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L' and M' standard stars for the Mauna Kea Observatories Near-Infrared system
We present L' and M' photometry, obtained at the United Kingdom InfraredTelescope (UKIRT) using the Mauna Kea Observatories Near-Infrared(MKO-NIR) filter set, for 46 and 31 standard stars, respectively. The L'standards include 25 from the in-house `UKIRT Bright Standards' withmagnitudes deriving from Elias et al. and observations at the InfraredTelescope Facility in the early 1980s, and 21 fainter stars. The M'magnitudes derive from the results of Sinton and Tittemore. We estimatethe average external error to be 0.015 mag for the bright L' standardsand 0.025 mag for the fainter L' standards, and 0.026 mag for the M'standards. The new results provide a network of homogeneously observedstandards, and establish reference stars for the MKO system, in thesebands. They also extend the available standards to magnitudes whichshould be faint enough to be accessible for observations with moderndetectors on large and very large telescopes.
| JHK Standard Stars on the CIT Photometric System
We present a set of 58 stars with JHK standard values on the CIT systemand with a suitable magnitude range for use with array detectors onsmall- to moderate-size telescopes. Each final value is based on six to47 measures (with a mean of 17) obtained on separate nights with the USNaval Observatory (USNO) NICMOS3 (HgCdTe) camera. The objects include 20primary CIT standards from Elias et al. and 38 secondary sourcesselected from the SAAO and UKIRT standards lists, cover a K-magnituderange between 6.0 and 10.8, and lie north of declination -20°. Thestars were reduced to the CIT system as defined by Elias et al.,producing a USNO system that is identical to the near-infrared CITsystem. This work densifies the original CIT system by nearly a factorof 3 and extends its range by about 3 mag. The SAAO and UKIRT standardsare also compared with the CIT system.
| Near-Infrared Photometric Survey of Proto-planetary Nebula Candidates
We present JHK' photometric measurements of 78 objects mostly consistingof proto-planetary nebula candidates. Photometric magnitudes aredetermined by means of imaging and aperture photometry. Unlike theobservations with a photometer with a fixed-sized beam, the method ofimaging photometry permits accurate derivation of photometric values,because the target sources can be correctly identified and confusionwith neighboring sources can be easily avoided. Of the 78 sourcesobserved, we report nearly 10 cases in which the source seems to havebeen misidentified or confused by nearby bright sources. We also presentnearly two dozen cases in which the source seems to have indicated avariability that prompts a follow-up monitoring. There are also a fewsources that show previously unreported extendedness. In addition, wepresent H-band finding charts of the target sources.
| A Multi-Band Photometric Study of Tidal Debris in a Compact Group of Galaxies: Seyfert's Sextet
In order to investigate the properties of the prominent tidal debrisfeature extending to the northeast of a compact group of galaxies,Seyfert's Sextet, we analyzed multi-band (U, B, V, VR, R, I, J, H, andK') photometric imaging data and obtained the following results: 1) Theradial surface brightness distribution of this tidal debris in Seyfert'sSextet (TDSS) in each band appears to be well approximated by anexponential profile. 2) The observed B-V color of TDSS is similar tothose of dwarf elliptical galaxies in nearby clusters. 3) Comparing thespectral energy distribution (SED) of TDSS with theoretical photometricevolution models and with the SED of the stars in the outer part of HCG79b, we find that its SED is comparable to that of a ~10Gyr-old stellarpopulation with solar metallicity, similar to the stellar population inthe outer part of HCG 79b. This suggests that TDSS consists of starsthat may have been liberated from HCG 79b by strong ga laxyinteractions, not a pre-existing dwarf galaxy as previously thought.
| 5 Micron Photometry of Late-Type Dwarfs
We present narrowband M photometry of nine low-mass dwarfs with spectraltypes ranging from M2.5 to L0.5. Combining the (L'-M') colors derivedfrom our observations with data from the literature, we find colorsconsistent with a Rayleigh-Jeans flux distribution for spectral typesearlier than M5, but enhanced F3.8/F4.7 fluxratios (negative [L'-M'] colors) at later spectral types. This probablyreflects increased absorption at M' due to the CO fundamental band. Wecompare our results against recent model predictions and briefly discussthe implications.
