Modeling the Neutral Hydrogen Interstellar Medium: A Better Kinematic Distance Tool
An advanced approach to the kinematic distance method is developed. Themethod is applicable to second- and third-quadrant Galactic objects withknown velocities. It is based on fitting a model of the density andvelocity features in an isothermal H I disk to observed H I data. Thevelocity field of the gas is modeled with a power law for basic circularrotation, underlying noncircular motions from a two-armed density wavepattern. With a reasonable number of adjustable parameters andconstraints the model reproduces observations toward many Galacticobjects, and accurate distances are found from the modeled velocityfield. High-resolution H I spectral line data from the Canadian GalacticPlane Survey (CGPS; Taylor et al.) are used to discriminate clouds fromthe intercloud medium (the ``stratum'') for which the model is intended.The ability of the model to reproduce these data is demonstrated in one-[Tb(v)] and two- [Tb(l, v)] dimensional fits.Distances to 22 H II regions and SNRs calculated by the fitted velocityfield compare extremely well with other kinematically independentdistances.
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On the Hipparcos parallaxes of O stars
We compare the absolute visual magnitude of the majority of bright Ostars in the sky as predicted from their spectral type with the absolutemagnitude calculated from their apparent magnitude and the Hipparcosparallax. We find that many stars appear to be much fainter thanexpected, up to five magnitudes. We find no evidence for a correlationbetween magnitude differences and the stellar rotational velocity assuggested for OB stars by Lamers et al. (1997, A&A, 325, L25), whosesmall sample of stars is partly included in ours. Instead, by means of asimulation we show how these differences arise naturally from the largedistances at which O stars are located, and the level of precision ofthe parallax measurements achieved by Hipparcos. Straightforwardlyderiving a distance from the Hipparcos parallax yields reliable resultsfor one or two O stars only. We discuss several types of bias reportedin the literature in connection with parallax samples (Lutz-Kelker,Malmquist) and investigate how they affect the O star sample. Inaddition, we test three absolute magnitude calibrations from theliterature (Schmidt-Kaler et al. 1982, Landolt-Börnstein; Howarth& Prinja 1989, ApJS, 69, 527; Vacca et al. 1996, ApJ, 460, 914) andfind that they are consistent with the Hipparcos measurements. AlthoughO stars conform nicely to the simulation, we notice that some B stars inthe sample of \citeauthor{La97} have a magnitude difference larger thanexpected.
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A radio and mid-infrared survey of northern bright-rimmed clouds
We have carried out an archival radio, optical and infrared wavelengthimaging survey of 44 Bright-Rimmed Clouds (BRCs) using the NRAO/VLA SkySurvey (NVSS) archive, images from the Digitised Sky Survey (DSS) andthe Midcourse Space eXperiment (MSX). The data characterise the physicalproperties of the Ionised Boundary Layer (IBL) of the BRCs. We haveclassified the radio detections as: that associated with the ionisedcloud rims; that associated with possible embedded Young Stellar Objects(YSOs); and that unlikely to be associated with the clouds at all. Thestars responsible for ionising each cloud are identified and acomparison of the expected ionising flux to that measured at the cloudrims is presented. A total of 25 clouds display 20 cm radio continuumemission that is associated with their bright optical rims. The ionisingphoton flux illuminating these clouds, the ionised gas pressure and theelectron density of the IBL are determined. We derive internal molecularpressures for 9 clouds using molecular line data from the literature andcompare these pressures to the IBL pressures to determine the pressurebalance of the clouds. We find three clouds in which the pressureexerted by their IBLs is much greater than that measured in the internalmolecular material. A comparison of external pressures around theremaining clouds to a global mean internal pressure shows that themajority of clouds can be expected to be in pressure equilibrium withtheir IBLs and hence are likely to be currently shocked byphotoionisation shocks. We identify one source which shows 20 cmemission consistent with that of an embedded high-mass YSO and confirmits association with a known infrared stellar cluster. This embeddedcluster is shown to contain early-type B stars, implying that at leastsome BRCs are intimately involved in intermediate to high mass starformation.Figure \ref{fig:images} and Table \ref{tbl:istars1} are only availablein electronic form at http://www.edpsciences.org
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A Galactic O Star Catalog
We have produced a catalog of 378 Galactic O stars with accuratespectral classifications that is complete for V<8 but includes manyfainter stars. The catalog provides cross-identifications with othersources; coordinates (obtained in most cases from Tycho-2 data);astrometric distances for 24 of the nearest stars; optical (Tycho-2,Johnson, and Strömgren) and NIR photometry; group membership,runaway character, and multiplicity information; and a Web-based versionwith links to on-line services.
