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1391. BeppoSAX Wide Field Camera X-Ray Source Catalog
ID:
ivo://nasa.heasarc/saxwfccat
Title:
BeppoSAX Wide Field Camera X-Ray Source Catalog
Short Name:
SAXWFCCAT
Date:
21 Feb 2025
Publisher:
NASA/GSFC HEASARC
Description:
This table contains the catalog of X-ray sources detected by the two Wide Field Cameras (WFCs) in complete observations on board BeppoSAX during its 6 years of operational lifetime, i.e., between April 1996 and April 2002. The BeppoSAX WFCs were coded mask instruments sensitive in the 2 - 28 keV energy band with a 40 x 40 square degree fields of view, pointing in opposite directions and perpendicularly to the BeppoSAX Narrow Field Instruments (NFI). The WFCs were usually operated simultaneously to NFI observations, each lasting up to several days. The WFCs observed thus the entire sky several times with a typical sensitivity of 2 to 10 mCrab. A systematic analysis of all WFC observations in the BeppoSAX archive has been carried out using the latest post-mission release of the WFC analysis software and calibrations. The catalog includes 253 distinct sources, obtained from a total sample of 8253 WFC detections. This table was created by the HEASARC in November 2007 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/472/705">CDS catalog J/A+A/472/705</a> file table3.dat. This is a service provided by NASA HEASARC .
1392. Berkeley 94 and Berkeley 96 UBVRcIcJHKs
ID:
ivo://CDS.VizieR/J/MNRAS/435/429
Title:
Berkeley 94 and Berkeley 96 UBVRcIcJHKs
Short Name:
J/MNRAS/435/429
Date:
21 Oct 2021
Publisher:
CDS
Description:
We have performed multiband UBVRcIcJHKs photometry of two young clusters located at large Galactocentric distances in the direction of the Perseus spiral arm. The obtained distances and colour excesses amount to 3.9+/-0.11kpc, E(B-V)=0.62+/-0.05 for Berkeley 94, and 4.3+/-0.15kpc, E(B-V)=0.58+/-0.06 for Berkeley 96. The respective ages, as measured from the comparison of the upper colour-magnitude diagrams to model isochrones, amount to log10Age(yr)=7.5+/-0.07 and 7.0+/-0.07, respectively. A sequence of optical pre-main-sequence (PMS) members is proposed in both clusters. In addition, samples of objects showing (H-Ks) excess are found. Part of these are suggested to be PMS cluster members of lower mass than the optical candidates. The spatial distribution of these sources, the comparison to Galactic models and to the expected number of contaminating distant red galaxies, and the spectral energy distribution in particular cases support this suggestion. The spatial distributions shown by members in different mass ranges can be interpreted in terms of the results from numerical simulations. According to these, different initial conditions and evolutionary dynamical paths are suggested for the clusters. Berkeley 94 would have formed under supervirial conditions, and followed the so-called warm collapse model in its evolution, whereas Berkeley 96 would have formed with a subvirial structure, and would have evolved following a cold collapse path. Both processes would be able to reproduce the suggested degree of mass segregation and their spatial distribution by mass range. Finally, the mass distributions of the clusters, from the most massive stars down to PMS stars around 1.3M_{sun}_, are calculated. An acceptable general agreement with the Salpeter initial mass function slope is found.
1393. Berkeley 21 BVI photometry
ID:
ivo://CDS.VizieR/J/MNRAS/299/834
Title:
Berkeley 21 BVI photometry
Short Name:
J/MNRAS/299/834
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present CCD BVI photometry of the old open cluster Berkeley 21, one of the most distant clusters in the Galactic anticentre direction, and possibly the lowest metallicity object in the open clusters sample. Its position and metal abundance make it very important for the study of the Galactic disc. Using the synthetic colour-magnitude diagram method, we estimate values for the distance modulus (m-M)_0_=13.4-13.6, reddening E(B-V)=0.74-0.78 (with possible differential absorption), and age= 2.2-2.5Gyr.
