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Spectrophotometric analysis of the T Tauri star GQ Lupi A
Context: GQ Lup A is a classical T Tauri star that shows clear signs ofaccretion through the presence of inverse P Cygni profiles in its mainemission lines. Recently, Neuhäuser et al. (2005, A&A, 435,L13) found a co-moving sub-stellar companion of GQ Lup A, raising theimportance of determining precise stellar parameters, system age, anddistance to GQ Lup. Aims: Our main objective is to usespectrophotometric time series to determine GQ Lup A stellar parametersand predict its photospheric spectral distribution. The excess spectralluminosity can then be measured and employed to test predictions ofmagnetospheric accretion models of classical T Tauri stars. Methods: We present the analysis of 18 spectrophotometric observationsof the T Tauri star GQ Lup A (K7) obtained with the Boller & Chivensspectrograph at the 1.52 m ESO telescope in La Silla. We also revisitedarchival photometric data of this star, comparing previous light curvevariability with our more recent data. Results: We determined thephotospheric flux of GQ Lup A on each observing night and obtained thestellar radius (Rstar = 1.8 ± 0.3 Rȯ),adopting a mean distance of 150 ± 20 pc to the Lupus 1 cloud.Assuming a K7 V temperature of 4060 K, the luminosity of GQ Lup A isLstar = 0.8 ± 0.3 Lȯ. Standardevolutionary models indicate a stellar mass of Mstar = 0.8± 0.2 Mȯ and an age of 3 ± 2 Myr. GQ Lup Aspectral lines are consistent with a projected rotational velocity of vsin i = 6.5 ± 2.0 km s-1. We measured the excessemission - veiling - and used the resulting photospheric spectraldistribution to calculate a stellar extinction (A_V) of 0.5 ±0.1. The veiling was found to be variable and periodic at 10.7 ±1.6 days, which is consistent with the period of GQ Lup A obtained fromarchival B band photometric data (10.43 ± 0.12 days). The starexhibits strong emission lines with substantial variability in flux. Theemission line fluxes are strongly correlated with one another but notwith veiling.
| The effect of activity on stellar temperatures and radii
Context: Recent analyses of low-mass eclipsing binary stars haveunveiled a significant disagreement between the observations andpredictions of stellar structure models. Results show that theoreticalmodels underestimate the radii and overestimate the effectivetemperatures of low-mass stars but yield luminosities that accord withobservations. A hypothesis based upon the effects of stellar activitywas put forward to explain the discrepancies. Aims: In this paper westudy the existence of the same trend in single active stars and providea consistent scenario to explain systematic differences between activeand inactive stars in the H-R diagram reported earlier. Methods: Theanalysis is done using single field stars of spectral types late-K and Mand computing their bolometric magnitudes and temperatures throughinfrared colours and spectral indices. The properties of the stars insamples of active and inactive stars are compared statistically toreveal systematic differences. Results: After accounting for a numberof possible bias effects, active stars are shown to be cooler thaninactive stars of similar luminosity therefore implying a larger radiusas well, in proportions that are in excellent agreement with those foundfrom eclipsing binaries. Conclusions: The present results generalisethe existence of strong radius and temperature dependences on stellaractivity to the entire population of low-mass stars, regardless of theirmembership in close binary systems.Tables 1 and 2 are 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/cgi-bin/qcat?J/A+A/478/507
| Speckle interferometry of nearby multiple stars. IV. Measurements in 2004 and new orbits
The results of speckle interferometric observations of 104 binary and 6triple stars performed at the BTA 6 m telescope in 2004 October arepresented. Nearby low-mass stars are mostly observed for the program,among which 59 there are new binaries recently discovered by theHipparcos astrometric satellite. Concurrently with thediffraction-limited position measurements we obtained 154 brightnessratio measurements of binary and multiple star components in differentbands of the visible spectrum. New, first-resolved binaries are thesymbiotic star CH Cyg with a weak companion at 0.043″ separationand the pair of red dwarfs, GJ 913 = HIP 118212. In addition, we derivedthe orbital parameters for two interferometric systems: the CN-giantpair HD 210211 = HIP 109281 (P = 10.7 yr) and the G2V-K2V G2V-K2V binaryGJ 9830 = HIP 116259 (P = 15.7 yr).
