|A high-resolution spectroscopy survey of β Cephei pulsations in bright stars|
We present a study of absorption line-profile variations in early-B typenear-main-sequence stars without emission lines. We have surveyed atotal of 171 bright stars using the Nordic Optical Telescope (NOTSA),William Herschel Telescope (ING) and Coudé Auxiliary Telescope(ESO). Our sample contains 75% of all O9.5-B2.5 III-V non-emission-linestars brighter than 5.5 mag. We obtained high signal-to-noise,high-resolution spectra of the SiIII λ4560 triplet - for 125stars of our sample we obtained more than one spectrum - and examinedthese for pulsational-like line-profile variations and/or structure. Weconclude that about half of our sample stars show evidence forline-profile variations (LPV). We find evidence for LPV in about 65% ofour sample stars brighter than V=5.5. For stars with rotationalbroadening V sin i 100 km s-1, we find evidence for LPVin about 75% of the cases. We argue that it is likely that these LPV areof pulsational origin, and that hence more than half of thesolar-neighbourhood O9.5-B2.5 III-V stars is pulsating in modes that canbe detected with high-resolution spectroscopy. We detected LPV in 64stars previously unknown to be pulsators, and label these stars as newβ Cep candidates. We conclude that there is no obvious differencein incidence of (pulsational) LPV for early-B type near-main-sequencestars in binaries or in OB associations, with respect to single fieldstars.
|New periodic variables from the Hipparcos epoch photometry|
Two selection statistics are used to extract new candidate periodicvariables from the epoch photometry of the Hipparcos catalogue. Theprimary selection criterion is a signal-to-noise ratio. The dependenceof this statistic on the number of observations is calibrated usingabout 30000 randomly permuted Hipparcos data sets. A significance levelof 0.1 per cent is used to extract a first batch of candidate variables.The second criterion requires that the optimal frequency be unaffectedif the data are de-trended by low-order polynomials. We find 2675 newcandidate periodic variables, of which the majority (2082) are from theHipparcos`unsolved' variables. Potential problems with theinterpretation of the data (e.g. aliasing) are discussed.
|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%.
|The Distribution of Dust Clouds in the Interstellar Medium|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJ...457..764D&db_key=AST
|The ROSAT all-sky survey catalogue of optically bright OB-type stars.|
For the detailed statistical analysis of the X-ray emission of hot starswe selected all stars of spectral type O and B listed in the Yale BrightStar Catalogue and searched for them in the ROSAT All-Sky Survey. Inthis paper we describe the selection and preparation of the data andpresent a compilation of the derived X-ray data for a complete sample ofbright OB stars.
|A catalog of far-ultraviolet point sources detected with the fast FAUST Telescope on ATLAS-1|
We list the photometric measurements of point sources made by the FarUltraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 spaceshuttle mission. The list contains 4698 Galactic and extragalacticobjects detected in 22 wide-field images of the sky. At the locationssurveyed, this catalog reaches a limiting magnitude approximately afactor of 10 fainter than the previous UV all-sky survey, TDl. Thecatalog limit is approximately 1 x 10-14 ergs A sq cm/s,although it is not complete to this level. We list for each object theposition, FUV flux, the error in flux, and where possible anidentification from catalogs of nearby stars and galaxies. Thesecatalogs include the Michigan HD (MHD) and HD, SAO, the HIPPARCOS InputCatalog, the Position and Proper Motion Catalog, the TD1 Catalog, theMcCook and Sion Catalog of white dwarfs, and the RC3 Catalog ofGalaxies. We identify 2239 FAUST sources with objects in the stellarcatalogs and 172 with galaxies in the RC3 catalog. We estimate thenumber of sources with incorrect identifications to be less than 2%.
