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The brightest stars of the σ Orionis cluster
Context: The very young σ Orionis cluster (~3 Ma) is a cornerstonein understanding the formation of stars and substellar objects down toplanetary masses. However, its stellar population is far from beingcompletely known. Aims: This study's purpose is to identify andcharacterise the most massive stars of σ Orionis to complementcurrent and future deep searches for brown dwarfs and planetary-massobjects in the cluster. Methods: I have cross-correlated thesources in the Tycho and 2MASS catalogues in a region of 30 arcminradius with its centre in the O-type star σ Ori A. In this area, Istudied the membership in the Ori OB 1b association of the brighteststars in the optical using astrometric, X-ray, and both infrared andoptical photometric data from public catalogues, and spectroscopic datafrom the literature. Results: A list of 26 young stars, fourcandidate young stars, and 16 probable foreground stars has arisen fromthe study. Seven young stars probably harbour discs (four are new).There is no mass dependence of the disc frequency in the cluster. I havederived the first mass spectrum for σ Orionis from 1.1 to 24M_ȯ (α = +2.0+0.2-0.1; roughlySalpeter-like). I also provide additional proof of the existence ofseveral spatially superimposed stellar populations in the direction ofσ Orionis. Finally, the cluster may be closer and older thanpreviously thought.
| Searching for links between magnetic fields and stellar evolution. I. A survey of magnetic fields in open cluster A- and B-type stars with FORS1
Context: .About 5% of upper main sequence stars are permeated by astrong magnetic field, the origin of which is still matter of debate. Aims: . With this work we provide observational material to studyhow magnetic fields change with the evolution of stars on the mainsequence, and to constrain theory explaining the presence of magneticfields in A and B-type stars. Methods: . Using FORS1 inspectropolarimetric mode at the ESO VLT, we have carried out a survey ofmagnetic fields in early-type stars belonging to open clusters andassociations of various ages. Results: . We have measured themagnetic field of 235 early-type stars with a typical uncertainty of 100 G. In our sample, 97 stars are Ap or Bp stars. For thesetargets, the median error bar of our field measurements was 80 G.A field has been detected in about 41 of these stars, 37 of which werenot previously known as magnetic stars. For the 138 normal A and B-typestars, the median error bar was 136 G, and no field was detected in anyof them.
| Ultra low-mass star and substellar formation in σ Orionis
The nearby young σ Orionis cluster (360 pc, 3 Myr) isbecoming one of the most important regions for the study of ultralow-mass star formation and its extension down to the mass regimes ofthe brown dwarfs and planetary-mass objects. Here, I introduce theσ Orionis cluster and present three studies that the {JOVIAN}group is developing: a pilot programme of near-infrared adaptive-opticsimaging of stars of the cluster, intermediate-resolution opticalspectroscopy of a large sample of stars of the cluster and a study ofthe mass function down to the planetary-mass domain. This paper is asummary of the content of four posters that I presented in the Ultralow-mass star formation and evolution Workshop, as single author or onbehalf of different collaborations.
| Herbig Ae/Be Stars in nearby OB Associations
We have carried out a study of the early-type stars in nearby OBassociations spanning an age range of ~3-16 Myr, with the aim ofdetermining the fraction of stars that belong to the Herbig Ae/Be class.We studied the B, A, and F stars in the nearby (<=500 pc) OBassociations Upper Scorpius, Perseus OB2, Lacerta OB1, and Orion OB1,with membership determined from Hipparcos data. We also included in ourstudy the early-type stars in the Trumpler 37 cluster, part of the CepOB2 association. We obtained spectra for 440 Hipparcos stars in theseassociations, from which we determined accurate spectral types, visualextinctions, effective temperatures, luminosities and masses, usingHipparcos photometry. Using colors corrected for reddening, we find thatthe Herbig Ae/Be stars and the classical Be (CBe) stars occupy clearlydifferent regions in the JHK diagram. Thus, we use the location on theJHK diagram, as well as the presence of emission lines and of strong 12μm flux relative to the visual, to identify the Herbig Ae/Be stars inthe associations. We find that the Herbig Ae/Be stars constitute a smallfraction of the early-type stellar population even in the youngerassociations. Comparing the data from associations with different agesand assuming that the near-infrared excess in the Herbig Ae/Be starsarises from optically thick dusty inner disks, we determined theevolution of the inner disk frequency with age. We find that the innerdisk frequency in the age range 3-10 Myr in intermediate-mass stars islower than that in the low-mass stars (<1 Msolar) inparticular, it is a factor of ~10 lower at ~3 Myr. This indicates thatthe timescales for disk evolution are much shorter in theintermediate-mass stars, which could be a consequence of more efficientmechanisms of inner disk dispersal (viscous evolution, dust growth, andsettling toward the midplane).
