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|Research Note Hipparcos photometry: The least variable stars|
The data known as the Hipparcos Photometry obtained with the Hipparcossatellite have been investigated to find those stars which are leastvariable. Such stars are excellent candidates to serve as standards forphotometric systems. Their spectral types suggest in which parts of theHR diagrams stars are most constant. In some cases these values stronglyindicate that previous ground based studies claiming photometricvariability are incorrect or that the level of stellar activity haschanged. Table 2 is only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/367/297
|Sixth Catalogue of Fundamental Stars (FK6). Part III. Additional fundamental stars with direct solutions|
The FK6 is a suitable combination of the results of the HIPPARCOSastrometry satellite with ground-based data, measured over a longinterval of time and summarized mainly in the FK5. Part III of the FK6(abbreviated FK6(III)) contains additional fundamental stars with directsolutions. Such direct solutions are appropriate for single stars or forobjects which can be treated like single stars. Part III of the FK6contains in total 3272 stars. Their ground-based data stem from thebright extension of the FK5 (735 stars), from the catalogue of remainingSup stars (RSup, 732 stars), and from the faint extension of the FK5(1805 stars). From the 3272 stars in Part III, we have selected 1928objects as "astrometrically excellent stars", since their instantaneousproper motions and their mean (time-averaged) ones do not differsignificantly. Hence most of the astrometrically excellent stars arewell-behaving "single-star candidates" with good astrometric data. Thesestars are most suited for high-precision astrometry. On the other hand,354 of the stars in Part III are Δμ binaries in the sense ofWielen et al. (1999). Many of them are newly discovered probablebinaries with no other hitherto known indication of binarity. The FK6gives, besides the classical "single-star mode" solutions (SI mode),other solutions which take into account the fact that hidden astrometricbinaries among "apparently single-stars" introduce sizable "cosmicerrors" into the quasi-instantaneously measured HIPPARCOS proper motionsand positions. The FK6 gives, in addition to the SI mode, the "long-termprediction (LTP) mode" and the "short-term prediction (STP) mode". TheseLTP and STP modes are on average the most precise solutions forapparently single stars, depending on the epoch difference with respectto the HIPPARCOS epoch of about 1991. The typical mean error of anFK6(III) proper motion in the single-star mode is 0.59 mas/year. This isa factor of 1.34 better than the typical HIPPARCOS errors for thesestars of 0.79 mas/year. In the long-term prediction mode, in whichcosmic errors are taken into account, the FK6(III) proper motions have atypical mean error of 0.93 mas/year, which is by a factor of about 2better than the corresponding error for the HIPPARCOS values of 1.83mas/year (cosmic errors included).
|FAUST observations in the Fourth Galactic Quadrant*|
We analyse UV observations with FAUST of four sky fields in the generaldirection of the Fourth Galactic Quadrant, in which we detect 777 UVsources. This is ~50 per cent more than detected originally by Bowyer etal. We discuss the source detection process and the identification of UVsources with optical counterparts. For the first time in this project weuse ground-based objective-prism information for two of the fields, toselect the best-matching optical objects with which to identify the UVsources. Using this, and correlations with existing catalogues, wepresent reliable identifications for ~75 per cent of the sources. Mostof the remaining sources have assigned optical counterparts but, lackingadditional information, we offer only plausible identifications. Wediscuss the types of objects found, and compare the observed populationwith predictions of our UV Galaxy model.
|A catalog of far-ultraviolet point sources detected with the fast FAUST Telescope on ATLAS-1|
We list the photometric measurements of point sources made by the FarUltraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 spaceshuttle mission. The list contains 4698 Galactic and extragalacticobjects detected in 22 wide-field images of the sky. At the locationssurveyed, this catalog reaches a limiting magnitude approximately afactor of 10 fainter than the previous UV all-sky survey, TDl. Thecatalog limit is approximately 1 x 10-14 ergs A sq cm/s,although it is not complete to this level. We list for each object theposition, FUV flux, the error in flux, and where possible anidentification from catalogs of nearby stars and galaxies. Thesecatalogs include the Michigan HD (MHD) and HD, SAO, the HIPPARCOS InputCatalog, the Position and Proper Motion Catalog, the TD1 Catalog, theMcCook and Sion Catalog of white dwarfs, and the RC3 Catalog ofGalaxies. We identify 2239 FAUST sources with objects in the stellarcatalogs and 172 with galaxies in the RC3 catalog. We estimate thenumber of sources with incorrect identifications to be less than 2%.
