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Panning for gold, but finding helium: Discovery of the ultra-stripped supernova SN 2019wxt from gravitational-wave follow-up observations

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cris.lastimport.scopus2024-02-12T20:57:22Z
dc.abstract.enWe present the results from multi-wavelength observations of a transient discovered during an intensive follow-up campaign of S191213g, a gravitational wave (GW) event reported by the LIGO-Virgo Collaboration as a possible binary neutron star merger in a low latency search. This search yielded SN 2019wxt, a young transient in a galaxy whose sky position (in the 80% GW contour) and distance (∼150 Mpc) were plausibly compatible with the localisation uncertainty of the GW event. Initially, the transient's tightly constrained age, its relatively faint peak magnitude (M<SUB>i</SUB> ∼ −16.7 mag), and the r-band decline rate of ∼1 mag per 5 days appeared suggestive of a compact binary merger. However, SN 2019wxt spectroscopically resembled a type Ib supernova, and analysis of the optical-near-infrared evolution rapidly led to the conclusion that while it could not be associated with S191213g, it nevertheless represented an extreme outcome of stellar evolution. By modelling the light curve, we estimated an ejecta mass of only ∼0.1 M<SUB>⊙</SUB>, with <SUP>56</SUP>Ni comprising ∼20% of this. We were broadly able to reproduce its spectral evolution with a composition dominated by helium and oxygen, with trace amounts of calcium. We considered various progenitor channels that could give rise to the observed properties of SN 2019wxt and concluded that an ultra-stripped origin in a binary system is the most likely explanation. Disentangling genuine electromagnetic counterparts to GW events from transients such as SN 2019wxt soon after discovery is challenging: in a bid to characterise this level of contamination, we estimated the rate of events with a volumetric rate density comparable to that of SN 2019wxt and found that around one such event per week can occur within the typical GW localisation area of O4 alerts out to a luminosity distance of 500 Mpc, beyond which it would become fainter than the typical depth of current electromagnetic follow-up campaigns.
dc.affiliationUniwersytet Warszawski
dc.contributor.authorAgudo, I.
dc.contributor.authorAmati, L.
dc.contributor.authorAn, T.
dc.contributor.authorBauer, F. E.
dc.contributor.authorBenetti, S.
dc.contributor.authorBernardini, M. G.
dc.contributor.authorBeswick, R.
dc.contributor.authorBhirombhakdi, K.
dc.contributor.authorBoer, T. de
dc.contributor.authorBranchesi, M.
dc.contributor.authorBrennan, S. J.
dc.contributor.authorBrocato, E.
dc.contributor.authorCaballero-García, M. D.
dc.contributor.authorCappellaro, E.
dc.contributor.authorRodríguez, N. Castro
dc.contributor.authorCastro-Tirado, A. J.
dc.contributor.authorChambers, K. C.
dc.contributor.authorChassande-Mottin, E.
dc.contributor.authorChaty, S.
dc.contributor.authorChen, T. -W.
dc.contributor.authorColeiro, A.
dc.contributor.authorCovino, S.
dc.contributor.authorD'Ammando, F.
dc.contributor.authorD'Avanzo, P.
dc.contributor.authorD'Elia, V.
dc.contributor.authorFiore, A.
dc.contributor.authorFlörs, A.
dc.contributor.authorFraser, M.
dc.contributor.authorFrey, S.
dc.contributor.authorFrohmaier, C.
dc.contributor.authorFulton, M.
dc.contributor.authorGalbany, L.
dc.contributor.authorGall, C.
dc.contributor.authorGao, H.
dc.contributor.authorGarcía-Rojas, J.
dc.contributor.authorGhirlanda, G.
dc.contributor.authorGiarratana, S.
dc.contributor.authorGillanders, J. H.
dc.contributor.authorGiroletti, M.
dc.contributor.authorGompertz, B. P.
