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K-band magnitude of the red clump as a distance indicator
We have investigated how the K-band magnitude of the red clump [M_K(RC)]depends on age and metallicity, using 2MASS infrared data for a sampleof 24 open clusters with known distances. We show that a constant valueof M_K(RC)=-1.57 ± 0.05 is a reasonable assumption to use indistance determinations for clusters with metallicity between -0.5 and+0.4 dex and age between 108.5 and 109.9 years.Figures 8 and 9 are available in electronic form at http://www.aanda.org
| On the current status of open-cluster parameters
We aim to characterize the current status of knowledge on the accuracyof open-cluster parameters such as the age, reddening and distance.These astrophysical quantities are often used to study the globalcharacteristics of the Milky Way down to the very local stellarphenomena. In general, the errors of these quantities are neglected orset to some kind of heuristic standard value. We attempt to give somerealistic estimates for the accuracy of available cluster parameters byusing the independently derived values published in the literature. Intotal, 6437 individual estimates for 395 open clusters were used in ourstatistical analysis. We discuss the error sources depending ontheoretical as well as observational methods and compare our resultswith those parameters listed in the widely used catalogue by Dias et al.In addition, we establish a list of 72 open clusters with the mostaccurate known parameters which should serve as a standard table in thefuture for testing isochrones and stellar models.
| Kinematics of the Open Cluster System in the Galaxy
Absolute proper motions and radial velocities of 202 open clusters inthe solar neighborhood, which can be used as tracers of the Galacticdisk, are used to investigate the kinematics of the Galaxy in the solarvicinity, including the mean heliocentric velocity components(u1,u2,u3) of the open cluster system,the characteristic velocity dispersions(σ1,σ2,σ3), Oortconstants (A,B) and the large-scale radial motion parameters (C,D) ofthe Galaxy. The results derived from the observational data of propermotions and radial velocities of a subgroup of 117 thin disk young openclusters by means of a maximum likelihood algorithm are:(u1,u2,u3) =(-16.1+/-1.0,-7.9+/-1.4,-10.4+/-1.5) km s-1,(σ1,σ2,σ3) =(17.0+/-0.7,12.2+/-0.9,8.0+/-1.3) km s-1,(A,B) =(14.8+/-1.0,-13.0+/-2.7) km s-1 kpc-1, and (C,D) =(1.5+/-0.7,-1.2+/-1.5) km s-1 k pc-1. A discussionon the results and comparisons with what was obtained by other authorsis given.
| Survey for Transiting Extrasolar Planets in Stellar Systems. II. Spectrophotometry and Metallicities of Open Clusters
We present metallicity estimates for seven open clusters based onspectrophotometric indices from moderate-resolution spectroscopy.Observations of field giants of known metallicity provide a correlationbetween the spectroscopic indices and the metallicity of open clustergiants. We use χ2 analysis to fit the relation ofspectrophotometric indices to metallicity in field giants. The resultingfunction allows an estimate of the target-cluster giants' metallicitieswith an error in the method of +/-0.08 dex. We derive the followingmetallicities for the seven open clusters: NGC 1245, [M/H]=-0.14+/-0.04NGC 2099, [M/H]=+0.05+/-0.05 NGC 2324, [M/H]=-0.06+/-0.04 NGC 2539,[M/H]=-0.04+/-0.03 NGC 2682 (M67), [M/H]=-0.05+/-0.02 NGC 6705,[M/H]=+0.14+/-0.08 NGC 6819, [M/H]=-0.07+/-0.12. These metallicityestimates will be useful in planning future extrasolar planet transitsearches, since planets may form more readily in metal-richenvironments.
| 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.
