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| Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
| 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
| The proper motions of fundamental stars. I. 1535 stars from the Basic FK5
A direct combination of the positions given in the HIPPARCOS cataloguewith astrometric ground-based catalogues having epochs later than 1939allows us to obtain new proper motions for the 1535 stars of the BasicFK5. The results are presented as the catalogue Proper Motions ofFundamental Stars (PMFS), Part I. The median precision of the propermotions is 0.5 mas/year for mu alpha cos delta and 0.7mas/year for mu delta . The non-linear motions of thephotocentres of a few hundred astrometric binaries are separated intotheir linear and elliptic motions. Since the PMFS proper motions do notinclude the information given by the proper motions from othercatalogues (HIPPARCOS, FK5, FK6, etc.) this catalogue can be used as anindependent source of the proper motions of the fundamental stars.Catalogue (Table 3) is only available at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strastg.fr/cgi-bin/qcat?J/A+A/365/222
| Determination of the temperatures of selected ISO flux calibration stars using the Infrared Flux Method
Effective temperatures for 420 stars with spectral types between A0 andK3, and luminosity classes between II and V, selected for a fluxcalibration of the Infrared Space Observatory, ISO, have been determinedusing the Infrared Flux Method (IRFM). The determinations are based onnarrow and wide band photometric data obtained for this purpose, andtake into account previously published narrow-band measures oftemperature. Regression coefficients are given for relations between thedetermined temperatures and the photometric parameters (B2-V1), (b-y)and (B-V), corrected for interstellar extinction through use ofHipparcos parallaxes. A correction for the effect of metallicity on thedetermination of integrated flux is proposed. The importance of aknowledge of metallicity in the representation of derived temperaturesfor Class V, IV and III stars by empirical functions is discussed andformulae given. An estimate is given for the probable error of eachtemperature determination. Based on data from the ESA HipparcosAstrometry Satellite.
| Towards a fundamental calibration of stellar parameters of A, F, G, K dwarfs and giants
I report on the implementation of the empirical surface brightnesstechnique using the near-infrared Johnson broadband { (V-K)} colour assuitable sampling observable aimed at providing accurate effectivetemperatures of 537 dwarfs and giants of A-F-G-K spectral-type selectedfor a flux calibration of the Infrared Space Observatory (ISO). Thesurface brightness-colour correlation is carefully calibrated using aset of high-precision angular diameters measured by moderninterferometry techniques. The stellar sizes predicted by thiscorrelation are then combined with the bolometric flux measurementsavailable for a subset of 327 ISO standard stars in order to determineone-dimensional { (T, V-K)} temperature scales of dwarfs and giants. Theresulting very tight relationships show an intrinsic scatter induced byobservational photometry and bolometric flux measurements well below thetarget accuracy of +/- 1 % required for temperature determinations ofthe ISO standards. Major improvements related to the actual directcalibration are the high-precision broadband { K} magnitudes obtainedfor this purpose and the use of Hipparcos parallaxes for dereddeningphotometric data. The temperature scale of F-G-K dwarfs shows thesmallest random errors closely consistent with those affecting theobservational photometry alone, indicating a negligible contributionfrom the component due to the bolometric flux measurements despite thewide range in metallicity for these stars. A more detailed analysisusing a subset of selected dwarfs with large metallicity gradientsstrongly supports the actual bolometric fluxes as being practicallyunaffected by the metallicity of field stars, in contrast with recentresults claiming somewhat significant effects. The temperature scale ofF-G-K giants is affected by random errors much larger than those ofdwarfs, indicating that most of the relevant component of the scattercomes from the bolometric flux measurements. Since the giants have smallmetallicities, only gravity effects become likely responsible for theincreased level of scatter. The empirical stellar temperatures withsmall model-dependent corrections are compared with the semiempiricaldata by the Infrared Flux Method (IRFM) using the large sample of 327comparison stars. One major achievement is that all empirical andsemiempirical temperature estimates of F-G-K giants and dwarfs are foundto be closely consistent between each other to within +/- 1 %. However,there is also evidence for somewhat significant differential effects.These include an average systematic shift of (2.33 +/- 0.13) % affectingthe A-type stars, the semiempirical estimates being too low by thisamount, and an additional component of scatter as significant as +/- 1 %affecting all the comparison stars. The systematic effect confirms theresults from other investigations and indicates that previousdiscrepancies in applying the IRFM to A-type stars are not yet removedby using new LTE line-blanketed model atmospheres along with the updatedabsolute flux calibration, whereas the additional random component isfound to disappear in a broadband version of the IRFM using an infraredreference flux derived from wide rather than narrow band photometricdata. Table 1 and 2 are only available in the electronic form of thispaper