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Triggered Star Formation in the W5 H II Region
Young, massive stars can have a profound effect on the surroundinginterstellar medium. The triggering of star formation by an H II regionexpanding into nearby molecular material is an example of this type ofinteraction. This paper presents a multiwavelength study of the W5star-forming region investigating the possibility of triggered starformation. The ionizing sources and the morphologies of the ionized andmolecular gas and the dust are examined. A population of YSOs isidentified. Statistical evidence for triggering of these YSOs isdiscussed in terms of the spatial dependence of the star formationefficiency and the clustering and correlation of the YSO sources withrespect to the molecular gas and the H II region. Evidence for directinteractions between the components is discussed, on both large scalesand the scale of individual objects. Timescales for the expansion of theH II region, triggering processes, and the ages of the YSOs are comparedto establish a plausible sequence of events.
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The Anatomy of the Perseus Spiral Arm: 12CO and IRAS Imaging Observations of the W3-W4-W5 Cloud Complex
Panoramic images of 12CO J = 1-0 and thermal dust emissions from theW3-W4-W5 region of the outer Galaxy are presented. These data andrecently published H I 21 cm line emission images provide a ~1'resolution perspective to the dynamics and thermal energy content of theinterstellar gas and dust components contained within a 9 deg arc of thePerseus spiral arm. We tabulate the molecular properties of 1560 cloudsidentified as closed surfaces within the l-b-v CO data cube at athreshold of 0.9 K T^{*}R . Relative surface densities of themolecular (28:1) and atomic (2.5:1) gas components determined within thearm and interarm velocity intervals demonstrate that the gas componentthat enters the spiral arm is predominantly atomic. Molecular cloudsmust necessarily condense from the compressed atomic material thatenters the spiral arm and are likely short lived within the interarmregions. From the distribution of centroid velocities of clouds, wedetermine a random cloud-to-cloud velocity dispersion of 4 km s-1 overthe width of the spiral arm but find no clear evidence within themolecular gas for streaming motions induced by the spiral potential. Thefar-infrared images are analyzed with the CO J = 1-0 and H I 21 cm lineemission. The enhanced UV radiation field from members of the Cas OB6association and embedded newborn stars provide a significant source ofheating to the extended dust component within the Perseus arm relativeto the quiescent cirrus regions. Much of the measured far-infrared flux(69% at 60 mu m and 47% at 100 mu m) originates from regions associatedwith star formation rather than the extended, infrared cirrus component.
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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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ICCD speckle observations of binary stars. XIX - an astrometric/spectroscopic survey of O stars
We present the results of a speckle interferometric survey made with theCHARA speckle camera and 4 m class telescopes of Galactic O-type starswith V less than 8. We can detect with the speckle camera binaries inthe angular separation range 0.035-1.5 arcsec with delta M less than 3,and we have discovered 15 binaries among 227 O-type systems. We combinedour results on visual binaries with measurements of wider pairs from theWashington Double Star Catalog and fainter pairs from the HipparcosCatalog, and we made a literature survey of the spectroscopic binariesamong the sample. We then investigated the overall binary frequency ofthe sample and the orbital characteristics of the known binaries.Binaries are common among O stars in clusters and associations but lessso among field and especially runaway stars. There are many triplesystems among the speckle binaries, and we discuss their possible rolein the ejection of stars from clusters. The period distribution of thebinaries is bimodal in log P, but we suggest that binaries with periodsof years and decades may eventually be found to fill the gap. The massratio distribution of the visual binaries increases toward lower massratios, but low mass ratio companions are rare among close,spectroscopic binaries. We present distributions of the eccentricity andlongitude of periastron for spectroscopic binaries with ellipticalorbits, and we find strong evidence of a bias in the longitude ofperiastron distribution.
