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A Multiwavelength Study of 1WGA J1346.5-6255: A New γ Cas Analog Unrelated to the Background Supernova Remnant G309.2-00.6
1WGA J1346.5-6255 is a ROSAT X-ray source found within the radio lobesof the supernova remnant (SNR) G309.2-00.6. It appears to coincide withthe bright and early-type star HD 119682, in the galactic open clusterNGC 5281. Its radio morphology, consisting of two brightened anddistorted arcs of emission on opposite sides of the 1WGA J1346.5-6255source and of a jetlike feature and break in the shell, suggest that1WGA J1346.5-6255/G309.2-00.6 is a young analog of the microquasarpowering the W50 nebula SS 433. This motivated us to study this sourceat X-ray and optical wavelengths. We present new Chandra observations of1WGA J1346.5-6255, archival XMM-Newton observations of G309.2-00.6, andoptical spectroscopic observations of HD 119682, to search for X-rayjets from 1WGA J1346.5-6255, study its association with the SNR, andtest for whether HD 119682 represents its optical counterpart. We findno evidence for jets from 1WGA J1346.5-6255 down to an unabsorbed fluxof 2.6×10-13 ergs cm-2 s (0.5-7.5 keV), werule out its association with G309.2-00.6, and we confirm that HD 119682is its optical counterpart. We derive a distance of 1.2+/-0.3 kpc,consistent with the distance estimate to NGC 5281 (1.3+/-0.3 kpc), andmuch smaller than the distance derived to G309.2-00.6. We discuss thenature of the source, unveil that HD 119682 is a Be star, and suggest itis a new member of the recently proposed group of γ Cas analogs.The Chandra and XMM-Newton X-ray light curves show variability ontimescales of hundreds of seconds, and the presence of a possible periodof ~1500 s that could be the rotational period of an accreting neutronstar or white dwarf in this γ Cas analog.
| Extraordinarily Hot X-Ray Emission from the O9 Emission-Line Star HD 119682
We present new optical and X-ray observations to show that the X-raysource 1WGA J1346.5-6255 previously associated with the SNR G309.2-0.6can be unequivocally identified with the emission-line star HD 119682located in the foreground open cluster NGC 5281. Images from Chandra inthe X-ray band as well as from Magellan in the narrow optical Hαband show a coincidence of the source positions within 0.5". The X-raysource appears extremely hot for an OB star identified as of O9.7e type.XMM-Newton spectra show plasma temperatures of 1 and >8 keV with anX-ray luminosity of (6.2+/-0.1)×1032 ergss-1. The optical and X-ray properties are very reminiscent ofthe prototype emission-line star γ Cas. We discuss theramifications of this similarity with respect to very early typeemission-line stars as a new class of hard X-ray sources.
| Proper motion determination of open clusters based on the UCAC2 catalogue
We present the kinematics of hundreds of open clusters, based on theUCAC2 Catalogue positions and proper motions. Membership probabilitieswere obtained for the stars in the cluster fields by applying astatistical method uses stellar proper motions. All open clusters withknown distance were investigated, and for 75 clusters this is the firstdetermination of the mean proper motion. The results, including the DSSimages of the cluster's fields with the kinematic members marked, areincorporated in the Open Clusters Catalogue supported on line by ourgroup.
| The Evolutionary Status of Be Stars: Results from a Photometric Study of Southern Open Clusters
Be stars are a class of rapidly rotating B stars with circumstellardisks that cause Balmer and other line emission. There are threepossible reasons for the rapid rotation of Be stars: they may have beenborn as rapid rotators, spun up by binary mass transfer, or spun upduring the main-sequence (MS) evolution of B stars. To test the variousformation scenarios, we have conducted a photometric survey of 55 openclusters in the southern sky. Of these, five clusters are probably notphysically associated groups and our results for two other clusters arenot reliable, but we identify 52 definite Be stars and an additional 129Be candidates in the remaining clusters. We use our results to examinethe age and evolutionary dependence of the Be phenomenon. We find anoverall increase in the fraction of Be stars with age until 100 Myr, andBe stars are most common among the brightest, most massive B-type starsabove the zero-age main sequence (ZAMS). We show that a spin-up phase atthe terminal-age main sequence (TAMS) cannot produce the observeddistribution of Be stars, but up to 73% of the Be stars detected mayhave been spun-up by binary mass transfer. Most of the remaining Bestars were likely rapid rotators at birth. Previous studies havesuggested that low metallicity and high cluster density may also favorBe star formation. Our results indicate a possible increase in thefraction of Be stars with increasing cluster distance from the Galacticcenter (in environments of decreasing metallicity). However, the trendis not significant and could be ruled out due to the intrinsic scatterin our data. We also find no relationship between the fraction of Bestars and cluster density.
