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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 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
| 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.
| 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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Datos observacionales y astrométricos
| Constelación: | Can Mayor |
| Ascensión Recta: | 06h53m27.58s |
| Declinación: | -24°06'42.5" |
| Magnitud Aparente: | 8.786 |
| Distancia: | 595.238 parsecs |
| Movimiento Propio en Ascensión Recta: | -4 |
| Movimiento Propio en Declinación: | 2.8 |
| B-T magnitude: | 8.724 |
| V-T magnitude: | 8.781 |
Catálogos y designaciones:
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