| The Orbit of the Brown Dwarf Binary Gliese 569B
We present photometric, astrometric, and spectroscopic observations ofthe nearby (9.8 pc) low-mass binary Gl 569Bab (in turn being a companionto the early-M star Gl 569A) made with the Keck adaptive opticsfacility. Having observed Gl 569Bab since 1999 August, we are able tosee orbital motion and to determine the orbital parameters of the pair.We find the orbital period to be 892+/-25 days, the semimajor axis to be0.90+/-0.02 AU, the eccentricity to be 0.32+/-0.02, and the inclinationof the system to be 34deg+/-3deg (1 σ). Thetotal mass is found to be 0.123+0.027-0.022Msolar (3 σ). In addition, we have obtainedlow-resolution (R=1500-1700) near-infrared spectra of each of thecomponents in the J and K bands. We determine the spectral types of theobjects to be M8.5 V (Gl 569Ba) and M9 V (Gl 569Bb) with an uncertaintyof half a subclass. We also present new J- and K-band photometry thatallows us to place the objects in the H-R diagram accurately. Mostlikely the binary system is comprised of two brown dwarfs with a massratio of 0.89 and with an age of approximately 300 Myr.
| Red Quasars and Quasar Evolution: The Case of BAL QSO FIRST J155633.8+351758
We present the first near-infrared spectroscopic observations of theradio-loud broad absorption line quasi-stellar object (QSO), FIRSTJ155633.8+351758. The spectrum is similar to that of a reddened QSO andshows strong emission lines of Hα and Hβ, as well as strongFe II emission blends near Hβ. The redshift of the object, measuredfrom the Hα and Hβ lines, is zBLR=1.5008+/-0.0007,slightly larger than the redshift of zmetal=1.48, estimatedfrom the broad metal absorption features. Thus, the broad metalabsorption features are blue shifted with respect to the systemicvelocity. The width of the Hα emission line (FWHM~4100 km s-1) is typical of that observed in QSO broad-line regions, but theBalmer decrement (Hα/Hβ~5.8) is larger than that of mostoptically selected QSOs. Both the Balmer decrement and the slope of therest-frame UV-optical continuum independently suggest a modest amount ofextinction along the line of sight to the broad-line region(EB-V~0.5 for SMC-type screen extinction at the redshift ofthe QSO). The implied gas column density along the line of sight is muchless than that implied by the weak X-ray flux of the object, suggestingthat either the broad emission and absorption line regions have a lowdust-to-gas ratio or that the rest-frame optical light encounterssignificantly lower mean column density lines of sight than the X-rayemission. From the rest-frame UV-optical spectrum, we are able toconstrain the stellar mass content of the system(<3×1011 Msolar). Comparing this masslimit with the black hole mass estimated from the bolometric luminosityof the QSO, we find it possible that the ratio of the black hole tostellar mass is comparable to the Magorrian value, which would implythat the Magorrian relation is already in place at z=1.5. However,multiple factors favor a much larger black hole-to-stellar mass ratio.This would imply that if the Magorrian relation characterizes the latehistory of QSOs and if the situation observed for F1556+3517 is typicalof the early evolutionary history of QSOs, central black hole massesdevelop more rapidly than bulge masses. Based on observations at theKitt Peak National Observatory.
| Do galaxy mergers form elliptical galaxies? A comparison of kinematic and photometric properties
We present near-infrared K-band imaging and spectroscopy of a sample ofgalaxy mergers, which we use to derive light profile indices, absolutemagnitudes and central velocity dispersions. We find that the lightdistributions of mergers more nearly resemble those of ellipticals thanthose of bulges, but that the mergers lie well away from the FundamentalPlane defined by the ellipticals. We interpret this as being due toenhancement of the K-band surface brightness of the mergers by asignificant population of supergiant stars, and independent evidence forsuch a population is inferred from measurements of the depth of the2.3-μm CO absorption feature.
