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arXiv 2017年

作者： Lu, Nanyao Zhao, Yinghe Díaz-Santos, Tanio Xu, C. Kevin Gao, Yu Armus, Lee Isaak, Kate G. Mazzarella, Joseph M. van der Werf, Paul P. Appleton, Philip N. Charmandaris, Vassilis Evans, Aaron S. Howell, Justin Iwasawa, Kazushi Leech, Jamie Lord, Steven Petric, Andreea O. Privon, George C. Sanders, David B. Schulz, Bernhard Surace, Jason A. Beijing100012 China South American Center for Astronomy CAS Camino El Observatorio 1515 Las Condes Santiago Chile Infrared Processing and Analysis Center California Institute of Technology MS 100-22 PasadenaCA91125 United States Yunnan Observatories CAS Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650011 China Purple Mountain Observatory CAS Nanjing210008 China Nucleo de Astronomia de la Facultad de Ingenieria Universidad Diego Portales Av. Ejercito Libertador 441 Santiago Chile Spitzer Science Center California Institute of Technology MS 220-6 PasadenaCA91125 United States Keplerlaan 1 Noordwijk2201 AZ Netherlands Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands Department of Physics University of Crete HeraklionGR-71003 Greece IAASARS National Observatory of Athens PenteliGR-15236 Greece Department of Astronomy University of Virginia 530 McCormick Road CharlottesvilleVA22904 United States National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States Martí i Franqués 1 Barcelona08028 Spain ICREA Pg. Lluís Companys 23 Barcelona08010 Spain Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom SETI Institute 189 Bernardo Ave Suite 100 Mountain ViewCA94043 United States Gemini Observatory Northern Operations Center 670 N. Aohoku Place HiloHI96720 Departamento de Astronomía Universidad de Concepción Casilla 160-C Concepción Chile Pontificia Universidad Católica de Chile Instituto de Astrofisica Casilla 306 Santiago 22 Chile University of Hawaii Institute for Astronomy 2680 Woodlawn Drive HonoluluHI96822 United States

We describe a Herschel Space Observatory 194-671 µm spectroscopic survey of a sample of 121 local luminous infrared galaxies and report the fluxes of the CO J to J−1 rotational transitions for 4 ≤ J ≤ 13, the [N ii] 205 µm line, the [C i] lines at 609 and 370 µm, as well as additional and usually fainter lines. The CO spectral line energy distributions (SLEDs) presented here are consistent with our earlier work, which was based on a smaller sample, that calls for two distinct molecular gas components in general: (i) a cold component, which emits CO lines primarily at J 4 and likely represents the same gas phase traced by CO (1−0), and (ii) a warm component, which dominates over the mid-J regime (4 10. The flux ratios of the two [C i] lines imply modest excitation temperatures of 15 to 30 K;the [C i] 370 µm line scales more linearly in flux with CO (4−3) than with CO (7−6). These findings suggest that the [C i] emission is predominately associated with the gas component defined in (i) above. Our analysis of the stacked spectra in different far-infrared (FIR) color bins reveals an evolution of the SLED of the rotational transitions of H2O vapor as a function of the FIR color in a direction consistent with infrared photon pumping. Copyright © 2017, The Authors. All rights reserved.

关键词： Molecules

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Substellar objects around the sdB eclipsing Binaries

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Journal of Physics: Conference Series 2016年第7期728卷

作者： Liying Zhu Shengbang Qian Wenping Liao Ergang Zhao Linjia Li Yunnan Observatories Chinese Academy of Sciences (CAS) P.O. Box 110 650011 Kunming P. R. China Key laboratory of the structure and evolution of celestial objects Chinese Academy of Sciences P.O. Box 110 650011 Kunming P. R. China University of the Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block 100049 Beijing P. R. China

The sdB-type eclipsing binary consists a very hot subdwarf B (sdB) type primary and a low mass secondary with short period. They are detached binaries and show very narrow eclipse profiles, which benefits the determination of the precise eclipse times. With the precise times of light minimum, we can detected small mass objects around them by analyzing the observed-calculated (O-C) curve based on the light time effect. For searching the substellar objects orbiting around the binaries, we have monitored sdB-type eclipsing binaries for decades. A group of brown dwarfs and planets have been detected since then. In the present paper, we focus on the target NSVS07826147, which may be another exoplanet host candidate among the group of the sdB-type eclipsing binaries.

