期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 870, 期 1, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/2041-8213/aaedb0
关键词
supernovae: general; supernovae: individual (SN 2018oh)
资金
- NASA Science Mission directorate
- NASA [NNG17PX03C, 80NSSC18K0303, PF6-170148, NNX16AB5G, NAS5-26555]
- HST [GO-12577, HST AR-12851]
- National Aeronautics and Space Administration [NNX12AT65G, NNX14AM74G]
- National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate
- National Science Foundation [AST-1238877]
- DOE (USA)
- NSF (USA)
- MISE (Spain)
- STFC (UK)
- HEFCE (UK)
- NCSA (UIUC)
- KICP (U. Chicago)
- CCAPP (Ohio State)
- MIFPA (Texas AM)
- CNPQ (Brazil)
- FAPERJ (Brazil)
- FINEP (Brazil)
- MINECO (Spain)
- DFG (Germany)
- Argonne Lab
- UC Santa Cruz
- University of Cambridge
- CIEMAT-Madrid
- University of Chicago
- University College London
- DES-Brazil Consortium
- University of Edinburgh
- ETH Zurich
- Fermilab
- University of Illinois
- ICE (IEEC-CSIC)
- IFAE Barcelona
- Lawrence Berkeley Lab
- LMU Munchen
- University of Michigan
- NOAO
- University of Nottingham
- Ohio State University
- OzDES Membership Consortium
- University of Pennsylvania
- University of Portsmouth
- SLAC National Lab
- Stanford University
- University of Sussex
- Texas AM University
- NSF [AST1518052, AST-1815935, AST-1821967, 1821987, 1813466, 1813708, AST-1515559]
- Gordon & Betty Moore Foundation
- Heising-Simons Foundation
- Alfred P. Sloan Foundation
- David and Lucile Packard Foundation
- STFC [ST/P000312/1, ST/N002520/1]
- US National Science Foundation [1313484]
- National Research, Development and Innovation Office (NKFIH), Hungary - European Union [GINOP 2.3.2-15-2016-00033]
- Lendulet Program of the Hungarian Academy of Sciences [LP2018-7/2018, LP2012-31]
- NKFIH [K-115709]
- National Research, Development and Innovation Fund of Hungary under the PD 17 funding scheme [PD123910]
- Chinese Academy of Sciences
- People's Government of Yunnan Province
- National Natural Science Foundation of China (NSFC) [11178003, 11325313, 11633002]
- National Program on Key Research and Development Project [2016YFA0400803]
- National Science Foundation of China (NSFC) [11403096, 11773067]
- Youth Innovation Promotion Association of the CAS
- Western Light Youth Project
- Key Research Program of the CAS [KJZD-EW-M06]
- NSFC [11203034]
- Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences
- EU/FP7-ERC [615929]
- Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) [CE170100013]
- NASA - Space Telescope Science Institute [HST-HF2-51357.001-A]
- NASA K2 Cycle 4 Grant [NNX17AE92G, NNX17AI64G]
- NASA K2 cycle 5 grant [80NSSC18K0302]
- NASA [NNX17AE92G, 1002375] Funding Source: Federal RePORTER
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1313484] Funding Source: National Science Foundation
- STFC [ST/R000514/1, ST/P00038X/1, ST/P000312/1] Funding Source: UKRI
We 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.
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