The fast transient AT 2023clx in the nearby LINER galaxy NGC 3799 as a tidal disruption of a very low-mass star

doi:10.1051/0004-6361/202449296

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	The fast transient AT 2023clx in the nearby LINER galaxy NGC 3799 as a tidal disruption of a very low-mass star
	Charalampopoulos, P.1; Kotak, R.1; Wevers, T.2,3; Leloudas, G.4; Kravtsov, T.1,5; Pursiainen, M.6; Ramsden, P.7,8,9; Reynolds, T. M.1,10; Aamer, A.9; Anderson, J. P.5,11; Arcavi, I.12; Cai YZ(蔡永志)13,14,15 ; Chen, T.-W.16; Dennefeld, M.17; Galbany, L.18,19; Gromadzki, M.20; Gutiérrez, C. P.18,19; Ihanec, N.20,21; Kangas, T.1,22; Kankare, E.1; Kool, E.1,22,23; Lawrence, A.24; Lundqvist, P.23; Makrygianni, L.25; Mattila, S.1,26; Müller, T. E.18,19; Nicholl, M.9; Onori, F.27; Sahu, A.6; Smartt, S. J.9,28; Sollerman, J.23; Wang, Y.29,30; Young, D. R.9
发表期刊	ASTRONOMY & ASTROPHYSICS
	2024-09-24
卷号	689
DOI	10.1051/0004-6361/202449296
产权排序	第13完成单位
收录类别	SCI ; EI
关键词	black hole physics methods: observational galaxies: nuclei
摘要	We present an extensive analysis of the optical and ultraviolet (UV) properties of AT 2023clx, the closest optical/UV tidal disruption event (TDE) to date (z = 0.01107), which occurred in the nucleus of the interacting low-ionization nuclear emission-line region (LINER) galaxy, NGC 3799. After correcting for the host reddening (E(B - V)(h) = 0.179 mag), we find its peak absolute g-band magnitude to be -18.03 +/- 0.07 mag, and its peak bolometric luminosity to be L-pk = (1.57 +/- 0.19)x10(43) erg s(-1). AT 2023clx displays several distinctive features: first, it rose to peak within 10.4 +/- 2.5 days, making it the fastest rising TDE to date. Our SMBH mass estimate of (M) over bar (BH) approximate to 10(6.0) M-circle dot -estimated using several standard methods- rules out the possibility of an intermediate-mass BH as the reason for the fast rise. Dense spectral follow-up reveals a blue continuum that cools slowly and broad Balmer and He II lines as well as weak He I lambda lambda 5876,6678 emission features that are typically seen in TDEs. The early, broad (width similar to 15 000 km s(-1)) profile of H alpha matches theoretical expectations from an optically thick outflow. A flat Balmer decrement (L-H alpha/L-H beta similar to 1.58) suggests that the lines are collisionally excited rather than being produced via photoionisation, in contrast to typical active galactic nuclei. A second distinctive feature, seen for the first time in TDE spectra, is a sharp, narrow emission peak at a rest wavelength of similar to 6353 angstrom. This feature is clearly visible up to 10 d post-peak; we attribute it to clumpy material preceding the bulk outflow, which manifests as a high-velocity component of H alpha (-9584 km s(-1)). Its third distinctive feature is the rapid cooling during the first similar to 20 days after peak, reflected as a break in the temperature evolution. Combining these findings, we propose a scenario for AT 2023clx involving the disruption of a very low-mass star (less than or similar to 0.1 M-circle dot) with an outflow launched in our line of sight and with disruption properties that led to efficient circularisation and prompt accretion disc formation, observed through a low-density photosphere.