| A complete sample of radio sources in the North Ecliptic Cap, selected at 38MHz - III. Further imaging observations and the photometric properties of the sample
Further imaging observations of a sample of radio sources in the NorthEcliptic Cap are presented and a number of new identifications are made.Using redshifts from spectroscopic data presented in a companion paperby Lacy et al., the photometric properties of the galaxies in the sampleare discussed. It is shown that: (1) out to at least z~0.6 radiogalaxies are good standard candles irrespective of radio luminosity; (2)for 0.6<~z<~1 a large fraction of the sample has magnitudes andcolours consistent with a non-evolving giant elliptical, and (3) athigher redshifts, where the R-band samples the rest-frame UV flux, mostobjects have less UV luminosity than expected if they form their stellarpopulations at a constant rate from a high redshift to z~1 in unobscuredstar-forming regions (assuming an Einstein-de Sitter cosmology). Theconsequences of these observations are briefly discussed.
| New Near-Infrared Spectroscopy of the High-Redshift Quasar B1422+231 at Z = 3.62
We present new near-infrared (rest-frame UV-to-optical) spectra of thehigh-redshift, gravitationally lensed quasar B1422+231 (z=3.62).Diagnostic emission lines of Fe II, O III lambda5007, and Hβ,commonly used to determine the excitation, ionization, and chemicalabundances of radio-quiet and radio-loud quasars, were detected. Our newdata show that the ratio Fe II (UV)/Hβ=18.1+/-4.6 and Fe II(optical)/Hβ=2.3+/-0.6 are higher than those reported by Kawara etal. by factors of 1.6 and 3.3, respectively, although the ratio [O III]lambda5007/Hβ=0.19+/-0.02 is nearly the same between the twomeasurements. The discrepancy of the line flux ratios between themeasurements is likely due to improved data and fitting proceduresrather that to intrinsic variability. While approximately half of thehigh-z quasars observed to date have much more extreme Fe II(optical)/Hβ ratios, the line ratio measured for B1422+231 areconsistent with the observed range of Fe II (optical) ratios of low-zquasars.
| Towards a fundamental calibration of stellar parameters of A, F, G, K dwarfs and giants
I report on the implementation of the empirical surface brightnesstechnique using the near-infrared Johnson broadband { (V-K)} colour assuitable sampling observable aimed at providing accurate effectivetemperatures of 537 dwarfs and giants of A-F-G-K spectral-type selectedfor a flux calibration of the Infrared Space Observatory (ISO). Thesurface brightness-colour correlation is carefully calibrated using aset of high-precision angular diameters measured by moderninterferometry techniques. The stellar sizes predicted by thiscorrelation are then combined with the bolometric flux measurementsavailable for a subset of 327 ISO standard stars in order to determineone-dimensional { (T, V-K)} temperature scales of dwarfs and giants. Theresulting very tight relationships show an intrinsic scatter induced byobservational photometry and bolometric flux measurements well below thetarget accuracy of +/- 1 % required for temperature determinations ofthe ISO standards. Major improvements related to the actual directcalibration are the high-precision broadband { K} magnitudes obtainedfor this purpose and the use of Hipparcos parallaxes for dereddeningphotometric data. The temperature scale of F-G-K dwarfs shows thesmallest random errors closely consistent with those affecting theobservational photometry alone, indicating a negligible contributionfrom the component due to the bolometric flux measurements despite thewide range in metallicity for these stars. A more detailed analysisusing a subset of selected dwarfs with large metallicity gradientsstrongly supports the actual bolometric fluxes as being practicallyunaffected by the metallicity of field stars, in contrast with recentresults claiming somewhat significant effects. The temperature scale ofF-G-K giants is affected by random errors much larger than those ofdwarfs, indicating that most of the relevant component of the scattercomes from the bolometric flux measurements. Since the giants have smallmetallicities, only gravity effects become likely responsible for theincreased level of scatter. The empirical stellar temperatures withsmall model-dependent corrections are compared with the semiempiricaldata by the Infrared Flux Method (IRFM) using the large sample of 327comparison stars. One major achievement is that all empirical andsemiempirical temperature estimates of F-G-K giants and dwarfs are foundto be closely consistent