- ID:
- ivo://CDS.VizieR/J/A+A/375/670
- Title:
- Photographic observations of radio stars
- Short Name:
- J/A+A/375/670
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- At the Engelhardt Astronomical Observatory (EAO), we observed photographic positions of 113 Galactic Radio Sources (GRS) in the system PPM catalogue (Rizvanov & Dautov, 1998, Kinematics and physics celestial bodies, 5, 457). Analysis of their accuracy is made by comparison with the Hipparcos catalogue (Perryman et al., 1997, Vat. <I/239>) and astrometric catalogue of radio stars in the radio window from the article of Walter et al. (1990A&AS...86..357W).
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- ID:
- ivo://CDS.VizieR/J/A+A/374/968
- Title:
- Photometric and kinematic properties of LPVs
- Short Name:
- J/A+A/374/968
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The table gives individual absolute K and IRAS 12 and 25 luminosities of 800 LPVs. They are obtained by applying the Luri-Mennessier (LM, see below) calibration method to a sample composed of stars which are either of type M (O-rich), C (C-rich) or S (C/O~1), including Mira (M), SR (of both type a and b) and L variables. Astrometric data is taken exclusively from the HIPPARCOS Catalogue. Radial velocities are taken from the HIPPARCOS Input Catalogue. K band photometric data are gathered from various sources. Infrared magnitudes are derived from the fluxes measured by the IRAS satellite: m(12)=3.63-2.5log(F(12)) and m(25)=2.07-2.5log(F(25)) The stellar population from which the sample is extracted is assumed to be composed of several distinct groups that can differ in kinematics, luminosity or spatial distribution. The LM method determines the number of significant discriminating groups and produces, for each group, unbiased estimates of the mean parameters of the galactic and luminosity model. In a second step the method uses a Bayesian rule to statistically assign each star to a group. Table gives these assignations denoted as G(G') i.e. to group G in K and G'in IRAS. Three groups are identified in the K band. They can be interpreted as the galactic disk (D), old disk (OD) and extended disk (ED) populations. Four groups are identified in the IRAS bands. They are similar to those identified in the K band except that the old disk group is divided into ``bright'' (ODb) and ``faint'' (ODf) subgroups. Let us add that D, ODb and ED correspond to thick circumstellar envelope stars, while ODf is mainly composed of stars with a thin (or even lacking) envelope.
- ID:
- ivo://CDS.VizieR/VII/147
- Title:
- Photometric Catalog of Northern Bright Galaxies
- Short Name:
- VII/147
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Galaxies are the most massive, luminous astronomical objects bound by self gravity and comprise the major fraction of luminous mass in the universe. Recent investigations of galaxies often require statistical analysis of a large body of observational data. High degree of homogeneity of the data is the key point to the success of such investigations. This catalog presents homogeneous photometric parameters of 791 northern bright galaxies on the basis of modern photographic surface photometry. Sample galaxies are taken from the Revised Shapley-Ames Catalog of Bright Galaxies (Sandage and Tammann 1981) and most of them are members of the Local Super-cluster. Observations were made with the 105cm Schmidt telescope at the Kiso Observatory, Institute of Astronomy, University of Tokyo, in the photographic V band (Kodak IIa-D emulsion combined with a Schott GG 495 filter) mostly during 1984-1988. Sample galaxies photographed on a total of 280 Schmidt plates were scanned with the PDS 2020 GMS microdensitometer at the Kiso Observatory during April-August 1988. Data reduction for standard surface photometry was carried out using a software library SPIRAL (Ichikawa et al. 1987; Okamura 1988) during July-September 1988. The intensive plate measurement and data reduction secure high homogeneity of the present data. This catalog is the first machine-readable version (Ver.1) of Part II (The Catalog) of the 'Photometric Atlas of Northern Bright Galaxies' (Kodaira et al. 1990), which also includes in Part III illustrative information such as images, isophotal maps, luminosity profiles, and ellipses fitted to the isophotes. Image data of sample galaxies can be obtained in FITS format magnetic tapes upon request, and it is planned to distribute them on CD-ROMs. We request that those errors in this catalog that are found by the user be transmitted to S. Ichikawa, National Astronomical Observatory, Mitaka, Tokyo 181 Japan (e-mail : richika@c1.mtk.nao.ac.jp) so that they can be corrected in future versions.
