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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.
| Cepheid Masses: FUSE Observations of S Muscae
S Mus is the Cepheid with the hottest known companion. The largeultraviolet flux means that it is the only Cepheid companion for whichthe velocity amplitude could be measured with the echelle mode of theHST GHRS. Unfortunately, the high temperature is difficult to constrainat wavelengths longer than 1200 Å because of the degeneracybetween temperature and reddening. We have obtained a FUSE spectrum inorder to improve the determination of the temperature of the companion.Two regions that are temperature sensitive near 16,000 K but relativelyunaffected by H2 absorption (940 Å and the Lyβwings) have been identified. By comparing FUSE spectra of S Mus B withspectra of standard stars, we have determined a temperature of17,000+/-500 K. The resulting Cepheid mass is 6.0+/-0.4Msolar. This mass is consistent with main-sequenceevolutionary tracks with a moderate amount of convective overshoot.Based on observations made with the NASA-CNES-CSA Far UltravioletSpectroscopic Explorer satellite. FUSE is operated for NASA by JohnsHopkins University, under NASA contract NAS5-32985.
| FUSE Measurements of Far-Ultraviolet Extinction. I. Galactic Sight Lines
We present extinction curves that include data down to far-ultravioletwavelengths (FUV; 1050-1200 Å) for nine Galactic sight lines. TheFUV extinction was measured using data from the Far UltravioletSpectroscopic Explorer. The sight lines were chosen for their unusualextinction properties in the infrared through the ultraviolet; that theyprobe a wide range of dust environments is evidenced by the large spreadin their measured ratios of total to selective extinction,RV=2.43-3.81. We find that extrapolation of the Fitzpatrick& Massa relationship from the ultraviolet appears to be a goodpredictor of the FUV extinction behavior. We find that predictions ofthe FUV extinction based on the Cardelli, Clayton, & Mathis (CCM)dependence on RV give mixed results. For the seven extinctioncurves well represented by CCM in the infrared through ultraviolet(x<8 μm-1), the FUV extinction is well predicted inthree sight lines, overpredicted in two sight lines, and underpredictedin two sight lines. A maximum entropy method analysis using a simplethree-component grain model shows that seven of the nine sight lines inthe study require a larger fraction of grain materials to be in dustwhen FUV extinction is included in the models. Most of the added grainmaterial is in the form of small (radii <~ 200 Å) grains.Based on observations with the NASA-CNES-CSA Far UltravioletSpectroscopic Explorer, which is operated by the Johns HopkinsUniversity under NASA contract NAS5-32985.
| Far Ultraviolet Spectroscopic Explorer Snapshot Survey of O VI Variability in the Winds of 66 OB-Type Stars
We have used the Far Ultraviolet Spectroscopic Explorer to conduct asnapshot survey of O VI variability in the winds of 66 OB-type stars inthe Galaxy and the Magellanic Clouds. These time series consist of twoor three observations separated by intervals ranging from a few days toseveral months. Although these time series provide the bare minimum ofinformation required to detect variations, this survey demonstrates thatthe O VI doublet in the winds of OB-type stars is variable on variousscales in both time and velocity. For spectral types from O3 to B1, 64%vary in time. At spectral types later than B1, no wind variability isobserved. In view of the limitations of this survey, this fractionrepresents a lower limit on the true incidence of variability in the OVI wind lines, which is very common and probably ubiquitous. Incontrast, for S IV and P V, only a small percentage of the whole sampleshows wind variations, although this may be principally due to selectioneffects. The observed variations extend over several hundreds ofkilometers per second of the wind profile and can be strong. The widthover which the wind O VI profile varies is only weakly correlated withthe terminal velocity (v&infy;), but a significantcorrelation (close to a 1:1 relationship) is derived between the maximumvelocity of the variation and v&infy;. High-velocity O VIwind absorption features (possibly related to the discrete absorptioncomponents seen in other wind lines) are also observed in 46% of thecases for spectral types from O3 to B0.5. These features are variable,but the nature of their propagation cannot be determined from thissurvey. If X-rays can produce sufficient O VI by Auger ionization of OIV and the X-rays originate from strong shocks in the wind, this studysuggests that stronger shocks occur more frequently nearv&infy;, causing an enhancement of O VI nearv&infy;.
| 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.
