Authors
W Li, X Wang, József Vinkó, J Mo, G Hosseinzadeh, DJ Sand, J Zhang, H Lin, T Zhang, L Wang, Z Chen, D Xiang, L Rui, F Huang, X Li, X Zhang, L Li, E Baron, JM Derkacy, X Zhao, H Sai, K Zhang, DA Howell, C McCully, I Arcavi, S Valenti, D Hiramatsu, J Burke, A Rest, P Garnavich, BE Tucker, G Narayan, E Shaya, S Margheim, A Zenteno, A Villar, G Dimitriadis, RJ Foley, Y-C Pan, DA Coulter, OD Fox, SW Jha, DO Jones, DN Kasen, CD Kilpatrick, AL Piro, AG Riess, C Rojas-Bravo, BJ Shappee, TW-S Holoien, KZ Stanek, MR Drout, K Auchettl, CS Kochanek, JS Brown, S Bose, D Bersier, J Brimacombe, P Chen, S Dong, S Holmbo, JA Muñoz, RL Mutel, RS Post, JL Prieto, J Shields, D Tallon, TA Thompson, PJ Vallely, S Villanueva, SJ Smartt, KW Smith, KC Chambers, HA Flewelling, ME Huber, EA Magnier, CZ Waters, ASB Schultz, J Bulger, TB Lowe, M Willman, K Sárneczky, A Pál, JC Wheeler, A Bódi, Zs Bognár, B Csák, B Cseh, G Csörnyei, O Hanyecz, B Ignácz, Cs Kalup, R Könyves-Tóth, L Kriskovics, A Ordasi, I Rajmon, A Sódor, R Szabó, R Szakáts, G Zsidi, P Milne, JE Andrews, N Smith, C Bilinski, PJ Brown, J Nordin, SC Williams, Lluis Galbany, J Palmerio, IM Hook, C Inserra, K Maguire, Régis Cartier, A Razza, CP Gutiérrez, JJ Hermes, JS Reding, BC Kaiser, JL Tonry, AN Heinze, L Denneau, H Weiland, B Stalder, G Barentsen, J Dotson, T Barclay, M Gully-Santiago, C Hedges, AM Cody, S Howell, J Coughlin, JE Van Cleve, J Vinícius de Miranda Cardoso, KA Larson, KM McCalmont-Everton, CA Peterson, SE Ross, LH Reedy, D Osborne, C McGinn, L Kohnert, L Migliorini, A Wheaton, B Spencer, C Labonde, G Castillo, G Beerman, K Steward, M Hanley, R Larsen
Publication date
2018/12/28
Journal
The Astrophysical Journal
Volume
870
Issue
1
Pages
12
Publisher
IOP Publishing
Description
Supernova (SN) 2018oh (ASASSN-18bt) is the first spectroscopically confirmed Type Ia supernova (SN Ia) observed in the Kepler field. The Kepler data revealed an excess emission in its early light curve, allowing us to place interesting constraints on its progenitor system. Here we present extensive optical, ultraviolet, and near-infrared photometry, as well as dense sampling of optical spectra, for this object. SN 2018oh is relatively normal in its photometric evolution, with a rise time of 18.3±0.3 days and Δm 15 (B)= 0.96±0.03 mag, but it seems to have bluer B− V colors. We construct the" UVOIR" bolometric light curve having a peak luminosity of 1.49× 10 43 erg s− 1, from which we derive a nickel mass as 0.55±0.04 M⊙ by fitting radiation diffusion models powered by centrally located 56 Ni. Note that the moment when nickel-powered luminosity starts to emerge is+ 3.85 days after the first light in the Kepler data …
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