| The Gemini Deep Planet Survey
We present the results of the Gemini Deep Planet Survey, a near-infraredadaptive optics search for giant planets and brown dwarfs around 85nearby young stars. The observations were obtained with the Altairadaptive optics system at the Gemini North telescope, and angulardifferential imaging was used to suppress the speckle noise of thecentral star. Typically, the observations are sensitive to angularseparations beyond 0.5" with 5 σ contrast sensitivities inmagnitude difference at 1.6 μm of 9.5 at 0.5", 12.9 at 1", 15.0 at2", and 16.5 at 5". These sensitivities are sufficient to detect planetsmore massive than 2 MJ with a projected separation in therange 40-200 AU around a typical target. Second-epoch observations of 48stars with candidates (out of 54) have confirmed that all candidates areunrelated background stars. A detailed statistical analysis of thesurvey results is presented. Assuming a planet mass distributiondn/dm~m-1.2 and a semimajor-axis distributiondn/da~a-1, the 95% credible upper limits on the fraction ofstars with at least one planet of mass 0.5-13 MJ are 0.28 forthe range 10-25 AU, 0.13 for 25-50 AU, and 0.093 for 50-250 AU; thisresult is weakly dependent on the semimajor-axis distribution power-lawindex. The 95% credible interval for the fraction of stars with at leastone brown dwarf companion having a semimajor axis in the range 25-250 AUis 0.019+0.083-0.015, irrespective of anyassumption on the mass and semimajor-axis distributions. Theobservations made as part of this survey have resolved the stars HD14802, HD 166181, and HD 213845 into binaries for the first time.Based on observations obtained at the Gemini Observatory, which isoperated by the Association of Universities for Research in Astronomy,Inc., under a cooperative agreement with the NSF on behalf of the Geminipartnership: the National Science Foundation (United States), theParticle Physics and Astronomy Research Council (United Kingdom), theNational Research Council (Canada), CONICYT (Chile), the AustralianResearch Council (Australia), CNPq (Brazil), and CONICET (Argentina).
| GJ 900: A new hierarchical system with low-mass components
Speckle interferometric observations made with the 6 m telescope of theSpecial Astrophysical Observatory of the Russian Academy of Sciences in2000 revealed the triple nature of the nearby ( π Hip =51.80 ± 1.74 mas) low-mass young (≈ 200 Myr) star GJ 900. Theconfiguration of the triple system allowed it to be dynamicallyunstable. Differential photometry performed from 2000 through 2004yielded I- and K-band absolute magnitudes and spectral types for thecomponents to be I A =6.66±0.08, I B=9.15±0.11, I C =10.08±0.26, K A=4.84±0.08, K B =6.76±0.20, K C=7.39±0.31, Sp A ≈K5‑K7, Sp B≈M3‑M4, Sp C ≈M5‑M6. The“mass-luminosity” relation is used to estimate theindividual masses of the components: M A ≈0.64 Mȯ, M B ≈0.21 M ȯ, M C ≈0.13 M ȯ. From the observations of thecomponents’ relative motion in the period 2000 2006, we concludethat GJ 900 is a hierarchical triple star with the possible orbitalperiods PA-BC≈80 yrs and PBC≈20 yrs. Ananalysis of the 2MASS images of the region around GJ 900 leads us tosuggest that the system can include other very-low-mass components.
