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arXiv 2021年

作者： Huber, Daniel White, Timothy R. Metcalfe, Travis S. Chontos, Ashley Fausnaugh, Michael M. Ho, Cynthia S.K. van Eylen, Vincent Ball, Warrick H. Basu, Sarbani Bedding, Timothy R. Benomar, Othman Bossini, Diego Breton, Sylvain Buzasi, Derek L. Campante, Tiago L. Chaplin, William J. Christensen-Dalsgaard, Jørgen Cunha, Margarida S. Deal, Morgan García, Rafael A. Muñoz, Antonio García Gehan, Charlotte González-Cuesta, Lucía Jiang, Chen Kayhan, Cenk Kjeldsen, Hans Lundkvist, Mia S. Mathis, Stéphane Mathur, Savita Monteiro, Mário J.P.F.G. Nsamba, Benard Ong, Jia Mian Joel Pakštiene, Erika Serenelli, Aldo M. Aguirre, Victor Silva Stassun, Keivan G. Stello, Dennis Stilling, Sissel Norgaard Winther, Mark Lykke Wu, Tao Barclay, Thomas Daylan, Tansu Günther, Maximilian N. Hermes, J.J. Jenkins, Jon M. Latham, David W. Levine, Alan M. Ricker, George R. Seager, Sara Shporer, Avi Twicken, Joseph D. Vanderspek, Roland K. Winn, Joshua N. Institute for Astronomy University of Hawai‘i 2680 Woodlawn Drive HonoluluHI96822 United States School of Physics University of Sydney NSW2006 Australia Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark White Dwarf Research Corporation 9020 Brumm Trail GoldenCO80403 United States Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology 77 Massachusetts Ave. CambridgeMA02139 United States Mullard Space Science Laboratory University College London Holmbury St Mary Dorking Surrey RH5 6NT United Kingdom School of Physics and Astronomy University of Birmingham BirminghamB15 2TT United Kingdom Department of Astronomy Yale University P.O. Box 208101 New HavenCT06520-8101 United States Center for Space Science New York University Abu Dhabi United Arab Emirates Division of Solar and Plasma Astrophysics NAOJ Mitaka Tokyo Japan Instituto de Astrofísica e Ciências do Espaço Universidade do Porto CAUP Rua das Estrelas Porto4150-762 Portugal AIM CEA CNRS Université Paris-Saclay Université Paris Diderot Sorbonne Paris Cité Gif-sur-YvetteF-91191 France Dept. of Chemistry & Physics Florida Gulf Coast University 10501 FGCU Blvd. S. Fort MyersFL33965 United States Departamento de Física e Astronomia Faculdade de Ciências da Universidade do Porto Rua do Campo Alegre s/n Porto4169-007 Portugal Max-Planck-Institut für Sonnensystemforschung Justus-von-Liebig-Weg 3 Göttingen37077 Germany Tenerife La Laguna38205 Spain Departamento de Astrofísica Tenerife La LagunaE-38206 Spain Department of Astronomy and Space Sciences Science Faculty Erciyes University Melikgazi Kayseri38030 Turkey Institute of Theoretical Physics and Astronomy Vilnius University Sauletekio av. 3 Vilnius10257 Lithuania Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1 GarchingD-85748 Germany Instituto de Astrofísica e Ciências do Espaço Universidade d

We present an analysis of the first 20-second cadence light curves obtained by the TESS space telescope during its extended mission. We find a precision improvement of 20-second data compared to 2-minute data for bright stars when binned to the same cadence (≈ 10-25% better for T . 8 mag, reaching equal precision at T ≈ 13 mag), consistent with pre-flight expectations based on differences in cosmic ray mitigation algorithms. We present two results enabled by this improvement. First, we use 20-second data to detect oscillations in three solar analogs (γ Pav, ζ Tuc and π Men) and use asteroseismology to measure their radii, masses, densities and ages to ≈ 1%, ≈ 3%, ≈ 1% and ≈ 20% respectively, including systematic errors. Combining our asteroseismic ages with chromospheric activity measurements we find evidence that the spread in the activity-age relation is linked to stellar mass and thus convection-zone depth. Second, we combine 20-second data and published radial velocities to re-characterize π Men c, which is now the closest transiting exoplanet for which detailed asteroseismology of the host star is possible. We show that π Men c is located at the upper edge of the planet radius valley for its orbital period, confirming that it has likely retained a volatile atmosphere and that the "asteroseismic radius valley’ remains devoid of planets. Our analysis favors a low eccentricity for π Men c (2,1 . 2400) if it formed via high-eccentricity migration. Combined, these early results demonstrate the strong potential of TESS 20-second cadence data for stellar astrophysics and exoplanet science. Copyright © 2021, The Authors. All rights reserved.

