- ID:
- ivo://CDS.VizieR/J/A+AS/127/251
- Title:
- Giants and supergiants ROSAT data
- Short Name:
- J/A+AS/127/251
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present X-ray data for all late-type (A,F,G,K,M) giants and supergiants (luminosity classes I to III-IV) listed in the Bright Star Catalogue that have been detected in the ROSAT all-sky survey. The selection of the sample stars, the data analysis, the criteria for an accepted match between star and X-ray source, and the determination of X-ray fluxes are described.
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Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/603/L7
- Title:
- 6 giants atomic data and equivalent widths
- Short Name:
- J/A+A/603/L7
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We observed six He-clump stars of the intermediate-age stellar cluster Gaia1 with the MIKE/MAGELLAN spectrograph. A possible extra-galactic origin of this cluster, recently discovered thanks to the first data release of the ESA Gaia mission, has been suggested, based on its orbital parameters. Abundances for Fe, {alpha}, proton- and neutron-capture elements have been obtained. We find no evidence of intrinsic abundance spreads. The iron abundance is solar ([FeI/H]=+0.00+/-0.01; {sigma}=0.03dex). All the other abundance ratios are generally solar-scaled, similar to the Galactic thin disk and open cluster stars of similar metallicity. The chemical composition of Gaia1 does not support an extra-galactic origin for this stellar cluster, which can be considered as a standard Galactic open cluster.
7323. Giants DDO photometry
- ID:
- ivo://CDS.VizieR/J/AJ/100/1191
- Title:
- Giants DDO photometry
- Short Name:
- J/AJ/100/1191
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A sample of G and K giants approximately 4kpc from the Sun, covering the abundance range from solar to extreme halo has been selected without kinematic bias in a field aligned to measure galactic rotation. Accurate abundances, distances, and radial velocities have been measured. This sample has been combined with nonkinematically selected solar neighborhood objects taken from the literature, in order to examine the kinematics of the transition from disk to "thick disk" to halo. The metal-rich objects in the sample, with 0>[Fe/H]>-0.8, rotate rapidly around the galactic center and have low azimuthal velocity dispersion, {sigma}_{phi}_=40+/-10km/s. For objects in the range -0.5>[Fe/H]>-0.8, we find a small value for the asymmetric drift of 35+/-10km/s. We associate these objects with the thick disk, confirming the kinematical results of Ratnatunga and Freeman (1989, Cat.<V/65>) and others. In the abundance range -1.0>[Fe/H]>=-1.6 we find, in addition to objects with normal halo kinematics, objects in a disk configuration, confirming the results of Norris, Bessell, and Pickles (1985ApJS...58..463N). This disk is rotating rapidly, V_rot_=170+/-15km/s, and has a scale height of 1.4+/-0.7kpc, these kinematical and spatial properties are similar to those of the thick disk. We show that these objects have different kinematics from that of the globular clusters and a sample of local RR Lyraes in the same abundance range. This suggests to us that these objects are better associated with the thick disk than the halo, and we refer to them as "metal-weak thick-disk stars". Hence we suggest that the conventional chemical description of the thick disk (Gilmore and Wyse, 1985AJ.....90.2015G) be widened to include stars with abundances as low as [Fe/H]=-1.6. At the galactic plane, the density of these metal-weak thick-disk stars is similar to that of halo stars, so they significantly affect the measurement, from samples selected on abundance, of the components of the velocity ellipsoid for the halo in the solar neighborhood. For the halo giants in our sample we measure {sigma}_{phi}_=102+/-24 and V_rot_=17+/-24km/s. The rotation velocity and velocity ellipsoid for the metal-weak halo in the solar neighborhood have been rederived for objects with [Fe/H]<=-1.6 from the large sample of Norris (1986ApJS...61..667N), thus removing the possibility of contamination by metal-weak thick-disk stars. We derive V_rot_=25+/-15km/s and ({sigma}_r_, {sigma}_{phi}_, {sigma}_{theta}_)=(133+/-8, 98+/-13, 94+/-6)km/s. These values are more consistent with other information about the shape of the halo. For a description of the DDO photometric system, see e.g. <GCPD/12>
- ID:
- ivo://CDS.VizieR/J/A+A/658/A48
- Title:
- 7 giants/subgiants limb-darkening coefficients
- Short Name:
- J/A+A/658/A48
