Determination of R_V towards galactic O stars
We present new measurements of the interstellar reddening parameterRV=AV/E(B-V) towards 35 O stars. The results arecombined with measurements from the literature for 60 stars to study thebehaviour of RV with heliocentric distance. RV isthe single basic parameter which characterizes the interstellarextinction from the near-infrared to the far-UV spectral region. Theabsolute extinction AV, from which RV is derived,is best determined by optical and near-infrared photometry (Cardelli etal. \cite{r3}). We consider important the derivation of RVwith the same technique in the direction of as many as possible galacticO stars.
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A multi-wavelength study of the Sharpless 151 region
Results are presented of an extensive, multi-wavelength study of thearea around the evolved HII region Sh 2-151. We discuss the excitationof the HII region, and analyze its interaction with molecular clouds inthe vicinity, the clouds themselves, and their embedded objects. Wepresent KOSMA 3-m (12) CO(2-1) and (3-2) observations of a 26(') x46(')region around Sh 2-151. These observations reveal five clouds, with atotal mass of 2.9x10(4) Msun. A small (2(') x4(') ) region tothe SW of Sh 2-151 was mapped in several CO and CS transitions with theIRAM 30-m telescope. The latter region contains 1.8x 10(3)Msun of molecular mass, and hosts an IRAS- and H_2O masersource (WB89-234). Tracers of higher (column-) densities, such as C(18)O and CS, show the existence of two clumps (N(H_2) \approxprox 1-2 x10(22) cm(-2) ) connected by a ridge of warm (Tkin ~ 36 K)narrow-line (Delta v((12) CO)<1 km s(-1) ) gas. The southern clumpcontains the IRAS/maser source, exhibits a molecular outflow (M$~prox5M_{\odot}, \taudyn ~prox 2\times 10^5 yr), and is thereforeprobably a region of active star formation. In the northern clump theline profiles have an intermediate width (1-3 km s^{-1}; partly due tothe presence of two emission components) and are non-gaussian(shoulders, wings) at several positions. IRAS (HIRES) observations showthere is also FIR emission associated with the northern clump. NIR (J,H, K, H_2) observations show the presence of several red star-likeobjects and diffuse emission in both clumps; some of the diffuseemission is stronger and more extended in K and H_2, and may be due todust emission around embedded objects. HIRES data reveal thatIRAS23004+5642 (WB89-234) nearly coincides with the H_2O maser and theoutflow, and not with the strong, narrow-line CO-emitting gas detectedtowards the point source catalog position. The linewidth of thisrelatively low-density warm gas, the heating source of which is as yetunknown, indicates the absence of dynamical interaction with both Sh2-151 and the embedded IR sources. >From the HIRES 60\mum and 100\mumdata we derive dust temperatures of 30-40 K, the highest valuesoccurring near the maser, and a dust mass of \sim30 M_{\odot}; assuminga gas-to-dust ratio of 100, this implies we detect \sim10% of the dust.Evidence from the available (literature) data leads to the conclusionthat the exciting star(s) of Sh 2-151 has (have) not yet beenidentified. We suspect that one or more early type (
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UBV beta Database for Case-Hamburg Northern and Southern Luminous Stars
A database of photoelectric UBV beta photometry for stars listed in theCase-Hamburg northern and southern Milky Way luminous stars surveys hasbeen compiled from the original research literature. Consisting of over16,000 observations of some 7300 stars from over 500 sources, thisdatabase constitutes the most complete compilation of such photometryavailable for intrinsically luminous stars around the Galactic plane.Over 5000 stars listed in the Case-Hamburg surveys still lackfundamental photometric data.
