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New insights on the complex planetary nebula Hen 2-113
We report on infrared observations of the planetary nebula Hen 2-113obtained with VLT/NACO, VLTI/MIDI, VLT/ISAAC and TIMMI at the ESO 3.6 m.Hen 2-113 exhibits a clear ring-like structure superimposed to a morediffuse environment visible in the L' (3.8 μm), M' (4.78 μm) and8.7 μm bands. No clear core at 8.7 μm and no fringes through the Nband could be detected for this object with MIDI. A qualitativeinterpretation of the object structure is proposed using a diabolo-likegeometrical model. The PAH content of the nebula was also studied withISAAC and TIMMI observations. This indicates that the PAHs are mostlyconcentrated towards the lobes of the diabolo and the bipolar lobes ofthe nebula. In L' band, a void 0.3 arcsec in diameter was discoveredwith NACO around the central source. The L' and M' fluxes from thecentral source were derived from NACO data indicating an importantinfrared excess with respect to the expected stellar emission based onstellar models and short wavelength data. The observed flux from thissource in the L' and M' is about 300 and 800 times respectively thanthose expected from a model including only the central star. Moreover,the central object appears resolved in L' band with measured FWHM of 155mas. This infrared excess can be explained by emission from a cocoon ofhot dust (T1000 K) with a total mass~10-9~Mȯ.
| Chromospheric models of solar analogues with different activity levels
We computed chromospheric models of the Sun as a star and of nine solaranalogues. The atmospheric models were constructed to obtain the bestpossible match with the Ca II K and Hβ lines, including theasymmetry of the lines due to macroscopic velocity fields. The starswere chosen with 0.62 < B-V< 0.68 (the solar B-V=0.65) and have awide variety of magnetic activity levels, which allows us to study thedifferences in atmospheric structures induced by activity. For the lessactive stars we found that the changes with activity are in the regionof the temperature minimum, while the most active stars show changes allalong their atmospheric structures, mainly in the upper chromosphere.Regarding the macroscopic velocity fields, we can distinguish betweenthe two groups. The most active group has a velocity field in thetemperature-minimum region, and the other group in the chromosphericplateau. We also computed the net radiative losses for each model, andfound that they depend linearly on the usual index of chromosphericactivity, SCa II.
| NEXXUS: A comprehensive ROSAT survey of coronal X-ray emission among nearby solar-like stars
We present a final summary of all ROSAT X-ray observations of nearbystars. All available ROSAT observations with the ROSAT PSPC, HRI and WFChave been matched with the CNS4 catalog of nearby stars and the resultsgathered in the Nearby X-ray and XUV-emitting Stars data base, availablevia www from the Home Page of the Hamburger Sternwarte at the URLhttp://www.hs.uni-hamburg.de/DE/For/Gal/Xgroup/nexxus. Newvolume-limited samples of F/G-stars (dlim = 14 pc), K-stars(dlim = 12 pc), and M-stars (dlim = 6 pc) areconstructed within which detection rates of more than 90% are obtained;only one star (GJ 1002) remains undetected in a pointed follow-upobservation. F/G-stars, K-stars and M-stars have indistinguishablesurface X-ray flux distributions, and the lower envelope of the observeddistribution at FX ≈ 104 erg/cm2/sis the X-ray flux level observed in solar coronal holes. Large amplitudevariations in X-ray flux are uncommon for solar-like stars, but maybemore common for stars near the bottom of the main sequence; a largeamplitude flare is reported for the M star LHS 288. Long term X-raylight curves are presented for α Cen A/B and Gl 86, showingvariations on time scales of weeks and demonstrating that α Cen Bis a flare star.Tables 1-3 are also 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/417/651
| Target Selection for SETI. II. Tycho-2 Dwarfs, Old Open Clusters, and the Nearest 100 Stars
We present the full target list and prioritization algorithm developedfor use by the microwave search for technological signals at the SETIInstitute. We have included the Catalog of Nearby Habitable StellarSystems (HabCat, described in Paper I), all of the nearest 100 stars and14 old open clusters. This is further augmented by a subset of theTycho-2 catalog based on reduced proper motions, and this larger catalogshould routinely provide at least three target stars within the largeprimary field of view of the Allen Telescope Array. The algorithm forprioritizing objects in the full target list includes scoring based onthe subset category of each target (i.e., HabCat, cluster, Tycho-2, ornearest 100), its distance (if known), and its proximity to the Sun onthe color-magnitude diagram.