between each other to within +/- 1 %. However,there is also evidence for somewhat significant differential effects.These include an average systematic shift of (2.33 +/- 0.13) % affectingthe A-type stars, the semiempirical estimates being too low by thisamount, and an additional component of scatter as significant as +/- 1 %affecting all the comparison stars. The systematic effect confirms theresults from other investigations and indicates that previousdiscrepancies in applying the IRFM to A-type stars are not yet removedby using new LTE line-blanketed model atmospheres along with the updatedabsolute flux calibration, whereas the additional random component isfound to disappear in a broadband version of the IRFM using an infraredreference flux derived from wide rather than narrow band photometricdata. Table 1 and 2 are only available in the electronic form of thispaper
| Near-Infrared Spectroscopy of the High-Redshift Quasar S4 0636+68 at Z = 3.2
We present near-infrared (observed frame) spectra of the high-redshiftquasar S4 0636+68 at z = 3.2, which was previously thought to be one ofa group of ``strong'' Fe ii emitters [i.e., F(Fe iilambdalambda4434-4684)/F(Hβ) > 1]. Our K-band spectrum clearlyshows emission lines of Hβ and [O iii] lambdalambda4959, 5007, aswell as optical Fe ii emission. Our computed value of F(Fe iilambdalambda4434-4684)/F(Hβ) ~= 0.8 for S4 0636+68 is less thanpreviously thought and, in fact, is comparable to values found forradio-loud, flat-spectrum, low-z quasars. Therefore S4 0636+68 appearsnot to be a strong optical Fe ii emitter. Although more than half (5/8)of the high-z quasars observed to date are still classified as strongoptical Fe ii emitters, their Fe ii/Hβ ratios, for the most part,follow the same trend as do those of low-z quasars, i.e., ananticorrelation in EW(Fe ii)/EW(Hβ) versus EW([O iii])/EW(Hβ),with radio-loud quasars having a mean value of EW(Fe ii)/EW(Hβ)approximately half that of radio-quiet quasars at comparable values ofEW([O iii])/EW(Hβ).
| Young red supergiants and the near-infrared light appearance of disk galaxies
We have searched for spatial variations in the 2.3 m photometric COindex within the disks of three nearby galaxies. This index measures thestrength of the absorption bands of molecular CO in stellar atmospheresand is strong in cool, low surface gravity stars, reaching the largestvalues for red supergiants. We observe significant spatial CO indexvariations in two galaxies, indicating that the dominant stellarpopulation in the NIR is not everywhere the same. Central CO index peaksare present in two galaxies; these could be due to either metallicitygradients or to recent star formation activity. In addition, significantazimuthal CO index variations are observed in one. Because strongazimuthal metallicity gradients are physically implausible in diskgalaxies, these features are most naturally explained by the presence ofa young stellar population. The fraction of 2 m light due to youngstellar populations in star-forming regions can be calculated from ourdata. Overall, young stellar populations can contribute 3 percent of theNIR flux of a (normal) galaxy, which is consistent with other globalproperties. Locally, this fraction may rise to 33 percent. Thus, youngstars do not dominate the total NIR flux, but can be locally dominant instar-forming regions, and can bias estimates of spiral arm amplitude orother nonaxisymmetric structures in galaxies' mass distributions.
| The near-infrared extinction law and limits on the pre-main-sequence population of the Rho Ophiuchi dark cloud
We describe new techniques to measure the NIR extinction law and toplace limits on the premain-sequence stellar population of a dark cloud.We analyze JHK imaging data for the central 1 sq deg of the Rho Ophiuchicloud core and show that nearly all stars projected onto regions of lowCS intensity, ICS 10 K km/s, are background stars. Most sources atlarger CS intensities lie within cloud material. We use the backgroundstars to derive the slope of the NIR extinction law, E(J-H)/E(H-K) =1.57 +/- 0.03. This result is consistent with previous extinction lawsbut has a factor of two to three smaller uncertainty. The new Rho Ophextinction law yields strong constraints on the number of previouslyundiscovered premain-sequence stars in the cloud, 46 +/- 11, and thenumber of previously undiscovered young stars with near-IR excesses, 15+/- 4. Neither limit exceeds the number of known premain-sequence starsin the cloud about 100. Thus, current samples of premain-sequence starsare reasonably complete for K = 14 or less.
