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SN 2017fgc: A fast-expanding Type Ia supernova exploded in massive shell galaxy NGC 474

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arXiv 2021年

作者： Zeng, Xiangyun Wang, Xiaofeng Esamdin, Ali Pellegrino, Craig Burke, Jamison Stahl, Benjamin E. Zheng, Weikang Filippenko, Alexei V. Howell, D. Andrew Sand, D.J. Valenti, Stefano Mo, Jun Xi, Gaobo Liu, Jialian Zhang, Jujia Li, Wenxiong Iskandar, Abdusamatjan Zhang, Mengfan Lin, Han Sai, Hanna Xiang, Danfeng Wei, Peng Zhang, Tianmeng Reichart, D.E. Brink, Thomas G. McCully, Curtis Hiramatsu, Daichi Hosseinzadeh, Griffin Jeffers, Benjamin T. Ross, Timothy W. Stegman, Samantha Wang, Lifan Zhang, Jicheng Ma, Shuo Xinjiang Astronomical Observatory Chinese Academy of Sciences Xinjiang Urumqi830011 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing100049 China Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science of Technology Beijing100044 China Department of Physics University of California Santa BarbaraCA93106-9530 United States Las Cumbres Observatory 6740 Cortona Drive GoletaCA93117-5575 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States Department of Physics University of California BerkeleyCA94720-7300 United States Marc J. Staley Graduate Fellow Miller Senior Fellow Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States Department of Physics University of California DavisCA95616 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 The School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China Department of Physics and Astronomy University of North Carolina at Chapel Hill Chapel HillNC27599 United States Center for Astrophysics Harvard and Smithsonian 60 Garden Street CambridgeMA02138-1516 United States Las CumbresObservatory 6740 Cortona Drive GoletaCA9311-5575 United States Department of Chemistry University of Wisconsin MadisonWI53706 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas AandM University Department of Physics and A

We present extensive optical photometric and spectroscopic observations of the high-velocity (HV) Type Ia supernova (SN Ia) 2017fgc, covering the phase from ∼12 d before to ∼ 389 d after maximum brightness. SN 2017fgc is similar to normal SNe Ia, with an absolute peak magnitude of MB max ≈ -19:32 ± 0:13 mag and a post-peak decline of Δm15(B) = 1:05 ± 0:07 mag. Its peak bolometric luminosity is derived as (1:32 ± 0:13) × 1043erg s-1, corresponding to a 56Ni mass of 0:51 ± 0:03Mo. The light curves of SN 2017fgc are found to exhibit excess emission in the UBV bands in the early nebular phase and pronounced secondary shoulder/maximum features in the RrIi bands. Its spectral evolution is similar to that of HV SNe Ia, with a maximum-light Si II velocity of 15;000 ± 150 km s-1and a post-peak velocity gradient of ∼ 120 ± 10 km s-1d-1. The Fe II and Mg II lines blended near 4300 Å and the Fe II, Si II, and Fe III lines blended near 4800 Åare obviously stronger than those of normal SNe Ia. Inspecting a large sample reveals that the strength of the two blends in the spectra, and the secondary peak in the i=r-band light curves, are found to be positively correlated with the maximum-light Si II velocity. Such correlations indicate that HV SNe Ia may experience more complete burning in the ejecta and/or that their progenitors have higher metallicity. Examining the birthplace environment of SN 2017fgc suggests that it likely arose from a stellar environment with young and high-metallicity populations. © 2021, CC BY.

关键词： Supernovae

Photometric and spectroscopic studies of superoutbursts of three dwarf novae independently identified by the SVOM/GWAC system in 2018

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arXiv 2019年

作者： Wang, J. Li, H.L. Xin, L.P. Han, X.H. Meng, X.M. Brink, T.G. Cai, H.B. Dai, Z.G. Filippenko, A.V. Hsia, C.-H. Huang, L. Jia, L. Li, G.W. Li, Y.B. Liang, E.W. Lu, X.M. Mao, J. Qiu, P. Qiu, Y.L. Ren, J.J. Turpin, D. Wang, H.J. Wang, X.G. Wang, X.Y. Wu, C. Xu, Y. Yan, J.Z. Zhang, J.B. Zheng, W. Wei, J.Y. Guangxi Key Laboratory for Relativistic Astrophysics School of Physical Science and Technology Guangxi University Nanning530004 China Key Laboratory of Space Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Department of Astronomy University of California BerkeleyCA94720-3411 United States School of Astronomy and Space Science Nanjing University Nanjing210000 China State Key Laboratory of Lunar and Planetary Sciences Macau University of Science and Technology Taipa999078 China Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210034 China

