- ID:
- ivo://CDS.VizieR/VII/31B
- Title:
- Star Clusters/Associations. I. Associations
- Short Name:
- VII/31B
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The catalog contains data and bibliographical citations for all 70 associations of the second edition of the "Catalogue of Star Clusters and Associations (CSCA)" edited by Alter et al. (1970) which includes data for open clusters, associations, globular clusters and extragalactic objects up to 1967 and "Supplement to the CSCA" by Ruprecht et al. (1982), which contains the supplementary data up to the end of 1973. Thus, the literature is covered through 1973. The catalog includes the years of the literature, references, authors, abbreviated journal references, diameters, distances and color indices of the associations, number of stars and spectral types of the stars in the associations, and identification of the Palomar Observatory Sky Survey Chart on which the association appears.
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- ID:
- ivo://CDS.VizieR/VII/101A
- Title:
- Star Clusters/Associations. III. Open Clusters
- Short Name:
- VII/101A
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This catalogue includes the Open Clusters of the supplement up to 1973 of the "Catalogue of Star Clusters and Associations" by Alter G., Ruprecht J., Vanysek V., Budapest 1970. The file "main.dat" contains the original data. For each cluster, the first line contains the running number (OCL) followed by various designations. The first five figures represent the galactic longitude (in 0.01degree), 'N' or 'S' for North or South galactic hemisphere, and galactic latitude (in 0.01degree). The second line contains the 1950 coordinates, the 50-yr precession, the galactic direction cosines and the position on the POSS charts. For each cluster a number of bibliographic records follow containing: YEAR: Year of the literature reference NAME: Author PUBLICATION: Reference AD: Angular diameter of the cluster in arc minutes DIST: Distance of the cluster (pc) LD: Linear diameter of the cluster (pc) N: Number of stars studied CI: Color index SP: Spectra P: Positions RV: Radial velocity (km/s) MT: Integrated magnitude NOTE: Notes The file "clusters" has been created from first and second lines; missing equatorial coordinates were derived from the galactic ones.
- ID:
- ivo://CDS.VizieR/III/216
- Title:
- Stellar Radial Velocities 1991-1998
- Short Name:
- III/216
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The present catalogue is the third version and supersedes the first one (1991-1994) published by Malaroda et al. (2000A&AS..144....1M, Cat. <III/204>). We have revised the issues of the journals listed in Table 1, for the period 1991-1998. It is not a complete list of all journals devoted to astronomical literature, but they are the most important ones and those available at our libraries. We prepared a plain ASCII file with the object identifications as provided by the authors. This file was transferred to the SIMBAD database, and, using the proper formats and filters, we have retrieved the identification for each object according to the rules of SIMBAD. In the same way we have also retrieved: the J2000 coordinates, the V magnitude, and the spectral classification for each object.
- ID:
- ivo://CDS.VizieR/III/249
- Title:
- Stellar radial velocities bibliographic catalog
- Short Name:
- III/249
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- The present catalogue is the twelfth version and the continuation of the first one (1991-1994) published by Malaroda et al. (2000A&AS..144....1M). Since the 2005 version, we present the catalogue in a database for helping the search. We have revised the issues of the journals listed in Table 1, for the period 1991-2006June. It is not a complete list of all journals devoted to astronomical literature, but they are the most important ones and those available at our libraries. We prepared a plain ASCII file with the object identifications as provided by the authors. This file was transferred to the SIMBAD database, and, using the proper for mats and filters, we have retrieved the identification for each object according to the rules of SIMBAD. In the same way we have also retrieved: the J2000 coordinates, the V magnitude, and the spectral classification for each object.
- ID:
- ivo://CDS.VizieR/III/204
- Title:
- Stellar radial velocities bibliographic catalog
- Short Name:
- III/204
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a bibliographic catalogue of stellar radial velocities with 13359 entries for stars in the Galaxy and the Magellanic Clouds, obtained from the issues of several journals published in the period 1991-1994. We have tried to follow the structure of previous compilations although we have relied on data retrieved from the SIMBAD database.
- ID:
- ivo://CDS.VizieR/J/ApJS/248/21
- Title:
- Swift long gamma-ray bursts
- Short Name:
- J/ApJS/248/21
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The exact relationship between the long gamma-ray burst (LGRB) rate and the cosmic star formation rate (CSFR) is essential for using LGRBs as cosmological probes. In this work, we collect a large sample composed of 371 Swift LGRBs with known redshifts and prompt emission properties. We first compare the rest-frame prompt properties of these bursts in different redshift bins, finding negligible redshift evolution of the luminosity of LGRBs with L_iso_>~10^51^erg/s between z~1 and z~4. Then, by utilizing the CSFR obtained from the large-scale cosmological hydrodynamical simulation, the Illustris simulation, we calculate the cumulative redshift distribution of LGRBs under different metallicity thresholds. After comparing with our sample, we find that the predictions with a moderate threshold between 0.3Z_{sun}_<=Z_th_<=1.0Z_{sun}_ are consistent with the sample between redshift 0<z<3, while at higher redshifts, between 3<z<5, all metallicity thresholds fit the data well. When changing to an empirical model based on observations, the predictions show similar results as well. After comparing with the metallicity distribution of the observed LGRB host galaxies between 0<z<1, we confirm that the production of LGRBs in galaxies with super-solar metallicity is suppressed. Nevertheless, considering that a significant fraction of stars are born in sub-solar metallicity environments at z>~3, we suggest that, as a first approximation, LGRBs can be used as direct tracers of the CSFR in this redshift range.