| Photometric Identification of the Low-Mass Population of Orion OB1b. I. The σ Orionis Cluster
We report an optical photometric survey of 0.89 deg2 of theOrion OB1b association centered on σ Ori. This region includesmost of the σ Ori cluster, the highest-density region within OrionOB1b. We have developed a statistical procedure to identify the young,low-mass, pre-main-sequence population of the association. We estimatethat the cluster has ~160 members in the mass range (0.2<=M<=1.0Msolar). The cluster has a radius of ~3-5 pc and an estimatedage of 2.5+/-0.3 Myr. We estimate that the total mass of the cluster is225+/-30 Msolar. This mass is similar to the estimated massof the ~5×105 yr old cluster NGC 2024. NGC 2024 andσ Ori appear to be a well-matched pair of clusters, except for the~2 Myr difference in their ages.
| Photoelectric Photometry of Stars in the Orion Standard Region
Magnitudes and color indices in the Vilnius seven-color photometricsystem are given for 108 stars in the Orion standard region around theOrion Belt and the star lambda Orionis. New spectral and luminosityclasses, estimated from the photometric data, are given for some of thestars.
| The Tokyo PMC catalog 90-93: Catalog of positions of 6649 stars observed in 1990 through 1993 with Tokyo photoelectric meridian circle
The sixth annual catalog of the Tokyo Photoelectric Meridian Circle(PMC) is presented for 6649 stars which were observed at least two timesin January 1990 through March 1993. The mean positions of the starsobserved are given in the catalog at the corresponding mean epochs ofobservations of individual stars. The coordinates of the catalog arebased on the FK5 system, and referred to the equinox and equator ofJ2000.0. The mean local deviations of the observed positions from theFK5 catalog positions are constructed for the basic FK5 stars to comparewith those of the Tokyo PMC Catalog 89 and preliminary Hipparcos resultsof H30.
| A search for Lambda Bootis stars in OB associations
A search for Lambda Bootis stars in two OB associations, Orion OB1 andLacerta OB1, has been carried out. One Lambda Bootis star has beendiscovered in the Orion OB1 association. In addition, nine A-type starswhich appear to be slightly metal weak have been found in the twoassociations. The Lambda Bootis star is situated on the Zero-Age MainSequence (ZAMS). The discovery of these stars strengthens the hypothesisthat the Lambda Bootis stars are related to a short-lived evolutionaryphase associated with the arrival of the star on the ZAMS.
| Liste des étoiles Ap et Am dans les amas ouverts (édition révisée)
Not Available
| Liste des étoiles Ap et Am dans les amas ouverts (Edition révisée)
Not Available
| 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.
| Catalog of AP and AM stars in open clusters
The previous results of Raab (1922), Markarian (1951), and Collinder(1931) have been used to catalog Ap and Am stars that are in the fieldof open clusters. Tabular data are presented for the clusterdesignation, the HD or HDE number, the right ascension (1900), thedeclination (1900), and the magnitude. Also listed are the spectraltypes and, for certain stars, the probability of cluster membership.
| A Photoelectric Search for Ap-Stars in the Orion Association
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1981A&A....94..134J&db_key=AST
| A photometric study of the Orion OB 1 association. III - Subgroup analyses
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1978ApJS...36..497W&db_key=AST
| A photometric study of the Orion OB 1 association. I - Observational data.
A catalog of observational data is presented for stars in the region ofthe young stellar association Orion OB 1. Photoelectric observationsobtained in the uvby-beta and UBV systems are compiled along withprevious photoelectric and spectroscopic data for all these stars aswell as for several bright members of the association with availablephotometric indices. Mean weighted values are computed for thephotometric data and summarized in tables expected to be reasonablycomplete for association members earlier than spectral type A0.Membership criteria are derived, and qualitative membershipprobabilities summarized, for the 526 stars in the final program. Theanalytical procedures are discussed for association stars of B,intermediate, and AF types. Effects of the nebular environment andvarious calibrations of Balmer-line and four-color indices areconsidered for the determination of absolute magnitudes for the B-typestars.
| Spectral classification in the belt of ORI OB1.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1976AJ.....81..537G&db_key=AST
| The Meridian Proper Motions of 161 Stars in the Region of the Belt of Orion.
Not Available
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Membre dels grups següents:
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Dades d'Observació i Astrometria
| Constel·lació: | Orion |
| Ascensió Recta: | 05h37m40.48s |
| Declinació: | -02°26'36.8" |
| Magnitud Aparent: | 8.498 |
| Distancia: | 396.825 parsecs |
| Moviment propi RA: | -3.3 |
| Moviment propi Dec: | -3.9 |
| B-T magnitude: | 8.616 |
| V-T magnitude: | 8.508 |
Catàlegs i designacions:
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