- ID:
- ivo://CDS.VizieR/V/140
- Title:
- Photometric rotation periods of stars in {alpha} Per
- Short Name:
- V/140
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results from a photometric monitoring program of primarily solar-type open cluster stars obtained during 1994 and 1995. Several members of the {alpha} Persei cluster have been monitored and the corresponding relation between coronal x-ray activity and rotation period derived. The relation among mid-G/K type members illustrates both the previously noticed downturn in L_X_/L_bol_ at high rotation rates and the sharp decrease in coronal activity at long rotation periods as seen among Pleiades stars. Intensive observation of one slowly rotating G-type member of IC 4665 has enabled a period determination of 8-10 days to be made and illustrates the need for (and limitations of) high quality observations.
- ID:
- ivo://CDS.VizieR/J/ApJS/228/9
- Title:
- Physical parameters of ~300000 SDSS-DR12 QSOs
- Short Name:
- J/ApJS/228/9
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We use the Sloan Digital Sky Survey (SDSS) Quasar Data Release 12 (DR12Q), containing nearly 300000 active galactic nuclei (AGNs), to calculate the monochromatic luminosities at 5100, 3000, and 1350{AA}, derived from the broadband extinction-corrected SDSS magnitudes. After matching these sources to their counterparts from the SDSS Quasar Data Release 7 (DR7Q), we find very high correlations between our luminosities and DR7Q spectra-based luminosities with minute mean offsets (~0.01dex) and dispersions of differences of 0.11, 0.10, and 0.12dex, respectively, across a luminosity range of 2.5dex. We then estimate the black hole (BH) masses of the AGNs using the broad line region radius-disk luminosity relations and the FWHM of the MgII and CIV emission lines, to provide a catalog of 283033 virial BH mass estimates (132451 for MgII, 213071 for CIV, and 62489 for both) along with the estimates of the bolometric luminosity and Eddington ratio for 0.1<z<5.5 and for roughly a quarter of the sky covered by SDSS. The BH mass estimates from Mg II turned out to be closely matched to the ones from DR7Q with a dispersion of differences of 0.34dex across a BH mass range of ~2dex. We uncovered a bias in the derived CIV FWHMs from DR12Q as compared to DR7Q, which we correct empirically. The CIV BH mass estimates should be used with caution because the CIV line is known to cause problems in the estimation of BH mass from single-epoch spectra. Finally, after the FWHM correction, the AGN BH mass estimates from CIV closely match the DR7Q ones (with a dispersion of 0.28dex), and more importantly the MgII and CIV BH masses agree internally with a mean offset of 0.07dex and a dispersion of 0.39dex.
276. PNe in NGC 5128
- ID:
- ivo://CDS.VizieR/J/ApJS/88/423
- Title:
- PNe in NGC 5128
- Short Name:
- J/ApJS/88/423
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.
- ID:
- ivo://CDS.VizieR/J/ApJS/171/146
- Title:
- Population synthesis in the blue. IV
- Short Name:
- J/ApJS/171/146
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a new set of model predictions for 16 Lick absorption line indices from H{delta} through Fe5335 and UBV colors for single stellar populations with ages ranging between 1 and 15Gyr, [Fe/H] ranging from -1.3 to +0.3, and variable abundance ratios. The models are based on accurate stellar parameters for the Jones library stars and a new set of fitting functions describing the behavior of line indices as a function of effective temperature, surface gravity, and iron abundance. The abundances of several key elements in the library stars have been obtained from the literature in order to characterize the abundance pattern of the stellar library, thus allowing us to produce model predictions for any set of abundance ratios desired. We develop a method to estimate mean ages and abundances of iron, carbon, nitrogen, magnesium, and calcium that explores the sensitivity of the various indices modeled to those parameters. The models are compared to high-S/N data for Galactic clusters spanning the range of ages, metallicities, and abundance patterns of interest. Essentially all line indices are matched when the known cluster parameters are adopted as input. Comparing the models to high-quality data for galaxies in the nearby universe, we reproduce previous results regarding the enhancement of light elements and the spread in the mean luminosity-weighted ages of early-type galaxies.
