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Beryllium Abundances in F and G Dwarfs in the Pleiades and α Persei Clusters from Keck High-Resolution Echelle Spectrometer Observations
While there are many observations of Li in open clusters, there are veryfew of the companion light element Be. As we have seen in the study ofBe in the Hyades by Boesgaard & King, the two elements togetherprovide important and unique information on the extent and nature ofinterior mixing in solar-like stars. We have obtained high-resolution(45,000) spectra of the Be II resonance lines in the 14 Pleiades andfour α Per dwarfs of spectral types F and G with the Keck Itelescope and High-Resolution Echelle Spectrometer. The signal-to-noiseratio in the Be spectral region is typically 40 pixel-1.These two clusters have similar ages and have solar metallicity.Abundances of Be were determined by spectrum synthesis using the newestversion of MOOG. For the F dwarfs where there is only a weak Li dip,there is no indication of a Be dip as was found in the Hyades inassociation with its deep Li dip. Thus, the observed light elementdepletion in the F dwarfs in the Hyades and in field stars is occurringduring main-sequence evolution, and Be depletion does not become evidentuntil ages of more than 100 Myr. The Pleiades G dwarfs are apparentlyundepleted in Be and the mean value for logN(Be/H)+12.00 in stars coolerthan 6000 K is 1.26+/-0.10, compared to the Hyades mean of 1.31+/-0.07.The star-to-star dispersion in Be in the Pleiades is comparable to thequoted errors. The four α Per stars have lower Be abundances thanthe Pleiades with a mean of 1.02 dex. The differences in these twoclusters in their Li and Be abundances relative to the Hyades is thoughtto be due to their younger age and possibly their lower metallicity.
| Lithium abundances from the 6104 Å line in cool Pleiades stars
Lithium abundances determined by spectral synthesis from both the 6708Å resonance line and the 6104 Å subordinate line arereported for 11 Pleiades late-G and early-K stars observed at theWilliam Herschel Telescope. Firm detections of the weak subordinate lineare found for four objects, marginal detections for four, and upperlimits for the remaining three stars. Some of these spectra werepreviously analysed by Russell (1996), where he reported that abundancesderived from the 6104 Å line were systematically higher than thoseobtained from the 6708 Å line by 0.2-0.7 dex. He also reported areduced spread in the 6104 Å line abundances compared with thosedetermined from the 6708 Å feature. Using spectral synthesis wehave re-analysed Russell's data, along with our own. Our results do notentirely support Russell's conclusions. We report a ~ 0.7 dex scatter inthe abundances from 6708 Å and a scatter at least as large fromthe 6104 Å line. We find that this is partly explained by ourinclusion of a nearby Fe Ii line and careful modelling of damping wingsin the strong metal lines close to the 6104 Å feature; neglect ofthese leads to overestimates of the Li abundance which are most severein those objects with the weakest 6104 Å lines, thus reducing theabundance scatter. We find a reasonable correlation between the 6104Å and 6708 Å Li abundances, although four stars have 6104Å-determined abundances which are significantly larger than the6708 Å-determined values by up to 0.5 dex, suggesting problemswith the homogeneous, 1-dimensional atmospheres being used. We show thatthese discrepancies can be explained, although probably not uniquely, bythe presence of star spots with plausible coverage fractions. Theaddition of spots does not significantly reduce the apparent scatter inLi abundances, leaving open the possibility that at least some of thespread is caused by real star-to-star differences in pre-main sequenceLi depletion.
| Search for X-ray flares in the Pleiades using SoHO LASCO C3 images.
Not Available
| Search for gamma Doradus variable stars in the Pleiades cluster
Photometric observations in the uvbybeta system of A-F type stars in thePleiades cluster have been performed in order to detect pulsatingvariable stars of gamma Doradus type in the lower part of the Cepheidinstability strip. In order to obtain more information about thebehaviour of the studied objects and to be able to distinguish betweenlong period variable and non-variable stars, two statistical methodshave been developed. Several of these stars show some type ofvariability but only two of the observed objects, H1284 and S29, can besafely classified as gamma Dor stars. Furthermore, these observationshave provided us with Strömgren and Hβ photometry,non-existing up to now for some of them, which permitted us to perform aphotometric study of the Pleiades cluster.
