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HST Snapshot Study of Variable Stars in Globular Clusters: Inner Region of NGC 6441We present the results of a Hubble Space Telescope snapshot program to survey the inner region of the metal-rich globular cluster NGC 6441 for its variable stars. A total of 57 variable stars was found including 38 RR Lyrae stars, 6 Population II Cepheids, and 12 long period variables. Twenty-four of the RR Lyrae stars and all of the Population II Cepheids were previously undiscovered in ground-based surveys. Of the RR Lyrae stars observed in h s survey, 26 are pulsating in the fundamental mode with a mean period of 0.753 d and 12 are first-overtone mode pulsators with a mean period of 0.365 d. These values match up very well with those found in ground-based surveys. Combining all the available data for NGC 6441, we find mean periods of 0.759 d and 0.375 d for the RRab and RRc stars, respectively. We also find that the RR Lyrae in this survey are located in the same regions of a period-amplitude diagram as those found in ground-based surveys. The overall ratio of RRc to total RR Lyrae is 0.33. Although NGC 6441 is a metal-rich globular cluster and would, on that ground, be expected either to have few RR Lyrae stars, or to be an Oosterhoff type I system, its RR Lyrae more closely resemble those in Oosterhoff type II globular clusters. However, even compared to typical Oosterhoff type II systems, the mean period of its RRab stars is unusually long. We also derived I-band period-luminosity relations for the RR Lyrae stars. Of the six Population II Cepheids, five are of W Virginis type and one is a BL Herculis variable star. This makes NGC 6441, along with NGC 6388, the most metal-rich globular cluster known to contain these types of variable stars. Another variable, V118, may also be a Population II Cepheid given its long period and its separation in magnitude from the RR Lyrae stars. We examine the period-luminosity relation for these Population II Cepheids and compare it to those in other globular clusters and in the Large Magellanic Cloud. We argue that there does not appear to be a change in the period-luminosity relation slope between the BL Herculis and W Virginis stars, but that a change of slope does occur when the RV Tauri stars are added to the period-luminosity relation.
Document ID
20040000086
Document Type
Preprint (Draft being sent to journal)
Authors
Pritzl, Barton J.
(Michigan State Univ. East Lansing, MI, United States)
Smith, Horace A.
(Michigan State Univ. East Lansing, MI, United States)
Stetson, Peter B.
(Dominion Astrophysical Observatory Victoria, British Columbia, Canada)
Catelan, Marcio
(Pontificia Univ. Catolica de Chile Santiago, Chile)
Sweigart, Allen V.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Layden, Andrew C.
(Bowling Green State Univ. OH, United States)
Rich, R. Michael
(California Univ. Los Angeles, CA, United States)
Date Acquired
August 21, 2013
Publication Date
January 1, 2003
Subject Category
Astronomy
Report/Patent Number
astro-ph/030539v1
Funding Number(s)
CONTRACT_GRANT: NAS5-26555
CONTRACT_GRANT: FONDECYT-1030954
CONTRACT_GRANT: DIPUC-2002-04E
Distribution Limits
Public
Copyright
Public Use Permitted.
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