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New Young Brown Dwarfs in the Orion Molecular Cloud 2/3 Region
Forty new low-mass members with spectral types ranging from M4 to M9have been confirmed in the Orion Molecular Cloud (OMC) 2/3 region.Through deep, I-, z'-, J-, H-, and K-band photometry of a20'×20' field in OMC 2/3, we selected browndwarf candidates for follow-up spectroscopy. Low-resolution far-red andnear-infrared spectra were obtained for the candidates, and 19 youngbrown dwarfs in the OMC 2/3 region are confirmed. They exhibit spectraltypes of M6.5-M9, corresponding to approximate masses of 0.075-0.015Msolar using the evolutionary models of Baraffe et al. Atleast one of these bona fide young brown dwarfs has strong H?emission, indicating that it is actively accreting. In addition, weconfirm 21 new low-mass members with spectral types of M4-M6,corresponding to approximate masses of 0.35-0.10 Msolar inOMC 2/3. By comparing pre-main-sequence tracks to the positions of themembers in the H-R diagram, we find that most of the brown dwarfs areless than 1 Myr, but find a number of low-mass stars with inferred agesgreater than 3 Myr. The discrepancy in the stellar and substellar agesis due to our selection of only low-luminosity sources; however, thepresence of such objects implies the presence of an age spread in theOMC 2/3 region. We discuss possible reasons for this apparent agespread.Some of the observations presented here were obtained at the MMTObservatory, Whipple Observatory, W. M. Keck Observatory, Las CampanasObservatory, Mount Graham International Observatory, and Apache PointObservatory. The MMT Observatory is a joint facility of the SmithsonianInstitution and the University of Arizona. The W. M. Keck Observatory isoperated as a scientific partnership among the California Institute ofTechnology, the University of California, and the National Aeronauticsand Space Administration. The W. M. Keck Observatory was made possibleby the generous financial support of the W. M. Keck Foundation. TheApache Point Observatory 3.5 m telescope is owned and operated by theAstrophysical Research Consortium. In addition, this publication makesuse of data products from the Two Micron All Sky Survey, which is ajoint project of the University of Massachusetts and the InfraredProcessing and Analysis Center/California Institute of Technology,funded by the National Aeronautics and Space Administration and theNational Science Foundation.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| An Infrared Spectroscopic Sequence of M, L, and T Dwarfs
We present a 0.6-4.1 μm spectroscopic sequence of M, L, and T dwarfs.The spectra have R≡λ/Δλ~2000 from 0.9 to 2.4μm and R=2500-200 from 2.9 to 4.1 μm. These new data nearly doublethe number of L and T dwarfs that have reported L-band spectra. Thenear-infrared spectra are combined with previously published red-opticalspectra to extend the wavelength coverage to ~0.6 μm. Prominentatomic and molecular absorption features are identified includingneutral lines of Al, Fe, Mg, Ca, Ti, Na, and K and 19 new weakCH4 absorption features in the H-band spectra of mid- tolate-type T dwarfs. In addition, we detect for the first time the 0-0band of the A 4Π-X 4Σ-transition of VO at ~1.06 μm in the spectra of L dwarfs and the P-and R-branches of the ν3 band of CH4 in thespectrum of a T dwarf. The equivalent widths of the refractory atomicfeatures all decrease with increasing spectral type and are absent by aspectral type of ~L0, except for the 1.189 μm Fe I line, whichpersists to at least ~L3. We compute the bolometric luminosities of thedwarfs in our sample with measured parallaxes and find good agreementwith previously published results that use L'-band photometry to accountfor the flux emitted from 2.5 to 3.6 μm. Finally, 2MASSJ2224381-0158521 (L4.5) has an anomalously red spectrum and thestrongest Δν=+2 CO bands in our sample. This may be indicativeof unusually thick condensate clouds and/or low surface gravity.Based in part on data collected at Subaru telescope, which is operatedby the National Astronomical Observatory of Japan.
