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Speckle observations with PISCO in Merate - I. Astrometric measurements of visual binaries in 2004
We present relative astrometric measurements of visual binaries madewith the Pupil Interferometry Speckle camera and Coronagraph (PISCO) atthe 1-m Zeiss telescope of Brera Astronomical Observatory, in Merate. Weprovide 135 new observations of 103 objects, with angular separations inthe range 0.1-4.0 arcsec and with an accuracy better than ~0.01 arcsec.Our sample is made of orbital couples as well as binaries whose motionis still uncertain. Our purpose is to improve the accuracy of the orbitsand constrain the masses of the components.This work already leads to the revision of the orbits of three systems(ADS 5447, 8035 and 8739).
| Observed Orbital Eccentricities
For 391 spectroscopic and visual binaries with known orbital elementsand having B0-F0 IV or V primaries, we collected the derivedeccentricities. As has been found by others, those binaries with periodsof a few days have been circularized. However, those with periods up toabout 1000 or more days show reduced eccentricities that asymptoticallyapproach a mean value of 0.5 for the longest periods. For those binarieswith periods greater than 1000 days their distribution of eccentricitiesis flat from 0 to nearly 1, indicating that in the formation of binariesthere is no preferential eccentricity. The binaries with intermediateperiods (10-100 days) lack highly eccentric orbits.
| Adaptive Optics Photometry and Astrometry of Binary Stars
We present astrometric and photometric measurements of 39 binary starsmade with the adaptive optics system on the 3.6 m AdvancedElectro-Optical System (AEOS) telescope, taken from 2002 November to2003 March. The binaries have separations ranging from 0.08" to 5.11"and differential magnitudes ranging from 0.096 to 7.9. Also, we includea list of observations of 23 known binaries that we were unable toresolve. In the process of these measurements, we discovered three newcompanions to two previously known binary stars. We also discuss theeffects of scintillation and anisoplanatism on measurements of binarystar photometry in adaptive optics images. Suggestions on how tominimize these effects are then given.Based on observations made at the Maui Space Surveillance Systemoperated by Detachment 15 of the US Air Force Research Laboratory'sDirected Energy Directorate.
| B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?
Projected rotational velocities (vsini) have been measured for 216 B0-B9stars in the rich, dense h and χ Persei double cluster and comparedwith the distribution of rotational velocities for a sample of fieldstars having comparable ages (t~12-15 Myr) and masses (M~4-15Msolar). For stars that are relatively little evolved fromtheir initial locations on the zero-age main sequence (ZAMS) (those withmasses M~4-5 Msolar), the mean vsini measured for the h andχ Per sample is slightly more than 2 times larger than the meandetermined for field stars of comparable mass, and the cluster and fieldvsini distributions differ with a high degree of significance. Forsomewhat more evolved stars with masses in the range 5-9Msolar, the mean vsini in h and χ Per is 1.5 times thatof the field; the vsini distributions differ as well, but with a lowerdegree of statistical significance. For stars that have evolvedsignificantly from the ZAMS and are approaching the hydrogen exhaustionphase (those with masses in the range 9-15 Msolar), thecluster and field star means and distributions are only slightlydifferent. We argue that both the higher rotation rates and the patternof rotation speeds as a function of mass that differentiatemain-sequence B stars in h and χ Per from their field analogs werelikely imprinted during the star formation process rather than a resultof angular momentum evolution over the 12-15 Myr cluster lifetime. Wespeculate that these differences may reflect the effects of the higheraccretion rates that theory suggests are characteristic of regions thatgive birth to dense clusters, namely, (1) higher initial rotationspeeds; (2) higher initial radii along the stellar birth line, resultingin greater spin-up between the birth line and the ZAMS; and (3) a morepronounced maximum in the birth line radius-mass relationship thatresults in differentially greater spin-up for stars that become mid- tolate-B stars on the ZAMS.
