CHARM2: An updated Catalog of High Angular Resolution Measurements
We present an update of the Catalog of High Angular ResolutionMeasurements (CHARM, Richichi & Percheron \cite{CHARM}, A&A,386, 492), which includes results available until July 2004. CHARM2 is acompilation of direct measurements by high angular resolution methods,as well as indirect estimates of stellar diameters. Its main goal is toprovide a reference list of sources which can be used for calibrationand verification observations with long-baseline optical and near-IRinterferometers. Single and binary stars are included, as are complexobjects from circumstellar shells to extragalactic sources. The presentupdate provides an increase of almost a factor of two over the previousedition. Additionally, it includes several corrections and improvements,as well as a cross-check with the valuable public release observationsof the ESO Very Large Telescope Interferometer (VLTI). A total of 8231entries for 3238 unique sources are now present in CHARM2. Thisrepresents an increase of a factor of 3.4 and 2.0, respectively, overthe contents of the previous version of CHARM.The catalog is only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/431/773
|
Video observation of meteors at Yunnan Observatory
In the last 20 years, with the development of the CCD and imageintensifiers, the use of small flexible video meteor observation systemshas gradually increased, with the prospect that one day videoobservation will replace the visual observation and ordinaryphotographic observations. In this paper we report on the research anddevelopment of the No.1 meteor-comet video camera system of YunnanObservatory and some preliminary observed results. The system consistsof 5 changeable modules; it has a 36° large-field camera dedicatedto the observation of meteors, with which a magnitude 6 star can berecorded on a single frame with an accuracy of about 0.2 mag. We alsopresent a comparison of the video camera system with the traditionalphotographic system, and outline the merits, possible improvements andfuture development of the video system.
|
The latitude and epoch for the formation of the southern Greek constellations
Not Available
|
Research Note Hipparcos photometry: The least variable stars
The data known as the Hipparcos Photometry obtained with the Hipparcossatellite have been investigated to find those stars which are leastvariable. Such stars are excellent candidates to serve as standards forphotometric systems. Their spectral types suggest in which parts of theHR diagrams stars are most constant. In some cases these values stronglyindicate that previous ground based studies claiming photometricvariability are incorrect or that the level of stellar activity haschanged. Table 2 is only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/367/297
|
Red supergiants in the LMC - III: luminous F and G stars
New BVRI observations for 40 and spectrophotometric measurements for 23F to G LMC supergiant candidates (and 3 galactic F to G supergiants) arepresented. The errors of the BVRI data are 0.01 to 0.03 mag in mostcases. The wavelength range of the spectra is 3400 to 6400 Angstroms,their resolution 10 Angstroms. The mean error of the fluxes is 0.03 mag.Spectral indices measuring the strengths of the Hβ , Hγ ,Hdelta , NaD and CaII H+K lines, the CHα_ {0} and CNbeta_ {0}bands, of the Balmer jump and the slope of the continuum redwards arediscussed as measures of effective temperature and luminosity on thebasis of galactic stars with accurate MK types and parallaxes. TheHγ line and the continuum gradient are very good temperaturecriteria, the CHα_ {0} band and especially the Balmer jump forluminosity. The luminosity classification given for F to G supergiantcandidates in the LMC in the literature is often doubtful. 5 of the 23stars observed spectrophotometrically turn out to be probably galacticforeground dwarfs on the basis both of the Balmer jump and thecomparison of their flux distributions with synthetic ones based on theKurucz model atmospheres. Surface gravities derived purely on the basisof flux distributions and such ones given by models of stellar evolutionagree with each other for dwarfs and giants only. For supergiants theformer are about 1.0 dex higher than the latter. As a consequenceeffective temperatures and metallicities given by these two methodsdeviate from each other for such stars, too. The intrinsic colours andtemperatures of galactic and LMC supergiants do not differ. Withabsolute magnitudes up to -9.6 mag the upper luminosity limit in the LMCdoes not exceed that in the Galaxy, where Ia-0 supergiants haveMV of up to -9.5 mag. The metallicities of the supergiantsshow a rather large scatter. Nevertheless the mean metallicities of 0.02+/- 0.09 dex for the Galaxy and -0.26 +/- 0.10 dex for the LMC agreewell with other observations.