| Radial velocities. Measurements of 2800 B2-F5 stars for HIPPARCOS
Radial velocities have been determined for a sample of 2930 B2-F5 stars,95% observed by the Hipparcos satellite in the north hemisphere and 80%without reliable radial velocity up to now. Observations were obtainedat the Observatoire de Haute Provence with a dispersion of 80Ä,mm(-1) with the aim of studying stellar and galactic dynamics.Radial velocities have been measured by correlation with templates ofthe same spectral class. The mean obtained precision is 3.0 km s(-1)with three observations. A new MK spectral classification is estimatedfor all stars. Based on observations made at the Haute ProvenceObservatory, France and on data from The Hipparcos Catalogue, ESA.Tables 4, 5 and 6 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr or viahttp://cdsweb.u-strasbg.fr/Abstract.htm
| A study of some stars with circumstellar dust envelopes. I
We present the results of a study of circumstellar dust envelopes of 36stars of early(O-B-A) types in the directions of the associations CasOB1, Cas OB2, Per OB1, and Ori OB1. We determine the absorption at 1640Å, the linear radius of the dust envelopes, the mean value of thecoefficient k, and the masses of the envelopes. They differsignificantly from one another.
| Far-ultraviolet stellar photometry: A field in Orion
Far-ultraviolet photometry for 625 objects in Orion is presented. Thesedata were extracted from electrographic camera images obtained duringsounding rocket flights in 1975 and 1982. The 1975 images were centeredclose to the belt of Orion while the 1982 images were centeredapproximately 9 deg further north. One hundred and fifty stars fell inthe overlapping region and were observed with both cameras. Sixty-eightpercent of the objects were tentatively identified with known starsusing the SIMBAD database while another 24% are blends of objects tooclose together to separate with our resolution. As in previous studies,the majority of the identified ultraviolet sources are early-type stars.However, there are a significant number for which no such identificationwas possible, and we suggest that these are interesting objects whichshould be further investigated. Seven stars were found which were brightin the ultraviolet but faint in the visible. We suggest that some ofthese are nearby white dwarfs.
| 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.
| The Orion complex according to observations of the space telescope Glazar.
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.
| Stars of Early Types in the Region of Stellar Association OB1 Observed with the Glazar Telescope
Not Available
| The visually brightest early-type supergiants in the spiral galaxies NGC 2403, M81, and M101
Moderate-resolution spectroscopy of the candidate brightest blue starsin the nearby spirals NGC 2403, M81, and M101 reveals that many are notsingle stars, but compact H II regions, clusters, and multiple systems.This is an additional and serious limitation on their use as distanceindicators. The derivation of the luminosities of the confirmed singleblue supergiants is discussed, and, combining these results withprevious work on the brightest red supergiants, a brief discussion andcomparison of the evolution of their most massive stars are given. Theproperties of the brightest blue and red stars in NGC 2403 and M81 arebasically in agreement with the pattern of massive-star evolutionobserved in Local Group galaxies. The distance to M101 is stillcontroversial, but at the larger distance modulus, the luminosities ofits brightest early and late-type supergiants place them beyond theEddington limit for their initial mass and temperature.
| Spectroscopic studies of stars in ORI OB1 /Belt/
MK spectral classifications are presented for 120 B- and A-type stars inthe Belt subgroup of the Ori OB1 association. Combined with otherpublished spectroscopic data, and the assumed absolute magnitudes givenby Schmidt-Kaler (1965) and Lesh (1979), a mean corrected distancemodulus of 8.56 + or - 0.11 is computed for the eastern region, whilefor the remainder of the Belt a modulus of 8.20 + or - 0.05 is derived.Several B9-A2 subgiants and A7-F0 main-sequence stars were observed inthe western and central regions of the Belt. The ages of these starsimply a spread in formation ages for these subgroups from about 1million yr to at least 10 million yr.
| 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
| Two sparse open clusters in the region of Collinder 132.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977PASP...89..803C&db_key=AST
| Spectral types in the ORI OB1 association.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977PASP...89..797A&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.
| KURZE MITTEILUNG. Zur Expansion der Assoziation Cep III
Not Available
| The Meridian Proper Motions of 161 Stars in the Region of the Belt of Orion.
Not Available
| Two-Dimensional Spectral Classification by Narrow-Band Photometry for B Stats in Clusters and Associations.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1958ApJ...128..185C&db_key=AST
| A Study of the Orion Aggregate of Early-Type Stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1952ApJ...116..251S&db_key=AST
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Besorolás csoportokba:
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Pozíciós és asztrometriai adatok
| Csillagkép: | Orion |
| Rektaszcenzió: | 05h41m36.04s |
| Deklináció: | -03°43'52.3" |
| Vizuális fényesség: | 7.726 |
| Távolság: | 188.324 parszek |
| RA sajátmozgás: | 16.6 |
| Dec sajátmozgás: | -9.9 |
| B-T magnitude: | 7.721 |
| V-T magnitude: | 7.726 |
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