| Astrophysical parameters of Galactic open clusters
We present a catalogue of astrophysical data for 520 Galactic openclusters. These are the clusters for which at least three most probablemembers (18 on average) could be identified in the ASCC-2.5, a catalogueof stars based on the Tycho-2 observations from the Hipparcos mission.We applied homogeneous methods and algorithms to determine angular sizesof cluster cores and coronae, heliocentric distances, mean propermotions, mean radial velocities, and ages. For the first time we derivedistances for 200 clusters, radial velocities for 94 clusters, and agesof 196 clusters. This homogeneous new parameter set is compared withearlier determinations, where we find, in particular, that the angularsizes were systematically underestimated in the literature.
| New variable stars in open clusters. I. Methods and results for 20 open clusters
We present high precision CCD photometry of 1791 objects in 20 openclusters with an age of 10 Myr to 1 Gyr. These observations wereperformed within the Δ a photometric system which is primarilyused to detect chemically peculiar stars of the upper main sequence.Time bases range from 30 min up to 60 days with data from severalnights. We describe the time series analysis reaching a detection limitof down to 0.006 mag for apparent variability. In total, we havedetected 35 variable objects of which four are not members of theircorresponding clusters. The variables cover the entireHertzsprung-Russell diagram, hence they are interesting targets forfollow-up observations.Based on observations obtained at Complejo Astronómico elLeoncito (CASLEO), operated under the agreement between the ConsejoNacional de Investigaciones Científicas y Técnicas de laRepública Argentina and the National Universities of La Plata,Córdoba y San Juan; ESO-La Silla and UTSO-Las Campanas.
| Theoretical isochrones for the Delta a photometric system
We have calculated theoretical isochrones for the photometric Delta asystem to derive astrophysical parameters such as the age, reddening anddistance modulus for open clusters. The Delta a system samples the fluxdepression at 520 nm which is highly efficient to detect chemicallypeculiar (CP) objects of the upper main sequence. The evolutionarystatus of CP stars is still a matter of debate and very important totest, for example, the dynamo and diffusion theories. In fact, thedynamo or fossil origin of the magnetic fields present in this kind ofstar is still not clear. Using the stellar evolutionary models by Claret(\cite{Cla95}), a grid of isochrones with different initial chemicalcompositions for the Delta a system was generated. The published dataof 23 open clusters were used to fit these isochrones with astrophysicalparameters (age, reddening and distance modulus) from the literature. Asan additional test, isochrones with the same parameters for Johnson UBVdata of these open clusters were also considered. The fits show a goodagreement between the observations and the theoretical grid. We findthat the accuracy of fitting isochrones to Delta a data without theknowledge of the cluster parameters is between 5 and 15%.
| Proper Motions of Open Star Clusters and the Rotation Rate of the Galaxy
The mean proper motions of 167 Galactic open clusters withradial-velocity measurements are computed from the data of the Tycho-2catalog using kinematic and photometric cluster membership criteria. Theresulting catalog is compared to the results of other studies. The newproper motions are used to infer the Galactic rotation rate at the solarcircle, which is found to be ω0=+24.6±0.8 km s-1 kpc-1.Analysis of the dependence of the dispersion of ω0 estimates onheliocentric velocity showed that even the proper motions of clusterswith distances r>3 kpc contain enough useful information to be usedin kinematic studies demonstrating that the determination of propermotions is quite justified even for very distant clusters.
| Deep-sky dedication.