| Searching for Planetary Transits in Galactic Open Clusters: EXPLORE/OC
Open clusters potentially provide an ideal environment for the searchfor transiting extrasolar planets, since they feature a relatively largenumber of stars of the same known age and metallicity at the samedistance. With this motivation, over a dozen open clusters are now beingmonitored by four different groups. We review the motivations andchallenges for open cluster transit surveys for short-period giantplanets. Our photometric monitoring survey of Galactic southern openclusters, the Extrasolar Planet Occultation Research/Open Clusters(EXPLORE/OC) project, was designed with the goals of maximizing thechance of finding and characterizing planets and of providing astatistically valuable astrophysical result in the case of nodetections. We use the EXPLORE/OC data from two open clusters, NGC 2660and NGC 6208, to illustrate some of the largely unrecognized issuesfacing open cluster surveys, including severe contamination by Galacticfield stars (>80%) and the relatively low number of cluster membersfor which high-precision photometry can be obtained. We discuss how acareful selection of open cluster targets under a wide range of criteriasuch as cluster richness, observability, distance, and age can meet thechallenges, maximizing chances to detect planet transits. In addition,we present the EXPLORE/OC observing strategy to optimize planetdetection, which includes high-cadence observing and continuouslyobserving individual clusters rather than alternating between targets.
| On the Galactic Disk Metallicity Distribution from Open Clusters. I. New Catalogs and Abundance Gradient
We have compiled two new open cluster catalogs. In the first one, thereare 119 objects with ages, distances, and metallicities available, whilein the second one, 144 objects have both absolute proper motion andradial velocity data, of which 45 clusters also have metallicity dataavailable. Taking advantage of the large number of objects included inour sample, we present an iron radial gradient of about -0.063+/-0.008dex kpc-1 from the first sample, which is quite consistentwith the most recent determination of the oxygen gradient from nebulaeand young stars, about -0.07 dex kpc-1. By dividing clustersinto age groups, we show that the iron gradient was steeper in the past,which is consistent with the recent result from Galactic planetarynebulae data, and also consistent with inside-out galactic diskformation scenarios. Based on the cluster sample, we also discuss themetallicity distribution, cluster kinematics, and space distribution. Adisk age-metallicity relation could be implied by those properties,although we cannot give conclusive result from the age- metallicitydiagram based on the current sample. More observations are needed formetal-poor clusters. From the second catalog, we have calculated thevelocity components in cylindrical coordinates with respect to theGalactic standard of rest for 144 open clusters. The velocitydispersions of the older clusters are larger than those of youngclusters, but they are all much smaller than that of the Galactic thickdisk stars.
| Search for variable stars in the open cluster NGC 2539
We present UBVI absolute and V-band time-series CCD photometric resultsfor the intermediate-age open cluster NGC 2539. From the empiricalzero-age main sequence and theoretical isochrone fitting in color-colorand color-magnitude diagrams, we estimated the physical parameters ofthis cluster as follows: the color excess of E(B-V)=0.06 +/- 0.03, thedistance modulus of (V-MV)0=10.2 +/- 0.1 and theage of log t = 8.8 ( ~ 630 Myr). By carefully examining the time-seriesimages, we discovered seven new variable stars in the observed clusterfield. Considering the light curves, periods and positions on thecolor-magnitude diagram, we classified them as five eclipsing binarystars, one delta Scuti star and one gamma Doradus candidate. The gammaDoradus candidate might not be a cluster member because it is locatedredder by about Delta (B-V) = 0.2 than the cool edge of gamma Doradusinstability strip.
| 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.
