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Pulkovo compilation of radial velocities for 35495 stars in a common system.
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| Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I.
We have embarked on a project, under the aegis of the Nearby Stars(NStars)/Space Interferometry Mission Preparatory Science Program, toobtain spectra, spectral types, and, where feasible, basic physicalparameters for the 3600 dwarf and giant stars earlier than M0 within 40pc of the Sun. In this paper, we report on the results of this projectfor the first 664 stars in the northern hemisphere. These resultsinclude precise, homogeneous spectral types, basic physical parameters(including the effective temperature, surface gravity, and overallmetallicity [M/H]), and measures of the chromospheric activity of ourprogram stars. Observed and derived data presented in this paper arealso available on the project's Web site.
| Stellar Kinematic Groups. II. A Reexamination of the Membership, Activity, and Age of the Ursa Major Group
Utilizing Hipparcos parallaxes, original radial velocities and recentliterature values, new Ca II H and K emission measurements,literature-based abundance estimates, and updated photometry (includingrecent resolved measurements of close doubles), we revisit the UrsaMajor moving group membership status of some 220 stars to produce afinal clean list of nearly 60 assured members, based on kinematic andphotometric criteria. Scatter in the velocity dispersions and H-Rdiagram is correlated with trial activity-based membership assignments,indicating the usefulness of criteria based on photometric andchromospheric emission to examine membership. Closer inspection,however, shows that activity is considerably more robust at excludingmembership, failing to do so only for <=15% of objects, perhapsconsiderably less. Our UMa members demonstrate nonzero vertex deviationin the Bottlinger diagram, behavior seen in older and recent studies ofnearby young disk stars and perhaps related to Galactic spiralstructure. Comparison of isochrones and our final UMa group membersindicates an age of 500+/-100 Myr, some 200 Myr older than thecanonically quoted UMa age. Our UMa kinematic/photometric members' meanchromospheric emission levels, rotational velocities, and scattertherein are indistinguishable from values in the Hyades and smaller thanthose evinced by members of the younger Pleiades and M34 clusters,suggesting these characteristics decline rapidly with age over 200-500Myr. None of our UMa members demonstrate inordinately low absolutevalues of chromospheric emission, but several may show residual fluxes afactor of >=2 below a Hyades-defined lower envelope. If one defines aMaunder-like minimum in a relative sense, then the UMa results maysuggest that solar-type stars spend 10% of their entire main-sequencelives in periods of precipitously low activity, which is consistent withestimates from older field stars. As related asides, we note six evolvedstars (among our UMa nonmembers) with distinctive kinematics that liealong a 2 Gyr isochrone and appear to be late-type counterparts to diskF stars defining intermediate-age star streams in previous studies,identify a small number of potentially very young but isolated fieldstars, note that active stars (whether UMa members or not) in our samplelie very close to the solar composition zero-age main sequence, unlikeHipparcos-based positions in the H-R diagram of Pleiades dwarfs, andargue that some extant transformations of activity indices are notadequate for cool dwarfs, for which Ca II infrared triplet emissionseems to be a better proxy than Hα-based values for Ca II H and Kindices.
| Pre-main-sequence stars in the young open cluster NGC 1893. I. A spectroscopic search for candidates in the area photometrically surveyed
We present low-resolution spectroscopy of the majority of the stars inthe field of NGC 1893 which were classified asnon-members based on the photometry of Marco et al. (2001). We separatefield stars from pre-main-sequence members based on a combination ofspectral type and photometric indices which allows us to determine thereddening to the objects. For candidates to pre-main-sequence objects,we present intermediate-resolution spectra. We confirm 3 F-typeemission-line objects as massive T Tauri stars in NGC1893 and find two good candidates for being absorption-lineHerbig A stars. A B5 star is a very good candidate for anabsorption-line Herbig B star. We also investigate the nature ofemission-line B-type stars close to the cluster centre. Availableevidence suggests that both classical Be stars and Herbig Be stars arepresent in NGC 1893. Based on observations obtainedat the Asiago Observatory (Italy), the Isaac Newton Telescope (La Palma,Spain) and Observatoire de Haute Provence (CNRS, France).
