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Cool Star Oxygen Abundances from Spectral Synthesis of TiO Bands
We have used spectral synthesis of the γ 0-0 TiO band at 7054Å to determine oxygen abundances in dwarfs previously analyzed foriron and titanium abundances from their atomic lines. With theabundances of Fe and Ti held fixed, the band profiles are sensitive tothe oxygen abundances. For the late K and M dwarfs analyzed, the [O/Fe]trend agrees with previous work for higher mass stars from to . Beyond, the TiO band becomes too weak to analyze except in cooler stars forwhich Ti abundances are difficult to determine because their Ti I linesare frequently blended. We find that the abundance trend derived for ourstars matches those derived for solar neighborhood stars by othermethods.
| Lucky Imaging of M subdwarfs
Context: The knowledge of the binary properties of metal-poor andsolar-metallicity stars can shed light on the potential differencesbetween the formation processes responsible for both types of objects.Aims: The aim of the project is to determine the binary properties(separation, mass ratio, frequency of companions) for M subdwarfs, thelow-metallicity counterparts of field M dwarfs, and investigate anypotential differences between both populations. Methods: We haveobtained high-resolution imaging in the optical for a sample of 24early-M subdwarfs and nine extreme subdwarfs with the “LuckyImaging” technique using the AstraLux instrument on the Calar Alto2.2-m telescope. Results: We are sensitive to companions atseparations larger than 0.1 arcsec and differences of ~2 mag at 0.1arcsec and ~5 mag at 1 arcsec. We have found no companion around the 24subdwarfs under study and one close binary out of nine extremesubdwarfs. A second image of LHS 182 taken three months later with thesame instrument confirms the common proper motion of the binaryseparated by about 0.7 arcsec. Moreover, we do not confirm the commonproper motion of the faint source reported by Riaz and collaborators at~2 arcsec from LHS 1074. Conclusions: We derive a binaryfrequency of 3±3% for M subdwarfs from our sample of 33 objectsfor separations larger than about five astronomical units. Adding to oursample the additional 28 metal-poor early-M dwarfs observed with theHubble Space Telescope by Riaz and collaborators, we infer a binaryfraction of 3.7±2.6% (with a 1σ confidence limit),significantly lower than the fraction of resolved binary M dwarfs (~20%)over the same mass and separation ranges. This result suggests a sharpcut-off in the multiplicity fraction from G to M subdwarfs, indicatingthat the metallicity plays a role at lower masses and/or anenvironmental effect governing the formation of metal-poor M dwarfscompared to their metallicity counterparts.Based on observations collected at theCentro Astronómico Hispano Alemán (CAHA) at Calar Alto,operated jointly by theMax-Planck Institut für Astronomie and the Instituto deAstrofísica de Andalucía (CSIC).
| Cool Subdwarf Investigations. II. Multiplicity
Cool subdwarfs of types K and M are the fainter counterparts of coolmain-sequence dwarfs that dominate the Galactic population. In thispaper, we present the results of an optical speckle survey of 62confirmed cool subdwarf systems within 60 pc. We have resolved twonew companions and confirmed two previously known companions withseparations 0farcs13-3farcs29. After including previously known widecompanions and all known spectroscopic binaries, we determine themultiplicity rate of cool subdwarfs to be 26% ± 6%, which issomewhat lower than comparable main-sequence stars that have amultiplicity rate of 37% ± 5%. We find that only 3% of the coolsubdwarfs surveyed have companions within 10 AU, 3% have companionsbetween 10 and 100 AU, and 14% have companions beyond 100 AU.The other 6% of cool subdwarfs are spectroscopic binaries. This is verydifferent from K/M dwarfs that have most companions (13%) at separationscloser than 10 AU. However, because a search for close binariesamong a large sample of nearby cool subdwarfs remains elusive, it is notyet settled whether or not the multiplicity rates are significantlydifferent. Nonetheless, several different observational results andtheories pointing to a possible dearth of subdwarf multiples arediscussed.
