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arXiv 2018年

作者： Li, Rui Shu, Yiping Wang, Jiancheng Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District 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 Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Purple Mountain Observatory Chinese Academy of Sciences 2 West Beijing Road Nanjing Jiangsu210008 China Institute of Astronomy Madingley Road CambridgeCB3 0HA United Kingdom

We measure the total mass-density profiles out to three effective radii for a sample of 63 z ∼ 0.5, massive early-type galaxies (ETGs) acting as strong gravitational lenses through a joint analysis of lensing and stellar dynamics. The compilation is selected from three galaxy-scale strong-lens samples including the Baryon Oscillation Spectro- scopic Survey (BOSS) Emission-Line Lens Survey (BELLS), BELLS for GALaxy-Lya EmitteR sYstems Survey, and Strong Lensing Legacy Survey (SL2S). Utilizing the wide source-redshift coverage (0.8-3.5) provided by these three samples, we build a statistically significant ensemble of massive ETGs for which robust mass measurements can be achieved within a broad range of Einstein radii up to three effective radii. Char- acterizing the three-dimensional total mass-density distribution by a power-law profile as ρ ∞ r-γ, we find that the average logarithmic density slope for the entire sample is (γ) = 2.000+0.033-0.032 (68%CL) with an intrinsic scatter δ = 0.180+0.032-0.028. Further parame- terizing (γ) as a function of redshift z and ratio of Einstein radius to effective radius Rein/Reff, we find the average density distributions of these massive ETGs become steeper at larger radii and later cosmic times with magnitudes d(γ)/dz = -0.309+0.166-0.160 and d(γ)/d log10 Rein/Reff= 0.194+0.092-0.083. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

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Forbidden hugs in pandemic times: IV. Panchromatic evolution of three luminous red novae

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Astronomy and Astrophysics 2023年 671卷

作者： Pastorello, A. Valerin, G. Fraser, M. Reguitti, A. Elias-Rosa, N. Filippenko, A.V. Rojas-Bravo, C. Tartaglia, L. Reynolds, T.M. Valenti, S. Andrews, J.E. Ashall, C. Bostroem, K.A. Brink, T.G. Burke, J. Cai, Y.-Z. Cappellaro, E. Coulter, D.A. Dastidar, R. Davis, K.W. Dimitriadis, G. Fiore, A. Foley, R.J. Fugazza, D. Galbany, L. Gangopadhyay, A. Geier, S. Gutiérrez, C.P. Haislip, J. Hiramatsu, D. Holmbo, S. Howell, D.A. Hsiao, E.Y. Hung, T. Jha, S.W. Kankare, E. Karamehmetoglu, E. Kilpatrick, C.D. Kotak, R. Kouprianov, V. Kravtsov, T. Kumar, S. Li, Z.-T. Lundquist, M.J. Lundqvist, P. Matilainen, K. Mazzali, P.A. McCully, C. Misra, K. Morales-Garoffolo, A. Moran, S. Morrell, N. Newsome, M. Padilla Gonzalez, E. Pan, Y.-C. Pellegrino, C. Phillips, M.M. Pignata, G. Piro, A.L. Reichart, D.E. Rest, A. Salmaso, I. Sand, D.J. Siebert, M.R. Smartt, S.J. Smith, K.W. Srivastav, S. Stritzinger, M.D. Taggart, K. Tinyanont, S. Yan, S.-Y. Wang, L. Wang, X.-F. Williams, S.C. Wyatt, S. Zhang, T.-M. De Boer, T. Chambers, K. Gao, H. Magnier, E. INAF Osservatorio Astronomico di Padova Vicolo dell Osservatorio 5 Padova35122 Italy Universitá Degli Studi di Padova Dipartimento di Fisica e Astronomia Vicolo dell Osservatorio 2 Padova35122 Italy School of Physics O Brien Centre for Science North University College Dublin Dublin 4 Belfield Ireland Instituto de Astrofísica Facultad de Ciencias Exactas Universidad Andres Bello Fernández Concha 700 Las Condes Santiago Chile Nuncio Monsenor Sótero Sanz 100 Santiago Providencia8320000 Chile CSIC Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Tuorla Observatory Department of Physics and Astronomy University of Turku Turku20014 Finland Niels Bohr Institute University of Copenhagen Jagtvej 128 København N2200 Denmark Department of Physics and Astronomy University of California Davis 1 Shields Avenue DavisCA95616-5270 United States Gemini Observatory 670 North A ohoku Place HiloHI96720-2700 United States Department of Physics Virginia Tech 850 West Campus Drive BlacksburgVA24061 United States DIRAC Institute Department of Astronomy University of Washington 3910 15th Avenue NE SeattleWA98195-0002 United States Las Cumbres Observatory 6740 Cortona Dr. Suite 102 GoletaCA93117 United States Department of Physics University of California Santa BarbaraCA93106 United States Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Tsinghua University Beijing100084 China School of Physics Trinity College Dublin University of Dublin Dublin Ireland Fondazione Bruno Kessler Trento38123 Italy INFN-TI