| 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
| WIYN Open Cluster Study. X. The K-Band Magnitude of the Red Clump as a Distance Indicator
In an effort to improve the utility of the helium-burning red clumpluminosity as a distance indicator, we explore the sensitivity of theK-band red clump absolute magnitude [MK(RC)] to metallicityand age. We rely upon JK photometry for 14 open clusters and twoglobular clusters from the Second Incremental Data Release of the TwoMicron All Sky Survey (2MASS) Point Source Catalog. The distances,metallicities, and ages of the open clusters are all on an internallyconsistent system, while the K(RC) values are measured from the 2MASSdata. For clusters younger than ~2 Gyr, MK(RC) is insensitiveto metallicity but shows a dependence on age. In contrast, for clustersolder than ~2 Gyr, MK(RC) is influenced primarily by themetallicity of the population and shows little or no dependence on theage. Theoretical red clump models based on the formalism of Girardi etal. reinforce this finding. Over comparable metallicity and age ranges,our average MK(RC) value is in accord with that based onsolar neighborhood red clump stars with Hipparcos parallaxes. Lastly, wecompute the distance to the open cluster NGC 2158 using our red clumpcalibration. Adopting an age of 1.6+/-0.2 Gyr and [Fe/H]=-0.24+/-0.06,our calibration yields a distance of (m-M)V=14.38+/-0.09.
| Abundance Gradient from Open Clusters and Implications for the Galactic Disk Evolution
We compile a new sample of 89 open clusters with ages, distances andmetallicities available. We derive a radial iron gradient of about-0.099±0.008 dexkpc (unweighted) for the whole sample, which issomewhat greater than the most recent determination of oxygen gradientfrom nebulae and young stars. By dividing the clusters into age groups,we show that the iron gradient was steeper in the past and has evolvedslowly in time. Current data show a substantial scatter of the clustermetallicities indicating that the Galactic disk has undergone a veryrapid, inhomogeneous enrichment.Also, based on a simple, but quitesuccessful model of chemical evolution of the Milky Way disk, we make adetailed calculation of the iron abundance gradient and its timeevolution. The predicted current iron gradient is about -0.072 dexkpc.The model also predicts a steady flattening of the iron gradient withtime, which agrees with the result from our open cluster sample.
| Radial velocities, binarity, and kinematic membership in open clusters with blue straggler candidates
Not Available
| The Galactic System of Open Star Clusters: A Personal Perspective
Technology is now allowing for the investigation of star clustersoutside of the Milky Way. As attention turns to the extragalactic starclusters, a perception that the system of star clusters in the Milky Wayis well understood may grow, resulting in the neglect of these importantobjects. In this review, the status of our understanding of the MilkyWay's open star cluster population will be discussed. Specifically, Iwill attempt to illustrate not only the important information that canand must be learned from these nearby star clusters, but also the degreeto which our understanding of the Galactic open clusters remainsincomplete.
| Search for Variable Stars in Two Old Open Clusters: NGC2506 and NGC2420
We present results of photometric observations of two old open clusters:NGC 2506 and NGC 2420. V-band time-series and UBVI absolute CCDphotometric observations were carried out to search for variable starsand to investigate their physical properties. From the UBVI photometryof NGC 2506, we obtain interstellar reddening of E(B-V)=0.04+/-0.03 mag,distance modulus (V-M_V)_0=12.5+/-0.1 mag, and age log(t/yr)=9.25. Frommonitoring of 590 stars with 304 CCD frames taken for ten nights, threedelta Sct stars and one eclipsing binary star are discovered in NGC2506. For the other cluster, NGC 2420, we have examined light variationsof 505 stars using 347 time-series data obtained for five nights,finding no variable star. It should be noted that we have found no gammaDor star among main-sequence stars near F0 in these two old openclusters, which is consistent with the suggestion that gamma Dor-typephenomenon occurs in stars younger than log(t/yr)=8.4. On the otherhand, it has been known that color-magnitude diagrams of these twoclusters show well-established binary sequences, implying high incidenceof binary systems: >=20% for NGC 2506 and approx 50% for NGC 2420.However, only one eclipsing binary star was found in these two clusters.
