Contents
Images
Upload your image
DSS Images Other Images
Related articles
Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters
The availability of the Hipparcos Catalogue has triggered many kinematicand dynamical studies of the solar neighbourhood. Nevertheless, thosestudies generally lacked the third component of the space velocities,i.e., the radial velocities. This work presents the kinematic analysisof 5952 K and 739 M giants in the solar neighbourhood which includes forthe first time radial velocity data from a large survey performed withthe CORAVEL spectrovelocimeter. It also uses proper motions from theTycho-2 catalogue, which are expected to be more accurate than theHipparcos ones. An important by-product of this study is the observedfraction of only 5.7% of spectroscopic binaries among M giants ascompared to 13.7% for K giants. After excluding the binaries for whichno center-of-mass velocity could be estimated, 5311 K and 719 M giantsremain in the final sample. The UV-plane constructed from these datafor the stars with precise parallaxes (σπ/π≤20%) reveals a rich small-scale structure, with several clumpscorresponding to the Hercules stream, the Sirius moving group, and theHyades and Pleiades superclusters. A maximum-likelihood method, based ona Bayesian approach, has been applied to the data, in order to make fulluse of all the available stars (not only those with precise parallaxes)and to derive the kinematic properties of these subgroups. Isochrones inthe Hertzsprung-Russell diagram reveal a very wide range of ages forstars belonging to these groups. These groups are most probably relatedto the dynamical perturbation by transient spiral waves (as recentlymodelled by De Simone et al. \cite{Simone2004}) rather than to clusterremnants. A possible explanation for the presence of younggroup/clusters in the same area of the UV-plane is that they have beenput there by the spiral wave associated with their formation, while thekinematics of the older stars of our sample has also been disturbed bythe same wave. The emerging picture is thus one of dynamical streamspervading the solar neighbourhood and travelling in the Galaxy withsimilar space velocities. The term dynamical stream is more appropriatethan the traditional term supercluster since it involves stars ofdifferent ages, not born at the same place nor at the same time. Theposition of those streams in the UV-plane is responsible for the vertexdeviation of 16.2o ± 5.6o for the wholesample. Our study suggests that the vertex deviation for youngerpopulations could have the same dynamical origin. The underlyingvelocity ellipsoid, extracted by the maximum-likelihood method afterremoval of the streams, is not centered on the value commonly acceptedfor the radial antisolar motion: it is centered on < U > =-2.78±1.07 km s-1. However, the full data set(including the various streams) does yield the usual value for theradial solar motion, when properly accounting for the biases inherent tothis kind of analysis (namely, < U > = -10.25±0.15 kms-1). This discrepancy clearly raises the essential questionof how to derive the solar motion in the presence of dynamicalperturbations altering the kinematics of the solar neighbourhood: doesthere exist in the solar neighbourhood a subset of stars having no netradial motion which can be used as a reference against which to measurethe solar motion?Based on observations performed at the Swiss 1m-telescope at OHP,France, and on data from the ESA Hipparcos astrometry satellite.Full Table \ref{taba1} is only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/430/165}
| The Indo-US Library of Coudé Feed Stellar Spectra
We have obtained spectra for 1273 stars using the 0.9 m coudéfeed telescope at Kitt Peak National Observatory. This telescope feedsthe coudé spectrograph of the 2.1 m telescope. The spectra havebeen obtained with the no. 5 camera of the coudé spectrograph anda Loral 3K×1K CCD. Two gratings have been used to provide spectralcoverage from 3460 to 9464 Å, at a resolution of ~1 Å FWHMand at an original dispersion of 0.44 Å pixel-1. For885 stars we have complete spectra over the entire 3460 to 9464 Åwavelength region (neglecting small gaps of less than 50 Å), andpartial spectral coverage for the remaining stars. The 1273 stars havebeen selected to provide broad coverage of the atmospheric parametersTeff, logg, and [Fe/H], as well as spectral type. The goal ofthe project is to provide a comprehensive library of stellar spectra foruse in the automated classification of stellar and galaxy spectra and ingalaxy population synthesis. In this paper we discuss thecharacteristics of the spectral library, viz., details of theobservations, data reduction procedures, and selection of stars. We alsopresent a few illustrations of the quality and information available inthe spectra. The first version of the complete spectral library is nowpublicly available from the National Optical Astronomy Observatory(NOAO) via ftp and http.
