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A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun
Traditionally, runaway stars are O- and B-type stars with large peculiarvelocities. We would like to extend this definition to young stars (upto ?50 Myr) of any spectral type and to identify those present in theHipparcos catalogue by applying different selection criteria, such aspeculiar space velocities or peculiar one-dimensional velocities.Runaway stars are important for studying the evolution of multiple starsystems or star clusters, as well as for identifying the origins ofneutron stars. We compile the distances, proper motions, spectral types,luminosity classes, V magnitudes and B-V colours, and we utilizeevolutionary models from different authors to obtain star ages. We studya sample of 7663 young Hipparcos stars within 3 kpc from the Sun. Theradial velocities are obtained from the literature. We investigate thedistributions of the peculiar spatial velocity and the peculiar radialvelocity as well as the peculiar tangential velocity and itsone-dimensional components and we obtain runaway star probabilities foreach star in the sample. In addition, we look for stars that aresituated outside any OB association or OB cluster and the Galactic planeas well as stars for which the velocity vector points away from themedian velocity vector of neighbouring stars or the surrounding local OBassociation/cluster (although the absolute velocity might be small). Wefind a total of 2547 runaway star candidates (with a contamination ofnormal Population I stars of 20 per cent at most). Thus, aftersubtracting these 20 per cent, the runaway frequency among young starsis about 27 per cent. We compile a catalogue of runaway stars, which isavailable via VizieR.
| Masses and luminosities of O- and B-type stars and red supergiants
Massive stars are of interest as progenitors of supernovae, i.e.neutron stars and black holes, which can be sources of gravitationalwaves. Recent population synthesis models can predict neutron star andgravitational wave observations but deal with a fixed supernova rate oran assumed initial mass function for the population of massive stars. Here we investigate those massive stars, which are supernovaprogenitors, i.e. with O- and early B-type stars, and also allsupergiants within 3 kpc. We restrict our sample to those massive starsdetected both in 2MASS and observed by Hipparcos, i.e. only those starswith parallax and precise photometry. To determine the luminositieswe calculated the extinctions from published multi-colour photometry,spectral types, luminosity class, all corrected for multiplicity andrecently revised Hipparcos distances. We use luminosities andtemperatures to estimate the masses and ages of these stars usingdifferent models from different authors. Having estimated theluminosities of all our stars within 3 kpc, in particular for all O- andearly B-type stars, we have determined the median and mean luminositiesfor all spectral types for luminosity classes I, III, and V. Ourluminosity values for supergiants deviate from earlier results: Previouswork generally overestimates distances and luminosities compared to ourdata, this is likely due to Hipparcos parallaxes (generally moreaccurate and larger than previous ground-based data) and the fact thatmany massive stars have recently been resolved into multiples of lowermasses and luminosities. From luminosities and effective temperatureswe derived masses and ages using mass tracks and isochrones fromdifferent authors. From masses and ages we estimated lifetimes andderived a lower limit for the supernova rate of ?20 events/Myraveraged over the next 10 Myr within 600 pc from the sun. These data arethen used to search for areas in the sky with higher likelihood for asupernova or gravitational wave event (like OB associations).
| A CCD Search for Variable Stars of Spectral Type B in the Northern Hemisphere Open Clusters. VII. NGC 1502
We present results of variability search in the field of the young opencluster NGC 1502. Eight variable stars were discovered. Of six otherstars in the observed field that were suspected for variability, weconfirm variability of two, including one ? Cep star, NGC 1502-26.The remaining four suspects were found to be constant in our photometry.In addition, UBVIC photometry of the well-known massiveeclipsing binary SZ Cam was obtained.The new variable stars include: two eclipsing binaries of which one is arelatively bright detached system with an EA-type light curve, an?2 CVn-type variable, an SPB candidate, a field RR Lyrstar and three other variables showing variability of unknown origin.The variability of two of them is probably related to their emission inH?, which has been measured by means of the ? index obtainedfor 57 stars brighter than V?16 mag in the central part of theobserved field. Four other non-variable stars with emission in H?were also found.Additionally, we provide VIC photometry for stars down toV=17 mag and UB photometry for about 50 brightest stars in the observedfield. We also show that the 10 Myr isochrone fits very well theobserved color-magnitude diagram if a distance of 1 kpc and meanreddening, E(V-IC)=0.9 mag are adopted.
| Stellar Rotation in Young Clusters. II. Evolution of Stellar Rotation and Surface Helium Abundance
We derive the effective temperatures and gravities of 461 OB stars in 19young clusters by fitting the Hγ profile in their spectra. We usesynthetic model profiles for rotating stars to develop a method toestimate the polar gravity for these stars, which we argue is a usefulindicator of their evolutionary status. We combine these results withprojected rotational velocity measurements obtained in a previous paperon these same open clusters. We find that the more massive B starsexperience a spin-down as predicted by the theories for the evolution ofrotating stars. Furthermore, we find that the members of binary starsalso experience a marked spin-down with advanced evolutionary state dueto tidal interactions. We also derive non-LTE-corrected heliumabundances for most of the sample by fitting the He Iλλ4026, 4387, 4471 lines. A large number of heliumpeculiar stars are found among cooler stars withTeff<23,000 K. The analysis of the high-mass stars (8.5Msolar
| Stellar Rotation in Young Clusters. I. Evolution of Projected Rotational Velocity Distributions
Open clusters offer us the means to study stellar properties in sampleswith well-defined ages and initial chemical composition. Here we presenta survey of projected rotational velocities for a large sample of mainlyB-type stars in young clusters to study the time evolution of therotational properties of massive stars. The survey is based onmoderate-resolution spectra made with the WIYN 3.5 m and CTIO 4 mtelescopes and Hydra multi-object spectrographs, and the target starsare members of 19 young open clusters with an age range of approximately6-73 Myr. We made fits of the observed lines He I λλ4026,4387, 4471, and Mg II λ4481, using model theoretical profiles tofind projected rotational velocities for a total of 496 OB stars. Wefind that there are fewer slow rotators among the cluster B-type starsrelative to nearby B stars in the field. We present evidence consistentwith the idea that the more massive B stars (M>9 Msolar)spin down during their main-sequence phase. However, we also find thatthe rotational velocity distribution appears to show an increase in thenumbers of rapid rotators among clusters with ages of 10 Myr and higher.These rapid rotators appear to be distributed between the zero age andterminal age main-sequence locations in the Hertzsprung-Russell diagram,and thus only a minority of them can be explained as the result of aspin-up at the terminal age main sequence due to core contraction. Wesuggest instead that some of these rapid rotators may have been spun upthrough mass transfer in close binary systems.