| Proper-motion binaries in the Hipparcos catalogue. Comparison with radial velocity data
Context: .This paper is the last in a series devoted to the analysis ofthe binary content of the Hipparcos Catalogue. Aims: .Thecomparison of the proper motions constructed from positions spanning ashort (Hipparcos) or long time (Tycho-2) makes it possible to uncoverbinaries with periods of the order of or somewhat larger than the shorttime span (in this case, the 3 yr duration of the Hipparcos mission),since the unrecognised orbital motion will then add to the propermotion. Methods: .A list of candidate proper motion binaries isconstructed from a carefully designed χ2 test evaluatingthe statistical significance of the difference between the Tycho-2 andHipparcos proper motions for 103 134 stars in common between the twocatalogues (excluding components of visual systems). Since similar listsof proper-motion binaries have already been constructed, the presentpaper focuses on the evaluation of the detection efficiency ofproper-motion binaries, using different kinds of control data (mostlyradial velocities). The detection rate for entries from the NinthCatalogue of Spectroscopic Binary Orbits (S_B^9) is evaluated, as wellas for stars like barium stars, which are known to be all binaries, andfinally for spectroscopic binaries identified from radial velocity datain the Geneva-Copenhagen survey of F and G dwarfs in the solarneighbourhood. Results: .Proper motion binaries are efficientlydetected for systems with parallaxes in excess of ~20 mas, and periodsin the range 1000-30 000 d. The shortest periods in this range(1000-2000 d, i.e., once to twice the duration of the Hipparcos mission)may appear only as DMSA/G binaries (accelerated proper motion in theHipparcos Double and Multiple System Annex). Proper motion binariesdetected among S_B9 systems having periods shorter than about400 d hint at triple systems, the proper-motion binary involving acomponent with a longer orbital period. A list of 19 candidate triplesystems is provided. Binaries suspected of having low-mass(brown-dwarf-like) companions are listed as well. Among the 37 bariumstars with parallaxes larger than 5 mas, only 7 exhibit no evidence forduplicity whatsoever (be it spectroscopic or astrometric). Finally, thefraction of proper-motion binaries shows no significant variation amongthe various (regular) spectral classes, when due account is taken forthe detection biases.Full Table [see full textsee full text] is 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/cgi-bin/qcat?J/A+A/464/377
| Search for associations containing young stars (SACY). I. Sample and searching method
We report results from a high-resolution optical spectroscopic surveyaimed to search for nearby young associations and young stars amongoptical counterparts of ROSAT All-Sky Survey X-ray sources in theSouthern Hemisphere. We selected 1953 late-type (B-V~≥~0.6),potentially young, optical counterparts out of a total of 9574 1RXSsources for follow-up observations. At least one high-resolutionspectrum was obtained for each of 1511 targets. This paper is the firstin a series presenting the results of the SACY survey. Here we describeour sample and our observations. We describe a convergence method in the(UVW) velocity space to find associations. As an example, we discuss thevalidity of this method in the framework of the β Pic Association.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| The Carina-Near Moving Group
We identify a group of ~20 comoving, mostly southern hemisphere, ~200Myr old stars near Earth. Of the stars likely to be members of thisCarina-Near moving group, in either its nucleus (~30 pc from Earth) orits surrounding stream, all but three are plausible members of amultiple star system. The nucleus is (coincidentally) located quiteclose to the nucleus of the AB Doradus moving group notwithstanding thatthe two groups have substantially different ages and Galactic spacemotions, UVW.
| Resolved Hubble space spectroscopy of ultracool binary systems
Using the low-resolution mode of the Space Telescope ImagingSpectrograph (STIS) aboard the Hubble Space Telescope (HST), we obtainspectra from 20 spatially-resolved, ultracool dwarfs, eighteen of whichbelong to nine very low-mass binary systems with known angularseparations in the range 0.37 arcsec-0.098 arcsec. For these dwarfs, wederive their spectral types to be in the range dM7.5 to dL6 by eitherobtaining their PC3 index value or by comparing our STIS spectra withground-based spectra of similar spectral resolution from Martínet al. (1999b). We have searched for Hα emission in each object,but the emission is clearly detected in only two of them. We find thatthe distribution of Hα emission in our sample is statisticallydifferent from that of single field dwarfs, suggesting an intriguinganti-correlation between chromospheric activity and binarity for M7-M9.5dwarfs. We provide strength measuments of the main photosphericfeatures. We derive calibrations of spectral subclasses versus F814W andK-band absolute magnitudes for a subset of 10 dwarfs in 5 binaries thathave known trigonometric parallaxes.
| Speckle interferometry of nearby multiple stars. III.