| Tidal Effects in Binaries of Various Periods
We found in the published literature the rotational velocities for 162B0-B9.5, 152 A0-A5, and 86 A6-F0 stars, all of luminosity classes V orIV, that are in spectroscopic or visual binaries with known orbitalelements. The data show that stars in binaries with periods of less thanabout 4 days have synchronized rotational and orbital motions. Stars inbinaries with periods of more than about 500 days have the samerotational velocities as single stars. However, the primaries inbinaries with periods of between 4 and 500 days have substantiallysmaller rotational velocities than single stars, implying that they havelost one-third to two-thirds of their angular momentum, presumablybecause of tidal interactions. The angular momentum losses increase withdecreasing binary separations or periods and increase with increasingage or decreasing mass.
| Kinematics of Hipparcos Visual Binaries. II. Stars with Ground-Based Orbital Solutions
This paper continues kinematical investigations of the Hipparcos visualbinaries with known orbits. A sample, consisting of 804 binary systemswith orbital elements determined from ground-based observations, isselected. The mean relative error of their parallaxes is about 12% andthe mean relative error of proper motions is about 4%. However, even 41%of the sample stars lack radial velocity measurements. The computedGalactic velocity components and other kinematical parameters are usedto divide the stars with known radial velocities into kinematical agegroups. The majority (92%) of binaries from the sample are thin diskstars, 7.6% have thick disk kinematics and only two binaries have halokinematics. Among them, the long-period variable Mira Ceti has a verydiscordant {Hipparcos} and ground-based parallax values. From the wholesample, 60 stars are ascribed to the thick disk and halo population.There is an urgent need to increase the number of the identified halobinaries with known orbits and substantially improve the situation withradial velocity data for stars with known orbits.
| Rotational Velocities of B Stars
We measured the projected rotational velocities of 1092 northern B starslisted in the Bright Star Catalogue (BSC) and calibrated them againstthe 1975 Slettebak et al. system. We found that the published values ofB dwarfs in the BSC average 27% higher than those standards. Only 0.3%of the stars have rotational velocities in excess of two-thirds of thebreakup velocities, and the mean velocity is only 25% of breakup,implying that impending breakup is not a significant factor in reducingrotational velocities. For the B8-B9.5 III-V stars the bimodaldistribution in V can be explained by a set of slowly rotating Ap starsand a set of rapidly rotating normal stars. For the B0-B5 III-V starsthat include very few peculiar stars, the distributions in V are notbimodal. Are the low rotational velocities of B stars due to theoccurrence of frequent low-mass companions, planets, or disks? Therotational velocities of giants originating from late B dwarfs areconsistent with their conservation of angular momentum in shells.However, we are puzzled by why the giants that originate from the earlyB dwarfs, despite having 3 times greater radii, have nearly the samerotational velocities. We find that all B-type primaries in binarieswith periods less than 2.4 days have synchronized rotational and orbitalmotions; those with periods between 2.4 and 5.0 days are rotating withina factor 2 of synchronization or are ``nearly synchronized.'' Thecorresponding period ranges for A-type stars are 4.9 and 10.5 days, ortwice as large. We found that the rotational velocities of the primariesare synchronized earlier than their orbits are circularized. The maximumorbital period for circularized B binaries is 1.5 days and for Abinaries is 2.5 days. For stars of various ages from 107.5 to1010.2 yr the maximum circularized periods are a smoothexponential function of age.