| Statistics of binaries in the Pleiades cluster
We present a statistical analysis of binaries in galactic clusters,based on photometric properties. Synthetic clusters are used to solvethe deconvolution problem. If the colour-magnitude relation for singlestars is given and if triple stars are treated as binaries, thedistribution of systems in a colour-magnitude diagram (CMD) can be usedto determine cluster properties. They include the maximum number ofsingle stars N1max which is compatible with the distributionof systems, a standard deviation sigma (describing the scatter of starson the main sequence), a critical mass ratio q_c, and the mass ratiodistribution in the case of N_1=N1max. In the general case(N_1<= N1max) the mass ratio distribution can bedetermined for q>q_c, and in favourable cases (if N_1 is sufficientlylarge) for all mass ratios. A first application concerns thePleiades cluster in the colour range 0.2<= B-V<0.98. The concentration of systems near the main sequence in the CMDis used to derive an approximation for the colour-magnitude relation. Asmall positive number c is involved as a parameter. The mass ratiodistribution depends sensitively on c and increases towards small massratios, at least up to q =~ 0.5 and probably up to q =~ 0.3. Thedistribution is bimodal, with a peak at q=1. Photometric arguments showthat c<~ 0.02. A binary frequency of 60-70% as expected from clustersimulations (Kroupa \cite{krou}) requires c<~ 0.03. An adjustment oftwo parameters (c=0.02 and a 70% binary frequency) is sufficient toreproduce the mass ratio distribution for binaries in the galacticfield. This suggests that the mass ratio distribution in the Pleiades issimilar to the distribution in the field, in accordance with aconjecture of Bouvier et al. (\cite{brn}, BRN).
| Deep ROSAT HRI observations of the Pleiades
In a deep X-ray survey of the Pleiades open cluster, we use the ROSATHigh Resolution Imager to explore a region of the cluster formerlysurveyed with the PSPC. These new observations substantially improveupon both the sensitivity and the spatial resolution for this region ofthe Pleiades, allowing us to detect 18 cluster members not detectedbefore and 16 members not included in the catalogs used in previoussurveys. The high sensitivity of the present observations permits us toobtain more stringent upper limits for 72 additional members and alsoprovides sufficient numbers of stars to enable us to explore thedependence of L_x on stellar rotation for the slow rotators of thePleiades. Using the new high sensitivity X-ray observations and therecent rotational measurements we discuss the activity-rotationrelationship in the Pleiades solar type stars. We also present newphotometric observations of optical counterparts of a number of X-raysources detected in previous surveys but not yet identified. Table~2 isavailable in electronic form at CDS via ftp 130.79.128.5
| The Pleiades and alpha Persei Clusters
The upper-main-sequence members of the Pleiades and alpha Perseiclusters, considered as members of the Local Association, yield meanparallaxes that are only 4% larger than the mean values from Hipparcosobservations. The (log T_eff, M_V) diagram reveals that in thetemperature range from 6000 to 8000 K, the Hyades and alpha Perseimain-sequence members are nearly identical and several tenths of amagnitude brighter than similar stars on the Pleiades main sequence. Thedeparture of the Pleiades main sequence cannot be traced to either ageor heavy-element abundance differences in the range thought to apply tothese clusters. A 50% increase in the helium abundance of Pleiades overHyades stars could account for the luminosity difference. Alternativeexplanations are that the Pleiades cluster is rejected from superclustermembership and/or that the Hipparcos parallax results for the Pleiadesare in error by some 10%.