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The white dwarf binary pathways survey - II. Radial velocities of 1453 FGK stars with white dwarf companions from LAMOST DR 4

arXiv

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arXiv 2017年

作者： Rebassa-Mansergas, A. Ren, J.J. Irawati, P. García-Berro, E. Parsons, S.G. Schreiber, M.R. Gänsicke, B.T. Rodríguez-Gil, P. Liu, X. Manser, C. Palomo-Nevado, S. Jiménez-Ibarra, F. Costero, R. Echevarría, J. Michel, R. Zorotovic, M. Hollands, M. Han, Z. Luo, A. Villaver, E. Kong, X. Departament de Física Universitat Politècnica de Catalunya c/Esteve Terrades 5 Castelldefels08860 Spain Institute for Space Studies of Catalonia c/Gran Capità 2–4 Edif. Nexus 201 Barcelona08034 Spain National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China National Astronomical Research Institute of Thailand 191 Siriphanich Building Huay Kaew Road Chiang Mai50200 Thailand Deparment of Physics & Astronomy University of Sheffield SheffieldS3 7RH United Kingdom Instituto de Física y Astronomía Universidad de Valparaíso Avenida Gran Bretaña 1111 Valparaíso Chile Millenium Nucleus"Protoplanetary Disks in ALMA Early Science" Universidad de Valparaíso Avenida Gran Bretaña 1111 Valparaíso Chile Department of Physics University of Warwick CoventryCV4 7AL United Kingdom Instituto de Astrofísica de Canarias c/ Vía Láctea s/n La Laguna TenerifeE-38205 Spain Universidad de La Laguna Departamento de Astrofísica La Laguna TenerifeE- 38206 Spain Department of Astronomy Peking University Beijing100871 China Instituto de Astronomía Universidad Nacional Autónoma de México Ciudad Universitaria 70-264 México D.F.C.P. 04510 Mexico Instituto de Astronomía Universidad Nacional Autónoma de México 877 Ensenada Baja CaliforniaC.P.22830 Mexico Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan observatories Chinese Academy of Sciences P.O. Box 110 KunmingYunnan Province650011 China Departamento de Física Teórica Universidad Autónoma de Madrid CantoblancoMadrid28049 Spain

We present the second paper of a series of publications aiming at obtaining a better understanding regarding the nature of type Ia supernovae (SN Ia) progenitors by studying a large sample of detached F, G and K main sequence stars in close orbits with white dwarf companions (i.e. WD+FGK binaries). We employ the LAMOST (Large Sky Area Multi-object Fibre Spectroscopic Telescope) data release 4 spectroscopic data base together with GALEX (Galaxy evolution Explorer) ultraviolet fluxes to identify 1,549 WD+FGK binary candidates (1,057 of which are new), thus doubling the number of known sources. We measure the radial velocities of 1,453 of these binaries from the available LAMOST spectra and/or from spectra obtained by us at a wide variety of different telescopes around the globe. The analysis of the radial velocity data allows us to identify 24 systems displaying more than 3σ radial velocity variation that we classify as close binaries. We also discuss the fraction of close binaries among WD+FGK systems, which we find to be ∼10 per cent, and demonstrate that high-resolution spectroscopy is required to efficiently identify double-degenerate SN Ia progenitor candidates. Copyright © 2017, The Authors. All rights reserved.