关键词： Extrasolar planets

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Is the X-ray pulsating companion of HD 49798 a possible type Ia supernova progenitor?

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Research in Astronomy and Astrophysics 2015年第11期15卷 1813-1822页

作者： Dong-Dong Liu Wei-Hong Zhou Cheng-Yuan Wu Bo Wang Yunnan Observatories Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences University of Chinese Academy of Sciences National Astronomical Observatories Chinese Academy of Sciences Yunnan Minzu University

HD 49798（a hydrogen depleted subdwarf O6 star） with its massive white dwarf（WD） companion has been suggested to be a progenitor candidate of a type Ia supernova（SN Ia）. However, it is still uncertain whether the companion of HD 49798 is a carbon-oxygen（CO） WD or an oxygen-neon（ONe） WD. A CO WD will explode as an SN Ia when its mass grows and approaches the Chandrasekhar limit, but the outcome of an accreting ONe WD is likely to be a neutron star. We generated a series of Monte Carlo calculations that incorperate binary population synthesis to simulate the formation of ONe WD ＋ He star systems. We found that there is almost no orbital period as large as HD 49798 with its WD companion in these ONe WD ＋ He star systems based on our simulations, which means that the companion of HD 49798 might not be an ONe WD. We suggest that the companion of HD 49798 is most likely a CO WD, which can be expected to increase its mass to the Chandrasekhar limit by accreting He-rich material from HD 49798. Thus, HD 49798 and its companion may produce an SN Ia as a result of its future evolution.

关键词： progenitor primordial likely uncertain depleted ejection neutron orbital unstable dwarf

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Strip Smoke and Cloud Recognition in Satellite Image

Strip Smoke and Cloud Recognition in Satellite Image

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International Congress on Image and Signal Processing, BioMedical Engineering and Informatics (CISP-BMEI)

作者： Sheng Miao Hong Lin Hao Gao Liang Dong Southwest Forestry University Kunming China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming China Radio astronomy research group Yunnan observatory of Chinese academy of science Kunming China

ISBN: (纸本)9781509037117

Forest fire detection based on the satellite image is an important method for fire warning. In the early stage of the forest fire, smoke is a key feature to detect. But both the smoke and cloud are mist shape, which has similar shape. For most smoke satellite image, The smoke is in the shape of a strip, for this feature, an method using edge detection to recognize smoke and cloud has been proposed. This algorithm detect the region covered with mist, and recognize the shape of the mist area using edge detection, to effectively recognize cloud and smoke. More than 30 images with cloud and strip smoke are used to test this method show the method can effectively detect strip smoke.

关键词： Shape Satellites Histograms Strips Image edge detection Satellite broadcasting

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Carbon stars identified from LAMOST DR4 using machine learning

arXiv

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arXiv 2017年

作者： Li, Yin-Bi Luo, A-Li Du, Chang-De Zuo, Fang Wang, Meng-Xin Zhao, Gang Jiang, Bi-Wei Zhang, Hua-Wei Liu, Chao Qin, Li Wang, Rui Du, Bing Guo, Yan-Xin Wang, Bo Han, Zhan-Wen Xiang, Mao-Sheng Huang, Yang Chen, Bing-Qiu Chen, Jian-Jun Kong, Xiao Hou, Wen Song, Yi-Han Wang, You-Fen Wu, Ke-Fei Zhang, Jian-Nan Zhang, Yong Wang, Yue-Fei Cao, Zi-Huang Hou, Yong-Hui Zhao, Yong-Heng Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China Beijing100190 China Department of Astronomy Beijing Normal University Beijing100875 China Department of Astronomy School of Physics Peking University Beijing100871 China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy of Sciences Kunming650216 China South-Western Institute for Astronomy Research Yunnan University Kunming650500 China LAMOST Fellow Nanjing Institute of Astronomical Optics & Technology National Astronomical Observatories Chinese Academy of Sciences Nanjing210042 China