| The rotational velocity of low-mass stars in the Pleiades cluster
We present new {vsin i} measurements for 235 low-mass stars in thePleiades. The differential rotational broadening has been resolved forall the stars in our sample. These results, combined with previouslypublished measurements, provide a complete and unbiased rotation dataset for stars in the mass range from 0.6 to 1.2{Msun}.Applying a numerical inversion technique on the {vsin i} distributions,we derive the distributions of equatorial velocities for low-massPleiades members. We find that half of the Pleiades dwarfs with a massbetween 0.6 to 1 {Msun} have rotation rates lower than 10{ kms(-1) }. Comparison of the rotational distributions of low-mass membersbetween IC 2602/2391 (~ 35 Myr) and the Pleiades (~ 100 Myr) suggeststhat G dwarfs behave like solid-bodies and follow Skumanich's law duringthis time span. However, comparison between Pleiades and older clusters-M34 (~ 200 Myr) and Hyades (~ 600 Myr)- indicates that the braking ofslow rotators on the early main sequence is weaker than predicted by anasymptotical Skumanich's law. This strongly supports the view thatangular momentum tapped in the radiative core of slow rotators on thezero age main sequence (ZAMS) resurfaces into the convective envelopebetween Pleiades and Hyades age. For the G-dwarfs, we derive acharacteristic coupling time scale between the core and the envelope ofabout 100-200 Myr, which accounts for the observed evolution of surfacerotation from the ZAMS to the Hyades. The relationship between rotationand coronal activity in the Pleiades is in agreement with previousobservations in other clusters and field stars. We show that the Rossbydiagram provides an excellent description of the X-ray activity for allstars in the mass domain studied. The Pleiades data for slow andmoderate rotators fills the gap between the X-ray-rotation correlationfound for slow rotators and the X-ray ``saturation plateau'' observedfor young fast rotators. The transition between increasing X-ray fluxwith rotation and X-ray saturation is observed at log (P/tau)=0.8+/-0.1. These results strengthen the hypothesis that the``saturation'' of the angular momentum loss process depends on thestellar mass. Based on observations collected at the Observatoire deHaute-Provence with ELODIE at the 193cm telescope and with CORAVEL atthe 1m-swiss telescope
| Investigation of the Pleiades cluster. IV. The radial structure
On the basis of the best available member list and duplicityinformation, we have studied the radial distribution of 270 stars andmultiple systems earlier than K0 in the Pleiades. Five new long periodspectroscopic binaries have been identified from the CORAVELobservations. We have found a clear mass segregation between binariesand single stars, which is explained by the greater average mass of themultiple systems. The mass function of the single stars and primariesappears to be significantly different. While the central part of thecluster is spherical, the outer part is clearly elliptical, with anellipticity of 0.17. The various parameters describing the Pleiades are(for a distance of 125 pc): core radius rc = 0fdg6 (1.4 pc),tidal radius rt = 7fdg4 (16 pc), half mass radius r_{m/2} =0fdg88 (1.9 pc), harmonic radius /line{r} = 1fdg82 (4 pc). Low-massstars (later than K0) probably extend further out and new proper motionand radial velocity surveys over a larger area and to fainter magnitudeswould be very important to improve the description of the clusterstructure and complete mass function. Based on observations collected atthe Haute-Provence Observatory (France). Table~3 is available only 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 catalogue of [Fe/H] determinations: 1996 edition
A fifth Edition of the Catalogue of [Fe/H] determinations is presentedherewith. It contains 5946 determinations for 3247 stars, including 751stars in 84 associations, clusters or galaxies. The literature iscomplete up to December 1995. The 700 bibliographical referencescorrespond to [Fe/H] determinations obtained from high resolutionspectroscopic observations and detailed analyses, most of them carriedout with the help of model-atmospheres. The Catalogue is made up ofthree formatted files: File 1: field stars, File 2: stars in galacticassociations and clusters, and stars in SMC, LMC, M33, File 3: numberedlist of bibliographical references The three files are only available inelectronic form at the Centre de Donnees Stellaires in Strasbourg, viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5), or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| ROSAT Observations of the Pleiades. I. X-Ray Characteristics of a Coeval Stellar Population
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJS..102...75M&db_key=AST
| High-precision positions and proper motions of 441 stars in the Pleiades astrometric standard region.
Not Available
| Membership probabilities in the Pleiades field.
