XRISM/Xtend Transient Search (XTS) detected an X-ray flare possibly from an M dwarf star

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dc.contributor.authorYoneyama, T.
dc.contributor.authorFukushima, K.
dc.contributor.authorHayashi, K.
dc.contributor.authorPottschmidt, Katja
dc.contributor.authoret al
dc.date.accessioned2025-10-03T19:33:44Z
dc.date.issued2025-03-10
dc.descriptionAuthors: T. Yoneyama (Chuo U.), K. Fukushima, K. Hayashi, Y. Kanemaru, S. Ogawa, T. Yoshida (JAXA), M. Audard (U. de Geneve), E. Behar (Technion), S. Inoue (Kyoto U.), Y. Ishihara (Chuo U.), T. Kohmura (TUS), Y. Maeda (JAXA), M. Mizumoto (UTEF), N. Nagashima (Chuo U.), M. Nobukawa (NUE), K. Pottschmidt (UMBC, NASA GSFC, CRESST), M. Shidatsu (Ehime U.), H. Sugai (Chuo U.), Y. Terada (Saitama U.), Y. Terashima (Ehime U.), Y. Tsuboi (Chuo U.), H. Uchida (Kyoto U.), T. Yanagi (Chuo U.), , M. Yoshimoto (Osaka U.)
dc.description.abstractXRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1748-2832 on 2025-03-09 TT. The source position is determined to be (R.A., Dec.) = (266.890 -28.538), with a systematic error of ∼ 40 arcsec. A plausible counterpart is an X-ray source CXOGCS J174734.5-283215, a potential M dwarf star located ∼ 14 asec apart from the position of XRISM J1748-2832. Another counterpart candidate is a YSO candidate SPICY 64348 located ∼ 21 arcsec apart from XRISM J1748-2832. Distances to CXOGCS J174734.5-283215 and SPICY 64348 are ∼ 590 and ∼ 500 pc, respectively by Gaia DR3. The flare started on 2025-03-09 at 06:25 TT, rapidly peaked at 06:31 TT, and then exponentially decayed in ∼ 3 ksec. The timing properties are derived by fitting the 0.4 – 2.0 keV light curve with a constant + burst model in the QDP software package. The flux at the flare phase is calculated as 1.2 × 10⁻¹² erg s⁻¹ cm⁻² (0.4 – 2.0 keV). A systematic error of roughly 20% should be added to the statistical error. Corresponding luminosity is 5.1 D²₅₉₀ ₚ꜀ × 10³¹ erg s⁻¹ . We derived the above systematic error for the flux by comparing our derived values for the sources detected with XTS in several observations with those for the corresponding X-ray counterparts. We estimated the systematic error for the source position from the separations between the detected sources with the corresponding counterparts in the same field of view.
dc.description.urihttps://www.astronomerstelegram.org/?read=17071
dc.format.extent2 pages
dc.genrearticles
dc.identifierdoi:10.13016/m2jxsy-7ghx
dc.identifier.citationYoneyama, T., K. Fukushima, K. Hayashi, K. Pottschmidt, et al. “XRISM/Xtend Transient Search (XTS) Detected an X-Ray Flare Possibly from an M Dwarf Star.” The Astronomer’s Telegram, March 10, 2025. https://www.astronomerstelegram.org/?read=17071.
dc.identifier.urihttp://hdl.handle.net/11603/40319
dc.language.isoen
dc.publisherThe Astronomer's Telegram
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Physics Department
dc.relation.ispartofUMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
dc.relation.ispartofUMBC Faculty Collection
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.subject X-ray flare
dc.subjectX-ray source XRISM J1748-2832
dc.titleXRISM/Xtend Transient Search (XTS) detected an X-ray flare possibly from an M dwarf star
dc.typeText
dcterms.creatorhttps://orcid.org/0000-0002-4656-6881

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