We report our photometric and spectroscopic follow-up observations of the superoutbursts of three dwarf novae (GWAC 180415A, GWAC 181017A and GWAC 181211A) identified independently by the Ground Wide-angle Cameras system, one of the ground-based instruments of the China-France SVOM mission. Based on a combination of our photometry and that taken from the AAVSO, our period analysis of the superhumps enables us to determine the mass ratios to be 0.0967-0.1163, 0.1879-0.1883 and 0.0981-0.1173 for GWAC 180415A, GWAC 181017A and GWAC 181211A, respectively. GWAC 180415A can be firmly identified as a WZ sge-type dwarf novae due to its long duration (∼ 2 weeks) multiple rebrightenings with amplitudes of 3-4 magnitudes, the early superhump associated with a double-wave modulation and the low mass ratio. The inferred low mass ratio and location in the Ε − Porb diagram suggest that GWAC 181211A is a WZ sge-type dwarf novae candidate. The measured Balmer decrements suggest the Balmer line emission is produced from an optical thick region in GWAC 180415A and GWAC 181017A, and from an optical thin region in GWAC 181211A. Copyright © 2019, The Authors. All rights reserved.

关键词： Photometry

SN 2020wnt: A slow-evolving carbon-rich superluminous supernova with no O ii lines and a bumpy light curve

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arXiv 2022年

作者： Gutiérrez, C.P. Pastorello, A. Bersten, M. Benetti, S. Orellana, M. Fiore, A. Karamehmetoglu, E. Kravtsov, T. Reguitti, A. Reynolds, T.M. Valerin, G. Mazzali, P. Sullivan, M. Cai, Y.-Z. Elias-Rosa, N. Fraser, M. Hsiao, E.Y. Kankare, E. Kotak, R. Kuncarayakti, H. Li, Z. Mattila, S. Mo, J. Moran, S. Ochner, P. Shahbandeh, M. Tomasella, L. Wang, X. Yan, S. Zhang, J. Zhang, T. Stritzinger, M.D. University of Turku FI-20014 Finland Tuorla Observatory Department of Physics and Astronomy University of Turku FI-20014 Finland INAF Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 PadovaI-35122 Italy Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata Paseo del Bosque S/N La PlataB1900FWA Argentina CCT CONICET UNLP. Paseo del Bosque S/N La PlataB1900FWA Argentina The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8583 Japan Universidad Nacional de Río Negro. Sede Andina Mitre 630 Bariloche8400 Argentina Argentina Fondazione Bruno Kessler Trento Italy INFN TIFPA Trento Institute for Fundamental Physics and Applications Via Sommarive 14 TrentoI-38123 Italy Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Departamento de Ciencias Físicas Universidad Andrés Bello Avda. República 252 Santiago Chile Millennium Institute of Astrophysics Nuncio Monsenor Sótero Sanz 100 Providencia Santiago Chile Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen N2200 Denmark Department of Physics and Astronomy G. Galilei University of Padova Vicolo dell'Osservatorio 3 Padova35122 Italy Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Max-Planck-Institut für Astrophysik Karl-Schwarzschild Str. 1 GarchingD-85748 Germany School of Physics and Astronomy University of Southampton SouthamptonSO17 1BJ United Kingdom Tsinghua University Beijing100084 China Institute of Space Sciences ICE CSIC Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain School of Physics O'Brien Centre for Science North University College Dublin Dublin Ireland Department of Physics Florida State University 77 Chieftan Way TallahasseeFL32306 United States Turku Collegium for Science Medicine and Technology University of Turku TurkuFI-20014

