Статья

A Luminous Red Optical Flare and Hard X-Ray Emission in the Tidal Disruption Event AT 2024kmq

A. Y. Q. HoDepartment of Astronomy, Cornell University, Ithaca, NY 14853, USAYuhan YaoDepartment of Astronomy, University of California, Berkeley, 501 Campbell Hall, Berkeley, CA 94720, USATatsuya MatsumotoDepartment of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, 606-8502, JapanGenevieve SchroederDepartment of Astronomy, Cornell University, Ithaca, NY 14853, USAEric R. CoughlinDepartment of Physics, Syracuse University, Syracuse, NY 13210, USAD. A. PerleyAstrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UKIgor AndreoniUniversity of North Carolina at Chapel Hill, 120 E. Cameron Ave., Chapel Hill, NC 27514, USAE. BellmDIRAC Institute, Department of Astronomy, University of Washington, 3910 15th Ave. NE, Seattle, WA 98195, USAX. ChenIPAC, California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USAR. ChornockDepartment of Astronomy, University of California, Berkeley, 501 Campbell Hall, Berkeley, CA 94720, USASofia CovarrubiasDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAKaustav K. DasDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAC. FremlingDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAM. GilfanovMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, GermanyK-Ryan HindsAstrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UKDan JarvisAstrophysics Research Cluster, School of Mathematical and Physical Sciences, University of Sheffield, Sheffield S3 7RH, UKM. M. KasliwalDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAChang LiuCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, 1800 Sherman Ave., Evanston, IL 60201, USAJ. LymanDepartment of Physics, University of Warwick, Coventry CV4 7AL, UKFrank J. MasciIPAC, California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USAThomas A. PrinceDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAVikram RaviDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAR. Michael RichDepartment of Physics and Astronomy, UCLA, 430 Portola Plaza, Box 951547, Los Angeles, CA 90095-1547, USAReed RiddleCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USAJason SevillaDepartment of Astronomy, Cornell University, Ithaca, NY 14853, USARoger M. SmithCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USAJ. SollermanDepartment of Astronomy, The Oskar Klein Centre, Stockholm University, AlbaNova, 10691 Stockholm, SwedenJean J. SomalwarDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAGokul P. SrinivasaragavanJoint Space-Science Institute, University of Maryland, College Park, MD 20742, USAR. SunyaevMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, GermanyJada L. VailDepartment of Astronomy, Cornell University, Ithaca, NY 14853, USAJ. WiseAstrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UKSeokjun YunDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA

2025en

ABI

Аннотация

Abstract We present the optical discovery and multiwavelength follow-up observations of AT 2024kmq, a likely tidal disruption event (TDE) associated with a supermassive ( M BH ∼ 10 8 M ⊙ ) black hole in a massive galaxy at z = 0.192. The optical light curve of AT 2024kmq exhibits two distinct peaks: an early fast (timescale 1 day) and luminous ( M ≈ −20 mag) red peak, then a slower (timescale 1 month) blue peak with a higher optical luminosity ( M ≈ −22 mag) and featureless optical spectra. The second component is similar to the spectroscopic class of “featureless TDEs” in the literature, and during this second component we detect highly variable, luminous ( L X ≈ 10 44 erg s −1 ), and hard ( f ν ∝ ν −1.5 ) X-ray emission. Luminous (10 29 erg s −1 Hz −1 at 10 GHz) but unchanging radio emission likely arises from an underlying active galactic nucleus. The luminosity, timescale, and color of the early red optical peak can be explained by synchrotron emission, or alternatively by thermal emission from material at a large radius ( R ≈ a few × 10 15 cm). Possible physical origins for this early red component include an off-axis relativistic jet, and shocks from self-intersecting debris leading to the formation of the accretion disk. Late-time radio observations will help distinguish between the two possibilities.

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Идентификаторы

DOI: 10.3847/1538-4357/ade8f2

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Цитирований: 2Использованных источников: 0

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