| The geometry of stellar motions in the nucleus region of the Ursa Major kinematic group
The structure of the central part of the UMa stellar kinematic group wasconsidered according to the data from Hipparcos, Tycho and ACTcatalogues. We have shown that in the space occupied by the nucleusthere are several populations of stars. The first includes ten starswhich are very compactly located in the proper motion diagram and have anormal proper motion distribution. The second group includes six starswith large kinematic difference and there are six field stars placedhere too. The question about their coexistence in a common region ofspace remains open. The well-known stars Mizar and Alcor appear tobelong to the different subsystems and do not belong to a unique stellarsystem. The published radial velocities, as a rule, are determined withinsufficient accuracy compared to the errors of the currently availableproper motions. A high precision in the radial velocities measurementsis necessary for a thorough study of the kinematics of stars inside UMastar system.
| High resolution spectroscopy over lambda lambda 8500-8750 Å for GAIA. I. Mapping the MKK classification system
We present an Echelle+CCD high resolution spectroscopic atlas (0.25Ä/pix dispersion, 0.43 Ä FWHM resolution and 20 000 resolvingpower) mapping the MKK classification system over the interval lambdalambda 8500-8750 Ä. The wavelength interval is remarkably free fromtelluric lines and it is centered on the near-IR triplet of Ca II, thehead of hydrogen Paschen series and several strong metallic lines. Thespectra of 131 stars of types between O4 and M8 and luminosity classes Ithrough V are included in the atlas. Special care was put in maintainingthe highest instrumental homogeneity over the whole set of data. Thecapability to derive accurate MKK spectral types from high resolutionobservations over the interval lambda lambda 8500-8750 Ä isdiscussed. The observations have been performed as part of an evaluationstudy of possible spectroscopic performances for the astrometric missionGAIA planned by ESA. Tables~3 and 4 are only available in electronicform at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)or via http://cdsweb.u-strasbg.fr/ Abstract.html}\fnmsep\thanks{ Thespectra of the stars listed in Table~2 are also available in electronicform at the CDS or via the personal HomePagehttp://ulisse.pd.astro.it/Astro/Atlases/}\fnmsep\thanks{ Figures 3--28are only available in electronic form at http://www.edpsciences.com
| GAIA Spectroscopy: Proposing the 8500--8750 Angstroms Region and Evaluating the Performances
We propose the Gaia spectroscopic observations to be performed over thewavelength interval 8500--8750 Angstroms, with an optimal dispersion of0.25 Angstroms/pix (or 1000 pixels budget per spectrum) and a 2 pixelPSF. In this paper, on the base of extensive observations as well assynthetic spectra and simulations, we review the spectroscopicperformances expected for Gaia: radial and rotational velocities,spectral classification, detection of mass-loss and spectralpeculiarities, chemical abundance analysis and reddening estimates fromthe 8620 Angstroms diffuse interstellar band. Lower dispersion spectra(corresponding to smaller pixel budgets) are considered too.
| A spectroscopic study of the long-period dwarf nova DX Andromedae
We present time-resolved spectra of the double-lined dwarf nova DX Andin quiescence from two campaigns in 1989 and 1993. Using an unusualmethod, we have reconstructed the radial velocity amplitudes and phasesof the absorption and emission line components from data suffering fromserious wavelength calibration problems by measuring the relativemotions of as well as the phase shift between the two line systems. Weare thus able to refine the orbital period and to determine a long-termephemeris. The relative contribution of the primary to the total lightwas measured as a function of wavelength, permitting to correct theabsorption line spectrum for the veiling effect. The secondary starexhibits several spectral peculiarities: in addition to the enhanced CaI absorption lines reported previously, we find several Cr I lines to besignificantly stronger than in a comparison star of similar spectraltype.
| Spectroscopy of the dwarf nova CG Draconis.
