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The Extinction Toward the Galactic Bulge from RR Lyrae Stars
We present mean reddenings toward 3525 RR0 Lyrae stars from the Galacticbulge fields of the MACHO Survey. These reddenings are determined usingthe color at minimum V-band light of the RR0 Lyrae stars themselves andare found to be in general agreement with extinction estimates at thesame location obtained from other methods. Using 3256 stars located inthe Galactic Bulge, we derive the selective extinction coefficientRV,VR = AV/E(V - R) = 4.3 ± 0.2. This valueis what is expected for a standard extinction law with RV,BV= 3.1 ± 0.3.
| Stellar evolution through the ages: period variations in galactic RRab stars as derived from the GEOS database and TAROT telescopes
Context: The theory of stellar evolution can be more closely tested ifwe have the opportunity to measure new quantities. Nowadays,observations of galactic RR Lyr stars are available on a time baselineexceeding 100 years. Therefore, we can exploit the possibility ofinvestigating period changes, continuing the pioneering work started byV. P. Tsesevich in 1969. Aims: We collected the available times ofmaximum brightness of the galactic RR Lyr stars in the GEOS RR Lyrdatabase. Moreover, we also started new observational projects,including surveys with automated telescopes, to characterise the O-Cdiagrams better. Methods: The database we built has proved to be a verypowerful tool for tracing the period variations through the ages. Weanalyzed 123 stars showing a clear O-C pattern (constant, parabolic orerratic) by means of different least-squares methods. Results: Clearevidence of period increases or decreases at constant rates has beenfound, suggesting evolutionary effects. The median values are β =+0.14 d Myr-1 for the 27 stars showing a period increase andβ = -0.20 d Myr-1 for the 21 stars showing a perioddecrease. The large number of RR Lyr stars showing a period decrease(i.e., blueward evolution) is a new and intriguing result. There is anexcess of RR Lyr stars showing large, positive β values. Moreover,the observed β values are slightly larger than those predicted bytheoretical models.Tables 3, 4, 5 and Figs. 2, 3 are only available in electronic form athttp://www.aanda.org
| The GEOS RR Lyr Survey
Not Available
| Analysis of RR Lyrae Stars in the Northern Sky Variability Survey
We use data from the Northern Sky Variability Survey (NSVS), obtainedfrom the first-generation Robotic Optical Transient Search Experiment(ROTSE-I), to identify and study RR Lyrae variable stars in the solarneighborhood. We initially identified 1197 RRab (RR0) candidate starsbrighter than the ROTSE median magnitude V=14. Periods, amplitudes, andmean V magnitudes are determined for a subset of 1188 RRab stars withwell-defined light curves. Metallicities are determined for 589 stars bythe Fourier parameter method and by the relationship between period,amplitude, and [Fe/H]. We comment on the difficulties of clearlyclassifying RRc (RR1) variables in the NSVS data set. Distances to theRRab stars are calculated using an adopted luminosity-metallicityrelation with corrections for interstellar extinction. The 589 RRabstars in our final sample are used to study the properties of the RRabpopulation within 5 kpc of the Sun. The Bailey diagram of period versusamplitude shows that the largest component of this sample belongs toOosterhoff type I. Metal-rich ([Fe/H]>-1) RRab stars appear to beassociated with the Galactic disk. Our metal-rich RRab sample mayinclude a thin-disk, as well as a thick-disk population, although theuncertainties are too large to establish this. There is some evidenceamong the metal-rich RRab stars for a decline in scale height withincreasing [Fe/H], as was found by Layden. The distribution of RRabstars with -1<[Fe/H]<-1.25 indicates that within this metallicityrange the RRab stars are a mixture of stars belonging to halo and diskpopulations.
| A catalogue of RR Lyrae stars from the Northern Sky Variability Survey
A search for RR Lyrae stars has been conducted in the publicly availabledata of the Northern Sky Variability Survey. Candidates have beenselected by the statistical properties of their variation; the standarddeviation, skewness and kurtosis with appropriate limits determined froma sample 314 known RRab and RRc stars listed in the General Catalogue ofVariable Stars. From the period analysis and light-curve shape of over3000 candidates 785 RR Lyrae have been identified of which 188 arepreviously unknown. The light curves were examined for the Blazhkoeffect and several new stars showing this were found. Six double-mode RRLyrae stars were also found of which two are new discoveries. Somepreviously known variables have been reclassified as RR Lyrae stars andsimilarly some RR Lyrae stars have been found to be other types ofvariable, or not variable at all.