| Molecular hydrogen in the central regions of southern infrared galaxies
An extensive set of molecular hydrogen observations of centers ofsouthern infrared galaxies is presented. Our data are combined withpublished infrared and radio observations to investigate therelationship between nuclear and circumnuclear activity. We convert theobservational data to absolute luminosities, by applying the knowndistances. The resulting dataset covers several decades in luminosityfor the various parameters, which observe fairly tight correlations. Theparameters of our (power law) fits are, at the level of accuracyachieved, not dependent on the type of nuclear activity: while thedataset comprises a mixture of alleged Seyfert, Liner & starburstgalaxies, single fits match the complete sample well enough. Inparticular, non-thermal nuclei (AGN) present in some of the galaxies inthe current sample, do not stand out in the parameters we investigated.The absence of a significant dependence on the nuclear type isconsistent with the idea that the ever present starbursts energeticallydominate a possible `AGN in a dusty environment'-component in mostgalaxy nuclei with infrared excesses. The size of the H_2 emittingregion is found to be proportional to the square root of the 21 cm radiocontinuum luminosity. The excitation of the circumnuclear H_2 isdominated by shocks. If the H_2 extent marks the size of an inner cavityin the dense molecular material surrounding a galaxy nucleus and theradio luminosity is proportional to the mechanical luminosity of(circum)nuclear winds. This result then indicates that the cavity sizeoccurs at constant pressure in the sample galaxies, in accordance withthe superwind model by Heckman et al. (1990) [ApJS, 74, 833]. Ourresults, together with those obtained by others, thus suggest thatluminosities and size scales of excited gas associated with activenuclei are dominated by the mechanical energy input. Given thedifficulties of uniquely establishing the presence of an AGN, we cannotexclude that (a large fraction of the) infrared luminous galaxiesprocure part of their radiated energy through accretion onto a massivedark object.
| ROSAT X-ray observations of a complete, volume-limited sample of late-type giants.
We have investigated a complete sample of the nearest 39 late typegiants (d<=25pc) for which we have probed the X-ray luminosityfunction with unprecedented sensitivity by deep (3...18ksec) ROSATPSPC-observations in the pointed mode, together with ROSAT All-Skysurvey (RASS) data. We confirm the X-ray dividing line for luminosityclass III giants as proposed by Haisch et al. (1991, 1992) and we findevidence, that essentially all luminosity class III giants withB-V<1.2 or spectral type
| 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
| Evolved GK stars near the Sun. 2: The young disk population
From a sample of nearly 2000 GK giants a group of young disk stars withwell determined space motions has been selected. The zero point of theluminosity calibrations, both from the ultraviolet flux (modifiedStroemgren system) and that in the region of 4200 to 4900 A (DDOsystem), show a discontinuity of about a half magnitude at the border ofthe young disk and old disk domains. The population separation is basedon the space velocity components, which are also an age discriminant,with the population interface near 2 x 109 yr, based onmodels with convective overshoot at the core. This age corresponds togiant masses near 1.7 solar mass, near the critical mass separating theyoung stars that do not burn helium in degenerate cores from older starsthat do. Ten percent of both populations show CN anomalies in that thederived value of P(Fe/H) from CN (Cm) and fromFe(M1) differ by more than 0.1 dex and the weak and strong CNstars occur equally in the old disk but the weak CN stars predominate inthe young disk. Peculiar stars, where flux distortions affect theluminosity calibrations, are of the CH+(Ba II) and CH-(weak G band)variety and represent less than 1% of the stars in both populations. Theyoung disk giants are restricted to ages greater than about109 yr, because younger stars are bright giants orsupergiants (luminosity class 2 or 1), and younger than about 2 x109 yr, because the old disk-young disk boundary occurs near1.7 solar mass. The distribution of heavy element abundances, P(Fe/H),for young disk giants is both more limited in range (+/- 0.4 dex) and isskewed toward higher abundances, compared with the nearly normaldistribution for old disk giants. The distribution of (U,V) velocityvectors gives (U,V,W) and their dispersions = (+17.6 +/- 18.4, -14.8 +/-8.4, -6.9 +/- 13.0) and (+3.6 +/- 38.4, -20.7 +/- 27.5, -6.7 +/-17.3)km/s for young and old disk giants, respectively.
