WFRF:(Kann D.A.)
Sökning: WFRF:(Kann D.A.) > The Peculiar Short-...
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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 04061naa a2200697 4500 | |
| 001 | oai:DiVA.org:su-207106 | |
| 003 | SwePub | |
| 008 | 220707s2022 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-2071062 URI |
| 024 | 7 | a https://doi.org/10.3847/1538-4357/ac60a22 DOI |
| 040 | a (SwePub)su | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a ref2 swepub-contenttype |
| 072 | 7 | a art2 swepub-publicationtype |
| 100 | 1 | a Rossi, A.4 aut |
| 245 | 1 0 | a The Peculiar Short-duration GRB 200826A and Its Supernova |
| 264 | c 2022-06-08 | |
| 264 | 1 | b American Astronomical Society,c 2022 |
| 338 | a print2 rdacarrier | |
| 520 | a Gamma-ray bursts (GRBs) are classified into long and short events. Long GRBs (LGRBs) are associated with the end states of very massive stars, while short GRBs (SGRBs) are linked to the merger of compact objects. GRB 200826A was a peculiar event, because by definition it was an SGRB, with a rest-frame duration of similar to 0.5 s. However, this event was energetic and soft, which is consistent with LGRBs. The relatively low redshift (z = 0.7486) motivated a comprehensive, multiwavelength follow-up campaign to characterize its host, search for a possible associated supernova (SN), and thus understand the origin of this burst. To this aim we obtained a combination of deep near-infrared (NIR) and optical imaging together with spectroscopy. Our analysis reveals an optical and NIR bump in the light curve whose luminosity and evolution are in agreement with several SNe associated to LGRBs. Analysis of the prompt GRB shows that this event follows the E-p,E-i-E-iso relation found for LGRBs. The host galaxy is a low-mass star-forming galaxy, typical of LGRBs, but with one of the highest star formation rates, especially with respect to its mass (log M-*/M-circle dot = 8.6, SFR similar to 4.0 M-circle dot yr(-1)). We conclude that GRB 200826A is a typical collapsar event in the low tail of the duration distribution of LGRBs. These findings support theoretical predictions that events produced by collapsars can be as short as 0.5 s in the host frame and further confirm that duration alone is not an efficient discriminator for the progenitor class of a GRB. | |
| 650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
| 700 | 1 | a Rothberg, B.4 aut |
| 700 | 1 | a Palazzi, E.4 aut |
| 700 | 1 | a Kann, D. A.4 aut |
| 700 | 1 | a D'Avanzo, P.4 aut |
| 700 | 1 | a Amati, L.4 aut |
| 700 | 1 | a Klose, S.4 aut |
| 700 | 1 | a Perego, A.4 aut |
| 700 | 1 | a Pian, E.4 aut |
| 700 | 1 | a Guidorzi, C.4 aut |
| 700 | 1 | a Pozanenko, A. S.4 aut |
| 700 | 1 | a Savaglio, S.4 aut |
| 700 | 1 | a Stratta, G.4 aut |
| 700 | 1 | a Agapito, G.4 aut |
| 700 | 1 | a Covino, S.4 aut |
| 700 | 1 | a Cusano, F.4 aut |
| 700 | 1 | a D'Elia, V.4 aut |
| 700 | 1 | a De Pasquale, M.4 aut |
| 700 | 1 | a Della Valle, M.4 aut |
| 700 | 1 | a Kuhn, O.4 aut |
| 700 | 1 | a Izzo, L.4 aut |
| 700 | 1 | a Loffredo, E.4 aut |
| 700 | 1 | a Masetti, N.4 aut |
| 700 | 1 | a Melandri, A.4 aut |
| 700 | 1 | a Minaev, P. Y.4 aut |
| 700 | 1 | a Nicuesa Guelbenzu, A.4 aut |
| 700 | 1 | a Paris, D.4 aut |
| 700 | 1 | a Paiano, S.4 aut |
| 700 | 1 | a Plantet, C.4 aut |
| 700 | 1 | a Rossi, F.4 aut |
| 700 | 1 | a Salvaterra, R.4 aut |
| 700 | 1 | a Schulze, Steveu Stockholms universitet,Oskar Klein-centrum för kosmopartikelfysik (OKC),Fysikum4 aut0 (Swepub:su)stsc6413 |
| 700 | 1 | a Veillet, C.4 aut |
| 700 | 1 | a Volnova, A. A.4 aut |
| 710 | 2 | a Stockholms universitetb Oskar Klein-centrum för kosmopartikelfysik (OKC)4 org |
| 773 | 0 | t Astrophysical Journald : American Astronomical Societyg 932:1q 932:1x 0004-637Xx 1538-4357 |
| 856 | 4 | u https://doi.org/10.3847/1538-4357/ac60a2y Fulltext |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-207106 |
| 856 | 4 8 | u https://doi.org/10.3847/1538-4357/ac60a2 |
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