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A revisit to agglomerates of early-type Hipparcos stars
% We study the spatial structure and sub-structure of regions rich in{Hipparcos} stars with blue B_T-V_T colours. These regions, whichcomprise large stellar complexes, OB associations, and young openclusters, are tracers of on-going star formation in the Galaxy. TheDBSCAN (Density-Based Spatial Clustering of Applications with Noise)data clustering algorithm is used to look for spatial overdensities ofearly-type stars. Once an overdensity, ``agglomerate'', is identified,we carry out a data and bibliographic compilation of their star membercandidates. The actual membership in agglomerate of each early-type staris studied based on its heliocentric distance, proper motion, andprevious spectro-photometric information. We identify 35 agglomerates ofearly-type {Hipparcos} stars. Most of them are associated to previouslyknown clusters and OB associations. The previously unknown P Puppisagglomerate is subject of a dedicated study with Virtual Observatorytools. It is actually a new, nearby, young open cluster (d ˜ 470pc, age ˜ 20 Ma) with a clear radial density gradient. We list PPuppis and other six agglomerates (including NGC 2451 A, vdBH 23, andTrumpler 10) as new sites for substellar searches because of theiryouth, closeness, and spatial density. We investigate in detail thesub-structure in the Orion, CMa-Pup and Pup-Vel OB complexes(``super-agglomerates''). We confirm or discover some stellaroverdensities in the Orion complex, like the 25 Ori group, the Horseheadregion (including the σ Orionis cluster), and the η Orionisagglomerate. Finally, we derive accurate parallactic distances to thePleiades, NGC 2451 A, and IC 2391, describe several field early-typestars at d < 200 pc, and discuss the incompleteness of our search.
| The Structure and the Distance of Collinder 121 from Hipparcos and Photometry: Resolving the Discrepancy
We present further arguments that the Hipparcos parallaxes for some ofthe clusters and associations represented in the Hipparcos catalogshould be used with caution in the study of the Galactic structure. Ithas already been shown that the discrepancy between the Hipparcos andground-based parallaxes for several clusters including the Pleiades,Coma Ber, and NGC 6231 can be resolved by recomputing the Hipparcosastrometric solutions with an improved algorithm diminishing correlatederrors in the attitude parameters. Here we present new parallaxesobtained with this algorithm for another group of stars with discrepantdata-the galactic cluster Cr 121. The original Hipparcos parallaxes ledde Zeeuw et al. to conclude that Cr 121 and the surrounding associationof OB stars form a relatively compact and coherent moving group at adistance of ~=550-600 pc. Our corrected parallaxes reveal a differentspatial distribution of young stellar populace in this area. Both thecluster Cr 121 and the extended OB association are considerably moredistant (750-1000 pc), and the latter has a large depth probablyextending beyond 1 kpc. Therefore, not only are the recalculatedparallaxes in complete agreement with the photometric uvbyβparallaxes, but the structure of the field they reveal is no longer indiscrepancy with that found by the photometric method.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| New Estimates of the Solar-Neighborhood Massive Star Birthrate and the Galactic Supernova Rate
The birthrate of stars of masses >=10 Msolar is estimatedfrom a sample of just over 400 O3-B2 dwarfs within 1.5 kpc of the Sunand the result extrapolated to estimate the Galactic supernova ratecontributed by such stars. The solar-neighborhood Galactic-plane massivestar birthrate is estimated at ~176 stars kpc-3Myr-1. On the basis of a model in which the Galactic stellardensity distribution comprises a ``disk+central hole'' like that of thedust infrared emission (as proposed by Drimmel and Spergel), theGalactic supernova rate is estimated at probably not less than ~1 normore than ~2 per century and the number of O3-B2 dwarfs within the solarcircle at ~200,000.
| Catalog of Galactic OB Stars
An all-sky catalog of Galactic OB stars has been created by extendingthe Case-Hamburg Galactic plane luminous-stars surveys to include 5500additional objects drawn from the literature. This work brings the totalnumber of known or reasonably suspected OB stars to over 16,000.Companion databases of UBVβ photometry and MK classifications forthese objects include nearly 30,000 and 20,000 entries, respectively.