资助项目	Research Council of Finland[340613]; Research Council of Finland[350458]; VILLUM FONDEN[19054]; STFC[2742655]; STFC[ST/X006506/1]; STFC[ST/T000198/1]; STFC[ST/X001253/1]; European Research Council (ERC)[948381]; European Research Council (ERC)[852097]; ANID, Millennium Science Initiative[ICN12_009]; Israel Science Foundation[2752/19]; United States - Israel Binational Science Foundation (BSF)[2018166]; Pazy foundation[216312]; National Natural Science Foundation of China (NSFC)[12303054]; Instituto de Astrofisica de Andalucia (IAA)[202401AU070063]; Yunnan Fundamental Research Projects; University of Copenhagen and NOT[202302AN360001]; International Centre of Supernovae, Yunnan Key Laboratory; Instrument Centre for Danish Astrophysics (IDA); Yushan Young Fellow Program by the Ministry of Education, Taiwan; Finnish Centre for Astronomy with ESO (FINCA) via Academy of Finland; Spanish Ministerio de Ciencia e Innovacion (MCIN); University of Massachusetts[PID2020-115253GA-I00]; Agencia Estatal de Investigacion (AEI); Infrared Processing and Analysis Center/California Institute of Technology - National Aeronautics and Space Administration[PID2020-115253GA-I00]; Infrared Processing and Analysis Center/California Institute of Technology - National Aeronautics and Space Administration[FJC2021-047124-I]; European Union Next Generation EU/PRTR funds; National Science Foundation[20215AT016]; Centro Superior de Investigaciones Cientificas (CSIC); Program Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M]; Departament de Recerca i Universitats de la Generalitat de Catalunya[2021-SGR-01270]; Secretary of Universities and Research (Government of Catalonia); Horizon 2020 Research and Innovation Programme of the European Union[2021 BP 00168]; UK Space Agency[ST/Y000692/1]; MIUR, PRIN[2020KB33TP]; UK Research and Innovation Fellowship[MR/T020784/1]; Warwick Astrophysics PhD prize scholarship; Strategic Priority Research Program of the Chinese Academy of Sciences[XDB0550200]; European Organisation for Astronomical Research in the Southern Hemisphere under ESO DDT[110.25AX]; EPESSTO+ under ESO program[108.220C]; EPESSTO+ under ESO program[111.24PR]; University of Turku; University of Oslo; Finland and Norway; University of Iceland; Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain; Instituto de Astrofisica de Canarias under NOT programmes
项目资助者	Research Council of Finland[340613, 350458] ; VILLUM FONDEN[19054] ; STFC[2742655, ST/X006506/1, ST/T000198/1, ST/X001253/1] ; European Research Council (ERC)[948381, 852097] ; ANID, Millennium Science Initiative[ICN12_009] ; Israel Science Foundation[2752/19] ; United States - Israel Binational Science Foundation (BSF)[2018166] ; Pazy foundation[216312] ; National Natural Science Foundation of China (NSFC)[12303054] ; Instituto de Astrofisica de Andalucia (IAA)[202401AU070063] ; Yunnan Fundamental Research Projects ; University of Copenhagen and NOT[202302AN360001] ; International Centre of Supernovae, Yunnan Key Laboratory ; Instrument Centre for Danish Astrophysics (IDA) ; Yushan Young Fellow Program by the Ministry of Education, Taiwan ; Finnish Centre for Astronomy with ESO (FINCA) via Academy of Finland ; Spanish Ministerio de Ciencia e Innovacion (MCIN) ; University of Massachusetts[PID2020-115253GA-I00] ; Agencia Estatal de Investigacion (AEI) ; Infrared Processing and Analysis Center/California Institute of Technology - National Aeronautics and Space Administration[PID2020-115253GA-I00, FJC2021-047124-I] ; European Union Next Generation EU/PRTR funds ; National Science Foundation[20215AT016] ; Centro Superior de Investigaciones Cientificas (CSIC) ; Program Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M] ; Departament de Recerca i Universitats de la Generalitat de Catalunya[2021-SGR-01270] ; Secretary of Universities and Research (Government of Catalonia) ; Horizon 2020 Research and Innovation Programme of the European Union[2021 BP 00168] ; UK Space Agency[ST/Y000692/1] ; MIUR, PRIN[2020KB33TP] ; UK Research and Innovation Fellowship[MR/T020784/1] ; Warwick Astrophysics PhD prize scholarship ; Strategic Priority Research Program of the Chinese Academy of Sciences[XDB0550200] ; European Organisation for Astronomical Research in the Southern Hemisphere under ESO DDT[110.25AX] ; EPESSTO+ under ESO program[108.220C, 111.24PR] ; University of Turku ; University of Oslo ; Finland and Norway ; University of Iceland ; Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain ; Instituto de Astrofisica de Canarias under NOT programmes[66-019, 66-506, 67-021] ; [306531]
