PMO OpenIR
Seeing Double: ASASSN-18bt Exhibits a Two-component Rise in the Early-time K2 Light
Shappee, B. J.1; Holoien, T. W. -S.2; Drout, M. R.2; Auchettl, K.3,4,5; Stritzinger, M. D.6,7; Kochanek, C. S.3,8; Stanek, K. Z.3,8; Shaya, E.9; Narayan, G.10; Brown, J. S.8; Bose, S.11; Bersier, D.12; Brimacombe, J.13; Chen, Ping11; Dong, Subo11; Holmbo, S.6; Katz, B.14; Munoz, J. A.15,16; Mutel, R. L.17; Post, R. S.18; Prieto, J. L.19,20; Shields, J.8; Tallon, D.17; Thompson, T. A.3,8; Vallely, P. J.8; Villanueva, S., Jr.8; Denneau, L.1; Flewelling, H.1; Heinze, A. N.1; Smith, K. W.21; Stalder, B.22; Tonry, J. L.1; Weiland, H.1; Barclay, T.23,24; Barentsen, G.25,26; Cody, A. M.25,26; Dotson, J.25; Foerster, F.27; Garnavich, P.28; Gully-Santiago, M.25,26; Hedges, C.25,26; Howell, S.25; Kasen, D.29,30; Margheim, S.31; Mushotzky, R.9; Rest, A.10,32; Tucker, B. E.33,34,35; Villar, A.36; Zenteno, A.37; Beerman, G.38; Bjella, R.38; Castillo, G.38; Coughlin, J.25,39; Elsaesser, B.38; Flynn, S.38; Gangopadhyay, R.38; Griest, K.38; Hanley, M.38; Kampmeier, J.38; Kloetzel, R.38; Kohnert, L.38; Labonde, C.38; Larsen, R.38; Larson, K. A.40; McCalmont-Everton, K. M.40; McGinn, C.38; Migliorini, L.38; Moffatt, J.38; Muszynski, M.38; Nystrom, V.38; Osborne, D.38; Packard, M.38; Peterson, C. A.40; Redick, M.38; Reedy, L. H.38; Ross, S. E.40; Spencer, B.38; Steward, K.38; Van Cleve, J. E.25,39; Vinicius de Miranda Cardoso, J.25,41; Weschler, T.38; Wheaton, A.38; Bulger, J.1; Chambers, K. C.1; Flewelling, H. A.1; Huber, M. E.1; Lowe, T. B.1; Magnier, E. A.1; Schultz, A. S. B.1; Waters, C. Z.1; Willman, M.1; Baron, E.42,43; Chen, Zhihao44,45; Derkacy, James M.42; Huang, Fang44,45,46; Li, Linyi44,45; Li, Wenxiong44,45,47; Li, Xue44,45; Mo, Jun44,45; Rui, Liming44,45; Sai, Hanna44,45; Wang, Lifan48,49,50; Wang, Lingzhi51; Wang, Xiaofeng44,45; Xiang, Danfeng44,45; Zhang, Jicheng44,45; Zhang, Jujia52; Zhang, Kaicheng44,45,53; Zhang, Tianmeng51; Zhang, Xinghan44,45; Zhao, Xulin54; Brown, P. J.49,50; Hermes, J. J.55; Nordin, J.56; Points, S.37; Sodor, A.57; Strampelli, G. M.32,58
2019
Source PublicationASTROPHYSICAL JOURNAL
ISSN0004-637X
Volume870Issue:1Pages:14
Corresponding AuthorShappee, B. J.(shappee@hawaii.edu)
AbstractOn 2018 February 4.41, the All-Sky Automated Survey for SuperNovae (ASAS-SN) discovered ASASSN-18bt in the K2 Campaign 16 field. With a redshift of z = 0.01098 and a peak apparent magnitude of B-max = 14.31, ASASSN-18bt is the nearest and brightest SNe Ia yet observed by the Kepler spacecraft. Here we present the discovery of ASASSN-18bt, the K2 light curve, and prediscovery data from ASAS-SN and the Asteroid Terrestrial-impact Last Alert System. The K2 early-time light curve has an unprecedented 30-minute cadence and photometric precision for an SN. Ia light curve, and it unambiguously shows a similar to 4 day nearly linear phase followed by a steeper rise. Thus, ASASSN-18bt joins a growing list of SNe Ia whose early light curves are not well described by a single power law. We show that a double-power-law model fits the data reasonably well, hinting that two physical processes must be responsible for the observed rise. However, we find that current models of the interaction with a nondegenerate companion predict an abrupt rise and cannot adequately explain the initial, slower linear phase. Instead, we find that existing published models with shallow Ni-56 are able to span the observed behavior and, with tuning, may be able to reproduce the ASASSN-18bt light curve. Regardless, more theoretical work is needed to satisfactorily model this and other early-time SNe. Ia light curves. Finally, we use Swift X-ray nondetections to constrain the presence of circumstellar material (CSM) at much larger distances and lower densities than possible with the optical light curve. For a constant-density CSM, these nondetections constrain rho < 4.5 x 10(5) cm(-3) at a radius of 4 x 10(15) cm from the progenitor star. Assuming a wind-like environment, we place mass loss limits of <(M)over dot> < 8 x 10(-6) M-circle dot yr(-1). for v(w) =. 100 km s(-1), ruling out some symbiotic progenitor systems. This work highlights the power of well-sampled early-time data and the need for immediate multiband, high-cadence follow-up for progress in understanding SNe Ia.