We present the analysis of SN 2020wnt, an unusual hydrogen-poor super-luminous supernova (SLSN-I), at a redshift of 0.032. The light curves of SN 2020wnt are characterised by an early bump lasting ∼ 5 days, followed by a bright main peak. The SN reaches a peak absolute magnitude of Mmaxr = −20.52 ± 0.03 mag at ∼ 77.5 days from explosion. This magnitude is at the lower end of the luminosity distribution of SLSNe-I, but the rise-time is one of the longest reported to date. Unlike other SLSNe-I, the spectra of SN 2020wnt do not show O ii, but strong lines of C ii and Si ii are detected. Spectroscopically, SN 2020wnt resembles the Type Ic SN 2007gr, but its evolution is significantly slower. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2020wnt luminosity can be explained by radioactive powering. The progenitor of SN 2020wnt is likely a massive and extended star with a pre-SN mass of 80 Mo and a pre-SN radius of 15 Ro that experiences a very energetic explosion of 45 × 1051 erg, producing 4 Mo of 56Ni. In this framework, the first peak results from a post-shock cooling phase for an extended progenitor, and the luminous main peak is due to a large nickel production. These characteristics are compatible with the pair-instability SN scenario. We note, however, that a significant contribution of interaction with circumstellar material cannot be ruled out. Copyright © 2022, The Authors. All rights reserved.

关键词： Supernovae

Numerical Modelling of Tertiary Tides

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arXiv 2018年

作者： Gao, Yan Correia, Alexandre C.M. Eggleton, Peter P. Han, Zhanwen Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Department of Physics University of Coimbra Coimbra3004-516 Portugal CIDMA Department of Physics University of Aveiro Aveiro3810-193 Portugal ASD Imcce Psl University Paris Observatory 77 Av. Denfert-Rochereau Paris75014 France Lawrence Livermore National Laboratory 7000 East Ave LivermoreCA94551 United States

Stellar systems consisting of multiple stars tend to undergo tidal interactions when the separations between the stars are short. While tidal phenomena have been exten-sively studied, a certain tidal effect exclusive to hierarchical triples (triples in which one component star has a much wider orbit than the others) has hardly received any attention, mainly due to its complexity and consequent resistance to being modelled. This tidal effect is the tidal perturbation of the tertiary by the inner binary, which in turn depletes orbital energy from the inner binary, causing the inner binary separa-tion to shrink. In this paper, we develop a fully numerical simulation of these "tertiary tides"by modifying established tidal models. We also provide general insight as to how close a hierarchical triple needs to be in order for such an effect to take place, and demonstrate that our simulations can effectively retrieve the orbital evolution for such systems. We conclude that tertiary tides are a significant factor in the evolution of close hierarchical triples, and strongly influence at least ∼ 1% of all multiple star systems. Copyright © 2018, The Authors. All rights reserved.

关键词： Astrophysics

Study of photometric phase curve with new brightness model:refining phase function system parameters of asteroid(107)Camilla

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Research in Astronomy and Astrophysics 2016年第9期16卷 117-122页

作者： Yi-Bo Wang Xiao-Bin Wang Ao Wang Yunnan Observatories Chinese Academy of SciencesKunming 650011China University of Chinese Academy of Sciences Beijing 100049China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650011China

We characterize the morphology of the photometric phase curve model of an asteroid with a three- parameter magnitude phase function H - G1 - G2 system by considering the effect of brightness variation arising from a triaxial ellipsoid representing the asteroid＇s shape. Applying this new model and a Markov Chain Monte Carlo method, we refine the photometric phase curve of asteroid （107） Camilla and obtain its absolute magnitude H = 7.026-0.054^＋0.052 mag, and phase function parameters G1=0.489-0.044^＋0.043 and G2 = 0.259-0.023^＋***, we also determine （107） Camilla＇s orientation of pole （74.1°-4.5°^＋4.3°,50.2°-5.0°^＋5.4°）. with rotational period of 4.843928-0.000001^＋0.000001 h, and axial ratios a/b ： 1.409-0.020^＋0.020 And b/c =1.249-0.060^＋0.063. Furthermore, according to the values of phase function parameters G1 and G2, we infer that asteroid （107） Camilla is an X-type asteroid.

