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arXiv 2019年

作者： Zhou, Hongyan Shi, Xiheng Yuan, Weimin Hao, Lei Chen, Xiangjun Ge, Jian Ji, Tuo Jiang, Peng Li, Ge Liu, Bifang Liu, Guilin Liu, Wenjuan Lu, Honglin Pan, Xiang Shen, Juntai Shu, Xinwen Sun, Luming Tian, Qiguo Wang, Huiyuan Wang, Tinggui Wu, Shengmiao Yang, Chenwei Zhang, Shaohua Zhong, Zhihao Antarctic Astronomy Research Division Key Laboratory for Polar Science of the State Oceanic Administration Polar Research Institute of China Shanghai China School of Astronomy and Space Sciences University of Science and Technology of China Hefei China Key Laboratory for Research in Galaxies and Cosmology of Chinese Academy of Sciences Department of Astronomy University of Science and Technology of China Hefei China National Astronomical Observatories of China Chinese Academy of Sciences Beijing China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing China Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai China Department of Astronomy University of Florida Bryant Space Science Center GainesvilleFL United States Yunnan Observatories Chinese Academy of Sciences Kunming China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming China Department of Physics Anhui Normal University Wuhu China

Quasars are high-luminosity active galactic nuclei believed to be powered by accretion of interstellar matter onto a super-massive black hole (SMBH) therein. Most of the observed energy is released in an accretion disk of inspiralling gas surrounding the SMBH. An enormous amount of fueling material, up to several tens solar masses per year, is expected to be transported inwards and consumed in the end. However, basic questions remain unanswered as to whether and how the accretion disks are supplied with external gas, since no disk-feeding inflow has hitherto been observed clearly. Here we report the discovery of highly redshifted broad absorption lines arising from neutral hydrogen and helium atoms in a small sample of quasars. Their absorption troughs show a broad range of Doppler velocities from zero extending continuously inward up to as high as ∼ 5, 000 km s−1, comparable to the free-fall speeds close to the SMBH and constraining the fastest in-falling gas to be within 104 gravitational radii. We thus see through streams of cold gas moving with a radially inward velocity component that spans an immense gradient—a result of gravitational acceleration by the central SMBH. Extensive photo-ionization modeling for the archetypical object SDSS J103516.20+142200.6 indicates the inflowing gas to be dense, thick and moderately ionized, with a characteristic distance to the SMBH of ∼ 1, 000 gravitational radii, possibly overlapping or close to the outer accretion disk. Our results present the first compelling evidence for the long-sought inflow directly feeding quasars’ accretion disks with external materials, likely originating from the dusty torus at a parsec scale. Our approach provides a new tool to probe the bulk of the so far elusive fueling inflows in quasars. Their studies may help address some of the fundamental questions concerning accretion physics, the onset and sustainment of quasar activity, and the SMBH growth at centers of most galaxies. Copyright © 2019,

关键词： Galaxies

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Massive stars exploding in a He-rich circumstellar medium − X. Flash spectral features in the Type Ibn SN 2019cj and observations of SN 2018jmt

