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Strong-lensing measurement of the mass-density profile out to 3 effective radii for z ∼ 0.5 early-type galaxies

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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

The interaction of core-collapse supernova ejecta with a stellar companion

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arXiv 2018年

作者： Liu, Zheng-Wei Tauris, T.M. Ropke, F.K. Moriya, T.J. Kruckow, .M. Stanclie, R.J. Izzard, R.G. Yunnan Observatories Key Laboratory for the Structure and Evolution of Celestial Objects Cas Kunming650216 Center for Astronomical Mega-Science Cas Beijing China Argelander-Institut fur Astronomie Auf dem Hugel 71 BonnD-53121 Germany Heidelberger Institutfur Theoretische Studien Schloss-Wolfsbrunnenweg 35 HeidelbergD-69118 Zentrum fur Astronomie der Universitat Heidelberg Institut fur Theoretische Astrophysik Philosophenweg 12 HeidelbergD-69120 Germany National Astronomical Observatory of Japan MitakaTōkyō-to Japan University of Surrey Guildford SurreyGU2 7XH United Kingdom

The progenitors of many core-collapse supernovae (CCSNe) are expected to be in binary systems. By performing a series of three-dimensional hydrodynamical simulations, we investigate how CCSN explosions affect their binary companion. We find that the amount of removed stellar mass, the resulting impact velocity, and the chemical contamination of the companion that results from the impact of the SN ejecta, strongly increases with decreasing binary separation and increasing explosion energy. Also, it is foud that the impact effects of CCSN ejecta on the structure of main-sequence (MS) companions, and thus their long term post-explosion evolution, is in general not be dramatic. Copyright © 2018, The Authors. All rights reserved.

关键词： Supernovae

The double blue straggler sequence in NGC 2173: a field contamination artefact?

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arXiv 2018年

作者： Li, Chengyuan Deng, Licai de Grijs, Richard Jiang, Dengkai Xin, Yu Department of Physics and Astronomy Macquarie University Balaclava Road SydneyNSW2109 Australia Department of Astronomy China West Normal University Nanchong637002 China School of Astronomy and Space Science University of the Chinese Academy of Sciences 20A Datun Road Beijing100012 China International Space Science Institute–Beijing 1 Nanertiao Zhongguancun Beijing100190 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China