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- Large spectroscopic surveys of the Milky Way need to be calibrated against a sample of benchmark stars to ensure the reliable determination of atmospheric parameters. Here we present new fundamental stellar parameters of seven giant and subgiant stars that will serve as benchmark stars for large surveys. The aim is to reach a precision of 1% in the effective temperature. This precision is essential for accurate determinations of the full set of fundamental parameters and abundances of stars observed by the stellar surveys. We observed HD121370 (eta Boo), HD161797 (mu Her), HD175955, HD182736, HD185351, HD188512 (beta Aql), and HD189349 using the high angular resolution optical interferometric instrument PAVO at the CHARA Array. The limb-darkening corrections were determined from 3D model atmospheres based on the STAGGER grid. The Teff were determined directly from the Stefan-Boltzmann relation, with an iterative procedure to interpolate over tables of bolometric corrections. We estimated surface gravities from comparisons to Dartmouth stellar evolution model tracks. The spectroscopic observations were collected from the ELODIE and FIES spectrographs. We estimated metallicities ([Fe/H]) from a 1D non-local thermodynamic equilibrium (NLTE) abundance analysis of unblended lines of neutral and singly ionised iron. For six of the seven stars we measure Teff to better than 1%. For one star, HD189349, the uncertainty in Teff is 2% due to an uncertain bolometric flux. We do not recommend this star as a benchmark until this measurement can be improved. Median uncertainties for all stars in logg and [Fe/H]} are 0.034dex and 0.07dex, respectively. This study presents updated fundamental stellar parameters of seven giant and subgiant stars that can be used as a new set of benchmarks. All the fundamental stellar parameters were based on consistently combining interferometric observations, 3D limb-darkening modelling and spectroscopic analysis. This paper in this series follows our previous papers including dwarf stars and stars in the metal-poor range.
- ID:
- ivo://CDS.VizieR/J/A+AS/121/95
- Title:
- Giant stars abundances in 24 clusters
- Short Name:
- J/A+AS/121/95
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have obtained high resolution, high signal-to-noise ratio CCD echelle spectra of 10 bright red giants in 3 globular clusters (47 Tuc, NGC 6752 and NGC 6397) roughly spanning the whole range of metallicities of the galactic globular cluster system. The analysis of this newly acquired material reveals no significant evidence of star-to-star variation of the [Fe/H] ratio in these three clusters. Moreover, a large set of high quality literature data (equivalent widths from high dispersion CCD spectra) was re-analyzed in an homogeneous and self-consistent way to integrate our observations and derive new metal abundances for more than 160 bright red giants in 24 globular clusters (i.e. about 16% of the known population of galactic globulars). This set was then used to define a new metallicity scale for globular clusters which is the result of high quality, direct spectroscopic data, of new and updated model atmospheres from the grid of Kurucz (1992), and of a careful fine abundance analysis; this last, in turn, is based on a common set of both atomic and atmospheric parameters for all the stars examined.
- ID:
- ivo://CDS.VizieR/J/A+A/645/A14
- Title:
- GIBS sources equivalent widths
- Short Name:
- J/A+A/645/A14
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We developed a set of procedures to automatically detect and measure the DIB around 8620{AA} (the Gaia DIB) for a wide range of temperatures. The method was tested on about 5000 spectra from the Giraffe Inner Bulge Survey (GIBS; Zoccali et al., 2014A&A...562A..66Z), and 4194 reasonable fitting results were got. We made use of the reddenings, E(J-Ks), from the extinction map developed by Surot et al. (2020arXiv201002723S). A linear correlation between the equivalent width (EW) and E(J-Ks) was derived as E(J-Ks)/EW = 1.875, according to E(B-V)/EW = 2.721, which is highly consistent with previous results toward similar sightlines. After a correction based on the Vista Variables in the Via Lactea (VVV; Minniti et al., 2010NewA...15..433M) database for both EW and E(J-Ks), the coefficient derived from individual GIBS fields, E(J-Ks)/EW=1.884, is also in perfect agreement with literature values. Based on a subsample of 1015 stars toward the Galactic center, we determined a rest-frame wavelength of the Gaia DIB as 8620.55{AA}. A Gaussian profile is proved to be a proper and stable assumption for the Gaia DIB as no intrinsic asymmetry is found.
