keV. From the galaxy
population as determined by existing studies of the cluster, we estimate a
tidal disruption rate of 1.2 x 10^{-4} galaxy^{-1} year^{-1} if we assume a
contribution to the observable rate from galaxies whose range of luminosities
corresponds to a central black hole mass (M_bh) between 10^6 and 10^8 M_sun.Comment: 24 pages, including 6 figures and 2 tables Accepted for publication
in the Astrophysical Journa
Spectral Models for Low-luminosity Active Galactic Nuclei in LINERs: The Role of Advection-dominated Accretion and Jets
We perform an exploratory study of the physical properties of accretion flows
and jets in low-luminosity active galactic nuclei (LLAGNs) by modeling the
spectral energy distributions (SEDs) of 12 LLAGNs in low-ionization nuclear
emission-line regions (LINERs). These SEDs we constructed from high-resolution
radio, X-ray and optical/UV observations of the immediate vicinity of the black
hole. We adopt a coupled accretion-jet model comprising an inner
advection-dominated accretion flow (ADAF) and an outer standard thin disk. We
present best-fit models in which either the ADAF or the jet dominate the X-ray
emission. Six sources in our sample display an optical-UV excess with respect
to ADAF and jet models; this excess can be explained as emission from the
truncated disk with transition radii 30-225 Rs in four of them. In almost all
sources the optical emission can also be attributed to unresolved, old stellar
clusters with masses ~1E7-1E8 Msun. We find evidence for a correlation between
the accretion rate and jet power and an anti-correlation between the
radio-loudness and the accretion rate. We confirm previous findings that the
radio emission is severely underpredicted by ADAF models and explained by the
relativistic jet. We find evidence for a nonlinear relation between the X-ray
and bolometric luminosities and a slight IR excess in the average model SED
compared to that of quasars. We suggest that the hardness of the X-ray spectrum
can be used to identify the X-ray emission mechanism and discuss directions for
progress in understanding the origin of the X-rays.Comment: Accepted for publication in MNRAS. 27 pages, 22 figures. arXiv admin
note: substantial text overlap with arXiv:1112.464
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