语种	英语
学科领域	天文学 ; 恒星与银河系
文章类型	Article
出版者	EDP SCIENCES S A
出版地	17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
ISSN	0004-6361
URL	查看原文
WOS记录号	WOS:001321216400017
WOS研究方向	Astronomy & Astrophysics
WOS类目	Astronomy & Astrophysics
关键词[WOS]	SUPERMASSIVE BLACK-HOLES ; X-RAY-EMISSION ; DIGITAL SKY SURVEY ; GALACTIC NUCLEI ; OPTICAL RISE ; FOLLOW-UP ; E PLUS ; EVENT ; OUTFLOW ; FAINT
EI入藏号	20244017143568
EI主题词	Photoionization
EI分类号	1301.1.3 - 1301.2.1.1.1 - 1302.1.2 - 802.2 Chemical Reactions
引用统计
文献类型	期刊论文
版本	出版稿
条目标识符	http://ir.ynao.ac.cn/handle/114a53/27629
专题	南方基地中国科学院天体结构与演化重点实验室
作者单位	1.Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland; 2.Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; 3.European Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile; 4.DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Kgs. Lyngby, Denmark; 5.European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile; 6.Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK; 7.Institute for Gravitational Wave Astronomy, University of Birmingham, Birmingham B15 2TT, UK; 8.School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UK; 9.Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK; 10.Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, København N DK-2200, Denmark; 11.Millennium Institute of Astrophysics MAS, Nuncio Monsenor Sotero Sanz 100, Off. 104, Providencia, Santiago, Chile; 12.School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel; 13.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, P.R. China; 14.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, P.R. China; 15.International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, P.R. China; 16.Graduate Institute of Astronomy, National Central University, 300 Jhongda Road, 32001 Jhongli, Taiwan; 17.Sorbonne Université, CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98bis Bd Arago 75014 Paris, France; 18.Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain; 19.Institut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain; 20.Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, PL-00-478 Warszawa, Poland; 21.Isaac Newton Group of Telescopes, ING, 38700 La Palma, S.C. Tenerife, Spain; 22.Finnish Centre for Astronomy with ESO (FINCA), FI-20014 University of Turku, Finland; 23.The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm, Sweden; 24.Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK; 25.Department of Physics, Lancaster University, Lancaster LA1 4YB, UK; 26.School of Sciences, European University Cyprus, Diogenes Street, Engomi, 1516 Nicosia, Cyprus; 27.INAF-Osservatorio Astronomico d’Abruzzo, Via M. Maggini snc, I-64100 Teramo, Italy; 28.Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK; 29.National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Beijing 100101, China; 30.Physics & Astronomy, University of Southampton, Southampton, Hampshire SO17 1BJ, UK
推荐引用方式 GB/T 7714	Charalampopoulos, P.,Kotak, R.,Wevers, T.,et al. The fast transient AT 2023clx in the nearby LINER galaxy NGC 3799 as a tidal disruption of a very low-mass star[J]. ASTRONOMY & ASTROPHYSICS,2024,689.
APA	Charalampopoulos, P..,Kotak, R..,Wevers, T..,Leloudas, G..,Kravtsov, T..,...&Young, D. R..(2024).The fast transient AT 2023clx in the nearby LINER galaxy NGC 3799 as a tidal disruption of a very low-mass star.ASTRONOMY & ASTROPHYSICS,689.
MLA	Charalampopoulos, P.,et al."The fast transient AT 2023clx in the nearby LINER galaxy NGC 3799 as a tidal disruption of a very low-mass star".ASTRONOMY & ASTROPHYSICS 689(2024).

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