| 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
| UBV photometric study and basic parameters of the southern open cluster NGC 2539
We present UBV photoelectric observations of 345 stars in the field ofthe southern open cluster NGC 2539. The analysis of these data allows todetermine that 169 stars are probable members of the cluster mainsequence, while 23 are possible members. The CC and CM diagrams reveal awell-defined main sequence and a populous red giant branch. We derive areddening E(B-V) = 0.06 and an apparent distance modulus V-M_v = 10.60,equivalent to a distance of 1210 pc. The age, determined by fittingisochrones computed by the Geneva group with mass loss and moderate coreovershooting, turns out to be 630 Myr, which places this cluster withinthe Hyades-age group. The isochrone for log t = 8.80 reproduces well themorphology of the upper main sequence band in the two CM diagrams,including the binary ridge. Although this isochrone also reproduces wellthe general shape of the observed red giant pattern, it appears to be alittle too bright and too red. This fact could be probably due to theuncertainty on the exact value of the mixing-length parameter. However,mass loss during the evolution of the red giants might also partiallyaccount for their location in the HR diagram. The low contamination ofthe upper main sequence of the cluster CM diagrams and its populated redgiant branch makes NGC 2539 a very good target for testing oftheoretical models. Based on observations made at Las CampanasObservatory (Chile) and at European Southern Observatory, La Silla(Chile). Table 1 is only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Foreground and background dust in star cluster directions
This paper compares reddening values E(B-V) derived from the stellarcontent of 103 old open clusters and 147 globular clusters of the MilkyWay with those derived from DIRBE/IRAS 100 mu m dust emission in thesame directions. Star clusters at |b|> 20deg showcomparable reddening values between the two methods, in agreement withthe fact that most of them are located beyond the disk dust layer. Forvery low galactic latitude lines of sight, differences occur in thesense that DIRBE/IRAS reddening values can be substantially larger,suggesting effects due to the depth distribution of the dust. Thedifferences appear to arise from dust in the background of the clustersconsistent with a dust layer where important extinction occurs up todistances from the Plane of ~ 300 pc. For 3 % of the sample asignificant background dust contribution might be explained by higherdust clouds. We find evidence that the Milky Way dust lane and higherdust clouds are similar to those of several edge-on spiral galaxiesrecently studied in detail by means of CCD imaging.
| A report on the studies of star clusters with the UPSO 104-cm Sampurnanand telescope during last 25 years
Not Available
| Some Revised Observational Constraints on the Formation and Evolution of the Galactic Disk
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....114.2556T&db_key=AST
| An analysis of the AP spectroscopic binary HD 59435.
HD 59435 is a double-lined spectroscopic binary (SB2), with slowlyrotating components of very similar luminosity. It was studied throughhigh-resolution spectroscopy, photometry and CORAVEL observations.Orbital elements are presented. The orbital period is 1387 days. Theline of sight lies close to the orbital plane, but no eclipses have beenobserved so far. The primary is an evolved G8 or K0 star, which haslikely just descended the Red Giant Branch. The secondary is a cool Apstar close to the end of its main-sequence life. It shows lines resolvedinto magnetically split components, from which its mean magnetic fieldmodulus can be diagnosed. The field varies with a remarkably largerelative amplitude, over a rotation period which is at least of theorder of 3 years.
| 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
| On Coagulation and the Stellar Mass Spectrum
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...452..652A&db_key=AST
| Tidal circularization and the eccentricity of binaries containing giant stars.
We show that the predicted amount of tidal circularization in a detachedbinary containing a giant is, according to Zahn's theory, determinedonly by observable properties of its orbit, and a single integral alongthe giant's stellar evolutionary sequence. We perform these integrals,display them graphically, and provide fitting formulae. Spectroscopicbinaries in open clusters are ideal for testing the theory of tidalcircularization, since the stars' mass, luminosity and temperature canall be determined with precision. We apply our calculations to 28binaries in 12 open clusters. We show that the orbital parameters of allcan be understood within the circularization theory, and that the mixinglength parameter in Zahn's theory is well constrained:1<~α<~3. We show that the orbital period alone does notseparate circular and eccentric orbits, and point out that theeccentricity of the orbit can sometimes distinguish between giant starsand core helium burning `clump' stars even in circumstances where thisis difficult spectroscopically. In some special types of binary systems,the circularization is sensitive to aspects of stellar evolution theorythat are not well understood: the maximum depth of penetration of theouter convective zone, the radius at first dredge-up, the maximum radiiof stars at the tips of the giant and asymptotic giant branches. It thusappears that the orbits of binaries containing giants may prove to be auseful tool for studying stellar evolution.