关键词： Velocity

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Radio observations of the fine structure inside a post-CME current sheet

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Research in Astronomy and Astrophysics 2014年第7期14卷 843-854页

作者： Guan-Nan Gao Min Wang Jun Lin Ning Wu Cheng-Ming Tan Berhard Kliem Yang Su Yunnan Observatories Chinese Academy of Sciences University of Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy of Sciences Key Laboratory of Solar Activity National Astronomical ObservatoriesChinese Academy of Sciences School of Tourism and Geography Yunnan Normal University Institute of Physics and Astronomy University of Potsdam IGAM-Kanzelhhe Observatory Institute of PhysicsUniversity of GrazUniversittsplatz 58010 GrazAustria

A solar radio burst was observed in a coronal mass ejection/flare event by the Solar Broadband Radio Spectrometer at the Huairou Solar Observing Station on2004 December 1. The data exhibited various patterns of plasma motions, suggestive of the interaction between sunward moving plasmoids and the flare loop system during the impulsive phase of the event. In addition to the radio data, the associated whitelight, Hα, extreme ultraviolet light, and soft and hard X-rays were also studied.

关键词： Sun： coronal mass ejections （CMEs）-- Sun： flares -- Sun： solar radio bursts -- Sun： magnetic reconnection

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MULTI-WAVELENGTH OBSERVATIONS OF GRB 111228A AND IMPLICATIONS FOR THE FIREBALL AND ITS ENVIRONMENT

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The Astrophysical Journal 2016年第2期817卷

作者： Li-Ping Xin Yuan-Zhu Wang Ting-Ting Lin En-Wei Liang Hou-Jun Lü Shu-Qing Zhong Yuji Urata Xiao-Hong Zhao Chao Wu Jian-Yan Wei Kui-Yun Huang Yu-Lei Qiu Jin-Song Deng Key Laboratory of Space Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences China GXU-NAOC Center for Astrophysics and Space Sciences Department of Physics Guangxi University Nanning 530004 China Guangxi Key Laboratory for the Relativistic Astrophysics Nanning 530004 China Institute of Astronomy National Central University Chung-Li 32054 Taiwan Academia Sinica Institute of Astronomy and Astrophysics Taipei 106 Taiwan Yunnan Observatories Chinese Academy of Sciences P.O. Box 110 650011 Kunming China Key Laboratory for the Structure and Evolution of Celestial Bodies Chinese Academy of Sciences P.O. Box 110 650011 Kunming China Department of Mathematics and Science National Taiwan Normal University Lin-kou District New Taipei City 24449 Taiwan

Observations of very early multi-wavelength afterglows are critical to reveal the properties of the radiating fireball and its environment as well as the central engine of gamma-ray bursts (GRBs). We report our optical observations of GRB 111228A from 95 s to about 50 hr after the burst trigger and investigate its properties of the prompt gamma-rays and the ambient medium using our data and the data from the Swift and Fermi missions. Our joint optical and X-ray spectral fits to the afterglow data show that the ambient medium features a low dust-to-gas ratio. Incorporating the energy injection effect, our best fit to the afterglow light curves with the standard afterglow model via the Markov Chain Monte Carlo technique shows that , , cm−3. The low medium density likely implies that the afterglow jet may be in a halo or in a hot ISM. A chromatic shallow decay segment observed in the optical and X-ray bands is well explained with the long-lasting energy injection from the central engine, which would be a magnetar with a period of about 1.92 ms inferred from the data. The Ep of its time-integrated prompt gamma-ray spectrum is ~26 KeV. Using the initial Lorentz factor () derived from our afterglow model fit, it is found that GRB 111228A satisfies the relation and bridges the typical GRBs and low luminosity GRBs in this relation.