| The mineralogy, geometry and mass-loss history of IRAS 16342-3814
We present the 2-200 mu m Infrared Space Observatory (ISO) spectrum and3.8-20 mu m ISAAC and TIMMI2 images of the extreme OH/IR star IRAS16342-3814. Amorphous silicate absorption features are seen at 10 and 20mu m, together with crystalline silicate absorption features up toalmost 45 mu m. No other OH/IR star is known to have crystallinesilicate features in absorption up to these wavelengths. This suggeststhat IRAS 16342-3814 must have, or recently had, an extremely highmass-loss rate. Indeed, preliminary radiative transfer calculationssuggest that the mass-loss rate may be as large as 10-3Msun yr-1. The 3.8 mu m ISAAC image shows abipolar reflection nebula with a dark equatorial waist or torus, similarto that seen in optical images taken with the Hubble Space Telescope(HST). The position angle of the nebula decreases significantly withincreasing wavelength, suggesting that the dominant source of emissionchanges from scattering to thermal emission. Still, even up to 20 mu mthe nebula is oriented approximately along the major axis of the nebulaseen in the HST and ISAAC images, suggesting that the torus must be verycold, in agreement with the very red ISO spectrum. The 20 mu m imageshows a roughly spherically symmetric extended halo, approximately 6''in diameter, which is probably due to a previous phase of mass-loss onthe AGB, suggesting a transition from a (more) spherically symmetric toa (more) axial symmetric form of mass-loss at the end of the AGB. Usinga simple model, we estimate the maximum dust particle sizes in the torusand in the reflection nebula to be 1.3 and 0.09 mu m respectively. Thesize of the particles in the torus is large compared to typical ISMvalues, but in agreement with high mass-loss rate objects like AFGL 4106and HD161796. We discuss the possible reason for the difference inparticle size between the torus and the reflection nebula.Based on observations with ISO, an ESA project with instruments fundedby ESA Member States (especially the PI countries: France, Germany, TheNetherlands and the UK) with the participation of ISAS and NASA. The SWSis a joint project of SRON and MPE. Also based on observations obtainedat the European Southern Observatory (ESO).
| 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 radii and spectra of the nearest stars
We discuss direct measurements of the radii of 36 stars located closerthan 25 parsecs to the Sun. We present the data on 307 radii and 326spectral types and luminosity classes for the nearest stars locatedinside the sphere with a radius of 10 parsecs.
| UBV(RI)C photometry of Hipparcos red stars
We present homogeneous and standardized UBV(RI)C photometryfor nearly 550 M stars selected from the Hipparcos satellite data baseusing the following selection criteria: lack of obvious variability (noHipparcos variability flag); δ<+10°(V-I)>1.7 and Vmagnitude fainter than about 7.6. Comparisons are made between thecurrent photometry, other ground-based data sets and Hipparcosphotometry. We use linear discriminant analysis to determine aluminosity segregation criterion for late-type stars, and principalcomponent analysis to study the statistical structure of the colourindices and to calibrate absolute magnitude in terms of (V-I) for thedwarf stars. Various methods are used to determine the mean absolutemagnitude of the giant stars. We find 10 dwarf stars, apparentlypreviously unrecognized (prior to Hipparcos) as being within 25pc,including five within 20pc.
| 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.
