WFRF:(Bilinski Christopher)
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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 04168naa a2200649 4500 | |
| 001 | oai:DiVA.org:su-159008 | |
| 003 | SwePub | |
| 008 | 180910s2018 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1590082 URI |
| 024 | 7 | a https://doi.org/10.3847/1538-4357/aacb352 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 Bose, Subhash4 aut |
| 245 | 1 0 | a ASASSN-15nx :b A Luminous Type II Supernova with a Perfect Linear Decline |
| 264 | c 2018-07-27 | |
| 264 | 1 | b American Astronomical Society,c 2018 |
| 338 | a print2 rdacarrier | |
| 520 | a We report a luminous Type II supernova, ASASSN-15nx, with a peak luminosity of M-v = -20 mag that is between those of typical core-collapse supernovae and super-luminous supernovae. The post-peak optical light curves show a long, linear decline with a steep slope of 2.5 mag (100 day)(-1) (i.e., an exponential decline in flux) through the end of observations at phase approximate to 260 day. In contrast, the light curves of hydrogen-rich supernovae (SNe II-P/L) always show breaks in their light curves at phase similar to 100 day, before settling onto Co-56 radioactive decay tails with a decline rate of about 1 mag (100 day)(-1). The spectra of ASASSN-15nx do not exhibit the narrow emission-line features characteristic of Type IIn SNe, which can have a wide variety of light-curve shapes usually attributed to strong interactions with a dense circumstellar medium (CSM). ASASSN-15nx has a number of spectroscopic peculiarities, including a relatively weak and triangular-shaped H alpha emission profile with no absorption component. The physical origin of these peculiarities is unclear, but the long and linear post-peak light curve without a break suggests a single dominant powering mechanism. Decay of a large amount of Ni-56 (M-Ni = 1.6 +/- 0.2 M-circle dot) can power the light curve of ASASSN-15nx, and the steep light-curve slope requires substantial gamma-ray escape from the ejecta, which is possible given a low-mass hydrogen envelope for the progenitor. Another possibility is strong CSM interactions powering the light curve, but the CSM needs to be sculpted to produce the unique light-curve shape and avoid producing SN IIn-like narrow emission lines. | |
| 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 |
| 653 | a supernovae: general | |
| 653 | a supernovae: individual (ASASSN-15nx) | |
| 700 | 1 | a Dong, Subo4 aut |
| 700 | 1 | a Kochanek, C. S.4 aut |
| 700 | 1 | a Pastorello, Andrea4 aut |
| 700 | 1 | a Katz, Boaz4 aut |
| 700 | 1 | a Bersier, David4 aut |
| 700 | 1 | a Andrews, Jennifer E.4 aut |
| 700 | 1 | a Prieto, J. L.4 aut |
| 700 | 1 | a Stanek, K. Z.4 aut |
| 700 | 1 | a Shappee, B. J.4 aut |
| 700 | 1 | a Smith, Nathan4 aut |
| 700 | 1 | a Kollmeier, Juna4 aut |
| 700 | 1 | a Benetti, Stefano4 aut |
| 700 | 1 | a Cappellaro, E.4 aut |
| 700 | 1 | a Chen, Ping4 aut |
| 700 | 1 | a Elias-Rosa, N.4 aut |
| 700 | 1 | a Milne, Peter4 aut |
| 700 | 1 | a Morales-Garoffolo, Antonia4 aut |
| 700 | 1 | a Tartaglia, Leonardou Stockholms universitet,Institutionen för astronomi,Oskar Klein-centrum för kosmopartikelfysik (OKC)4 aut0 (Swepub:su)leta1160 |
| 700 | 1 | a Tomasella, L.4 aut |
| 700 | 1 | a Bilinski, Christopher4 aut |
| 700 | 1 | a Brimacombe, Joseph4 aut |
| 700 | 1 | a Frank, Stephan4 aut |
| 700 | 1 | a Holoien, T. W. -S.4 aut |
| 700 | 1 | a Kilpatrick, Charles D.4 aut |
| 700 | 1 | a Kiyota, Seiichiro4 aut |
| 700 | 1 | a Madore, Barry F.4 aut |
| 700 | 1 | a Rich, Jeffrey A.4 aut |
| 710 | 2 | a Stockholms universitetb Institutionen för astronomi4 org |
| 773 | 0 | t Astrophysical Journald : American Astronomical Societyg 862:2q 862:2x 0004-637Xx 1538-4357 |
| 856 | 4 | u https://arxiv.org/pdf/1804.00025.pdf |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-159008 |
| 856 | 4 8 | u https://doi.org/10.3847/1538-4357/aacb35 |
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