In this work, we present a catalog of 2651 carbon stars from the fourth Data Release (DR4) of the Large Sky Area Multi-Object Fiber Spectroscopy Telescope (LAMOST). Using an efficient machine-learning algorithm, we find out these stars from more than seven million spectra. As a by-product, 17 carbon-enhanced metal-poor (CEMP) turnoff star candidates are also reported in this paper, and they are preliminarily identified by their atmospheric parameters. Except for 176 stars that could not be given spectral types, we classify the other 2475 carbon stars into five subtypes including 864 C-H, 226 C-R, 400 C-J, 266 C-N, and 719 barium stars based on a series of spectral features. Furthermore, we divide the C-J stars into three subtypes of CJ(H), C-J(R), C-J(N), and about 90% of them are cool N-type stars as expected from previous literature. Beside spectroscopic classification, we also match these carbon stars to multiple broadband photometries. Using ultraviolet photometry data, we find that 25 carbon stars have FUV detections and they are likely to be in binary systems with compact white dwarf companions. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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Followup observations of SDSS and CRTS candidate cataclysmic variables II

arXiv

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arXiv 2017年

作者： Szkody, Paula Everett, Mark E. Dai, Zhibin Serna-Grey, Donald Department of Astronomy University of Washington Box 351580 SeattleWA98195 United States National Optical Astronomy Observatories 950 N. Cherry Ave TucsonAZ United States Department of Astronomy University of Washington Box 351580 SeattleWA98195 United States Key Laboratory for the Structure and Evolution of Celestial Objects 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

Spectra of 38 candidate or known cataclysmic variables are presented. Most are candidate dwarf novae or systems containing possible highly magnetic white dwarfs, while a few (KR Aur, LS Peg, V380 Oph amd V694 Mon) are previously known objects caught in unusual states. Individual spectra are used to confirm a dwarf nova nature or other classification while radial velocities of 15 systems provide orbital periods and velocity amplitudes that aid in determining the nature of the objects. Our results substantiate a polar nature for four objects, find an eclipsing SW Sex star below the period gap, another as a likely intermediate polar, as well as two dwarf novae with periods in the middle of the gap. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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First photometric study of ultrashort-period contact binary 1SWASP J140533.33+114639.1

arXiv

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arXiv 2017年

作者： Zhang, Bin Qian, Sheng-bang Michel, R. Soonthornthum, B. Zhu, Li-ying P. O. Box 110 Kunming650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P. O. Box 110 Kunming650216 China University of Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China Instituto de Astronomía UNAM Ensenada Mexico National Astronomical Research Institute of Thailand 191 Siriphanich Bidg. 2nd Fl. Huay Kaew Rd. Suthep District Muang Chiang Mai50200 Thailand

In this paper, CCD photometric light curves for the short-period eclipsing binary 1SWASP J140533.33+114639.1 (hereafter J1405) in the BV R bands are presented and analyzed using the 2013 version of the Wilson-Devinney (W-D) code. It is discovered that the J1405 is a W-subtype shallow contact binary with a contact degree of f = 7.9± 0.5% and a mass ratio of q = 1.55 ± 0.02. In order to explain the asymmetric light curves of the system, a cool star-spot on the more massive component was employed. This shallow contact eclipsing binary may be formed from a short-period detached system through the orbital shrinkage due to angular momentum loss. Based on (O − C) method, the variation of the orbital period was studied using all the available times of the minimum light. The (O − C) diagram reveals that the period is increasing continuously at a rate of dP/dt = +2.09 × 10−7days yr−1, which can be explained by mass transfer from the less massive component to the more massive one. Copyright © 2017, The Authors. All rights reserved.

关键词： Photometry

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MULTI-COLOR OPTICAL MONITORING OF THE QUASAR 3C 273 FROM 2005 TO 2016

arXiv

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arXiv 2017年

作者： Xiong, Dingrong Bai, Jinming Zhang, Haojing Fan, Junhui Gu, Minfeng Yi, Tingfeng Zhang, Xiong 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 Department of Physics Yunnan Normal University Kunming650500 China Center for Astrophysics Guangzhou University Guangzhou510006 China Astronomy Science and Technology Research Laboratory Department of Education of Guangdong Province Guangzhou510006 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China

We have monitored the quasar 3C 273 in optical V, R and I bands from 2005 to 2016. Intraday variability (IDV) is detected on seven nights. The variability amplitudes for most of nights are less than 10% and four nights more than 20%. When considering the nights with time spans > 4 hours, the value of duty cycle (DC) is 14.17 per cent. Over the twelve years, the overall magnitude and color index variabilities are ΔI = 0m.67, ΔR = 0m.72, ΔV = 0m.68, and Δ(V − R) = 0m.25 respectively. The largest clear IDV has an amplitude of 42% over just 5.8 minutes and the weakest detected IDV is 5.4% over 175 minutes. The BWB (bluer when brighter) chromatic trend is dominant for 3C 273 and appears at different flux levels on intraday timescales. The BWB trend exists for short-term timescales and intermediate-term timescales but different timescales have different correlations. There is no BWB trend for our whole time-series data sets. A significant anti-correlation between BWB trend and length of timescales is found. Combining with V -band data from previous works, we find a possible quasi-periodicity of P = 3918 ± 1112 days. The possible explanations for the observed variability, BWB chromatic trend and periodicity are discussed. Copyright © 2017, The Authors. All rights reserved.