|The fate of the solid matter orbiting HR 4796A|
We have obtained optical spectra, 2 micrometers speckle images, and anupper limit to the 800 micrometers flux for HR 4796A, and opticalspectra for its physical companion separated by 7.7 arcsecs, HR 4796B.We detect H-beta, H-gamma, and the calcium H and K lines in emissionfrom HR 4796B; these data are consistent with the hypothesis that it islater than spectral type M2 and lies substantially above themain-sequence. From the location of HR 4796B on the H-R diagram, theestimated age of this star is 3 x 106 yr, and assuming thisage for the entire system, we find from our 2 micrometers speckle datathat there is no close stellar companion to HR 4796A (M greater than0.125 solar mass) between 11 and 120 AU from the star. From the IRAS andground-based photometry, it seems that there is a hole in the dustdistribution around HR 4796A with an inner radius of betweenapproximately 40 and approximately 200 AU. The observed circumstellardust grains, which lie at D greater than 40 AU from the star, are likelyto be at least 3 micrometers in radius in order to be gravitationallybound to HR 4796A, if the circumstellar dust cloud is optically thin.Since they are larger than almost all interstellar grains, thecircumstellar dust grains probably grew by coalescence. Because theexisting grains at D greater than 40 AU have undergone measurablecoalescence, it is possible that particles that presumably once existedat D less than 40 AU, where the collision times were shorter than at Dgreater than 40 AU, grew into macroscopic objects. A likely explanationfor the dust hole is that there is a companion located at about half theinner radius of the dust hole, or between 20 and 100 AU from the star.If such a companion exists, it must have a mass less than 0.125 solarmass. Since grain coalescence has occurred, this putative companionpossibly could be a planet.
|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 position corrections of 1400 stars observed with PA II in San Juan.|
|Improved Mean Positions and Proper Motions for the 995 FK4 Sup Stars not Included in the FK5 Extension|
|The late A-type stars - Refined MK classification, confrontation with Stromgren photometry, and the effects of rotation|
The MK spectral classification for late A-type stars is refined and theeffects of rotation of spectral classification and uvby(beta) photometryfor these stars are examined. It is found that, for A3 stars, the4417/4481 A wavelength ratio produces results that are inconsistent withthe Stark broadening of the H lines. It is suggested that this ratio isnot useful as a luminosity criterion at any spectral type.Self-consistent sequences of narrow- and broadline standards areestablished. The results of the refined classification system arecompared with Stromgren photometry, showing a set of low-v sin i A-typestars with anomalously large delta(c1) indices for theirluminosity types. It is proposed that these stars are rapid rotatorsseen at fairly low inclination angles.
|Starbursts, binary stars, and blue stragglers in local superclusters and groups. I - The very young disk and young disk populations|
The distributions in the HR diagram with theoretical time-constant locifor stars in several young clusters and superclusters are compared todemonstrate that 'blue stragglers' in these aggregates are mostfrequently simply single massive (mode B) stars formed in bursts of starformation that occur at discrete intervals in time following theformation of the bulk of the low-mass (mode A) stars in the aggregate.The characteristics of the close binary systems in these aggregates areexamined to show that, in several cases, mass transfer by Roche lobeoverflow has or will occur and that, in some instances, the system wouldhave appeared as a blue straggler prior to the mass-transfer event, and,in other instances, mass transfer will lead to the identification of thesystem as a blue straggler. Thus, it is concluded that the bluestraggler phenomenon has at least two distinct physical origins: it mayoriginate from delayed formation (starbursts) or from 'delayedevolution' in some close binaries (mass transfer from an evolvedprimary).