We present photometric and spectroscopic data on three extragalactic luminous red novae (LRNe): AT 2018bwo, AT 2021afy, and AT 2021blu. AT 2018bwo was discovered in NGC 45 (at about 6.8 Mpc) a few weeks after the outburst onset. During the monitoring period, the transient reached a peak luminosity of 1040 erg s1. AT 2021afy, hosted by UGC 10043 (49.2 Mpc), showed a double-peaked light curve, with the two peaks reaching a similar luminosity of 2.1(±0.6) - 1041 erg s1. Finally, for AT 2021blu in UGC 5829 (∼8.6 Mpc), the pre-outburst phase was well-monitored by several photometric surveys, and the object showed a slow luminosity rise before the outburst. The light curve of AT 2021blu was sampled with an unprecedented cadence until the object disappeared behind the Sun, and it was then recovered at late phases. The light curve of LRN AT 2021blu shows a double peak, with a prominent early maximum reaching a luminosity of 6.5 - 1040 erg s1, which is half of that of AT 2021afy. The spectra of AT 2021afy and AT 2021blu display the expected evolution for LRNe: a blue continuum dominated by prominent Balmer lines in emission during the first peak, and a redder continuum consistent with that of a K-type star with narrow absorption metal lines during the second, broad maximum. The spectra of AT 2018bwo are markedly different, with a very red continuum dominated by broad molecular features in absorption. As these spectra closely resemble those of LRNe after the second peak, AT 2018bwo was probably discovered at the very late evolutionary stages. This would explain its fast evolution and the spectral properties compatible with that of an M-type star. From the analysis of deep frames of the LRN sites years before the outburst, and considerations of the light curves, the quiescent progenitor systems of the three LRNe were likely massive, with primaries ranging from about 13 M for AT 2018bwo, to 141+4 Mo for AT 2021blu, and over 40 M for AT 2021afy. © 2023 The Authors.

关键词： Luminance

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Application of screened Coulomb potential in fitting DBV star PG 0112+104

arXiv

引用

arXiv 2017年

作者： Chen, H. Institute of Astrophysics Chuxiong Normal University Chuxiong675000 China School of Physics and Electronical Science Chuxiong Normal University Chuxiong675000 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P.O. Box 110 Kunming650011 China

With 78.7 days of observations for PG 0112+104, a pulsating DB star, from Campaign 8 of Kepler 2 mission, Hermes et al. made a detailed mode identification. A reliable mode identification, with 5 l = 1 modes, 3 l = 2 modes, and 3 l = 1 or 2 modes, was identified. Grids of DBV star models are evolved by WDEC with element diffusion effect of pure Coulomb potential and screened Coulomb potential. Fitting the identified modes of PG 0112+104 by the calculated ones, we studied the difference of element diffusion effect between adopting pure Coulomb potential and screened Coulomb potential. Our aim is to reduce the fitting error by studying new input physics. The starting models including their chemical composition profile are from white dwarf models evolved by MESA. They were calculated following the stellar evolution from the main sequence to the start of the white dwarf cooling sequences. The optimal parameters are basically consistent with that of previous spectroscopic and asteroseismological studies. The pure and screened Coulomb potential lead to different composition profiles of the C/O-He interface area. High k modes are very sensitive to the area. However, most of the observed modes for PG 0112+104 are low k modes. The σRMS taking the screened Coulomb potential is reduced by 4% compared with taking the pure Coulomb potential when fitting the identified low k modes of PG 0112+104. Fitting the Kepler 2 data with our models improved the σRMS of the fit by 27%. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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Physical parameters and orbital period variation of a newly discovered cataclysmic variable GSC 4560-02157