关键词： gamma-ray burst: individual (GRB 130702A, GRB 111228A)

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Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star

arXiv

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arXiv 2017年

作者： Arcavi, Iair Howell, D. Andrew Kasen, Daniel Bildsten, Lars Hosseinzadeh, Griffin McCully, Curtis Wong, Zheng Chuen Katz, Sarah Rebekah Gal-Yam, Avishay Sollerman, Jesper Taddia, Francesco Leloudas, Giorgos Fremling, Christoffer Nugent, Peter E. Horesh, Assaf Mooley, Kunal Rumsey, Clare Cenko, S. Bradley Graham, Melissa L. Perley, Daniel A. Nakar, Ehud Shaviv, Nir J. Bromberg, Omer Shen, Ken J. Ofek, Eran O. Cao, Yi Wang, Xiaofeng Huang, Fang Rui, Liming Zhang, Tianmeng Li, Wenxiong Li, Zhitong Zhang, Jujia Valenti, Stefano Guevel, David Shappee, Benjamin Kochanek, Christopher S. Holoien, Thomas W.-S. Filippenko, Alexei V. Fender, Rob Nyholm, Anders Yaron, Ofer Kasliwal, Mansi M. Sullivan, Mark Blagorodnova, Nadja Walters, Richard S. Lunnan, Ragnhild Khazov, Danny Andreoni, Igor Laher, Russ R. Konidaris, Nick Wozniak, Przemek Bue, Brian Las Cumbres Observatory GoletaCA93117 United States Kavli Institute for Theoretical Physics University of California Santa BarbaraCA93106 United States Department of Physics University of California Santa BarbaraCA93106 United States Nuclear Science Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics University of California BerkeleyCA94720 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot76100 Israel The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Juliane Maries vej 30 Copenhagen2100 Denmark Computational Research Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Racah Institute of Physics Hebrew University of Jerusalem Jerusalem91904 Israel Department of Physics Astrophysics University of Oxford Denys Wilkinson Building OxfordOX1 3RH United Kingdom Astrophysics Group Cavendish Laboratory 19 J. J. Thomson Avenue CambridgeCB3 0HE United Kingdom Astrophysics Science Division NASA Goddard Space Flight Center Code 661 GreenbeltMD20771 United States Joint Space-Science Institute University of Maryland College ParkMD20742 United States Department of Astronomy University of Washington Box 351580 U.W. SeattleWA98195-1580 United States Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Raymond and Beverly Sackler School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel eScience Institute University of Washington Box 351570 U.W. SeattleWA98195-1580 United States Tsinghua University Beijing100084 China Key Laboratory of Optical Astronomy National Astronomical Observatories of China Chinese

Every supernova hitherto observed has been considered to be the terminal explosion of a star. Moreover, all supernovae with absorption lines in their spectra show those lines decreasing in velocity over time, as the ejecta expand and thin, revealing slower moving material that was previously hidden. In addition, every supernova that exhibits the absorption lines of hydrogen has one main light-curve peak, or a plateau in luminosity, lasting approximately 100 days before declining1. Here we report observations of iPTF14hls, an event that has spectra identical to a hydrogen-rich core-collapse supernova, but characteristics that differ extensively from those of known supernovae. The light curve has at least five peaks and remains bright for more than 600 days;the absorption lines show little to no decrease in velocity;and the radius of the line-forming region is more than an order of magnitude bigger than the radius of the photosphere derived from the continuum emission. These characteristics are consistent with a shell of several tens of solar masses ejected by the star at supernova-level energies a few hundred days before a terminal explosion. Another possible eruption was recorded at the same position in 1954. Multiple energetic pre-supernova eruptions are expected to occur in stars of 95–130 solar masses, which experience the pulsational pair instability2, 3, 4, 5. That model, however, does not account for the continued presence of hydrogen, or the energetics observed here. Another mechanism for the violent ejection of mass in massive stars may be required. Copyright © 2017, The Authors. All rights reserved.