Keywordsupernovae: individual (ASASSN-18bt, SN 2018oh)
DOI10.3847/1538-4357/aaec79
WOS KeywordWHITE-DWARF MODELS ; I SUPER-NOVAE ; ECCENTRICITY OSCILLATIONS ; EVOLUTION ; COMPANION ; BINARIES ; SPECTRA ; SYSTEMS ; STARS
Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000454551600002
PublisherIOP PUBLISHING LTD
Citation statistics
Cited Times:9[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/20485
Collection中国科学院紫金山天文台
Corresponding AuthorShappee, B. J.
Affiliation1.Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA
2.Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA
3.Ohio State Univ, Ctr Cosmol & AstroParticle Phys CCAPP, 191 W Woodruff Ave, Columbus, OH 43210 USA
4.Ohio State Univ, Dept Phys, 191 W Woodruff Ave, Columbus, OH 43210 USA
5.Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Blegdamsvej 17, DK-2100 Copenhagen, Denmark
6.Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus, Denmark
7.Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA
8.Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA
9.Univ Maryland, Dept Astron, College Pk, MD 20742 USA
10.Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA
11.Peking Univ, Kavli Inst Astron & Astrophys, Yi He Yuan Rd 5, Beijing 100871, Peoples R China
12.Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England
13.Coral Towers Observ, Cairns, Qld 4870, Australia
14.Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel
15.Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain
16.Univ Valencia, Observ Astron, E-46980 Valencia, Spain
17.Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA
18.Post Observ, Lexington, MA 02421 USA
19.Univ Diego Portales, Nucleo Astron, Fac Ingn & Ciencias, Av Ejercito 441, Santiago, Chile
20.Millennium Inst Astrophys, Santiago, Chile
21.Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland
22.LSST, 950 North Cherry Ave, Tucson, AZ 85719 USA
23.NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA
24.Univ Maryland Baltimore Cty, 1000 Hilltop Cir, Baltimore, MD 21250 USA
25.NASA, Ames Res Ctr, Moffett Field, CA 94035 USA
26.Bay Area Environm Res Inst, POB 25, Moffett Field, CA 94035 USA
27.Univ Chile, Ctr Math Modeling, Santiago, Chile
28.Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA
29.Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA
30.Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA
31.Gemini Observ, La Serena, Chile
32.Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA
33.Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Via Cotter Rd, Canberra, ACT 2611, Australia
34.ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia
35.Australian Natl Univ, Natl Ctr Publ Awareness Sci, Canberra, ACT 2601, Australia
36.Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA
37.Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile
38.Univ Colorado, LASP, Boulder, CO 80303 USA
39.SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA
40.Ball Aerosp & Technol Corp, Boulder, CO 80301 USA
41.Univ Fed Campina Grande, Campina Grande, Brazil
42.Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA
43.Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
44.Tsinghua Univ, Phys Dept, Beijing 100084, Peoples R China
45.Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China
46.Shanghai Jiao Tong Univ, Sch Phys & Astron, Dept Astron, Shanghai 200240, Peoples R China
47.Las Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA
48.Chinese Acad Sci, Purple Mt Observ, Nanjing 210034, Jiangsu, Peoples R China
49.Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA
50.Texas A&M Univ, Dept Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA
51.Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China
52.Chinese Acad Sci, Yunnan Astron Observ China, Kunming 650011, Yunnan, Peoples R China
53.Univ Texas Austin, Dept Astron, Austin, TX 78712 USA
54.Tianjin Univ Technol, Sch Sci, Tianjin 300384, Peoples R China
55.Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA
56.Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany
57.Konkoly Observ Budapest, MTA CSFK, Konkoly Thege M Ut 15-17, H-1121 Budapest, Hungary
58.Univ La Laguna, Calle Padre Herrera, San Cristobal De Laguna 38200, Santa Cruz De T, Spain
Recommended Citation
GB/T 7714
Shappee, B. J.,Holoien, T. W. -S.,Drout, M. R.,et al. Seeing Double: ASASSN-18bt Exhibits a Two-component Rise in the Early-time K2 Light[J]. ASTROPHYSICAL JOURNAL,2019,870(1):14.
APA Shappee, B. J..,Holoien, T. W. -S..,Drout, M. R..,Auchettl, K..,Stritzinger, M. D..,...&Strampelli, G. M..(2019).Seeing Double: ASASSN-18bt Exhibits a Two-component Rise in the Early-time K2 Light.ASTROPHYSICAL JOURNAL,870(1),14.
MLA Shappee, B. J.,et al."Seeing Double: ASASSN-18bt Exhibits a Two-component Rise in the Early-time K2 Light".ASTROPHYSICAL JOURNAL 870.1(2019):14.
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