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
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An IUE Atlas of Pre-Main-Sequence Stars. I. Co-added Final Archive Spectra from the SWP Camera
We have identified 50 T Tauri stars (TTS) and 74 Herbig Ae/Be (HAEBE)stars observed in the IUE short-wavelength bandpass (1150-1980 Å).Each low-resolution (R~6 Å) spectrum was visually inspected forsource contamination and data quality, and then all good spectra werecombined to form a single time-averaged spectrum for each star. Use ofIUE Final Archive spectra processed with NEWSIPS reduces fixed patternnoise in individual spectra, allowing significant signal-to-noise ratiogains in our co-added spectra. For the TTS observed by IUE, we measuredfluxes and uncertainties for 17 spectral features, including twocontinuum windows and four fluoresced H2 complexes. Thirteenof the 32 accreting TTS observed by IUE have detectable H2emission, which until now had been reported only for T Tau. Using anempirical correlation between H2 and C IV line flux, we showthat lack of sensitivity can account for practically all nondetections,suggesting that H2 fluorescence may be intrinsically strongin all accreting TTS systems. Comparison of IUE and GHRS spectra of TTau show extended emission primarily, but not exclusively, in lines ofH2. We also fit reddened main-sequence templates to 72 HAEBEstars, determining extinction and checking spectral types. Several ofthe HAEBE stars could not be fitted well or yielded implausibly lowextinctions, suggesting the presence of a minority emission componenthotter than the stellar photosphere, perhaps caused by white dwarfcompanions or heating in accretion shocks. We identified broadwavelength intervals in the far-UV that contain circumstellar absorptionfeatures ubiquitous in B5-A4 HAEBE stars, declining in prominence forearlier spectral types, perhaps caused by increasing ionization of metalresonance lines. For 61 HAEBE stars, we measured or set upper limits ona depth index that characterizes the strength of circumstellarabsorption and compared this depth index with published IR properties.
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High S/N Echelle spectroscopy in young stellar groups. II. Rotational velocities of early-type stars in SCO OB2.
We investigate the rotational velocities of early-type stars in the ScoOB2 association. We measure v.sin(i) for 156 established and probablemembers of the association. The measurements are performed with threedifferent techniques, which are in increasing order of expectedv.sin(i): 1) converting the widths of spectral lines directly tov.sin(i), 2) comparing artificially broadened spectra of low v.sin(i)stars to the target spectrum, 3) comparing the HeI λ4026 lineprofile to theoretical models. The sample is extended with literaturedata for 47 established members of Sco OB2. Analysis of the v.sin(i)distributions shows that there are no significant differences betweenthe subgroups of Sco OB2. We find that members of the binary populationof Sco OB2 on the whole rotate more slowly than the single stars. Inaddition, we find that the B7-B9 single star members rotatesignificantly faster than their B0-B6 counterparts. We test varioushypotheses for the distribution of v.sin(i) in the association. Theresults show that we cannot clearly exclude any form of randomdistribution of the direction and/or magnitude of the intrinsicrotational velocity vector. We also investigate the effects of rotationon colours in the Walraven photometric system. We show that positions ofB7-B9 single dwarfs above the main sequence are a consequence ofrotation. This establishes the influence of rotation on the Walravencolours, due primarily to surface gravity effects.
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Incidence of X-ray sources among magnetic chemically peculiar stars
Cash & Snow (1982) and Golub et al. (1983) have detected X-rayemission from 3 out of 7 observed magnetic chemically peculiar (CP)stars. Although the incidence of X-ray sources apparently is very high,these authors concluded that such emission is not unquestionable becauseof the presence of a companion. To determine the incidence of X-raysources among hot CP stars, I have checked the list of B-type starsmeasured by Grillo et al. (1992) selecting 90 stars. Of the 4 magneticCP stars showing X-ray emission 3 are members of a binary system. Thusit appears that detectable X-ray emission from magnetic CP stars is notvery common and still questionable. To find out whether HD 37017presents X-ray emission (Drake et al. 1987) or not (Grillo et al. 1992),I have analyzed an HRI frame from the ROSAT satellite finding noevidence for X-ray emission at this star's position.