| Cool Subdwarf Investigations. I. New Thoughts on the Spectral Types of K and M Subdwarfs
Using new spectra of 88 K- and M-type subdwarfs, we consider novelmethods for assigning their spectral types and take steps towarddeveloping a comprehensive spectral sequence for subdwarf types K3.0 toM6.0. The types are assigned based on the overall morphology of spectracovering 6000-9000 Å. The types and sequence presented link thespectral types of cool subdwarfs to their main-sequence counterparts,with emphasis on the relatively opacity-free region from 8200-9000Å. When available, supporting abundance, kinematic, andtrigonometric parallax information is used to provide more completeportraits of the observed subdwarfs. We find that the CaHn (n = 1-3) andTiO5 indices often used for subdwarf spectral typing are affected incomplicated ways by combinations of the subdwarfs' temperatures,metallicities, and gravities, and we use model grids to evaluate thetrends in all three parameters. Because of the complex interplay ofthese three characteristics, it is not possible to identify a star as an"extreme" subdwarf simply based on very low metallicity, and we suggestthat the modifiers "extreme" or "ultra" only outline locations onspectroscopic indices plots, and should not be used to imply low or verylow metallicity stars. In addition, we propose that "VI" be used toidentify a star as a subdwarf, rather than the confusing "sd" prefix,which is also used for hot O and B subdwarfs that are unrelated to thecool subdwarfs discussed in this paper.
| Revised Metallicity Classes for Low-Mass Stars: Dwarfs (dM), Subdwarfs (sdM), Extreme Subdwarfs (esdM), and Ultrasubdwarfs (usdM)
The current classification system of M stars on the main sequencedistinguishes three metallicity classes (dwarfs: dM; subdwarfs: sdM; andextreme subdwarfs: esdM). The spectroscopic definition of these classesis based on the relative strength of prominent CaH and TiO molecularabsorption bands near 7000 Å, as quantified by three spectroscopicindices (CaH2, CaH3, and TiO5). The boundaries between the metallicityclasses were initially defined from a relatively small sample of only 79metal-poor stars (subdwarfs and extreme subdwarfs). We re-examine thisclassification system in light of our ongoing spectroscopic survey ofstars with proper motion μ>0.45'' yr-1,which has increased the census of spectroscopically identifiedmetal-poor M stars to over 400 objects. Kinematic separation of diskdwarfs and halo subdwarfs suggest deficiencies in the currentclassification system. Observations of common proper motion doublesindicates that the current dM/sdM and sdM/esdM boundaries in the [TiO5,CaH2+CaH3] index plane do not follow isometallicity contours, leavingsome binaries inappropriately classified as dM+sdM or sdM+esdM. Wepropose a revision of the classification system based on an empiricalcalibration of the TiO/CaH ratio for stars of near solar metallicity. Weintroduce the parameter ζTiO/CaH, which quantifies theweakening of the TiO band strength due to metallicity effect, withvalues ranging from ζTiO/CaH=1 for stars of near-solarmetallicity to ζTiO/CaH~=0 for the most metal-poor (andTiO depleted) subdwarfs. We redefine the metallicity classes based onthe value of the parameter ζTiO/CaH and refine thescheme by introducing an additional class of ultrasubdwarfs (usdM). Weintroduce sequences of sdM, esdM, and usdM stars to be used as formalclassification standards.Based on observations conducted at the MDM observatory, operated jointlyby the University of Michigan, Dartmouth College, Ohio State University,Columbia University, and the University of Ohio.Based on observations conducted at the Lick Observatory, operated by theUniversity of California system.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Calibrating M Dwarf Metallicities Using Molecular Indices
We report progress in the calibration of a method to determine cooldwarf star metallicities using molecular band strength indices. Themolecular band index to metallicity relation can be calibrated usingchemical abundances calculated from atomic-line equivalent widthmeasurements in high-resolution spectra. Building on previous work, wehave measured Fe and Ti abundances in 32 additional M and K dwarf starsto extend the range of temperature and metallicity covered. A test ofour analysis method using warm star-cool star binaries shows we cancalculate reliable abundances for stars warmer than 3500 K. We have usedabundance measurements for warmer binary or cluster companions toestimate abundances in six additional cool dwarfs. Adding stars measuredin our previous work and others from the literature provides 76 starswith Fe abundance and CaH2 and TiO5 index measurements. The CaH2molecular index is directly correlated with temperature. TiO5 depends ontemperature and metallicity. Metallicity can be estimated to within+/-0.3 dex within the bounds of our calibration, which extends fromroughly [Fe/H]=+0.05 to -1.0, with a limited extension to -1.5.