关键词： Galaxies

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Discovery of two broad absorption line quasars at redshift about 4.75 using the Lijiang 2.4 m telescope

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Science China(Physics,Mechanics & Astronomy) 2015年第9期58卷 90-94页

作者： YI WeiMin WU XueBing WANG FeiGe YANG JinYi YANG Qian BAI JinMing Yunnan Observatories Chinese Academy of Sciences University of the Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Department of Astronomy School of Physics Peking University Kavli Institute for Astronomy and Astrophysics Peking University

The ultraviolet broad absorption lines have been seen in the spectra of quasars at high redshift, and are generally considered to be caused by outflows with velocities from thousands kilometers per second to one tenth of the speed of light. They provide crucial implications for the cosmological structures and physical evolutions related to the feedback of active galactic nuclei(AGNs).Recently, through a dedicated program of optically spectroscopic identifications of selected quasar candidates at redshift 5 by using the Lijiang 2.4 m telescope, we discovered two luminous broad absorption line quasars(BALQSOs) at redshift about 4.75. One of them may even have the potentially highest absorption Balnicity Index(BI) ever found to date, which is remarkably characterized by its deep, broad absorption lines and sub-relativistic outflows. Further physical properties, including the metal abundances,variabilities, evolutions of the supermassive black holes(SMBH) and accretion disks associated with the feedback process, can be investigated with multi-wavelength follow-up observations in the future.

关键词： high-redshift active galactic nuclear（AGN） broad absorption line quasar（BALQSO） outflow

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NEUTRAL CARBON EMISSION IN LUMINOUS INFRARED GALAXIES THE [Ci] LINES AS TOTAL MOLECULAR GAS TRACERS

arXiv

引用

arXiv 2017年

作者： Jiao, Qian Zhao, Yinghe Zhu, Ming Lu, Nanyao Gao, Yu Zhang, Zhi-Yu Beijing100012 China Key Laboratory of Radio Astronomy CAS Beijing100012 China University of Chinese Academy of Sciences Beijing100012 China Yunnan Observatories CAS Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650011 China Center for Astronomical Mega-Science CAS 20A Datun Road Chaoyang District Beijing100012 China Purple Mountain Observatory CAS Nanjing210008 China Camino El Observatorio 1515 Las Condes Santiago Chile Key Laboratory of Radio Astronomy CAS Nanjing210008 China Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom ESO Karl Schwarzschild Strasse 2 Garching MunichD-85748 Germany

We present a statistical study on the (formula presented) lines (hereafter [C i] (1−0) and [C i] (2−1), respectively) and the CO (1−0) line for a sample of (ultra)luminous infrared galaxies [(U)LIRGs]. We explore the correlations between the luminosities of CO (1−0) and [C i] lines, and find that L′CO(1−0) correlates almost linearly with both (formula presented), suggesting that [C i] lines can trace total molecular gas mass at least for (U)LIRGs. We also investigate the dependence of (formula presented) and (formula presented)on the far-infrared color of 60-to-100 µm, and find non-correlation, a weak correlation and a modest correlation, respectively. Under the assumption that these two carbon transitions are optically thin, we further calculate the [C i] line excitation temperatures, atomic carbon masses, and the mean [C i] line flux-to-H2 mass conversion factors for our sample. The resulting H2 masses using these [C i]-based conversion factors roughly agree with those derived from L′CO(1−0) and CO-to-H2 conversion factor. Copyright © 2017, The Authors. All rights reserved.