| Three-dimensional Spectral Classification of Low-Metallicity Stars Using Artificial Neural Networks
We explore the application of artificial neural networks (ANNs) for theestimation of atmospheric parameters (Teff, logg, and [Fe/H])for Galactic F- and G-type stars. The ANNs are fed withmedium-resolution (Δλ~1-2 Å) non-flux-calibratedspectroscopic observations. From a sample of 279 stars with previoushigh-resolution determinations of metallicity and a set of (external)estimates of temperature and surface gravity, our ANNs are able topredict Teff with an accuracy ofσ(Teff)=135-150 K over the range4250<=Teff<=6500 K, logg with an accuracy ofσ(logg)=0.25-0.30 dex over the range 1.0<=logg<=5.0 dex, and[Fe/H] with an accuracy σ([Fe/H])=0.15-0.20 dex over the range-4.0<=[Fe/H]<=0.3. Such accuracies are competitive with theresults obtained by fine analysis of high-resolution spectra. It isnoteworthy that the ANNs are able to obtain these results withoutconsideration of photometric information for these stars. We have alsoexplored the impact of the signal-to-noise ratio (S/N) on the behaviorof ANNs and conclude that, when analyzed with ANNs trained on spectra ofcommensurate S/N, it is possible to extract physical parameter estimatesof similar accuracy with stellar spectra having S/N as low as 13. Takentogether, these results indicate that the ANN approach should be ofprimary importance for use in present and future large-scalespectroscopic surveys.
| The early-type galaxy population in Abell 2218
We present high signal-to-noise, moderate-resolution spectroscopy of 48early-type members of the rich cluster Abell 2218 at z=0.18, taken withthe LDSS2 spectrograph on the 4.2-m William Herschel Telescope. Thissample both is larger and spans a wider galaxy luminosity range, down toMB*+1, than previous studies. In addition to the relatively large sizeof the sample, we have detailed morphological information from archivalHubble Space Telescope imaging for 20 of the galaxies. We combine themorphological, photometric, kinematic and line-strength information tocompare A2218 with similar samples drawn from local clusters and toidentify evolutionary changes between the samples which have occurredover the last ~3Gyr. The overall picture is one of little or noevolution in nearly all of the galaxy parameters. Zero-point offsets inthe Faber-Jackson, Mgb-σ and Fundamental Planerelations are all consistent with passively evolving stellarpopulations. The slopes of these relations have not changedsignificantly in the 3Gyr between A2218 and today. We do however find asignificant spread in the estimated luminosity-weighted ages of thestellar populations in the galaxies, based on line diagnostic diagrams.This age spread is seen in both the discy early-type galaxies (S0) andalso the ellipticals. We observe both ellipticals with a strongcontribution from a young stellar population and lenticulars dominatedby old stellar populations. On average, we find no evidence forsystematic differences between the populations of ellipticals andlenticulars. In both cases there appears to be little evidence fordifferences between the stellar populations of the two samples. Thispoints to a common formation epoch for the bulk of the stars in most ofthe early-type galaxies in A2218. This result can be reconciled with theclaims of rapid morphological evolution in distant clusters if thesuggested transformation from spirals to lenticulars does not involvesignificant new star formation.
| The effective temperature scale of giant stars (F0-K5). II. Empirical calibration of Teff versus colours and [Fe/H]
We present calibrations of the effective temperatures of giant starsversus [Fe/H] and colours (U-V), (B-V), (R-I), (V-R), (V-I), (V-K),(J-H), (J-K), (I-K), (V-L'), (b-y) and (u-b). These calibrations arebased on a large sample of field and globular cluster stars whichroughly cover spectral types from F0 to K5. Their effectivetemperatures, scaled to direct Teff determinations viareliable angular diameter measurements, were derived by applying theinfrared flux method. The empirical relations have been fitted topolynomials of the form theta_ {eff} = P(colour,[Fe/H]) by using theleast squares method. The precision of the fits ranges from 40 K for(V-K) to 170 K for (J-H). We tabulate intrinsic colours of giant starsin the ranges: 3500 K <= Teff <= 8000 K; -3.0 <=[Fe/H] <= +0.5. We also present the calibration of BC(V) as afunction of log(Teff) and metallicity. Finally, we comparethe resulting scale of temperatures with previous works.