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Research in Astronomy and Astrophysics 2016年第10期16卷 55-62页

作者： Zhong-Tao Han Sheng-Bang Qian Irina Voloshina Vladimir G. Metlov Li-Ying Zhu Lin-Jia Li Yunnan Observatories Chinese Academy of Sciences Kunming 650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650216China University of Chinese Academy of Sciences Beijing 100049 China Sternberg Astronomical Institute Moscow State University Universitetskij prospect 13 Moscow 119992 Russia

GSC 4560-02157 is a new eclipsing cataclysmic variable with an orbital period of 0.265359 days. By using the published V- and R-band data together with our observations, we discovered that the O - C curve of GSC 4560-02157 may show a cyclic variation with a period of 3.51 years and an amplitude of 1.40 min. If this variation is caused by a light travel-time effect via the existence of a third body, then its mass can be derived as M3 sin i1≈ 91.08 Mjup, and it should be a low-mass star. In addition, several physical parameters were measured. The color of the secondary star was determined to be V - R = 0.77（±0.03） which corresponds to a spectral type of K2-3. The secondary star＇s mass was estimated as M2 = 0.73（±0.02） Mo by combing the derived V - R value around phase 0 with the assumption that it obeys the mass-luminosity relation for main sequence stars. This mass is consistent with the mass-period relation for CV donor stars. For the white dwarf, the eclipse durations and contacts of the white dwarf yield an upper limit on the white dwarf＇s radius corresponding to a lower limit on mass of M1 ≈ 0.501 M⊙. The overestimated radius and previously published spectral data indicate that the boundary layer may have a very high temperature.

关键词： techniques： photometric -- stars： binaries： cataclysmic variables -- stars： individual：GSC 4560-02157

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A Polarization Sequence for Type Ia Supernovae?

arXiv

引用

arXiv 2017年

作者： Meng, X. Zhang, J. Han, Z. 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 20A Datun Road Chaoyang District Beijing100012 China

Early polarization observations on Type Ia supernovae (SNe Ia) may reveal the geometry of supernova ejecta, and then put constraints on their explosion mechanism and their progenitor model. We performed a literature search of SNe Ia with polarization measurements and determined the polarization and relative equivalent width (REW) of Si II 635.5-nm absorption feature at -5 days after the maximum light. We found that either the distribution of observed polarization degree is bimodal, i.e. the broad line SNe Ia have systematically higher polarization than all other SNe Ia, or all kind of SNe Ia share the same polarization sequence, i.e. the polarization of Si II 635.5-nm absorption feature increases with the REW. We also discussed the potential meaning of the discovery on the explosion mechanism and progenitor model of SNe Ia. Copyright © 2017, The Authors. All rights reserved.

关键词： Supernovae

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The broad-lined Type-Ic supernova SN 2022xxf with extraordinary two-humped light curves

