Galactic clusters with associated Cepheid variables. IV. C2128+488 (Anon. Platais) and V1726 Cygni

Show simple item record

dc.creator Turner, David Gerald, 1945-
dc.creator Mandushev, Georgi I.
dc.creator Forbes, Douglas
dc.date.accessioned 2016-11-22T16:44:08Z
dc.date.available 2016-11-22T16:44:08Z
dc.date.issued 1994-05
dc.identifier.issn 0004-6256
dc.identifier.uri http://library2.smu.ca/handle/01/26686
dc.description Publisher's version/PDF en_CA
dc.description.abstract New photoelectric UBV photometry of 32 stars, photographic UBV photometry of 120 stars, and spectroscopic observations of 8 stars are presented for C 2128+488 (Anon. Platais), the cluster associated with the 4[d over dot]237 s-Cepheid V1726 Cygni. The resulting photometry, spectral classifications, and radial velocities are used with spectroscopic and proper motion data previously published by Platais and others for the Cepheid and other stars in this field in a detailed cluster analysis. The newly obtained cluster distance modulus is V[subscript 0]-M[subscript V] = 10.98 [plus or minus] 0.02 s.e. (d = 1568 [plus or minus] 13 pc), and a value of R = A[subscript V]/E[subscript B-V = 3.07 [plus or minus] 0.27 s.e. is found to describe the dust extinction in the field. A space reddening of E[subscript B-V] = 0.43 [plus or minus] 0.02 is derived for V1726 Cyg from two late B-type companions which bracket the Cepheid, as well as from the reddenings of other stars in the field. Its resulting luminosity as a probable cluster member is [angled bracket]M[subscript V][angled bracket] = -3.42 [plus or minus] 0.07. A cluster radial velocity of -15.4 [plus or minus] 0.2 km s[superscript -1] and a cluster turnoff point at spectral type B7 are both consistent with the likely membership of V1726 Cyg, as are the available proper motion data. The small amplitude, sinusoidal light curve, and location of V1726 Cyg on the blue edge of the Cepheid instability strip are consistent with the properties expected for overtone pulsation, although such a possibility appears to imply an unrealistically small value ([Beta]=0.5 [plus or minus] 0.2) for the color coefficient in the PLC relation. A more reasonable value of [Beta]=2.1 [plus or minus] 0.2 is derived for the color term applicable to galactic cluster Cepheids in this program when V1726 Cyg is assumed to be pulsating in the fundamental mode. en_CA
dc.language.iso en en_CA
dc.publisher American Astronomical Society en_CA
dc.relation.uri http://dx.doi.org/10.1086/116988
dc.rights Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
dc.subject.lcsh Stars -- Open clusters
dc.subject.lcsh Cepheids
dc.subject.lcsh Astronomical photometry
dc.subject.lcsh UBV system (Astronomy)
dc.title Galactic clusters with associated Cepheid variables. IV. C2128+488 (Anon. Platais) and V1726 Cygni en_CA
dc.type Text en_CA
dcterms.bibliographicCitation Astronomical Journal 107(5), 1796-1805. (1994) en_CA


Files in this item


 

Copyright statement:

 
Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
 
Published Version: http://dx.doi.org/10.1086/116988
 
 

This item appears in the following Collection(s)

Show simple item record