PMO OpenIR
K2 Observations of SN 2018oh Reveal a Two-component Rising Light Curve for a Type Ia Supernova
Dimitriadis, G.1; Foley, R. J.1; Rest, A.2,3; Kasen, D.4,5; Piro, A. L.6; Polin, A.4,7; Jones, D. O.1; Villar, A.8; Narayan, G.3; Coulter, D. A.1; Kilpatrick, C. D.1; Pan, Y. -C.1; Rojas-Bravo, C.1; Fox, O. D.2; Jha, S. W.9; Nugent, P. E.4,7; Riess, A. G.2,3; Scolnic, D.10; Drout, M. R.6; Barentsen, G.11,12; Dotson, J.11; Gully-Santiago, M.11,12; Hedges, C.11,12; Cody, A. M.11,12; Barclay, T.13,14; Howell, S.11; Garnavich, P.15; Tucker, B. E.16,17,18; Shaya, E.19; Mushotzky, R.19; Olling, R. P.19; Margheim, S.20; Zenteno, A.21; Coughlin, J.; Van Cleve, J. E.11,22; Vinicius de Miranda Cardoso, J.11,23; Larson, K. A.24; McCalmont-Everton, K. M.24; Peterson, C. A.24; Ross, S. E.24; Reedy, L. H.25; Osborne, D.25; McGinn, C.25; Kohnert, L.25; Migliorini, L.25; Wheaton, A.25; Spencer, B.25; Labonde, C.25; Castillo, G.25; Beerman, G.25; Steward, K.25; Hanley, M.25; Larsen, R.25; Gangopadhyay, R.25; Kloetzel, R.25; Weschler, T.25; Nystrom, V.25; Moffatt, J.25; Redick, M.25; Griest, K.25; Packard, M.25; Muszynski, M.25; Kampmeier, J.25; Bjella, R.25; Flynn, S.25; Elsaesser, B.25; Chambers, K. C.26; Flewelling, H. A.26; Huber, M. E.26; Magnier, E. A.26; Waters, C. Z.26; Schultz, A. S. B.26; Bulger, J.26; Lowe, T. B.26; Willman, M.26; Smartt, S. J.27; Smith, K. W.27; Points, S.21; Strampelli, G. M.2,28; Brimacombe, J.29; Chen, P.30; Munoz, J. A.31,32; Mutel, R. L.33; Shields, J.34; Vallely, P. J.34; Villanueva, S., Jr.34; Li, W.35,36,37; Wang, X.35,36; Zhang, J.35,36,38,39,40; Lin, H.35,36; Mo, J.35,36; Zhao, X.41; Sai, H.35,36; Zhang, X.35,36; Zhang, K.35,36,42; Zhang, T.43; Wang, L.43,44,46,47; Zhang, J.; Baron, E.45; DerKacy, J. M.45; Li, L.35,36; Chen, Z.35,36; Xiang, D.35,36; Rui, L.35,36; Wang, L.; Huang, F.35,36,48; Li, X.35,36; Hosseinzadeh, G.37,49; Howell, D. A.37,49; Arcavi, I.37,49,50; Hiramatsu, D.37,49; Burke, J.37,49; Valenti, S.51; Tonry, J. L.26; Denneau, L.26; Heinze, A. N.26; Weiland, H.26; Stalder, B.52; Vinko, J.42,53,54; Sarneczky, K.53; Pal, A.53; Bodi, A.53,55; Bognar, Zs.53; Csak, B.53; Cseh, B.53; Csornyei, G.53; Hanyecz, O.53; Ignacz, B.53; Kalup, Cs.53; Konyves-Toth, R.53; Kriskovics, L.53; Ordasi, A.53; Rajmon, I.56; Sodor, A.53; Szabo, R.53; Szakats, R.53; Zsidi, G.53; Williams, S. C.57; Nordin, J.58; Cartier, R.21; Frohmaier, C.59; Galbany, L.60; Gutierrez, C. P.61; Hook, I.57; Inserra, C.61; Smith, M.61; Sand, D. J.62; Andrews, J. E.62; Smith, N.62; Bilinski, C.62
2019
Source PublicationASTROPHYSICAL JOURNAL LETTERS
ISSN2041-8205
Volume870Issue:1Pages:16
Corresponding AuthorDimitriadis, G.()
AbstractWe present an exquisite 30 minute cadence Kepler (K2) light curve of the Type Ia supernova (SN Ia) 2018oh (ASASSN-18bt), starting weeks before explosion, covering the moment of explosion and the subsequent rise, and continuing past peak brightness. These data are supplemented by multi-color Panoramic Survey Telescope (Pan-STARRS1) and Rapid Response System 1 and Cerro Tololo Inter-American Observatory 4 m Dark Energy Camera (CTIO 4-m DECam) observations obtained within hours of explosion. The K2 light curve has an unusual two-component shape, where the flux rises with a steep linear gradient for the first few days, followed by a quadratic rise as seen for typical supernovae (SNe). Ia. This "flux excess" relative to canonical SN. Ia behavior is confirmed in our i-band light curve, and furthermore, SN 2018oh is especially blue during the early epochs. The flux excess peaks 2.14 +/- 0.04 days after explosion, has a FWHM of 3.12 +/- 0.04 days, a blackbody temperature of T=17,500(-9,000)(+11,500) K, a peak luminosity of 4.3 +/- 0.2 x 10(37) erg s(-1), and a total integrated energy of 1.27 +/- 0.01 x 10(43) erg. We compare SN 2018oh to several models that may provide additional heating at early times, including collision with a companion and a shallow concentration of radioactive nickel. While all of these models generally reproduce the early K2 light curve shape, we slightly favor a companion interaction, at a distance of similar to 2x10(12) cm based on our early color measurements, although the exact distance depends on the uncertain viewing angle. Additional confirmation of a companion interaction in future modeling and observations of SN 2018oh would provide strong support for a single-degenerate progenitor system.