| The region of Collinder 121
The distribution of bright B-type stars in a field with a radius of5° centred at the Galactic open cluster Cr 121 is studied utilizingStrömgren and Hβ photometry. All PPM stars earlier thanspectral type A0 are used, revealing a loose nearby structure at adistance of 660-730pc, and a compact more distant group, which appearsto be a genuine cluster: Cr 121. Based on similar coordinates, distancesand positions on the colour-magnitude (CM) and Hertzsprung-Russell (HR)diagrams, 11 photometric cluster members are selected at a mean distanceof 1085(+/-41 standard error) pc. The results are discussed in the lightof both classical and Hipparcos points of view.
| A HIPPARCOS Census of the Nearby OB Associations
A comprehensive census of the stellar content of the OB associationswithin 1 kpc from the Sun is presented, based on Hipparcos positions,proper motions, and parallaxes. It is a key part of a long-term projectto study the formation, structure, and evolution of nearby young stellargroups and related star-forming regions. OB associations are unbound``moving groups,'' which can be detected kinematically because of theirsmall internal velocity dispersion. The nearby associations have a largeextent on the sky, which traditionally has limited astrometricmembership determination to bright stars (V<~6 mag), with spectraltypes earlier than ~B5. The Hipparcos measurements allow a majorimprovement in this situation. Moving groups are identified in theHipparcos Catalog by combining de Bruijne's refurbished convergent pointmethod with the ``Spaghetti method'' of Hoogerwerf & Aguilar.Astrometric members are listed for 12 young stellar groups, out to adistance of ~650 pc. These are the three subgroups Upper Scorpius, UpperCentaurus Lupus, and Lower Centaurus Crux of Sco OB2, as well as VelOB2, Tr 10, Col 121, Per OB2, alpha Persei (Per OB3), Cas-Tau, Lac OB1,Cep OB2, and a new group in Cepheus, designated as Cep OB6. Theselection procedure corrects the list of previously known astrometricand photometric B- and A-type members in these groups and identifiesmany new members, including a significant number of F stars, as well asevolved stars, e.g., the Wolf-Rayet stars gamma^2 Vel (WR 11) in Vel OB2and EZ CMa (WR 6) in Col 121, and the classical Cepheid delta Cep in CepOB6. Membership probabilities are given for all selected stars. MonteCarlo simulations are used to estimate the expected number of interloperfield stars. In the nearest associations, notably in Sco OB2, thelater-type members include T Tauri objects and other stars in the finalpre-main-sequence phase. This provides a firm link between the classicalhigh-mass stellar content and ongoing low-mass star formation. Detailedstudies of these 12 groups, and their relation to the surroundinginterstellar medium, will be presented elsewhere. Astrometric evidencefor moving groups in the fields of R CrA, CMa OB1, Mon OB1, Ori OB1, CamOB1, Cep OB3, Cep OB4, Cyg OB4, Cyg OB7, and Sct OB2, is inconclusive.OB associations do exist in many of these regions, but they are eitherat distances beyond ~500 pc where the Hipparcos parallaxes are oflimited use, or they have unfavorable kinematics, so that the groupproper motion does not distinguish it from the field stars in theGalactic disk. The mean distances of the well-established groups aresystematically smaller than the pre-Hipparcos photometric estimates.While part of this may be caused by the improved membership lists, arecalibration of the upper main sequence in the Hertzsprung-Russelldiagram may be called for. The mean motions display a systematicpattern, which is discussed in relation to the Gould Belt. Six of the 12detected moving groups do not appear in the classical list of nearby OBassociations. This is sometimes caused by the absence of O stars, but inother cases a previously known open cluster turns out to be (part of) anextended OB association. The number of unbound young stellar groups inthe solar neighborhood may be significantly larger than thoughtpreviously.
| Supplementary southern standards for UBV(RI)c photometry
We present UBV(RI)c photometry for 80 southern red and blue stars foruse as additional standards. The data are tied to the Johnson UBV andCousins (RI)c systems and extend the range of the available stars forcolor equation determination, especially in (U-B) for blue stars and(V-R) and (V-I) for red stars. Comparisons with published data are madeand particularly good agreement is found with Bessell for the red(Gliese) stars.
| An Interstellar Conduction Front within a Wolf-Rayet Ring Nebula Observed with the Goddard High Resolution Spectrograph
With the High Resolution Spectrograph aboard the Hubble Space Telescopewe obtained high signal-to-noise ratio (S/N >~ 200--600 per 17 km s-1resolution element) spectra of narrow absorption lines toward theWolf-Rayet star HD 50896. The ring nebula S308 that surrounds this staris thought to be caused by a pressure-driven bubble bounded bycircumstellar gas (most likely from a red supergiant or luminous bluevariable progenitor) pushed aside by a strong stellar wind. Ourobservation has shown for the first time that blueshifted (~70 km s-1relative to the star) absorption components of C IV and N V arise in aconduction front between the hot interior of the bubble and the coldshell of swept-up material. These lines set limits on models of theconduction front. Nitrogen in the shell appears to be overabundant by afactor 10. The P Cygni profiles of N V and C IV are variable, possiblybecause of a suspected binary companion to HD 50896.