| Proper identification of RR Lyrae stars brighter than 12.5 mag
RR Lyrae stars are of great importance for investigations of Galacticstructure. However, a complete compendium of all RR-Lyraes in the solarneighbourhood with accurate classifications and coordinates does notexist to this day. Here we present a catalogue of 561 local RR-Lyraestars (V_max ≤ 12.5 mag) according to the magnitudes given in theCombined General Catalogue of Variable Stars (GCVS) and 16 fainter ones.The Tycho2 catalogue contains ≃100 RR Lyr stars. However, manyobjects have inaccurate coordinates in the GCVS, the primary source ofvariable star information, so that a reliable cross-identification isdifficult. We identified RR Lyrae from both catalogues based on anintensive literature search. In dubious cases we carried out photometryof fields to identify the variable. Mennessier & Colome (2002,A&A, 390, 173) have published a paper with Tyc2-GCVSidentifications, but we found that many of their identifications arewrong.
| RR Lyrae stars: kinematics, orbits and z-distribution
RR Lyrae stars in the Milky Way are good tracers to study the kinematicbehaviour and spatial distribution of older stellar populations. Arecently established well documented sample of 217 RR Lyr stars withV<12.5 mag, for which accurate distances and radial velocities aswell as proper motions from the Hipparcos and Tycho-2 catalogues areavailable, has been used to reinvestigate these structural parameters.The kinematic parameters allowed to calculate the orbits of the stars.Nearly 1/3 of the stars of our sample have orbits staying near the MilkyWay plane. Of the 217 stars, 163 have halo-like orbits fulfilling one ofthe following criteria: Θ < 100 km s-1, orbiteccentricity >0.4, and normalized maximum orbital z-distance>0.45. Of these stars roughly half have retrograde orbits. Thez-distance probability distribution of this sample shows scale heightsof 1.3±0.1 kpc for the disk component and 4.6±0.3 kpc forthe halo component. With our orbit statistics method we found a(vertical) spatial distribution which, out to z=20 kpc, is similar tothat found with other methods. This distribution is also compatible withthe ones found for blue (HBA and sdB) halo stars. The circular velocityΘ, the orbit eccentricity, orbit z-extent and [Fe/H] are employedto look for possible correlations. If any, it is that the metal poorstars with [Fe/H] <1.0 have a wide symmetric distribution aboutΘ=0, thus for this subsample on average a motion independent ofdisk rotation. We conclude that the Milky Way possesses a halo componentof old and metal poor stars with a scale height of 4-5 kpc having randomorbits. The presence in our sample of a few metal poor stars (thus partof the halo population) with thin disk-like orbits is statistically notsurprising. The midplane density ratio of halo to disk stars is found tobe 0.16, a value very dependent on proper sample statistics.
| The GEOS RR Lyr Survey
Not Available
| Subsystems of RR Lyrae Variable Stars in Our Galaxy
We have used published, high-accuracy, ground-based and satelliteproper-motion measurements, a compilation of radial velocities, andphotometric distances to compute the spatial velocities and Galacticorbital elements for 174 RR Lyrae (ab) variable stars in the solarneighborhood. The computed orbital elements and published heavy-elementabundances are used to study relationships between the chemical,spatial, and kinematic characteristics of nearby RR Lyrae variables. Weobserve abrupt changes of the spatial and kinematic characteristics atthe metallicity [Fe/H]≈-0.95 and also when the residual spatialvelocities relative to the LSR cross the critical value V res≈290km/s. This provides evidence that the general population of RR Lyraestars is not uniform and includes at least three subsystems occupyingdifferent volumes in the Galaxy. Based on the agreement between typicalparameters for corresponding subsystems of RR Lyrae stars and globularclusters, we conclude that metal-rich stars and globular clusters belongto a rapidly rotating and fairly flat, thick-disk subsystem with a largenegative vertical metallicity gradient. Objects with larger metaldeficiencies can, in turn, be subdivided into two populations, but usingdifferent criteria for stars and clusters. We suggest that field starswith velocities below the critical value and clusters with extremelyblue horizontal branches form a spherical, slowly rotating subsystem ofthe protodisk halo, which has a common origin with the thick disk; thissubsystem has small but nonzero radial and vertical metallicitygradients. The dimensions of this subsystem, estimated from theapogalactic radii of orbits of field stars, are approximately the same.Field stars displaying more rapid motion and clusters with redderhorizontal branches constitute the spheroidal subsystem of the accretedouter halo, which is approximately a factor of three larger in size thanthe first two subsystems. It has no metallicity gradients; most of itsstars have eccentric orbits, many display retrograde motion in theGalaxy, and their ages are comparatively low, supporting the hypothesisthat the objects in this subsystem had an extragalactic origin.
