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Class I and Class II methanol masers in high-mass star-forming regions
Context. Among the tracers of the earliest phases in the massive starformation process, methanol masers have gained increasing importance.The phenomenological distinction between Class I and II methanol masersis based on their spatial association with objects such as jets, cores,and ultracompact Hii regions, but is also believed to correspond todifferent pumping mechanisms: radiation for Class II masers, collisionsfor Class I masers. Aims: We surveyed a large sample of massivestar-forming regions in Class I and II methanol masers. The sampleconsists of 296 sources, divided into two groups named high and lowaccording to their [25-12] and [60-12] IRAS colours. Previous studiesindicate that the two groups may contain similar sources in differentevolutionary stages, with the high sources representing the more evolvedstages. Therefore, the sample can be used to assess a sequence for theoccurrence of Class I and II methanol masers during the evolution of amassive star-forming region. Methods: We observed the 6 GHz(Class II) CH3OH maser with the Effelsberg 100-m telescope,and the 44 GHz and 95 GHz (Class I) CH3OH masers with theNobeyama 45-m telescope. Results: We detected 55 sources in theClass II line (39 high and 16 low, 12 new detections); 27 sources in the44 GHz Class I line (19 high and 8 low, 17 new detections); 11 sourcesin the 95 GHz Class I line (eight high and three low, all except one arenew detections). The detection rate of Class II masers decreases withthe distance of the source (as expected), whereas that of Class I maserspeaks at ~5 kpc. This could be due to the Class I maser spots beingspread over a region ?1 pc, comparable to the telescope beamdiameter at a distance of ~5 kpc. We also find that the two Class Ilines have similar spectral shapes at 44 GHz and 95 GHz, which confirmsthat they have the same origin. Conclusions: Our statisticalanalysis shows that the ratio between the detection rates of Class IIand Class I methanol masers is basically the same in high and lowsources. Therefore, both maser types seem to be equally associated witheach evolutionary phase. In contrast, all maser species (includingH2O) have about three times higher detection rates in highthan in low sources. This could indicate that the phenomena from whichall masers originate become progressively more active with time duringthe earliest evolutionary phases of a high-mass star-forming region.Appendices are only available in electronic form at http://www.aanda.org
| Be phenomenon in open clusters: results from a survey of emission-line stars in young open clusters
Emission-line stars in young open clusters are identified to study theirproperties, as a function of age, spectral type and evolutionary state.207 open star clusters were observed using the slitless spectroscopymethod and 157 emission stars were identified in 42 clusters. We havefound 54 new emission-line stars in 24 open clusters, out of which 19clusters are found to house emission stars for the first time. About 20per cent clusters harbour emission stars. The fraction of clustershousing emission stars is maximum in both the 0-10 and 20-30 Myr age bin(~40 per cent each). Most of the emission stars in our survey belong toClassical Be class (~92 per cent) while a few are Herbig Be stars (~6per cent) and Herbig Ae stars (~2 per cent). The youngest clusters tohave Classical Be stars are IC 1590, NGC 637 and 1624 (all 4 Myr old)while NGC 6756 (125-150 Myr) is the oldest cluster to have Classical Bestars. The Classical Be stars are located all along the main sequence(MS) in the optical colour-magnitude diagrams (CMDs) of clusters of allages, which indicates that the Be phenomenon is unlikely due to corecontraction near the turn-off. The distribution of Classical Be stars asa function of spectral type shows peaks at B1-B2 and B6-B7 spectraltypes. The Be star fraction [N(Be)/N(B+Be)] is found to be less than 10per cent for most of the clusters and NGC 2345 is found to have thelargest fraction (~26 per cent). Our results indicate there could be twomechanisms responsible for the Classical Be phenomenon. Some are bornClassical Be stars (fast rotators), as indicated by their presence inclusters younger than 10 Myr. Some stars evolve to Classical Be stars,within the MS lifetime, as indicated by the enhancement in the fractionof clusters with Classical Be stars in the 20-30 Myr age bin.