| Absolute proper motions of open clusters. I. Observational data
Mean proper motions and parallaxes of 205 open clusters were determinedfrom their member stars found in the Hipparcos Catalogue. 360 clusterswere searched for possible members, excluding nearby clusters withdistances D < 200 pc. Members were selected using ground basedinformation (photometry, radial velocity, proper motion, distance fromthe cluster centre) and information provided by Hipparcos (propermotion, parallax). Altogether 630 certain and 100 possible members werefound. A comparison of the Hipparcos parallaxes with photometricdistances of open clusters shows good agreement. The Hipparcos dataconfirm or reject the membership of several Cepheids in the studiedclusters. Tables 1 and 2 are only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| 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.
| The HI distribution in the environment of the WR star HD 50896
The neutral matter distribution from the interstellar medium (ISM)located in the vicinity of the galactic Wolf-Rayet (WR) star HD 50896has been examined by means of HI 21-cm line observations obtained withboth low [half-power beamwidth (HPBW)~=34 arcmin] and intermediate(HPBW~=9 arcmin) angular resolution. The most interesting discovery is ahuge ovoidal HI minimum spanning the velocity range +1.5 to +10.0 kms^-1, created, very likely, by the joint action of the progenitor of HD50896 and the WR itself. Inside this cavity, two minima are clearlydiscernible. The WR star is offset with respect to either thegeometrical centre of the main HI void or the inner HI minima. Aphysical link between S308, the ring nebula associated with HD 50896,and one of the HI minima is suggested by our data. A kinematicaldistance of ~1 kpc for HD 50896 is derived based on the radial velocityof the HI cavity. The dual HI minimum geometry observed inside the mainHI cavity, a feature also seen in the HI distribution of the ISM locatedclose to other galactic WR stars, may be a consequence of theinteraction process itself. The ovoidal shape of the main cavity cannotbe explained within the framework of the standard interstellar bubbletheory. Elongated bubbles may result when the large-scale galacticmagnetic field is taken into account.
| An Einstein Observatory SAO-based catalog of B-type stars
About 4000 X-ray images obtained with the Einstein Observatory are usedto measure the 0.16-4.0 keV emission from 1545 B-type SAO stars fallingin the about 10 percent of the sky surveyed with the IPC. Seventy-fourdetected X-ray sources with B-type stars are identified, and it isestimated that no more than 15 can be misidentified. Upper limits to theX-ray emission of the remaining stars are presented. In addition tosummarizing the X-ray measurements and giving other relevant opticaldata, the present extensive catalog discusses the reduction process andanalyzes selection effects associated with both SAO catalog completenessand IPC target selection procedures. It is concluded that X-rayemission, at the level of Lx not less than 10 exp 30 ergs/s, is quitecommon in B stars of early spectral types (B0-B3), regardless ofluminosity class, but that emission, at the same level, becomes lesscommon, or nonexistent, in later B-type stars.
| 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.
| 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).
| Photometric search for Ap-stars in open cluster. IV - NGC 2287, CR 121, NGC 2422 and supplementary measurements in NGC 1662 and NGC 2516
Additional results are presented concerning the search for Ap-stars inopen clusters with the photoelectric peculiarity index Delta-a (Maitzen,1976). NGC 2287-56, NGC 2422-P3, and NGC 1662-4 are found to beCP2-stars as members in their respective clusters. The findings indicatethat HD 51088, which is also peculiar according to its Delta-a value,may be a member of one of the two very young star concentrationspreviously called Cr 121. It is determined that there is only a smallprobability for HD 49333 to be a member of NGC 2287, and that HD 49333is very likely to be a CP4 ( = He weak) star with a Delta-a significantfor peculiarity. It was necessary to reject 10 other stars with reportedindications of peculiarity as CP2 stars since their Delta-a values werenormal. It is concluded that the frequency of peculiar objects is ratherlow in the actual sample considering the number of CP2 detections.
| 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.
| Collinder 121: a Young Southern Open Cluster Similar to H and χ Persei
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1967ApJ...149..107F&db_key=AST
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Observation and Astrometry data
| Constellation: | おおいぬ座 |
| Right ascension: | 06h54m41.20s |
| Declination: | -24°15'20.4" |
| Apparent magnitude: | 8.772 |
| Distance: | 564.972 parsecs |
| Proper motion RA: | -6.8 |
| Proper motion Dec: | 5 |
| B-T magnitude: | 8.599 |
| V-T magnitude: | 8.758 |
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