| 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.
| The apparent distribution of red giant spectroscopic binaries in open clusters
The projected radial distribution of 88 red giant spectroscopic binarieshas been compared to that of 260 single giants in 14 intermediate-ageand old clusters. The radial extension of the available data is ofcrucial importance, and the clusters have been partitioned in twogroups. In the first group, with most complete data, only one cluster(M67) shows a statistically significant concentration of spectroscopicbinaries towards the inner regions relative to single giants. Centralconcentration of binaries is observed, without statistical significance,for three younger clusters. The segregation does not depend on theperiod of the binaries, but qualitively seems to depend on the totalmass of the binary. For the 7 clusters of the second group, no effect isvisible. These clusters are either not old enough (8.45 less than logtless than 9.25) or, more probably, the radial extension of the existingphotometric studies is too small. Simulation with real data tends tofavor the latter explanation.
| An evolutionary model for the Wolf Rayet nebula NGC 2539
The main outer ring of the Wolf-Rayet (WR) nebula NGC 2539 expandsradially with velocity approximately = 26 km/s. The dynamics aremodelled as the interaction of the winds from the O progenitor and thepresent WR stage with clumpy molecular cloud material and Red Supergiantejecta. In both stages, the bubbles are driven by wind momentum. Thenecessary radiative energy loss probably occurs in boundary layersbetween cool clumps and hot shocked wind.
| A revised effective-temperature calibration for the DDO photometric system
A revised effective-temperature calibration for the David DunlapObservatory (DDO) photometric system is presented. Recently publishedphotometric and spectroscopic observations of field and open-cluster Gand K stars allow a better definition of the solar-abundance fiducialrelation in the DDO C0(45-48) vs. C0(42-45)diagram. The ability of the DDO system to predict MK spectral types of Gand K giants is demonstrated. The new DDO effective temperaturecalibration reproduces satisfactorily the infrared temperature scale ofBell and Gustafsson (1989). It is shown that Osborn's (1979) calibrationunderestimates the effective temperatures of K giants by approximately170 K and those of late-type dwarfs by approximately 150 K.
| Integrated photometric properties of open clusters
Galactic open clusters provide an abundant sample of stellar aggregatesof various sizes, ages and metal abundances, apt to constitute atemplate for comparison with star systems in other galaxies. In thispaper we present and discuss a standard methodology to synthesize U,B,Vfluxes and colours, and apply it to a set of 138 open clusters. Resultsare compared with previous ones available in the literature. We wereable to calibrate a mass-luminosity relation by which we evaluated themass of ~400 open clusters, leading to a well defined present-day massfunction. The number-complete sample of galactic open clusters presentedin Battinelli & Capuzzo-Dolcetta (1991) is enlarged of a 15%.
| An observational age-metallicity relation for the Galaxy
An observational Age-Metallicity Diagram for the Galaxy has beenconstructed on the base of star cluster data available in theliterature. This diagram exhibits two independent and simultaneousmetallicity enhancement processes identified with two dynamical galacticsubstructures: the thin and the thick disks. Within the observationaluncertainties both these processes can be satisfactory approximated byInfall-Inflow models of the chemical evolution with different high,although rapidly decaying with time, Star Formation and Infall Rates.The comparison of the galactic age-metallicity relations with that forthe Large Magellanic Cloud shows some similarities between processes ofthe chemical enhancement in the Large Magellanic Cloud and the Thin Disksubsystem in the Galaxy.
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