- ID:
- ivo://CDS.VizieR/VI/19
- Title:
- UBV Photoelectric Sequences in SA 92-115
- Short Name:
- VI/19
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The UBV system was originally defined by ten bright standard stars, primarily in the northern sky. These stars are too bright to be used with large telescopes and cannot be reached from southern observatories. This catalog is a careful compilation of data on fainter stars in the equatorial Selected Areas. They are intended as a new set of standards which can be used to define the UBV system at fainter magnitudes in both hemispheres. The stars range in V between 6.0 and 14.9 with most between 9.0 and 13.0.
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- ID:
- ivo://CDS.VizieR/J/ApJ/541/841
- Title:
- UBV photometry and ages of Trapezium systems
- Short Name:
- J/ApJ/541/841
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We sought to determine the maximum age of Trapezium systems by studying possible trapezium systems that were selected independently of their occurrence in H II regions. We started with the unpublished catalog by Allen, Tapia & Parrao (1977RMxAA...3..119A) of all the known visual systems having three or more stars in which the maximum separation is less than 3.0 times the minimum separation. Their catalog has 968 such systems whose most frequent primary type is F, which does not describe young systems. With a CCD on the Kitt Peak 0.9m telescope we obtained UBV frames for 265 systems accessible with our equipment on Kitt Peak. The frames were used to obtain UBV photometry for about 1500 stars with an accuracy of 0.04mag between V=7 and 14mag. Also these frames were used to obtain astrometry with an accuracy of +/-0.015{deg} in position angle and +/-0.01" in separation. For the brightest star in each system we obtained a spectral type to determine the distance and reddening to the system.
- ID:
- ivo://CDS.VizieR/II/248
- Title:
- UBV photometry and proper motions in M13
- Short Name:
- II/248
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The first epoch plates of 8 globular clusters, available in the plate collection of the Pulkovo Observatory, were taken with the normal astrograph at the end of the last and beginning of this century. These plates had been measured previously by N. Gamalei [1948, IzPul, 141] in order to determine the proper motions of the clusters. From 40 to 62 stars were used for this purpose and these were assumed to be cluster members on the basis of their proximity to the cluster centers. The epoch differences ranged from 30 to 45 years. As this time interval has now increased considerably (by about a factor of two), it is planned to redetermine the proper motions of these clusters, using more precise criteria for the selection of stars belonging to the cluster. In the previous study (N. Gamalei [1948, IzPul, 141]) only a limited number of field reference stars were measured, and as more complete data on the cluster, cluster members and field stars is desirable all the star images on the plates in an area 80'x80' will be measured in the present program. For future studies of the orbits of galactic clusters it is important that the absolute proper motions be on one system and therefore special attention should be devoted to this problem. The present paper is a continuation of an investigation of M13 and deals with the determination of the proper motions and U, B, V magnitudes of separate stars and also a redetermination of the proper motions of the cluster. The U, B, V magnitudes of the majority of 923 stars with measured proper motions were found from plates (table 2) taken with the 2 meter Schmidt telescope at Tautenburg and kindly lent to us by Professor N. Richter. The photoelectric standards as given by Savedoff [1956AJ.....61..254S] (table 7) and also U B V magnitudes of six bright field stars (table 8) observed by Mayer were used for calibration. A comparison of the determined B and V magnitudes of stars within an area of about 10'x10' centered on the cluster with those obtained by other authors indicates that the probable external errors do not exceed +/-0.03mag (table 15). However as the photoelectric magnitudes of fainter field stars were not available, a slight systematic error may be present in the derived magnitudes of these stars. Data on the plates used for the determination of the proper motions were given in Kadla [1963AZh....40..691K]. The relative proper motion of M 13, redetermined on the basis of a larger number of cluster members (80 in all, measured on 4 pairs of plates with a mean epoch difference equal to 61.4 years) is found to be {mu}x=+0.0008", {mu}y=-0.0014" with a probable error of +/-0.0002".
- ID:
- ivo://CDS.VizieR/J/A+A/405/1087
- Title:
- UBV photometry and radial velocities of V497 Cep
- Short Name:
- J/A+A/405/1087
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- New light and radial-velocity curves of V497 Cep, a binary in the open cluster NGC 7160, were obtained and the linear ephemeris of the system was refined to HJD(Min I)=(2446299.1596+/-0.0064)+(1.2028287d+/-0.0000015)dxE. The first light and radial-velocity curve solutions allowed us to derive the basic physical properties of this astrophysically important binary.
