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

School of Physics and Astronomy

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

71 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
Article number	12
Journal	Astrophysical Journal
Volume	870
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/aaec74
State	Published - 1 Jan 2019

Funding

Funders	Funder number
People's Government of Yunnan Province
Ma Huateng Foundation
National Optical Astronomy Observatories
Mt. Cuba Astronomical Foundation
Villum Fonden
Chinese Academy of Sciences South America Center for Astronomy
Ministry of Finance
Ohio State University
Australian Research Council Centre of Excellence
Nemzeti Kutatási Fejlesztési és Innovációs Hivatal
EU Horizon 2020 ERC
European Commission
Heising-Simons Foundation
Alfred P. Sloan Foundation
David and Lucile Packard Foundation
EU/FP7-ERC
National Research, Development and Innovation Office
National Science Foundation	1813466, 0908816, 1821987, AST-1821967, 1813176, 1821967, 1313484, AST-1518052, 1817099, 1311862, AST-1515927, 1515927, 1815935, 1813708
Space Telescope Science Institute	NAS5-26555, NNX17AE92G
Seventh Framework Programme	615929
Gordon and Betty Moore Foundation	GBMF5490
Australian Research Council	CE170100013
National Aeronautics and Space Administration	NNX17AI64G, 80NSSC18K0303, 80NSSC18K0302, NNG17PX03C, PF6-170148, NNX13AF35G, HST AR-12851, GO-12577, #HST-HF2-51357.001-A, NNX16AB5G
Chinese Academy of Sciences	11 XDB09000000
Fundação para a Ciência e a Tecnologia	Incentivo/SAU/LA0001/2013
Science and Technology Facilities Council	ST/J001465/1
Tsinghua University	20161080144
National Program on Key Research and Development Project	2016YFA0400803
Key Research Program of the CAS	KJZD-EW-M06
National Natural Science Foundation of China	11325313, 11633002, 11761141001
National Research, Development and Innovation Fund of Hungary	PD123910
Youth Innovation Promotion Association of the Chinese Academy of Sciences	2018081
Magyar Tudományos Akadémia	LP2012-31, K-115709, LP2018-7/ 2018
Horizon 2020 Framework Programme	758638
CAS South America Center for Astronomy	11403096, 11773067
Collaborating Research Program	OP201702

Keywords

supernovae: general
supernovae: individual (SN 2018oh)

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{73a3883b469f4c9099021ae9205dd579,

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 = "אנגלית",

volume = "870",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

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 - https://www.scopus.com/pages/publications/85059872177

U2 - 10.3847/1538-4357/aaec74

DO - 10.3847/1538-4357/aaec74

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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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