| Molecules in the starburst galaxy Henize 2-10
The starburst dwarf galaxy He 2-10 has been partially mapped in the H2(1-0) S1 line, and in the (12)CO 3 to 2, 2 to 1 and 1 to 0 transitions.The (13)CO lines for these transitions have also been measured at thecenter position. The observations show that the H2 line is most likelyshock excited, while the CO measurements indicate the presence of bothcold (Tex less than 10 K) and hot (Tex greaterthan 50 K) molecular gas. The hot molecular gas must be optically thinin all three (12)CO transitions, and have a ((12)CO)/((13)CO) isotopicabundance ratio of about 30. The cold J = 1-0 emission is eitheroptically thin with a similar isotopic abundance ratio, or opticallythick with an anomalously high ((12)CO)/((13)CO) ratio greater than 100.Estimates for the total molecular gas mass and the dust mass are derivedand compared with those of NGC 1569 and IIZw40. The starburst processappears to proceed in a similar manner in all three galaxies.
| Evolved GK stars near the sun. I - The old disk population
A sample of nearly two thousand GK giants with intermediate band, (R,I),DDO and Geneva photometry has been assembled. Astrometric data is alsoavailable for most of the stars. The some 800 members of the old diskpopulation in the sample yield accurate luminosities (from two sources),reddening values and chemical abundances from calibrations of thephotometric parameters. Less than one percent of the objects arepeculiar in the sense that the flux distribution is abnormal. Thepeculiarity is signaled by strong CH (and Ba II) and weak CH. The CH+stars are all spectroscopic binaries, probably with white dwarfcompanions, whereas the CH- stars are not. A broad absorption band,centered near 3500 A, is found in the CH+ stars whereas the CH- objectshave a broad emission feature in the same region. The intensity of theseabsorptions and emissions are independent of the intensity of abnormalspectral features. Ten percent of the old disk sample have a heavyelement abundance from one and a half to three times the solar value.The distribution of the heavy element abundances is nearly a normal onewith a peak near solar abundance and ranges three times to one sixthsolar. The distribution of the (U, V) velocities is independent of theheavy element abundance and does not appear to be random. Ten percent ofthe old disk stars show a CN anomaly, equally divided between CN strongand CN weak. Several stars of individual astrometric or astrophysicalimportance are isolated.
| Optical Polarization of 1000 Stars Within 50-PARSECS from the Sun
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&AS..101..551L&db_key=AST
| JHKLM standard stars in the ESO system
A list of 199 standard stars suitable for the ESO standard photometricsystem at JHKLM is given. Faint stars (although brighter than K = 7.7)to be used on larger telescopes are included. This list is based on ananalysis of all infrared photometric observations carried out at LaSilla from 1979 until 1989 inclusive. The accuracy of the data (about0.02 mag. at J, H, K, L, and M) is similar to the one achieved at SAAOand CTIO. Comparisons with these systems, as well as with the AAO andMSSO systems, are made: it is shown that the ESO system is very close tothe other ones, with the exception of CTIOs.
| Radiatively and shock excited H2 in Magellanic H II regions
Various H2 transitions were observed in five objects in the SMC in orderto identify the H2 excitation mechanism. Observed line ratios indicatethat N83B and N81 are radiatively excited. The remaining objects eithercontain a shock-excited H2 component or have densities sufficiently highthat collisional de-excitation influences observed line ratios. In bothcases, radiative excitation is the energetically dominant mechanism inall objects. For the observed H2 clouds, volume densities of200-10,000/cu cm are derived, with a mean of 5000/cu cm. If significantsubparsec clumping occurs, densities may be higher. Limits on shockcontributions to the observed H2 emission suggest shock velocities lessthan 10 km/s (J-type shocks) or less than 15-23 km/s (C-type shocks). Itis inferred from this that early-type stars in the observed objects havestellar winds weaker than Galactic O-type stars. The strength of theobserved near-IR He I transitions is briefly discussed.
| Physical data of the fundamental stars.