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Wolf-Rayet stars and O-star runaways with HIPPARCOS. I. Kinematics
Reliable systemic radial velocities are almost impossible to secure forWolf-Rayet stars, difficult for O stars. Therefore, to study the motions- both systematic in the Galaxy and peculiar - of these two relatedtypes of hot, luminous star, we have examined the Hipparcos propermotions of some 70 stars of each type. We find that (a) both groupsfollow Galactic rotation in the same way, (b) both have a similarfraction of ``runaways'', (c) mean kinetic ages based on displacementand motion away from the Galactic plane tend to slightly favour thecluster ejection over the the binary supernova hypothesis for theirformation, and (d) those with significant peculiar supersonic motionrelative to the ambient ISM, tend to form bow shocks in the direction ofthe motion. Based on data from the ESA Hipparcos astrometry satellite.Table~1 is only available in electronic form at the CDS via anonymousftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
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Extinction law survey based on UV ANS photometry
The paper presents an extensive survey of interstellar extinction curvesderived from the ANS photometric measurements of early type starsbelonging to our Galaxy. This survey is more extensive and deeper thanany other one, based on spectral data. The UV color excesses aredetermined with the aid of 'artificial standards', a new techniqueproposed by the authors which allows the special check of Sp/L match ofa target and the selected standard. The results indicate that extinctionlaw changes from place to place.
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Photoelectric photometry of OB stars in the Vilnius system
Not Available
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The interstellar 217 NM band - A third catalogue of equivalent widths
A catalog of equivalent widths of the 217 nm interstellar absorptionband as well as other parameters characterizing the extinction curve inthe ultraviolet has been compiled for 790 O and B stars. A relativelytight correlation between the equivalent width of the 217 nm band andE(B-V) indicates that the absorber of this band is connected with thepopulation of larger interstellar grains responsible for the visualextinction. The parameter characterizing the amount of extinction in thefar UV is only weakly correlated with E(B-V), a result in accord withthe assumption that a second population of very small grains causes therapid increase of the far-UV extinction.
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Intrinsic UV colour indices of early-type stars
Intrinsic UV colors of the early-type stars have been determined using anew method based on the assumption that there is a linear correlationbetween UV color excesses and E(B-V). This method makes it possible toinclude all stars with available photometry independent of reddening.Results derived from ANS photometric data are presented. These includeintrinsic UV colors covering all ANS photometric bands for spectraltypes O6-AO. It is also shown that this method, based on perfectcorrelation between UV and visual extinction, fails for the shortwavelength color index CI(1550 A-1800 A).
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A Wide-Angle Astrometric Standard in the Moscow Zenith Zone
Not Available
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The initial mass function for massive stars
A machine readable catalog of over 750 galactic O stars with publishedphotometry, spectral types, and luminosity classes has been compiled.The catalog is probably complete to a distance of about 2.5 kpc. Fromthis volume-limited data, the initial mass function (IMF) for stars moremassive than 20 solar masses has been derived. This IMF differs fromthat of Miller and Scalo (1979) and of Lequeux (1979), in havingproportionately more O type stars and not as steep a fall-off in numberof stars with increasing mass. Dividing the sample into stars inside andoutside the solar circle, a substantial difference in the IMF of themost massive stars is found. There are proportionally more toward thegalactic center. This gradient in the IMF may be related to the observedspace density of Wolf-Rayet stars, which are descendants of O typestars.
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Nitrogen anomalies in O-type stars - A new spectroscopic criterion
A spectroscopic analysis was performed on 95 O-type stars to detectnitrogen overabundance in an investigation of spectroscopic criteria. Itis found that the N III 4514 A line is a good indicator of the abundancevariations of N in O-type stars, and it is suggested that the ONphenomenon is a continuous one rather than a marked discontinuitybetween normal O stars and those showing nitrogen overabundance.Anomalies are investigated for several early O stars, and it isconcluded that mass transfer in close binary systems and high mass lossrates due to stellar winds are the most probable mechanisms to produceON stars.
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Studies of luminous stars in nearby galaxies. I. Supergiants and O stars in the Milky Way.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1978ApJS...38..309H&db_key=AST
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A catalogue of galactic O stars. The ionization of the low density interstellar medium by runaway stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974RMxAA...1..211C&db_key=AST
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A new general O type stars catalogue
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973A&AS...12..277G&db_key=AST
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The Law of Interstellar Reddening and Absorption.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1956ApJ...124..367H&db_key=AST
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Studies in Galactic STRUCTURE.II.LUMINOSITY Classification for 1270 Blue Giant Stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1955ApJS....2...41M&db_key=AST
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Polarization of Stellar Radiation. III. The Polarization of 841 Stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1951ApJ...114..241H&db_key=AST
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A Finding List of O and B Stars of High Luminosity.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1951ApJ...113..141N&db_key=AST
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Studies of Faint B-Type Stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1950ApJ...111..495P&db_key=AST
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