| Metallicity of M dwarfs. I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence
We obtained high resolution ELODIE and CORALIE spectra for bothcomponents of 20 wide visual binaries composed of an F-, G- or K-dwarfprimary and an M-dwarf secondary. We analyse the well-understood spectraof the primaries to determine metallicities ([Fe/H]) for these 20systems, and hence for their M dwarf components. We pool thesemetallicities with determinations from the literature to obtain aprecise (±0.2 dex) photometric calibration of M dwarfmetallicities. This calibration represents a breakthrough in a fieldwhere discussions have had to remain largely qualitative, and it helpsus demonstrate that metallicity explains most of the large dispersion inthe empirical V-band mass-luminosity relation. We examine themetallicity of the two known M-dwarf planet-host stars, Gl876 (+0.02 dex) and Gl 436 (-0.03 dex), inthe context of preferential planet formation around metal-rich stars. Wefinally determine the metallicity of the 47 brightest single M dwarfs ina volume-limited sample, and compare the metallicity distributions ofsolar-type and M-dwarf stars in the solar neighbourhood.
| Probing the LHS Catalog. II. Faint Proper-Motion Stars
We present low-resolution spectroscopic observations of faintproper-motion stars from the LHS Catalogue, concentrating on stars withmr>16.5 and μ>0.5" yr-1. The presentpaper includes observations and spectral classifications for 294 Mdwarfs, M subdwarfs (sdM), and extreme M subdwarfs (esdM). We alsoidentify white dwarfs among the faintest LHS stars. We havecross-referenced this sample against the Two Micron All Sky Survey(2MASS) sources, and list data for the detected objects. We discussstars of individual interest, as well as the characteristics of theoverall sample. As expected, a significant number of the stars in thisproper-motion-selected sample are halo subdwarfs, including an esdMdwarf, LHS 3481, that is likely to lie within 20 pc of the Sun. None ofthe subdwarfs show Hα emission.
| 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.
| Metallicity measurements using atomic lines in M and K dwarf stars
We report the first survey of chemical abundances in M and K dwarf starsusing atomic absorption lines in high-resolution spectra. We havemeasured Fe and Ti abundances in 35 M and K dwarf stars using equivalentwidths measured from λ/Δλ~ 33000 spectra. Ouranalysis takes advantage of recent improvements in model atmospheres oflow-temperature dwarf stars. The stars have temperatures between 3300and 4700 K, with most cooler than 4100 K. They cover an iron abundancerange of -2.44 < [Fe/H] < +0.16. Our measurements show [Ti/Fe]decreasing with increasing [Fe/H], a trend similar to that measured forwarmer stars, where abundance analysis techniques have been tested morethoroughly. This study is a step towards the observational calibrationof procedures to estimate the metallicity of low-mass dwarf stars usingphotometric and low-resolution spectral indices.
| 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.
| Revised Coordinates and Proper Motions of the Stars in the Luyten Half-Second Catalog
We present refined coordinates and proper-motion data for the highproper-motion (HPM) stars in the Luyten Half-Second (LHS) catalog. Thepositional uncertainty in the original Luyten catalog is typicallygreater than 10" and is often greater than 30". We have used the digitalscans of the POSS I and POSS II plates to derive more accurate positionsand proper motions of the objects. Out of the 4470 candidates in the LHScatalog, 4323 objects were manually reidentified in the POSS I and POSSII scans. A small fraction of the stars were not found because of thelack of finder charts and digitized POSS II scans. The uncertainties inthe revised positions are typically ~2" but can be as high as ~8" in afew cases, which is a large improvement over the original data.Cross-correlation with the Tycho-2 and Hipparcos catalogs yielded 819candidates (with mR<~12). For these brighter sources, theposition and proper-motion data were replaced with the more accurateTycho-2/Hipparcos data. In total, we have revised proper-motionmeasurements and coordinates for 4040 stars and revised coordinates for4330 stars. The electronic version of the paper5 contains the updated information on all 4470stars in the LHS catalog.
| M-Subdwarfs: Spectroscopic Classification and the Metallicity Scale
We present a spectroscopic classification system for M-dwarfs andM-subdwarfs based on quantitative measures of TiO and CaH features inthe region lambda lambda 6200 - 7400 Angstroms. Our sample of cool starscovers the range from solar metallicity stars to the most extremesubdwarfs known. Using synthetic spectra computed by Allard andHauschildt (1995), we derive metallicities for the stars. Stars areclassified as dwarfs (M V), subdwarfs (sdM), or extreme subdwarfs(esdM). These classifications correspond to [m/H] ~ 0.0, -1.2, and -2.0respectively. Our metallicity scale agrees with theoretical HR diagramsand HST globular cluster measurements. We discuss some nearby subdwarfsof particular interest in light of our metallicity scale.
