Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/29004
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Margutti, R. | en_US |
dc.contributor.author | Metzger, B. D. | en_US |
dc.contributor.author | Chornock, R. | en_US |
dc.contributor.author | Vurm, I. | en_US |
dc.contributor.author | Roth, N. | en_US |
dc.contributor.author | Grefenstette, B. W. | en_US |
dc.contributor.author | Savchenko, V. | en_US |
dc.contributor.author | Cartier, R. | en_US |
dc.contributor.author | Steiner, J. F. | en_US |
dc.contributor.author | Terreran, G. | en_US |
dc.contributor.author | Margalit, B. | en_US |
dc.contributor.author | Migliori, G. | en_US |
dc.contributor.author | Milisavljevic, D. | en_US |
dc.contributor.author | Alexander, K. D. | en_US |
dc.contributor.author | Bietenholz, M. | en_US |
dc.contributor.author | Blanchard, P. K. | en_US |
dc.contributor.author | Bozzo, E. | en_US |
dc.contributor.author | Brethauer, D. | en_US |
dc.contributor.author | Chilingarian, I. V. | en_US |
dc.contributor.author | Coppejans, D. L. | en_US |
dc.contributor.author | Ducci, L. | en_US |
dc.contributor.author | Ferrigno, C. | en_US |
dc.contributor.author | Fong, W. | en_US |
dc.contributor.author | Götz, D. | en_US |
dc.contributor.author | Guidorzi, C. | en_US |
dc.contributor.author | Hajela, A. | en_US |
dc.contributor.author | Hurley, K. | en_US |
dc.contributor.author | Kuulkers, E. | en_US |
dc.contributor.author | Laurent, P. | en_US |
dc.contributor.author | MEREGHETTI, Sandro | en_US |
dc.contributor.author | Nicholl, M. | en_US |
dc.contributor.author | Patnaude, D. | en_US |
dc.contributor.author | Ubertini, P. | en_US |
dc.contributor.author | Banovetz, J. | en_US |
dc.contributor.author | Bartel, N. | en_US |
dc.contributor.author | Berger, E. | en_US |
dc.contributor.author | Coughlin, E. R. | en_US |
dc.contributor.author | Eftekhari, T. | en_US |
dc.contributor.author | Frederiks, D. D. | en_US |
dc.contributor.author | Kozlova, A. V. | en_US |
dc.contributor.author | Laskar, T. | en_US |
dc.contributor.author | Svinkin, D. S. | en_US |
dc.contributor.author | Drout, M. R. | en_US |
dc.contributor.author | MacFadyen, A. | en_US |
dc.contributor.author | Paterson, K. | en_US |
dc.date.accessioned | 2020-12-18T11:51:51Z | - |
dc.date.available | 2020-12-18T11:51:51Z | - |
dc.date.issued | 2019 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/29004 | - |
dc.description.abstract | We present the first extensive radio to γ-ray observations of a fast-rising blue optical transient, AT 2018cow, over its first ∼100 days. AT 2018cow rose over a few days to a peak luminosity L <SUB>pk</SUB> ∼ 4 × 10<SUP>44</SUP> erg s<SUP>-1</SUP>, exceeding that of superluminous supernovae (SNe), before declining as L ∝ t <SUP>-2</SUP>. Initial spectra at δt ≲ 15 days were mostly featureless and indicated large expansion velocities v ∼ 0.1c and temperatures reaching T ∼ 3 × 10<SUP>4</SUP> K. Later spectra revealed a persistent optically thick photosphere and the emergence of H and He emission features with v ∼ 4000 km s<SUP>-1</SUP> with no evidence for ejecta cooling. Our broadband monitoring revealed a hard X-ray spectral component at E ≥ 10 keV, in addition to luminous and highly variable soft X-rays, with properties unprecedented among astronomical transients. An abrupt change in the X-ray decay rate and variability appears to accompany the change in optical spectral properties. AT 2018cow showed bright radio emission consistent with the interaction of a blast wave with v <SUB>sh</SUB> ∼ 0.1c with a dense environment (\dot{M}∼ {10}<SUP>-3</SUP>-{10}<SUP>-4</SUP> {M}<SUB>☉ </SUB>{yr}}<SUP>-1</SUP> for v <SUB> w </SUB> = 1000 km s<SUP>-1</SUP>). While these properties exclude <SUP>56</SUP>Ni-powered transients, our multiwavelength analysis instead indicates that AT 2018cow harbored a “central engine,” either a compact object (magnetar or black hole) or an embedded internal shock produced by interaction with a compact, dense circumstellar medium. The engine released ∼10<SUP>50</SUP>-10<SUP>51.5</SUP> erg over ∼10<SUP>3</SUP>-10<SUP>5</SUP> s and resides within low-mass fast-moving material with equatorial-polar density asymmetry (M <SUB>ej,fast</SUB> ≲ 0.3 M <SUB>☉</SUB>). Successful SNe from low-mass H-rich stars (like electron-capture SNe) or failed explosions from blue supergiants satisfy these constraints. Intermediate-mass black holes are disfavored by the large environmental density probed by the radio observations. | en_US |
dc.language.iso | eng | en_US |
dc.title | An Embedded X-Ray Source Shines through the Aspherical AT 2018cow: Revealing the Inner Workings of the Most Luminous Fast-evolving Optical Transients | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/aafa01 | en_US |
dc.identifier.scopus | 2-s2.0-85062033314 | en_US |
dc.identifier.isi | 000458043400018 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/aafa01 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 872 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 18 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2019ApJ...872...18M | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.orcid | 0000-0003-3259-7801 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
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