关键词： minor planets, asteroids general phase curve -- minor planets, asteroids individual （107）Camilla -- techniques photometric

Secondary-electron radiation accompanying hadronic GeV-TeV gamma-rays from supernova remnants

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arXiv 2018年

作者： Huang, Yan Li, Zhuo Wang, Wei Zhao, Xiaohong Department of Astronomy School of Physics Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China School of Physics and Technology Wuhan University Wuhan430072 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China

The synchrotron radiation from secondary electrons and positrons (SEPs) generated by hadronic interactions in the shock of supernova remnant (SNR) could be a distinct evidence of cosmic ray (CR) production in SNR shocks. Here we provide a method where the observed gamma-ray flux from SNRs, created by pion decays, is directly used to derive the SEP distribution and hence the synchrotron spectrum. We apply the method to three gamma-ray bright SNRs. In the young SNR RX J1713.7-3946, if the observed GeV-TeV gamma-rays are of hadronic origin and the magnetic field in the SNR shock is B 0.5mG, the SEPs may produce a spectral bump at 10−5 − 10−2eV, exceeding the predicted synchrotron component of the leptonic model, and a soft spectral tail at 100keV, distinct from the hard spectral slope in the leptonic model. In the middle-aged SNRs IC443 and W44, if the observed gamma-rays are of hadronic origin, the SEP synchrotron radiation with B ∼ 400 − 500µG can well account for the observed radio flux and spectral slopes, supporting the hadronic origin of gamma-rays. Future microwave to far-infrared and hard X-ray (>100keV) observations are encouraged to constraining the SEP radiation and the gamma-ray origin in SNRs. Copyright © 2018, The Authors. All rights reserved.

关键词： Gamma rays

The spin of the second-born black hole in coalescing binary black holes

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arXiv 2018年

作者： Qin, Y. Fragos, T. Meynet, G. Andrews, J. Sørensen, M. Song, H.F. Geneva Observatory University of Geneva SauvernyCH-1290 Switzerland DARK Niels Bohr Institute University of Copenhagen Copenhagen2100 Denmark Foundation for Research and Technology - Hellas IESL Voutes Heraklion71110 Greece Physics Department & Institute of Theoretical & Computational Physics University of Crete Heraklion Crete71003 Greece College of Physics Guizhou University Guiyang CityGuizhou Province550025 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011

Context. Various binary black hole formation channels have been proposed since the first gravitational event GW150914 was discovered by the Advanced Laser Interferometer Gravitational-Wave Observatory (AdLIGO). For all evolutionary channels based on the evolution of isolated binaries, the immediate progenitor of the binary black hole is a close binary system composed of a black hole and a helium star. Aims. We study the spin angular momentum evolution of the helium star in order to constrain the spin of the second-born black hole. Methods. We perform detailed stellar structure and binary evolution calculations that take into account, mass-loss, internal differential rotation, and tidal interactions between the helium star and the black hole companion, where we also calculate the strength of the tidal interactions from first principles based on the structure of the helium stars. We systematically explore the parameter space of initial binary properties, including initial black hole and helium star masses, initial rotation of the helium star as well as metallicity. Results. We argue that the spin of the first-born black hole at its birth is negligible (. 0.1), hence the second-born black hole’s spin dominates the measured effective spin, χeff, from gravitational wave events of double black hole mergers. We find that tides can be important only when orbital periods are shorter than 2 days. Upon core collapse, the helium star produces a black hole (the second-born black hole in the system) with a spin that can span the entire range from zero to maximally spinning. We show that the bimodal distribution of the spin of the second-born black hole obtained in recent papers is mainly due to oversimplifying assumptions. We find an anti-correlation between the merging timescale of the two black holes, Tmerger, and the effective spin χeff. Finally, we provide new prescriptions for the tidal coefficient E2 for both H-rich and the helium-rich stars. Conclusions. To understand the

关键词： Gravity waves

The Radio and -ray variability analysis of S5 0716+714

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arXiv 2018年

作者： Li, H.Z. Jiang, Y.G. Yi, T.F. Guo, D.F. Chen, X. Zhang, H.M. Gao, Q.G. Lu, F.W. Ren, J.Y. Physics Department Yuxi Normal University Yuxi653100 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment Institute of Space Sciences Shandong University Weihai264209 China Physics Department Yunan Normal University Kunming Yunnan650092 China GXU-NAOC Center for Astrophysics and Space Sciences Department of Physics Guangxi University Nanning530004 China Guangxi Key Laboratory for the Relativistic Astrophysics Nanning530004 China

We have studied the variability of S5 0716+714 at radio 15 GHz and -ray band using three different methods. A possible periodicity of P15GHz = 266.0 ± 11.5 and P = 344.0 ± 16.4 days are obtained for radio 15 GHz and -ray light curves, respectively. The variability may be related to the intrinsically emission mechanism. The difference between the variability timescales of radio 15 GHz and -ray may be due to that the emission of radio 15 GHz is produced via the synchrotron process, while the -ray is produced by both the SSC and EC processes. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

