Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

W. Li; X. Wang; J. Vinkó; J. Mo; G. Hosseinzadeh; D. J. Sand; J. Zhang; H. Lin; T. Zhang; L. Wang; J. Zhang; Z. Chen; D. Xiang; L. Rui; F. Huang; X. Li; X. Zhang; L. Li; E. Baron; J. M. Derkacy; X. Zhao; H. Sai; K. Zhang; L. Wang; D. A. Howell; C. McCully; I. Arcavi; S. Valenti; D. Hiramatsu; J. Burke; A. Rest; P. Garnavich; B. E. Tucker; G. Narayan; E. Shaya; S. Margheim; A. Zenteno; A. Villar; G. Dimitriadis; R. J. Foley; Y. C. Pan; D. A. Coulter; O. D. Fox; S. W. Jha; D. O. Jones; D. N. Kasen; C. D. Kilpatrick; A. L. Piro; A. G. Riess; C. Rojas-Bravo; B. J. Shappee; T. W.S. Holoien; K. Z. Stanek; M. R. Drout; K. Auchettl; C. S. Kochanek; J. S. Brown; S. Bose; D. Bersier; J. Brimacombe; P. Chen; S. Dong; S. Holmbo; J. A. Muñoz; R. L. Mutel; R. S. Post; J. L. Prieto; J. Shields; D. Tallon; T. A. Thompson; P. J. Vallely; S. Villanueva; S. J. Smartt; K. W. Smith; K. C. Chambers; H. A. Flewelling; M. E. Huber; E. A. Magnier; C. Z. Waters; A. S.B. Schultz; J. Bulger; T. B. Lowe; M. Willman; K. Sárneczky; A. Pál; J. C. 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; J. E. Andrews; N. Smith; C. Bilinski; P. J. Brown; J. Nordin; S. C. Williams; L. Galbany; J. Palmerio; I. M. Hook; C. Inserra; K. Maguire; Régis Cartier; A. Razza; C. P. Gutiérrez; J. J. Hermes; J. S. Reding; B. C. Kaiser; J. L. Tonry; A. N. Heinze; L. Denneau; H. Weiland; B. Stalder; G. Barentsen; J. Dotson; T. Barclay; M. Gully-Santiago; C. Hedges; A. M. Cody; S. Howell; J. Coughlin; J. E.Van Cleve; J. Vinícius De Miranda Cardoso; K. A. Larson; K. M. McCalmont-Everton; C. A. Peterson; S. E. Ross; L. H. 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; R. Gangopadhyay; R. Kloetzel; T. Weschler; V. Nystrom; J. Moffatt; M. Redick; K. Griest; M. Packard; M. Muszynski; J. Kampmeier; R. Bjella; S. Flynn; B. Elsaesser

doi:10.3847/1538-4357/aaec74

Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

W. Li, X. Wang, J. Vinkó, J. Mo, G. Hosseinzadeh, D. J. Sand, J. Zhang, H. Lin, T. Zhang, L. Wang, J. Zhang, Z. Chen, D. Xiang, L. Rui, F. Huang, X. Li, X. Zhang, L. Li, E. Baron, J. M. DerkacyX. Zhao, H. Sai, K. Zhang, L. Wang, D. A. Howell, C. McCully, I. Arcavi, S. Valenti, D. Hiramatsu, J. Burke, A. Rest, P. Garnavich, B. E. Tucker, G. Narayan, E. Shaya, S. Margheim, A. Zenteno, A. Villar, G. Dimitriadis, R. J. Foley, Y. C. Pan, D. A. Coulter, O. D. Fox, S. W. Jha, D. O. Jones, D. N. Kasen, C. D. Kilpatrick, A. L. Piro, A. G. Riess, C. Rojas-Bravo, B. J. Shappee, T. W.S. Holoien, K. Z. Stanek, M. R. Drout, K. Auchettl, C. S. Kochanek, J. S. Brown, S. Bose, D. Bersier, J. Brimacombe, P. Chen, S. Dong, S. Holmbo, J. A. Muñoz, R. L. Mutel, R. S. Post, J. L. Prieto, J. Shields, D. Tallon, T. A. Thompson, P. J. Vallely, S. Villanueva, S. J. Smartt, K. W. Smith, K. C. Chambers, H. A. Flewelling, M. E. Huber, E. A. Magnier, C. Z. Waters, A. S.B. Schultz, J. Bulger, T. B. Lowe, M. Willman, K. Sárneczky, A. Pál, J. C. 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, J. E. Andrews, N. Smith, C. Bilinski, P. J. Brown, J. Nordin, S. C. Williams, L. Galbany, J. Palmerio, I. M. Hook, C. Inserra, K. Maguire, Régis Cartier, A. Razza, C. P. Gutiérrez, J. J. Hermes, J. S. Reding, B. C. Kaiser, J. L. Tonry, A. N. Heinze, L. Denneau, H. Weiland, B. Stalder, G. Barentsen, J. Dotson, T. Barclay, M. Gully-Santiago, C. Hedges, A. M. Cody, S. Howell, J. Coughlin, J. E.Van Cleve, J. Vinícius De Miranda Cardoso, K. A. Larson, K. M. McCalmont-Everton, C. A. Peterson, S. E. Ross, L. H. 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, R. Gangopadhyay, R. Kloetzel, T. Weschler, V. Nystrom, J. Moffatt, M. Redick, K. Griest, M. Packard, M. Muszynski, J. Kampmeier, R. Bjella, S. Flynn, B. Elsaesser

