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Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i
This work is the second part of the set of measurements of v sin i forA-type stars, begun by Royer et al. (\cite{Ror_02a}). Spectra of 249 B8to F2-type stars brighter than V=7 have been collected at Observatoirede Haute-Provence (OHP). Fourier transforms of several line profiles inthe range 4200-4600 Å are used to derive v sin i from thefrequency of the first zero. Statistical analysis of the sampleindicates that measurement error mainly depends on v sin i and thisrelative error of the rotational velocity is found to be about 5% onaverage. The systematic shift with respect to standard values fromSlettebak et al. (\cite{Slk_75}), previously found in the first paper,is here confirmed. Comparisons with data from the literature agree withour findings: v sin i values from Slettebak et al. are underestimatedand the relation between both scales follows a linear law ensuremath vsin inew = 1.03 v sin iold+7.7. Finally, thesedata are combined with those from the previous paper (Royer et al.\cite{Ror_02a}), together with the catalogue of Abt & Morrell(\cite{AbtMol95}). The resulting sample includes some 2150 stars withhomogenized rotational velocities. Based on observations made atObservatoire de Haute Provence (CNRS), France. Tables \ref{results} and\ref{merging} are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.125.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/393/897
| Bispectrum speckle interferometry of the massive protostellar object S140 IRS 1: Evidence for multiple outflows
Bispectrum speckle interferometry is employed to explore the immediateenvironment of the deeply embedded young stellar object S140 IRS 1. AK'-band (2.0-2.3 mu m) diffraction-limited resolution of 76 mas ( ~ 70AU) is achieved with the SAO 6 m telescope, as well as a dynamical rangeof more than 8 mag and a field of view of 13'' x 21''. Our imageexhibits many previously unseen complex structures. In addition to thebright, elongated, and very clumpy feature pointing from the centralsource to the south-east, which was already discussed in a previouspaper (Schertl et al. \cite{Schertl00}), we find several arc-likestructures north-east of IRS 1, extended diffuse emission south of IRS1, and four new point sources. The diffuse and fragmentary structuresclose to IRS 1 appear to trace circumstellar material swept up byenergetic outflows. In combination with molecular line emission mapsfrom the literature, our image provides direct confirmation that twodistinct bipolar outflow systems continue to be driven from IRS 1 onscales between 3\arcsec and 100\arcsec. A system of three arc-likestructures to the north-east is consistent with cavities excavated by aprecessing jet or wind-driven outflow. We discuss the implications forthe nature of the central source. Based based on observations obtainedat the Special Astrophysical Observatory with the 6 m telecope.
| Diffraction-limited bispectrum speckle interferometry and speckle polarimetry of the young bipolar outflow source S140 IRS1
We present bispectrum speckle interferometry and speckle polarimetry ofthe deeply embedded infrared bipolar outflow source S140 IRS1, a massiveprotostellar object in the L1204 molecular cloud. Using the SAO 6 mtelescope, we obtained 280 mas resolution polarization maps of S140 IRS1as well as a K-band image with diffraction-limited resolution lambda /Dof 76 mas, which is the highest angular resolution image of a youngoutflow source ever obtained in the infrared. Our data suggest that thecentral source is marginally resolved with a FWHM diameter ofapproximately 20 mas ( ~ 20 AU). The most remarkable feature in ourimage is a bright extended and very clumpy structure pointing away fromthe central source in exactly the same direction as the blue-shifted COoutflow lobe. A centro-symmetric pattern of high polarization in thisfeature suggests that we see scattered light from the central source. Weinterprete this feature as the clumpy inner surface of a partiallyevacuated cavity in the circumstellar envelope around IRS1, which hasbeen excavated by the strong outflow from IRS1.