Final Moments II: Observational Properties and Physical Modeling of CSM-Interacting Type II Supernovae

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arXiv 2024年

作者： Jacobson-Galán, W.V. Dessart, L. Davis, K.W. Kilpatrick, C.D. Margutti, R. Foley, R.J. Chornock, R. Terreran, G. Hiramatsu, D. Newsome, M. Padilla Gonzalez, E. Pellegrino, C. Howell, D.A. Filippenko, A.V. Anderson, J.P. Angus, C.R. Auchettl, K. Bostroem, K.A. Brink, T.G. Cartier, R. Coulter, D.A. de Boer, T. Drout, M.R. Earl, N. Ertini, K. Farah, J.R. Farias, D. Gall, C. Gao, H. Gerlach, M.A. Guo, F. Haynie, A. Hosseinzadeh, G. Ibik, A.L. Jha, S.W. Jones, D.O. Langeroodi, D. LeBaron, N. Magnier, E.A. Piro, A.L. Raimundo, S.I. Rest, A. Rest, S. Michael Rich, R. Rojas-Bravo, C. Sears, H. Taggart, K. Villar, V.A. Wainscoat, R.J. Wang, X.-F. Wasserman, A.R. Yan, S. Yang, Y. Zhang, J. Zheng, W. Department of Astronomy University of California BerkeleyCA94720-3411 United States Institut d'Astrophysique de Paris CNRS-Sorbonne Université 98 bis boulevard Arago ParisF-75014 France Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Northwestern University EvanstonIL60202 United States Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States Department of Physics University of California BerkeleyCA94720-7300 United States Las Cumbres Observatory 6740 Cortona Dr. Suite 102 GoletaCA93117 United States Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138-1516 United States The NSF AI Institute for Artificial Intelligence and Fundamental Interactions United States Department of Physics University of California Santa Barbara Santa BarbaraCA93111 United States Department of Astronomy University of Virginia CharlottesvilleVA22904 United States European Southern Observatory Alonso de Córdova 3107 Casilla 19 Santiago Chile Millennium Institute of Astrophysics MAS Nuncio Monsenor Sotero Sanz 100 Off. 104 Providencia Santiago Chile DARK Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen2200 Denmark Astrophysics Research Centre School of Mathematics and Physics Queen's University Belfast BelfastBT7 1NN United Kingdom School of Physics The University of Melbourne VIC3010 Australia Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States LSST-DA Catalyst Gemini Observatory NSF's National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Space Telescope Science Institute BaltimoreMD21218 United States Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States David A. Dunlap Department of Astronomy and Astrophysics University of Toronto 50 St. George Street TorontoONM5S 3H4 Canada Department of As

We present ultraviolet/optical/near-infrared observations and modeling of Type II supernovae (SNe II) whose early-time (δt 15 cm) circumstellar material (CSM). The observed electron-scattering broadened line profiles (i.e., IIn-like) of H i, He i/ii, C iv, and N iii/iv/v from the CSM persist on a characteristic timescale (tIIn) that marks a transition to a lower-density CSM and the emergence of Doppler-broadened features from the fast-moving SN ejecta. Our sample, the largest to date, consists of 39 SNe with early-time IIn-like features in addition to 35 "comparison" SNe with no evidence of early-time IIn-like features, all with ultraviolet observations. The total sample consists of 50 unpublished objects with a total of 474 previously unpublished spectra and 50 multiband light curves, collected primarily through the Young Supernova Experiment and Global Supernova Project collaborations. For all sample objects, we find a significant correlation between peak ultraviolet brightness and both tIIn and the rise time, as well as evidence for enhanced peak luminosities in SNe II with IIn-like features. We quantify mass-loss rates and CSM density for the sample through matching of peak multiband absolute magnitudes, rise times, tIIn and optical SN spectra with a grid of radiation hydrodynamics and non-local thermodynamic equilibrium (nLTE) radiative-transfer simulations. For our grid of models, all with the same underlying explosion, there is a trend between the duration of the electron-scattering broadened line profiles and inferred mass-loss rate: tIIn ≈ 3.8[M¤/(0.01 M☉ yr−1)] days. Copyright © 2024, The Authors. All rights reserved.

关键词： Supernovae