Not Available
| Proper motions of open clusters based on the TYCHO2 Catalogue. II. Clusters farther than 1 kpc
We determined the mean absolute proper motion of 94 open clusterssituated farther than 1 kpc from the Sun. The results are derived fromthe stellar proper motion data given in the Tycho2 Catalogue. The meanproper motion of the clusters and membership probability of individualstars were obtained from the proper motion data by applying thestatistical method proposed by Sanders (\cite{Sanders1971}). Themeasurements made use of a large number of stars, usually several tens,for each cluster. The total number of stars investigated in the fieldsof the clusters is 4864 of which 2021 were considered members. For 55clusters, this is the first determination of the proper motion. Based onobservations of the ESA Hipparcos satellite. Tables 1 to 95 are onlyavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/388/168
| The blue to red supergiant ratio in young clusters at various metallicities
We present new determinations of the blue to red supergiant ratio (B/R)in young open clusters at various metallicities. For this purpose, weexamine the HR diagrams of 45 clusters in the Galaxy and of 4 clustersin the Magellanic Clouds. The identification of supergiants is based onspectroscopic measurements (with photometric counts to check theresults). The new counts confirm the increase of the B/R ratio when themetallicity increases with the following normalized relation:(B/R)/((B/R)sun) =~ 0.05* e3(Z)/(Zsun)}, where Zsun=0.02 and(B/R)sun is the value of B/R at Zsun which dependson the definition of B and R and on the age interval considered (e.g.for spectroscopic counts including clusters with log age between 6.8 and7.5, (B/R)sun =~ 3 when B includes O, B and A supergiants).
| CCD photometric search for peculiar stars in open clusters. II. NGC 2489, NGC 2567, NGC 2658, NGC 5281 and NGC 6208
High accurate photometric data in the three filter, narrow-band Deltaa-system for five open clusters (NGC 2489, NGC 2567, NGC 2658, NGC 5281and NGC 6208) are presented permitting one to detect apparent chemicallypeculiar stars. The ages and distances are wide spread to improve thestatistics of peculiar stars in our Milky Way. A total of 235 starswithin these clusters have been observed. We have detected ten apparentpeculiar objects (six with significant positive and four with negativeDelta a-values) in four open clusters. Although three of them within theboundaries of NGC 2567 are probably not members of this cluster. Sinceno Strömgren uvbybeta data are available from the literature,Johnson UBV photometry was used to test and calibrate our photometricdata. The results from a comparison of both systems are excellent. Basedon observations at ESO-La Silla and UTSO-Las Campanas. Tables 4 to 8 areonly available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/373/153 Figure 1 is onlyavailable in electronic form at http://www.edpsciences.org
| Photometric and kinematic studies of open star clusters. III. NGC 4103, NGC 5281, and NGC 4755
We present CCD photometry and proper motion studies of the three openstar clusters NGC 4103, NGC 5281, and NGC 4755 (kappa Cru). By fittingisochrones to the colour magnitude diagrams, we found that all threeobjects are young open star clusters with ages of at most t=45 Myr. Theyare located at distances from approx. 1600 pc to 2200 pc, derived fromdistance moduli (m-M)_0 ranging from 11 mag to 12 mag. We combinedmembership determinations based on proper motions and statistical fieldstar subtraction to derive the initial mass function (IMF) of theclusters. The shape of the IMFs could be represented by power laws withexponents of Gamma =-1.46 +/- 0.22 for NGC 4103, Gamma =-1.60 +/- 0.50for NGC 5281, and Gamma =-1.68 +/- 0.14 for NGC 4755, when - as areference - Salpeter's (\cite{salpeter}) value would be Gamma =-1.35.These results agree well with other IMF studies of open star clusters.Partly based on observations from ESO, La Silla.
