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Title:
BV Photometry of Variable Stars in the Northeast Arm of the Small Magellanic Cloud [ Erratum: 2002AJ....124.2341S ]
Authors:
Sharpee, Brian; Stark, Michele; Pritzl, Barton; Smith, Horace; Silbermann, Nancy; Wilhelm, Ronald; Walker, Alistair
Affiliation:
AA(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824 ), AB(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824; Department of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802. ), AC(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824; National Optical Astronomy Observatory (NOAO), P.O. Box 26732, Tucson, AZ 85726 ), AD(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824 ), AE(SIRTF Science Center, Mail Stop 220-6, California Institute of Technology, Pasadena, CA 91125 ), AF(Department of Physics, Texas Tech University, Lubbock, TX 79409 ), AG(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, P.O. Box 26732, Tucson, AZ 85726 )
Publication:
The Astronomical Journal, Volume 123, Issue 6, pp. 3216-3254. (AJ Homepage)
Publication Date:
06/2002
Origin:
UCP
Astronomy Keywords:
Stars: Variables: Cepheids, Galaxies: Magellanic Clouds
DOI:
10.1086/340185
Bibliographic Code:
2002AJ....123.3216S

Abstract

B and V photometry has been obtained for variable stars in the northeast arm of the Small Magellanic Cloud (SMC). Periods and light curves have been determined for 237 periodic variables, including 201 Cepheids, 68 of which are newly discovered. Fundamental-mode Cepheids and first-overtone-mode Cepheids are generally well separated in the BV color-magnitude diagram, with the latter having bluer mean colors than the former. The Cepheid period-color relationship for this outlying SMC field is indistinguishable from that seen in more centrally located SMC fields and is bluer than theoretical predictions. The red edge to the populated portion of the instability strip shifts to bluer colors for fainter Cepheids. There is support from our sample for a previously reported steepening in the slope of the period-luminosity relation for fundamental-mode Cepheids near a period of 2 days. The Cepheids of the northeast arm may be closer to us than are those of the main body of the SMC, but the difference is smaller than or equal to about 4 kpc, comparable to the tidal radius of the SMC.

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