|Experiments with CP stars|
A method for fine-classification of stars is applied to a sample ofabout 100 stars within the approximate spectral type range B6-A5.Experiments have been performed to find a method for fine-classificationof A stars, both normal and chemically peculiar, within the MK system.It is found that, independent of the definition of the degree ofpeculiarity, no sharp border exists separating the CP stars from thenormal ones. It is also shown that spectral classification can, onaverage, be performed with almost the same accuracy for CP stars as forthe normal ones if cases of extreme peculiarity are avoided.
|Metallicism among A and F giant stars|
132 stars considered as A and F giants have been studied for theirproperties in the Geneva photometric system. It is shown that thissystem to derive the temperature, absolute magnitude and Fe/H value forstars in this part of the HR diagram. 36 percent of the stars of oursample exhibit an enhanced value Delta m2 that can be interpreted interms of Fe/H. The red limit of stars having an enhanced Fe/H value is0.225 in B2-V1 or 6500 K in Teff. This corresponds to the limit definedby Vauclair and Vauclair (1982) where the diffusion timescale is equalto the stellar lifetime and permits the assumption that the diffusion isthe process responsible for the metallicism observed in the A and Fgiants.
|First Stellar Catalog in Rio-Grande|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1985RMxAA..10..377M&db_key=AST
|A systematic search for members of the Hyades Supercluster. IV - The metallic-line stars and ultrashort-period Cepheids|
Bright Star Catalog stars with beta values in the 2.70-2.88 rangecontain 127 members of the Hyades Supercluster, which have been chosenon the basis of the direction of their proper motion. Available radialvelocities confirm supercluster membership for most of these stars.Exceptional regularity is noted in the values of the pulsation constantQ computed for the ultrashort period Cepheids on the basis of knownperiods, model masses and model radii. Outside the center of the Hyadescluster, the largest concentration of supercluster stars is in a regionof 30 pc radius, between 60 and 80 pc above the sun, where 30 percent ofthe expected stars in the temperature range presently discussed aresupercluster members.
|A Note about the Comparison Between the Old and New Slettebak Systems of Axial Rotational Velocities|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1984RMxAA...9....9G&db_key=AST
|The first astrolabe catalogue at Valinhos|
Individual corrections to the ascensions and declinations of 199 starsof the FK4 and FK4 Supplement, derived from the Danjon astrolabeobservations at Valinhos and covering the zone from +5 to -51 deg ofdeclination, are presented. The chain method of differences was used tomake the corrections. The observational station formulas used to obtainthe catalogue are cited and discussed and the systematic errors for thezone of the catalogue are given. The results are compared with those ofthe General Catalogue of Astrolabes.
|First astrolabe catalogue of Rio de Janeiro|
A catalogue of right ascensions and declinations of FK4 and FK4Supplement stars, obtained from astrolabe observations at Rio deJaneiro, is presented. The quantity and accuracy of the observations,the systematic errors of the catalogue, the group corrections, and theascension and declination corrections are considered.
|A photometric study of southern AP stars having right ascensions on the order of 12 HR|
The color variability periods of some southern Ap stars were determinedfrom uvby measurements. Observations were made of 25 Sex, HR 4327, betaHya, HD 112381, HR 4965, HR 5158, HR 5269, and HD 125630. Data wereinsufficient for determinations of the periods of the stars HR 4109(which may not vary), l Cen, and the v and y variations of HD 125630.The occurrences of short duration dips in the color variation curves ofseveral of the objects are discussed.
|Properties of Am, Delta Del and Delta SCT stars in the VBLUW system|
The spread with respect to the main sequence in the two-color diagramsfor 115 Am, Delta Del and Delta Sct, for which VBLUW photometricobservations have been obtained, is primarily attributed to gravityeffects. Exceptions to this rule can be recognized from a comparison oftheir positions in these diagrams and in the reddening-independentdiagram L-U/B-L, where some Delta Sct stars have experienced relativelyhigh reddenings, while others are presumably metal-poor. It is notedthat gravities and temperatures compare satisfactorily with those ofDavis Philip et al. (1976), which were based on uvby-beta photometry.