| Photoelectric Minima of Selected Eclipsing Binaries and Maxima of Pulsating Stars
Not Available
| Stars with the Largest Hipparcos Photometric Amplitudes
A list of the 2027 stars that have the largest photometric amplitudes inHipparcos Photometry shows that most variable stars are all Miras. Thepercentage of variable types change as a function of amplitude. Thiscompilation should also be of value to photometrists looking forrelatively unstudied, but large amplitude stars.
| Kinematics of Metal-poor Stars in the Galaxy. II. Proper Motions for a Large Nonkinematically Selected Sample
We present a revised catalog of 2106 Galactic stars, selected withoutkinematic bias and with available radial velocities, distance estimates,and metal abundances in the range -4.0<=[Fe/H]<=0.0. This updateof the 1995 Beers & Sommer-Larsen catalog includes newly derivedhomogeneous photometric distance estimates, revised radial velocitiesfor a number of stars with recently obtained high-resolution spectra,and refined metallicities for stars originally identified in the HKobjective-prism survey (which account for nearly half of the catalog)based on a recent recalibration. A subset of 1258 stars in this cataloghave available proper motions based on measurements obtained with theHipparcos astrometry satellite or taken from the updated AstrographicCatalogue (second epoch positions from either the Hubble Space TelescopeGuide Star Catalog or the Tycho Catalogue), the Yale/San Juan SouthernProper Motion Catalog 2.0, and the Lick Northern Proper Motion Catalog.Our present catalog includes 388 RR Lyrae variables (182 of which arenewly added), 38 variables of other types, and 1680 nonvariables, withdistances in the range 0.1 to 40 kpc.
| Systematics of RR Lyrae Statistical Parallax. II. Proper Motions and Radial Velocities
We investigate whether a misestimate of proper motions or radialvelocities could have been a source of substantial systematic errors inthe statistical parallax determination of the absolute magnitude of RRLyrae stars. In an earlier paper, we showed that the statisticalparallax method is extremely robust and rather insensitive to varioussystematic effects. The main potential problem with this method wouldtherefore arise from systematically bad observational inputs, propermotions, radial velocities, apparent magnitudes, and/or extinctions.Here we focus on the proper motions and radial velocities. We comparethree different catalogs of proper motions: Lick, Hipparcos, and the onecompiled by Wan et al. (WMJ). We find that the WMJ catalog is tooheterogeneous to be a reliable source. We analyze a sample of 165 haloRR Lyrae stars with either Lick or Hipparcos proper motions. For thestars with both Lick and Hipparcos proper motions, we use the weightedmeans of reported values. Various possible biases are investigatedthrough vigorous Monte Carlo simulations, and we evaluate the smallcorrections due to Malmquist bias, anisotropic positions of the stars onthe sky, and non-Gaussian distribution of stellar velocities. The meanRR Lyrae absolute magnitude is M_V = 0.74 +/- 0.12 at the meanmetallicity of the sample, <[Fe/H]> = -1.60, only 0.01 magbrighter than the value obtained in the previous study, which did notincorporate Hipparcos proper motions. To test for systematics in the RRLyrae radial velocities, we analyze a non-kinematically selected sample([Fe/H] <= -1.5) of 103 RR Lyrae stars with Hipparcos and/or Lickproper motions and 724 non-RR Lyrae stars from Beers &Sommer-Larsen. We find M_V = 0.79 +/- 0.12 at <[Fe/H]> = -1.79.Because the radial velocities in this sample are dominated by non-RRLyrae stars, the agreement of the two determinations suggests that thepure RR Lyrae sample is not significantly affected by systematics inradial velocities. If the two determination are combined (taking intoaccount the 0.45 correlation coefficient between them), the net resultis M_V = 0.77 +/- 0.10 at <[Fe/H]> = -1.71. The faint absolutemagnitudes of RR Lyrae stars confirmed by this analysis gives strongsupport to the short distance scale.