- ID:
- ivo://nasa.heasarc/gingaasmlc
- Title:
- Ginga ASM Source Lightcurves
- Short Name:
- GINGAASMLC
- Date:
- 27 Sep 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The GINGAASMLC database table contains information derived from the FITS lightcurves obtained with the ASM on board the Ginga mission. The lightcurves are rates as function of time, and they can be used with the general FITS tools within HEAsoft or XRONOS. The FITS lightcurves are a copy of the GINGA ASM lightcurves hosted at the DARTS archive at ISAS (<a href="https://darts.isas.jaxa.jp/astro/ginga/">https://darts.isas.jaxa.jp/astro/ginga/</a>). The plots in GIF format were generated by the HEASARC. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/gingabgd
- Title:
- GingaBackgroundLightcurves&Spectra
- Short Name:
- GINGABGD
- Date:
- 27 Sep 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The GINGABGD database table contains a summary of the contents of the Ginga pointed observations of (nominally empty) background fields. This table has been produced from the raw Ginga LAC First Reduction Files (FRFs), and contains information of the individual pointings in addition to FITS spectra and light curves, HDS and FITS data cubes and the plots produced during the pipeline processing. These products can be used with either the Ginga data analysis software or the <a href="/docs/xanadu/xanadu.html">XANADU software suite</a>. This archive (database and all the associated products) is a copy of the GINGABGD data products held at the Leicester Data Archive Service (<a href="http://ledas-www.star.le.ac.uk/">http://ledas-www.star.le.ac.uk/</a>). It was delivered to the HEASARC as part of archive exchange between data centers to facilitate the data transfer across the Atlantic. This is a service provided by NASA HEASARC .
7329. Ginga LAC Log
- ID:
- ivo://nasa.heasarc/gingalog
- Title:
- Ginga LAC Log
- Short Name:
- GINGA
- Date:
- 27 Sep 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The GINGALOG database table contains selected information from the Large Area Counter (LAC) aboard the third Japanese X-ray astronomy satellite Ginga. The Ginga experiment began on day 36, 5 February 1987 and ended in November 1991. Ginga consisted of the LAC, the all-sky monitor (ASM) and the gamma-ray burst detector (GBD). The satellite was in a circular orbit at 31 degree inclination with apogee 670 km and perigee 510 km, and with a period of 96 minutes. A Ginga observation consisted of varying numbers of major frames which had lengths of 4, 32, or 128 seconds, depending on the setting of the bitrate. Each GINGALOG database entry is the first record of a series of observations having the same values of "ACS MONITOR" (Attitude Control System). When this value changes, a new FITS file was written. The other Ginga catalog database, GINGAMODE is also a subset of the same LAC dump file used to create GINGALOG. GINGAMODE contains a listing whenever any of the following changes: "BITRATE", "LACMODE", "DISCRIMINATOR", or "ACS MONITOR". Thus, GINGAMODE monitors changes in several parameters and GINGALOG is a basic log of all the FITS files. Both databases point to the corresponding archived Flexible Image Transport System (FITS) files, but GINGAMODE may have more than one entry for a given FILE_LCURVE in the database. The user is invited to browse though the observations available from Ginga using GINGALOG or GINGAMODE, then extract the FITS files for more detailed analysis. The Ginga LAC Log Catalog was prepared from data sent to NASA/GSFC from the Institute of Space and Astronautical Science (ISAS) in Japan. This is a service provided by NASA HEASARC .
7330. Ginga LAC Mode Catalog
- ID:
- ivo://nasa.heasarc/gingamode
- Title:
- Ginga LAC Mode Catalog
- Short Name:
- GINGAMODE
- Date:
- 27 Sep 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The GINGAMODE database table contains selected information from the Large Area Counter (LAC) aboard the third Japanese X-ray astronomy satellite Ginga. The Ginga experiment began on day 36, 5 February 1987 and ended in November 1991. Ginga consisted of the LAC, the all-sky monitor (ASM) and the gamma-ray burst detector (GBD). The satellite was in a circular orbit at 31 degree inclination with apogee 670 km and perigee 510 km, and with a period of 96 minutes. A Ginga observation consisted of varying numbers of major frames which had lengths of 4, 32, or 128 seconds, depending on the setting of the bitrate. Each GINGAMODE database entry consists of data from the first record of a series of observations having the same values of the following: "BITRATE", "LACMODE", "DISCRIMINATOR", or "ACS MONITOR". When any of these changed, a new entry was written into GINGAMODE. The other Ginga catalog database, GINGALOG is also a subset of the same LAC dump file used to create GINGAMODE. GINGALOG contains a listing only whenever the "ACS monitor" (Attitude Control System) changes. Thus, GINGAMODE monitors changes in four parameters and GINGALOG is a basic log database mapping the individual FITS files. Ginga FITS files may have more than one entries in the GINGAMODE database. Both databases point to the same archived Flexible Image Transport System (FITS) files created from the LAC dump files. The user is invited to browse though the observations available from Ginga using GINGALOG or GINGAMODE, then extract the FITS files for more detailed analysis. The Ginga LAC Mode Catalog was prepared from data sent to NASA/GSFC from the Institute of Space and Astronautical Science (ISAS) in Japan. <p> Duplicate entries were removed from the HEASARC implementation of this catalog in June 2019. This is a service provided by NASA HEASARC .