| The effective temperature scale of giant stars (F0-K5). I. The effective temperature determination by means of the IRFM
We have applied the InfraRed Flux Method (IRFM) to a sample ofapproximately 500 giant stars in order to derive their effectivetemperatures with an internal mean accuracy of about 1.5% and a maximumuncertainty in the zero point of the order of 0.9%. For the applicationof the IRFM, we have used a homogeneous grid of theoretical modelatmosphere flux distributions developed by \cite[Kurucz (1993)]{K93}.The atmospheric parameters of the stars roughly cover the ranges: 3500 K<= T_eff <= 8000 K; -3.0 <= [Fe/H] <= +0.5; 0.5 <= log(g) <= 3.5. The monochromatic infrared fluxes at the continuum arebased on recent photometry with errors that satisfy the accuracyrequirements of the work. We have derived the bolometric correction ofgiant stars by using a new calibration which takes the effect ofmetallicity into account. Direct spectroscopic determinations ofmetallicity have been adopted where available, although estimates basedon photometric calibrations have been considered for some stars lackingspectroscopic ones. The adopted infrared absolute flux calibration,based on direct optical measurements of stellar angular diameters, putsthe effective temperatures determined in this work in the same scale asthose obtained by direct methods. We have derived up to fourtemperatures, TJ, TH, TK and T_{L'},for each star using the monochromatic fluxes at different infraredwavelengths in the photometric bands J, H, K and L'. They show goodconsistency over 4000 K, and there is no appreciable trend withwavelength, metallicity and/or temperature. We provide a detaileddescription of the steps followed for the application of the IRFM, aswell as the sources of error and their effect on final temperatures. Wealso provide a comparison of the results with previous work.
| Estimation of Stellar Metal Abundance. II. A Recalibration of the Ca II K Technique, and the Autocorrelation Function Method
We have recalibrated a method for the estimation of stellar metalabundance, parameterized as [Fe/H], based on medium-resolution (1-2Å) optical spectra (the majority of which cover the wavelengthrange 3700-4500 Å). The equivalent width of the Ca II K line (3933Å) as a function of [Fe/H] and broadband B-V color, as predictedfrom spectrum synthesis and model atmosphere calculations, is comparedwith observations of 551 stars with high-resolution abundances availablefrom the literature (a sevenfold increase in the number of calibrationstars that were previously available). A second method, based on theFourier autocorrelation function technique first described by Ratnatunga& Freeman, is used to provide an independent estimate of [Fe/H], ascalibrated by comparison with 405 standard-star abundances.Metallicities based on a combination of the two techniques for dwarfsand giants in the color range 0.30<=(B-V)_0<=1.2 exhibit anexternal 1 sigma scatter of approximately 0.10-0.20 dex over theabundance range -4.0<=[Fe/H]<=0.5. Particular attention has beengiven to the determination of abundance estimates at the metal-rich endof the calibration, where our previous attempt suffered from aconsiderable zero-point offset. Radial velocities, accurate toapproximately 10 km s^-1, are reported for all 551 calibration stars.
| An Estimate of H 0 from Keck Spectroscopy of the Gravitational Lens System 0957+561
We present long-slit LRIS/Keck spectroscopic observations of thegravitational lens system 0957+561. Averaged over all of our data, therest-frame velocity dispersion sigma v of the central lens galaxy G1 issigma v = 279 +/- 12 km s-1. However, there appears to be a significantdecrease in sigma v as a function of distance from the center of G1 thatis not typical of the brightest cluster galaxies. Within 0."2 of thecenter of G1, we find the average sigma v = 316 +/- 14 km s-1, whereasfor positions greater than 0."2 from the center of G1, we find theaverage sigma v = 266 +/- 12 km s-1. A plausible explanation is that G1contains a central massive dark object of mass MMDO ~ 4 x 109h^{-1}100 Mȯ (h100 = H0/100 km s-1 Mpc-1), whichcontributes to the central velocity dispersion, and that the outer valueof sigma v is the appropriate measure of the depth of the potential wellof G1. The determination of a luminosity-weighted estimate of sigma v isessential for a determination of H0 from Q0957+561; our accuratemeasurements remove one of the chief uncertainties in the assumed formof the mass distribution of the lens. Thus, with the recent apparentreduction in the uncertainty in the measurement of the time delay forthe images A and B of Q0957+561, Delta tau BA = 417 +/- 3 days (Kundicet al.), we obtain an estimate for the Hubble constant: H0 = 62 +/- 7 kms-1 Mpc-1. If for some reason the trend of sigma v with slit position isspurious and we should use the dispersion averaged along the slit, thenthe estimate of H0 increases to 67 +/- 8 km s-1 Mpc-1. These standarderrors, however, do not include any contribution from any errors in theassumed form of the mass distribution of the lens. In particular, weused the mass model described by Falco, Gorenstein, & Shapiro, asupdated by Grogin & Narayan. The reduced chi 2 of model fits to theavailable position and magnification data for this system is relativelyhigh (~4), indicating that the estimate of H0 may have a significantcontribution from model errors. Further observations, discussed herein,should allow such errors to be estimated reliably.
| Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
| The Mass-To-Light Ratios of the Draco and Ursa Minor Dwarf Spheroidal Galaxies.I. Radial Velocities from Multifiber Spectroscopy
We have measured 206 radial velocities for 94 probable members in theUrsa Minor dwarf spheroidal galaxy and 167 velocities for 91 probablemembers in the Draco dwarf spheroidal galaxy. These velocities wereobtained using the KPNO 4 m telescope with the Hydra multifiberpositioner and bench spectrograph in 1992,1993, and 1994. Bothsimulations and repeated measurements show that the median uncertaintyin these velocities is 4.0 km/s. Our velocities are compared with theother major datasets for Draco and Ursa Minor. Aside from a smallzero-point difference, there is excellent agreement between the Hydravelocities and the Olszewski et al. MMT echelle velocities. Comparisonwith the Hargreaves et al. Ursa Minor velocities reveals inconsistencieswhich we ascribe to underestimated errors in the Hargreaves et al. data,After correcting for zero-point differences, we combine the three majorsets of velocities. Our spectra recovered all of the known Carbon (C)stars in Draco and Ursa Minor and revealed one new C star in Draco andtwo in Ursa Minor. In addition, one star whose velocity is consistentwith membership in Ursa Minor has a deep and wide Hβ absorptionline in its spectrum. An initial discussion of the kinematics of the twogalaxies is presented. The systemic velocities of Draco and Ursa Minorare -293.3 +/- 1.0 and -247.4 +/- 1.0 km s^-1^, respectively. Ursa Minorshows apparent rotation about a position angle of 75^deg^ with anamplitude of about 3 km s^-1^; the morphological major axis is 53^deg^+/-5^deg^. No such rotation is found in Draco. We find a velocitydispersion of 10.4 +/- 0.9 km s^-1^ for Ursa Minor including all starsand 8.8 +/- 0.8 km s^-1^ excluding the star with the most extremevelocity. In Draco we find 10.7 +/- 0.9 km s^-1^ including all stars and8.5 +/- 0.7 km s^-1^ excluding the three stars with the most extremevelocities. These dispersions are consistent with the dispersionsmeasured in the other two studies and confirm that Draco and Ursa Minorhave the largest mass-to-light ratios of any of the dwarf spheroidals.
| On the problem of measurement of radial velocity.
Not Available
| Reddening estimation for halo red giants using UVBY photometry
Updated uvby observations for a larger sample of metal-deficient redgiants are presented and combined with a select sample of data from theliterature transformed to a common system. Using the reddening maps ofBurstein & Heiles (1982), new absolute magnitudes, distances,metallicities, and reddenings are derived for each star. Themetallicities are determined with a revised calibration of them1, (b-y) diagram based upon comparison to a complilation ofrecent spectrsoscopic abundances transformed to a common system. Thephotometric abundances agree very well with the spectroscopic; thedispersion among the residuals for 58 giants is +/- 0.16 dex. Thedereddened indices are used to show that for red giants with (Fe/H) lessthan -1.5, there is a well-defined relation in the c0,(b-y)0 diagram which exhibits only a weak dependence uponmetallicity. Use of the standard relations allows one to obtainreddening estimates for normal halo field giants and globular clustersin the appropriate metallicity range.
