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LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00004744naa a2200697 4500
001oai:DiVA.org:su-215789
003SwePub
008230331s2023 | |||||||||||000 ||eng|
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-2157892 URI
0247 a https://doi.org/10.1093/mnras/stac34772 DOI
040 a (SwePub)su
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Yang (杨轶), Yi4 aut
2451 0a The interaction of supernova 2018evt with a substantial amount of circumstellar matter – An SN 1997cy-like event
264 c 2022-11-28
264 1b Oxford University Press (OUP),c 2023
338 a print2 rdacarrier
520 a A rare class of supernovae (SNe) is characterized by strong interaction between the ejecta and several solar masses of circumstellar matter (CSM) as evidenced by strong Balmer-line emission. Within the first few weeks after the explosion, they may display spectral features similar to overluminous Type Ia SNe, while at later phase their observation properties exhibit remarkable similarities with some extreme case of Type IIn SNe that show strong Balmer lines years after the explosion. We present polarimetric observations of SN 2018evt obtained by the ESO Very Large Telescope from 172 to 219 d after the estimated time of peak luminosity to study the geometry of the CSM. The non-zero continuum polarization decreases over time, suggesting that the mass-loss of the progenitor star is aspherical. The prominent H α emission can be decomposed into a broad, time-evolving component and an intermediate-width, static component. The former shows polarized signals, and it is likely to arise from a cold dense shell (CDS) within the region between the forward and reverse shocks. The latter is significantly unpolarized, and it is likely to arise from shocked, fragmented gas clouds in the H-rich CSM. We infer that SN 2018evt exploded inside a massive and aspherical circumstellar cloud. The symmetry axes of the CSM and the SN appear to be similar. SN 2018evt shows observational properties common to events that display strong interaction between the ejecta and CSM, implying that they share similar circumstellar configurations. Our preliminary estimate also suggests that the circumstellar environment of SN 2018evt has been significantly enriched at a rate of ∼0.1 M⊙ yr−1 over a period of >100 yr. 
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
653 a polarization
653 a circumstellar matter
653 a supernovae: individual (SN2018evt)
7001 a Baade, Dietrich4 aut
7001 a Hoeflich, Peter4 aut
7001 a Wang, Lifan4 aut
7001 a Cikota, Aleksandar4 aut
7001 a Chen, Ting-Wanu Stockholms universitet,Institutionen för astronomi,Oskar Klein-centrum för kosmopartikelfysik (OKC),Max-Planck-Institut für Extraterrestrische Physik, Germany4 aut0 (Swepub:su)jach1916
7001 a Burke, Jamison4 aut
7001 a Hiramatsu, Daichi4 aut
7001 a Pellegrino, Craig4 aut
7001 a Howell, D. Andrew4 aut
7001 a McCully, Curtis4 aut
7001 a Valenti, Stefano4 aut
7001 a Schulze, Steveu Stockholms universitet,Oskar Klein-centrum för kosmopartikelfysik (OKC),Fysikum,Weizmann Institute of Science, Israel4 aut0 (Swepub:su)stsc6413
7001 a Gal-Yam, Avishay4 aut
7001 a Wang, Lingzhi4 aut
7001 a Filippenko, Alexei V.4 aut
7001 a Maeda, Keiichi4 aut
7001 a Bulla, Mattiau Stockholms universitet,Institutionen för astronomi,Oskar Klein-centrum för kosmopartikelfysik (OKC)4 aut0 (Swepub:su)mbull
7001 a Yao, Yuhan4 aut
7001 a Maund, Justyn R.4 aut
7001 a Patat, Ferdinando4 aut
7001 a Spyromilio, Jason4 aut
7001 a Wheeler, J. Craig4 aut
7001 a Rau, Arne4 aut
7001 a Hu, Lei4 aut
7001 a Li, Wenxiong4 aut
7001 a Andrews, Jennifer E.4 aut
7001 a Galbany, Llúis4 aut
7001 a Sand, David J.4 aut
7001 a Shahbandeh, Melissa4 aut
7001 a Hsiao, Eric Y.4 aut
7001 a Wang, Xiaofeng4 aut
7102 a Stockholms universitetb Institutionen för astronomi4 org
7730 t Monthly notices of the Royal Astronomical Societyd : Oxford University Press (OUP)g 519:2, s. 1618-1647q 519:2<1618-1647x 0035-8711x 1365-2966
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-215789
8564 8u https://doi.org/10.1093/mnras/stac3477

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