The Fermi-LAT Light Curve Repository

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arXiv 2023年

作者： Abdollahi, S. Ajello, M. Baldini, L. Ballet, J. Bastieri, D. Gonzalez, J. Becerra Bellazzini, R. Berretta, A. Bissaldi, E. Bonino, R. Brill, A. Bruel, P. Burns, E. Buson, S. Cameron, R.A. Caputo, R. Caraveo, P.A. Cibrario, N. Ciprini, S. Orestano, P. Cristarella Crnogorcevic, M. Cutini, S. D’Ammando, F. De Gaetano, S. Digel, S.W. Di Lalla, N. Di Venere, L. Domínguez, A. Ramazani, V. Fallah Fegan, S.J. Ferrara, E.C. Fiori, A. Fleischhack, H. Franckowiak, A. Fukazawa, Y. Fusco, P. Gammaldi, V. Gargano, F. Garrappa, S. Gasbarra, C. Gasparrini, D. Giglietto, N. Giordano, F. Giroletti, M. Green, D. Grenier, I.A. Guiriec, S. Gustafsson, M. Hays, E. Horan, D. Hou, X. Jóhannesson, G. Kerr, M. Kocevski, D. Kuss, M. Latronico, L. Li, J. Liodakis, I. Longo, F. Loparco, F. Lorusso, L. Lott, B. Lovellette, M.N. Lubrano, P. Maldera, S. Manfreda, A. Martí-Devesa, G. Mazziotta, M.N. Mereu, I. Meyer, M. Michelson, P.F. Mizuno, T. Monzani, M.E. Morselli, A. Moskalenko, I.V. Negro, M. Omodei, N. Orlando, E. Ormes, J.F. Paneque, D. Panzarini, G. Perkins, J.S. Persic, M. Pesce-Rollins, M. Pillera, R. Porter, T.A. Principe, G. Racusin, J.L. Rainò, S. Rando, R. Rani, B. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Sánchez-Conde, M. Parkinson, P.M. Saz Scargle, Jeff Scotton, L. Serini, D. Sgrò, C. Siskind, E.J. Spandre, G. Spinelli, P. Suson, D.J. Tajima, H. Thompson, D.J. Torres, D.F. Valverde, J. Venters, T. Wadiasingh, Z. Wagner, S. Wood, K. IRAP Université de Toulouse CNRS UPS CNES ToulouseF-31028 France Department of Physics and Astronomy Clemson University Kinard Lab of Physics ClemsonSC29634-0978 United States Università di Pisa Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Université Paris-Saclay Université Paris Cité CEA CNRS AIM Gif-sur-YvetteF-91191 Cedex France Istituto Nazionale di Fisica Nucleare Sezione di Padova PadovaI-35131 Italy Dipartimento di Fisica e Astronomia "G. Galilei" Università di Padova Via F. Marzolo 8 PadovaI-35131 Italy Center for Space Studies and Activities "G. Colombo" University of Padova Via Venezia 15 PadovaI-35131 Italy Instituto de Astrofísica de Canarias Observatorio del Teide C/Via Lactea s/n Tenerife La LagunaE-38205 Spain Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Dipartimento di Fisica Università degli Studi di Perugia PerugiaI-06123 Italy Dipartimento di Fisica "M. Merlin" dell’Università e del Politecnico di Bari via Amendola 173 BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Torino TorinoI-10125 Italy Dipartimento di Fisica Università degli Studi di Torino TorinoI-10125 Italy NASA Postdoctoral Program Fellow United States NASA Goddard Space Flight Center GreenbeltMD20771 United States Laboratoire Leprince-Ringuet CNRS IN2P3 École polytechnique Institut Polytechnique de Paris Palaiseau91120 France Department of physics and Astronomy Louisiana State University Baton RougeLA70803 United States Institut für Theoretische Physik and Astrophysik Universität Würzburg WürzburgD-97074 Germany W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Milano via E. Bassi

The Fermi Large Area Telescope (LAT) light curve repository (LCR) is a publicly available, continually updated library of gamma-ray light curves of variable Fermi-LAT sources generated over multiple timescales. The Fermi-LAT LCR aims to provide publication-quality light curves binned on timescales of 3 days, 7 days, and 30 days for 1525 sources deemed variable in the source catalog of the first 10 years of Fermi-LAT observations. The repository consists of light curves generated through full likelihood analyses that model the sources and the surrounding region, providing fluxes and photon indices for each time bin. The LCR is intended as a resource for the time-domain and multi-messenger communities by allowing users to quickly search LAT data to identify correlated variability and flaring emission episodes from gamma-ray sources. We describe the sample selection and analysis employed by the LCR and provide an overview of the associated data access portal. Copyright © 2023, The Authors. All rights reserved.

关键词： Gamma rays

A study in scarlet - I. Photometric properties of a sample of Intermediate Luminosity Red Transients