| 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
| Emission Lines in the Spectrum of the Red-Dwarf Flare Star EV Lac: Modeling of the Quiescent Chromosphere
We present spectral observations of the red-dwarf flare star EV Lac madeat the Crimean Astrophysical Observatory in 1994 and 1995, and describea method for semi-empirical modeling of the chromospheres of red dwarfsbased on their emission spectra. We have modeled the quiescent state ofthe chromosphere of EV Lac for the cases of a homogeneous chromosphereand of active regions covering one-half and one-third the stellarsurface. All models that are consistent with the observations indicate aregion with a small vertical temperature gradient, a so-calledtemperature plateau. The calculated structure of the stellarchromosphere is compared with that of the solar chromosphere.
| Building Reliable Models of M Dwarf Chromospheres: The Spectral Diagnostics
As part of an ongoing project to study how reliable are thechromospheric models constructed semiempirically to fit thechromospheric spectrum of cold stars, in this paper we study how changesin the assumed chromospheric structure of dM and dMe stars affect theemitted spectrum. In this way, we study if a given set of features canwholly determine the atmospheric structure, how large are theindeterminations in the atmospheric parameters deduced, and to whatextent the atmospheric model computed can be considered unique. We findthat the profiles of the Ca II K line or the Na D lines can be used todetermine the structure of the Tmin region and that theHα profile can provide good information on the structure of thechromosphere. The Lyα flux, in turn, can be used to constrain theposition of the transition region.
| Nearby Microlensing Events: Identification of the Candidates for theSpace Interferometry Mission
The Space Interferometry Mission (SIM) is the instrument of choice whenit comes to observing astrometric microlensing events where nearby,usually high proper motion, stars (``lenses'') pass in front of moredistant stars (``sources''). Each such encounter produces a deflectionin the source's apparent position that, when observed by SIM, can leadto a precise mass determination of the nearby lens star. We search forlens-source encounters during the 2005-2015 period using Hipparcos, ACT,and NLTT to select lenses, and USNO-A2.0 to search for the correspondingsources, and rank these by the SIM time required for a 1% massmeasurement. For Hipparcos and ACT lenses, the lens distance andlens-source impact parameter are precisely determined so that the eventsare well characterized. We present 32 candidates beginning with a 61 CygA event in 2012 that requires only a few minutes of SIM time. ProximaCentauri and Barnard's star each generate several events. For NLTTlenses, the distance is known only to a factor of 3, and the impactparameter only to 1''. Together, these produce uncertaintiesof a factor ~10 in the amount of SIM time required. We present a list of146 NLTT candidates and show how single-epoch CCD photometry of thecandidates could reduce the uncertainty in SIM time to a factor of ~1.5.
| Modelling of flares on late-type stars.
Stellar flare research is an exciting and rapidly developing field ofastrophysics. The Sun is an invaluable proving ground to testpredictions of flare theories and to develop analytical techniques forfuture stellar applications, because the lack of spatial resolution forstellar flares pushes us to extrapolate models of solar flares to thestellar situation. Stellar flares can sometimes be several orders ofmagnitude more energetic than their solar counterparts, which maysuggest that new phenomena are taking place which are not observed onthe Sun. Because of widely different energy ranges and atmosphericproperties, the investigation of stellar flares is seen as a potentialbreakthrough in our understanding of flares as a whole. Becauseflarelike physical processes occur in diverse astrophysicallyinteresting regimes, the field of solar and stellar flares, andtherefore, their modelling can serve as an astrophysical touchstone.
| 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
| Building reliable models of M dwarf chromospheres: the impact of the usual assumptions
We study different approximations usually made to simplify thecalculation of chromospheric models of M dwarf stars. The approximationswe discuss in details are: the assumption that the minority species arein LTE, the omission of the contribution of numerous atomic andmolecular lines (line blanketing) to the opacity, and the CompleteFrequency Redistribution for the Lyman alpha line. We consider a ``cold"chromospheric model corresponding to a low activity dM star and a ``hot"one corresponding to a very active dMe star. We find that theassumptions under study affect more strongly the cold than the hotmodel. In particular the approximation of Complete FrequencyRedistribution in the Lyman alpha line, through the statisticalequilibrium and ionization equilibrium equation, changes the electrondensity in the high chromosphere and strongly affects other lineprofiles.