dc.contributor.authorGromadzki, Mariusz
dc.contributor.authorHeintz, K. E.
dc.contributor.authorHjorth, J.
dc.contributor.authorHu, Y. -D.
dc.contributor.authorHuber, M. E.
dc.contributor.authorInkenhaag, A.
dc.contributor.authorIzzo, L.
dc.contributor.authorJin, Z. P.
dc.contributor.authorJonker, P. G.
dc.contributor.authorKann, D. A.
dc.contributor.authorKool, E. C.
dc.contributor.authorKotak, R.
dc.contributor.authorLeloudas, G.
dc.contributor.authorLevan, A. J.
dc.contributor.authorLin, C. -C.
dc.contributor.authorLyman, J. D.
dc.contributor.authorMagnier, E. A.
dc.contributor.authorMaguire, K.
dc.contributor.authorMandel, I.
dc.contributor.authorMarcote, B.
dc.contributor.authorSánchez, D. Mata
dc.contributor.authorMattila, S.
dc.contributor.authorMelandri, A.
dc.contributor.authorMichałowski, M. J.
dc.contributor.authorMoldon, J.
dc.contributor.authorNicholl, M.
dc.contributor.authorGuelbenzu, A. Nicuesa
dc.contributor.authorOates, S. R.
dc.contributor.authorOnori, F.
dc.contributor.authorOrienti, M.
dc.contributor.authorPaladino, R.
dc.contributor.authorParagi, Z.
dc.contributor.authorPerez-Torres, M.
dc.contributor.authorPian, E.
dc.contributor.authorPignata, G.
dc.contributor.authorPiranomonte, S.
dc.contributor.authorQuirola-Vásquez, J.
dc.contributor.authorRagosta, F.
dc.contributor.authorRau, A.
dc.contributor.authorRonchini, S.
dc.contributor.authorRossi, A.
dc.contributor.authorSánchez-Ramírez, R.
dc.contributor.authorSalafia, O. S.
dc.contributor.authorSchulze, S.
dc.contributor.authorSmartt, S. J.
dc.contributor.authorSmith, K. W.
dc.contributor.authorSollerman, J.
dc.contributor.authorSrivastav, S.
dc.contributor.authorStarling, R. L. C.
dc.contributor.authorSteeghs, D.
dc.contributor.authorStevance, H. F.
dc.contributor.authorTanvir, N. R.
dc.contributor.authorTesta, V.
dc.contributor.authorTorres, M. A. P.
dc.contributor.authorValeev, A.
dc.contributor.authorVergani, S. D.
dc.contributor.authorVescovi, D.
dc.contributor.authorWainscost, R.
dc.contributor.authorWatson, D.
dc.contributor.authorWiersema, K.
dc.contributor.authorWyrzykowski, Łukasz
dc.contributor.authorYang, J.
dc.contributor.authorYang, S.
dc.contributor.authorYoung, D. R.
dc.date.accessioned2024-01-25T16:12:50Z
dc.date.available2024-01-25T16:12:50Z
dc.date.copyright2023-07-20
dc.date.issued2023
dc.description.accesstimeAT_PUBLICATION
dc.description.financePublikacja bezkosztowa
dc.description.versionFINAL_PUBLISHED
dc.description.volume675
dc.identifier.doi10.1051/0004-6361/202244751
dc.identifier.issn0004-6361
dc.identifier.urihttps://repozytorium.uw.edu.pl//handle/item/115453
dc.identifier.weblinkhttp://adsabs.harvard.edu/abs/2023A&A...675A.201A
dc.languageeng
dc.pbn.affiliationastronomy
dc.relation.ispartofAstronomy and Astrophysics
dc.relation.pagesA201
dc.rightsCC-BY
dc.sciencecloudnosend
dc.titlePanning for gold, but finding helium: Discovery of the ultra-stripped supernova SN 2019wxt from gravitational-wave follow-up observations
dc.typeJournalArticle
dspace.entity.typePublication