| A revised HRD for individual components of binary systems from BaSeL BVRI synthetic photometry. Influence of interstellar extinction and stellar rotation
Johnson BVRI photometric data for individual components of binarysystems have been provided by ten Brummelaar et al. (\cite{Brummelaar}).This is essential because non-interacting binaries can be considered astwo single stars and therefore play a critical role in testing andcalibrating single-star stellar evolution sets of isochrones and theimplicit theory. While they derived the effective temperature (T_eff)from their estimated spectral type, we infer metallicity-dependent T_efffrom a minimizing method fitting the B-V, V-R and V-I colours. For thispurpose, a grid of 621 600 flux distributions were computed from theBasel Stellar Library (BaSeL 2.2) of model-atmosphere spectra, and theirtheoretical colours compared with the observed photometry. The BaSeLcolours show a very good agreement with the BVRI metallicity-dependentempirical calibrations of Alonso et al. (\cite{Alonso}), with thetemperatures being different by 3+/-3% in the range 4000-8000 K fordwarf stars. Before deriving the metallicity-dependent T_eff from theBaSeL models, we paid particular attention to the influence of reddeningand stellar rotation. We inferred the reddening from two differentmethods: (i) the MExcessNg code v1.1 (Méndez & van Altena\cite{Mendez}) and (ii) neutral hydrogen column density data. Acomparison of both methods shows a good agreement for the sample locatedinside a local sphere of ~ 500 pc, but we point out a few directionswhere the MExcess model overestimates the E(B-V) colour excess.Influence of stellar rotation on the BVRI colours can be neglectedexcept for 5 stars with large v sin i, the maximum effect on temperaturebeing less than 5%. Our final determinations provide effectivetemperature estimates for each component. They are in good agreementwith previous spectroscopic determinations available for a few primarycomponents, and with ten Brummelaar et al. below ~ 10 000 K.Nevertheless, we obtain an increasing disagreement with theirtemperatures beyond 10 000 K. Finally, we provide a revisedHertzsprung-Russell diagram (HRD) for the systems with the moreaccurately determined temperatures.
| Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
| 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 (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/367/297
| Michelson Interferometry with the Keck I Telescope
We report the first use of Michelson interferometry on the Keck Itelescope for diffraction-limited imaging in the near-infrared JHKLbands. By using an aperture mask located close to the f/25 secondary,the 10 m Keck primary mirror was transformed into a separate-element,multiple-aperture interferometer. This has allowed diffraction-limitedimaging of a large number of bright astrophysical targets, including thegeometrically complex dust envelopes around a number of evolved stars.The successful restoration of these images, with dynamic ranges inexcess of 200:1, highlights the significant capabilities of sparseaperture imaging as compared with more conventional filled-pupil speckleimaging for the class of bright targets considered here. In particular,the enhancement of the signal-to-noise ratio of the Fourier data,precipitated by the reduction in atmospheric noise, allows high-fidelityimaging of complex sources with small numbers of short-exposure imagesrelative to speckle. Multiepoch measurements confirm the reliability ofthis imaging technique, and our whole data set provides a powerfuldemonstration of the capabilities of aperture-masking methods whenutilized with the current generation of large-aperture telescopes. Therelationship between these new results and recent advances ininterferometry and adaptive optics is briefly discussed.
| ICCD Speckle Observations of Binary Stars. XXIII. Measurements during 1982-1997 from Six Telescopes, with 14 New Orbits
We present 2017 observations of 1286 binary stars, observed by means ofspeckle interferometry using six telescopes over a 15 year period from1982 April to 1997 June. These measurements constitute the 23dinstallment in CHARA's speckle program at 2 to 4 m class telescopes andinclude the second major collection of measurements from the MountWilson 100 inch (2.5 m) Hooker Telescope. Orbital elements are alsopresented for 14 systems, seven of which have had no previouslypublished orbital analyses.
| Binary Star Differential Photometry Using the Adaptive Optics System at Mount Wilson Observatory
We present photometric and astrometric results for 36 binary systemsobserved with the natural guide star adaptive optics system of the MountWilson Institute on the 100 inch (2.5 m) Hooker Telescope. Themeasurements consist of differential photometry in U, B, V, R, and Ifilters along with astrometry of the relative positions of systemcomponents. Magnitude differences were combined with absolute photometryfound in the literature of the combined light for systems to obtainapparent magnitudes for the individual components at standardbandpasses, which in turn led to color determinations and spectraltypes. The combination of these results with Hipparcos parallaxmeasurements yielded absolute magnitudes and allowed us to plot thecomponents on an H-R diagram. To further examine the reliability andself-consistency of these data, we also estimated system masses from thespectral types. Based on observations made at Mount Wilson Observatory,operated by the Mount Wilson Institute under an agreement with theCarnegie Institution of Washington.