| Early evolution of the Galactic halo revealed from Hipparcos observations of metal-poor stars
The kinematics of 122 red giant and 124 RR Lyrae stars in the solarneighborhood are studied using accurate measurements of their propermotions obtained by the Hipparcos astrometry satellite, combined withtheir published photometric distances, metal abundances, and radialvelocities. A majority of these sample stars have metal abundances of(Fe/H) = -1 or less and thus represent the old stellar populations inthe Galaxy. The halo component, with (Fe/H) = -1.6 or less, ischaracterized by a lack of systemic rotation and a radially elongatedvelocity ellipsoid. About 16 percent of such metal-poor stars have loworbital eccentricities, and we see no evidence of a correlation between(Fe/H) and e. Based on the model for the e-distribution of orbits, weshow that this fraction of low-e stars for (Fe/H) = -1.6 or less isexplained by the halo component alone, without introducing the extradisk component claimed by recent workers. This is also supported by theabsence of a significant change in the e-distribution with height fromthe Galactic plane. In the intermediate-metallicity range, we find thatstars with disklike kinematics have only modest effects on thedistributions of rotational velocities and e for the sample at absolutevalue of z less than 1 kpc. This disk component appears to constituteonly 10 percent for (Fe/H) between -1.6 and -1 and 20 percent for (Fe/H)between -1.4 and -1.
| The impact of HIPPARCOS on the RR Lyrae Distance Scale
Not Available
| Radial velocities and iron abundances of field RR Lyraes. I.
We present systemic velocities and iron abundances for 56 RR Lyraes, themajority of which have been observed by the HIPPARCOS satellite.Comparison between our systemic velocities and previous valuesidentifies several binary candidates only one of which, TU UMa, waspreviously suspected of being a binary. However, spectra of the unusualRR Lyrae BB Vir show no evidence of line doubling and hence do notsupport the recent claims that this star may have a Blue HorizontalBranch companion. Comparison between our abundances and previousdeterminations shows reasonable agreement except with the recent work of\cite[Layden (1994)]{Lay94} where we find systematic differences.Several of the stars included on the HIPPARCOS observing list as RRLyraes are shown to be mis-classified. Of particular interest are thestars V363 Cas and AT And which, by analogy with XZ Cet, may beanomalous Cepheids. The Appendix is available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| The Absolute Magnitude and Kinematics of RR Lyrae Stars Via Statistical Parallax
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996AJ....112.2110L&db_key=AST
| 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 Metallicities and Kinematics of RR Lyrae Variables.II. Galactic Structure and Formation from Local Stars
Abstract image available at:http://adsabs.harvard.edu/abs/1995AJ....110.2288L
| The Behlen Observatory variable star survey. Paper 3.
Finding charts, accurate coordinates and light curves are presented for146 variable stars including three which are newly discovered.Parameters descriptive of the light curves are tabulated includingperiods for eight stars which lacked them in the General Catalogue ofVariable Stars (the GCVS). GCVS periods of twelve stars were found to beseriously in error. The classification of the stars is discussed.Revisions or refinements of the classifications from the GeneralCatalogue of Variable of Stars are suggested for thirty-one stars. Ofthe nineteen stars classified as Bailey type c RR Lyrae stars in theGeneral Catalogue of Variable Stars, five are found to be short periodeclipsing or ellipsoidal variables. Seventeen percent of the Bailey typeab RR Lyrae stars and 14% of the type c's show scatter in their lightcurves which is suggestive of the Blazhko effect.