arXiv

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arXiv 2024年

作者： Wang, Z.-Y. Pastorello, A. Maeda, K. Reguitti, A. Cai, Y.-Z. Howell, D. Andrew Benetti, S. Buckley, D. Cappellaro, E. Carini, R. Cartier, R. Chen, T.-W. Elias-Rosa, N. Fang, Q.-L. Gal-Yam, A. Gangopadhyay, A. Gromadzki, M. Gan, W.-P. Hiramatsu, D. Hu, M.-K. Inserra, C. McCully, C. Nicholl, M. Olivares, F.E. Pignata, G. Pineda-García, J. Pursiainen, M. Ragosta, F. Rau, A. Roy, R. Sollerman, J. Tartaglia, L. Terreran, G. Valerin, G. Wang, Q. Wang, S.-Q. Young, D.R. Aryan, A. Bronikowski, M. Concepcion, E. Galbany, L. Lin, H. Melandri, A. Petrushevska, T. Ramirez, M. Shi, D.-D. Warwick, B. Zhang, J.-J. Wang, B. Wang, X.-F. Zhu, X.-J. School of Physics and Astronomy Beijing Normal University Beijing100875 China Department of Physics Faculty of Arts and Sciences Beijing Normal University Zhuhai519087 China INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan Merate23807 Italy Yunnan Observatories Chinese Academy of Sciences Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Las Cumbres Observatory 6740 Cortona Drive Suite 102 GoletaCA93117-5575 United States Department of Physics University of California Santa BarbaraCA93106-9530 United States South African Astronomical Observatory PO Box 9 Observatory Cape Town7935 South Africa INAF - Osservatorio Astronomico di Roma via Frascati 33 Monte Porzio CatoneI-00078 Italy Instituto de Estudios Astrofísicos Facultad de Ingeniería y Ciencias Universidad Diego Portales Av. Ejército Libertador 441 Santiago Chile Graduate Institute of Astronomy National Central University 300 Jhongda Road Jhongli32001 Taiwan Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain 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 Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warszawa00-478 Poland Guangxi Key Laboratory for Relativistic Astrophysics School of Physical Science and Technology Guangxi University Nanning530004 China 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 Tsinghua University Beijing10008

We present optical and near-infrared observations of two Type Ibn supernovae (SNe), SN 2018jmt and SN 2019cj. Their light curves have rise times of about 10 days, reaching an absolute peak magnitude of Mg(SN 2018jmt) = −19.07 ± 0.37 and MV(SN 2019cj) = −18.94 ± 0.19 mag, respectively. The early-time spectra of SN 2018jmt are dominated by a blue continuum, accompanied by narrow (600−1000 km s−1) He i lines with P-Cygni profile. At later epochs, the spectra become more similar to those of the prototypical SN Ibn 2006jc. At early phases, the spectra of SN 2019cj show flash ionisation emission lines of C iii, N iii and He ii superposed on a blue continuum. These features disappear after a few days, and then the spectra of SN 2019cj evolve similarly to those of SN 2018jmt. The spectra indicate that the two SNe exploded within a He-rich circumstellar medium (CSM) lost by the progenitors a short time before the explosion. We model the light curves of the two SNe Ibn to constrain the progenitor and the explosion parameters. The ejecta masses are consistent with either that expected for a canonical SN Ib (~ 2 M☉) or those from a massive WR star (> ~ 4 M☉), with the kinetic energy on the order of 1051 erg. The lower limit on the ejecta mass (> ~ 2 M☉) argues against a scenario involving a relatively low-mass progenitor (e.g., MZAMS ~ 10 M☉). We set a conservative upper limit of ~ 0.1 M☉ for the 56Ni masses in both SNe. From the light curve modelling, we determine a two-zone CSM distribution, with an inner, flat CSM component, and an outer CSM with a steeper density profile. The physical properties of SN 2018jmt and SN 2019cj are consistent with those expected from the core collapse of relatively massive, stripped-envelope (SE) stars. © 2024, CC BY.

关键词： Kinetic energy

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Statistical analysis on XMM-Newton X-ray flares of Mrk 421: distributions of peak flux and flaring time duration

arXiv

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arXiv 2018年

作者： Yan, Dahai Yang, Shenbang Zhang, Pengfei Dai, Benzhong Wang, Jiancheng Zhang, Li Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatory Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory of Astroparticle Physics of Yunnan Province Yunnan University Kunming650091 China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008