|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 determination of T_eff_ of B, A and F main sequence stars from the continuum between 3200 A and 3600 A.|
A method of determination of the effective temperature of B, A and Fmain sequence stars is proposed, using the slope of the continuumbetween 3200A and 3600A. The effective temperature calibration is basedon a sample of stars with energy distributions known from UV to the red.We have determined the Balmer jump and the effective temperatures for235 main sequence stars. The temperatures found have been compared withthose derived by Underhill et al. (1979), Kontizas & Theodossiou(1980), Theodossiou (1985), Morossi & Malagnini (1985). Thecomparison showed good agreement for most of the stars in common. On theother hand, the temperatures derived from the reddening-free colourfactor QUV, from the colour index (m1965-V) and from (B-V), given inGulati et al. (1989), are systematically lower than our temperatures,however the differences are within one-sigma error.
|The low filling factor of dust in the Galaxy|
The neighborhood of 745 luminous stars in the IRAS Skyflux plates wasexamined for the presence of dust heated by the nearby star. One-hundredtwenty-three dust clouds were found around only 106 of the stars with avolume filling factor of 0.006 and an intercloud separation of 46 pc.Nowhere was a region found where the dust is smoothly distributedthrough the volume of space heated by the star; hence an upper limit of0.06/cu cm is placed on the equivalent gas density in the intercloudregions. Due to the lack of IR emission near the star, it is found thatless than 1 percent of the stellar luminosity is reprocessed within 10pc of the star. The clouds have an average density of 0.22/cu cm and aradius of 1.9 pc, albeit with wide variations in their properties. Twodifferent scale heights of 140 and 540 pc were found for the number ofclouds around different groups of stars, which are interpreted asevidence for different distributions of dust in and out of the Galacticdisk.
|Fifth fundamental catalogue. Part 2: The FK5 extension - new fundamental stars|
The mean positions and proper motions for 3117 new fundamental starsessentially in the magnitude range about 4.5 to 9.5 are given in thisFK5 extension. Mean apparent visual magnitude is 7.2 and is on average2.5 magnitudes fainter then the basic FK5 which has a mean magnitude of4.7. (The basic FK5 gives the mean positions and proper motions for theclassical 1535 fundamental stars). The following are discussed: theobservational material, reduction of observations, star selection, andthe system for the FK5 extension. An explanation and description of thecatalog are given. The catalog of 3117 fundamental stars for the equinoxand epoch J2000.0 and B1950.0 is presented. The parallaxes and radialvelocities for 22 extension stars with large forecasting effects aregiven. Catalogs used in the compilation of the FK5 fundamental catalogare listed.
|Catalogue of i and w/w crit values for rotating early type stars|
|Empirical temperature calibrations for early-type stars|
Three temperature calibrations of suitable photometric quantities havebeen derived for O and B stars. A sample of 120 stars with reliableT(eff.) determinations has been used for establishing each calibration.The different calibrations have been critically discussed and compared.Temperature determinations for 1009 program stars have been obtainedwith an accuracy of the order of 10 percent.
|Effects of stellar rotation on the Geneva photometric system|
The effects of stellar rotation on colors and parameters of the Genevaphotometric system are considered, using homogeneous material. Attentionis focused on these parameters useful for deriving physical propertiesof B- and A-type stars. Two major photometric planes in this respect,the (X, Y) plane and the (d, Delta) plane, are not discernibly affectedby rotation. The temperature parameter, B(2) - V(1) is reddened byrotation to an extent that is in agreement with model calculations foruniformly rotating stars.
|Interstellar gas depletion and dust parameters|
A relationship is developed that correlates the relative abundances ofthe elements in the interstellar gas phase and the wavelength of maximuminterstellar polarization, lambda-max. The correlations of theobservational data available for the gas phase abundances of titanium,iron, magnesium, and carbon and the values of lambda-max support thetheory. However, to determine the chemical composition of the dustparticles, data on the interstellar gas depletion are needed, especiallyin lines of sight where lambda-max has extreme values.