| A survey of OH masers towards high mass protostellar objects
Context: Masers are important tracers of the early evolution of younghigh mass stars, but the relationship between different types of maserand the evolutionary state of the exciting source remains unclear. Aims: To determine whether OH masers are common towards candidate highmass protostellar objects. Methods: We present a survey of OH maseremission towards a sample of high mass protostellar objects made usingthe Nançay and GBT telescopes. Results: OH maser emission wasdetected towards 63 objects with 36 new detections. There are 56star-forming regions and 7 OH/IR candidates. Nearly half of the detectedsources have OH flux densities ⪉1 Jy. There is no evidence thatsources with OH masers have a different range of luminosities from thenon-maser sources. The results of this survey are compared with previousH2O and class II CH3OH maser observations of the same objects. Some ofthe detected sources are only associated with OH masers and some sourcesare only associated with the 1720 MHz OH maser line. The velocity rangeof the maser emission suggests that the water maser sources may bedivided into two groups. The detection rates and velocity range of theOH and Class II CH3OH masers support the idea that there is a spatialassociation of the OH and Class II CH3OH masers. The sources span a widerange in R, the ratio of the methanol maser peak flux to OH 1665 MHzmaser peak flux, however there are only a few sources with intermediatevalues of R, 8
| A catalogue of eclipsing variables
A new catalogue of 6330 eclipsing variable stars is presented. Thecatalogue was developed from the General Catalogue of Variable Stars(GCVS) and its textual remarks by including recently publishedinformation about classification of 843 systems and making correspondingcorrections of GCVS data. The catalogue1 represents thelargest list of eclipsing binaries classified from observations.
| Close binary stars in ob-association regions i. preliminary investigation
We performed a sample of O- and B-eclipsing binary stars inOB-association regions and obtained the preliminary list of 147 binariesin 45 OB-association regions. We tried to elucidate the question whether(or not) the close binaries belong to corresponding OB-associations,from the commonness of their proper motions, radial velocities anddistances. Based on the completeness of the data,the binaries aredevided into three groups and the scheme for calculation of degree ofbelonging of stars to OB-associations is developed. Necessary data arenot available for nine systems and they are given in a specific table.For 12 cases, the binaries project onto the regions of two associations.We show that 33 (22.3%) close binary stars are members, 65 (43.9%) areprobable members and 39 (26.4%) are less probable members of theOB-associations. We find that 11 binaries belong to the Galaxybackground. The comparison of the distributions of orbital periods forthe binaries in OB-associations and for O-, B-binaries of the Galaxybackground shows their considerable differences in the vicinity of thetwo-day period.
| The association of IRAS sources and 12CO emission in the outer Galaxy
We have revisited the question of the association of CO emission withIRAS sources in the outer Galaxy using data from the FCRAO Outer GalaxySurvey (OGS). The availability of a large-scale high-resolution COsurvey allows us to approach the question of IRAS-CO associations from anew direction - namely we examined all of the IRAS sources within theOGS region for associated molecular material. By investigating theassociation of molecular material with random lines of sight in the OGSregion we were able to construct a quantitative means to judge thelikelihood that any given IRAS-CO association is valid and todisentangle multiple emission components along the line of sight. Thepaper presents a list of all of the IRAS-CO associations in the OGSregion. We show that, within the OGS region, there is a significantincrease ( ~ 22%) in the number of probable star forming regions overprevious targeted CO surveys towards IRAS sources. As a demonstration ofthe utility of the IRAS-CO association table we present the results ofthree brief studies on candidate zone-of-avoidance galaxies with IRAScounterparts, far outer Galaxy CO clouds, and very bright CO clouds withno associated IRAS sources. We find that ~ 25% of such candidate ZOAGsare Galactic objects. We have discovered two new far outer Galaxystar-forming regions, and have discovered six bright molecular cloudsthat we believe are ideal targets for the investigation of the earlieststages of sequential star formation around HII regions. Finally, thispaper provides readers with the necessary data to compare othercatalogued data sets with the OGS data.Tables 1, 2 and A1 are only available in electronic form at the CDS viaanonymous ftp to\ cdsarc.u-strasbg.fr (130.79.128.5) or via\http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/399/1083