|
The central depth of the Ca II triplet lines as a discriminant of chromospheric activity in late type stars
Not Available
|
The ROSAT all-sky survey catalogue of optically bright late-type giants and supergiants
We present X-ray data for all late-type (A, F, G, K, M) giants andsupergiants (luminosity classes I to III-IV) listed in the Bright StarCatalogue that have been detected in the ROSAT all-sky survey.Altogether, our catalogue contains 450 entries of X-ray emitting evolvedlate-type stars, which corresponds to an average detection rate of about11.7 percent. The selection of the sample stars, the data analysis, thecriteria for an accepted match between star and X-ray source, and thedetermination of X-ray fluxes are described. Catalogue only available atCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
|
The Tokyo PMC catalog 90-93: Catalog of positions of 6649 stars observed in 1990 through 1993 with Tokyo photoelectric meridian circle
The sixth annual catalog of the Tokyo Photoelectric Meridian Circle(PMC) is presented for 6649 stars which were observed at least two timesin January 1990 through March 1993. The mean positions of the starsobserved are given in the catalog at the corresponding mean epochs ofobservations of individual stars. The coordinates of the catalog arebased on the FK5 system, and referred to the equinox and equator ofJ2000.0. The mean local deviations of the observed positions from theFK5 catalog positions are constructed for the basic FK5 stars to comparewith those of the Tokyo PMC Catalog 89 and preliminary Hipparcos resultsof H30.
|
Quantitative spectral classification based on photoelectric spectrum scanner measurements of F-K stars.
New criteria of quantitative spectral classification have beenintroduced and the method of stepwise linear regression to thesecriteria for quantitative spectral classification of F-K stars has beenapplied to the Bochum photoelectric spectra.
|
Giants with infrared excess.
We have correlated optical and infrared catalogs in order to extract alarge sample of luminosity class III stars with known infrared fluxdensities. For a non-negligible fraction of G and K giants, afar-infrared excess emission was found, starting beyond 25μm. Anexplanation in terms of present-day mass loss thus becomes unlikely,since the dust should then be warmer and the excess emission less far inthe infrared. We believe that the far-infrared excesses of theseobjects, most likely first-ascent giants, are related to the Vegaphenomenon. The dusty disks around these stars, gradually cooled downduring their main-sequence phase, could be reheated once the star leavesthe main sequence and enters the luminous post-main-sequence phase. Thefairly large sample we constructed enables us to derive an estimationfor the occurrence of excesses. This fraction of G or K giants withfar-infrared excess appears to be distinctly smaller than amongmain-sequence stars. Since the higher radiation field of giants couldlead to a larger evaporation rate of the circumstellar debris, this factdoes not conflict with our hypothesis.
|
The Pulkovo Spectrophotometric Catalog of Bright Stars in the Range from 320 TO 1080 NM
A spectrophotometric catalog is presented, combining results of numerousobservations made by Pulkovo astronomers at different observing sites.The catalog consists of three parts: the first contains the data for 602stars in the spectral range of 320--735 nm with a resolution of 5 nm,the second one contains 285 stars in the spectral range of 500--1080 nmwith a resolution of 10 nm and the third one contains 278 stars combinedfrom the preceding catalogs in the spectral range of 320--1080 nm with aresolution of 10 nm. The data are presented in absolute energy unitsW/m(2) m, with a step of 2.5 nm and with an accuracy not lower than1.5--2.0%.
|
Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
|
The position corrections of 1400 stars observed with PA II in San Juan.
Not Available
|
Second astrolabe catalogue of Santiago.