| 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 distance to the Wolf-Rayet star HD 50896
We present high-resolution observations (R approximately equals105) of the interstellar Na I D lines in the spectra of 23stars which are close to HD 50896 on the plane of the sky, plus HD 50896itself. The results are parameterized by using simple cloud models. Weconfirm that HD 50896 lies beyond the cluster Cr 121 (which is in thesame line of sight), and estimate D approximately equals 1.8 kpc.
| The Spectrum of EZ Canis Majoris (HD 50896) to the Lyman Limit with the Hopkins Ultraviolet Telescope
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993ApJ...416..372M&db_key=AST
| The first linear polarization spectra of Wolf-Rayet stars in the ultraviolet - EZ Canis Majoris and Theta MUSCAE
During the 1990 December Astro-1 Space Shuttle mission,spectropolarimetry was conducted in the wavelength region from 1400 to3200 A of the Wolf-Rayet stars EZ CMa (WN5) and Theta Mus (WC6 + O9.5I)with the Wisconsin Ultraviolet Photo-Polarimeter Experiment. The UVpolarization of EZ CMa displays features which correspond to emissionlines. This indicates a large, about 0.8 percent, intrinsic UV-continuumpolarization, and provides further evidence that the wind of EZ CMa ishighly distorted. The polarization of Theta Mus does not change acrossemission lines, or the strong interstellar 2200 A feature. Thepolarization decreases smoothly to shorter wavelengths, at constantposition angle. The combined UV-optical polarization spectrum of ThetaMus can be described well with interstellar polarization following aSerkowski law.
| Uvby-beta observations of 528 type B stars with V between the 8th and 9th magnitude
The paper presents uvby-beta measurements of 528 type B stars selectedfrom the SAO Catalog on the basis of two criteria: the spectral types inthe range B3-B5 and mV between the 8th and the 9th magnitude. Reddeningindependent (c1) values are estimated from the spectral classificationand compared to the observed values. No systematic trend with observed(b-y), H-beta, or spectral type appears to be present, but the range of(c1) residuals is surprisingly large. A rather large part of the starshas small beta values, smaller than for the BIa supergiants. Only twoare classified as O stars and most of them have the suffix e, ne, ornne. Most beta values for the O type stars are slightly above the upperlimit of 2.585 m.
| 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.
| Broad-band photometry of selected southern ultraviolet-bright stars.
Not Available
| The evolution of low ionization QSO absorption systems
A CCD spectroscopic survey of Mg II and Mg I absorption lines in a C IVselected sample of 35 metal systems, observed toward 12 QSOs between z =1.1 and z = 2.1, is reported. Six Mg I and 10 Mg II absorption lines aredetected in 33 C IV clouds, and some peculiarities are noted. Thecomplex or asymmetric line profiles reveal that multiple components arepresent and that variations in the C IV/Mg II and Mg II/Mg I ratio mayoccur often from one component to another with a velocity separationless than the velocity resolution of about 100 km/s. Comparison with theMg II absorption-line statistics at z-bar = 0.5 implies that, at z-bar =1.6, there are more strong absorbers per unit z with W(2796) greaterthan 0.6 A and fewer weak absorbers. The evolutionary parameter gammaappears to depend on W(min): its value drops as W(min) is reduced and isnegative at W(min) = 0.15 A. This suggests a different redshiftevolution for the population of weak and strong Mg II absorbers.
| The ultraviolet spectrum and interstellar environment of HD 50896
Data from 92 high-resolution IUE 1150-3274-A spectra are compiled intables and graphs and analyzed in detail to characterize HD 50896 andits interstellar environment. Findings reported include unexceptionaldepletions in the low-velocity H I system, strong low-velocity lines(attributed to excitation in an H II region associated with HD 50896 atdistance 2-3 kpc), an absorption system blueshifted by about 30 km/sfrom the low-velocity gas (attributed to ring nebula S308), andhigh-velocity absorption systems with evidence of grain destruction(attributed to an old SNR).