Not Available
| Einstein Observatory magnitude-limited X-ray survey of late-type giant and supergiant stars
Results are presented of an extensive X-ray survey of 380 giant andsupergiant stars of spectral types from F to M, carried out with theEinstein Observatory. It was found that the observed F giants orsubgiants (slightly evolved stars with a mass M less than about 2 solarmasses) are X-ray emitters at the same level of main-sequence stars ofsimilar spectral type. The G giants show a range of emissions more than3 orders of magnitude wide; some single G giants exist with X-rayluminosities comparable to RS CVn systems, while some nearby large Ggiants have upper limits on the X-ray emission below typical solarvalues. The K giants have an observed X-ray emission level significantlylower than F and F giants. None of the 29 M giants were detected, exceptfor one spectroscopic binary.
| Polycyclic aromatic hydrocarbons in the near-infrared spectra of 24 IRAS sources
Infrared spectra of 24 IRAS sources are presented. The observationsinclude the IRAS Low Resolution Spectra (LRS) and ground-basedthree-micron spectrophotometry. These sources were selected from theIRAS-LRS database because they have strong emission features at 7.7,8.6, and 11.3 micron in their LRS spectra. In all of them, thewell-known 3.3-micron emission feature is detected which sometimesoccurs together with a feature at 3.4 microns and/or an emission plateauat 3.4-3.6 microns. These observations are analyzed in the context ofthe polycyclic aromatic hydrocarbons (PAHs) hypothesis. The rather largesample of sources observed and the homogeneity of the data presentedmade it possible to perform a consistent analysis. In particular, theintensity ratio of the 11.3-micron to the 3.3-micron bands is studied,which is used to derive an average size of the emitting molecules. Theemission of a cooling molecule is calculated in the various bands of PAHmolecules measured in the laboratory. Discrepancies between thecalculated and the observed spectra are tentatively interpreted in termsof dehydrogenation of the molecules.
| The distribution of OB stars and dust in a Milky Way field at (l,b) = (335 deg, 0 deg)
New photoelectric UBV photometry for 103 stars and MK spectroscopy for110 stars in a 21 sq-deg field at (l,b) = (335 deg, 0 deg) are studied,in addition to previous data for stars in this field. Most of the 112 OBstars considered may be separated into three groups associated with thespiral structure of the inner galaxy: one at 1.34 + or - 0.05 kpc, oneat 2.41 + or - 0.08 kpc, and one at 3.69 + or - 0.23 kpc. The remaining21 stars lie along the line-of-sight, with some possibly being asdistant as 9 kpc. The dust is found to be distributed in two distinctclouds, one in the local arm at 190 + or - 30 pc and the other in aninterarm cloud of variable extinction at 690 + or - 70 pc.
| Trigonometric parallax results for southern luminosity class III stars
New trigonometric parallaxes are reported for ten bright, southernlate-type MK giants ranging in spectral type from K0 to M3.5. The listincludes HR 794, 1247, 2245, 2773, 3518, 3803, 5287, 5603, 6832, and6913. The modern parallaxes are compared with earlier results, and theluminosity calibration for these stars is discussed. A list of giants ispresented containing the best prospects for future parallax work onlate-type MK giants.
| NGC 2423 and the red giants of the Hyades supercluster
An extensive set of photometric data for members of the cluster NGC 2423is examined, and the results are compared with those for red giantmembers of the Hyades supercluster. Intermediate band and RI or H-betaobservations for 34 stars of the cluster are listed, and photometricparameters for A and F stars in the cluster are shown. Parameters arealso depicted for red giants in the Hyades supercluster, red giants ofHyades abundance, and M type variables in the Hyades supercluster. Theintrinsic (b-y), M(1) and (R-I),(b-y) relations for normal giants withHyades metal abundance are presented. NGC 2423 is shown to be verysimilar to the Hyades with red giants that match the luminosity andtemperature distribution of those in the Hyades. The red giants of theHyades which are within about 200 pc of the sun are found to haveparallel (U,V) motions with the main sequence stars of the Hyadesnuclear cluster.