1394. Berkeley 32 BVI photometry and spectroscopy
ID:
ivo://CDS.VizieR/J/MNRAS/368/471
Title:
Berkeley 32 BVI photometry and spectroscopy
Short Name:
J/MNRAS/368/471
Date:
21 Oct 2021
Publisher:
CDS
Description:
We have obtained medium- and low-resolution spectroscopy and BVI CCD imaging of Berkeley 32, an old open cluster which lies in the anticentre direction. From the radial velocities of 48 stars in the cluster direction, we found that 31 of them, in crucial evolutionary phases, are probable cluster members, with an average radial velocity of +106.7(sigma=8.5)km/s . From isochrone fitting to the colour-magnitude diagrams of Berkeley 32, we have obtained an age of 6.3Gyr, (m-M)0=12.48 and E(B-V)=0.10. The best fit is obtained with Z=0.008. A consistent distance, (m-M)_0_~=12.6+/-0.1, has been derived from the mean magnitude of red clump stars with confirmed membership; we may assume (m-M)_0_~=12.55+/-0.1. The colour-magnitude diagram of the nearby field observed to check for field stars contamination looks intriguingly similar to that of the Canis Major overdensity.
1395. Berkeley 58 & CG Cas UBV photometry
ID:
ivo://CDS.VizieR/J/MNRAS/388/444
Title:
Berkeley 58 & CG Cas UBV photometry
Short Name:
J/MNRAS/388/444
Date:
21 Oct 2021
Publisher:
CDS
Description:
Photoelectric, photographic and CCD UBV photometry, spectroscopic observations and star counts are presented for the open cluster Berkeley 58 to examine a possible association with the 4.37d Cepheid CG Cas. The cluster is difficult to separate from the early-type stars belonging to the Perseus spiral arm, in which it is located, but has reasonably well-defined parameters: an evolutionary age of ~10^8^yr, a mean reddening of E(B-V)(B0)=0.70+/-0.03 s.e. and a distance of 3.03+/-0.1kpc (V_0_-M_V_=12.40+/-0.12 s.d.). CG Cas is a likely cluster coronal member on the basis of radial velocity, and its period increase of +0.170+/- 0.01s/y and large light amplitude describe a Cepheid in the third crossing of the instability strip lying slightly blueward of strip centre. Its inferred reddening and luminosity are E(B-V)=0.64+/-0.02 s.e. and <M_V_>=-3.06+/-0.12. A possible K supergiant may also be a cluster member.
1396. Berkeley Extreme and Far-UV Spectrometer
ID:
ivo://archive.stsci.edu/befs
Title:
Berkeley Extreme and Far-UV Spectrometer
Short Name:
BEFS
Date:
22 Jul 2020 21:27:59
Publisher:
Space Telescope Science Institute Archive
Description:
The Berkeley Extreme and Far-UV Spectrometer (BEFS), flew on the Orbiting and Retrievable Far and Extreme Ultraviolet Spectrograph (ORFEUS)-SPAS I and II space shuttle missions in 1993 and 1996, returning high-resolution (/3000) FUV spectra (900-1200 Å) of 75 astrophysical objects from the first flight and more than 100 from the second. EUV spectra (400-900 Å) were obtained for a subset of these targets.
1397. Berkeley 90. III. Cluster parameters
ID:
ivo://CDS.VizieR/J/MNRAS/465/784
Title:
Berkeley 90. III. Cluster parameters
Short Name:
J/MNRAS/465/784
Date:
21 Oct 2021
Publisher:
CDS
Description:
The open cluster Berkeley 90 is the home to one of the most massive binary systems in the Galaxy, LS III +46 11, formed by two identical, very massive stars (O3.5 If* + O3.5 If*), and a second early-O system (LS III +46 12 with an O4.5 IV((f)) component at least). Stars with spectral types earlier than O4 are very scarce in the Milky Way, with no more than 20 examples. The formation of such massive stars is still an open question today, and thus the study of the environments where the most massive stars are found can shed some light on this topic. To this aim, we determine the properties and characterize the population of Berkeley 90 using optical, near-infrared and WISE photometry and optical spectroscopy. This is the first determination of these parameters with accuracy. We find a distance of 3.5+/-0.5kpc and a maximum age of 3Ma. The cluster mass is around 1000M_{sun}_ (perhaps reaching 1500M_{sun}_ if the surrounding population is added), and we do not detect candidate runaway stars in the area. There is a second population of young stars to the Southeast of the cluster that may have formed at the same time or slightly later, with some evidence for low-activity ongoing star formation.