We present spectroscopic observations of the dwarf nova CG Dra whichexhibits a two component spectrum. Absorption lines stand out clearlyand can be classified as belonging to spectral type K5 +/- 2. Thewavelength dependent veiling fraction could be determined. The emissionspectrum is not untypical for a dwarf nova but shows some peculiaritiesin the helium lines. Radial velocity measurements indicate a period ofeither 4^h^32^m^ or 5^h^37^m^, too short for the absorption linespectrum if interpreted within the canonical CV model. Worse, theabsorption line radial velocity amplitude is approximately a factor 30less than that for the Balmer lines and in phase with them. This cannoteasily be explained in the framework of standard CV models. However, itcannot be excluded that the RV variations of the absorption lines areaccidental and that the corresponding star is not a component of thecataclysmic variable.
| An Atlas of the infrared spectral region. II. The late-type stars (G - M)
This Atlas illustrates the behavior of late type stars (F, G, K and M)in the near infrared 8400-8800 Angstrom region with a resolution ofabout 2 degrees. Seventeen figures illustrate the spectral sequence andluminosity classes V, III, Ib and Ia. Four figures illustrate peculiarspectra, namely those of Am stars, composites, weak metal stars and Sand C type objects. The complete Atlas is also available as FITS filesfrom the CDS de Strasbourg and other data centers.
| The Tokyo PMC catalog 90-93: Catalog of positions of 6649 stars observed in 1990 through 1993 with Tokyo photoelectric meridian circle
The sixth annual catalog of the Tokyo Photoelectric Meridian Circle(PMC) is presented for 6649 stars which were observed at least two timesin January 1990 through March 1993. The mean positions of the starsobserved are given in the catalog at the corresponding mean epochs ofobservations of individual stars. The coordinates of the catalog arebased on the FK5 system, and referred to the equinox and equator ofJ2000.0. The mean local deviations of the observed positions from theFK5 catalog positions are constructed for the basic FK5 stars to comparewith those of the Tokyo PMC Catalog 89 and preliminary Hipparcos resultsof H30.
| Are Both Stars in a Classic T Tauri Binary Classic T Tauri Stars?
Large near-IR color excesses and emission-line spectra indicate thepresence of optically thick circumstellar accretion disks and activeboundary layers in young stars. We investigate whether this classic TTauri (TT) behavior is found in one or both members of a binary systempreviously identified as a TT on the basis of the unresolved light. Weconsider the angularly resolved Br gamma and, in one case, Na I, spectraof four close (1."3--2."6) TT systems. We also take into account theangularly resolved near-IR (K--L) colors of eight additional youngbinaries with separations between 0."3 and 2."5. We find that for all 12systems, both components show, or have shown in the history of theirobservation, evidence for TT behavior. We demonstrate that this cannotbe the result of random pairing of a population of single TT andweak-lined T Tauri (WT) stars. We speculate that the result that inner,AU-sized disks tend to survive for a similar length of time in bothcomponents of a close (0."3--2."6) binary suggests that a circumbinaryenvelope effectively regulates the common evolution of the inner disks.
| 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.
| Far-infrared observations of chromospherically active stars in stellar clusters.
Using the IRAS database we have searched for far-infrared emission froma large number of chromospherically active dwarf stars (including flarestars) in stellar clusters of different ages and distances. Only starsin the nearest clusters (<50pc) were detected by IRAS. Their 12μmluminosity (L_12_) is in the range 0.2-5x10^31^erg/s. We find that thedetected emission is photospheric in origin and that there is nocorrelation of flux either with age or with stellar-activity levels. Thecluster stars' far-infrared radiation characteristics are very similarto those of solar-vicinity field stars of similar spectral type andchromospheric activity.
| The general catalogue of trigonometric [stellar] paralaxes
Not Available
| Spectral classifications in the near infrared of stars with composite spectra. I. The study of MK standards.
