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Author Yang, S.-C. ♦ Sarajedini, Ata ♦ Holtzman, Jon A. ♦ Garnett, Donald R.
Source United States Department of Energy Office of Scientific and Technical Information
Content type Text
Language English
Subject Keyword ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ♦ GALAXIES ♦ LUMINOSITY ♦ SIMULATION ♦ STARS ♦ TELESCOPES ♦ OPTICAL PROPERTIES ♦ PHYSICAL PROPERTIES
Abstract We present the results of an extensive survey of RR Lyrae (RRL) stars in three fields along the major axis of the Triangulum Galaxy (M33). From images taken with the Advanced Camera for Surveys (ACS) Wide Field Channel on board the Hubble Space Telescope through two passbands (F606W and F814W), we have identified and characterized a total of 119 RRL variables (96 RRab (RR0) and 23 RRc (RR1)) in M33. Using the properties of 83 RRL stars (65 RRab and 18 RRc) in the innermost ACS field (hereafter DISK2), we find mean periods of (P{sub ab}) = 0.553 {+-} 0.008 (error1) {+-} 0.05 (error2) and (P{sub c}) = 0.325 {+-} 0.008 (error1) {+-} 0.05 (error2), where the 'error1' value represents the standard error of the mean and the 'error2' value is based on the error of an individual RRL period calculated from our synthetic light curve simulations. The distribution of RRab periods and the frequency of RRc stars (N{sub c} = n{sub c} /n{sub abc} = 0.22) strongly suggest that these RRLs follow the general characteristics of those in Oosterhoff type I Galactic globular clusters. The metallicities of 65 individual RRab stars are calculated from the period-amplitude-metallicity relationship, yielding a mean metallicity of ([Fe/H]) = -1.48 {+-} 0.05 dex, where the uncertainty is the standard error of the mean. The VI minimum-light colors of the RRab stars are used to calculate a mean line-of-sight reddening toward the DISK2 field of (E(V - I)) = 0.175. By adopting this line-of-sight reddening and using a relation between RRL luminosity and metallicity (M{sub V} = 0.23[Fe/H]+0.93), we estimate a mean distance modulus of ((m - M){sub 0}) = 24.52 {+-} 0.11 for M33, where the error is the quadratic sum of the uncertainties in the absolute and dereddened V magnitudes of the RRLs. The Oosterhoff I properties of the M33 field RRL stars agree well with those of RRL populations found in the M31 halo consistent with the past interaction history of these two galaxies.
ISSN 0004637X
Educational Use Research
Learning Resource Type Article
Publisher Date 2010-11-20
Publisher Place United States
Journal Astrophysical Journal
Volume Number 724
Issue Number 1


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