关键词： Supernovae

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Characteristics of Double Gamma-Ray Bursts

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Chinese Physics Letters 2014年第11期31卷 163-165页

作者：刘彤孙谋远侯书进李昂张富文顾为民卢炬甫 Department of Astronomy and Institute of Theoretical Physics and Astrophysics Xiamen University Xiamen 361005 Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 State Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences Beijing 100190 Department of Astronomy and Astrophysics and Institute for Gravitation and the Cosmos Pennsylvania State University University Park PA 16802 USA College of Physics and Electronic Engineering Nanyang Normal University Nanyang 473061 College of Science Guilin University of Technology Guilin 541004

Double gamma-ray bursts （DGRBs） have two well-separated sub-bursts in the main prompt emission and the typical time interval between them is in the hundreds of seconds. Among DGRBs, gamma-ray bursts （DGRBs） 110801A and 120716A are the ones with known redshifts. However, unlike GRB 110801A, we show that the two sub-bursts of GRB 120716A is severally similar to the short- and long-duration GRBs, thus it is difficult to explain the origin of GRB 120716A by the popular models on the central engine of GRBs. We suggest that some mechanisms of x-ray flares in GRBs, i.e., a post-merger millisecond pulsars or the jet precession in a black hole hyperaccretion system may produce the DGRB.

关键词： GAMMA ray bursts RED shift X-rays LIGHT curves PHYSICS research

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FIRST PHOTOMETRIC INVESTIGATION of the SOLAR-TYPE CONTACT BINARY GSC 1537-1557

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Astronomical Journal 2015年第1期150卷

作者： Xiang, F.-Y. Xiao, T.-Y. Zhang, B. Shi, X.-D. Physics Department Xiangtan University Funan Province Xiangtan 411105 China Yunnan Observatories Chinese Academy of Sciences (CAS) P.O. Box 110 Kunming 650011 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P.O. Box 110 Kunming 650011 China University of the Chinese Academy of Sciences Yuquan Road 19# Beijing 100049 China

By analyzing Rc and Ic light curves of the short-period solar-type eclipsing binary GSC 1537-1557 we discovered that it is a shallow contact binary with a degree of contact factor of . Photometric solutions reveal tha... 详细信息

By analyzing R_c and I_c light curves of the short-period solar-type eclipsing binary GSC 1537-1557 we discovered that it is a shallow contact binary with a degree of contact factor of . Photometric solutions reveal that GSC 1537-1557 is a W-type system with a mass ratio of where the less massive component (the primary star) is about 110 K hotter than the more massive one (the secondary star). The asymmetry and variation of the light curves were explained as the activity of spots on the solar-type component stars. By investigating all of the available times of light minima, we found that the observed-calculated (O-C) curve shows a cyclic variation with a small amplitude of 0.00335 days and a period of 8.1 years. The small-amplitude cyclic change in the curve was analyzed for the light-travel time effect via the presence of an extremely cool stellar companion. The mass of the third body was determined to be when is adopted for GSC 1537-1557. The semimajor axis of the outer obit is AU. © 2015. The American Astronomical Society. All rights reserved..

关键词： accretion, accretion disks BL Lacertae objects: general galaxies: active galaxies: jets quasars: general