| Classification of Population II Stars in the Vilnius Photometric System. I. Methods
The methods used for classification of Population II stars in theVilnius photometric system are described. An extensive set of standardswith known astrophysical parameters compiled from the literature sourcesis given. These standard stars are classified in the Vilnius photometricsystem using the methods described. The accuracy of classification isevaluated by a comparison of the astrophysical parameters derived fromthe Vilnius photometric system with those estimated from spectroscopicstudies as well as from photometric data in other systems. For dwarfsand subdwarfs, we find a satisfactory agreement between our reddeningsand those estimated in the uvbyscriptstyle beta system. The standarddeviation of [Fe/H] deter mined in the Vilnius system is about 0.2 dex.The absolute magnitude for dwarfs and subdwarfs is estimated with anaccuracy of scriptstyle <=0.5 mag.
| Infrared colors of low-mass stars
A total of 322 red dwarf stars are studied in a review of IR IJHKphotometry to discern chromospheric activity and kinematic dataregarding metallicity effects in the IR color:color diagrams. Themetallicity variations are employed to assess changes in the H(-)continuum opacity and water-vapor characterizations. The stars areclassified in terms of metal-richness with five categories includingyoung disk, old disk, and halo types with attention given to the inverserelationship between metallicity and water-band absorption strength. Theresults include IR photometric parallax relations for each metallicitygroup and absolute magnitudes for single stars as well as temperatures,intrinsic colors, and spectral types. The body of data is useful forconstraining models of the interiors and atmospheres of this class ofstars.
| Parallaxes and proper motions. XIX - The subdwarf sequence
Parallaxes and proper motions are presented for 19 stars in 15 starfields. Four of the stars were discovered in the course of the measuresto have significantly large proper motions and the data for them areincluded in the tables. The other 15 are all stars considered to besubluminous. Photometric and metallicity data for most of them arepresented. They appear not to conform to a straight linear relationbetween (FE/H) determined from the measured ultraviolet excess and theabsolute magnitude corrected to a B-V color of 0.6.
| Subdwarf studies. II - Abundances and kinematics from medium resolution spectra. III - The halo metallicity distribution
Stars previously identified as having UV excesses are observed at 1-Aresolution in the Ca II K-line region. Comparisons of these data withother samples and with Monte Carlo simulations involving a singlecomponent halo have yielded estimates of halo velocity dispersions androtation velocity, corrected for the kinematic biases in the sample. Itis suggested that the data are not consistent with a model in which thehalo formed from star formation in a dissipating, collapsing cloud; theyare, however, reconcilable with the formation of the halo stars bynumerous, independently evolving gas clouds. The metallicitydistribution of a sample of 372 kinematically selected halo stars isthen constructed, with a view to selection effects in the data. Goodagreement is noted between the globular cluster metallicity distributionand a stochastic model with a mean of 10 enrichments/fragment.
| Subdwarf studies. I - UBVRI photometry of NLTT stars
UBVRI photometry is presented for a sample of 1656 southern stars,including 1211 that were previously unmeasured, drown from the NLTTproper-motion catalog. The catalog is shown to be a rich source ofsubdwarfs. The normalized ultraviolet excess delta (U - B)0.6,photometric parallax, and interstellar reddening are calculated for eachstar when possible. Photometric parallaxes are compared withtrigonometric parallaxes from the literature. It is found that theformer do not have systematic errors greater than about 25 percent. Inagreement with other studies, the bluest subdwarfs are found at B - V =0.35. The selection of the program stars on the basis of large reducedproper motions restricted subgiant contamination of the sample to about5 percent and increased the discovery fraction of halo stars relative todisk stars. The claim is made here that the sample can be used toinvestigate the abundance distribution of the halo. The sample includesstars with ultraviolet excesses characteristic of disk abundances butwith velocities up to 150 km/s. These are believed to be stars that,quite expectedly, reside in the high-velocity tail of the disk velocitydistribution.
| High-proper-motion stars. II - Radial velocities of late-type dwarfs
Radial velocities are presented for 41 late-type stars of high propermotion. Nearly all of these are new. Three stars appear to have spacevelocities exceeding 400 km/s relative to the center of the Galaxy onthe basis of the currently available astrometric data. These cases areexamined in some detail.
| Bolometric luminosities and colors for K and M dwarfs and the subluminous stars of the halo
The H-R diagrams of dM, sdK, and sdM proper-motion stars are examined. Amethod for integrating energy distributions using discrete weights isproposed. The bolometric corrections are assessed at various wavelengthsand a method for obtaining luminosities even if a star lacks IR data ispresented. The color-luminosity diagrams suggest that high-velocity,low-metallicity stars of the halo are subluminous. It is found that theapparent cutoff in the halo is a bolometric magnitude of about 12 m.