A catalogue of proper motions and photographic B, V magnitudes for starsup to B=19mag within a region centered near Alcyone is presented. Thecatalogue is based on MAMA measurements of 8 plates taken with theTautenburg Schmidt telescope. The survey includes ca. 14500 stars andcovers a total field of about 9 square degrees. For stars brighter thanB=18mag an internal accuracy of 0.05mag and 2.5mas/year has beenestimated for photometric data and proper motions, respectively.Membership probabilities, proper motions and B, V magnitudes are listedfor 442 stars up to B=19mag in the Pleiades field.
| The integrated spectra of M32 and of 47 Tuc: A comparative study at high spectral resolution
Integrated spectra have been obtained for the elliptical galaxy M32 andfor the 'metal-rich' Galactic globular cluster 47 Tuc. The spectra coverthe wavelength interval lambda lambda 3800-4400 A at a resolution of 2.5A full width at half maximum (FWHM) and S/N ratio of approximately100:1. Similar data have been acquired for a library of 191 individualstars, and, to support the 47 Tuc observations, integrated spectra offour additional metal-rich Galactic globular clusters have beenobtained. These observations are used to compare in detail theintegrated spectra of M32 (the most extensively studied ellipticalgalaxy) and 47 Tuc (the best-studied metal-rich Galactic globularcluster). Although M32 and 47 Tuc have similar optical broadband colorsand overall spectral types, when viewed at 2.5 A resolution spectranumerous subtle differences between their integrated are clearlyvisible. A system of 13 spectral indices, many of them originallydefined in Rose (1984), has been used to quantify these differences.Altogether twelve diagnostic diagrams are presented to illustrate themanner in which the integrated spectrum of M32 differs from that of 47Tuc. These diagrams are used to place several strong constraints on thestellar populations in these two systems.
| The evolution of the lithium abundances of solar-type stars. III - The Pleiades
New measurements of lithium in more than 100 Pleiades F, G, and K dwarfsare reported. Abundances are determined from spectrum synthesis fits tothe data as well as from use of new covers of growth from the Li 6708-Afeature. It is argued that most Late-F and early-G dwarfs in thePleiades are consistent with the tight N(Li) vs mass relation seen inthe Hyades in the same mass range. Most Li-rich stars have abundances ator near the primordial level for Population I, and none exceed thatlevel by a significant amount. At any given color the stars that rotatefast have the most Li and have the strongest chromospheric activity.Ways in which an apparent spread in N(Li) could arise from anintrinsically tight n(Li)-mass relation are considered, and it isconcluded that the spread is probably real and is not an artifact ofline formation conditions or inhomogeneous atmospheres on the stars.
| Rotation and chromospheric emission among F, G, and K dwarfs of the Pleiades
High-resolution echelle spectra of more than 100 F, G, and K dwarfs inthe Pleiades are reported. Chromospheric activity in these stars ismeasured via comparisons of the profiles of H-alpha and the Ca II IRtriplet to chromospherically inactive field stars. Consistent dereddenedcolors are determined from the available photometry and temperatures arederived. Most G and K dwarfs in the Pleiades rotate slowly, but about 20percent of the stars are ultrafast rotators (UFRs). That fraction ofUFRs is independent of color, and the highest rotation rates are foundamong the K dwarfs. The Pleiades exhibit a broad range in the strengthof chromospheric emission at any one color. Most G and K dwarfs in thePleiades show H-alpha and the IR triple in absorption, with filling inof the line cores.
| Investigation of the Pleiades cluster. II - Binary stars in the F5-K0 spectral region
Coravel observations of 100 F5-K0 stars in the Pleiades cluster yielded13 spectroscopic binary stars, and 11 orbits were determined. All 11periods are shorter than 1000 days and the longest circular period is7.05 days. One single-lined spectroscopic binary belongs to a triplesystem, the orbital motion of which has been detected. Based on acomplete sample in the color range B-V = 0.40 - 0.90, (88 stars), thepercentage of spectroscopic binaries with P less than 1000 days is 13percent. The number of single:binary:triple stars is 56:30:2.
| A catalogue of Fe/H determinations - 1991 edition
A revised version of the catalog of Fe/H determinations published by G.Cayrel et al. (1985) is presented. The catalog contains 3252 Fe/Hdeterminations for 1676 stars. The literature is complete up to December1990. The catalog includes only Fe/H determinations obtained from highresolution spectroscopic observations based on detailed spectroscopicanalyses, most of them carried out with model atmospheres. The catalogcontains a good number of Fe/H determinations for stars from open andglobular clusters and for some supergiants in the Magellanic Clouds.