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

arXiv

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arXiv 2018年

作者： 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. Derkacy, J.M. Zhao, X. Sai, H. Zhang, K. Wang, L. Howell, D.A. McCully, C. Arcavi, I. Valenti, S. Hiramatsu, D. Burke, J. Rest, A. Garnavich, P. Tucker, B.E. Narayan, G. Shaya, E. Margheim, S. Zenteno, A. Villar, A. Dimitriadis, G. Foley, R.J. Pan, Y.-C. Coulter, D.A. Fox, O.D. Jha, S.W. Jones, D.O. Kasen, D.N. Kilpatrick, C.D. Piro, A.L. Riess, A.G. Rojas-Bravo, C. Shappee, B.J. Holoien, T.W.-S. Stanek, K.Z. Drout, M.R. Auchettl, K. Kochanek, C.S. Brown, J.S. Bose, S. Bersier, D. Brimacombe, J. Chen, P. Dong, S. Holmbo, S. Muñoz, J.A. Mutel, R.L. Post, R.S. Prieto, J.L. Shields, J. Tallon, D. Thompson, T.A. Vallely, P.J. Villanueva, S. Smartt, S.J. Smith, K.W. Chambers, K.C. Flewelling, H.A. Huber, M.E. Magnier, E.A. Waters, C.Z. Schultz, A.S.B. Bulger, J. Lowe, T.B. Willman, M. Sárneczky, K. Pál, A. Wheeler, J.C. Bódi, A. Bognár, Zs Csák, B. Cseh, B. Csörnyei, G. Hanyecz, O. Ignácz, B. Kalup, Cs Könyves-Tóth, R. Kriskovics, L. Ordasi, A. Rajmon, I. Sódor, A. Szabó, R. Szakáts, R. Zsidi, G. Milne, P. Andrews, J.E. Smith, N. Bilinski, C. Brown, P.J. Nordin, J. Williams, S.C. Galbany, L. Palmerio, J. Hook, I.M. Inserra, C. Maguire, K. Cartier, Régis Razza, A. Gutiérrez, C.P. Hermes, J.J. Reding, J.S. Kaiser, B.C. Tonry, J.L. Heinze, A.N. Denneau, L. Weiland, H. Stalder, B. Barentsen, G. Dotson, J. Barclay, T. Gully-Santiago, M. Hedges, C. Cody, A.M. Howell, S. Coughlin, J. van Cleve, J.E. Cardoso, J. Vinícius de Miranda Larson, K.A. McCalmont-Everton, K.M. Peterson, C.A. Ross, S.E. Reedy, L.H. Osborne, D. McGinn, C. Kohnert, L. Migliorini, L. Wheaton, A. Spencer, B. Labonde, C. PTSS / TNTS LCO KEGS UCSC ASAS-SN Pan-STARRS University of Arizona Swift ePESSTO University of North Carolina ATLAS Mission Team spacecraft team Tsinghua University Beijing100084 China Las Cumbres Observatory 6740 Cortona Dr Ste 102 GoletaCA93117-5575 United States Konkoly Observatory MTA CSFK Konkoly Thege M. ut 15-17 Budapest1121 Hungary Department of Optics & Quantum Electronics University of Szeged Dom ter 9 Szeged6720 Hungary Department of Astronomy University of Texas at Austin AustinTX78712 United States Department of Physics University of California Santa BarbaraCA93106-9530 United States Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Steward Observatory University of Arizona 933 North Cherry Avenue Rm. N204 TucsonAZ85721-0065 United States Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China National Astronomical Observatory of China Chinese Academy of Sciences Beijing100012 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210034 China George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy Texas A. & M. University Department of Physics and Astronomy 4242 TAMU College StationTX77843 United States Department of Astronomy School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Homer L. Dodge Department of Physics and Astronomy University of Oklahoma NormanOK United States School of Science Tianjin University of Technology Tianjin300384 China Chinese Academy of Sciences South America Center for Astronomy China-Chile Joint Center for Astronomy Camino El Observatorio 1515 SantiagoLas Condes Chile Raymond and Beverly Sackler School of Physics and Astronomy Tel Aviv University Te

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 to place interesting constraints on its progenitor system (Dimitriadis et al. 2018;Shappee et al. 2018b). 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 ∆m15(B) = 0.96±0.03 mag, but it seems to have bluer B − V colors. We construct the "uvoir" bolometric light curve having peak luminosity as 1.49×1043erg s−1, from which we derive a nickel mass as 0.55±0.04M☉ 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 non-degenerate 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 a SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers. Copyright © 2018, The Authors. All rights reserved.