| The first astrolabe catalogue at Valinhos
Individual corrections to the ascensions and declinations of 199 starsof the FK4 and FK4 Supplement, derived from the Danjon astrolabeobservations at Valinhos and covering the zone from +5 to -51 deg ofdeclination, are presented. The chain method of differences was used tomake the corrections. The observational station formulas used to obtainthe catalogue are cited and discussed and the systematic errors for thezone of the catalogue are given. The results are compared with those ofthe General Catalogue of Astrolabes.
| First astrolabe catalogue of Rio de Janeiro
A catalogue of right ascensions and declinations of FK4 and FK4Supplement stars, obtained from astrolabe observations at Rio deJaneiro, is presented. The quantity and accuracy of the observations,the systematic errors of the catalogue, the group corrections, and theascension and declination corrections are considered.
| Near infrared photometry. I - Homogenization of near-infrared data from southern bright stars
A single homogeneous data set containing near-infrared (JHKLM)photometry of bright stars in the Southern Hemisphere obtained fromdifferent sources is constructed based on the use of the Johnson systemas a standard. Data for 203 stars in the J, H, K and L bands and 87stars in the M band from the lists of Glass (1974), Engels et al.(1981), Wamsteker (1981) and Allen (1981, 1982) was combined bycomparison with the list of Johnson, followed by transformation into theJohnson J and K bands, the H band of Glass and Allen, an L band similarto that of Johnson but having the zero point of Glass, and the M band ofEngels. Average colors and spectral types are also obtained. The presentlist may be used to provide calibration objects in the range 1.2 to 5microns covering a wide range in color and brightness.
| Near-infrared observations of trapezium-type multiple systems Catalogue of observations and a new determination of the reddening law
Results are presented from a large scale near-infrared survey of smallsky areas of the Milky Way containing trapezium-type multiple starsystems located within young galactic clusters, H II regions or darknebulosities. Photometric maps at wavelength 2.2 microns complemented bybroadband JHKL photometry of the majority of the sources detected and ofthe star members of the systems were obtained. A number of randomlychosen comparison regions along the galactic plane were also mapped andthe results were also used, with recent semi-empirical models, todetermine the number of field stars expected for the program surveys.Analyses of the infrared two-color diagrams provide determinations ofthe values of the color excess ratios E(J-H)/E(H-K), E(H-K)/E(K-L) andE(J-K)/E(K-L). The resulting reddening law is found to differsignificantly from that in the direction of the Ophiuchus and Taurusdark clouds and possibly towards the Galactic Center.
| Infrared Observations of Southern Bright Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1981A&AS...45....5E&db_key=AST
| Catalogue of stars with CaII H and K emissions
Not Available
| Catalogue general des etoiles observees a l'astrolabe (1957-1975), corrections individuelles aux positions DU FK4.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1978A&AS...31..159B&db_key=AST
| Intermediate band photometry of late-type stars. II - Some stellar groups
Observations on the (R, I) system and a modified Stromgren system ofmembers of six stellar groups are used to demonstrate the chemicalhomogeneity of some 70% or 80% of the members assigned to the groups onthe basis of kinematics. The groups discussed are the Hyades, Wolf 630,Arcturus, Groombridge 1830, and Kapteyn's Star Groups as well as ananonymous group of a half dozen subdwarfs with (U, V) near (-150, -320)km/s. Standards for a previously described photometric system areextended, and additional F- and G-type standards for the (R, I) systemare presented. A simple relation is derived for computing the Fe/Habundance ratio for most stars in the corrected (R-I) interval from +0.2to +0.45 magnitude.
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| Takýmyýldýz: | Cetvel |
| Sað Açýklýk: | 16h19m50.40s |
| Yükselim: | -50°09'20.0" |
| Görünürdeki Parlaklýk: | 4.019 |
| Uzaklýk: | 39.093 parsek |
| özdevim Sað Açýklýk: | -158.4 |
| özdevim Yükselim: | -53.7 |
| B-T magnitude: | 5.388 |
| V-T magnitude: | 4.122 |
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