Keywordsupernovae: general supernovae: individual (SN 2018oh)
DOI10.3847/2041-8213/aaedb0
WOS KeywordCIRCUMSTELLAR MATERIAL ; RISE-TIME ; COMPANION ; EXPLOSION ; PROGENITORS ; BINARIES ; LAMBDA ; GALAXY ; GIANT ; OMEGA
Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000454558000001
PublisherIOP PUBLISHING LTD
Citation statistics
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/20491
Collection中国科学院紫金山天文台
Corresponding AuthorDimitriadis, G.
Affiliation1.Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA
2.Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA
3.Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA
4.Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA
5.Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA
6.Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA
7.Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA
8.Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA
9.State Univ New Jersey, Dept Phys & Astron, Rutgers, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA
10.Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA
11.NASA, Ames Res Ctr, Moffett Field, CA 94035 USA
12.Bay Area Environm Res Inst, POB 25, Moffett Field, CA 94035 USA
13.NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA
14.Univ Maryland Baltimore Cty, 1000 Hilltop Circle, Baltimore, MD 21250 USA
15.Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA
16.Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Canberra, ACT 2611, Australia
17.Australian Natl Univ, Natl Ctr Publ Awareness Sci, Canberra, ACT 2611, Australia
18.ARC Ctr Excellence All Sky Astrophys 3 Dimens AST, Bentley, WA, Australia
19.Univ Maryland, Dept Astron, College Pk, MD 20742 USA
20.Gemini Observ, La Serena, Chile
21.Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile
22.SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA
23.Univ Fed Campina Grande, Campina Grande, Brazil
24.Ball Aerosp & Technol Corp, Boulder, CO 80301 USA
25.Univ Colorado, LASP, Boulder, CO 80303 USA
26.Univ Hawaii, Inst Astron, 2680 Wood Lawn Dr, Honolulu, HI 96822 USA
27.Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland
28.Univ La Laguna, Calle Padre Herrera, E-38200 San Cristobal la Laguna, Spain
29.Coral Towers Observ, Cairns, Qld 4870, Australia
30.Peking Univ, Kavli Inst Astron & Astrophys, Yi He Yuan Rd 5, Beijing 100871, Peoples R China
31.Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain
32.Univ Valencia, Observ Astron, E-46980 Valencia, Spain
33.Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA
34.Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA
35.Tsinghua Univ, Phys Dept, Beijing 100084, Peoples R China
36.Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China
37.Las Cumbres Observ, 6740 Cortona Dr Ste 102, Goleta, CA 93117 USA
38.Chinese Acad Sci, Yunnan Astron Observ China, Kunming 650011, Yunnan, Peoples R China
39.Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650216, Yunnan, Peoples R China
40.Chinese Acad Sci, Ctr Astron Mega Sci, 20A Datun Rd, Beijing 100012, Peoples R China
41.Tianjin Univ Technol, Sch Sci, Tianjin 300384, Peoples R China
42.Univ Texas Austin, Dept Astron, Austin, TX 78712 USA
43.Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China
44.Chinese Acad Sci, South Amer Ctr Astron, China Chile Joint Ctr Astron, Camino El Observ 1515, Santiago, Chile
45.Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA
46.Chinese Acad Sci, Purple Mt Observ, Nanjing 210034, Jiangsu, Peoples R China
47.Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, 4242 TAMU, College Stn, TX 77843 USA
48.Shanghai Jiao Tong Univ, Sch Phys & Astron, Dept Astron, Shanghai 200240, Peoples R China
49.Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
50.Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel
51.Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA
52.LSST, 950 North Cherry Ave, Tucson, AZ 85719 USA
53.Konkoly Observ Budapest, MTA CSFK, Konkoly Thege M Ut 15-17, H-1121 Budapest, Hungary
54.Univ Szeged, Dept Opt & Quantum Elect, Dom Ter 9, H-6720 Szeged, Hungary
55.MTA CSFK, Lendulet Near Field Cosmol Res Grp, Budapest, Hungary
56.Berzsenyi Daniel High Sch, Karpat Utca 49-53, H-1133 Budapest, Hungary
57.Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England
58.Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany
59.Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England
60.Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA
61.Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England
62.Univ Arizona, Steward Observ, 933 North Cherry Ave,Room N204, Tucson, AZ 85721 USA
Recommended Citation
GB/T 7714
Dimitriadis, G.,Foley, R. J.,Rest, A.,et al. K2 Observations of SN 2018oh Reveal a Two-component Rising Light Curve for a Type Ia Supernova[J]. ASTROPHYSICAL JOURNAL LETTERS,2019,870(1):16.
APA Dimitriadis, G..,Foley, R. J..,Rest, A..,Kasen, D..,Piro, A. L..,...&Bilinski, C..(2019).K2 Observations of SN 2018oh Reveal a Two-component Rising Light Curve for a Type Ia Supernova.ASTROPHYSICAL JOURNAL LETTERS,870(1),16.
MLA Dimitriadis, G.,et al."K2 Observations of SN 2018oh Reveal a Two-component Rising Light Curve for a Type Ia Supernova".ASTROPHYSICAL JOURNAL LETTERS 870.1(2019):16.
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