| Two New Ejecta-dominated Galactic Supernova Remnants: G337.2-0.7 and G309.2-0.6
We present the analysis of new X-ray observations of two Galactic radiosupernova remnants (SNRs), G337.2-0.7 and G309.2-0.6. Both remnantsexhibit line-rich thermal spectra that require highly nonsolar elementalabundance ratios. In each case, Si and S are unequivocally overabundantcompared to solar, based purely on the measured equivalent width of theKα line complex. Detailed nonequilibrium ionization spectralanalysis of these remnants, using a single-temperature, singleionization age model, confirms the overabundances, yielding Si, S, andAr abundances many times their solar values: 3-5 times solar forG337.2-0.7 and greater than 3-10 times solar for G309.2-0.6. We alsofind that for both remnants, Ne and Mg are underabundant relative to Si,and for G309.2-0.6, Ca and Fe are relatively underabundant as well. Thisis the first detection of metal-rich, nonsolar abundance material inthese remnants, identifying them as young ejecta-dominated SNRs. Furthersupport for their youth comes from the distances that we estimate fromthe fitted column densities (less than 15 kpc for G337.2-0.7, and 4+/-2kpc for G309.2-0.6). From the implied sizes of the remnants at thesedistances we infer relatively young ages (2000-4500 years for G337.2-0.7and 700-4000 years for G309.2-0.6). Finally, we note that no compactobject has yet been found within G337.2-0.7, but an X-ray point sourceis evident within the radio shell of G309.2-0.6, although its natureremains unknown.
| Spectroscopic Binaries in Young Open Clusters
We have analysed the binarity and multiplicity characteristics of 120O-type stars in 22 very young open clusters and found marked differencesbetween the "rich" (N >= 6 O-type stars and primaries) and "poor" (N= 1) clusters. In the rich clusters, the binary frequencies vary between14% (1 SB among 7 stars) and 80% (8 SBs among 10 stars). Multiplesystems seem not to be frequent and stars are spread all over thecluster area. In poor clusters, the binary frequency of the O-typeobjects is nearly 100%, with orbital periods around 3 days. Severalbinaries are also eclipsing. Additional companions are always present.They form either hierarchical multiple stars or trapezium systems. Thesemassive multiple systems are generally found close to the clustercenter, although there are exceptions.
| 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
| G309.2-00.6 and jets in supernova remnants
We present Australia Telescope Compact Array observations of thesupernova remnant (SNR) G309.2-00.6. In a 1.3-GHz continuum image theremnant appears as a near-circular shell, but with two brightened anddistorted arcs of emission on opposite sides. Hi absorption against theSNR yields a distance in the range 5.4 to 14.1 kpc, corresponding to anage (1-20)x10^3 yr. On the basis of the morphology of the SNR we arguethat it is a younger analogue of the W 50/SS 433 system, and that itsunusual appearance is a result of opposed jets or outflows from acentral source. A jet-like feature and breaks in the shell can both beseen along the axis of proposed outflow, providing further support forthis interpretation; the central source itself is not detected. The SNRmay be interacting with the adjacent Hii region RCW 80 through anextension of the proposed outflow beyond its shell. This would put theSNR at the lower limit of its distance range and would imply an age<~4000 yr. We consider other SNRs similar to G309.2-00.6, and proposeremnants whose shells are affected by jets as one of several classes ofSNR from which the presence of a central source can be inferred.
| Absolute proper motions of 181 young open clusters.
Not Available
| Chemical Evolution of the Galactic Disk: Evidence for a Gradient Perpendicular to the Galactic Plane
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995AJ....110.2813P&db_key=AST
| Catalogue of blue stragglers in open clusters.
An extensive survey of blue straggler candidates in galactic openclusters of both hemispheres is presented. The blue stragglers wereselected considering their positions in the cluster colour-magnitudediagrams.They were categorized according to the accuracy of thephotometric measurements and membership probabilities. An amount of 959blue straggler candidates in 390 open clusters of all ages wereidentified and classified. A set of basic data is given for everycluster and blue straggler. The information is arranged in the form of acatalogue. Blue stragglers are found in clusters of all ages. Thepercentage of clusters with blue stragglers generally grows with age andrichness of the clusters. The mean ratio of the number of bluestragglers to the number of cluster main sequence stars is approximatelyconstant up to a cluster age of about 10^8.6^ yr and rises for olderclusters. In general, the blue stragglers show a remarkable degree ofcentral concentration.
| Formation and evolutionary properties of the Galactic open cluster system
Results are reported from a statistical analysis of observational dataon 100 open clusters within 2 kpc of the sun, selected from the catalogof Lynga (1987). The selection criteria and the completeness of thesample are discussed; the data are compiled in a table; and the analysisresults are presented in a series of graphs and characterized in detail.A cluster formation rate of 0.45 clusters/kpc Myr is found,significantly lower than the rates determined previously (using clusterswithin 1 kpc of the sun) and corresponding to a cluster star-formationefficiency of 0.0063. The low average cluster lifetime (about 10 Myr)suggests that clusters are formed as unstable systems.