Not Available
| Statistical Constraints for Astrometric Binaries with Nonlinear Motion
Useful constraints on the orbits and mass ratios of astrometric binariesin the Hipparcos catalog are derived from the measured proper motiondifferences of Hipparcos and Tycho-2 (Δμ), accelerations ofproper motions (μ˙), and second derivatives of proper motions(μ̈). It is shown how, in some cases, statistical bounds can beestimated for the masses of the secondary components. Two catalogs ofastrometric binaries are generated, one of binaries with significantproper motion differences and the other of binaries with significantaccelerations of their proper motions. Mathematical relations betweenthe astrometric observables Δμ, μ˙, and μ̈ andthe orbital elements are derived in the appendices. We find a remarkabledifference between the distribution of spectral types of stars withlarge accelerations but small proper motion differences and that ofstars with large proper motion differences but insignificantaccelerations. The spectral type distribution for the former sample ofbinaries is the same as the general distribution of all stars in theHipparcos catalog, whereas the latter sample is clearly dominated bysolar-type stars, with an obvious dearth of blue stars. We point outthat the latter set includes mostly binaries with long periods (longerthan about 6 yr).
| A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)
The LSPM catalog is a comprehensive list of 61,977 stars north of theJ2000 celestial equator that have proper motions larger than 0.15"yr-1 (local-background-stars frame). The catalog has beengenerated primarily as a result of our systematic search for high propermotion stars in the Digitized Sky Surveys using our SUPERBLINK software.At brighter magnitudes, the catalog incorporates stars and data from theTycho-2 Catalogue and also, to a lesser extent, from the All-SkyCompiled Catalogue of 2.5 million stars. The LSPM catalog considerablyexpands over the old Luyten (Luyten Half-Second [LHS] and New LuytenTwo-Tenths [NLTT]) catalogs, superseding them for northern declinations.Positions are given with an accuracy of <~100 mas at the 2000.0epoch, and absolute proper motions are given with an accuracy of ~8 masyr-1. Corrections to the local-background-stars propermotions have been calculated, and absolute proper motions in theextragalactic frame are given. Whenever available, we also give opticalBT and VT magnitudes (from Tycho-2, ASCC-2.5),photographic BJ, RF, and IN magnitudes(from USNO-B1 catalog), and infrared J, H, and Ks magnitudes(from 2MASS). We also provide an estimated V magnitude and V-J color fornearly all catalog entries, useful for initial classification of thestars. The catalog is estimated to be over 99% complete at high Galacticlatitudes (|b|>15deg) and over 90% complete at lowGalactic latitudes (|b|>15deg), down to a magnitudeV=19.0, and has a limiting magnitude V=21.0. All the northern starslisted in the LHS and NLTT catalogs have been reidentified, and theirpositions, proper motions, and magnitudes reevaluated. The catalog alsolists a large number of completely new objects, which promise to expandvery significantly the census of red dwarfs, subdwarfs, and white dwarfsin the vicinity of the Sun.Based on data mining of the Digitized Sky Surveys (DSSs), developed andoperated by the Catalogs and Surveys Branch of the Space TelescopeScience Institute (STScI), Baltimore.Developed with support from the National Science Foundation (NSF), aspart of the NASA/NSF NStars program.
| A New Multiple Stellar System in the Solar Neighborhood
Adaptive optics-corrected images obtained with the Coronagraphic Imagerwith Adaptive Optics instrument at the 8.2 m Subaru Telescope show thepresence of two subarcsecond companions to the nearby (d=19.3 pc) youngstar GJ 900, which was previously classified as a single member of theIC 2391 supercluster. The two companions are redder than the primary andshare the same proper motion. The projected separations of B and C fromthe primary are 10 and 14.5 AU, respectively. The estimated masses forthe two new companions depend strongly on the age of the system. For therange of ages found in the literature for IC 2391 supercluster members(from 35 to 200 Myr), the expected masses range from 0.2 to 0.4Msolar for the B component and from 0.09 to 0.22Msolar for the C component. The determination of the dynamicmass of the faintest component of GJ 900 will yield the age of thesystem using theoretical evolutionary tracks. The apparent separationsof the GJ 900 system components meet the observational criterion for anunstable Trapezium-type system, but this could be a projection effect.Further observations are needed to establish the nature of thisinteresting low-mass multiple system.