CIERA - Center for Interdisciplinary Exploration and Research in Astrophysics

Research output: Contribution to journal › Article › peer-review

66 Scopus citations

Abstract

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 × 10⁴³ erg s^-1, from which we derive a nickel mass as 0.55 ± 0.04 M _o by fitting radiation diffusion models powered by centrally located ⁵⁶Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of ⁵⁶Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a nondegenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia but is characterized by prominent and persistent carbon absorption features. The C ii features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in an SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers.

Original language	English (US)
Article number	12
Journal	Astrophysical Journal
Volume	870
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/aaec74
State	Published - Jan 1 2019

Funding

This work includes data obtained with the Swope Telescope at Las Campanas Observatory, Chile, as part of the Swope Time Domain Key Project (PI: Piro; co-PIs: Shappee, Drout, Madore, Phillips, Foley, and Hsiao). We thank I. Thompson and the Carnegie Observatory Time Allocation Committee for approving the Swope project and scheduling this program. Parts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) through project number CE170100013. EB and JD acknowledge partial support from NASA grant NNX16AB5G. IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation (NSF). This work makes use of observations from Las Cumbres Observatory. DAH, CM, and GH are supported by the US National Science Foundation under grant 1313484. Support for IA was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. The work made use of Swift/ UVOT data reduced by P. J. Brown and released in the Swift Optical/Ultraviolet Supernova Archive (SOUSA). SOUSA is supported by NASA’s Astrophysics Data Analysis Program through grant NNX13AF35G. Research by DJS is supported by NSF grants AST-1821967, 1821987, 1813708, and 1813466. This paper includes data collected by the K2 mission. Funding for the K2 mission is provided by the NASA Science Mission directorate. KEGS is supported in part by NASA K2 cycle 4 and 5 grants NNX17AI64G and 80NSSC18K0302, respectively. AR and his groups are supported in part by HST grants GO-12577 and HST AR-12851. This work is supported by Ma Huateng Foundation. We acknowledge the support of the staff of the Lijiang 2.4 m and Xinglong 2.16 m telescopes. Funding for the LJT has been provided by Chinese Academy of Sciences and the People’s Government of Yunnan Province. The LJT is jointly operated and administrated by Yunnan Observatories and the Center for Astronomical Mega-Science, CAS. This work is supported by the National Natural Science Foundation of China (NSFC grants 11325313, 11633002, and 11761141001), the National Program on Key Research and Development Project (grant No. 2016YFA0400803), and the Tsinghua University Initiative Scientific Research Program (20161080144). This work was also partially supported by the Collaborating Research Program (OP201702) of the Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences. This work is sponsored (in part) by the Chinese Academy of Sciences (CAS) through a grant to the CAS South America Center for Astronomy (CASSACA) in Santiago, Chile. J-JZ is supported by the NSFC (grants 11403096 and 11773067), the Key Research Program of the CAS (grant No. KJZD-EW-M06), the Youth Innovation Promotion Association of the CAS (grant 2018081), and the CAS “Light of West China” Program. FH is supported