arXiv

引用

arXiv 2023年

作者： Kuncarayakti, H. Sollerman, J. Izzo, L. Maeda, K. Yang, S. Schulze, S. Angus, C.R. Aubert, M. Auchettl, K. Della Valle, M. Dessart, L. Hinds, K. Kankare, E. Kawabata, M. Lundqvist, P. Nakaoka, T. Perley, D. Raimundo, S.I. Strotjohann, N.L. Taguchi, K. Cai, Y.-Z. Charalampopoulos, P. Fang, Q. Fraser, M. Gutiérrez, C.P. Imazawa, R. Kangas, T. Kawabata, K.S. Kotak, R. Kravtsov, T. Matilainen, K. Mattila, S. Moran, S. Murata, I. Salmaso, I. Anderson, J.P. Ashall, C. Bellm, E.C. Benetti, S. Chambers, K.C. Chen, T.-W. Coughlin, M. De Colle, F. Fremling, C. Galbany, L. Gal-Yam, A. Gromadzki, M. Groom, S.L. Hajela, A. Inserra, C. Kasliwal, M.M. Mahabal, A.A. Martin-Carrillo, A. Moore, T. Müller-Bravo, T.E. Nicholl, M. Ragosta, F. Riddle, R.L. Sharma, Y. Srivastav, S. Stritzinger, M.D. Wold, A. Young, D.R. Tuorla Observatory Department of Physics and Astronomy University of Turku FI-20014 Finland University of Turku FI-20014 Finland Department of Astronomy Oskar Klein Centre AlbaNova Stockholm10691 Sweden DARK Niels Bohr Institute University of Copenhagen Copenhagen Denmark Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan Henan Academy of Sciences Henan Zhengzhou450046 China The Oskar Klein Centre Department of Physics Stockholm University AlbaNova University Center StockholmSE 106 91 Sweden Université Clermont Auvergne CNRS IN2P3 LPC Clermont-Ferrand France School of Physics The University of Melbourne ParkvilleVIC3010 Australia Sydney2006 Australia Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Capodimonte Astronomical Observatory INAF-Napoli Salita Moiariello 16 NapoliI-80131 Italy Institut d’Astrophysique de Paris CNRS-Sorbonne Université 98 bis boulevard Arago ParisF-75014 France Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Turku Collegium for Science Medicine and Technology University of Turku TurkuFI-20014 Finland Hiroshima Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Department of Physics and Astronomy University of California Los AngelesCA United States Department of Physics & Astronomy University of Southampton Southampton United Kingdom Benoziyo Center for Astrophysics The Weizmann Institute of Science Rehovot76100 Israel Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China School of Physics O’Brien Centre for Science North University College Dublin Belfield Dublin 4 Dublin Ireland Department of Physics Graduate School

We report on our study of supernova (SN) 2022xxf based on observations obtained during the first four months of its evolution. The light curves (LCs) display two humps of similar maximum brightness separated by 75 days, unprecedented for a broad-lined (BL) Type Ic supernova (SN IcBL). SN 2022xxf is the most nearby SN IcBL to date (in NGC 3705, z = 0.0037, at a distance of about 20 Mpc). Optical and near-infrared photometry and spectroscopy are used to identify the energy source powering the LC. Nearly 50 epochs of high signal-to-noise-ratio spectroscopy were obtained within 130 days, comprising an unparalleled dataset for a SN IcBL, and one of the best-sampled SN datasets to date. The global spectral appearance and evolution of SN 2022xxf points to typical SN Ic/IcBL, with broad features (up to ∼ 14000 km s−1) and a gradual transition from the photospheric to the nebular phase. However, narrow emission lines (corresponding to ∼ 1000−2500 km s−1) are present in the spectra from the time of the second rise, suggesting slower-moving circumstellar material (CSM). These lines are subtle, in comparison to the typical strong narrow lines of CSM-interacting SNe, for example, Type IIn, Ibn, and Icn, but some are readily noticeable at late times such as in Mg I λ5170 and [O I] λ5577. Unusually, the near-infrared spectra show narrow line peaks in a number of features formed by ions of O and Mg. We infer the presence of CSM that is free of H and He. We propose that the radiative energy from the ejecta-CSM interaction is a plausible explanation for the second LC hump. This interaction scenario is supported by the color evolution, which progresses to the blue as the light curve evolves along the second hump, and the slow second rise and subsequent rapid LC drop. SN 2022xxf may be related to an emerging number of CSM-interacting SNe Ic, which show slow, peculiar LCs, blue colors, and subtle CSM interaction lines. The progenitor stars of these SNe likely experienced an episode of m

关键词： Supernovae

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Low-mass active galactic nuclei on the fundamental plane of black hole activity

arXiv

引用

arXiv 2017年

作者： Qian, Lei Dong, Xiao-Bo Xie, Fu-Guo Liu, Wenjuan Li, Di CAS Key Laboratory of FAST NAOC Chinese Academy of Sciences Beijing100012 China Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming Yunnan650011 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China