| Detecting Embedded Intermediate-Mass Stars Using Mid-Infrared and H I 21 Centimeter Emission
A technique is presented to detect distant, young embedded B stars (andpossible clusters) from their imprint on the surrounding interstellarmedium. H I 21 cm and 12CO (J=1-0) line data from theCanadian Galactic Plane Survey are combined with mid-infrared imagesfrom the Midcourse Space Experiment (MSX) Galactic plane survey todetect the photodissociation regions (PDRs) and molecular gas associatedwith the embedded intermediate-mass stars. The technique has beenapplied to a section of the Galaxy covered by the 12CO FiveCollege Radio Astronomy Observatory outer Galaxy survey(102.5d
| Absolute proper motions of open clusters. I. Observational data
Mean proper motions and parallaxes of 205 open clusters were determinedfrom their member stars found in the Hipparcos Catalogue. 360 clusterswere searched for possible members, excluding nearby clusters withdistances D < 200 pc. Members were selected using ground basedinformation (photometry, radial velocity, proper motion, distance fromthe cluster centre) and information provided by Hipparcos (propermotion, parallax). Altogether 630 certain and 100 possible members werefound. A comparison of the Hipparcos parallaxes with photometricdistances of open clusters shows good agreement. The Hipparcos dataconfirm or reject the membership of several Cepheids in the studiedclusters. Tables 1 and 2 are only 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
| A survey of the 6.7 GHz methanol maser emission from IRAS sources. I. Data
We report the first results of a search for 6.7 GHz methanol masers inthe direction of 1399 IRAS objects north of declination-20deg with the flux densities greater than 100 Jy at 60 mu mand the flux density ratio F60/F25>1.Observations were made with the sensitivity of 1.7 Jy and the velocityresolution of 0.04 km s-1 using the 32-m Toruń radiotelescope. Maser emission was found in 182 sources, including 70 newdetections. 32 new sources were identified with objects of radioemission associated with star-forming regions. Comparison of the presentdata set with other observations suggests that about 65% of methanolmasers exhibit moderate or strong variations on time-scales of about 4and 8 years. Table 2 is 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/Abstract.html
| A search for spectroscopic binaries among Herbig Ae/Be stars
We present the results of a spectroscopic survey of binaries among 42bright (m_V<11) Herbig Ae/Be stars in both hemispheres. Radialvelocity variations were found in 7 targets, 4 are new spectroscopicbinaries. The Li I 6 708 Angstroms absorption line (absent feature insimple HAeBe stars spectra) indicates the presence of a cooler companionin 6 HAeBe spectrum binaries, 4 of which are new detections. Few starsclassified as possible Herbig Ae/Be stars are not confirmed as such.While for short-period (P<100 days) spectroscopic binaries, theobserved binary frequency is 10%, the true spectroscopic binaryfrequency for Herbig Ae/Be stars may be as high as 35%. Based onobservations collected at the European Southern Observatory (ESO), LaSilla, Chile and at the Observatoire de Haute--Provence (OHP),Saint--Michel l'Observatoire, France. Table 1 only available inelectronic form at CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html
| A HIPPARCOS Census of the Nearby OB Associations
A comprehensive census of the stellar content of the OB associationswithin 1 kpc from the Sun is presented, based on Hipparcos positions,proper motions, and parallaxes. It is a key part of a long-term projectto study the formation, structure, and evolution of nearby young stellargroups and related star-forming regions. OB associations are unbound``moving groups,'' which can be detected kinematically because of theirsmall internal velocity dispersion. The nearby associations have a largeextent on the sky, which traditionally has limited astrometricmembership determination to bright stars (V<~6 mag), with spectraltypes earlier than ~B5. The Hipparcos measurements allow a majorimprovement in this situation. Moving groups are identified in theHipparcos Catalog by combining de Bruijne's refurbished convergent pointmethod with the ``Spaghetti method'' of Hoogerwerf & Aguilar.Astrometric members are listed for 12 young stellar groups, out to adistance of ~650 pc. These are the three subgroups Upper Scorpius, UpperCentaurus Lupus, and Lower Centaurus Crux of Sco OB2, as well as VelOB2, Tr 10, Col 121, Per OB2, alpha Persei (Per OB3), Cas-Tau, Lac OB1,Cep OB2, and a new group in Cepheus, designated as Cep OB6. Theselection procedure corrects the list of previously known astrometricand photometric B- and A-type members in these groups and identifiesmany new members, including a significant number of F stars, as well asevolved stars, e.g., the Wolf-Rayet stars gamma^2 Vel (WR 11) in Vel OB2and EZ CMa (WR 6) in Col 121, and the classical Cepheid delta Cep in CepOB6. Membership probabilities are given for all selected stars. MonteCarlo simulations are used to estimate the expected number of interloperfield stars. In the nearest associations, notably in Sco OB2, thelater-type members include T Tauri objects and other stars in the finalpre-main-sequence phase. This provides a firm link between the classicalhigh-mass stellar content and ongoing low-mass star formation. Detailedstudies of these 12 groups, and their relation to the surroundinginterstellar medium, will be presented elsewhere. Astrometric evidencefor moving groups in the fields of R CrA, CMa OB1, Mon OB1, Ori OB1, CamOB1, Cep OB3, Cep OB4, Cyg OB4, Cyg OB7, and Sct OB2, is inconclusive.OB associations do exist in many of these regions, but they are eitherat distances beyond ~500 pc where the Hipparcos parallaxes are oflimited use, or they have unfavorable kinematics, so that the groupproper motion does not distinguish it from the field stars in theGalactic disk. The mean distances of the well-established groups aresystematically smaller than the pre-Hipparcos photometric estimates.While part of this may be caused by the improved membership lists, arecalibration of the upper main sequence in the Hertzsprung-Russelldiagram may be called for. The mean motions display a systematicpattern, which is discussed in relation to the Gould Belt. Six of the 12detected moving groups do not appear in the classical list of nearby OBassociations. This is sometimes caused by the absence of O stars, but inother cases a previously known open cluster turns out to be (part of) anextended OB association. The number of unbound young stellar groups inthe solar neighborhood may be significantly larger than thoughtpreviously.
| Catalogue of H-alpha emission stars in the Northern Milky Way
The ``Catalogue of Stars in the Northern Milky Way Having H-alpha inEmission" appears in Abhandlungen aus der Hamburger Sternwarte, Band XIin the year 1997. It contains 4174 stars, range {32degr <= l() II< 214degr , -10degr < b() II < +10degr } having the Hαline in emission. HBH stars and stars of further 99 lists taken from theliterature till the end of 1994 were included in the catalogue. We givethe cross-identification of stars from all lists used. The catalogue isalso available in the Centre de Données, Strasbourg ftp130.79.128.5 or http://cdsweb.u-strasbg.fr and at the HamburgObservatory via internet.
| Emission-Line Stars in the Vilnius Photometric System
Various types of emission-line stars, observed in the Vilniusphotometric system, are analyzed. They include Be-type stars, HerbigAe/Be stars, T Tauri-type stars and K- and M-type dwarfs with activechromospheres. It is shown that all stars of these types, except forlate-type dwarfs, in their active stages can be identified by theirinterstellar reddening-free parameters. For emission-line stars of B andA types interstellar reddening determination is also possible.
| Photoelectric Photometry of Herbig Ae/be and Related Stars in the Vilnius Photometric System
A catalog of photoelectric photometry of 62 Herbig Ae/Be and relatedstars in the Vilnius system is presented. It contains stars down to V =12 mag located mainly in the northern hemisphere and observed in theperiod of 1994--1996.
| Classification and Identification of IRAS Sources with Low-Resolution Spectra
IRAS low-resolution spectra were extracted for 11,224 IRAS sources.These spectra were classified into astrophysical classes, based on thepresence of emission and absorption features and on the shape of thecontinuum. Counterparts of these IRAS sources in existing optical andinfrared catalogs are identified, and their optical spectral types arelisted if they are known. The correlations between thephotospheric/optical and circumstellar/infrared classification arediscussed.
| Catalogue of stars in the northern Milky Way having H-alpha in emission
Not Available
| Eclipsing binaries as IRAS sources.
