Delayed appearance and evolution of coronal lines in the TDE AT2019qiz

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dc.catalogadordfo
dc.contributor.authorShort, P.
dc.contributor.authorLawrence, A.
dc.contributor.authorNicholl, M.
dc.contributor.authorWard, M.
dc.contributor.authorReynolds, T. M.
dc.contributor.authorMattila, S.
dc.contributor.authorYin, C.
dc.contributor.authorArcavi, I
dc.contributor.authorCarnall, A.
dc.contributor.authorCharalampopoulos, P.
dc.contributor.authorGromadzki, M.
dc.contributor.authorJonker, P. G.
dc.contributor.authorKim, Sam
dc.contributor.authorLeloudas, G.
dc.contributor.authorMandel, I
dc.contributor.authorOnori, F.
dc.contributor.authorPursiainen, M.
dc.contributor.authorSchulze, S.
dc.contributor.authorVillforth, C.
dc.contributor.authorWevers, T.
dc.date.accessioned2023-10-04T20:11:00Z
dc.date.available2023-10-04T20:11:00Z
dc.date.issued2023
dc.description.abstractTidal disruption events (TDEs) occur when a star gets torn apart by a supermassive black hole as it crosses its tidal radius. We present late-time optical and X-ray observations of the nuclear transient AT2019qiz, which showed the typical signs of an optical-UV transient class commonly believed to be TDEs. Optical spectra were obtained 428, 481, and 828 rest-frame days after optical light-curve peak, and a UV/X-ray observation coincided with the later spectrum. The optical spectra show strong coronal emission lines, including [Fe vii], [Fe x], [Fe xi], and [Fe xiv]. The Fe lines rise and then fall, except [Fe xiv] that appears late and rises. We observe increasing flux of narrow H & alpha; and H & beta; and a decrease in broad H & alpha; flux. The coronal lines have full width at half-maximum ranging from & SIM;150-300 km s(-1), suggesting they originate from a region between the broad- and narrow-line emitting gas. Between the optical flare and late-time observation, the X-ray spectrum softens dramatically. The 0.3-1 keV X-ray flux increases by a factor of & SIM;50, while the hard X-ray flux decreases by a factor of & SIM;6. Wide-field Infrared Survey Explorer fluxes also rose over the same period, indicating the presence of an infrared echo. With AT2017gge, AT2019qiz is one of two examples of a spectroscopically confirmed optical-UV TDE showing delayed coronal line emission, supporting speculations that Extreme Coronal Line Emitters in quiescent galaxies can be echos of unobserved past TDEs. We argue that the coronal lines, narrow lines, and infrared emission arise from the illumination of pre-existing material likely related to either a previous TDE or active galactic nucleus activity.
dc.fechaingreso.objetodigital2023-10-04
dc.fuente.origenWOS
dc.fuente.origenORCID
dc.identifier.doi10.1093/mnras/stad2270
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stad2270
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/75012
dc.identifier.wosidWOS:001052334400001
dc.information.autorucEscuela de Ingeniería ; Kim Sam ; 0000-0001-8332-0023 ; 237734
dc.issue.numero1
dc.language.isoen
dc.nota.accesoContenido parcial
dc.pagina.final1587
dc.pagina.inicio1568
dc.publisherOxford University Press
dc.revistaMonthly Notices of the Royal Astronomical Society
dc.rightsacceso restringido
dc.subjectaccretion
dc.subjectaccretion discs
dc.subjectblack hole physics
dc.subjecttransients: tidal disruption events
dc.subject.ddc520
dc.subject.deweyAstronomíaes_ES
dc.titleDelayed appearance and evolution of coronal lines in the TDE AT2019qiz
dc.typeartículo
dc.volumen525
sipa.codpersvinculados237734
sipa.indexWOS
sipa.trazabilidadWOS;2023-09-09
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