| The Gould plates
Most of the 1200 photographs of southern galactic star clusters anddouble stars taken by Benjamin A. Gould at Cordoba, Argentina, in1872-1882 are in the Harvard College Observatory plate collection. Arecent evaluation of these plates shows many to be in usable condition.Details of the characteristics of Gould's plates of galactic clusters,including limiting magnitudes, are presented.
| Photometric metal abundances of high-luminosity red stars in young and intermediate-age open clusters
UBV, DDO, and Washinton photometry has been obtained for G and K starslocated in or near 22 young and intermediate-age open clusters. Nearly65 percent of the observed stars are found to have a high probability ofbeing cluster members, while the remaining 35 percent are likely to bered field stars. Five clusters (NGC 2383, NGC 3033, Ruprecht 20, NGC5168, and NGC 6249) probably do not contain any red giants. Sixteenclusters are found to be nearly solar in composition; three are slightlymetal-poor or metal-rich; one (Ruprecht 20) is moderately metal-poor(Fe/H = -0.3); and another (NGC 5617) is moderately metal-rich (Fe/H =0.3). None of the clusters with derived Washington abundances appear tobe enriched in elements of the CNO group.
| The Sagittarius-Carina Arm Structure and Parameters of Spiral Pattern
Not Available
| Young stellar-gas complexes in the Galaxy
It is found that about 90 percent of OB-associations and o-b2 clusterssituated within 3 kpc of the sun can be united into complexes withdiameters of 150-700 pc. Almost all of these clusters contain giantmolecular clouds with a mass greater than about 100,000 solar masses. Anumber of complexes are associated with giant H I clouds; a few of thesmall complexes are situated in the HI caverns. The concentration ofOB-associations and young clusters in star complexes attests to theircommon origin in the supergiant gaseous clouds.
| A cluster analysis of young open clusters
Cluster analysis methods are used to consider the galactic distributionof 224 open clusters with an age up to 10 to the 8th yrs. Most of theseclusters enter condensations with characteristic dimensions of a fewhundred parsecs. Some condensations are so similar in terms of the age,integrated color, and radial velocity of their components, that thiscannot be considered a coincidence. This suggests that each condensationis a physical entity consisting of clusters apparently linked by acommon origin.
| Mass-losing red giants in open clusters
Mass-losing stars in open clusters with main-sequence turn-offs atintermediate mass have been searched for by using the IRAS data base.The absence of many strong 60 micron sources in open clusters impliesthat intermediate-mass stars lose much of their mass during an intensewind phase of rather short duration. For stars of about seven solarmasses, this phase, if it exists at all, lasts for not much more than100,000 yr. For stars of about four solar masses, the intense wind phaseappears to last considerably less than 10 million yr; it may well lastfor less than a million yr.
| Catalogue of UBV Photometry and MK Spectral Types in Open Clusters (Third Edition)
Not Available
| Open clusters and galactic structure
A total of 610 references to 434 clusters are employed in thecompilation of a catalog of open clusters with color-magnitude diagramson the UBV or RGU systems. Estimates of reddening, distance modulus, ageand number of cluster members are included. Although the sample isconsidered representative of the discoverable clusters in the galaxy,the observed distribution is nonuniform because of interstellarobscuration. Cluster distribution in the galactic plane is found to bedominated by the locations of dust clouds rather than by spiralstructure. The distributions of clusters as a function of age andrichness class show that the lifetimes of poor clusters are much shorterthan rich ones, and that clusters in the outer disk survive longer thanthose in the inner disk. An outer disk age which is only about 50% theage of the globular clusters is indicated by cluster statistics. Thethickening of the galactic disk with increasing galactocentric distancemay be due to either a younger dynamical age or a lower gravitationalpotential in the outer regions.
| Comparative Studies of Young Open Clusters - Part Two - an Atlas of Composite Colour-Magnitude Diagrams
Abstract image available at:http://adsabs.harvard.edu/abs/1981A&AS...44..467M
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