by the Collaborating Research Program (OP201702) of the Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences. We thank the Las Cumbres Observatory and its staff for its continuing support of the ASAS-SN project. ASAS-SN is supported by the Gordon and Betty Moore Foundation through grant GBMF5490 to Ohio State University and NSF grant AST-1515927. Development of ASAS-SN has been supported by NSF grant AST-0908816, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics at Ohio State University, the Chinese Academy of Sciences South America Center for Astronomy (CASSACA), the Villum Foundation, and George Skestos. Based in part on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO program 199.D-0143. LG was supported in part by the US National Science Foundation under grant AST-1311862. KM acknowledges support from the STFC through an Ernest Rutherford Fellowship and EU Horizon 2020 ERC grant No. 758638. CPG acknowledges support from EU/FP7-ERC grant No. [615929]. JV and his group at Konkoly Observatory are supported by the project “Transient Astrophysical Objects” GINOP 2.3.2-15-2016-00033 of the National Research, Development and Innovation Office (NKFIH), Hungary, funded by the European Union, and by the “Lendület” Program of the Hungarian Academy of Sciences, project Nos. LP2012-31 and LP2018-7/ 2018. This project has been supported by NKFIH grant K-115709. ZsB acknowledges the support provided by the National Research, Development and Innovation Fund of Hungary, financed under the PD_17 funding scheme, project No. PD123910. Support for JJH was provided by NASA through Hubble Fellowship grant #HST-HF2-51357.001-A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555, as well as NASA K2 Cycle 4 grant NNX17AE92G. SB, PC, and SD acknowledge Project 11573003, supported by NSFC. This research uses data obtained through the Telescope Access Program (TAP), which has been funded by the Strategic Priority Research Program–The Emergence of Cosmological Structures of the Chinese Academy of Sciences (grant No. 11 XDB09000000) and the Special Fund for Astronomy from the Ministry of Finance. The UCSC group is supported in part by NASA grants NNG17PX03C and 80NSSC18K0303, NSF grant AST-1518052, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation, and fellowships from the Alfred P. Sloan Foundation and the David and Lucile Packard Foundation to RJF.

Keywords

supernovae: general
supernovae: individual (SN 2018oh)

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.3847/1538-4357/aaec74

Cite this

Li, W., Wang, X., Vinkó, J., Mo, J., Hosseinzadeh, G., Sand, D. J., Zhang, J., Lin, H., Zhang, T., Wang, L., Zhang, J., Chen, Z., Xiang, D., Rui, L., Huang, F., Li, X., Zhang, X., Li, L., Baron, E., ... Elsaesser, B. (2019). Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations. Astrophysical Journal, 870(1), Article 12. https://doi.org/10.3847/1538-4357/aaec74

@article{b6f4e27425744013b2ea441169cd17c4,

title = "Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations",

abstract = "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 × 1043 erg s-1, from which we derive a nickel mass as 0.55 ± 0.04 M o by fitting radiation diffusion models powered by centrally located 56Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of 56Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a nondegenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia but is characterized by prominent and persistent carbon absorption features. The C ii features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in an SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers.",