| The Hamburg/RASS Catalogue of optical identifications. Northern high-galactic latitude ROSAT Bright Source Catalogue X-ray sources
We present the Hamburg/RASS Catalogue (HRC) of optical identificationsof X-ray sources at high-galactic latitude. The HRC includes all X-raysources from the ROSAT Bright Source Catalogue (RASS-BSC) with galacticlatitude |b| >=30degr and declination delta >=0degr . In thispart of the sky covering ~ 10 000 deg2 the RASS-BSC contains5341 X-ray sources. For the optical identification we used blue Schmidtprism and direct plates taken for the northern hemisphere Hamburg QuasarSurvey (HQS) which are now available in digitized form. The limitingmagnitudes are 18.5 and 20, respectively. For 82% of the selectedRASS-BSC an identification could be given. For the rest either nocounterpart was visible in the error circle or a plausibleidentification was not possible. With ~ 42% AGN represent the largestgroup of X-ray emitters, ~ 31% have a stellar counterpart, whereasgalaxies and cluster of galaxies comprise only ~ 4% and ~ 5%,respectively. In ~ 3% of the RASS-BSC sources no object was visible onour blue direct plates within 40\arcsec around the X-ray sourceposition. The catalogue is used as a source for the selection of(nearly) complete samples of the various classes of X-ray emitters.
| Improved Astrometry and Photometry for the Luyten Catalog. II. Faint Stars and the Revised Catalog
We complete construction of a catalog containing improved astrometry andnew optical/infrared photometry for the vast majority of NLTT starslying in the overlap of regions covered by POSS I and by the secondincremental Two Micron All Sky Survey (2MASS) release, approximately 44%of the sky. The epoch 2000 positions are typically accurate to 130 mas,the proper motions to 5.5 mas yr-1, and the V-J colors to0.25 mag. Relative proper motions of binary components are measured to 3mas yr-1. The false-identification rate is ~1% for11<~V<~18 and substantially less at brighter magnitudes. Theseimprovements permit the construction of a reduced proper-motion diagramthat, for the first time, allows one to classify NLTT stars intomain-sequence (MS) stars, subdwarfs (SDs), and white dwarfs (WDs). We inturn use this diagram to analyze the properties of both our catalog andthe NLTT catalog on which it is based. In sharp contrast to popularbelief, we find that NLTT incompleteness in the plane is almostcompletely concentrated in MS stars, and that SDs and WDs are detectedalmost uniformly over the sky δ>-33deg. Our catalogwill therefore provide a powerful tool to probe these populationsstatistically, as well as to reliably identify individual SDs and WDs.
| Hipparcos red stars in the HpV_T2 and V I_C systems
For Hipparcos M, S, and C spectral type stars, we provide calibratedinstantaneous (epoch) Cousins V - I color indices using newly derivedHpV_T2 photometry. Three new sets of ground-based Cousins V I data havebeen obtained for more than 170 carbon and red M giants. These datasetsin combination with the published sources of V I photometry served toobtain the calibration curves linking Hipparcos/Tycho Hp-V_T2 with theCousins V - I index. In total, 321 carbon stars and 4464 M- and S-typestars have new V - I indices. The standard error of the mean V - I isabout 0.1 mag or better down to Hp~9 although it deteriorates rapidly atfainter magnitudes. These V - I indices can be used to verify thepublished Hipparcos V - I color indices. Thus, we have identified ahandful of new cases where, instead of the real target, a random fieldstar has been observed. A considerable fraction of the DMSA/C and DMSA/Vsolutions for red stars appear not to be warranted. Most likely suchspurious solutions may originate from usage of a heavily biased color inthe astrometric processing.Based on observations from the Hipparcos astrometric satellite operatedby the European Space Agency (ESA 1997).}\fnmsep\thanks{Table 7 is 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/397/997
| The Palomar/MSU Nearby Star Spectroscopic Survey. III. Chromospheric Activity, M Dwarf Ages, and the Local Star Formation History
We present high-resolution echelle spectroscopy of 676 nearby M dwarfs.Our measurements include radial velocities, equivalent widths ofimportant chromospheric emission lines, and rotational velocities forrapidly rotating stars. We identify several distinct groups by theirHα properties and investigate variations in chromospheric activityamong early (M0-M2.5) and mid (M3-M6) dwarfs. Using a volume-limitedsample together with a relationship between age and chromosphericactivity, we show that the rate of star formation in the immediate solarneighborhood has been relatively constant over the last 4 Gyr. Inparticular, our results are inconsistent with recent large bursts ofstar formation. We use the correlation between Hα activity and ageas a function of color to set constraints on the properties of L and Tdwarf secondary components in binary systems. We also identify a numberof interesting stars, including rapid rotators, radial velocityvariables, and spectroscopic binaries. Observations were made at the 60inch telescope at Palomar Mountain, which is jointly owned by theCalifornia Institute of Technology and the Carnegie Institution ofWashington.