| Evolved GK stars near the sun. I - The old disk population
A sample of nearly two thousand GK giants with intermediate band, (R,I),DDO and Geneva photometry has been assembled. Astrometric data is alsoavailable for most of the stars. The some 800 members of the old diskpopulation in the sample yield accurate luminosities (from two sources),reddening values and chemical abundances from calibrations of thephotometric parameters. Less than one percent of the objects arepeculiar in the sense that the flux distribution is abnormal. Thepeculiarity is signaled by strong CH (and Ba II) and weak CH. The CH+stars are all spectroscopic binaries, probably with white dwarfcompanions, whereas the CH- stars are not. A broad absorption band,centered near 3500 A, is found in the CH+ stars whereas the CH- objectshave a broad emission feature in the same region. The intensity of theseabsorptions and emissions are independent of the intensity of abnormalspectral features. Ten percent of the old disk sample have a heavyelement abundance from one and a half to three times the solar value.The distribution of the heavy element abundances is nearly a normal onewith a peak near solar abundance and ranges three times to one sixthsolar. The distribution of the (U, V) velocities is independent of theheavy element abundance and does not appear to be random. Ten percent ofthe old disk stars show a CN anomaly, equally divided between CN strongand CN weak. Several stars of individual astrometric or astrophysicalimportance are isolated.
| A critical appraisal of published values of (Fe/H) for K II-IV stars
'Primary' (Fe/H) averages are presented for 373 evolved K stars ofluminosity classes II-IV and (Fe/H) values beween -0.9 and +0.21 dex.The data define a 'consensus' zero point with a precision of + or -0.018 dex and have rms errors per datum which are typically 0.08-0.16dex. The primary data base makes recalibration possible for the large(Fe/H) catalogs of Hansen and Kjaergaard (1971) and Brown et al. (1989).A set of (Fe/H) standard stars and a new DDO calibration are given whichhave rms of 0.07 dex or less for the standard star data. For normal Kgiants, CN-based values of (Fe/H) turn out to be more precise than manyhigh-dispersion results. Some zero-point errors in the latter are alsofound and new examples of continuum-placement problems appear. Thushigh-dispersion results are not invariably superior to photometricmetallicities. A review of high-dispersion and related work onsupermetallicity in K III-IV star is also given.
| Infrared observations of metal-deficient stars
Infrared magnitudes in the J, H, K and L bands for 64 metal-deficientstars spanning a wide range in effective temperature, luminosity andmetal content are presented. An accuracy of 0.02 magnitude is obtainedfor the JHK bands and 0.03 for the L filter. Infrared-infrared andoptical-infrared color-color diagrams are discussed and compared withthe mean intrinsic tracks for Population I stars. It is concluded thatinfrared colors are not notably dependent on metallicity, with someexceptions for the reddest giants, which can be also interpreted byresidual effects in the transformation equations between differentsystems. The near infrared photometric system of the Observatorio delTeide, from the Instituto de Astrofisica de Canarias, is also brieflydiscussed.
| Population studies. II - Kinematics as a function of abundance and galactocentric position for (Fe/H) of -0.6 or less
A catalog is presented of some 1200 Galactic objects which have radialvelocities and (Fe/H) abundances of -0.6 or less. These data areanalyzed to yield information on the kinematic properties of the olderpopulations of the Galaxy and on the interdependence between kinematicsand abundance. It is found that the kinematics of the availablekinematically selected stars differ from those of the nonkinematicallyselected objects. No evidence is found for any significant difference inthe kinematic properties of the various halo subgroups, nor for anydependence of kinematics on abundance. While the rotation of the halo issmall at about 37 km/s for (Fe/H) of -1.2 or less, it rises quickly forhigher abundances to a value of about 160 km/s at (Fe/H) = 0.6. Objectsin the abundance range -0.9 to -0.6 appear to belong predominantly to apopulation possessing the kinematic characteristics of a thick disk. Theimplications of these findings for the suggestion that globular clustersbelong to the same population as the noncluster objects, for the originof the thick disk, and for the mass of the Galaxy are discussed.
