2019ApJ...880..120H


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.09CEST05:47:45

2019ApJ...880..120H - Astrophys. J., 880, 120-120 (2019/August-1)

PS18kh: a new tidal disruption event with a non-axisymmetric accretion disk.

HOLOIEN T.W.-S., HUBER M.E., SHAPPEE B.J., ERACLEOUS M., AUCHETTL K., BROWN J.S., TUCKER M.A., CHAMBERS K.C., KOCHANEK C.S., STANEK K.Z., REST A., BERSIER D., POST R.S., ALDERING G., PONDER K.A., SIMON J.D., KANKARE E., DONG D., HALLINAN G., REDDY N.A., SANDERS R.L., TOPPING M.W. (The Pan-STARRS), BULGER J., LOWE T.B., MAGNIER E.A., SCHULTZ A.S.B., WATERS C.Z., WILLMAN M., WRIGHT D., YOUNG D.R. (The ASAS-SN), DONG S., PRIETO J.L., THOMPSON T.A. (The ATLAS), DENNEAU L., FLEWELLING H., HEINZE A.N., SMARTT S.J., SMITH K.W., STALDER B., TONRY J.L. and WEILAND H.

Abstract (from CDS):

We present the discovery of PS18kh, a tidal disruption event discovered at the center of SDSS J075654.53+341543.6 (d ≃ 322 Mpc) by the Pan-STARRS Survey for Transients. Our data set includes pre-discovery survey data from Pan-STARRS, the All-sky Automated Survey for Supernovae, and the Asteroid Terrestrial-impact Last Alert System as well as high-cadence, multiwavelength follow-up data from ground-based telescopes and Swift, spanning from 56 days before peak light until 75 days after. The optical/UV emission from PS18kh is well-fit as a blackbody with temperatures ranging from T ≃ 12,000 K to T ≃ 25,000 K and it peaked at a luminosity of L ≃ 8.8 x 1043 erg s–1. PS18kh radiated E = (3.45 ± 0.22) x 1050 erg over the period of observation, with (1.42 ± 0.20) x 1050 erg being released during the rise to peak. Spectra of PS18kh show a changing, boxy/double-peaked Hα emission feature, which becomes more prominent over time. We use models of non-axisymmetric accretion disks to describe the profile of the Hα line and its evolution. We find that at early times the high accretion rate leads the disk to emit a wind which modifies the shape of the line profile and makes it bell-shaped. At late times, the wind becomes optically thin, allowing the non-axisymmetric perturbations to show up in the line profile. The line-emitting portion of the disk extends from rin ∼ 60rg to an outer radius of rout ∼ 1400rg and the perturbations can be represented either as an eccentricity in the outer rings of the disk or as a spiral arm in the inner disk.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): accretion, accretion disks - black hole physics - galaxies: nuclei

Status at CDS : Associated data (images, light curves, etc...) being ingested in VizieR.

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME AT 2016fnl ev 00 29 57.04 +32 53 37.5           ~ 58 0
2 SN 2013hx SN* 01 35 33.28 -57 57 50.6           SNIc 14 1
3 NAME ATLAS 18nej ev 07 56 54.537 +34 15 43.61           ~ 34 0
4 SDSS J075654.53+341543.6 G 07 56 54.53880 +34 15 43.6392           ~ 3 0
5 ASASSN -14ae SN* 11 08 40.11 +34 05 52.4           ~ 75 0
6 NAME PS 15br SN* 11 25 19.23 +08 14 18.5           SNSL 10 0
7 SN 2008es SN* 11 56 49.13 +54 27 25.7           SNIIL 104 1
8 LEDA 43234 G 12 48 15.2244073438 +17 46 26.496619532   16.5       ~ 163 0
9 PSN K0905-001 SN? 14 57 03.10 +49 36 40.8           ~ 56 0
10 PS1-10jh ev 16 09 28.296 +53 40 23.52           ~ 109 0
11 PTF 09djl SN* 16 33 55.94 +30 14 16.3           SNII 47 0
12 iPTF 16axa ev 17 03 34.36 +30 35 36.8           ~ 30 0
13 ASASSN -15oi SN* 20 39 09.096 -30 45 20.71           ~ 68 0
14 SN 2015L ? 22 02 15.45 -61 39 34.6           ~ 117 2

    Equat.    Gal    SGal    Ecl

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2021.05.09-05:47:45

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