| High-velocity interstellar gas in the line of sight to the Wolf-Rayet star HD 50896
The large shell of interstellar gas (IG) discovered toward HD 50896 byHeckathorn and Fesen (1984) is characterized on the basis ofhigh-dispersion IUE SWP and LWR spectra of 19 objects located within 4deg of HD 50896 (but outside the optical ring nebula S308) at distances0.6-2.9 kpc (compared to 1.5 kpc for HD 50896). The IG is found to havetwo components (at velocities -80 and -125 km/s), diameter 90 pc orgreater, and distance 1.0 + or - 0.2 kpc, demonstrating that it is notrelated to HD 50896 and suggesting that it is a highly evolved supernovaremnant associated with cluster Cr 121.
| High-velocity interstellar gas in the line-of-sight to HD 50896
Using high-dispersion IUE spectra, a large interstellar shell structurewas discovered in the line-of-sight to the Wolf-Rayet star HD 50896.Blue-shifted interstellar absorption lines indicative of high-velocitygas are present in the spectra of four B stars located up to 2 deg awayfrom HD 50896 and at a distance of 1000 to 1400 parsecs, suggesting alinear diameter for the structure of at least 40 parsecs. Thesehigh-velocity components, present only in the low ionization lines andexhibiting nearly cosmic abundances, can be interpreted as a heretoforeunknown and extremely old supernova remnant. The existence of such asupernova remnant potentially associated with HD 50896, a runawayWolf-Rayet star believed to have a compact companion, implies that HD50896 may be a binary in its second Wolf-Rayet phase of evolution.
| A survey of ultraviolet objects
An all-sky survey of ultraviolet objects is presented together with astatistical analysis that leads to the conclusion that there is asignificantly higher population of hot subdwarfs lying below themain-sequence than hitherto thought. The distribution of all ultravioletobjects, main sequence ultraviolet objects, and MK unclassifiedultraviolet objects are shown in galactic coordinates, and the absolutemagnitudes and color-color diagrams for these groups are presented.Scale heights are derived, giving values similar to planetary nebulaefor the hottest groups.
| Optical observations of ultraviolet objects. I - Spectral classification of 103 stars /l = 200-275 deg/
Results are presented of a program of spectral classification of 103stars originally selected as ultraviolet objects from TD-1 satellitephotometry with the S2/68 experiment. Most of the objects appear to bespectroscopically normal stars; the method of selection yielded a sampleof relatively unreddened B stars at distances up to about 2 kpc. Thisresult is compared with recent studies of the spatial distribution ofinterstellar extinction in the same regions of the sky.
| The region of NGC 2287 and CR 121
Intermediate band and H-beta observations of 135 stars in the regions ofthe clusters NGC 2287 and Cr 121 are discussed, and a luminositycalibration of photometric parameters for late G- to early K-type brightgiants and supergiants is introduced. Results indicate that NGC 2287 isat a distance of 740 pc, very little reddened, 100-million years old,and contains three or four G8-K2 bright giants and supergiants and ablue straggler. Cr 121 is 1.17 kpc distant, very little reddened, 1.5million years old and an extension of CMa OB1. Cr 121 contains a nearerconcentration of stars at the same distance as NGC 2287, and theassociation appears to be the same age as CMa OB1, although presequencestars may exist. Intermingling of stars in CMa OB2 and NGC 2287 is alsoconsidered possible, and a test of the calibration of two methods ofluminosity determination of early A-type stars using photometricparameters shows them to be entirely consistent.
| H-beta photometry of southern early-type stars
H-beta photoelectric photometry is presented for 209 southern hemisphereearly-type stars from the HD catalog with galactic latitudes /b/ greaterthan 6 deg. Four-color photometry exists for all these stars and MKtypes for most of them. Absolute magnitudes have been estimated for allbut the emission-line stars and distances from the sun and the galacticplane determined.
| Four colour photometry of southern early-type stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1978MNRAS.182..629K&db_key=AST
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Группы:
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Наблюдательные данные и астрометрия
| Созвездие: | Большой Пёс |
| Прямое восхождение: | 06h58m02.11s |
| Склонение: | -22°52'34.0" |
| Видимая звёздная величина: | 8.811 |
| Расстояние: | 588.235 парсек |
| Собственное движение RA: | -4.8 |
| Собственное движение Dec: | 3.8 |
| B-T magnitude: | 8.627 |
| V-T magnitude: | 8.796 |
Каталоги и обозначения:
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