- ID:
- ivo://CDS.VizieR/J/A+A/427/933
- Title:
- Precise temperature of F-K field dwarfs
- Short Name:
- J/A+A/427/933
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Highly precise temperatures (sigma=10-15K) have been determined from line depth ratios for a set of 248 F-K field dwarfs of about solar metallicity (-0.5<[Fe/H]<+0.4), based on high resolution (R=42000), high S/N echelle spectra. A new gap has been discovered in the distribution of stars on the Main Sequence in the temperature range 5560 to 5610K. This gap coincides with a jump in the microturbulent velocity Vt and the well-known Li depression near 5600K in field dwarfs and open clusters. As the principal cause of the observed discontinuities in stellar properties we propose the penetration of the convective zone into the inner layers of stars slightly less massive than the Sun and related to it, a change in the temperature gradient.
- ID:
- ivo://CDS.VizieR/I/207
- Title:
- Preliminary list from Tycho observations (TIC data)
- Short Name:
- I/207
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The selection of the stars of the Tycho program is mainly based on the Tycho input catalogue (TIC), prepared by Egret et al. (1992) from existing ground-based catalogues. The TIC is far to be the definitive list of the stars that will appear in the final Tycho catalogue however. The number of stars included within (3 million) is several times larger than the number eventually expected. The selection of the TIC stars that will remain in the final catalogue is planned in two steps : The former is the "Recognition" that is based on the first year of the scientific mission. The latter step of selection is the final reduction of the Tycho data, which will require a few more years. The recognition was completed in 1992, and, among the 3,154,204 stars of the TIC, about two third were not found in the observations. This catalogue presents the 1,049,971 stars that are still in the programme. The selection is nor definitive, nor complete; but it should contain only a small percentage of stars that will still be discarded. On another side, some stars missing in the TIC have been added to the Tycho program, but the expected number of additional stars to appear in the final catalogue should be about 5 % or less. The list was announced in Halbwachs et al (1994). It is completed with data (coordinates and magnitudes) from the main file of the Tycho Input Catalogue. The cross-identifications with the Hipparcos Input Catalogue or with the INCA database included in catalogue I/197/ are not repeated here.
- ID:
- ivo://CDS.VizieR/J/A+A/597/A24
- Title:
- Probing the dynamical of Abell S1101
- Short Name:
- J/A+A/597/A24
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The galaxy cluster Abell S1101 (S1101 hereafter) deviates significantly from the X-ray luminosity versus velocity dispersion relation (L-sigma) of galaxy clusters in our previous study. Given reliable X-ray luminosity measurement combining XMM-Newton and ROSAT, this could most likely be caused by the bias in the velocity dispersion due to interlopers and low member statistic in the previous sample of member galaxies, which was solely based on 20 galaxy redshifts drawn from the literature. We intend to increase the galaxy member statistic to perform a precision measurement of the velocity dispersion and dynamical mass of S1101. We aim for a detailed substructure and dynamical state characterization of this cluster, and a comparison of mass estimates derived from (i) the velocity dispersion (M_vir_), (ii) the caustic mass computation (M_caustic_), and (iii) mass proxies from X-ray observations and the Sunyaev- Zeldovich (SZ) effect. We carried out new optical spectroscopic observations of the galaxies in this cluster field with VIMOS, obtaining a sample of ~60 member galaxies for S1101. We revised the cluster redshift and velocity dispersion measurements based on this sample and also applied the Dressler-Shectman substructure test. The completeness of cluster members within r200 was significantly improved for this cluster. Tests for dynamical substructure did not show evidence for major disturbances or merging activities in S1101. We find good agreement between the dynamical cluster mass measurements and X-ray mass estimates which confirms the relaxed state of the cluster displayed in the 2D substructure test. The SZ mass proxy is slightly higher than the other estimates. The updated measurement of the velocity dispersion erased the deviation of S1101 in the L-sigma relation.