关键词： Supernovae

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K2 Observations of SN 2018oh Reveal a Two-Component Rising Light Curve for a Type Ia Supernova

arXiv

引用

arXiv 2018年

作者： Dimitriadis, G. Foley, R.J. Rest, A. Kasen, D. Piro, A.L. Polin, A. Jones, D.O. Villar, A. Narayan, G. Coulter, D.A. Kilpatrick, C.D. Pan, Y.-C. Rojas-Bravo, C. Fox, O.D. Jha, S.W. Nugent, P.E. Riess, A.G. Scolnic, D. Drout, M.R. Barentsen, G. Dotson, J. Gully-Santiago, M. Hedges, C. Cody, A.M. Barclay, T. Howell, S. Garnavich, P. Tucker, B.E. Shaya, E. Mushotzky, R. Olling, R.P. Margheim, S. Zenteno, A. Coughlin, J. van Cleve, J.E. Cardoso, J. Vinícius de Miranda Larson, K.A. McCalmont-Everton, K.M. Peterson, C.A. Ross, S.E. Reedy, L.H. 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. Chambers, K.C. Flewelling, H.A. Huber, M.E. Magnier, E.A. Waters, C.Z. Schultz, A.S.B. Bulger, J. Lowe, T.B. Willman, M. Smartt, S.J. Smith, K.W. Points, S. Strampelli, G.M. Brimacombe, J. Chen, P. Muñoz, J.A. Mutel, R.L. Shields, J. Vallely, P.J. Jr, S. Villanueva Li, W. Wang, X. Zhang, J. Lin, H. Mo, J. Zhao, X. Sai, H. Zhang, X. Zhang, K. Zhang, T. Wang, L. Zhang, J. Baron, E. DerKacy, J.M. Li, L. Chen, Z. Xiang, D. Rui, L. Wang, L. Huang, F. Li, X. Hosseinzadeh, G. Howell, D.A. Arcavi, I. Hiramatsu, D. Burke, J. Valenti, S. Tonry, J.L. Denneau, L. Heinze, A.N. Weiland, H. Stalder, B. Vinkó, J. Sárneczky, K. Pál, A. Bódi, A. Bognár, Zs. Csák, B. Cseh, B. Csörnyei, G. Hanyecz, O. Ignácz, B. Kalup, Cs. Könyves-Tóth, R. Kriskovics, L. Ordasi, A. Rajmon, I. Sódor, A. Szabó, R. Szakáts, R. Zsidi, G. Williams, S.C. Nordin, J. Cartier, R. Frohmaier, C. Galbany, L. Gutiérrez, C.P. Hook, I. Inserra, C. Smith, M. Sand, D.J. Andrews, J.E. Smith, N. Bilinski, C. Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Department of Physics and Astronomy Rutgers State University of New Jersey 136 Frelinghuysen Road PiscatawayNJ08854 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States NASA Ames Research Center Moffett FieldCA94035 United States Bay Area Environmental Research Institute P.O. Box 25 Moffett FieldCA94035 United States NASA Goddard Space Flight Center 8800 Greenbelt Rd GreenbeltMD20771 United States University of Maryland Baltimore County 1000 Hilltop Cir BaltimoreMD21250 United States Department of Physics University of Notre Dame 225 Nieuwland Science Hall Notre DameIN46556-5670 United States Research School of Astronomy and Astrophysics Mount Stromlo Observatory Australian National University CanberraACT2611 Australia National Centre for the Public Awareness of Science Australian National University CanberraACT2611 Australia Australia Astronomy Department University of Maryland College ParkMD20742-2421 United States Gemini Observatory La Serena Chile Cerro Tololo Inter-American Observatory Casilla 603 La Serena Chile SETI Institute 189 Bernardo Avenue Mountain ViewCA94043

We present an exquisite, 30-min 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 Pan-STARRS1 and 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 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+11−9,000,500 K, a peak luminosity of 4.3±0.2×1037 erg s−1, and a total integrated energy of 1.27±0.01×1043 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 ∼2 × 1012 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. Copyright © 2018, The Authors. All rights reserved.

关键词： Explosions

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