Up to now the spectral classifications of the cool components ofcomposite spectra obtained in the 3800-4800A wavelength region have beenvery disparate. These disparities are due to the fact that the spectraof the evolved cool component are strongly veiled by that of the hotterdwarf component, which makes a classification very difficult. We proposeto study these systems in the near infrared (8380-8780A). In thisspectral domain the magnitude difference between the spectra of thecomponents is in general sufficiently large so that one observespractically only the spectrum of the cool component. In this first paperwe provide, for a sample of MK standards, the relations between theequivalent width (Wlambda_ ) of certain lines and thespectral classifications. For the cool G, K and M type stars, the linesconsidered are those of the calcium triplet (Ca II 8498, 8542 and 8662),of iron (Fe I 8621 and 8688), of titanium (Ti I 8426 and 8435) and ofthe blend λ8468. The use of certain line intensity ratiospermits, after eliminating partially the luminosity effects, a firstapproach to the spectral type. For the hotter stars of types O, B, A andF we study the behavior of the hydrogen lines (P12 and P14), the calciumlines (Ca II 8498 and 8542) as well as those of the oxygen (O I 8446).The latter line presents a very characteristic profile for stars of lowrotation and therefore in Am stars, which are frequently found among thecomposite spectrum binaries. Among the cooler stars of our sample, only6% present real anomalies with respect to the MK classifications. Thisresult is very encouraging for undertaking the classification of asample of composite spectra. The spectra were taken at the Observatoirede Haute-Provence (OHP) with the CARELEC spectrograph at the 193 cmtelescope, with a dispersion of 33 A/mm.
| Detection of EUV emission from the low activity dwarf HD 4628: Evidence for a cool corona
We present observations of low activity late-type stars obtained withthe Extreme Ultraviolet Explorer (EUVE). These stars are the slowestrotators, and acoustic heating may dominate their outer atmosphericheating process. We report detection of EUV emission from the lowacitivity K dwarf HD 4628 during the EUVE Deep Survey in the Lexan/boranband. This detection, in conjunction with the non-detection of thisobject in the ROSAT Position Sensitive Proportional Counter (PSPC)all-sky survey, suggests the existence of a cool corona with acharacteristic temperature of less than 106 K. The flux andspectral signature are consistent with current theories of acousticheating.
| The evolution of the lithium abundances of solar-type stars. II - The Ursa Major Group
We draw upon a recent study of the membership of the Ursa Major Group(UMaG) to examine lithium among 0.3 Gyr old solar-type stars. For most Gand K dwarfs, Li confirms the conclusions about membership in UMaGreached on the basis of kinematics and chromospheric activity. G and Kdwarfs in UMaG have less Li than comparable stars in the Pleiades. Thisindicates that G and K dwarfs undergo Li depletion while they are on themain sequence, in addition to any pre-main-sequence depletion they mayhave experienced. Moreover, the Li abundances of the Pleiades K dwarfscannot be attributed to main-sequence depletion alone, demonstratingthat pre-main-sequence depletion of Li also takes place. The sun's Liabundance implies that the main-sequence mechanism becomes lesseffective with age. The hottest stars in UMaG have Li abundances likethose of hot stars in the Pleiades and Hyades and in T Tauris, and thetwo genuine UMaG members with temperatures near Boesgaard's Li chasmhave Li abundances consistent with that chasm developing fully by 0.3Gyr for stars with UMaG's metallicity. We see differences in theabundance of Li between UMaG members of the same spectral types,indicating that a real spread in the lithium abundance exists withinthis group.
| Stellar kinematic groups. I - The Ursa Major group
The Ursa Major Group (UMaG) is studied as a test case for theauthenticity of Stellar Kinematic Groups, using Coravel radialvelocities, recent compilations of astrometric data, and newspectroscopic observations. Spectroscopic age indicators, particularlyindices of the strength of chromospheric emission, are applied tosolar-type candidate members of UMaG, and it is shown that stars thatmeet the spectroscopic criteria also have kinematics that agree betterwith the space motions of the nucleus of UMaG than does the startingsample as a whole. The primary limitation on the precision of kinematicsis now parallaxes instead of radial velocities. These more restrictivekinematic criteria are then applied to other UMaG candidates and a listsummarizing membership is presented. UMaG is also examined as a cluster,confirming its traditional age of 0.3 Gyr, and a mean Fe/H of -0.08 +/-0.09 for those stars most likely to be bona fide members.
| Magnetic structure in cool stars. XVII - Minimum radiative losses from the outer atmosphere
The emissions in several chromospheric and transition region lines andin coronal soft X-rays are analyzed for a sample of cool stars. Thenature of the lower-limit flux densities is explored, and evidence isgiven for the possibility of a basal, nonmagnetic heating mechanismbeing responsible for these emission fluxes up to, and perhapsincluding, the upper transition region. It is argued that the excessflux density, derived by subtraction of the basal flux density from theobserved stellar flux, is the proper measure of magnetic activity. Thelevel of the basal flux density as a function of color is determined tobe 2 x 10 exp 6 erg/sq cm/s for F-type stars and 2 x 10 exp 5 erg/sqcm/s for K-type stars.