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arXiv 2024年

作者： Valerin, G. Pastorello, A. Reguitti, A. Benetti, S. Cai, Y.-Z. Chen, T.-W. Eappachen, D. Elias-Rosa, N. Fraser, M. Gangopadhyay, A. Hsiao, E.Y. Howell, D.A. Inserra, C. Izzo, L. Jencson, J. Kankare, E. Kotak, R. Mazzali, P.A. Misra, K. Pignata, G. Prentice, S.J. Sand, D.J. Smartt, S.J. Stritzinger, M.D. Tartaglia, L. Valenti, S. Anderson, J.P. Andrews, J.E. Amaro, R.C. Brennan, S. Bufano, F. Callis, E. Cappellaro, E. Dastidar, R. Della Valle, M. Fiore, A. Fulton, M.D. Galbany, L. Heikkilä, T. Hiramatsu, D. Karamehmetoglu, E. Kuncarayakti, H. Leloudas, G. Lundquist, M. McCully, C. Müller-Bravo, T.E. Nicholl, M. Ochner, P. Padilla Gonzalez, E. Paraskeva, E. Pellegrino, C. Reichart, D.E. Reynolds, T.M. Roy, R. Salmaso, I. Singh, M. Turatto, M. Tomasella, L. Wyatt, S. Young, D.R. INAF - Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 PadovaI-35122 Italy INAF - Osservatorio Astronomico di Brera Via E. Bianchi 46 LC Merate23807 Italy 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 SRON Netherlands Institute for Space Research Niels Bohrweg 4 Leiden2333 CA Netherlands Department of Astrophysics IMAPP Radboud University Nijmegen P.O. Box 9010 Nijmegen6500 GL Netherlands Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain School of Physics O'Brien Centre for Science North University College Dublin Belfield Dublin 4 Ireland The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova Stockholm10691 Sweden Hiroshima Astrophysical Science Center Hiroshima University Higashi-Hiroshima Japan Department of Physics Florida State University 77 Chieftan Way TallahasseeFL32306 United States Las Cumbres Observatory 6740 Cortona Dr. Suite 102 GoletaCA93117 United States Department of Physics University of California Santa BarbaraCA93106 United States School of Physics & Astronomy Cardiff University Queens Buildings The Parade CardiffCF24 3AA United Kingdom INAF Osservatorio Astronomico di Capodimonte Salita Moiariello 16 NapoliI-80131 Italy DARK Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen2200 Denmark Caltech Mail Code 220-6 PasadenaCA91125 United States Tuorla Observatory Department of Physics and Astronomy University of Turku Turku20014 Finland Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Max-Planck-Institut für Astrophysik Karl-Schwarzs

Aims. We investigate the photometric characteristics of a sample of Intermediate Luminosity Red Transients (ILRTs), a class of elusive objects with peak luminosity between that of classical novae and standard supernovae. Our goal is to provide a stepping stone in the path to unveil the physical origin of such events, thanks to the analysis of the datasets collected. Methods. We present the multi-wavelength photometric follow-up of four ILRTs, namely NGC 300 2008OT-1, AT 2019abn, AT 2019ahd and AT 2019udc. Through the analysis and modelling of their spectral energy distribution and bolometric light curves we infer the physical parameters associated with these transients. Results. All four objects display a single peaked light curve which ends in a linear decline in magnitudes at late phases. A flux excess with respect to a single black body emission is detected in the infrared domain for three objects in our sample, a few months after maximum. This feature, commonly found in ILRTs, is interpreted as a sign of dust formation. Mid infrared monitoring of NGC 300 2008OT-1 761 days after maximum allows us to infer the presence of ∼10−3-10−5 Mo of dust, depending on the chemical composition and the grain size adopted. The late time decline of the bolometric light curves of the considered ILRTs is shallower than expected for 56Ni decay, hence requiring an additional powering mechanism. James Webb Space Telescope observations of AT 2019abn prove that the object has faded below its progenitor luminosity in the mid-infrared domain, five years after its peak. Together with the disappearance of NGC 300 2008OT-1 in Spitzer images seven years after its discovery, this supports the terminal explosion scenario for ILRTs. With a simple semi-analytical model we try to reproduce the observed bolometric light curves in the context of few Mo of material ejected at few 103 km s−1 and enshrouded in an optically thick circumstellar medium. © 2024, CC BY.

关键词： Giant stars

SN 2018zd: An unusual stellar explosion as part of the diverse type II supernova landscape

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arXiv 2020年

作者： Zhang, Jujia Wang, Xiaofeng Vinkó, József Zhai, Qian Zhang, Tianmeng Filippenko, Alexei V. Brink, Thomas G. Zheng, WeiKang Wyrzykowski, Lukasz Mikolajczyk, Przemyslaw Huang, Fang Rui, Liming Mo, Jun Sai, Hanna Zhang, Xinhan Wang, Huijuan DerKacy, James M. Baron, Eddie Sárneczky, K. Bódi, A. Csörnyei, G. Hanyecz, O. Ignácz, B. Kalup, Cs. Kriskovics, L. Könyves-Tóth, R. Ordasi, A. Pál, A. Sódor, Á. Szakáts, R. Vida, K. Zsidi, G. Kunming650216 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650216 China Center for Astronomical Mega-Science CAS 20A Datun Road Chaoyang District Beijing100012 China Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China Konkoly Observatory CSFK Konkoly-Thege M. ut 15-17 Budapest1121 Hungary ELTE Eötvös Loránd University Institute of Physics Pázmány Péter sétány 1/A Budapest1117 Hungary Department of Optics and Quantum Electronics University of Szeged Dóm tér 9 Szeged6720 Hungary Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Astronomical Institute University of Wroclaw M. Kopernika 11 Wroclaw51-622 Poland Department of Astronomy Shanghai Jiao Tong University Shanghai200240 China Homer L. Dodge Department of Physics and Astronomy University of Oklahoma NormanOK73019 United States ELTE Eötvös Loránd University Department of Astronomy Pázmány Péter sétány 1/A Budapest1117 Hungary MTA CSFK Lendület Near-Field Cosmology Research Group Konkoly Observatory Budapest1121 Hungary European Southern Observatory Karl-Schwarzschild-Strasse 2 Garching bei München85748 Germany

