2020ApJ...898..161H


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.09CEST05:40:43

2020ApJ...898..161H - Astrophys. J., 898, 161-161 (2020/August-1)

The rise and fall of ASASSN-18pg: following a TDE from early to late times.

HOLOIEN T.W.-S., AUCHETTL K., TUCKER M.A., SHAPPEE B.J., PATEL S.G., MILLER-JONES J.C.A., MOCKLER B., GROENEWALD D.N., HINKLE J.T., BROWN J.S., KOCHANEK C.S., STANEK K.Z., CHEN P., DONG S., PRIETO J.L., THOMPSON T.A., BEATON R.L., CONNOR T., COWPERTHWAITE P.S., DAHMEN L., FRENCH K.D., MORRELL N., BUCKLEY D.A.H., GROMADZKI M., ROY R., COULTER D.A., DIMITRIADIS G., FOLEY R.J., KILPATRICK C.D., PIRO A.L., ROJAS-BRAVO C., SIEBERT M.R. and VAN VELZEN S.

Abstract (from CDS):

We present nearly 500 days of observations of the tidal disruption event (TDE) ASASSN-18pg, spanning from 54 days before peak light to 441 days after peak light. Our data set includes X-ray, UV, and optical photometry, optical spectroscopy, radio observations, and the first published spectropolarimetric observations of a TDE. ASASSN-18pg was discovered on 2018 July 11 by the All-Sky Automated Survey for Supernovae (ASAS-SN) at a distance of d = 78.6 Mpc; with a peak UV magnitude of m ≃ 14, it is both one of the nearest and brightest TDEs discovered to-date. The photometric data allow us to track both the rise to peak and the long-term evolution of the TDE. ASASSN-18pg peaked at a luminosity of L ≃ 2.4 x 1044 erg s–1, and its late-time evolution is shallower than a flux ∝t–5/3 power-law model, similar to what has been seen in other TDEs. ASASSN-18pg exhibited Balmer lines and spectroscopic features consistent with Bowen fluorescence prior to peak, which remained detectable for roughly 225 days after peak. Analysis of the two-component Hα profile indicates that, if they are the result of reprocessing of emission from the accretion disk, the different spectroscopic lines may be coming from regions between ∼10 and ∼60 lt-days from the black hole. No X-ray emission is detected from the TDE, and there is no evidence of a jet or strong outflow detected in the radio. Our spectropolarimetric observations indicate that the projected emission region is likely not significantly aspherical, with the projected emission region having an axis ratio of >=0.65.

Abstract Copyright: © 2020. The American Astronomical Society. All rights reserved.

Journal keyword(s): Black holes - Accretion - Galaxy accretion disks - Black hole physics - Supermassive black holes - Tidal disruption

Status at CDS : Large table(s) will be appraised for possible ingestion in VizieR.

Simbad objects: 11

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Number of rows : 11

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 NAME AT 2019ahk ev 07 00 11.410 -66 02 25.16           ~ 18 0
3 NAME ATLAS 18nej ev 07 56 54.537 +34 15 43.61           ~ 34 0
4 ASASSN -19dj SN* 08 13 16.937 +22 38 53.80           ~ 19 0
5 ASASSN -14ae SN* 11 08 40.11 +34 05 52.4           ~ 75 0
6 LEDA 43234 G 12 48 15.2244073438 +17 46 26.496619532   16.5       ~ 163 0
7 NAME AT 2018dyb ev 16 10 58.774 -60 55 23.16           ~ 22 0
8 2MASX J16105891-6055250 G 16 10 58.920 -60 55 25.07           ~ 6 0
9 iPTF 16axa ev 17 03 34.36 +30 35 36.8           ~ 30 0
10 ICRF J193925.0-634245 Sy2 19 39 25.02671 -63 42 45.6255   18.87 18.37 17.64   ~ 1010 1
11 ASASSN -15oi SN* 20 39 09.096 -30 45 20.71           ~ 68 0

    Equat.    Gal    SGal    Ecl

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2021.05.09-05:40:43

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