The energy dissipation mechanism in blazar jet is unknown. Blazar’s flares could provide insights on this problem. Here we report statistical results of XMM-Newton X-ray flares of Mrk 421. We analyze all public XMM-Newton X-ray observations for Mrk 421, and construct the light curves. Through fitting light curves, we obtain the parameters of flare-profiles, such as peak flux (Fp) and flaring time duration (Tfl). It is found that both the distributions of Fp and Tfl obey a power-law form, with the same index of αF = αT ≈ 1. The statistical properties are consistent with the predictions by a self-organized criticality (SOC) system with energy dissipation in one-dimensional space. This is similar to solar flare, but with different space dimensions of the energy dissipation domain. This suggests that X-ray flaers of Mrk 421 are possibly driven by a magnetic reconnection mechanism. Moreover, in the analysis, we find that variability on timescale of ∼ 1000 s frequently appears. Such rapid variability indicates a magnetic field of ≥ 2.1δD−1/3 G (δD is the Doppler factor) in emission region. Copyright © 2018, The Authors. All rights reserved.

关键词： Energy dissipation

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Erratum: Variations of the mixing character of dipolar mixed modes in red giant stars

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Monthly Notices of the Royal Astronomical Society 2020年第1期497卷 167-172页

作者： C Jiang M Cunha J Christensen-Dalsgaard Q S Zhang School of Physics and Astronomy Sun Yat-Sen University No. 135 Xingang Xi Road Guangzhou 510275 P. R. China Instituto de Astrofísica e Ciências do Espaço Universidade do Porto CAUP Rua das Estrelas PT-4150-762 Porto Portugal jiangch53@*** Instituto de Astrofísica e Ciências do Espaço Universidade do Porto CAUP Rua das Estrelas PT-4150-762 Porto Portugal School of Physics and Astronomy University of Birmingham Birmingham B15 2TT United Kingdom Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Ny Munkegade 120 DK-8000 Aarhus C Denmark Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming 650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing 100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming 650216 China University of Chinese Academy of Sciences Beijing 100049 China

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ALMA REVEALS A GAS-RICH, MAXIMUM-STARBURST IN THE HYPERLUMINOUS, DUST-OBSCURED QUASAR W0533−3401 AT z ∼ 2.9

arXiv

引用

arXiv 2019年

作者： Fan, Lulu Knudsen, Kirsten K. Han, Yunkun Tan, Qing-hua CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China School of Astronomy and Space Sciences University of Science and Technology of China HefeiAnhui230026 China Shandong Provincial Key Lab of Optical Astronomy and Solar-Terrestrial Environment Institute of Space Science Shandong University Weihai264209 China Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory OnsalaSE-439 92 Sweden Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Purple Mountain Observatory & Key Laboratory for Radio Astronomy Chinese Academy of Sciences 8 Yuanhua Road Nanjing210034 China

We present ALMA observations and multiwavelength spectral energy distribution (SED) analysis in a WISE-selected, hyperluminous dust-obscured quasar W0533−3401 at z = 2.9. We derive its physical properties of each component, such as molecular gas, stars, dust and the central supermassive black hole (SMBH). Both the dust continuum at 3 mm and the CO(3 − 2) line are detected. The derived molecular gas mass Mgas = 8.4 × 1010 M☉ and its fraction fgas = 0.7 suggest that W0533−3401 is gas-rich. The star formation rate (SFR) has been estimated to be ∼ 3000 − 7000 M☉ yr−1 by using different methods. The high values of SFR and specific SFR suggest that W0533−3401 is a maximum-starburst. The corresponding gas depletion timescales are very short (tdepl ∼ 12 − 28 Myr). The CO(3 − 2) emission line is marginally resolved and has a velocity gradient, which is possibly due to a rotating gas disk, gas outflow or merger. Finally, we infer the black hole mass growth rate of W0533−3401 (Ṁ BH = 49 M☉ yr−1), which suggests a rapid growth of the central SMBH. The observed black hole to stellar mass ratio MBH/M* of W0533−3401, which is dependent on the adopted Eddington ratio, is over one order of magnitude higher than the local value, and is evolving towards the evolutionary trend of unobscured quasars. Our results are consistent with the scenario that W0533−3401, with both a gas-rich maximum-starburst and a rapid black hole growth, is experiencing a short transition phase towards an unobscured quasar. Copyright © 2019, The Authors. All rights reserved.