| Cygnus X-3 in outburst: quenched radio emission, radiation losses and variable local opacity
We present multiwavelength observations of Cygnus X-3 during an extendedoutburst in 1994 February-March. Intensive radio monitoring at 13.3, 3.6and 2.0cm is complemented by observations at (sub)millimetre andinfrared wavelengths, which find Cyg X-3 to be unusually bright andvariable, and include the first reported detection of the source at 0.45mm. We report the first confirmation of quenched radio emission prior toradio flaring independently of observations at Green Bank. Theobservations reveal evidence for wavelength-dependent radiation lossesand gradually decreasing opacity in the environment of the radio jet. Wefind that the radiation losses are likely to be predominantly inverseCompton losses experienced by the radio-emitting electrons in the strongradiation field of a luminous companion to the compact object. Weinterpret the decreasing opacity during the flare sequence as resultingfrom a decreasing proportion of thermal electrons entrained in the jet,reflecting a decreasing density in the region of jet formation. Wepresent, drawing in part on the work of other authors, a model basedupon mass transfer rate instability predicting gamma-ray, X-ray,infrared and radio trends during a radio flaring sequence.
| IRAS FSC 15307+3252: Gravitationally Lensed Seyfert or Cannibal Elliptical at Z = 0.93?
We present the highest spatial and spectral resolution near-infrareddata to date of the ~10^13^ h^-2^ L_sun_ IRAS source FSC 15307 + 3252 atz = 0.93, apparently the most luminous galaxy in the known universe.Deep H-band (2.2 micron) images taken in 0.4" seeing at the W. M. KeckTelescope reveal three components: (A) a bright elliptical source with acompact nucleus, (B) a resolved circular companion separated fromcomponent A by 2.0" (8 h^-1^ kpc for q_0_ = 0.5), and (C) a faintirregular component 1.7" from A. The surface brightness profile ofF15307-A is well characterized by a de Vaucouleurs r^1/4^ law with r_e_= 1.4" +/- 0.2" (6 h^-1^ kpc), a size comparable to local giantellipticals. The nucleus of component A is stellar in appearance withextended structure, possibly a second nucleus ~0.5" away. Our 1.1-1.4micron spectrum of the F15307 system with a resolution of 330 km s^-1^shows strong emission lines of [O I] λλ6300, 6364; blendedHα + [N II] λλ6548,6583; and [S II]λλ6716,6731. The ~900 km s^-1^ width of the forbiddenlines and the relative strengths of the emission lines arecharacteristic of Seyfert 2 galaxies. The Hα line also has a broad(1900 km s^-1^) component. In light of the recent discovery that FSC10214+4724, previously the most luminous known galaxy, is agravitationally lensed system, we explore the possibility that F15307 isalso lensed. Quantitative arguments are inconclusive, but aspects ofF15307's morphology do suggest lensing; the system bears a strongresemblance to quadruple-image gravitational lenses. On the other hand,given the r^1/4^ profile, the close companions, and the active nucleus,F15307 may in fact be a giant elliptical galaxy caught in the act ofgalactic cannibalism, a scenario that could also account for itsunparalleled luminosity.
| A study of 4C 13.66 - the final identification and redshift for the revised 3C sample
We use new optical and near-infrared data to identify the radio source4C 13.66 with a K=18.2 galaxy at z=1.45, and use new radio images tostudy its relatively unusual radio structure. Prior to this work 4C13.66 was the only radio source out of 173 in the revised 3C sample ofLaing, Riley & Longair without a spectroscopic redshift. We discussthe vital role of near-infrared spectroscopy in securing the finalredshift for this sample.
| UvbyHbeta_ photometry of main sequence A type stars.