| Supplementary southern standards for UBV(RI)c photometry
We present UBV(RI)c photometry for 80 southern red and blue stars foruse as additional standards. The data are tied to the Johnson UBV andCousins (RI)c systems and extend the range of the available stars forcolor equation determination, especially in (U-B) for blue stars and(V-R) and (V-I) for red stars. Comparisons with published data are madeand particularly good agreement is found with Bessell for the red(Gliese) stars.
| Chromospheric models of dwarf M stars.
We present chromospheric models for two dM stars considered as ``basal''stars due to the low level of chromospheric activity, and compare themwith the model for a very active, flare star obtained in a previouspaper. These models are not based on a single spectral feature, but onthe continuum in a broad wavelength range (3500-9000Å), on manyline profiles corresponding to three different atoms (H, Ca, Na), and onthe Mg II h and k flux. We show that a marked chromosphere is presenteven for stars with the lowest levels of activity, and that the activestars have both a chromospheric temperature rise at larger column massand a higher chromospheric temperature. These characteristics areresponsible for the presence of the Balmer lines in emission in the dMestars. We also show that the additional energy required to transform adM star into an active star must be deposited in the high chromosphere,just below the transition region.
| Astrometric positions of stars with high proper motions in the Southern Hemisphere
Several stars with large proper motions, cited by W.J. Luyten, wereincluded in the preliminary programme for the HIPPARCOS mission. Whenperforming preparatory measurements of plates, difficulties wereencountered in identifying certain of these stars when relying only onpublished coordinates. We have taken advantage of this work whichrelates to the southern sky in order to determine the astrometricposition of the greatest possible number of these objects, even forthose which were not included in the programme. Catalogue 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/Abstract.html
| The Palomar/MSU Nearby Star Spectroscopic Survey.II.The Southern M Dwarfs and Investigation of Magnetic Activity
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996AJ....112.2799H&db_key=AST
| Distribution and Corrlation of Age, Abundance, and Motion of Lower Main Sequence Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996AJ....111..466E&db_key=AST
| Correlations of Coronal X-Ray Emission with Activity, Mass, and Age of the Nearby K and M Dwarfs
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...450..401F&db_key=AST
| The X-Ray View of the Low-Mass Stars in the Solar Neighborhood
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...450..392S&db_key=AST
| A volume-limited ROSAT survey of extreme ultraviolet emission from all nondegenerate stars within 10 parsecs
We report the results of a volume-limited ROSAT Wide Field Camera (WFC)survey of all nondegenerate stars within 10 pc. Of the 220 known starsystems within 10 pc, we find that 41 are positive detections in atleast one of the two WFC filter bandpasses (S1 and S2), while weconsider another 14 to be marginal detections. We compute X-rayluminosities for the WFC detections using Einstein Imaging ProportionalCounter (IPC) data, and these IPC luminosities are discussed along withthe WFC luminosities throughout the paper for purposes of comparison.Extreme ultraviolet (EUV) luminosity functions are computed for singlestars of different spectral types using both S1 and S2 luminosities, andthese luminosity functions are compared with X-ray luminosity functionsderived by previous authors using IPC data. We also analyze the S1 andS2 luminosity functions of the binary stars within 10 pc. We find thatmost stars in binary systems do not emit EUV radiation at levelsdifferent from those of single stars, but there may be a fewEUV-luminous multiple-star systems which emit excess EUV radiation dueto some effect of binarity. In general, the ratio of X-ray luminosity toEUV luminosity increases with increasing coronal emission, suggestingthat coronally active stars have higher coronal temperatures. We findthat our S1, S2, and IPC luminosities are well correlated withrotational velocity, and we compare activity-rotation relationsdetermined using these different luminosities. Late M stars are found tobe significantly less luminous in the EUV than other late-type stars.The most natural explanation for this results is the concept of coronalsaturation -- the idea that late-type stars can emit only a limitedfraction of their total luminosity in X-ray and EUV radiation, whichmeans stars with very low bolometric luminosities must have relativelylow X-ray and EUV luminosities as well. The maximum level of coronalemission from stars with earlier spectral types is studied also. Tounderstand the saturation levels for these stars, we have compiled alarge number of IPC luminosities for stars with a wide variety ofspectral types and luminosity classes. We show quantitatively that ifthe Sun were completely covered with X-ray-emitting coronal loops, itwould be near the saturation limit implied by this compilation,supporting the idea that stars near upper limits in coronal activity arecompletely covered with active regions.