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Investigation of the stellar population of dark clouds associated with Rho OPH
Results of UBVR photoelectric photometry for 32 stars in Rho Oph darkclouds (RSF 1 Oph) are presented. Mean magnitudes and colors aredetermined on the basis of 30-70 observations of 12 known variables inthis region. The H-R diagram of the Rho Oph star aggregate is discussed.The main sequence dwarfs are present on the H-R diagram up to +8 m. Themain sequence extension of 1 Oph is a least 11 mag. The RSF 1 Ophluminosity function is discussed and a deficit of stars in the range of+2 m to +5 m is found.
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A homogeneous catalog of new UBV and H-beta photometry of B- and A-type stars in and around the Scorpius-Centaurus OB association
B- and A-type stars in and near the Sco-Cen OB association areinvestigated with UBV and H-beta photometry to acquire data relevant tothe luminosity function of Sco-Cen. The measurements generally consistof two 10-s integrations of U, B, V, (W, N) filters, and theobservations are corrected iteratively for atmospheric extinction andinstrumental response. The data presented give the mean V magnitude,mean B-V, mean U-B, and the estimated uncertainties for these values.The catalog provides a homogeneous catalog of data for a large fieldwith stellar objects delineating membership to the association Sco-Cenand that affect the luminosity function of the aggregate.
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An Einstein Observatory SAO-based catalog of B-type stars
About 4000 X-ray images obtained with the Einstein Observatory are usedto measure the 0.16-4.0 keV emission from 1545 B-type SAO stars fallingin the about 10 percent of the sky surveyed with the IPC. Seventy-fourdetected X-ray sources with B-type stars are identified, and it isestimated that no more than 15 can be misidentified. Upper limits to theX-ray emission of the remaining stars are presented. In addition tosummarizing the X-ray measurements and giving other relevant opticaldata, the present extensive catalog discusses the reduction process andanalyzes selection effects associated with both SAO catalog completenessand IPC target selection procedures. It is concluded that X-rayemission, at the level of Lx not less than 10 exp 30 ergs/s, is quitecommon in B stars of early spectral types (B0-B3), regardless ofluminosity class, but that emission, at the same level, becomes lesscommon, or nonexistent, in later B-type stars.
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Catalogue of Hydrogen Line Spectral Profiles of 236 B-Stars A-Stars and F-Stars
Not Available
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Walraven photometry of nearby southern OB associations
Homogeneous Walraven (VBLUW) photometry is presented for 5260 stars inthe regions of five nearby southern OB associations: Scorpio Centaurus(Sco OB2), Orion OB1, Canis Major OB1, Monoceros OB1, and Scutum OB2.Derived V and (B - V) in the Johnson system are included.
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The spectral energy distribution of early-type stars. II - The extinction law towards O-type stars
Photometric measurements through different pass-bands are used todetermine the color-excess E(B-V) for O-type stars in the UV and IRspectral regions. The results are used to examine the extinctioncharacter of the stars. It is found that, in the UV, each O-type starhas its own extinction character. In general, the visual and NIRextinction in the direction of O-type stars are normal.
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Physical parameters of stars in the Scorpio-Centaurus OB association
Walraven photometry is presented of established and probable members ofthe Scorpio-Centaurus OB association. For each star, effectivetemperature and surface gravity are derived using Kurucz (1979)atmosphere models. From the Straizys and Kuriliene (1981) tables,absolute magnitudes are calculated. Distance moduli and visualextinctions are determined for all stars. From a comparison of theHR-diagrams of the stars in each subgroup with theoretical isochrones,the ages of the three subgroups are derived. The distances to the threesubgroups are shown to be different; there is a general trend (alsowithin each subgroup) for the distances to be larger at higher galacticlongitudes. The visual extinction in the youngest subgroupUpper-Scorpius, is well correlated with the IRAS 100-micron map. Thedistance toward the Ophiuchus dark clouds is found to be 125 pc, basedon the photometric distances to the stars. Most of the early-type starsin Upper-Scorpius are located at the far side of the dark clouds.
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The velocity field of the outer Galaxy in the southern hemisphere. III - Determination of distances to O, B, and A type stars in the Walraven photometric system
The Walraven photometric system has been used to derive distances tostars of spectral types earlier than A7. The details of the observingprocedure are given, and the way the data were analyzed is described.The accuracy of the data is discussed, and the results are compared withthose of Gathier et al. (1986). The observational results for stars ineight well-studied star cluster are presented, compared with theliterature, and discussed.