| The Stars in Camelopardalis OB1: Their Distance and Evolutionary History
An investigation is undertaken of the optically identified Population Iobjects in the Cam OB1 region. From the analysis of these objects it isdetermined that the distance to the Cam OB1 stars is 975+/-90 pc. Atheoretical H-R diagram for the Cam OB1 stars reveals that starformation has been going on in the region for1×106-1×108 yr. At present, the mostactive site of star formation is Cam R1, which shows an asymmetry in thedistribution of optically identified Population I objects. The majorityof the pre-main-sequence stars lie in the northern half of theassociation, while the main-sequence stars and evolved stars lie in thesouthern half.
| 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
| Cross Identification in the Region of Cluster NGC 1502
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....114..222W&db_key=AST
| Ultraviolet Imaging Telescope Near-Ultraviolet Bright Object Catalog
We present a photometric catalog of 2244 objects detected by theUltraviolet Imaging Telescope in the near-ultraviolet (NUV; 1650A <λ < 2900 A) during the Astro Space Shuttle mission. Sources inthe catalog are as faint as m_nuv_ ~ 18.8, or f_nuv_ ~ 1.1 x 10^16^ ergss^-1^ cm^-2^ A^-1^, but the survey is not complete to this level.Optical catalogs were used to cross identify sources and derive NUV - Vcolors. A majority of the objects (88%) do indeed have proposed opticalidentifications from catalogs, and most are stars. Our purpose increating the catalog is to form a database useful for identifying veryblue objects and performing Galactic UV stellar population studies.
| UVBY and beta photometry for stars in the open cluster NGC 1502
New uvby and beta photoelectric photometry has been obtained for starsin NGC 1502, a young open cluster with relatively high interstellarreddening. It is shown that some of the previous published data for thecluster suffer from small systematic errors. After correction forzero-point differences, the previous data have been combined with thenew data and accurate values of the interstellar reddening (E(b-y) =0.54 mag) and distance modulus (V0 - Mv = 9.71mag) have been obtained. These are compared with similar valuescalculated from published UBV photometry and MK spectral types, whichagree well with the uvby(beta) analysis. It is found that the reddeningis not variable over the cluster field, contrary to previous estimates.The fact that systematic errors exist in precise photometry highlightsthe importance of a careful selection of standard stars in anyphotometry of reddened B-type stars.
| Ubvy + H-beta photometry of the young open clusters NGC 1502 and NGC 2169
This study presents results of a ubvy + H-beta photometric investigationof 22 and 14 stars, in the fields of NGC 1502 and NGC 2169,respectively, including new H-beta measurements for the 22 stars in NGC1502. A comparison with the findings of Perry et al. (1978) and Reimannand Pfau (1987) is discussed, with particular attention to the presenceof systematic errors present in the sequences of instrumental andstandard values. The membership of the observed stars is discussed onthe basis of the available photometric and radial velocity data.
| Near-infrared and Stromgren photometry of the open clusters NGC 663, NGC 1502 and NGC 1893
Observational data are presented regarding the three objects includingnear-IR JHK, Stromgren uvby, and H-beta photometry of the centralregions. The intrinsic photometric colors of average main-sequence starsare taken from previous studies to examine the data with m1 vs. b-y, c1vs. m1, beta vs. c1, J-H vs. H-K, and V-K vs. b-y diagrams. It isdetermined that the ages of and distance to NGC 663, NGC 1502, and NGC1893 are respectively 9 x 10 exp 6 yr and 2.5 kpc, 5 x 10 exp 6 yr and1.5 kpc, and 4 x 10 exp 6 yr and 4.3 kpc. The results indicate otherparameters, and considerable differental reddening is noted across NGC663. The total-to-selective extinction ratio is also examined showingthat it is smaller than the galactic value towards NGC 663 and 1893 andsignificantly lower than the average value for the ISM in NGC 1502. Itis concluded that the size distribution of the dust particles in thepresent line-of-sight has an inherent bias.
| Distance Moduli of Open Clusters.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1965ApJS...12..215H&db_key=AST
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| Takýmyýldýz: | Zurafa |
| Sað Açýklýk: | 04h07m51.76s |
| Yükselim: | +62°16'29.7" |
| Görünürdeki Parlaklýk: | 10.78 |
| özdevim Sað Açýklýk: | -0.3 |
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| B-T magnitude: | 11.376 |
| V-T magnitude: | 10.83 |
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