| Mesures de vitesses radiales. VIII. Accompagnement AU sol DU programme d'observation DU satellite HIPPARCOS
We publish 1879 radial velocities of stars distributed in 105 fields of4^{\circ} \times 4^{\circ}. We continue the PPO series \cite[(Fehrenbachet al. 1987;]{Feh87} \cite[Duflot et al. 1990, 1992 and 1995),]{Du90}using the Fehrenbach objective prism method. Table 1 only available inelectronic form at CDS via to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJS...99..135A&db_key=AST
| 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 A0 stars
A photometric grid, standardized on MK spectral standards, has been usedto compare spectral types and luminosity classes obtainedphotometrically with those in two extensive spectral surveys coveringthe entire sky. Major discrepancies include the spectroscopicclassification of B9.5, which may indicate an otherwise unrecognizedspectral peculiarity, a different A0/A1 spectral type boundary in thetwo samples involved, the well-known misclassification of weak heliumstars, and an appreciable percentage of stars which are called dwarfsspectroscopically but are of higher photometric luminosity. The spacemotion vectors of these stars for which radial velocities are available,and excluding the minimum of 25 percent that are spectroscopic binarieswithout orbital elements, show structure in their distribution in the(U, V)-plane, with members of the Local Association and the Hyades andSirius superclusters forming obvious concentrations. The members of theLocal Association in the samples are mainly old (more than 200 millionyears) mode A stars, although a few much younger stars are included. Themembers of the Hyades and Sirius superclusters contain many bluestragglers, including several peculiar stars of the Hg, Mn, and Sivarieties.
| Photometric variability of B- and A-type supergiants
Photometric observations of 16 early-type (O9 to A3) supergiants havebeen obtained. All but two of the stars are variable, with a range ofabout 0.05 mag. The light curves are irregular, but characteristic timescales or 'quasi-periods' can be identified. The ratio of thequasi-period to the theoretical period (for pulsation in the fundamentalradial mode) varies from 2-10 in the earliest-type supergiants to 0.2-2in the later-type supergiants. The variability is most likely due tononradial pulsation, at least in the O-B-type supergiants.
| Spectral classification from the ultraviolet line features of S2/68 spectra. III - Early A-type stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1978A&AS...33...15C&db_key=AST
| Space velocities and ages of nearby early-type stars
Photometric distances and space velocities have been calculated for 458B0-A0 stars with apparent magnitudes not exceeding 6.5. UsingStromgren's ubvy-beta photometry the effective temperature and theposition in bolometric magnitude over the zero-age main sequence of thestars were derived. These quantities were used to obtain age and massfor 423 of the stars by interpolation in the models of stellar evolutionfor the chemical composition (X Z) = (0.7, 0.03). A relation forderiving interstellar reddening for normal stars in the intermediategroup is given.
| Photoelectric H-alpha line photometry of early-type stars
A total of 293 bright stars of spectral types O, B, A, F and ofluminosity classes I through V have been measured with a photoelectricphotometer equipped with two interference filters of 30-A bandwidth, onecentered on H-alpha and the other at 6622 A. A correction term has beenallowed for the response of the photometric system and for the continuumenergy distribution in the two spectral regions considered. Theresulting photometric alpha indices of H-alpha line strength arecompared with previous H-alpha, H-beta, and H-gamma photometricmeasures, H-alpha equivalent widths, the MK spectral type, /u-b/, /c1/,and b-y indices of the uvby photometric system. The results emphasizethe advantage of using H-alpha line photometry to discriminate betweenemission-line effects and luminosity effects in early-type stars and todetect emission-line variability.
| Rotational Velocities of a0 Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974ApJS...28..101D&db_key=AST
| Four-color and Hβ photometry for the brighter AO type stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972A&AS....5..109C&db_key=AST
| A catalogue of proper motions for 437 A stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970A&AS....1..189F&db_key=AST
| Photoelectric observations of early A stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970A&AS....1..165J&db_key=AST
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Observation and Astrometry data
| Constellation: | ケフェウス座 |
| Right ascension: | 22h23m00.20s |
| Declination: | +62°25'12.0" |
| Apparent magnitude: | 6.04 |
| Distance: | 218.341 parsecs |
| Proper motion RA: | 17.3 |
| Proper motion Dec: | 13.5 |
| B-T magnitude: | 6.066 |
| V-T magnitude: | 6.035 |
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