THA 15-31: Discovery with VLT/X-shooter and Swift /UVOT of a new symbiotic star of the accreting-only variety

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dc.contributor.authorMunari, U.
dc.contributor.authorAlcalá, J.M.
dc.contributor.authorFrasca, A.
dc.contributor.authorMasetti, N.
dc.contributor.authorTraven, G.
dc.contributor.authorAkras, S.
dc.contributor.authorZampieri, L.
dc.date.accessioned2024-06-05T21:16:33Z
dc.date.available2024-06-05T21:16:33Z
dc.date.issued2022-05-01
dc.descriptionIndexación: Scopus.
dc.description.abstractWe report the discovery and characterization of a new symbiotic star of the accreting-only variety, which we observed in the optical/near-infrared (NIR) with VLT/X-shooter and in the X-rays/ultraviolet with Swift/UVOT+XRT. The new symbiotic star, THA 15-31, was previously described as a pre-main sequence star belonging to the Lupus 3 association. Our observations, ancillary data, and Gaia EDR3 parallax indicate that THA 15-31 is a symbiotic star composed of an M6III red giant and an accreting companion, is subject to EB 0.38 reddening, and is located at a distance of 12 kpc and at 1.8 kpc above the Galactic plane in the outskirts of the Bulge. The luminosity of the accreting companion is 100, placing THA 15-31 among the symbiotic stars accreting at a high rate (2.5 10-8 yr-1 if the accretion is occurring on a white dwarf of 1M). The observed emission lines originate primarily from H I, He I, and Fe II, with no He II or other high-excitation lines observed; a sharp central absorption superimposed on the Balmer emission lines is observed, while all other lines have a simple Gaussian-like profile. The emission from the companion dominates over the M6III red giant at U and B-band wavelengths, and is consistent with an origin primarily in an optically thick accretion disk. No significant photometric variability is observed at optical or NIR wavelengths, suggesting either a face-on orbital orientation and/or that the red giant is far from Roche-lobe filling conditions. The profile of emission lines supports a low orbital inclination if they form primarily in the accretion disk. An excess emission is present in AllWISE W3 (12 μm) and W4 (22 μm) data, radiating a luminosity, consistent with thermal emission from optically thin circumstellar dust. © 2022 Authors
dc.description.urihttps://www.aanda.org/articles/aa/full_html/2022/05/aa42058-21/aa42058-21.html
dc.identifier.citationAstronomy and Astrophysics, Volume 661, 1 May 2022, Article number A124
dc.identifier.doi10.1051/0004-6361/202142058
dc.identifier.issn0004-6361
dc.identifier.urihttps://repositorio.unab.cl/handle/ria/57368
dc.language.isoen
dc.publisherEDP Sciences
dc.rights.licenseATRIBUCIÓN 4.0 INTERNACIONAL CC BY 4.0 Deed
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/deed.es
dc.subjectBinaries: symbiotic
dc.subjectGeometrical optics
dc.subjectGiant stars
dc.subjectInfrared devices
dc.subjectIron compounds
dc.subjectLuminance
dc.subjectWhite dwarfs
dc.titleTHA 15-31: Discovery with VLT/X-shooter and Swift /UVOT of a new symbiotic star of the accreting-only variety
dc.typeArtículo
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