We present extensive observations of SN 2018zd covering the first ∼ 450 d after the explosion. This SN shows a possible shock-breakout signal ∼ 3.6 hr after the explosion in the unfiltered light curve, and prominent flash-ionisation spectral features within the first week. The unusual photospheric temperature rise (rapidly from ∼ 12, 000 K to above 18,000 K) within the earliest few days suggests that the ejecta were continuously heated. Both the significant temperature rise and the flash spectral features can be explained with the interaction of the SN ejecta with the massive stellar wind (0.18+−000510 M), which accounts for the luminous peak (Lmax = [1.36±0.63]×1043 erg s−1) of SN 2018zd. The luminous peak and low expansion velocity (v ≈ 3300 km s−1) make SN 2018zd to be like a member of the LLEV (luminous SNe II with low expansion velocities) events originated due to circumstellar interaction. The relatively fast post-peak decline allows a classification of SN 2018zd as a transition event morphologically linking SNe IIP and SNe IIL. In the radioactive-decay phase, SN 2018zd experienced a significant flux drop and behaved more like a low-luminosity SN IIP both spectroscopically and photometrically. This contrast indicates that circumstellar interaction plays a vital role in modifying the observed light curves of SNe II. Comparing nebular-phase spectra with model predictions suggests that SN 2018zd arose from a star of ∼ 12 M . Given the relatively small amount of 56Ni (0.013 − 0.035M), the massive stellar wind, and the faint X-ray radiation, the progenitor of SN 2018zd could be a massive asymptotic giant branch star which collapsed owing to electron capture. Copyright © 2020, The Authors. All rights reserved.

关键词： Expansion

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

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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

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

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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

Lunar-based Ultraviolet Telescope study of the well-known Algol-type binary TW Dra

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Research in Astronomy and Astrophysics 2016年第6期16卷 93-98页

作者： Wen-Ping Liao Sheng-Bang Qian Miloslav Zejdat 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 Department of Theoretical Physics and Astrophysics Masaryk University Kotlarska 2 CZ-611 37 Brno Czech Republic

By using the Lunar-based Ultraviolet Telescope （LUT） from 2014 December 2 to December 4, the first near-UV light curve of the well-known Algol-type binary TW Dra is reported, which is analyzed with the 2013 version of the W-D code. Our solutions confirmed that TW Dra is a semi-detached binary system where the secondary component fills its Roche lobe. The mass ratio and a high inclination are obtained （q = 0.47, i = 86.68°）. Based on 589 available data spanning more than one century, the complex period changes are studied. Secular increase and three cyclical changes are found in the corresponding orbital period analysis. The secular increase changes reveal mass transfer from the secondary component to the primary one at a rate of 6.8 × 10-7 M yr-1. One large cyclical change of 116.04 yr may be caused by disturbance of visual component ADS 9706B orbiting TW Dra （ADS 9706A）, while the other two cyclical changes with shorter periods of 22.47 and 37.27 yr can be explained as the result of two circumbinary companions that are orbiting around TW Dra, where the two companions are in simple 3 ： 5 orbit-rotation resonances. TW Dra itself is a basic binary in a possible sextuple system with the configuration （1 ＋ 1）＋（1 ＋ 1）＋（1 ＋ 1）, which further suggests that multiplicity may be a fairly common phenomenon in close binary systems.

关键词： stars： binaries： close -- stars： binaries： eclipsing -- stars： individual （TW Draco）