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Galactic Clusters with Associated Cepheid Variables. VI. Anonymous van den Bergh (C0634+031) and CV Monocerotis
A photometric UBVI_KC study, based upon a compilation of new andpreviously published photometry, is presented for the clustersurrounding the 5.38 day Cepheid CV Mon. Photoelectric, photographic,and CCD observations are presented for 200 stars lying within ~8' of CVMon, and the data are used with spectroscopic observations for starsnear the Cepheid to investigate the reddening and distance of clustermembers. The reddening law for the cluster field is described by therelation E_U - B/E_B - V = 0.77, and the ratio of total to selectiveextinction for the dust clouds obscuring cluster stars is characterizedby R = A_V/E_B - V = 3.20 +/- 0.04 s.e. The foreground dust complex islocated at a distance of ~900-1100 pc, whereas the cluster itself is1.65 +/- 0.03 kpc distant ( = 11.08 +/- 0.03 s.e.). CVMon shares not only a spatial coincidence with cluster stars-a featureconfirmed by star counts-but also a similar radial velocity andestimated age. Its derived luminosity as a cluster member is = -3.37 +/- 0.08 s.e., and its derived space reddening is E_B - V = 0.75+/- 0.02 [E_B - V(B0) = 0.80 +/- 0.02]. There is evidence for thepresence of two background groups in the field, one lying immediatelybeyond the cluster (d = 1.86 +/- 0.03 kpc) and a more distant group (d =3.02 +/- 0.08 kpc). The cluster itself exhibits photometricproperties-upper-main-sequence dispersion and main-sequencegaps-consistent with rapid rotation for hot cluster members. Suchfeatures are common in Cepheid-age clusters.
| Observational studies of Cepheids. II - BVRI photometry of 112 Cepheids
Over 4000 differentially determined photoelectric BVRI observations andthe resulting light curves are presented for 112 Cepheids accessiblefrom Northern Hemisphere observatories. The internal precision of thesedata is better than + or - 0.01 mag, and the accuracy of transformationto the Johnson BVRI system is nearly as good.
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