|A catalog of ultraviolet interstellar extinction excesses for 1415 stars|
Ultraviolet interstellar extinction excesses are presented for 1415stars with spectral types B7 and earlier. The excesses with respect to Vare derived from Astronomical Netherlands Satellite (ANS) 5-channel UVphotometry at central wavelengths of approximately 1550, 1800, 2500, and3300 A. A measure of the excess extinction in the 2200-A extinction bumpis also given. The data are valuable for investigating the systematicsof peculiar interstellar extinction and for studying the character of UVinterstellar extinction in the general direction of stars for which theextinction-curve shape is unknown.
|Catalogue of the energy distribution data in spectra of stars in the uniform spectrophotometric system.|
|The local system of early type stars - Spatial extent and kinematics|
Published uvby and H-beta photometric data and proper motions arecompiled and analyzed to characterize the structure and kinematics ofthe bright early-type O-A0 stars in the solar vicinity, with a focus onthe Gould belt. The selection and calibration techniques are explained,and the data are presented in extensive tables and graphs and discussedin detail. The Gould belt stars of age less than 20 Myr are shown togive belt inclination 19 deg to the Galactic plane and node-lineorientation in the direction of Galactic rotation, while the symmetricaldistribution about the Galactic plane and kinematic properties (purecircular differential rotation) of the belt stars over 60 Myr oldresemble those of fainter nonbelt stars of all ages. The unresolveddiscrepancy between the expansion observed in the youngest nearby starsand the predictions of simple models of expansion from a point isattributed to the inhomogeneous distribution of interstellar matter.
|The CH radical in diffuse interstellar clouds|
Observations of the interstellar CH A-X R2(1) line at 4300.3 A arepresented for 29 lines of sight extending from 140 to 2800 pc in theGalactic plane. A comparison of the CH and H2 column density shows thatN(CH) varies as N(H2) as expected for production of CH by a gas phasereaction network running in molecular hydrogen. The network alsoreproduces the observed ratio N(CH)/N(H2) for these diffuse interstellarclouds.
|Copernicus observations of C I - Pressures and carbon abundances in diffuse interstellar clouds|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1983ApJ...270...88J&db_key=AST
|An observational study of the influence of close companions on the pulsations of Beta Cephei stars|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1983A&A...121...45W&db_key=AST
|Copernicus observations of the N V resonance doublet in 53 early-type stars|
UV spectra in the wavelength interval 1170-1270 A are presented for 53early-type stars ranging in spectral type from O6.5 V to B2.5 IV. Thesample includes four Wolf-Rayet stars, seven known Oe-Be stars, and sixgalactic halo OB stars. A qualitative analysis of the stellar N vdoublet reveals that: (1) N v is present in all stars hotter and moreluminous than type B0 for the main sequence, B1 for giants, and B2 forsupergiants; (2) shell components of N v and an unidentified absorptionfeature at 1230 A are present in about half of the stars; (3) the columndensity of N v is well correlated with bolometric luminosity over thespectral range O6 to B2; and (4) the ratio of emission to absorptionequivalent width is a factor of 2 smaller in the main sequence starsthan in supergiants, which suggests that the wind structure changes as astar evolves. For several stars, this ratio is too small to be explainedby traditional wind models.
|Starlight polarization in the direction of two H I complexes|
Upper limits to the gas/dust ratio in the direction of two complexes arederived based on 21-cm line observations and starlight polarizationmeasurements. Elongated H I structures parallel to the galactic magneticfield suggest that the gas and dust comprise a common cloud or cloudsystem. Dust producing the starlight polarization is mixed with the H Igas, aiding in estimating the distance for the two H I complexes.Distances of 100 pc for the filament at low velocities and of 200 pc foran intermediate-velocity cloud complex (IVC) are established frompolarimetric data, and possible origins for the filaments and IVC aresuggested.