| Kinematics of metal-poor stars in the galaxy
We discuss the kinematic properties of a sample of 1936 Galactic stars,selected without kinematic bias, and with abundances (Fe/H) is less thanor equal to -0.6. The stars selected for this study all have measuredradial velocities, and the majority have abundances determined fromspectroscopic or narrow-/intermediate-band photometric techniques. Incontrast to previous examinations of the kinematics of the metal-poorstars in the Galaxy, our sample contains large numbers of stars that arelocated at distances in excess of 1 kpc from the Galactic plane. Thus, amuch clearer picture of the nature of the metal-deficient populations inthe Galaxy can now be drawn.
| Summary of Delta S metallicity measurements for bright RR Lyrae variables observed at Lick Observatory and KPNO between 1972 and 1987
From 1972 to 1987 we conducted a survey of the metallicity of faint RRLyrae variables in the Galactic halo, using the 'Butler system' of DeltaS. As part of the calibration of this program, we made approximately 500observations of bright RR Lyraes as abundance standards. We summarizeall the observations of these bright field RR Lyraes and provideaveraged values for the metallicity parameter Delta S. These averagesrepresent the most precise definition of the Butler system for themeasurement of RR Lyrae metallicities. The typical mean error is 0.3units in Delta S, which corresponds to 0.05 dex in (Fe/H). We alsobriefly discuss the weaknesses in the determination of (Fe/H) from DeltaS.
| Post-main-sequence and POST red giant branch variables with pulsation periods less than one day
Post-main-sequence (mass 1 to 3 solar masses) and post-giant branch (0.5to 1 solar mass) pulsators are discussed on the basis of four color andH beta light curves published elsewhere. The post-main-sequencevariables, called ultrashort period cepheid (USPC) (delta Sct), pulsatein the fundamental and first harmonic modes of radial pulsation and, inmany cases, in nonradial modes. The variables for which photometryallows accurate, luminosity estimates and are known to pulsatesimultaneously in the fundamental and first harmonic or in thefundamental mode alone, define a PL relation (MV = -2.80 logP - 0.60, fundamental). It is notable that the slope of this relation isin the range of slopes found for classical cepheids. Accurate Vphotometry is lacking for many of the variables known as 'anomalouscepheids', but the available data divide them into low mass,pseudocepheids (BL Her and W Vir stars) and post-main-sequence USPC(delta Sct) variables. Four USPC in NGC 5053 and six in NGC 6466, forwhich accurate photometry is available, give remarkably consistentmoduli of 16.06 +/- 0.05 and 15.98 +/- 0.08 mag, respectively, for theclusters, in which they are blue stragglers similar to SX Phe inKapteyn's star group. The assumption that the four post-giant branchvariables, called VSPC (RR Lyr), S Ari, SU Dra, and ST Leo in Kapteyn'sstar group and RR Lyr in the Groombridge 1830 group, are physicalmembers of these groups and share their V-velocities, leads to acalibration of the photometry for the derivation of reddening,luminosity, and heavy element abundance of 45 field variables. Theresulting reddenings are consistent with values obtained by othermethods and the metallicities are consistent with the most accuratelyavailable spectroscopic determinations of delta S and of Ca II K. Theluminosities of the bulk of the variables confirm Sandage's (1993)relation between MV and (Fe/H). Four or five of the fieldvariables are probably binary, including BB Vir which Kinman &Carreta (1992) have independently noted as double. The PL relation forUSPC (delta Sct) variables intersects the horizontal branch (HB) near P= 0.3d and at least two field very short period cepheid (VSPC) (RR Lyr)star, FW Lup (0.484 d) and ST Pic (0.486 d) may be first overtonepulsators of the USPC (delta Sct) variety. A dozen field VSPC (RR Lyr)stars populate a (Fe/H), MV relation with the same slope asthe other stars but displaced 0.7 mag toward higher luminosities. Theonly cluster variable found to populate this diplaced relation is No. 9in 47 Tuc, although ST Vir, which may be a member of the Arcturus group,should also be considered. The elevated luminosities are unlikely to becaused by either evolution or errors in the photometric indices. Apossible source of these apparently young VSPC(RR Lyr) variables withhalo metallicity is in second (or third) generation globular clustersformed during an episodic collapse of the galaxy that produced metalpoor stars but in a dynamical situation that hastened the disruption ofthe clusters, currently formed, before the still older globularclusters, created under conditions that have kept them in a moredisruptive free environment.