Positions for 350 FK5 and 164 FK5 Extension stars as determined with theDanjon astrolabe of Santiago and differences astrolabe-catalogue aregiven for Equinox J2000.0 and for the mean observation epoch of eachstar. The average mean error in alpha is +/-0.005s and +/-0.07" indelta. The mean epoch of observation of the catalogue is J1979.96.
|
The CA II triplet lines in cool stars
Observations of the infrared triplet lines of ionized calcium arepresented for 91 stars brighter than m_v_=+7.0 in the spectral rangeF8-M4 of all luminosity classes and over a range of metallicities [Fe/H]from -0.65 to +0.60. The above spectra have been obtained at a spectralresolution of 0.4 A with a coude echelle spectrograph using the ThomsonCCD as the detector. This study has been undertaken primarily toinvestigate the dependence of the Ca II triplet strengths over the broadrange of atmospheric parameters like luminosity, temperature andmetallicity. The Ca II triplet lines are a powerful diagnostic of thestellar populations in galaxies because of their sensitivity to theabove parameters. Our detailed analysis indicates a strong correlationbetween the equivalent width of the Ca II triplet lines and surfacegravity, much stronger in metal rich stars than in metal poor stars. TheCa II equivalent widths are fairly insensitive to temperature over therange of luminosity covered. However, they are found to be quitesensitive to metallicity, more conspicuously in supergiants than ingiants and dwarfs. Observations are compared with recent theoreticalcalculations of these lines in NLTE atmospheres.
|
Improved Mean Positions and Proper Motions for the 995 FK4 Sup Stars not Included in the FK5 Extension
Not Available
|
CCD observations of the H-alpha line in late G and K supergiants and their interpretation
CCD echelle spectra of the H-alpha line at 6563 A have been obtained fora sample of 30 G and K supergiants with a spectral resolution of about0.24 A. The data clearly indicate that the observed H-alpha profile is adeep absorption, implying large optical depths in the chromosphere.Also, the line cores are blueshifted in all the stars which suggests thechromospheres are expanding outward. Detailed radiative transfercalculations of H-alpha have been carried out in a spherically symmetricatmosphere with outward-positive velocity and temperature gradients,including explicitly the effects of ionization. The H-alpha lineprofiles have been computed for a wide range of parameters in order toreproduce the observed features of the line. Within the framework of ourmodel, the calculations reinforce the idea that the nonthermalvelocities have to be as large as 25-30 km/s to explain the large widthsof the observed profiles. The rates of mass outflow have been calculatedto lie in the range 10 exp -8 to 10 exp -9 solar mass/yr.
|
SAO stars with infrared excess in the IRAS Point Source Catalog
We have undertaken a search for SAO stars with infrared excess in theIRAS Point Source Catalog. In contrast to previous searches, the entireIRAS (12)-(25)-(60) color-color diagram was used. This selection yieldeda sample of 462 stars, of which a significant number are stars withcircumstellar material. The stars selected can be identified aspre-main-sequence stars, Be stars, protoplanetary systems, post-AGBstars, etc. A number of objects are (visual) binary stars.Characteristic temperatures and IR excesses are calculated and theirrelations to spectral type are investigated.
|
The calibration of the Stromgren photometric system for A, F and early G supergiants. I - The observational data
An empirical calibration of the Stromgren uvby-beta photometric systemfor the A, F, and early G supergiants is being derived. This paperexplains the observational program and the photometric reductiontechniques used and presents a catalog of new Stromgren photometry forover 600 A, F, and G supergiants.
|
Large and kinematically unbiased samples of G- and K-type stars. II - Observations of evolved stars in the Bright Star sample. III - Evolved young disk stars in the Bright Star sample
Four color and RI observations were obtained for a large sample ofG-type and K-type stars in the Bright Star Catalogue. Data are firstpresented for 110 evolved stars. Photometry of evolved young diskpopulation stars have then been calibrated for luminosity, reddening,and metallicity on the basis of results for members of the Hyades andSirius superclusters. New DDO results are given for 120 stars.
|
Stellar integrated fluxes in the wavelength range 380 NM - 900 NM derived from Johnson 13-colour photometry
Petford et al. (1988) have reported measured integrated fluxes for 216stars with a wide spread of spectral type and luminosity, and mentionedthat a cubic-spline integration over the relevant Johnson 13-colormagnitudes, converted to fluxes using Johnson's calibration, is inexcellent agreement with those measurements. In this paper a list of thefluxes derived in this way, corrected for a small dependence on B-V, isgiven for all the 1215 stars in Johnson's 1975 catalog with completeentries.