In a systematic search we looked for coincidences in the positions ofeclipsing binaries and IRAS point sources as evidence of a physicalassociation. In a detailed discussion of the available optical andinfrared data combined with model calculations, we show that 50-75% ofthe coincidences between eclipsing binaries and IRAS sources are real.We discuss a subsample of 44 stars in some detail and surveyed thevicinity of them on POSS and SRC/ESO atlases for possible opticalcounterparts and present identification maps. In the cases of BS Sco andV 718 Sco the infrared radiation may come from an accretion disk.
| A search for precursors of ultracompact HII regions in a sample of luminous IRAS sources. I. Association with ammonia cores.
We present observations of NH_3_ (1,1) and (2,2) lines in twoflux-limited samples of IRAS sources selected according to colourcriteria which should result in a high fraction of Young StellarObjects. The first sample contains sources (named 'Low') whoseevolutionary status is essentially unknown, while the second samplecontains sources (named 'High') possibly associated with ultracompactHII regions, the distinction being based on the IRAS [25-12] colour.Indications from a previous study of H_2_O maser emission suggest thatthe sources in the first group may be in an evolutionary phase prior tothe appearance of an HII region, thus being among the youngest knownhigh-mass forming objects. Low sources were detected in ammonia with alower rate than High sources (45% and 80% respectively); the onlydifference between the two groups is in the linewidths: the (1,1) linesare generally narrower than (2,2) lines in High sources (FWHMs medianvalues are 1.81km/s and 2.00km/s respectively), while the opposite istrue in Low sources (FWHMs median values are 1.72km/s and 1.33km/s forthe (1,1) and (2,2) lines respectively). We propose that the Low groupconsists of two distinct populations of evolutionary different objects,based on the (non-) association with ammonia emission. The Low sourcesshowing ammonia emission are characterized by more quiescent envelopesthan those surrounding High sources, and the relationships betweenrelevant physical quantities derived from our observations and the IRAScolours suggest that High sources, contrary to Low, may harbour objectswhich dominate the physical and dynamical properties of the clump, thuspossibly implying the relative youth of this subgroup of the Lowsources.
| 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 Initial Mass Function and Massive Star Evolution in the OB Associations of the Northern Milky Way
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...454..151M&db_key=AST
| IRAS LRS Spectra of the Sharpless H II Regions
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJS..100..389C&db_key=AST
| Infrared study of the HII region - molecular cloud complex S 142.
Not Available
| A new catalogue of members and candidate members of the Herbig Ae/Be (HAEBE) stellar group
A new up-to-date catalogue of Herbig Ae/Be (HAEBE) stars and relatedobjects is certainly needed, for both well-seasoned researchers and, inparticular, for new investigators starting to study the many interestingastrophysical properties of these very young objects. We present a briefdiscussion of the current observational characteristics that distinguishthis class from their main sequence counterparts. The HAEBE and relatedstars are listed in five tables, containing 287 objects. Table 1contains all Ae and Be stars which historically are recognized as trueHAEBE stars or potential candidate members. Table 2 gives the stars ofspectral type Fe, and emission line stars with very uncertain or unknownspectral type. In Table 3 are given all known Extreme Emission LineObjects (EELOs), of which most have not been identified to belong to anyspecific group. Table 4a and b list other Bep or B[e] stars with strongIR-excess and unknown spectral type. Table 5 contains the non-emissionline possible young objects. Furthermore, Table 6 contains 35 starsrejected from former published lists of HAEBE stars. In these tables weare including coordinates, spectral types, visual magnitudes, ranges inphotometric variability and references of several key publicationsrelated to each object. Relevant remarks, such as the presence of anebula in the vicinity of an object, are also given.
