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

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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

An extreme X-ray variability event of a weak-line quasar

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arXiv 2020年

作者： Ni, Q. Brandt, W.N. Yi, W. Luo, B. Timlin, J.D. Hall, P.B. Liu, Hezhen Plotkin, R.M. Shemmer, O. Vito, F. Wu, Jianfeng Department of Astronomy & Astrophysics Pennsylvania State University Davey Lab University ParkPA16802 United States Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Department of Physics Pennsylvania State University University ParkPA16802 United States Yunnan Observatories Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China School of Astronomy and Space Science Nanjing University Nanjing Jiangsu210093 China Key Laboratory of Modern Astronomy and Astrophysics Nanjing University Ministry of Education Nanjing Jiangsu210093 China Collaborative Innovation Center of Modern Astronomy and Space Exploration Nanjing210093 China Department of Physics & Astronomy York University 4700 Keele Street TorontoONM3J 1P3 Canada Department of Physics University of Nevada 1664 N. Virginia St RenoNV89557 United States Department of Physics University of North Texas DentonTX76203 United States Instituto de Astrofísica Centro de Astroingeniería Facultad de Física Pontificia Universidad Católica de Chile Casilla 306 Santiago 22 Chile Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100012 China Department of Astronomy Xiamen University Xiamen Fujian361005 China

We report the discovery of an extreme X-ray ux rise (by a factor of 20) of the weak-line quasar SDSS J153913.47+395423.4 (hereafter SDSS J1539+3954) at z = 1.935. SDSS J1539+3954 is the most-luminous object among radio-quiet type 1 AGNs where such dramatic X-ray variability has been observed. Before the X-ray ux rise, SDSS J1539+3954 appeared X-ray weak compared with the expectation from its UV ux;after the rise, the ratio of its X-ray ux and UV ux is consistent with the majority of the AGN population. We also present a contemporaneous HET spectrum of SDSS J1539+3954, which demonstrates that its UV continuum level remains generally unchanged despite the dramatic increase in the X-ray ux, and its C iv emission line remains weak. The dramatic change only observed in the X-ray ux is consistent with a shielding model, where a thick inner accretion disk can block our line of sight to the central X-ray source. This thick inner accretion disk can also block the nuclear ionizing photons from reaching the high-ionization broad emission-line region, so that weak high-ionization emission lines are observed. Under this scenario, the extreme X-ray variability event may be caused by slight variations in the thickness of the disk. This event might also be explained by gravitational light-bending effects in a reection model. Copyright © 2020, The Authors. All rights reserved.

关键词： Electromagnetic wave emission

Determining the evolutionary stage of the d scuti star hip 80088 with asteroseismology

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arXiv 2018年

作者： Chen, Xinghao Li, Yan Yunnan Observatories Chinese Academy of Sciences P.O. Box 110 Kunming650216 China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences P.O. Box 110 Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China

We have computed a grid of theoretical models to fit the twelve oscillation modes of HIP 80088 observed by K2. HIP 80088 is determined to be a pre-main sequence star, in which CN cycle has not arrived at the equilibrium state. Mass fractions of C12 and N14 in metal composition are 0.1277+0.0064-0.0049and 0.1092+0.0057-0.0074respectively, indicating that twenty-eight percent of C12 have turned into N14. Meanwhile, our fitting results show that physical parameters of HIP 80088 converge to a small range: M = 1.68-1.78 Mo, Z = 0.015-0.018, ve = 120-136 km s-1, log g = 4.114-4.125, R = 1.882-1.914 Ro, t0 = 7636-7723 s, and age = 9.03-10.21 Myr. Based on our model fittings, f3 is suggested to be one radial mode, f2, f4, f8, and f11 to be four l = 1 modes, and f1, f5, f6, f7, f9, f10, and f12 to be seven l = 2 modes. In particularly, we find that (f2, f4, f8) form one complete triplet with the averaged frequency spacing of 16.045 μHz , and (f5, f7, f9, f10) form four components of one quintuplet with the averaged frequency spacing of 13.388 μHz. The two averaged frequency spacings are not equal. Based on the best-fitting model, those l = 2 modes of HIP 80088 are found to be mixed modes, which are p-dominated modes with pronounced g-mode features, while oscillation modes with l = 1 are p modes. Copyright © 2018, The Authors. All rights reserved.