关键词： Molecules

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GRANDMA Observations of SN 2023wrk, a Luminous Type Ia Supernova with Significant Unburned Carbon in the Outer Ejecta

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Research Notes of the AAS 2024年第10期8卷 273-273页

作者： Cristina Andrade Pierre-Alexandre Duverne Jialian Liu Felipe Navarete Abdelaziz E. Abdelaziz Mohamed Abdelkareem Ilmah Abdi Mohamed Aboueisha Christophe Adami Shabnam Agayeva Vova Aivazyan Leandro de Almeida Dalya Akl Sarah Antier Yvan Arnaud Saad A. Ata Wageeh A. Badawy Chunhai Bai Reda Bendary Zouhair Benkhaldoun Kevin Borrot Eric Broens Yongzhi Cai Olivier Clerget Wagner Corradi Michael W. Coughlin Nicolas Delaunoy Franky Dubois Jean-Grégoire Ducoin Eslam Elhosseiny Thomas M. Esposito Ali Esamdin Pascal Foulon Roland Foulon Michael Freeberg Charles Galdies Priyadarshini Gokuldass Bruno Guillet Gamal M. Hamed Bruno Haremza Patrice Hello Yasser Hendy Patrick Huth Raguli Inasaridze Abdusamatjan Iskandar Aziz Kaeouach Tarek M. Kamel Sergey Karpov Raymond Kneip Nino Kochiashvili Petri Kuossari Liping Li Xin Li Jinzhong Liu Markus Lorber Raouf H. Mabrouk Denis Marchais Elisabeth Maris Isabel Márquez Martin Mašek Roger Ménard Nicola Meneghelli Mike Mitchell Kanthanakorn Noysena Mohammad Odeh Wataru Ono Gérard Parent Bruce Parker Julien Peloton Adam Popowicz Thierry Pradier Stephen Price Oleksandra Pyshna Yodgor Rajabov Fadi Saibi Sophie Saibi Denis Saint-Gelais Nelio Sasaki Marc Serrau Masao Shimizu Ahmed Shokry Andrii Simon Oleksii Sokoliuk Ali Takey Manasanun Tanasan Yusuf Tillayev Giuseppe Di Tommaso Iara Tosta e Melo Damien Turpin Xiaofeng Wang Zhenyu Wang Ibrahim Zead Jujia Zhang School of Physics and Astronomy University of Minnesota Minneapolis MN 55455 USA Université Paris Cité CNRS Astroparticule et Cosmologie F-75013 Paris France Physics Department Tsinghua University Beijing 100084 People's Republic of China SOAR Telescope/NSF’s NOIRLab Avda Juan Cisternas 1500 1700000 La Serena Chile National Research Institute of Astronomy and Geophysics (NRIAG) 1 El-marsad St. 11421 Helwan Cairo Egypt Physics Department American University of Sharjah Sharjah UAE Aix Marseille Univ CNRS CNES LAM Marseille France N.Tusi Shamakhy Astrophysical Observatory Azerbaijan National Academy of Sciences settl.Y. Mammadaliyev AZ 5626 Shamakhy Azerbaijan E. Kharadze Georgian National Astrophysical Observatory Mt.Kanobili Abastumani 0301 Adigeni Georgia Laboratório Nacional de Astrofísica R. dos Estados Unidos 154—Nações Itajubá—MG 37504-364 Brazil Université Côte d’Azur Observatoire de la Côte d’Azur CNRS Boulevard de l’Observatoire 06304 Nice France Unistellar Network France Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi Xinjiang 830011 People's Republic of China Oukaimeden Observatory High Energy Physics and Astrophysics Laboratory FSSM Cadi Ayyad University Morocco GRANDMA: Kilonova-Catcher Vereniging Voor Sterrenkunde Balen-Neetlaan 18A B-2400 Mol Belgium Yunnan Observatories Chinese Academy of Sciences Kunming 650216 People's Republic of China International Centre of Supernovae Yunnan Key Laboratory Kunming 650216 People's Republic of China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650216 People's Republic of China Adonis Observatory (private obs.) Poelkapellestraat 57 Langemark 8920 Belgium CPPM Aix Marseille Univ CNRS/IN2P3 CPPM Marseille France SETI Institute Carl Sagan Center 339 Bernardo Ave Suite 200 Mountain View CA 94043 USA Unistellar 5 allée Marcel Leclerc bâtiment B Marseille 13008 France Department of Astronomy University of

First detected on 2023 November 4 by the Gravitational-wave Optical Transient Observer, SN 2023wrk is a Type Ia Supernova at 40 Mpc, with significant unburned carbon in the outer ejecta. In this note, we present photometric and spectroscopic observations and analysis conducted by the Global Rapid Advanced Network Devoted to the Multi-messenger Addict over a 115 days period, which includes 78 days of measurements. The observations were contributed by both amateur and professional astronomers. J. Liu et al. analyzed the physical processes involved, and compared the evolution of color and spectral lines. We conclude that SN 2023wrk is the second 1999aa-like object with strong carbon absorption lines that has ever been found, which enriches our understanding of the subclass of 1999aa-like SNe.

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