keywords = "supernovae: general, supernovae: individual (SN 2018oh)",

author = "W. Li and X. Wang and J. Vink{\'o} and J. Mo and G. Hosseinzadeh and Sand, {D. J.} and J. Zhang and H. Lin and T. Zhang and L. Wang and J. Zhang and Z. Chen and D. Xiang and L. Rui and F. Huang and X. Li and X. Zhang and L. Li and E. Baron and Derkacy, {J. M.} and X. Zhao and H. Sai and K. Zhang and L. Wang and Howell, {D. A.} and C. McCully and I. Arcavi and S. Valenti and D. Hiramatsu and J. Burke and A. Rest and P. Garnavich and Tucker, {B. E.} and G. Narayan and E. Shaya and S. Margheim and A. Zenteno and A. Villar and G. Dimitriadis and Foley, {R. J.} and Pan, {Y. C.} and Coulter, {D. A.} and Fox, {O. D.} and Jha, {S. W.} and Jones, {D. O.} and Kasen, {D. N.} and Kilpatrick, {C. D.} and Piro, {A. L.} and Riess, {A. G.} and C. Rojas-Bravo and Shappee, {B. J.} and Holoien, {T. W.S.} and Stanek, {K. Z.} and Drout, {M. R.} and K. Auchettl and Kochanek, {C. S.} and Brown, {J. S.} and S. Bose and D. Bersier and J. Brimacombe and P. Chen and S. Dong and S. Holmbo and Mu{\~n}oz, {J. A.} and Mutel, {R. L.} and Post, {R. S.} and Prieto, {J. L.} and J. Shields and D. Tallon and Thompson, {T. A.} and Vallely, {P. J.} and S. Villanueva and Smartt, {S. J.} and Smith, {K. W.} and Chambers, {K. C.} and Flewelling, {H. A.} and Huber, {M. E.} and Magnier, {E. A.} and Waters, {C. Z.} and Schultz, {A. S.B.} and J. Bulger and Lowe, {T. B.} and M. Willman and K. S{\'a}rneczky and A. P{\'a}l and Wheeler, {J. C.} and A. B{\'o}di and Zs Bogn{\'a}r and B. Cs{\'a}k and B. Cseh and G. Cs{\"o}rnyei and O. Hanyecz and B. Ign{\'a}cz and Cs Kalup and R. K{\"o}nyves-T{\'o}th and L. Kriskovics and A. Ordasi and I. Rajmon and A. S{\'o}dor and R. Szab{\'o} and R. Szak{\'a}ts and G. Zsidi and P. Milne and Andrews, {J. E.} and N. Smith and C. Bilinski and Brown, {P. J.} and J. Nordin and Williams, {S. C.} and L. Galbany and J. Palmerio and Hook, {I. M.} and C. Inserra and K. Maguire and R{\'e}gis Cartier and A. Razza and Guti{\'e}rrez, {C. P.} and Hermes, {J. J.} and Reding, {J. S.} and Kaiser, {B. C.} and Tonry, {J. L.} and Heinze, {A. N.} and L. Denneau and H. Weiland and B. Stalder and G. Barentsen and J. Dotson and T. Barclay and M. Gully-Santiago and C. Hedges and Cody, {A. M.} and S. Howell and J. Coughlin and Cleve, {J. E.Van} and {Vin{\'i}cius De Miranda Cardoso}, J. and Larson, {K. A.} and McCalmont-Everton, {K. M.} and Peterson, {C. A.} and Ross, {S. E.} and Reedy, {L. H.} and D. Osborne and C. McGinn and L. Kohnert and L. Migliorini and A. Wheaton and B. Spencer and C. Labonde and G. Castillo and G. Beerman and K. Steward and M. Hanley and R. Larsen and R. Gangopadhyay and R. Kloetzel and T. Weschler and V. Nystrom and J. Moffatt and M. Redick and K. Griest and M. Packard and M. Muszynski and J. Kampmeier and R. Bjella and S. Flynn and B. Elsaesser",