关键词：

Determining the core radio luminosity function of radio agns via copula

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arXiv 2018年

作者： Yuan, Zunli Wang, Jiancheng Worrall, D.M. Zhang, Bin-Bin Mao, Jirong Yunnan Observatories 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 Beijing100012 China HH Wills Physics Laboratory University of Bristol Tyndall Avenue BristolBS8 1TL United Kingdom School of Astronomy and Space Science Nanjing University Nanjing210093 China Key Laboratory of Modern Astronomy and Astrophysics Nanjing University Ministry of Education China

The radio luminosity functions (RLFs) of active galactic nuclei (AGNs) are traditionally measured based on total emission, which doesn't reflect the current activity of the central black hole. The increasing interest in compact radio cores of AGNs requires determination of the RLF based on core emission (i.e., core RLF). In this work we have established a large sample (totaling 1207) of radio-loud AGNs, mainly consisting of radio galaxies (RGs) and steep-spectrum radio quasars (SSRQs). Based on the sample, we explore the relationship between core luminosity (Lc) and total luminosity (Lt) via a powerful statistical tool called "Copula". The conditional probability distribution p(log Lc | log Lt) is obtained. We derive the core RLF as a convolution of p(log Lc | log Lt) with the total RLF which was determined by previous work. We relate the separate RG and SSRQ core RLFs via a relativistic beaming model and find that SSRQs have an average Lorentz factor of γ = 9.84+3−2..6150, and that most are seen within 8◦ . θ . 45◦ of the jet axis. Compared with the total RLF which is mainly contributed by extended emission, the core RLF shows a very weak luminosity-dependent evolution, with the number density peaking around z ∼ 0.8 for all luminosities. Differences between core and total RLFs can be explained in a framework involving a combination of density and luminosity evolutions where the cores have significantly weaker luminosity evolution than the extended emission. Copyright © 2018, The Authors. All rights reserved.

关键词： Luminance

V752 Cen - A triple-lined spectroscopic contact binary with sudden and continuous period changes

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arXiv 2019年

作者： Zhou, X. Soonthornthum, B. Qian, S.-B. Lajús, E. Fernández P.O. Box 110 Kunming650216 China National Astronomical Research Institute of Thailand 260 Moo 4 T. Donkaew A. MaerimChiangmai50180 Thailand Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P. O. Box 110 Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China University of the Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata Paseo del Bosque s/n La Plata Pcia. Bs. As1900 Argentina Argentina

V752 Cen is a triple-lined spectroscopic contact binary. Its multi-color light curves were obtained in the years 1971 and 2018, independently. Photometric analyses reveal that the two sets of light curves produce almost consistent results. It contains a W-subtype totally eclipsing binary, and its mass ratio and fill-out factor are q = 3.35(1) and f = 29(2) %. The absolute elements of its two component stars were determined to be M1 = 0.39(2)M☉, M2 = 1.31(7)M☉, R1 = 0.77(1)R☉, R2 = 1.30(2)R☉, L1 = 0.75(3)L☉ and L2 = 2.00(7)L☉. The period of V752 Cen is 0.37023198 day. The 0.37-d period remained constant from its first measurement in 1971 until the year 2000. However, it changed suddenly around the year 2000 and has been increasing continuously at a rate of dP/dt = +5.05 × 10−7day · year−1 since then, which can be explained by mass transfer from the less massive component star to the more massive one with a rate of dMdt2 = 2.52 × 10−7M☉/year. The period variation of V752 Cen over the 48 years in which the period has been monitored is really unusual, and is potentially related to effects from the possible presence of a nearby third star or of a pair of stars in a second binary. Copyright © 2019, The Authors. All rights reserved.

关键词： Photometry

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