2024A&A...692A.262S


Query : 2024A&A...692A.262S

2024A&A...692A.262S - Astronomy and Astrophysics, volume 692A262 (2024/12-1)

Recurring tidal disruption events a decade apart in IRAS F01004-2237.

SUN L., JIANG N., DOU L., SHU X., ZHU J., DONG S., BUCKLEY D., CENKO S.B., FAN X., GROMADZKI M., LIU Z., WANG J., WANG T., WANG Y., WU T., YANG L., ZHANG F., ZHANG W. and ZHANG X.

Abstract (from CDS):

Context. In theory, recurring tidal disruption events (TDEs) may occur when a close stellar binary encounters a supermassive black hole, if one star is captured and undergoes repeating partial TDEs, or if both stars are tidally disrupted (double TDEs). In addition, independent TDEs may be observed over decades in some special galaxies where the TDE rate is extremely high. Exploring the diversity of recurring TDEs and probing their natures with rich observational data helps us to understand these mechanisms.
Aims. We report the discovery of a second optical flare that occurred in September 2021 in IRAS F01004-2237, where a first flare that occurred in 2010 had already been reported. We also present a detailed analysis of multi-band data. We aim to understand the nature of the flare and explore the possible causes of the recurring flares.
Methods. We describe our analysis of the position of the flare, the multi-band light curves (LCs), the optical and ultraviolet (UV) spectra, and the X-ray LC and spectra.
Results. The position of the flare coincides with the galaxy centre with a precision of 650 pc. The flare peaks in ∼50 days with an absolute magnitude of ∼ - 21 and fades in two years, roughly following L ∝ t–5/3. It maintains a nearly constant blackbody temperature of ∼22 000 K in later stages. Its optical and UV spectra show hydrogen and helium broad emission lines with full width at half maxima of 7000-21 000 km s–1 and a He II/Hα ratio of 0.3-2.3. It shows weak X-ray emission relative to UV emission, with X-ray flares lasting for < 2 - 3 weeks, during which the spectrum is soft with a power-law index of $ \Gamma=4.4^{+1.4}_{-1.3} $. These characters are consistent with a TDE, ruling out the possibilities of a supernova or an active galactic nucleus flare. With a TDE model, we infer a peak UV luminosity of 3.3 ± 0.2 × 1044 erg s–1 and an energy budget of 4.5 ± 0.2 × 1051 erg.
Conclusions. A TDE caused the flare that occurred in 2021. The two optical flares separated by 10.3 ± 0.3 years can be interpreted as repeating partial TDEs, double TDEs, or two independent TDEs. Although no definitive conclusion can be drawn, the partial TDEs interpretation predicts a third flare around 2033, and the independent TDEs interpretation predicts a high TDE rate of ≳10–2 yr–1 in F01004-2237, both of which can be tested by future observations.

Abstract Copyright: © The Authors 2024

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

Simbad objects: 31

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Number of rows : 31
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 AT 2021loi ev 01 00 39.619 +39 42 30.31           ~ 12 0
2 AT 2022agi ev 01 02 49.990 -22 21 57.24           ~ 6 0
3 IRAS 01003-2238 Sy2 01 02 49.9920152640 -22 21 57.262136544   18.62 18.9 17.83   ~ 192 0
4 2dFGRS TGS564Z081 Sy2 01 19 08.6635573080 -34 11 30.527946780   16.226   15.275   ~ 159 0
5 OGLE17aaj ev 01 56 24.93 -71 04 15.7           ~ 29 0
6 eRASSt J045650.3-203750 X 04 56 50.3 -20 37 50           ~ 40 0
7 MCG-02-13-040a Sy2 05 04 53.05680 -10 14 52.3356   15   14.22   ~ 67 1
8 ESO 253-3 Sy2 05 25 18.058 -46 00 21.36 15.95 15.10 14.77 13.95   ~ 80 0
9 ASASSN -14ko ev 05 25 18.13 -46 00 20.3           SNIIn 84 0
10 AT 2019avd Sy1 08 23 36.80 +04 23 03.4           ~ 47 0
11 AT 2020vdq ev 10 08 53.440 +42 43 00.23           ~ 37 0
12 QSO J1027+6050 QSO 10 27 38.5366210392 +60 50 16.466114004   17.95 17.66     ~ 40 0
13 [DDM2009] CSS100217 J102913+404220 SN* 10 29 13.0 +40 42 20           SNIIn 39 0
14 NAME Arp 299-B AT1 Rad 11 28 30.9875529 +58 33 40.783601           ~ 39 0
15 ASASSN -22ci ev 12 20 45.010 +49 33 04.68           ~ 31 0
16 2XMM J123103.2+110648 AG? 12 31 03.239 +11 06 48.60           ~ 56 0
17 IC 3599 Sy1 12 37 41.1939398400 +26 42 27.484266888   15.7 16.5     ~ 191 0
18 RX J133157.6-324319 X 13 31 57.90 -32 43 21.2           ~ 19 0
19 [VV2006] J133451.9-013836 QSO 13 34 51.9104599176 -01 38 35.467860480   20.81 20.70     ~ 21 0
20 SDSS J140941.88+552928.0 AGN 14 09 41.8833027816 +55 29 28.058874792           ~ 55 0
21 Z 49-155 Sy1 15 24 16.6702264008 +04 51 19.027331064   16.70 16.26     ~ 70 0
22 AT 2018dyk ev 15 33 08.01 +44 32 08.2           ~ 33 0
23 2MASS J16053409+2309501 Sy1 16 05 34.1334583656 +23 09 50.053619772   20.29 19.69     ~ 15 0
24 AT 2017bgt AGN 16 11 05.518 +02 34 02.14           ~ 35 0
25 3C 332.0 Sy1 16 17 42.5380089648 +32 22 34.372277976   18.25 17.45     ~ 268 1
26 SWIFT J164449.3+573451 G 16 44 47.81184000 +57 35 00.7113480           ~ 533 0
27 ASASSN -15oi SN* 20 39 09.096 -30 45 20.71           ~ 184 0
28 ASASSN -15lh ev 22 02 15.4 -61 39 34           ~ 187 1
29 AT 2018bcb ev 22 43 42.90 -16 59 08.1           ~ 39 0
30 AT 2018fyk ev 22 50 16.10 -44 51 53.5           ~ 114 0
31 AT 2023lli ev 22 57 39.470 +40 32 40.02           ~ 9 0

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