关键词： Galaxies

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Synchrotron polarization radiative transfer: Relativistic thermal electrons contribution

arXiv

引用

arXiv 2018年

作者： Mao, Jirong Covino, Stefano Wang, Jiancheng Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan Province650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China I-23807 Italy

Relativistic thermal electrons moving in a large-scale magnetic field can produce synchrotron radiation. Linear synchrotron polarization can also be produced by the relativistic thermal electrons. In this paper, we utilize a hybrid thermalnonthermal electron energy distribution to calculate circular synchrotron polarization. We further compute the radiative transfer of the synchrotron polarization in the optical and radio bands when we consider the contribution of the thermal electrons. We attempt to apply the polarization results to some astrophysical objects, such as kilonova like AT 2017gfo/GW170817, the fast radio burst (FRB), the Gamma-ray burst (GRB) afterglow, and the supernova remnant (SNR). The large optical depth of radiative transfer eαects the small polarization degrees of these populations when the media surrounding the synchrotron sources take heavy absorption to the polarized photons. We need a strong magnetic field in our model to reproduce the linear and circular polarization properties that were observed in FRB 140514. This indicates that FRBs have a neutron star origin. Copyright © 2018, The Authors. All rights reserved.

关键词： Polarization

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Search for γ-ray emission from dark matter particle interactions from the Andromeda and Triangulum galaxies with the Fermi Large Area Telescope

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Physical Review D 2019年第12期99卷 123027-123027页

作者： Mattia Di Mauro Xian Hou Christopher Eckner Gabrijela Zaharijas Eric Charles NASA Goddard Space Flight Center Greenbelt Maryland 20771 USA Catholic University of America Department of Physics Washington D.C. 20064 USA Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming 650216 People’s Republic of China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming 650216 People’s Republic of China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing 100012 People’s Republic of China Center for Astrophysics and Cosmology University of Nova Gorica Vipavska 13 SI-5000 Nova Gorica Slovenia SLAC National Accelerator Laboratory Stanford University Stanford California 94305 USA

The Andromeda (M31) and Triangulum (M33) galaxies are the closest Local Group galaxies to the Milky Way, being only 785 and 870 kpc away. These two galaxies provide an independent view of high-energy processes that are often obscured in our own Galaxy, including possible signals of dark matter (DM) particle interactions. The Fermi Large Area Telescope (Fermi-LAT) preliminary eight year list of sources includes both M31, which is detected as extended with a size of about 0.4°, and M33, which is detected as a pointlike source. The spatial morphology of M31 γ-ray emission could trace a population of unresolved sources and energetic particles originating in sources not related to massive star formation. Alternatively, the γ-ray emission could also be an indication of annihilation or decay of DM particles. We investigate these two possibilities using almost 10 years of data from the Fermi-LAT. An interpretation that involves only a DM γ-ray emission is in tension with the current limits from other searches, such as those targeting Milky Way dwarf spheroidal galaxies. When we include a template of astrophysical emission, tuned on γ-ray data or from observations of these galaxies in other wavelengths, we do not find any significant evidence for a DM contribution and we set limits for the annihilation cross section that probe the thermal cross section for DM masses up to a few tens of GeV in the bb¯ and τ+τ− channels. For models where the DM substructures have masses above 10−6 solar masses our limits probe the DM interpretation of the Fermi-LAT Galactic center excess. We provide also the lower limit for the DM lifetime assuming the same spatial models of the DM distribution in M31 and M33.