- ID:
- ivo://CDS.VizieR/J/ApJS/240/21
- Title:
- Symbiotic stars with 2MASS, WISE & Gaia data
- Short Name:
- J/ApJS/240/21
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a new census of Galactic and extragalactic symbiotic stars (SySts). This compilation contains 323 known and 87 candidate SySts. Of the confirmed SySts, 257 are Galactic and 66 extragalactic. The spectral energy distributions (SEDs) of 348 sources have been constructed using 2MASS and AllWISE data. Regarding the Galactic SySts, 74% are S types, 13% D, and 3.5% D'. S types show an SED peak between 0.8 and 1.7{mu}m, whereas D types show a peak at longer wavelengths between 2 and 4{mu}m. D' types, on the other hand, display a nearly flat profile. Gaia distances and effective temperatures are also presented. According to their Gaia distances, S types are found to be members of both thin and thick Galactic disk populations, while S+IR and D types are mainly thin disk sources. Gaia temperatures show a reasonable agreement with the temperatures derived from SEDs within their uncertainties. A new census of the OVI{lambda}6830 Raman-scattered line in SySts is also presented. From a sample of 298 SySts with available optical spectra, 55% are found to emit the line. No significant preference is found among the different types. The report of the OVI{lambda}6830 Raman-scattered line in non-SySts is also discussed as well as the correlation between the Raman-scattered OVI line and X-ray emission. We conclude that the presence of the OVI Raman-scattered line still provides a strong criterion for identifying a source as a SySt.
- ID:
- ivo://CDS.VizieR/J/ApJ/863/181
- Title:
- The fifth catalog of LMC Wolf-Rayet stars
- Short Name:
- J/ApJ/863/181
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We summarize the results of our 4yr survey searching for Wolf-Rayet (WR) stars in the Large Magellanic Cloud (LMC) and Small Magellanic Cloud. Over the course of this survey we have discovered 15 new WR stars and 12 Of-type stars. In this last year we discovered two rare Of-type stars: an O6.5f?p and an O6nfp, in addition to the two new Of?p stars discovered in our first year and the three Onfp stars discovered in our second and third years. However, even more exciting was our discovery of a new type of WR star, ones we are calling WN3/O3s owing to their spectroscopic signatures. We describe the completeness limits of our survey and demonstrate that we are sensitive to weak-lined WRs several magnitudes fainter than any we have discovered, arguing that there is not a population of fainter WRs waiting to be discovered. We discuss the nature of the WN3/O3s, summarizing the results of our extensive spectroscopy and modeling. We also examine the important claim made by others that the WN3/O3s are isolated compared to other massive stars. We find that if we use a more complete sample of reference massive stars, the WN3/O3s show the same spatial distribution as other early WNs, consistent with a common origin. Finally, we use this opportunity to present the "Fifth Catalog of LMC Wolf-Rayet Stars," which includes revised coordinates and updated spectral types for all 154 known LMC WRs.
- ID:
- ivo://CDS.VizieR/J/ApJS/249/32
- Title:
- The Multi-INstrument Burst ARchive (MINBAR)
- Short Name:
- J/ApJS/249/32
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the largest sample of type I (thermonuclear) X-ray bursts yet assembled, comprising 7083 bursts from 85 bursting sources. The sample is drawn from observations with Xenon-filled proportional counters on the long-duration satellites RXTE, BeppoSAX, and International Gamma-Ray Astrophysics Laboratory between 1996 February 8 and 2012 May 3. The burst sources were drawn from a comprehensive catalog of 115 burst sources, assembled from earlier catalogs and the literature. We carried out a consistent analysis for each burst light curve (normalized to the relative instrumental effective area) and provide measurements of rise time, peak intensity, burst timescale, and fluence. For bursts observed with the RXTE/PCA and BeppoSAX/Wide Field Camera we also provide time-resolved spectroscopy, including estimates of bolometric peak flux and fluence, and spectral parameters at the peak of the burst. For 950 bursts observed with the PCA from sources with previously detected burst oscillations, we include an analysis of the high time resolution data, providing information on the detectability and amplitude of the oscillations, as well as where in the burst they are found. We also present analysis of 118,848 observations of the burst sources within the sample time frame. We extracted 3-25keV X-ray spectra from most observations, and (for observations meeting our signal-to-noise criterion) we provide measurements of the flux, spectral colors, and, for selected sources, the position on the color-color diagram, for the best-fit spectral model. We present a description of the sample, a summary of the science investigations completed to date, and suggestions for further studies.
- ID:
- ivo://CDS.VizieR/J/ApJ/871/244
- Title:
- Times of X-ray minima & orbit numbers of Cyg X-3
- Short Name:
- J/ApJ/871/244
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- By using available archival X-ray data, we significantly extended the list of times of X-ray minima. The new list includes 65 data points obtained by critically reanalyzing RXTE ASM data, 88 data points based on observations by MAXI, and 2 data points based on observations by SUZAKU and AstroSat. Analyzing the data along with times of X-ray minima available from the literature, we provide the most accurate estimate of the rate of period change to date. We do not confirm the existence of a second derivative of the orbital period suggested by some authors earlier. Instead, we find that the changes in the period can be fit by a sum of quadratic and sinusoidal functions. The period of sinusoidal variations is 15.79yr. They can be related either to apsidal motion in the close binary with eccentricity e~0.03 or to the presence of a third body with a mass of about 0.7M_{sun}_ located at a distance ~16 au from the close binary.