| CA II H and K measurements made at Mount Wilson Observatory, 1966-1983
Summaries are presented of the photoelectric measurements of stellar CaII H and K line intensity made at Mount Wilson Observatory during theyears 1966-1983. These results are derived from 65,263 individualobservations of 1296 stars. For each star, for each observing season,the maximum, minimum, mean, and variation of the instrumental H and Kindex 'S' are given, as well as a measurement of the accuracy ofobservation. A total of 3110 seasonal summaries are reported. Factorswhich affect the ability to detect stellar activity variations andaccurately measure their amplitudes, such as the accuracy of the H and Kmeasurements and scattered light contamination, are discussed. Relationsare given which facilitate intercomparison of 'S' values with residualintensities derived from ordinary spectrophotometry, and for convertingmeasurements to absolute fluxes.
| Lithium, age, and metallicity in open clusters
It is shown that a strong relationship exists between Li abundance andage for stars in the temperature region 5950-6350 K. The relation isderived from mean Li abundances in eight open clusters ranging in agefrom 5 x 10 to the 7th to 8 x 10 to the 9th yr. The Li declinesexponentially with t exp(-0.3). It is suggested that, in thistemperature regime, simple microscopic diffusion is the cause of the Lidepletion. It is possible that there is a metallicity term in therelation, such that higher metallicity clusters with deeper convectionzones have less Li depletion, while lower metallicity cluster undergogreater depletion. This is consistent with expectations from diffusiontheory. Furthermore, the halo stars, with even lower metallicity andshallower convection zones, would have more diffusion and more Lidepletion; this is in agreement with recent theoretical work.
| Chemical composition of open clusters. I - Fe/H from high-resolution spectroscopy
Using high-resolution spectroscopy, the abundance ratios Fe/H, C/H, andC/Fe were determined for F dwarfs in the Alpha Per, the Pleiades, andthe Hyades clusters; the UMa, Hyades, and Wolf 630 moving groups; and aselection of bright F field dwarfs. The age span of these objects rangesfrom 5 x 10 to the 7th to 2 x 10 to the 9th yr. No evidence was found ofa trend in Fe/H with age for these clusters and groups, but there wereclear differences in Fe/H among these groups, indicating intrinsicdifferences in the metal content of the local gas out of which thesegroups were formed. No evidence was found for a trend of C/H with age ofthese stellar groups, but there were cluster-to-cluster variations,implying differences in the content of carbon in the precluster gas. TheC/H cluster differences followed the same pattern as the Fe/H clusterdifferences and yield C/Fe values which are constant, and equal to thesolar value, in all the groups.
| X-ray studies of coeval star samples. II - The Pleiades cluster as observed with the Einstein Observatory
Coronal X-ray emission of the Pleiades stars is investigated, andmaximum likelihood, integral X-ray luminosity functions are computed forPleiades members in selected color-index ranges. A detailed search isconducted for long-term variability in the X-ray emission of those starsobserved more than once. An overall comparison of the survey resultswith those of previous surveys confirms the ubiquity of X-ray emissionin the Pleiades cluster stars and its higher rate of emission withrespect to older stars. It is found that the X-ray emission from dA andearly dF stars cannot be proven to be dissimilar to that of Hyades andfield stars of the same spectral type. The Pleiades cluster members showa real rise of the X-ray luminosity from dA stars to early dF stars.X-ray emission for the young, solarlike Pleiades stars is about twoorders of magnitude more intense than for the nearby solarlike stars.
| Chemical abundances and ages of open clusters
The metal content of nine open clusters is discussed with the help ofresults from detailed spectral analyses of main-sequence and slightlyevolved stars, belonging to those clusters. This small sample ofclusters, out of about 1200 known, has, however, the advantage ofrepresenting the whole span of ages of open clusters with two young(Alpha Per, the Pleiades, with five intermediate age, including U Ma,Hyades, Coma, Praesepe, and NGC 752) and with two old (M 67 and NGC 188)clusters. It has also the advantage that the observations of almost allthe stars in these different clusters have been carried out on similar,when not identical telescopes, on similar high-resolution spectrographs,and similar detectors. The high signal/noise spectra of these clusterstars have been reduced with similar procedures, and interpreted withsimilar model atmosphere analyses. In taking into account the error barsattributed to the mean metal content parameter, Fe/H, of each cluster,one may conclude that only the Hyades cluster has a metal content whichdiffers significantly from that of the sun, being between 30 and 40percent higher than that of the sun.