| Photographic astrometry of binary and proper-motion stars. IV
Parallax data are given for 62 binary and proper motion stars based onobservations obtained between May 1987 and March 1988. The datapresented in tabular form include reference positions, identifiers (BDand GC numbers, if any), visual magnitudes, and spectral types. Massratio results for eight binary stars are also presented. Notes areprovided which indicate the inclusion or replacement of previousmeasurements and which reductions have been applied.
| Dwarf K and M stars of high proper motion found in a hemispheric survey
A recently completed visual/red spectral region objective-prism surveyof more than half the sky found some 2200 dwarf K and M stars ofnegligible proper motion (Stephenson, 1986). The present paper adds the1800-odd spectroscopically identified dwarfs that did prove to havesignificant proper motions. About half of these had previous spectralclassifications of some sort, especially by Vyssotsky (1952, 1956). Forthe great majority, the present coordinates are more accurate thanprevious data. The paper includes about 50 stars with unpublishedparallaxes, likely to have parallaxes of 0.05 arcsec or more. Combiningthe present data with the first paper suggests that the number oflow-proper-motion stars in that paper was not unreasonable.
| G. P. Kuiper's spectral classifications of proper-motion stars
Spectral classifications are listed for over 3200 stars, mainly of largeproper motion, observed and classified by Kuiper during the years1937-1944 at the Yerkes and McDonald Observatories. While Kuiper himselfpublished many of his types, and while improved classifications are nowavailable for many of these stars, much of value remains. For many ofthe objects, no other spectral data exist.
| The identification of subdwarfs from their parallaxes
Not Available
| Parallaxes and proper motions. XVII
Parallaxes and proper motions are presented for 23 stars in 19 starfields. Seven of the target stars and one other star have no previousparallax determinations. New photometry is also presented for two of thestars for which previous data had not been published. Two of the targetstars are resolved binaries for which both components were measuredseparately; one of the two is not a physical pair. This list is thefirst in the series which makes use of the PDS microdensitometer of theYale Observatory with five of the 19 star fields being measured there.The PDS measures are too few for a reliable direct comparison with thehand measures, but they appear to be more accurate. This is also thefirst list to report parallaxes of subdwarf candidates. Subluminousstars now form a second commitment of the program along with the K and Mdwarfs which have formerly dominated the program.
| High-tangential-velocity stars
Two lists of high tangential velocity (greater than 100 km/s) starscontained in the Lowell Northern Hemisphere proper motion surveycatalogue have been compiled, the stellar distances being inferred fromeither trigonometric or spectroscopic parallaxes. The information givenincludes equatorial coordinates, corrected photographic magnitudes,proper motions, trigonometric or spectroscopic parallaxes, and spectraltypes.
| Predicted infrared brightness of stars within 25 parsecs of the sun
Procedures are given for transforming selected optical data intoinfrared flux densities or irradiances. The results provide R, T(eff)blackbody approximations for about 2000 of the stars in Woolley et al.'sCatalog of Stars (1970) within 25 pc of the sun, and additional whitedwarfs, with infrared flux densities predicted for them at ninewavelengths from 2.2 to 101 microns including the Infrared AstronomySatellite bands.
| U.S. Naval Observatory parallaxes of faint stars. VI
Trigonometric parallaxes determined at the U.S. Naval Observatory fromplate material obtained with the 1.55-m astrometric reflector arelisted. Included are parallax determinations for 89 single stars and forboth components of four common-proper-motion binary systems. Of these,94 are considered 'definitive' in the sense that they are based onsufficient plate material (generally, 40-50 plates per series) coveringa sufficient time interval (average of 4.6 yr per series); thus furtherprecision can be expected to accrue only as (approximately) the squareroot of the total number of plates employed in the solution.
| Catalogs of proper-motion stars. I - Stars brighter than visual magnitude 15 and with annual proper motion of 1 arcsec or more
Abstract image available at:http://adsabs.harvard.edu/abs/1979ApJS...39...89E
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Dades d'Observació i Astrometria
| Constel·lació: | Pisces |
| Ascensió Recta: | 02h02m52.14s |
| Declinació: | +05°42'20.5" |
| Magnitud Aparent: | 12.283 |
| Distancia: | 27.647 parsecs |
| Moviment propi RA: | 2325.1 |
| Moviment propi Dec: | -713.8 |
| B-T magnitude: | 13.565 |
| V-T magnitude: | 12.389 |
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