Properties of M31. II. A cepheid disk sample derived from the first year of ps1 pandromeda data

Please use this identifier to cite or link to this item: https://ir.lib.ncu.edu.tw/handle/987654321/100965

Title:	Properties of M31. II. A cepheid disk sample derived from the first year of ps1 pandromeda data
Authors:	饒兆聰;Kodric, Mihael;Riffeser, Arno;Hopp, Ulrich;Seitz, Stella;Koppenhoefer, Johannes;Bender, Ralf;Goessl, Claus;Snigula, Jan;Lee, Chien-Hsiu;Ngeow, Chow-Choong;Chambers, K. C.;Magnier, E. A.;Price, P. A.;Burgett, W. S.;Hodapp, K. W.;Kaiser, N.;Kudritzki, R.-P.
Contributors:	理學院天文研究所
Keywords:	Age;Astronomical instruments;ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;Automation;Cepheid variables;CEPHEIDS;CLASSIFICATION;Curvature;DECOMPOSITION;Disks;DUSTS;EVOLUTION;FILTERS;GALAXIES;INSTABILITY;LUMINOSITY;SPATIAL DISTRIBUTION;Stars
Date:	2013-04-01
Issue Date:	2026-04-21 14:19:43 (UTC+8)
Publisher:	IOP Publishing Ltd.;United States: American Astronomical Society
Abstract:	摘要： We present a sample of Cepheid variable stars toward M31 based on the first year of regular M31 observations of the PS1 survey in the r sub(P1) and i sub(P1) filters. We describe the selection procedure for Cepheid variable stars from the overall variable source sample and develop an automatic classification scheme using Fourier decomposition and the location of the instability strip. We find 1440 fundamental mode (classical delta ) Cep stars, 126 Cepheids in the first overtone mode, and 147 belonging to the Population II types. Two hundred ninety-six Cepheids could not be assigned to one of these classes and three hundred fifty-four Cepheids were found in other surveys. These 2009 Cepheids constitute the largest Cepheid sample in M31 known so far and the full catalog is presented in this paper. We briefly describe the properties of our sample in its spatial distribution throughout the M31 galaxy, in its age properties, and we derive an apparent period-luminosity relation (PLR) in our two bands. The Population I Cepheids nicely follow the dust pattern of the M31 disk, whereas the 147 Type II Cepheids are distributed throughout the halo of M31. We outline the time evolution of the star formation in the major ring found previously and find an age gradient. A comparison of our PLR to previous results indicates a curvature term in the PLR. 出版者： United States: American Astronomical Society 出版日期： 2013-04-01 出處： The Astronomical Journal, 2013-04, Vol.145 (4), p.106--21 資源來源： Institute of Physics Journals 識別號： ISSN: 0004-6256 識別號： ISSN: 1538-3881 識別號： EISSN: 1538-3881 識別號： DOI: 10.1088/0004-6256/145/4/106
Appears in Collections:	[Graduate Institute of Astronomy] journal & Dissertation

Files in This Item:

File	Description	Size	Format
index.html		0Kb	HTML	14	View/Open

社群 sharing

Loading...