We present Stroemgren uvby and Hbeta_ photometry for a set of575 northern main sequence A type stars, most of them belonging to theHipparcos Input Catalogue, with V from 5mag to 10mag and with knownradial velocities. These observations enlarge the catalogue we began tocompile some years ago to more than 1500 stars. Our catalogue includeskinematic and astrophysical data for each star. Our future goal is toperform an accurate analysis of the kinematical behaviour of these starsin the solar neighbourhood.
| 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.
| M Giant Kinematics in Off-Axis Fields between 150 and 300 Parsecs from the Galactic Center
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...449..623B&db_key=AST
| The Nuclear Energy Sources Powering Bright Infrared-selected Galaxies
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...447..545A&db_key=AST
| Near Infrared Imaging of Dwarf Ellipticals Irregulars and Blue Compact Galaxies in the Virgo Cluster
New near-IR images are presented for 13 dwarf galaxies in the Virgocluster. Together with previous data these provide a data base of JHKimaging for 26 dwarf ellipticals (dEs), dwarf irregulars (dIs) and bluecompact dwarfs (BCDs). These images show the dIs to be highly asymmetricand unrelaxed, implying that they are dynamically young and unevolved.This is consistent with their blue near-IR and optical-IR colours whichare most easily explained by young stellar populations. The dEs aresymmetrical and apparently relaxed, with very uniform colours indicatingthat they are dominated by old stars. They generally have exponentiallight profiles, but the brighter galaxies tend to exhibit more cuspedlight distributions, similar to the de Vaucouleurs profiles of brightellipticals. The BCDs have moderately asymmetric light profiles, andparadoxically red colours, possibly indicating an intermediate-agestellar population. They are probably dEs which have undergone bursts ofstar formation in the last few X 10^9^ years, whilst the dIs are afundamentally distinct population. Colour gradients are present in manyof the galaxies, invariably in the sense that the nuclei are redder thanthe surrounding galaxy light.
| Deep Infrared Array Photometry of Globular Clusters. I. M4
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1994ApJ...423..640D&db_key=AST
| A filter for deep near-infrared imaging
The K passband (central wavelength 2.2 microns, FWHM 0.4 micron) is thelongest wavelength standard near-IR passband through which deepground-based imaging is possible. Thermal emission from telescope,instrument, and sky limits the depth to which such imaging can reach byproducing strongly temperature-dependent backgrounds in the range11-13.5 mag/sq arcsec. This paper describes how a passband, which isdenoted as K-prime, located slightly shortward of the standard Kpassband (central wavelength 2.1 microns), yet still within the sameatmospheric window, leads to a significantly lower thermal component ofthe background, reducing the background surface brightness by up to 0.9mag sq arcsec, and thereby allowing deeper imaging to be obtained in thesame integration time. The photometric differences between the K-primefilter and the standard K filter are discussed.
| Color evolution in high-redshift galaxies
The Simultaneous Photometer for Infrared and Visual Light has been usedto observe 40 radio- and 39 optically-selected giant elliptical galaxiesof known redshift in the 0.019-1.6 range. There is no indication in theresults obtained of differences between the colors of radio and nonradiogalaxies, with the exception of H-K in the z=0.2-0.4 range; the H-Kcolor is best fitted by a passively evolving model with little residualstar formation. Some galaxies exhibit strong blueward deviations. Thisbehavior is most easily explained by star formation episodes involvingsmall fractions of the total number of stars.
| Infrared standard stars
The results of an observational program aimed at setting up a network offaint near-infrared standards of sufficient accuracy are reported. Thenetwork covers both northern and southern hemispheres and includesstandards red enough to provide at least a limited check on colortransformations. The standards are set up at J (1.2 micron), H (1.6micron), K (2.2 microns), and L (3.5 microns), and their H2O and COmolecular absorption indices are determined. The problem of colortransformations between observatories is discussed briefly. Allmagnitudes presented are transformed to the natural system defined bythe CIT observations.
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Datos observacionales y astrométricos
| Constelación: | Serpiente |
| Ascensión Recta: | 15h21m34.53s |
| Declinación: | +24°20'36.1" |
| Magnitud Aparente: | 7.249 |
| Distancia: | 132.45 parsecs |
| Movimiento Propio en Ascensión Recta: | -36.2 |
| Movimiento Propio en Declinación: | -9.4 |
| B-T magnitude: | 7.299 |
| V-T magnitude: | 7.254 |
Catálogos y designaciones:
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