- ID:
- ivo://CDS.VizieR/J/PASP/102/1392
- Title:
- UBV photometry from HK survey. I
- Short Name:
- J/PASP/102/1392
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Photoelectric photometry is presented for a sample of 139 halo stars drawn an extension of the HK (Ca II H & K lines) objective-prism survey of Beers, Preston and Shectmann (1988ApJS...67..461) to the Northern Galactic hemisphere. The candidates for which photometry is reported here were selected to span a wide range of types, but are dominated by stars classified as type AB, A, or "metal-poor" (MP).
- ID:
- ivo://CDS.VizieR/J/AcA/41/167
- Title:
- UBV photometry in Berkeley 32
- Short Name:
- J/AcA/41/167
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- CCD photometry on the UBV and Washington systems, is presented for Be32, a so far unstudied rich open cluster located in the Galactic anticentre. Morphology of cluster and colour-magnitude diagram indicates that it is an old object with age close to ages of NGC 188 and NGC 2243 (about 6Gyr on the scale of VandenBerg isochrones). The cluster reddening is E(B-V)=0.16 and the estimated metallicity is [Fe/H]=-0.37+/-0.05. The apparent distance modulus is between 12.8 and 13.1.
- ID:
- ivo://CDS.VizieR/J/AJ/116/1275
- Title:
- UBV photometry in 5 fields of the LMC
- Short Name:
- J/AJ/116/1275
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present UBV photometry of four fields within Shapley Constellation III and one field on the edge of the shell. Our fields cover roughly 20% of the region, mostly in the southern half. Determinations are made of ages of the fields, the star formation densities, and the initial mass function (IMF) slopes.
- ID:
- ivo://CDS.VizieR/J/ApJ/452/210
- Title:
- UBV photometry in LH 47/48
- Short Name:
- J/ApJ/452/210
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We examine the stellar population of an OB association, LH 47/48, which is associated with a superbubble H II region, DEM 152 in the N44 nebular complex of the Large Magellanic Cloud. With CCD photometry and spectroscopy of the massive stars, we find no evidence that an unusual stellar population gave rise to the shell morphology of the gas. The slope of the initial mass function, {Gamma}=1.3+/-0.2, is consistent with that of other OB associations in the LMC, and there is no significant difference in the initial mass function internal or external to the supershell. The inferred stellar ionizing flux is consistent with the observed nebular H alpha flux. We do find evidence for triggered star formation: the H-R diagram suggests an age of >10Myr for the population interior to the bubble with more recent, <5Myr, star formation on the exterior. Using the detailed data on the stellar population, we compare a numerical form of the Weaver et al. (1977ApJ...218..377W) evolutionary model for wind-driven bubbles with the observed shell kinematics. We find a substantial discrepancy: the observed shell radius is too small and/or expansion velocity too large to be explained with this version of the model. We discuss possible explanations for the inconsistency.
1669. UBV photometry in M15
- ID:
- ivo://CDS.VizieR/J/AJ/124/3255
- Title:
- UBV photometry in M15
- Short Name:
- J/AJ/124/3255
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this series of two papers, we describe a project with the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST) to measure the line-of-sight velocities of stars in the central few arcseconds of the dense globular cluster M15. This first paper focuses on the observations and reduction of the data. We "scanned" the central region of M15 spectroscopically by consecutively placing the 0.1" HST/STIS slit at 18 adjacent positions. The spectral pixel size exceeds the velocity dispersion of M15. This puts the project at the limit of what is feasible with STIS, and exceedingly careful and complicated data reduction and analysis were required.
- ID:
- ivo://CDS.VizieR/J/AJ/84/1305
- Title:
- UBV photometry in NGC 6528
- Short Name:
- J/AJ/84/1305
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- On the basis of its color-magnitude diagram NGC 6528 is one of the two most metal-rich globular clusters that have so far been found in the Galaxy. Such a conclusion is consistent with Morgan's metallic line-strength classification of the integrated spectrum of this cluster. The reddening of NGC 6528 is estimated to be E(B-V)=0.52+/-0.07, from which R=6.1kpc and Z=-0.4kpc.