| X-ray studies of coeval star samples. III - X-ray emission in the Ursa Major stream
Results are reported from a comprehensive survey of X-ray emission fromstars known or suspected to be members of the UMa cluster and/or stream.Of the 42 UMa member stars surveyed, 18 were detected as X-ray sources,and spectral analysis was performed for 10 stars with sufficient X-raycounts. Consideration is given to relations between X-ray luminosity,color, and kinematics of the sample stars, and the X-ray spectra of theUMa stars are discussed in the context of the general problem of stellarX-ray temperatures. Also confirmed is the lack of X-ray-emitting Adwarfs among UMa members; among stars of later spectra type there is arather large dispersion in X-ray luminosity. This dispersion cannotreadily be explained by contamination with field star interlopers andappears rather to be a property of the UMa X-ray luminosity distributionfunction.
| The Perkins catalog of revised MK types for the cooler stars
A catalog is presented listing the spectral types of the G, K, M, and Sstars that have been classified at the Perkins Observatory in therevised MK system. Extensive comparisons have been made to ensureconsistency between the MK spectral types of stars in the Northern andSouthern Hemispheres. Different classification spectrograms have beengradually improved in spite of some inherent limitations. In thecatalog, the full subclasses used are the following: G0, G5, G8, K0, K1,K2, K3, K4, K5, M0, M1, M2, M3, M4, M5, M6, M7, and M8. Theirregularities are the price paid for keeping the general scheme of theoriginal Henry Draper classification.
| A list of MK standard stars
Not Available
| 1988 Revised MK Spectral Standards for Stars GO and Later
Not Available
| Chromospheric and transition-region emission from young solar-type stars in clusters, kinematic groups, and the field
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1987AJ.....93..920S&db_key=AST
| 1985 revised MK spectral standards : stars GO and later
Not Available
| Stellar chromospheres and coronae in the Ursa Major Cluster stars
IUE spectra of 18 proposed members of the Ursa Major Cluster andEinstein X-ray images of 11 of these stars are discussed. Thirteenstars, six in the nucleus and seven in the extended comoving stream, areprobably true members of the UMa Cluster in that their brightultraviolet and X-ray surface fluxes indicate youth. Four stars, one inthe nucleus and three in the stream, exhibit weak ultraviolet and/orX-ray emission suggesting that they are old field stars that have thesame space motion as the UMa Cluster. The X-ray surface fluxes of theUMa Cluster stars appear to be brighter than those of the Hyades Clusterstars, consistent with their relative ages. It is argued thatchromospheres and transition regions could be present in dwarf starshotter than B-V of about 0.30, but are unobservable in IUE spectra dueto the rapid increase in photospheric flux in hotter stars.
| Revised MK Spectral Standard Stars Later than G0
Not Available
| Revised MK spectral types for G, K, and M stars
A catalog of spectral types of 552 G, K, and M stars is presented, whichis classified on the revised MK system. Stellar representatives of thehalo, disk, and arm populations in all parts of the sky are included.Photoelectric V magnitudes are given, as are intensity estimates of anyfeatures which make the spectrum appear peculiar as compared to thespectrum of a similar normal star. Abundance indices are also providedin the following lines or bands: CN, barium, Fe, calcium, and CH.
| Spectral types in the Ursa major stream.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1978PASP...90..429L&db_key=AST
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Pozíciós és asztrometriai adatok
| Csillagkép: | Kis Medve |
| Rektaszcenzió: | 14h12m27.05s |
| Deklináció: | +67°35'10.2" |
| Vizuális fényesség: | 8.546 |
| Távolság: | 38.625 parszek |
| RA sajátmozgás: | 142.5 |
| Dec sajátmozgás: | -11.1 |
| B-T magnitude: | 9.555 |
| V-T magnitude: | 8.63 |
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