| Metallicity in galactic clusters from high signal-to-noise spectroscopy
High-quality spectroscopic data on selected F dwarfs in six Galacticclusters are used to determine global (Fe/H) values for the clusters.For the two youngest clusters, Pleiades and Alpha Per, the (Fe/H) valuesare solar: 0.017 + or - 0.055. The Hyades and Praesepe are slightlymetal-enhanced at (Fe/H) = + 0.125 + or - 0.032, even though they are anorder of magnitude older than the Pleiades. Coma and the UMa Group atthe age of the Hyades are slightly metal-deficient with (Fe/H) = - 0.082+ or - 0.039. The lack of an age-metallicity relationship indicates thatthe enrichment and mixing in the Galactic disk have not been uniform ontime scales less than a billion years.
| Lithium in old open clusters - NGC 188
Echelle spectra which include the Li I line at 6707 A are reported forseven main-sequence stars and one subgiant in NGC 188. The Li I line isdetected in five of the six dwarfs which are highly probable clustermembers. The derived atmospheric Li/H ratios exceed the solar value byfactors ranging approximately from 10 to 40, although these apparentlyclosely solarlike stars are about twice as old as the sun. The variationof the lithium abundance with stellar mass along the main sequences ofthe Pleiades, the Hyades, NGC 752, and NGC 188 are compared. Theresulting evolutionary pattern indicates that the lithium fraction inthe Galactic gas has shown no appreciable change from Li/H of roughly 10to the -9th since the birth of NGC 188 about 10 Gyr ago, except that theabundance could have been higher by an uncertain but possiblyappreciable factor at the beginning of that epoch.
| Lithium in the Pleiades and Alpha Persei clusters
Observations of the Li region in the 23 F dwarfs of the Pleiades andAlpha Per clusters were performed with a TI CCD at the coudespectrographof the 200-inch telescope with a spectral resolution of 0.2 A and 2sigma signal-to-noise ratios of 100-300. All 21 of the stars observed inthe temperature region of 6100-7300 K show strong Li I lines with valuesof log N(Li) near 3.0; the mean is 2.98 + or - 0.13. The data suggestthat the significant decrease in surface Li, possibly caused bydiffusion or differential rotation, occurs for cluster stars between theages of 5 x 10 to the 7th to 5 x 10 to the 8th yr.
| Some Occultation Observations of the Pleiades at McDonald
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1988AJ.....95..117F&db_key=AST
| Determination of the Proper Motions for Stars in the Region of the Pleiades - Part One
Not Available
| The abundance of lithium in pleiades F stars
The abundance of lithium has been determined for 18 stars in thePleiades cluster with spectral types from A7V to G0V. The pronounced dipin the lithium abundance among the mid-F stars which has been reportedfor other, older star clusters is not present in the Pleiades. Theremoval of lithium from the surfaces of middle-F dwarfs therefore occursprincipally after about 100 Myr on the main sequence.
| The distribution of rotational velocities for low-mass stars in the Pleiades
The available spectral type and color data for late-type Pleiadesmembers have been reanalyzed, and new reddening estimates are obtained.New photometry for a small number of stars and a compilation of H-alphaequivalent widths for Pleiades dwarfs are presented. These data are usedto examine the location of the rapid rotators in color-magnitudediagrams and the correlation between chromospheric activity androtation. It is shown that the wide range of angular momenta exhibitedby Pleiades K and M dwarfs is not necessarily produced by a combinationof main-sequence spin-downs and a large age spread; it can also resultfrom a plausible spread in initial angular momenta, coupled with initialmain-sequence spin-down rates that are only weakly dependent onrotation. The new reddening estimates confirm Breger's (1985) finding oflarge extinctions confined to a small region in the southern portion ofthe Merope nebula.
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Наблюдательные данные и астрометрия
| Созвездие: | Телец |
| Прямое восхождение: | 03h43m58.80s |
| Склонение: | +23°52'57.9" |
| Видимая звёздная величина: | 9.707 |
| Собственное движение RA: | 20.6 |
| Собственное движение Dec: | -44.4 |
| B-T magnitude: | 10.378 |
| V-T magnitude: | 9.763 |
Каталоги и обозначения:
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