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Stellar multiplicity in the Scorpius-Centaurus association
Radial velocities are determined for 81 members of the Sco-Cenassociation in order to discover the radial velocity variables. Thefirst orbits are computed for 10 systems, along with improved orbitalelements for another seven systems, using published observations in bothcases. The axial rotation of the association members is used to testwhether both subgroups identified in the association follow the proposedcorrelation between percentage of binaries and axial rotation. Theperiod distribution is studied using all the information available onbinary systems (spectroscopic binaries, visual binaries, and commonproper-motion stars). The total observed multiplicity is derived, and aprobable significant difference in the total multiplicity is foundbetween the two subgroups. An attempt is made to obtain the truemultiplicity using appropriate incompleteness numbers, and somestatistical information about the distribution of the secondary massesis derived. Systems with similar masses seem to be favored regardless oforbital period.
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Quantitative Spectral Peculiarity Indices of Cp-Stars of the Upper Main Sequence
Not Available
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Spectroscopy of hot horizontal-branch stars in globular clusters. I - NGC 6397
Spectra have been obtained, with moderate signal-to-noise ratio, forfour, blue horizontal-branch (BHB) stars in the metal-poor globularcluster NGC 6397 using a photon-counting detector. These photometricallyselected stars have effective temperatures near 12,000 K. The observedH-delta profiles suggest values of log g near 2.8, putting these starsabove the main sequence of population I. At an apparent signal-to-noiseratio of 25:1 between 3900 A and 4200 A, the only identifiableabsorption lines other than the Balmer lines are weak He I 4026 A and CaII 3933 A (presumably interstellar). The scatter in the observedstrengths of He I 4026 A for several field stars makes it uncertainwhether or not He I is underabundant in these cluster BHB stars. Anexamination of the cores of the H-delta profiles suggests that thecluster HB stars are probably slow rotators.
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The spectral energy distribution of early type stars. I - A catalogue of photometric data of 259 stars from 0.15 to 4.8 microns
For the derivation of physical parameters (e.g., effective temperatureand radius) of early-type stars from their intrinsic spectral-energydistribution, and for the study of foreground interstellar and/orcircumstellar matter, a sample of 237 O, B, and A stars was chosen fromthe ANS catalog (Wesselius et al., 1982). The ANS ultraviolet and theJohnson UBV data (mostly from Nicolet's catalog, 1978) of these starswere supplemented with visual Walraven WULBV, red VRI, and near-infraredJHKLM measurements. All these data are given in the present catalog.Data for 22 stars of spectral type later than A are also included.
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Velocities of rotation of chemically peculiar stars
An analysis of the velocities of rotation of 77 peculiar stars, membersof open clusters and associations in the age range log t = 6.4-8.7, wasmade based on observations with the OZSP spectrograph of the 6-mtelescope. It was concluded that there is no loss of angular momentum bypeculiar stars in the process of gravitational contraction as theyapproach the zero-age main sequence and in the stage of evolution withinthe main sequence. A statistically significant difference was obtainedin the velocities of rotation of peculiar stars in different zones ofthe Scorpio-Centaurus association: Stars of the core (t = 4 million yr)rotate faster on the average than stars in the outer zones of theassociation (t = 12 million yr).
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The BP and AP stars in the Scorpius-Centaurus moving cluster. II
High-resolution 6-m telescope spectra of ten peculiar stars and fourstars of luminosity class Vb (broad hydrogen lines) in the Sco-Cenmoving cluster provide the degree P and type of peculiarity as well asquantitative spectral types of rotational velocities. Values of theeffective temperature and surface gravity log g are determined for 29peculiar stars in the clusters. Class Vb stars have log g larger by0.2-0.4 than stars on the initial main sequence.
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Infrared photometry of southern early-type stars
The paper presents infrared photometry tied to the JHKL (1.2-3.5microns) broadband photometric system for 229 southern early-type stars.To determine data for stars of low reddening intrinsic visual-IR colorindices were used; the E(V-K)/E(B-V) diagram was applied to evaluate theratio of total selective extinction. A mean value of R = 3.12 plus orminus 0.05 was found for stars close to the galactic plane, but a highervalue of R (about 4.0) applies to the Orion and Sco-Oph regions.Infrared two-color diagrams were used to investigate the occurrence ofinfrared excess emission in different classes of shell star; no excesseswere found for supergiants or Of stars. It is concluded that theanomalous position HD 164740 in the two-color diagrams is produced bystrong infrared excess and not by a peculiar extinction law.