year = "2019",

month = jan,

day = "1",

doi = "10.3847/1538-4357/aaec74",

language = "English (US)",

volume = "870",

journal = "Astrophysical Journal",

issn = "0004-637X",

number = "1",

}

Li, W, Wang, X, Vinkó, J, Mo, J, Hosseinzadeh, G, Sand, DJ, Zhang, J, Lin, H, Zhang, T, Wang, L, Zhang, J, Chen, Z, Xiang, D, Rui, L, Huang, F, Li, X, Zhang, X, Li, L, Baron, E, Derkacy, JM, Zhao, X, Sai, H, Zhang, K, Wang, L, Howell, DA, McCully, C, Arcavi, I, Valenti, S, Hiramatsu, D, Burke, J, Rest, A, Garnavich, P, Tucker, BE, Narayan, G, Shaya, E, Margheim, S, Zenteno, A, Villar, A, Dimitriadis, G, Foley, RJ, Pan, YC, Coulter, DA, Fox, OD, Jha, SW, Jones, DO, Kasen, DN, Kilpatrick, CD, Piro, AL, Riess, AG, Rojas-Bravo, C, Shappee, BJ, Holoien, TWS, Stanek, KZ, Drout, MR, Auchettl, K, Kochanek, CS, Brown, JS, Bose, S, Bersier, D, Brimacombe, J, Chen, P, Dong, S, Holmbo, S, Muñoz, JA, Mutel, RL, Post, RS, Prieto, JL, Shields, J, Tallon, D, Thompson, TA, Vallely, PJ, Villanueva, S, Smartt, SJ, Smith, KW, Chambers, KC, Flewelling, HA, Huber, ME, Magnier, EA, Waters, CZ, Schultz, ASB, Bulger, J, Lowe, TB, Willman, M, Sárneczky, K, Pál, A, Wheeler, JC, Bódi, A, Bognár, Z, Csák, B, Cseh, B, Csörnyei, G, Hanyecz, O, Ignácz, B, Kalup, C, Könyves-Tóth, R, Kriskovics, L, Ordasi, A, Rajmon, I, Sódor, A, Szabó, R, Szakáts, R, Zsidi, G, Milne, P, Andrews, JE, Smith, N, Bilinski, C, Brown, PJ, Nordin, J, Williams, SC, Galbany, L, Palmerio, J, Hook, IM, Inserra, C, Maguire, K, Cartier, R, Razza, A, Gutiérrez, CP, Hermes, JJ, Reding, JS, Kaiser, BC, Tonry, JL, Heinze, AN, Denneau, L, Weiland, H, Stalder, B, Barentsen, G, Dotson, J, Barclay, T, Gully-Santiago, M, Hedges, C, Cody, AM, Howell, S, Coughlin, J, Cleve, JEV, Vinícius De Miranda Cardoso, J, Larson, KA, McCalmont-Everton, KM, Peterson, CA, Ross, SE, Reedy, LH, Osborne, D, McGinn, C, Kohnert, L, Migliorini, L, Wheaton, A, Spencer, B, Labonde, C, Castillo, G, Beerman, G, Steward, K, Hanley, M, Larsen, R, Gangopadhyay, R, Kloetzel, R, Weschler, T, Nystrom, V, Moffatt, J, Redick, M, Griest, K, Packard, M, Muszynski, M, Kampmeier, J, Bjella, R, Flynn, S & Elsaesser, B 2019, 'Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations', Astrophysical Journal, vol. 870, no. 1, 12. https://doi.org/10.3847/1538-4357/aaec74

TY - JOUR

T1 - Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

AU - Li, W.

AU - Wang, X.

AU - Vinkó, J.

AU - Mo, J.

AU - Hosseinzadeh, G.

AU - Sand, D. J.

AU - Zhang, J.

AU - Lin, H.

AU - Zhang, T.

AU - Wang, L.

AU - Zhang, J.

AU - Chen, Z.

AU - Xiang, D.

AU - Rui, L.

AU - Huang, F.

AU - Li, X.

AU - Zhang, X.

AU - Li, L.

AU - Baron, E.

AU - Derkacy, J. M.

AU - Zhao, X.

AU - Sai, H.

AU - Zhang, K.

AU - Wang, L.

AU - Howell, D. A.

AU - McCully, C.

AU - Arcavi, I.

AU - Valenti, S.

AU - Hiramatsu, D.

AU - Burke, J.

AU - Rest, A.

AU - Garnavich, P.

AU - Tucker, B. E.

AU - Narayan, G.

AU - Shaya, E.

AU - Margheim, S.

AU - Zenteno, A.

AU - Villar, A.

AU - Dimitriadis, G.

AU - Foley, R. J.

AU - Pan, Y. C.

AU - Coulter, D. A.

AU - Fox, O. D.

AU - Jha, S. W.

AU - Jones, D. O.

AU - Kasen, D. N.

AU - Kilpatrick, C. D.

AU - Piro, A. L.

AU - Riess, A. G.

AU - Rojas-Bravo, C.

AU - Shappee, B. J.

AU - Holoien, T. W.S.

AU - Stanek, K. Z.

AU - Drout, M. R.

AU - Auchettl, K.

AU - Kochanek, C. S.

AU - Brown, J. S.

AU - Bose, S.

AU - Bersier, D.

AU - Brimacombe, J.

