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Title:
Assessing potential cluster Cepheids from a new distance and reddening parametrization and Two Micron All Sky Survey photometry
Authors:
Majaess, D. J.; Turner, D. G.; Lane, D. J.
Affiliation:
AA(Department of Astronomy and Physics, Saint Mary's University, Halifax, Nova Scotia B3H 3C3, Canada; Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, Canada; Harvard College Observatory Photographic Plate Stacks, 60 Garden Street, Cambridge, MA 02138, USA), AB(Department of Astronomy and Physics, Saint Mary's University, Halifax, Nova Scotia B3H 3C3, Canada; Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, Canada; Harvard College Observatory Photographic Plate Stacks, 60 Garden Street, Cambridge, MA 02138, USA), AC(Department of Astronomy and Physics, Saint Mary's University, Halifax, Nova Scotia B3H 3C3, Canada; The Abbey Ridge Observatory, Stillwater Lake, Nova Scotia, Canada)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 390, Issue 4, pp. 1539-1548. (MNRAS Homepage)
Publication Date:
11/2008
Origin:
MNRAS
Astronomy Keywords:
stars: distances , stars: fundamental parameters , Cepheids
DOI:
10.1111/j.1365-2966.2008.13834.x
Bibliographic Code:
2008MNRAS.390.1539M

Abstract

A framework is outlined to assess Cepheids as potential cluster members from readily available photometric observations. A relationship is derived to estimate colour excess and distance for individual Cepheids through a calibration involving recently published Hubble Space Telescope parallaxes and a cleaned sample of established cluster Cepheids. Photometric V - J colour is found to be a viable parameter for approximating a Cepheid's reddening. The non-universal nature of the slope of the Cepheid period-luminosity relation for BV photometry is confirmed. By comparison, the slopes of the VJ and VI relations seem relatively unaffected by metallicity. A new Galactic Cepheid confirmed here, GSC 03729-01127 (F6-G1 Ib), is sufficiently coincident with the coronal regions of Tombaugh 5 to warrant follow-up radial velocity measures to assess membership. CCD photometry and O-C diagrams are presented for GSC 03729-01127 and the suspected cluster Cepheids AB Cam and BD Cas. Fourier analysis of the photometry for BD Cas and recent estimates of its metallicity constrain it to be a Population I overtone pulsator rather than a Type II s-Cepheid. AB Cam and BD Cas are not physically associated with the spatially adjacent open clusters Tombaugh 5 and King 13, respectively; the latter being much older (logtau ~= 9) than believed previously. Rates of period change are determined for the three Cepheids from archival and published data. GSC 03729-01127 and AB Cam exhibit period increases, implying fifth and third crossings of the instability strip, respectively, while BD Cas exhibits a period decrease, indicating a second crossing, with possible superposed trends unrelated to binarity. More importantly, the observed rates of period change confirm theoretical predictions. The challenges and prospects for future work in this area of research are discussed.
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