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An ultraviolet extinction study of the rho Ophiuchi dark cloud
Five-band ultraviolet spectrophotometry has been carried out for 54stars in the upper Scorpius complex. Of these, 14 stars in the rhoOphiuchi dark cloud and 13 in the surrounding area are found to be freeof spectral peculiarities and contamination by scattered light fromnearby bright stars. The dark cloud stars give extinction curves whichare significantly lower than the average extinction curves derived byother investigators and also those observed for localized regions suchas the area around Cygnus X-1 and the Cepheus OB III cluster. Thisimplies that the dust in the upper Scorpius region, especially that inthe rho Ophiuchi dark cloud has larger average size than the normalinterstellar medium. R, the ratio of total-to-selective extinction, isfound to be 4.2. The effects of a lower extinction curve on thechemistry of a dark cloud is also briefly discussed.
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Catalogue of photometric data related to surface magnetic fields for B-type stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1980A&AS...41..111C&db_key=AST
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Prediction of spectral classification from photometric observations - Application of the UVBY beta photometry and the MK spectra classification. II - General case
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1980A&A....85...93M&db_key=AST
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Prediction of spectral classification from photometric observations-application to the UVBY beta photometry and the MK spectral classification. I - Prediction assuming a luminosity class
An algorithm based on multiple stepwise and isotonic regressions isdeveloped for the prediction of spectral classification from photometricdata. The prediction assumes a luminosity class with reference touvbybeta photometry and the MK spectral classification. The precisionattained is about 90 percent and 80 percent probability of being withinone spectral subtype respectively for luminosity groups I and V and forluminosity groups III and IV. A list of stars for which discrepanciesappear between photometry and spectral classification is given.
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Spectrophotometry in the upper Scorpius region
The low dispersion spectrophotometric measures of 29 stars in the upperScorpius region, made from 1964 to 1969 with an old-type spectrumscanner, employing a 91 cm telescope with a 60 A slit, are examined.Equivalent widths of H-beta, H-gamma, and H-delta are measured alongwith the size of the Balmer discontinuity, the gradients in theultraviolet and the blue-green-yellow parts of the spectrum. The resultsof the intensity distributions, the spectral intensity distributions,and some measured quantities are presented in tabulated form.
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Stellar rotation on the zero age main sequence
Analysis of rotational velocities of unevolved members in clustersindicates that for a given mass the dispersion in the true rotationalvelocities is small for normal, single main-sequence stars. The envelopeof highest rotation of rich clusters and associations is utilized toderive the rotational velocities on the zero age main sequence. It issuggested (1) that the zero age main-sequence rotation curve defines thestar's stability against fission and (2) that the frequency ofspectroscopic binaries in a cluster is determined by the total angularmomentum available to the gas cloud before fragmentation.
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An infrared study of the Ophiuchus dark cloud
A near-infrared survey has been conducted of nearly 18 square degrees ofthe Ophiuchus dark cloud complex. Additional observations have been madeof selected objects found in this survey and of the brighter objectsfound by Grasdalen et al. and by Vrba et al. in this region in order toidentify and study the young stars associated with the cloud. Theseobservations show that very recent star formation has been largelyrestricted to a small region at the center of the dark cloud complex, nomore than a few parsecs in extent. Most of the young stars do not appearto be main-sequence stars. At least three of these objects appear to besurrounded by infrared reflection nebulae. Many of the objects studiedare background K and M giants which can be used to determine thenear-infrared extinction due to the cloud.
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Detection of errors in spectral classification by cluster analysis
Cluster analysis methods are applied to the photometric catalogue ofuvby-beta measurements by Hauck and Lindemann (1973) and point out 249stars the spectral type of which should be reconsidered or thephotometric indices of which should be redetermined.
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Photoelectric observations of lunar occultations.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975MNRAS.170..229H&db_key=AST
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The ratio of total to selective absorption in the rho OPH cloud.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974MNRAS.168..371W&db_key=AST
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Interstellar dust in the rho OPH dark cloud.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973ApJ...182...95C&db_key=AST
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