| Late-type members of young stellar kinematic groups - I. Single stars
This is the first paper of a series aimed at studying the properties oflate-type members of young stellar kinematic groups. We concentrate ourstudy on classical young moving groups such as the Local Association(Pleiades moving group, 20-150Myr), IC 2391 supercluster (35Myr), UrsaMajor group (Sirius supercluster, 300Myr), and Hyades supercluster(600Myr), as well as on recently identified groups such as the Castormoving group (200Myr). In this paper we compile a preliminary list ofsingle late-type possible members of some of these young stellarkinematic groups. Stars are selected from previously established membersof stellar kinematic groups based on photometric and kinematicproperties as well as from candidates based on other criteria such astheir level of chromospheric activity, rotation rate and lithiumabundance. Precise measurements of proper motions and parallaxes takenfrom the Hipparcos Catalogue, as well as from the Tycho-2 Catalogue, andpublished radial velocity measurements are used to calculate theGalactic space motions (U, V, W) and to apply Eggen's kinematic criteriain order to determine the membership of the selected stars to thedifferent groups. Additional criteria using age-dating methods forlate-type stars will be applied in forthcoming papers of this series. Afurther study of the list of stars compiled here could lead to a betterunderstanding of the chromospheric activity and their age evolution, aswell as of the star formation history in the solar neighbourhood. Inaddition, these stars are also potential search targets for directimaging detection of substellar companions.
| Catalogue of [Fe/H] determinations for FGK stars: 2001 edition
The catalogue presented here is a compilation of published atmosphericparameters (Teff, log g, [Fe/H]) obtained from highresolution, high signal-to-noise spectroscopic observations. This newedition has changed compared to the five previous versions. It is nowrestricted to intermediate and low mass stars (F, G and K stars). Itcontains 6354 determinations of (Teff, log g, [Fe/H]) for3356 stars, including 909 stars in 79 stellar systems. The literature iscomplete between January 1980 and December 2000 and includes 378references. The catalogue is made up of two tables, one for field starsand one for stars in galactic associations, open and globular clustersand external galaxies. The catalogue is distributed through the CDSdatabase. Access to the catalogue with cross-identification to othersets of data is also possible with VizieR (Ochsenbein et al.\cite{och00}). The catalogue (Tables 1 and 2) is only available inelectronic form 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/373/159 and VizieRhttp://vizier.u-strasbg.fr/.
| Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable 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/qcar?J/A+A/367/521
| The ROSAT Bright Survey: II. Catalogue of all high-galactic latitude RASS sources with PSPC countrate CR > 0.2 s-1
We present a summary of an identification program of the more than 2000X-ray sources detected during the ROSAT All-Sky Survey (Voges et al.1999) at high galactic latitude, |b| > 30degr , with countrate above0.2 s-1. This program, termed the ROSAT Bright Survey RBS, isto more than 99.5% complete. A sub-sample of 931 sources with countrateabove 0.2 s-1 in the hard spectral band between 0.5 and 2.0keV is to 100% identified. The total survey area comprises 20391deg2 at a flux limit of 2.4 x 10-12 ergcm-2 s-1 in the 0.5 - 2.0 keV band. About 1500sources of the complete sample could be identified by correlating theRBS with SIMBAD and the NED. The remaining ~ 500 sources were identifiedby low-resolution optical spectroscopy and CCD imaging utilizingtelescopes at La Silla, Calar Alto, Zelenchukskaya and Mauna Kea. Apartfrom completely untouched sources, catalogued clusters and galaxieswithout published redshift as well as catalogued galaxies with unusualhigh X-ray luminosity were included in the spectroscopic identificationprogram. Details of the observations with an on-line presentation of thefinding charts and the optical spectra will be published separately.Here we summarize our identifications in a table which contains opticaland X-ray information for each source. As a result we present the mostmassive complete sample of X-ray selected AGNs with a total of 669members and a well populated X-ray selected sample of 302 clusters ofgalaxies with redshifts up to 0.70. Three fields studied by us remainwithout optical counterpart (RBS0378, RBS1223, RBS1556). While the firstis a possible X-ray transient, the two latter are isolated neutron starcandidates (Motch et al. 1999, Schwope et al. 1999).