|Spectral Classification and DDO Photometry of a Southern Group of Stars with Common Motions - Part One|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1982PASP...94..304L&db_key=AST
|Observational stability in AM stars|
Differential photoelectric photometry is carried out in metallic-linestars suspected of variability and in the pulsating Am: star HR 8210.The pulsational stability of classical Am stars is confirmed and thehypothesis that the Am phenomenon is the result of diffuse elementseparation is still consistent with the observations. The variability ofHR 8210 is confirmed too. The behavior of this star should beinterpreted as evidence of a multiple-period structure.
|Properties of AM stars in the Geneva photometric system|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1980A&A....92..289H&db_key=AST
|UBVRI photometry of 225 AM stars|
UBVRI photometry of 225 Am stars taken from Mendoza's (1974) catalog ispresented. The results are compared with those obtained by Feinstein(1974) for 21 of the stars and with the values of Johnson et al. (1966).It is assumed that in the first approximation the (V-I) color index ofan unreddened Am star is equal to that of a normal main-sequence star; astandard main sequence is defined for A and early F stars, and thefive-color photometry is analyzed by means of plots of U-V vs. V-I, B-Vvs. V-I, and V-R vs. V-I. Mean color deficiencies of Am stars areexamined, and it is suggested that an unreddened star located below themain-sequence A0-F2 line in the (V-I, U-V) plane is a photometric Amstar. It is concluded that: (1) photometric Am stars have colordeficiencies (as a function of V-I) which, on the average, are 0.07 magin (U-V) color index and 0.025 mag in (B-V) color index; (2) Am starswith V-R less than 0.25 mag may also have a color deficiency of about0.01 mag; (3) Am stars with V-R greater than 0.3 mag may have a colorexcess of approximately 0.01 mag; and (4) Am stars with V-R between 0.25and 0.3 mag may have normal colors.
|Absolute luminosity calibration of Stroemgren's 'late group'|
A statistical parallax method based on the principle of maximumlikelihood is used to calibrate absolute luminosities for samples ofcooler stars constituting the 'late group' defined by Stromgren (1966).The samples examined include 415 stars of all luminosity classes and asubset comprising 86 main-sequence stars. Linear calibration relationsinvolving the Stromgren beta, (b-y), and bracketted c1 indices arederived which yield mean absolute magnitudes with an accuracy of 0.09magnitude for the overall sample and 0.13 magnitude for themain-sequence subsample. Several second-order relations are considered,and the results are compared with Crawford's (1975) calibrations as wellas with mean absolute magnitudes obtained from trigonometric parallaxes.The possible effect of interstellar absorption on the calibrationrelations is also investigated.
|Bright metallic-line and pulsating A stars.|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1976PASP...88..402E&db_key=AST
|Results of stellar ultraviolet photometry aboard the Cosmos 215 satellite|
The paper discusses ultraviolet photometry of 36 A and B stars performedon board the Cosmos 215 satellite with parallel telescopes and two UVphotometers with maximum responses at 2740 and 2275 A, respectively. Thestars were identified by means of a magnetometer and two photometersthat detected stellar fluxes in bands near the B and V bands of the UBVsystem. Monochromatic fluxes at wavelengths of 2740 and 2275 A aredetermined for the 36 stars, and the results for 15 of them are comparedwith previous measurements at or near the same wavelengths. The previousdata for nine stars are found to be in satisfactory agreement with thepresent measurements within their error limits, but the results for sixstars differ from OAO 2 data. Two-color (U2740 - V) - (B - V) and (U2275- V) - B-V) diagrams are plotted and shown not to contradict apreviously determined relation between standard color indices.
|Multicolor photometry of metallic-line stars. III. A photometric catalogue|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974RMxAA...1..175M&db_key=AST
|Southern peculiar stars with abnormal spectra|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973A&AS...12...79B&db_key=AST
|Catalogue of AM stars with known spectral types|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973A&AS...10..385H&db_key=AST
|Rotational Velocities and Spectral Types of Some A-Type Stars|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972PASP...84..584L&db_key=AST
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|Proper motion RA:||-107.6|
|Proper motion Dec:||1.1|
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