|Interstellar gas in the GUM Nebula|
A survey of the interstellar gas near the Gum Nebula by opticalobservation of 67 stars at Ca II, 42 stars at Na I, and 14 stars in theUV with the Copernicus satellite provided radial velocities and columndensities for all resolved absorption components. Velocity dispersionsfor gas in the Gum Nebula are not significantly larger than in thegeneral interstellar medium; the ionization structure is predominantlythat of an H II region with moderately high ionization. Denser, morehighly ionized clouds are concentrated toward the Gum Nebula; theseclouds do not show the anomalously high ionization observed in the Velaremnant clouds.
|The depletion of interstellar gaseous iron|
The Copernicus UV telescope was used to measure equivalent widths ofinterstellar Fe II resonance lines toward 55 early-type stars; themeasurements permit the determination of Fe II column densities. Thedepletion of interstellar gaseous iron was obtained by combining thesemeasurements with the results from a previous atomic and molecularhydrogen survey program; the derived depletions refer mostly to matterin H I regions. As an example, the nearly normal gaseous iron abundancein the distant high-latitude intermediate-velocity cloud toward HD 93521is consistent with the idea that these clouds are produced by galacticsupernova explosions.
|A survey of interstellar H I from L-alpha absorption measurements. II|
This paper presents interstellar H I column densities, mean H I spacedensities, total neutral hydrogen column densities, and total meanhydrogen space densities toward 100 stars surveyed in the L-alpha regionwith the U2 detector of the Copernicus satellite. The data for 47 starsare compared with OAO 2 results, and ratios of gas to E(B-V) colorexcess are computed for 30 'intercloud' stars, 45 'cloud' stars, and thecombined sample of 75 stars. A definitive value of 5.8 x 10 to the 21stpower atoms/sq cm per mag is obtained for the mean ratio of totalneutral hydrogen to color excess, indicating that this ratio seems to bea constant, independent of location in the sky, except possibly towardstars with anomalous extinction. The anomalous ratio determined for RhoOph is examined, and the galactic distribution of neutral hydrogen isevaluated. The following values are estimated for matter in the galacticplane within 500 pc of the sun: a total mean hydrogen space density of1.15 atoms/cu cm, a mean H2 space density of 0.143 molecule/cu cm(possibly a lower limit), and a mean H I space density of 0.86 atom/cucm (a possible overestimate).
|A search for Beta Canis Majoris stars|
The results of a search for southern Beta CMa stars are presented.Photoelectric photometry of thirty-one candidates shows that eight ofthese are previously unrecognized probable or certain Beta CMavariables. Four of these stars are members of the galactic cluster NGC3293. One Delta Sct variable and one eclipsing binary were discovered. Afew other stars are probably ellipsoidal variables.
|A survey of interstellar molecular hydrogen. I|
Data from the Copernicus satellite's ultraviolet telescope were used tosurvey column densities of atomic and molecular hydrogen from a largesample of early-type stars; these data have bearing on an eventualunderstanding of diffuse and dense interstellar clouds. Column densitiesare derived by fitting damping profiles to the observed spectra, most ofwhich exhibit strong damping lines in the lower rotational levelssurveyed. Plots of dust column density, fractional abundance ofmolecular hydrogen, and the logarithm of fractional abundance versustotal gas column density are given for many of the stars; stars withabnormally large or small hydrogen column densities, as well as somedistant stars at high galactic latitudes, are considered. Equilibriumand nonequilibrium theories accounting for the abundance of interstellarhydrogen are compared, and support is found in the data for an accountwhich balances hydrogen formation on interstellar grains withdestruction through photodissociation. Overall averages for atomic andmolecular hydrogen levels in the galactic plane are also calculated.
|Search for Beta Cephei stars south of declination -20 deg. I - Incidence of light variability among early B giants and subgiants: Summer objects|
|Structure and age of the local association /Pleiades group/|
Intermediate-band indices are used to derive luminosities for some 500early-type stars with well-determined proper motions and radialvelocities. Space motion vectors and galactic coordinates are computedfor the stars considered. It is found that the local association membersare mainly concentrated in the Sco-Cen region in the Southern Hemisphereand the Cas-Tau region in the north.
|60th Name-List of Variable Stars|