| The ROSAT all-sky survey catalogue of the nearby stars
We present X-ray data for all entries of the Third Catalogue of NearbyStars \cite[(Gliese & Jahreiss 1991)]{gli91} that have been detectedas X-ray sources in the ROSAT all-sky survey. The catalogue contains1252 entries yielding an average detection rate of 32.9 percent. Inaddition to count rates, source detection parameters, hardness ratios,and X-ray fluxes we also list X-ray luminosities derived from Hipparcosparallaxes. Catalogue also available at CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Metallicity and photospheric abundances in field K and M dwarfs
Elemental abundances in late-type stars are of interest in several ways:they determine the location of the stars in the HR diagram and thereforetheir ages, as well as the atmospheric structure in their middle andupper photospheres. Especially in the case of chromospherically activelate-type stars the question arises to what degree the upper photosphereis influenced by the nearby chromosphere. Analysing S/N~200 andDeltalambda/lambda~20000 data, we found a mean metallicity index[M/H]=-0.2 for programme K and M field stars based on an analysis ofspectra in the region 5500-9000 Angstroms. We also found that the CaI6162-Angstroms transition is a potential surface gravity indicator forK-type stars. For the chromospheric activity interval4.4
| Chromospheric modelling of the Hα and NA I D lines in five M dwarfs of low to high activity level
We have obtained simultaneous high resolution Hα and Na I Dspectra of five dwarf M stars that span a wide range in chromosphericactivity level. The observed Na I D lines exhibit behavior that isqualitatively similar to that of more well established diagnostics suchas the Ca II HK lines: as the activity level, as indicated by theHα line, increases, the absorption core brightens and thendevelops an emission reversal. We compare the observed profiles withcomputed non-LTE profiles from a grid of chromospheric/transition regionmodels. We find that the Hα and Na I D lines tend to be in generalagreement as indicators of approximate chromospheric activity level.However, the Hα line systematically indicates a value for the massloading at the onset of the Transition Region and the location of T_minthat is 0.4 dex lower in column mass density than that indicated by Na ID. Therefore, the profile of both lines cannot be simultaneously wellfit for all but one of our stars. We also find, in agreement with thepioneering study of Andretta et al. (\cite{adb}), that for dMe stars theshape of the Na I D emission cores is a much more sensitive indicator ofchromospheric thickness (or, equivalently, chromospheric steepness) thanis Hα , and, therefore, provides a powerful diagnostic complementto Hα . Finally, we investigate the dependence of the predictedline profiles on the values of the stellar parameters and conclude thatthe inferred chromospheric pressure is sensitive to the choice of T_effand log g, especially among dMe stars. Specifically, among dMe stars, amodel in which the value of T_eff is too small or too large byapproximately 200 K, or in which the value of log g is too large or toosmall by 0.5 dex, will give rise to closest fit values of the columnmass density at the location of the Transition Region and T_min that aretoo small or too large, respectively, by approximately 0.3 dex. As aresult, discrepancies between the stellar parameters of our photosphericmodel and those of the program objects allow us to extract only upper orlower limits for the values of the column mass density at criticalpoints in the chromospheric structure
| The evolutionary status of activity-selected solar-type stars and of T Tauri stars as derived from HIPPARCOS parallaxes: evidence for long-lived T Tauri disks?