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The Dominion Radio Astrophysical Observatory Galactic Plane Survey Pilot Project: The W3/W4/W5/HB 3 Region
The Dominion Radio Astrophysical Observatory, in collaboration withother sites, recently began a Galactic plane survey. The data from thepilot project for this survey are presented here. They cover theW3/W4/W5/HB 3 Galactic complex in the Perseus arm. Ten fields wereobserved to produce mosaic images of this region at two continuumfrequencies, 408 and 1420 MHz, as well as in the 21 cm spectral line ofatomic hydrogen at 127 velocities covering +55.5 to -153.9 km s-1. At1420 MHz (continuum and spectral line), an area of approximately 8 deg x6 deg (l x b) is imaged with a resolution of 1.'00 x 1.'14 (east-west bynorth-south) whereas, at 408 MHz, the coverage was 14 deg x 10 deg (l xb) with a resolution of 3.'5 x 4.'0 (east-west by north-south). Thespectral-line data cube constitutes the highest resolution atomichydrogen study of the entire complex to date. A wealth of large-scalefilaments, arcs, bubbles, and shells is revealed.
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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.
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Radio continuum emission from stars: a catalogue update.
An updated version of my catalogue of radio stars is presented. Somestatistics and availability are discussed.
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On the Connection Between Radial Systems of Dark Globules and Stellar Associations
We study the connection between radial systems of dark globules andstellar associations. It is shown that of the 17 systems of type 1 inTable 1 of [1] 16 radial systems are connected with known associations.A new association is found (missing from the catalogs) connected withthe remaining system (System No. 2). Four systems of the six systems oftype 2 (Table 2 of [1]) are connected with known associations. A newmethod of determining the distance to associations is proposed, usingthe mean linear thickness of dark globules of radial systems connectedwith these associations as the criterion for distance. Using this methodwe make the distance to the association Cyg OB 9 more precise and answerthe question whether several radial systems belong to the correspondingstellar associations.
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Intrinsic colour indices of O- and B- type stars in the Vilnius photometric system.
Not Available
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Distribution and motions of OB stars in the direction of H and KHI Perseus.
Not Available
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Radial Systems of Dark Globules - Part One
Not Available
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A survey of radio emission from Galactic OB stars
Radio continuum observations of 88 O-type and early B-type stars areexamined. Results are presented for a subset of these stars which formsa distance-limited sample of all OB stars within 2.5 kpc of the sun.Mass loss rates are derived for HD 15570, HD 166734, HD 151804, HD152408, Alpha Cam, HD 169454, and Zeta Sco. All of these very luminousOB stars are found to be losing mass at a rate on the order of 10 to the-5 solar masses/yr. Multifrequency observations confirm the free-freeinterpretation for Zeta Pup and provide evidence for variability in thefree-free sources P Cygni and Cyg OB2 No. 12.
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H-alpha as a tracer of mass loss from OB stars
This paper investigates the use of the H-alpha emission from stellarwinds of OB stars to determine the stellar mass-loss rate. The power inH-alpha emitted by the wind can be parameterized in terms of thetemperature and the density field of the wind. A simple expression isderived which relates the observed H-alpha luminosity to the stellarmass-loss rate, the stellar radius, the velocity law, and the stellareffective temperature. This expression is calibrated for the influenceof the velocity law using a sample of Galactic OB stars with UVmass-loss rates. Consequently, the results depend on the validity of theUV rates. The derived velocity law for O stars turns out to be inagreement with the radiation-pressure-driven wind theory. There isevidence for a dependence of the velocity-law gradient on spectral type.The results for B stars, however, are more uncertain due to thedependence on the adopted mass accretion rate/L relation. Application ofthe calibrated H-alpha luminosity/mass-loss rate relation to a sample of149 galactic OB stars shows that mass accretion rate can be reliablydetermined from H-alpha. Due to the moderate amount of observing timerequired to derive mass accretion rate from H-alpha, this method may beapplied successfully to investigate mass-loss effects in extra-Galacticstars.