1398. Berkeley Low-Latitude H I Survey
ID:
ivo://CDS.VizieR/VIII/11
Title:
Berkeley Low-Latitude H I Survey
Short Name:
VIII/11
Date:
21 Oct 2021
Publisher:
CDS
Description:
This survey consists of H I 21-cm spectra covering galactic latitudes from -10 degrees to +10 degrees and galactic longitudes from 10degrees to 250degrees. The observations were made with the Hat Creek 85-foot telescope between 1968 and 1970. The individual spectra contain 238 points per profile spaced every 5kHz and cover a velocity range of 250km/s. The velocity resolution is 2km/s (half-power of each filter) and the half-power beamwidth is 35arcmin. The spacing between points observed on the sky are 0.25degrees in galactic latitude and 0.5degrees in galactic longitude. Each spectrum or record consists of a header followed by 238 antenna temperatures. The header contains the galactic longitude, galactic latitude, and central velocity (LSR). The catalog contains a total of 38961 spectra.
1399. Berkeley 93 RVB photometry
ID:
ivo://CDS.VizieR/J/AJ/107/2101
Title:
Berkeley 93 RVB photometry
Short Name:
J/AJ/107/2101
Date:
21 Oct 2021
Publisher:
CDS
Description:
While performing galactic and extragalactic studies near the galactic plane in Cepheus. CCD frames in B, V, and R were taken of the faint (V>=16m), previously unstudied open star cluster Berkeley 93 (Be 93). Our results indicate that this object is the core of a larger aggregate, is slightly evolved, strongly reddened [E(B-V)~1.5], and shows a pronounced variable reddening that is probably due to the location of the cluster inside (near the border) a dust cloud. By far the reddest, and obviously most evolved star is a (variable) carbon star that-because of its reddening and location-appears to be a cluster member. We present arguments in favour of a large distance of more than 5kpc for Be 93 which possibly belongs to the galactic warp. As an addendum, we present six star concentrations discovered on the POSS or ESO/SERC atlas that might represent hitherto uncatalogued open star clusters of "Berkeley type."
1400. Berkeley 39 stars photometry and abundances
ID:
ivo://CDS.VizieR/J/A+A/548/A122
Title:
Berkeley 39 stars photometry and abundances
Short Name:
J/A+A/548/A122
Date:
21 Oct 2021
Publisher:
CDS
Description:
The most massive star clusters include several generations of stars with a different chemical composition (mainly revealed by an Na-O anti-correlation) while low-mass star clusters appear to be chemically homogeneous. We are investigating the chemical composition of several clusters with masses of a few 10^4^M_{sun}_ to establish the lower mass limit for the multiple stellar population phenomenon. Using VLT/FLAMES spectra we determine abundances of Fe, O, Na, and several other elements ({alpha} Fe-peak, and neutron-capture elements) in the old open cluster Berkeley 39. This is a massive open cluster: M~10^4^M_{sun}_, approximately at the border between small globular clusters and large open clusters. Our sample size of about 30 stars is one of the largest to be studied for abundances in any open cluster, and could be useful to determine improved cluster parameters, like age, distance, and reddening, when coupled with precise, well-calibrated photometry. We find that Berkeley 39 is slightly metal- poor, <[Fe/H]>~=-0.20, in agreement with previous studies of this cluster. More importantly, we do not detect any star-to-star variation in the abundances of Fe, O, and Na, within quite stringent upper limits. The r.m.s. scatter is of 0.04, 0.10, and 0.05dex for Fe, O, and Na, respectively. Such a small spread can be entirely explained by the noise in the spectra and by uncertainties in the atmospheric parameters. We conclude that Berkeley 39 is a single-population cluster.

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