|
Absolute flux calibration of the H and K lines of CA II - Chromospheric radiative losses in F and G-type stars
Ca II H and K spectra of 81 (mainly Southern) F and G stars are analyzedusing two different calibration methods. It is shown that, for spectraof sufficiently high resolution, and for stars of relatively lowrotation rates, the calibrations of Linsky et al. (1979) and of Pasquiniet al. (1988) give essentially the same results. These calibrations areused to derive absolute surface fluxes in the H and K lines of Ca II for64 stars. It is shown that several late-F and early-G giants andsupergiants have Ca II H and K fluxes in excess of about 10 to the 6therg/sq cm s, much larger than those typically observed for normal giantsof later spectral types.
|
Spectrophotometry of bright F-, G-, K- and M-type stars. I - Measurements of 60 southern and equatorial stars
Spectral energy distributions were photoelectrically measured from 320nm to 860 nm with a resolution of 1 nm in equidistant steps of 1 nm for60 bright southern and equatorial stars of intermediate and latespectral types for all luminosity classes. Flux curves for individualstars are plotted with a resolution of 1 nm and tabulated in steps of 5nm. Typical internal mean errors of fluxes measured in different nightsare less than 0.02 mag in the spectral range from 400 nm to 860 nm, andrise to a maximum of about 0.05 mag for wavelengths below 400 nm.
|
Catalogue of the energy distribution data in spectra of stars in the uniform spectrophotometric system.
Not Available
|
Observations of emission from certain stars at millimeter wavelengths
The paper presents results of observations of five alpha(2) CVn-typestars, five emission-line stars, the object SS 433, and four possiblerelated objects at 13.5 and 8.15 mm. It is confirmed that stars ofalpha(2) CVn-type are not characterized by significant radio emission.Emission variations from the emission-line star MWC 349 were detectedthat could be caused by optical luminosity variations of the star.Observations of SS 433 do not exclude the presence of an extendedenvelope around this object with dimensions and mass close to those ofthe envelope around MWC 349. It is also found that 2013 + 370 could beclassified as a BL Lac object.
|
A determination of the effective temperatures, accelerations of gravity, and metallicity parameters of late-type stars from data on energy distribution in their spectra
The effective temperatures and surface gravities are determined for 297F-M stars for which detailed spectrum energy distribution curves areavailable. For some of the stars, the Fe/H ratio is estimated. Theaccuracy of the values obtained is found to be comparable to that of theestimates based on narrow-band photometry.
|
Atmospheric extinction in the /U-B/ color index
Various methods for obtaining the atmospheric extinction in the (U-B)color index taking into account the dependence of extinction coefficienton the intrinsic color index of the star are examined. Numericalintegrations are performed to determine synthetic color indices for 32stars of spectral classes O9 to M0 and luminosity classes I, III and Vthrough 0, 1 and 2 air masses, resulting in three (u-b) color indicesfor each star. Photometric reduction of the color indices to the (U-B)color index was then performed by the classical method, by the methodproposed by Gutierrez-Moreno et al. (1966) and various modifications ofit, and by the method proposed by Moffat and Vogt (1977). Comparisonwith observations of 71 stars in the standard region E5, nine extinctionstandard stars and 25 Johnson standard stars in the UBV reveals that thereduction of (U-B) by the classical method gives internal errors betweentwo and three times larger than those obtained for (B-V) and V, whilethe methods of Gutierrez-Moreno et al. and Moffat and Vogt providegreatly improved accuracy.
|
Catalogue of stars with CaII H and K emissions
Not Available
|
Luminosity and velocity distributions of high-luminosity red stars. IV. The G-type giants
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974PASP...86..129E&db_key=AST
|
Ca II K emission in southern late-type stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969MNRAS.144..333W&db_key=AST
|
INHABITED SKY