We have used the Hipparcos parallaxes to study the evolutionary statusof a sample of stars with spectral types from late F to M0 (hereafter``solar-type stars''), selected on the basis of their activity, mainlyfrom Einstein-based surveys. The parallaxes have been used to place theobjects in the H-R diagram, determining their age by comparison withtheoretical evolutionary tracks and observational main sequences. Thisage is compared with age estimates derived from the lithium abundance,the activity level and the presence of circumstellar disks. Tocomplement our sample at the young end we have also studied theHipparcos-determined distances of a sample of optically-selectedpre-main sequence stars, mostly classical T Tauri stars (CTTS). SomeCTTS appear to be much nearer to us than previously determined, and faraway from their putative parent cloud. This implies a significantlylarger age providing observational evidence for the existence oflong-lived T Tauri disks which could produce slow rotators on theZero-Age Main Sequence (ZAMS). None of the above-mentioned age proxiesappears to reliably and unambiguously select very young stars in therange of spectral types considered here, with some apparently very youngobjects effectively lying onto or very close to the main sequence. Theattribution of ages to young solar-type stars on the basis of any of thestandard proxies may thus significantly under- or over-estimate theevolutionary age of the object. Caution must therefore be exercised whenattributing ages to individual stars, and claims about the large numberof PMS stars found in X-ray based surveys may need to be at least inpart reconsidered in this light. Based on data from the ESA Hipparcossatellite.
| Young Cool Stars in the Solar Neighborhood.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....114.1673S&db_key=AST
| HIPPARCOS distances of X-ray selected stars: implications on their nature as stellar population.
We present the parallaxes, measured by Hipparcos, for a sample of X-rayselected stars. The stars belong to the stellar sample of the EinsteinExtended Medium Sensitivity Survey. They are all at galactic latitude|b|>20deg, and are generally far away from known star formingregions. Several of these stars show lithium abundance and activitylevel typical of very young stars with ages comparable to that of thePleiades. We show that the majority of our sample stars are on the mainsequence, with only =~20% being giants. We do not find a significantpresence of pre-main sequence stars in our sample, notwithstanding thefact that some of our stars have a considerable lithium abundance,showing that the stars observed are most likely young and activemain-sequence objects.
| The intrinsic LY α to H α ratio in M dwarf stars.
Using Ly α line profiles generated from a grid of M dwarf modelatmospheres we calculate the attenuation factor [i.e.Lyα(obs)/Lyα(intrin)] due to the interstellar medium as afunction of hydrogen column density. Then using selected modelatmospheres, attenuation factors were calculated for those M dwarfs withavailable Ly α observations. The prime motivation in this work hasbeen to look afresh at the intrinsic Ly α to H α flux ratio,an important constraint in the radiative transfer modelling of M dwarfs.For those active dMe stars where both lines were observed, the intrinsicratio is ~3-5 (with ~50% variation). The major uncertainty in this workhas been the interstellar hydrogen column density, emphasizing the needfor further work in this area and in particular an accurate model of itsvariation in all directions.
| Lithium abundance in field K and M dwarfs
It is widely accepted that lithium abundance in late-type starscorrelates with other stellar characteristics, such as age,chromospheric activity and rotation. For example, the post-main-sequenceactive components of RSCVn binaries have been compared with inactivefield stars of the same spectral type and found to have excess lithium.In stars with deep convective zones lithium is expected to be destroyedin a relatively short time. This is most dramatically true in themain-sequence stars of the latest type. In this paper we have examinedthe lithium abundances in a sample of late-K and M-type dwarfs. Highsignal-to-noise ratio, high spectral resolution spectra have beenobtained of the Li i resonance doublet (lambda6707.8A). Evidence for anappreciable lithium abundance has been found in stars as late as earlyto mid-M. Furthermore, there is evidence for a correlation between thisLi abundance and chromospheric activity in the case of K dwarfs while Mdwarfs do not appear to follow such a relation.
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Observation and Astrometry data
| Constellation: | Pisces |
| Right ascension: | 23h35m00.28s |
| Declination: | +01°36'19.5" |
| Apparent magnitude: | 9.555 |
| Distance: | 19.305 parsecs |
| Proper motion RA: | 342.6 |
| Proper motion Dec: | 33.7 |
| B-T magnitude: | 11.326 |
| V-T magnitude: | 9.702 |
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