2019ApJ...883..111H


Query : 2019ApJ...883..111H

2019ApJ...883..111H - Astrophys. J., 883, 111-111 (2019/October-1)

Discovery and early evolution of ASASSN-19bt, the first TDE detected by TESS.

HOLOIEN T.W.-S., VALLELY P.J., AUCHETTL K., STANEK K.Z., KOCHANEK C.S., FRENCH K.D., PRIETO J.L., SHAPPEE B.J., BROWN J.S., FAUSNAUGH M.M., DONG S., THOMPSON T.A., BOSE S., NEUSTADT J.M.M., CACELLA P., BRIMACOMBE J., KENDURKAR M.R., BEATON R.L., BOUTSIA K., CHOMIUK L., CONNOR T., MORRELL N., NEWMAN A.B., RUDIE G.C., SHISHKOVKSY L. and STRADER J.

Abstract (from CDS):

We present the discovery and early evolution of ASASSN-19bt, a tidal disruption event (TDE) discovered by the All-Sky Automated Survey for Supernovae (ASAS-SN) at a distance of d ≃ 115 Mpc and the first TDE to be detected by TESS. As the TDE is located in the TESS Continuous Viewing Zone, our data set includes 30 minute cadence observations starting on 2018 July 25, and we precisely measure that the TDE begins to brighten ∼8.3 days before its discovery. Our data set also includes 18 epochs of Swift UVOT and XRT observations, 2 epochs of XMM-Newton observations, 13 spectroscopic observations, and ground data from the Las Cumbres Observatory telescope network, spanning from 32 days before peak through 37 days after peak. ASASSN-19bt thus has the most detailed pre-peak data set for any TDE. The TESS light curve indicates that the transient began to brighten on 2019 January 21.6 and that for the first 15 days, its rise was consistent with a flux ∝t2 power-law model. The optical/UV emission is well fit by a blackbody spectral energy distribution, and ASASSN-19bt exhibits an early spike in its luminosity and temperature roughly 32 rest-frame days before peak and spanning up to 14 days, which has not been seen in other TDEs, possibly because UV observations were not triggered early enough to detect it. It peaked on 2019 March 4.9 at a luminosity of L ≃ 1.3 x 1044 erg s–1 and radiated E ≃ 3.2 x 1050 erg during the 41 day rise to peak. X-ray observations after peak indicate a softening of the hard X-ray emission prior to peak, reminiscent of the hard/soft states in X-ray binaries.

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

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

VizieR on-line data: <Available at CDS (J/ApJ/883/111): table2.dat>

Simbad objects: 15

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Number of rows : 15
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 AT 2016fnl ev 00 29 57.050 +32 53 37.27           ~ 104 0
2 NAME SEP reg 06 00 00.000 -66 33 38.55           ~ 173 0
3 LEDA 307968 Sy2 07 00 11.3999000016 -66 02 24.822544596   16.99   15.63   ~ 7 0
4 AT 2019ahk ev 07 00 11.410 -66 02 25.16           ~ 35 0
5 2MASS J07003124-6610452 BLL 07 00 31.2536435688 -66 10 45.229749384 16.38 15.99 15.89     ~ 76 3
6 ATLAS 18nej ev 07 56 54.537 +34 15 43.61           ~ 63 0
7 SN 2018oh SN* 09 06 39.6 +19 20 18           SNIa-norm 74 0
8 ASASSN -14ae SN* 11 08 40.11 +34 05 52.4           ~ 104 0
9 LEDA 43234 AG? 12 48 15.2253025968 +17 46 26.475426228   16.5       ~ 264 0
10 AT 2018dyb ev 16 10 58.774 -60 55 23.16           ~ 44 0
11 GRB 110328A gB 16 44 49 +57 34.9           ~ 450 0
12 iPTF 16axa ev 17 03 34.36 +30 35 36.8           ~ 42 0
13 ASASSN -15oi SN* 20 39 09.096 -30 45 20.71           ~ 129 0
14 SWIFT J2058.4+0516 X 20 58 19.898 +05 13 32.25           ~ 137 0
15 AT 2018fyk ev 22 50 16.10 -44 51 53.5           ~ 66 0

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