关键词： Cosmic ray sources Gamma ray astronomy Particle dark matter

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SOLAR MODELS WITH CONVECTIVE OVERSHOOT, THE SOLAR-WIND MASS LOSS, AND A PMS DISK ACCRETION: HELIOSEISMIC QUANTITIES, LI DEPLETION AND NEUTRINO FLUXES

arXiv

引用

arXiv 2019年

作者： Zhang, Qian-Sheng Li, Yan Christensen-Dalsgaard, Jørgen Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Aarhus CDK-8000 Denmark Kavli Institute for Theoretical Physics University of California Santa Barbara CA93106-4030 United States

Helioseismic observations have revealed many properties of the Sun: the depth and the helium abundance of the convection zone, the sound-speed and the density profiles in the solar interior. Those constraints have been used to judge the stellar evolution theory. With the old solar composition (e.g., GS98), the solar standard model is in reasonable agreement with the helioseismic constraints. However, a solar model with revised composition (e.g., AGSS09) with low abundance Z of heavy elements cannot be consistent with those constraints. This is the so-called "solar abundance problem", standing for more than ten years even with the recent upward revised Ne abundance. Many mechanisms have been proposed to mitigate the problem. However, there is still not a low-Z solar model satisfying all helioseismic constraints. In this paper, we report a possible solution to the solar abundance problem. With some extra physical processes that are not included in the standard model, solar models can be significantly improved. Our new solar models with convective overshoot, the solar wind, and an early mass accretion show consistency with helioseismic constraints, the solar Li abundance, and observations of solar neutrino fluxes. Copyright © 2019, The Authors. All rights reserved.

关键词： Solar wind

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Multi-wavelength observations of the BL Lac object Fermi J1544-0649: One year after its awakening

arXiv

引用

arXiv 2020年

作者： Tam, P.H.T. Pal, P.S. Cui, Y.D. Jiang, N. Sotnikova, Y. Yang, C.W. Wang, L.Z. Tang, B.T. Li, Y.B. Mao, J. Kong, A.K.H. Zhong, Z.H. Ding, J. Mufakharov, T. Fan, J.F. Dou, L.M. Shen, R.F. Ai, Y.L. School of Physics and Astronomy Sun Yat-sen University Guangzhou510275 China CAS Key Laboratory for Researches in Galaxies and Cosmology University of Sciences and Technology of China Hefei Anhui230026 China Special Astrophysical Observatory Russian Academy of Sciences Nizhnij Arkhyz369167 Russia Polar Research Institute of China 451 Jinqiao Road Shanghai200136 China Chinese Academy of Sciences South America Center for Astronomy China-Chile Joint Center for Astronomy Camino El Observatorio #1515 Las Condes Santiago Chile Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Institute of Astronomy National Tsing Hua University 101 Section 2. Kuang-Fu Road Hsinchu30013 Taiwan Department of Astronomy & Astrophysics University of California Santa Cruz 1156 High Street Santa CruzCA95060 United States Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Kazan Federal University 18 Kremlyovskaya St. Kazan420008 Russia Center for Astrophysics Guangzhou University Guangzhou510006 China

We report observations of a transient source Fermi J1544-0649 from radio to γrays. Fermi J1544-0649 was discovered by the Fermi-LAT in May 2017. Followup Swift-XRT observations revealed three flaring episodes through March 2018, and the peak X-ray flux is about 103 higher than the ROSAT all-sky survey (RASS) flux upper limit. Optical spectral measurements taken by the Magellan 6.5-m telescope and the Lick-Shane telescope both show a largely featureless spectrum, strengthening the BL Lac interpretation first proposed by Bruni et al. (2018). The optical and mid-infrared (MIR) emission goes to a higher state in 2018, when the flux in high energies goes down to a lower level. Our RATAN-600m measurements at 4.8 GHz and 8.2 GHz do not indicate any significant radio flux variation over the monitoring seasons in 2017 and 2018, nor deviate from the archival NVSS flux level. During GeV flaring times, the spectrum is very hard (Γγ ∼1.7) in the GeV band and at times also very hard ((ΓX 2) in the X-rays, similar to a high-synchrotron-peak (or even an extreme) BL Lac object, making Fermi J1544-0649 a good target for ground-based Cherenkov telescopes. Copyright © 2020, The Authors. All rights reserved.