| Hα Interferometric Optical and Near Infrared Photometric Studies of Star Forming Regions - Part Two - the NGC7380E / SH:2-142 / NGC7380 Complex
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1994A&A...283..963C&db_key=AST
| Predicting the Secondary Minima Depths and Spectra of the Main Components for the Dm-Type Eclipsing Variable Stars
Not Available
| IRAS sources beyond the solar circle. III - Observations of H2O, OH, CH3OH and CO
We have used the 100-m Effelsberg and 32-m Medicina radiotelescopes tosearch for H2O maser emission (22.235 GHz) towards 1143 IRAS sources,for OH (1665/67 MHz) towards 303 IRAS sources, and for CH3OH (12.179GHz) towards 19 IRAS sources. The IRAS sources have been selected tohave colors of premain sequence objects. To obtain an estimate of thekinematic distance, we observed (C-12)O (J = 2 to 1) and (C-12)O (J = 3to 2) with the KOSMA 3-m telescope towards 25 sources showing H2Oemission and not yet observed in CO. This paper presents theobservational results in form of tables with line parameters or upperlimits and spectra of detected sources.
| Systematic variations in the wavelength dependence of interstellar linear polarization
New observations of the wavelength dependence of interstellar linearpolarization, p(lambda), which were performed to investigate theinfluence of the environment on the effective size distribution of thealigned polarizing particles, are presented. Optical and IR measurementswere obtained simultaneously in eight photometric passbands between Uand K, giving a coherent data set for a total of 105 reddened stars. Thecontention that variations of K and lambda-max are correlated isconfirmed, and the empirical linear relationship between K andlambda-max found by Wilking et al. (1980, 1982, 1983) is revised to K +0.01 +/-0.05 + (1.66 +/-0.09)lambda-max. There is some cosmic scatter ofthe data about this line. The same linear dependence of K on l-max seenoverall provides a consistent representation of the systematicpolarization in changes within individual regions with rather differingenvironments. It is argued that the grain size distribution in denseregions is modified by coagulation which removes the smaller particleswithout major modification of the larger ones.
| Early-type emission-line stars with large infrared excesses
A catalog is presented of early-type emission-line stars obtained bycross-identification between Wackerling's catalog and the IRAS catalogof point sources. A study of the distribution in space of the starsshows that these stars belong to the extreme Population I; thus thepresent compilation provides a rather complete sample for further studyof the evolution of pre- and post-main sequence stars of medium and highmasses.
| Water masers associated with dense molecular clouds and ultracompact H II regions
Results are reported from a study surveying the occurrence of the H2O22GHz maser emission from bright IR sources in star-forming regions. Asample of 260 sources was selected from the IRAS Point Source Catalog,following the color selection criteria suggested by Richards et al.(1987), to identify dense molecular clouds where star formation might beat the earliest stages. Water vapor emission toward 32 sources wasdetected. Twelve new maser sources were found, all characterized byrather low integrated fluxes and narrow components. On the basis of FIRcolor indices and the maser detection rates, and from a comparison withother classes of objects, it is suggested that the sources included inthe sample not associated with ultracompact H II regions contain a highfraction of candidate molecular clouds with embedded high massprotostars still in the accretion phase.
| IRAS sources beyond the solar circle. I - CO observations
C-12O (J = 1-0) has been observed with the 15-m SEST and the 30-m IRAMtelescope in the direction of 1302 IRAS sources with colors of starforming regions located within 10 deg of the galactic plane in theinterval between 85 and 280 deg. Emission components with line profilesthat are non-Gaussian (showing, e.g., possible self-absorption or wings)are identified; this information may serve as a basis for selectingsources for future research. For all components, kinematic heliocentricand galactocentric distances, and distances from the galactic plane arederived. For those components which may be associated with the IRASsources, bolometric luminosities are derived. These data will beanalyzed and compared with HI data in subsequent papers.
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Dades d'Observació i Astrometria
| Constel·lació: | Cepheus |
| Ascensió Recta: | 22h47m49.56s |
| Declinació: | +58°08'49.6" |
| Magnitud Aparent: | 10.149 |
| Moviment propi RA: | -8.9 |
| Moviment propi Dec: | 3.8 |
| B-T magnitude: | 10.623 |
| V-T magnitude: | 10.189 |
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