It is widely known that in active galactic nuclei (AGNs) and black hole X-ray binaries (BHXBs), there is a tight correlation among their radio luminosity (LR), X-ray luminosity (LX) and BH mass (MBH), the so-called 'fundamental plane' (FP) of BH activity. Yet the supporting data are very limited in the MBH regime between stellar mass (i.e., BHXBs) and 106.5 M☉ (namely, the lower bound of supermassive BHs in common AGNs). In this work, we developed a new method to measure the 1.4 GHz flux directly from the images of the VLA FIRST survey, and apply it to the type-1 low-mass AGNs in the Dong et al. (2012) sample. As a result, we obtained 19 new low-mass AGNs for FP research with both MBH estimates (MBH ≈ 105.5−6.5 M☉), reliable X-ray measurements, and (candidate) radio detections, tripling the number of such candidate sources in the literature. Most (if not all) of the low-mass AGNs follow the standard radio/X-ray correlation and the universal FP relation fitted with the combined dataset of BHXBs and supermassive AGNs by Gültekin et al. (2009);the consistency in the radio/X-ray correlation slope among those accretion systems supports the picture that the accretion and ejection (jet) processes are quite similar in all accretion systems of different MBH. In view of the FP relation, we speculate that the radio loudness R (i.e., the luminosity ratio of the jet to the accretion disk) of AGNs depends not only on Eddington ratio, but probably also on MBH. Copyright © 2017, The Authors. All rights reserved.

关键词： Galaxies

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The first photometric study of the short period shallow contact system LO Comae

arXiv

引用

arXiv 2017年

作者： Zhang, Y. Han, Q.W. Liu, J.Z. Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi830011 China Yunnan Observatory Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China University of Chinese Academy of Sciences Beijing100049 China

In this paper, the first complete photometric light curves in the B, V, and R passbands for an eclipsing binary LO Com are presented, and the photometric solution for the LO Com is derived by analyzing these light curves by using the Wilson and Devinney code. From the photometric solution, it is found that the LO Com is a W-type W UMa binary with a mass ratio of q = m2=m1= 2:478 and a contact degree of f = (3.2±0.25)%. By combining the two new minimum times with those published earlier in the literature, we have found that the (O-C) curve shows a downward parabolic variation corresponding to a long-term decrease in the orbital period with a rate of dP/dt = -1.18×10-7days yr-1. This long-term decrease in its orbital period may be caused by mass transfer from the more massive component to the less massive one. Copyright © 2017, The Authors. All rights reserved.

关键词： Photometry

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The progenitors of type Ia supernovae in the semidetached binaries with red giant donors

arXiv

引用

arXiv 2017年

作者： Liu, D. Wang, B. Ge, H. Chen, X. Han, Z. Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China

Context. The companions of the exploding carbon-oxygen white dwarfs (CO WDs) for producing type Ia supernovae (SNe Ia) are still not conclusively confirmed. A red-giant (RG) star has been suggested to be the mass donor of the exploding WD, named as the symbiotic channel. However, previous studies on the this channel gave a relatively low rate of SNe Ia. Aims. We aim to systematically investigate the parameter space, Galactic rates and delay time distributions of SNe Ia from the symbiotic channel by employing a revised mass-transfer prescription. Methods. We adopted an integrated mass-transfer prescription to calculate the mass-transfer process from a RG star onto the WD. In this prescription, the mass-transfer rate varies with the local material states. Results. We evolved a large number of WD+RG systems, and found that the parameter space of WD+RG systems for producing SNe Ia is significantly enlarged. This channel could produce SNe Ia with intermediate and old ages, contributing to at most 5% of all SNe Ia in the Galaxy. Our model increases the SN Ia rate from this channel by a factor of 5. We suggest that the symbiotic systems RS Oph and T CrB are strong candidates for the progenitors of SNe Ia. Conclusions. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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Accreting CO material onto ONe white dwarfs towards accretion-induced collapse

arXiv

引用

arXiv 2017年

作者： Wu, C. Wang, B. Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 University of Chinese Academy of Sciences Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China

The final outcomes of accreting ONe white dwarfs (ONeWDs) have been studied for several decades, but there are still some issues not resolved. Recently, some studies suggested that the deflagration of oxygen would occur for accreting ONe WDs with Chandrasekhar masses. In this paper, we aim to investigate whether ONe WDs can experience accretion-induced collapse (AIC) or explosions when their masses approach the Chandrasekhar limit. Employing the stellar evolution code modules for experiments in stellar astrophysics (MESA), we simulate the long-Term evolution of ONe WDs by accreting CO material. The ONe WDs undergo weak multicycle carbon flashes during the mass-Accretion process, leading to the mass increase of the WDs. We found that different initialWDmasses and mass-Accretion rates have influence on the evolution of central density and temperature. However, the central temperature cannot reach the explosive oxygen ignition temperature due to the neutrino cooling. This work implies that the final outcome of accreting ONe WDs is electron-capture induced collapse rather than thermonuclear explosion. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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