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The kinematical and binary properties of association and field O stars
A catalog of 195 Galactic O-type stars brighter than V = 8.0 mag hasbeen compiled to compare the velocity distribution and binary frequencyamong cluster and association, field, and runaway stars. Both the fieldstars and runaway stars have a larger dispersion in peculiar radialvelocity, a more positive mean peculiar radial velocity, and a widerz-distribution than stars found in clusters and associations, which isconsistent with the ejection of field and runaway stars from theirbirthplaces in associations. Visual binaries are common among stars inclusters and associations, but their incidence is a factor of 2 loweramong field stars, and they are absent in the runaway stars. Similarly,there is a deficiency of spectroscopic binaries among field stars, andespecially the runaway stars, relative to the numbers found in clustersand associations. Many of these properties can be understood in terms ofejection through close gravitational interactions with binary starsduring an early high number density epoch in the evolution of clusters.
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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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Catalog of O-B stars observed with Tokyo Meridian Circle
A catalog of the O-B stars, selected from 'Blaauw-Parenago' list andRubin's catalog, has been compiled on the FK4 system by the observationsmade with Gautier 8-inch Meridian Circle at the Tokyo AstronomicalObservatory during the period, 1971 to 1979. It contains 1059 stars andwas compiled for the future establishment of high precision propermotions of O-B stars.
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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.
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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.
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Catalog of BV magnitudes and spectral classes of 6000 stars
The present catalog, compiled at the Abastumani Observatory, contains BVmagnitudes and spectral classes of about 6000 stars up to V(lim) = 13.0min five circular areas of 18 sq deg located near the salactic-equatorplane. The catalog is intended for star-statistics studies ofstar-formation regions.
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Mass loss rates for northern OB-stars
A mass loss survey of 44 O- and early B-type stars in northern OBassociations is presented. For 22 stars mass loss rates were derivedfrom H-alpha equivalent widths using the method of Klein and Castor(1978). For 15 stars upper limits of the mass loss rates were estimated.For the remaining 7 stars H-alpha and H-beta equivalent width values aregiven but no quantitative evaluation of M-dot was possible. The resultsare compared with present ideas concerning the relation between massloss and other basic stellar parameters.
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Additional Variable Stars in the Northern Luminous Stars Catalogues
Not Available
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Kinematic properties of supergiants in the Perseus spiral arm
Analysis of the space motions of supergiants in the Perseus arm regionindicates that the stellar peculiar-velocity field has a large-scalenonuniformity probably resulting both from the presence of sizablegroups of young stars and from systematic motions in the arm aspredicted by density-wave theory. Proper motions are tabulated for 78stars.
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The structure of bright-rimmed molecular clouds
High spatial resolution, 30 arcsec observations of bright-rimmedmolecular clouds in the J = 2-1 and J = 1-0 lines of (C-12)O and (C-13)Oare presented, and their physical and kinematical properties areexamined. The clouds are individually discussed, showing contour mapsand profiles. The physical properties of the rims, their spatial extent,velocity, density, and temperature structure, and the variation ofmolecular abundances across them are considered. In general, the gasdensities increase close to the rims, but temperature enhancements occurover comparatively extended regions. Near the rims the gas kinematics isvaried: velocity gradients are observed in several regions, and in IC1396 line broadening is distinguishable. There is a definite decline inCO abundance near the well-resolved rim in NGC 1977. In none of theclouds does interaction with the adjacent H II region appear to havesubstantially affected the course of star formation.
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Neutral hydrogen in the CAS OB6 association
The present investigation of neutral hydrogen distribution andkinematics around the H II regions W 3, W 4, and W 5, as well as the SNRHB3 (which belongs to the Cas OB6 association), has discovered thedevelopment of an expanding neutral shell around W 4 which suggests thatW 4 is the oldest H II region in the association. The neutral shellexpansion is of the blister type, and on a scale of 50-100 pc, due toits location at the edge of a large neutral and molecular cloud complex.The shell has reached W 3 in the west, and may have initiated starformation, while tunnels direct away from the W 4 cavity towards W 5 inthe east, where an expanding shell has begun to form.
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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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Four-color and H-beta photometry for O-A0 type stars in three regions near the galactic equator
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1982A&AS...49..561W&db_key=AST
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