| A photometric search for halo binaries. I - New observatinal data. II - Results
Carney (1982) has reported JHK photometry for 76 Hyades dwarfs. Inconnection with the present investigation, results of similarobservations of field halo stars are provided along with some uvbyphotometry. In addition, older spectrophotometric and photometric dataused previously for temperature determinations have been collected. Theinfrared and uvby data were obtained primarily with the objective ofidentifying binaries with dissimilar components among a sample of fieldhalo dwarfs by comparing metallicity insensitive blue and infraredcolors. Attention is given to 111 spectrophotometric scans of 89 stars,67 uvby measures of 41 stars, 127 UBV measures of 87 stars, 147 (RI)Jmeasures of 127 stars, 8 JHK measures of eight stars in the 'HCO'system, and 212 JHK measures of 137 stars in the 'CIT' system. Themajority of these stars are dwarfs, and most of them are metal poor. Theresults of a search for binaries in 71 halo dwarf stars are alsopresented, taking into account a few other dwarfs of special interest.
| A photoelectric measurement of magnesium for late-type stars
A photoelectric index of MgH + Mg b for late-type stars has been createdby the addition of one filter bandpass to the DDO system. Measurementsshow that this index has good sensitivity to surface gravity for Kstars, and suggest that it can differentiate metal-poor halo giants fromdisk stars. From this index, involving measurement through two filtersalone, it appears that membership can be determined for stars on thegiant branch of globular clusters. It is possible that the index couldbe used, after calibration with cluster giants, to determine ages ofgiant stars in the field.
| Dynamical studies of globular clusters based on photoelectric radial velocities of individual stars. I - M3
Velocities of 111 stars in the globular cluster M3 have been measured byusing the Palomar cross-correlation radial-velocity spectrometer.Typical measuring accuracy is about 1 km/s. No velocity variation innonpulsating stars is found; the implication that the incidence ofbinarism with separations in the range 0.3-10 AU is very much smallerthan in the Population I field is clear. 'Thermal equilibrium' models ofthe King-Mitchie (1962, 1963) type with several components andanisotropic velocity distributions are constructed and found torepresent the cluster dynamics and observed light distributionadequately. The existence of two very high-velocity objects and somedifficulty with the Roche limit indicate that the thermal-equilibriummodels do not describe the high-energy end of the distribution functionadequately. There is no evidence for any very heavy remnants, and nomass that is not accounted for by evolution of the adopted mass function(which is steeper than that in the solar neighborhood).
| Intermediate-band photometry of late-type stars. VIII - Nonvariable stars in the halo population near the sun
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1979ApJ...229..158E&db_key=AST
| Absolute spectral energy distributions and /Fe/H/ values of metal-poor stars and globular clusters
Absolute spectral energy distributions for 65 metal-poor stars, spanninga wide range in temperature, luminosity, and metal content, are given.Five local globular clusters and five M31 globulars are also described.The wavelength index sequence of O'Connell (1970, 1973) has been used.Continuum and feature indices are compared internally and with those ofthe Population I stellar sequence of O'Connell. His discussion of theusefulness of these indices as temperature, luminosity, and metallicitycriteria is extended to metal-poor objects. Empirical relationshipsbetween /Fe/H/ color, and certain feature indices have been calibratedand applied to 19 objects with previously undetermined /Fe/H/ values.
| An adaptation of the Stromgren four-color system to photographic photometry.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973A&A....26..263S&db_key=AST
| The Luminosities of Late-Type Stars of Differing Metal Abundance
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972ApJ...177..665J&db_key=AST
| Determination of atmospheric parameters for G and K giants by means of photoelectric indices.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971A&A....15..123H&db_key=AST
| A Note on Stars With Motions of More Than 100 Km/Sec Perpendicular to the Galactic Plane and Galactic Mass Models
Not Available
| Stars with Motions of More Than 100 km/sec Perpendicular to the Galactic Plane
Not Available
| Six-Color Photometry of Stars. XII. Colors of Hyades and Subdwarf Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969ApJ...155..899S&db_key=AST
| Photoelectric spectrophotometry of stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1963AJ.....68..413V&db_key=AST
| A Catalogue of High-Velocity Stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1955ApJS....2..195R&db_key=AST
|
Submit a new article
Related links
Submit a new link
Member of following groups:
|
Observation and Astrometry data
| Constellation: | うしかい座 |
| Right ascension: | 14h26m54.16s |
| Declination: | +28°35'20.4" |
| Apparent magnitude: | 8.182 |
| Distance: | 318.471 parsecs |
| Proper motion RA: | 71.5 |
| Proper motion Dec: | -151.6 |
| B-T magnitude: | 9.36 |
| V-T magnitude: | 8.28 |
Catalogs and designations:
|