| The very short period Cepheid (RR Lyr) variables. 2: Light and color curves of variables in the solar vicinity
Four color and H beta observations for 43 very short period Cepheids(VSPC, RRLyr) variables have been obtained with the Cerro Tololo andKitt Peak reflectors. The color systems are defined in Eggen (1982).Contemporary, photo-electric V-light curves have been used to establishthe phasing and the resulting periods used to compute the phases for thepresent observations. These phases are then adjusted to fit the V-lightcurves and the resulting periods and adjusted phases are given.
| BB Virginis: an RR Lyrae in a binary system?
Not Available
| The Oosterhoff period-metallicity relation for RR Lyrae stars at the blue fundamental edge of the instability strip.
It is argued that the division of cluster variables into two nearlydiscrete period groups, which is the Oosterhoff dichotomy, is due to acombination of the continuous variation of period with metallicity andthe blueward progression of cluster horizontal branches such as M13 outof the instability strip for intermediate metallicities for (Fe/H)between about -1.7 and -1.9. The subsequent evolutionary tracks,starting beyond the blue side of the instability strip, move into thestrip above the zero-age horizontal branch, producing longer periods inthis metallicity range. The strong variation of period with metallicityis seen both in the cluster data and in the field star data.
| Infrared photometry and radial velocities of field RR Lyraes
Infrared photometry of 110 field RR Lyraes is presented along withradial velocities of 13 field RR Lyraes. The methods used are described.
| A re-analysis of the period shifts in RR Lyrae stars
The period shift in both field and globular cluster RR Lyrae stars isexamined. The stellar pulsation theory called the Sandage Period Shiftto determine the mean M(V) of RR Lyrae stars is investigated. Theadvantages of (V-K) compared to (B-V) as a temperature indicator for RRLyraes are discussed in detail. Period shift-metallicity relations arederived using recently published infrared photometry of field RR Lyraesand globular cluster RR Lyraes. Other method for determining mean M(V)for RR Lyraes are critically reviewed. It is argued that results formain sequence fitting, statistical parallax, and Red Giant Branch theoryare presently too uncertain to be used. The slope of themass-metallicity relation from pulsation theory is in seriousdisagreement with that from Horizontal Branch Theory.
| Astrophysics in 1992
An overview of astrophysics research in 1992 is presented. Attention isgiven to investigations of the sun, extrasolar-system planets, thesearch for brown dwarfs, triggered star formation, gamma-ray sources,the unified model of active galaxies, and large-scale lumpiness in theuniverse. The solar system and Milky Way are discussed briefly, andvarious corrections and updates are given.
| The reddening of type AB RR Lyrae stars
The paper modifies Sturch's (1966) method for deriving, from observednear-minimum light colors, EB-V values for RR Lyrae starswith Bailey's types for a or b light curves in order to avoid the use ofreddening and metallicity-sensitive U-B colors. The Delta(S), (Fe/H)calibration is examined, and blanketing corrections are derived fromsynthetic colors of models by Kurucz (1975, 1979). Sturch's finding thatthe intrinsic blanketing-corrected near-minimum light B-V color of avariable can be estimated from its period is verified. The inherentaccuracy of the method is discussed and found to depend appreciably oncycle-to-cycle color variations. Comparisons are made with otherreddening determinations. The blanketing corrections determined bySturch from delta(U-B) values are found to make his EB-Vvalues less than those found in the present study, while his estimatedintrinsic colors make his EB-V values greater than thosefound in this study.
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| Csillagkép: | Szűz |
| Rektaszcenzió: | 13h51m40.78s |
| Deklináció: | +06°25'51.4" |
| Vizuális fényesség: | 11.319 |
| RA sajátmozgás: | -51.1 |
| Dec sajátmozgás: | -2.3 |
| B-T magnitude: | 11.245 |
| V-T magnitude: | 11.313 |
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