AU - Chen, P.

AU - Dong, S.

AU - Holmbo, S.

AU - Muñoz, J. A.

AU - Mutel, R. L.

AU - Post, R. S.

AU - Prieto, J. L.

AU - Shields, J.

AU - Tallon, D.

AU - Thompson, T. A.

AU - Vallely, P. J.

AU - Villanueva, S.

AU - Smartt, S. J.

AU - Smith, K. W.

AU - Chambers, K. C.

AU - Flewelling, H. A.

AU - Huber, M. E.

AU - Magnier, E. A.

AU - Waters, C. Z.

AU - Schultz, A. S.B.

AU - Bulger, J.

AU - Lowe, T. B.

AU - Willman, M.

AU - Sárneczky, K.

AU - Pál, A.

AU - Wheeler, J. C.

AU - Bódi, A.

AU - Bognár, Zs

AU - Csák, B.

AU - Cseh, B.

AU - Csörnyei, G.

AU - Hanyecz, O.

AU - Ignácz, B.

AU - Kalup, Cs

AU - Könyves-Tóth, R.

AU - Kriskovics, L.

AU - Ordasi, A.

AU - Rajmon, I.

AU - Sódor, A.

AU - Szabó, R.

AU - Szakáts, R.

AU - Zsidi, G.

AU - Milne, P.

AU - Andrews, J. E.

AU - Smith, N.

AU - Bilinski, C.

AU - Brown, P. J.

AU - Nordin, J.

AU - Williams, S. C.

AU - Galbany, L.

AU - Palmerio, J.

AU - Hook, I. M.

AU - Inserra, C.

AU - Maguire, K.

AU - Cartier, Régis

AU - Razza, A.

AU - Gutiérrez, C. P.

AU - Hermes, J. J.

AU - Reding, J. S.

AU - Kaiser, B. C.

AU - Tonry, J. L.

AU - Heinze, A. N.

AU - Denneau, L.

AU - Weiland, H.

AU - Stalder, B.

AU - Barentsen, G.

AU - Dotson, J.

AU - Barclay, T.

AU - Gully-Santiago, M.

AU - Hedges, C.

AU - Cody, A. M.

AU - Howell, S.

AU - Coughlin, J.

AU - Cleve, J. E.Van

AU - Vinícius De Miranda Cardoso, J.

AU - Larson, K. A.

AU - McCalmont-Everton, K. M.

AU - Peterson, C. A.

AU - Ross, S. E.

AU - Reedy, L. H.

AU - Osborne, D.

AU - McGinn, C.

AU - Kohnert, L.

AU - Migliorini, L.

AU - Wheaton, A.

AU - Spencer, B.

AU - Labonde, C.

AU - Castillo, G.

AU - Beerman, G.

AU - Steward, K.

AU - Hanley, M.

AU - Larsen, R.

AU - Gangopadhyay, R.

AU - Kloetzel, R.

AU - Weschler, T.

AU - Nystrom, V.

AU - Moffatt, J.

AU - Redick, M.

AU - Griest, K.

AU - Packard, M.

AU - Muszynski, M.

AU - Kampmeier, J.

AU - Bjella, R.

AU - Flynn, S.

AU - Elsaesser, B.

PY - 2019/1/1

Y1 - 2019/1/1

N2 - 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 × 1043 erg s-1, from which we derive a nickel mass as 0.55 ± 0.04 M o by fitting radiation diffusion models powered by centrally located 56Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of 56Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a nondegenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia but is characterized by prominent and persistent carbon absorption features. The C ii features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in an SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers.

AB - 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 × 1043 erg s-1, from which we derive a nickel mass as 0.55 ± 0.04 M o by fitting radiation diffusion models powered by centrally located 56Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of 56Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a nondegenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia but is characterized by prominent and persistent carbon absorption features. The C ii features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in an SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers.

KW - supernovae: general

KW - supernovae: individual (SN 2018oh)

UR - http://www.scopus.com/inward/record.url?scp=85059872177&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85059872177&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/aaec74

DO - 10.3847/1538-4357/aaec74

M3 - Article

AN - SCOPUS:85059872177

SN - 0004-637X

VL - 870

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 12

ER -

Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

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