| The MSSSO near-infrared photometric system
The JHKL photometric system currently used at the Mount Stromlo andSiding Spring Observatories (MSSSO) is described via an extensive listof standard-star values and filter transmission curves. At JHK thissystem is identical to the Mount Stromlo Observatory (MSO) systemdefined by Jones and Hyland (1982), except for small zero-pointdifferences which we impose here. Transformations are given between theMSSSO system and several near-infrared photometric systems in use inother observatories and the homogenized JHKL system proposed by Besselland Brett (1988).
| Infrared sources in the neighbourhood of the Sun.
Not Available
| Far infrared properties of late type dwarfs. Infrared fluxes of K & M dwarfs
IRAS fluxes/upper limits are presented for a large sample of K and Mdwarfs. Good agreement is found between the 12 micrometer fluxes andthose derived from the photospheric models of Mould (1976).Relationships between the optical and infrared colors are derived. Theactive dMe/dKe stars appear systematically brighter in the infraredcompared with the less active dM/dK stars, which could be attributed tomore efficient nonradiative heating in their atmosphere. Any systematicdifferences found in our results when compared with those obtained fromprevious studies are attributed to the different analysis packages used.
| The importance of surface inhomogeneities for K and M dwarf chromospheric fluxes
We present published and archived spectroscopic and spectrophotometricdata of H-alpha, Ca II, Mg II, and X-rays for a large sample of K and Mdwarfs. The data set points to the importance that surfaceinhomogeneities have in the flux luminosity diagrams in these late-typedwarfs, irrespective of whether the Balmer lines are in emission orabsorption. Although supporting the fact that cooler stars exhibitincreasing levels of surface activity, evident through an increasingincidence of Balmer emission, surface inhomogeneities, or variations inthe local temperature and density structure, at the chromospheric level,dominate the total Ca II and Mg II fluxes. We show that the flux-fluxand luminosity-luminosity relations indicate differing extents ofinhomogeneity from the chromosphere through to the corona. A goodcorrelation between Ca II and Mg II fluxes indicates that they areformed in overlapping regions of the chromosphere, so that thecontribution of surface inhomogeneities is not evident from thisparticular flux-flux diagram. In the region of the upper chromospherethrough to the transition and corona, the correlation between Ly-alphaand X-ray fluxes indicates regions with similar levels of arealinhomogeneity. This appears to be uncorrelated with that at thechromospheric level.
| 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.
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Наблюдательные данные и астрометрия
| Созвездие: | Волк |
| Прямое восхождение: | 15h32m12.93s |
| Склонение: | -41°16'32.1" |
| Видимая звёздная величина: | 9.395 |
| Расстояние: | 5.934 парсек |
| Собственное движение RA: | -1174.9 |
| Собственное движение Dec: | -1030.4 |
| B-T magnitude: | 11.25 |
| V-T magnitude: | 9.549 |
Каталоги и обозначения:
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