关键词： Surveys

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SN 2020pvb: a Type IIn-P supernova with a precursor outburst

arXiv

引用

arXiv 2024年

作者： Elias-Rosa, Nancy Brennan, Seán J. Benetti, Stefano Cappellaro, Enrico Pastorello, Andrea Kozyreva, Alexandra Lundqvist, Peter Fraser, Morgan Anderso, Joseph P. Cai, Yong-Zhi Chen, Ting-Wan Dennefeld, Michel Gromadzki, Mariusz Gutiérrez, Claudia P. Ihanec, Nada Inserra, Cosimo Kankare, Erkki Kotak, Rubina Mattila, Seppo Moran, Shane Müller-Bravo, Tomás E. Pessi, Priscila J. Pignata, Giuliano Reguitti, Andrea Reynolds, Thomas M. Smartt, Stephen J. Smith, Ken Tartaglia, Leonardo Valerin, Giorgio de Boer, Thomas Chambers, Kenneth Gal-Yam, Avishay Gao, Hua Geier, Stefan Mazzali, Paolo A. Nicholl, Matt Ragosta, Fabio Rest, Armin Yaron, Ofer Young, David R. INAF – Osservatorio Astronomico di Padova vicolo dell’Osservatorio 5 PadovaI-35122 Italy Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden School of Physics O’Brien Centre for Science North University College Dublin Belfield Dublin 4 Ireland Heidelberger Institut für Theoretische Studien Schloss-Wolfsbrunnenweg 35 Heidelberg69118 Germany European Southern Observatory Alonso de Córdova 3107 Casilla 19 Santiago Chile Nuncio Monseñor Sótero Sanz 100 Off. 104 Providencia Santiago Chile Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China Graduate Institute of Astronomy National Central University 300 Jhongda Road Jhongli32001 Taiwan 98bis Boulevard Arago ParisF-75014 France Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warszawa00-478 Poland BarcelonaE-08034 Spain Cardiff Hub for Astrophysics Research and Technology School of Physics & Astronomy Cardiff University Queens Buildings The Parade CardiffCF24 3AA United Kingdom Tuorla Observatory Department of Physics and Astronomy University of Turku FI-20014 Finland Turku Collegium for Science Medicine and Technology University of Turku TurkuFI-20014 Finland School of Sciences European University Cyprus Diogenes street Engomi Nicosia1516 Cyprus Instituto de Alta Investigación Universidad de Tarapacá Casilla 7D Arica Chile MerateI-23807 Italy Cosmic DAWN centre Niels Bohr Institute University of Copenhagen Jagtvej 128 København N2200 Denmark Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Astrophysics Research Centre School of Mathematics and Physics Queen’s University Be

We present photometric and spectroscopic data sets for SN 2020pvb, a Type IIn-P supernova (SN) similar to SNe 1994W, 2005cl, 2009kn and 2011ht, with a precursor outburst detected (PS1 w-band ∼ -13.8 mag) around four months before the B-band maximum light. SN 2020pvb presents a relatively bright light curve peaking at MB = -17.95 ± 0.30 mag and a plateau lasting at least 40 days before it went in solar conjunction. After this, the object is no longer visible at phases > 150 days above -12.5 mag in the B-band, suggesting that the SN 2020pvb ejecta interacts with a dense spatially confined circumstellar envelope. SN 2020pvb shows in its spectra strong Balmer lines and a forest of Fe ii lines with narrow P Cygni profiles. Using archival images from the Hubble Space Telescope, we constrain the progenitor of SN 2020pvb to have a luminosity of log(L/L☉) 5.4, ruling out any single star progenitor over 50 M☉. All in all, SN 2020pvb is a Type IIn-P whose progenitor star had an outburst ∼ 0.5 yr before the final explosion, the material lost during this outburst is probably playing a role in shaping the physical properties of the supernova. Copyright © 2024, The Authors. All rights reserved.

关键词： Supernovae

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