| Two-colour photometry for 9473 components of close Hipparcos double and multiple stars
Using observations obtained with the Tycho instrument of the ESAHipparcos satellite, a two-colour photometry is produced for componentsof more than 7 000 Hipparcos double and multiple stars with angularseparations 0.1 to 2.5 arcsec. We publish 9473 components of 5173systems with separations above 0.3 arcsec. The majority of them did nothave Tycho photometry in the Hipparcos catalogue. The magnitudes arederived in the Tycho B_T and V_T passbands, similar to the Johnsonpassbands. Photometrically resolved components of the binaries withstatistically significant trigonometric parallaxes can be put on an HRdiagram, the majority of them for the first time. Based on observationsmade with the ESA Hipparcos satellite.
| Orbits of Five Visual Double Stars
This paper revises and discusses the orbits and other parameters of thedouble stars WDS 01497-1414, WDS 05413+1632, WDS 11136+5525, WDS20311+3333, and WDS 20494+1124.
| A Second Catalog of Orbiting Astronomical Observatory 2 Filter Photometry: Ultraviolet Photometry of 614 Stars
Ultraviolet photometry from the Wisconsin Experiment Package on theOrbiting Astronomical Observatory 2 (OAO 2) is presented for 614 stars.Previously unpublished magnitudes from 12 filter bandpasses withwavelengths ranging from 1330 to 4250 Å have been placed on thewhite dwarf model atmosphere absolute flux scale. The fluxes wereconverted to magnitudes using V=0 for F(V)=3.46x10^-9 ergs cm^-2 s^-1Å^-1, or m_lambda=-2.5logF_lambda-21.15. This second catalogeffectively doubles the amount of OAO 2 photometry available in theliterature and includes many objects too bright to be observed withmodern space observatories.
| Speckle Interferometry at the US Naval Observatory. III.
Position angles and separations resulting from 2578 speckleinterferometric observations of 590 binary stars are tabulated. This isthe third in a series of papers presenting measures obtained using the66 cm refractor at the US Naval Observatory in Washington, DC, andcovers the period from 1995 June through 1996 December. Program starsrange in separation from 0.2" to 4.3", with a limiting magnitude ofV=11. Random errors are estimated to be 17.0 mas in separation and0.56d/rho in position angle, where rho is the separation in arcseconds.These are the first results acquired using an improved intensified CCDdetector. The new detector, in concert with an intensity-filteringtechnique applied in software, has permitted a 1 mag increase in dynamicrange, to 3.5 mag, for pairs separated by about 2". The instrumentationand calibration are briefly described, with an emphasis on thecharacteristics of the new detector. The software filter used toincrease the dynamic range is also described.
| Diffraction-limited speckle masking interferometry of binary stars with the SAO 6-m telescope.
Not Available
| New orbits.
Not Available
| On the normal spectral energy distribution of stars: Spectral types O9-B5
The normal energy distributions for fifteen spectral subtypes from O9 toB5 for luminosity classes V, IV, and III are derived. Threephotometrically uniform catalogs served as the source of thespectrophotometric data used. Synthetic color indices for all spectraltypes are calculated using the energy distribution curves obtained.Comparison of these indices with the expected normal color indicessuggests that the energy distributions derived are reliable.
| ICCD Speckle Observations of Binary Stars. XVI. Measurements During 1982-1989 from the Perkins 1.8-M Telescope.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....114.1623F&db_key=AST
| UBV photometry of Be stars at Hvar: 1972--1990
A summary of results of the systematic UBV photoelectric monitoring ofbright northern Be stars carried out at the Hvar Observatory between1972 and 1990 is presented. Altogether, 76 Be stars of all luminosityclasses were observed and 13,848 UBV measurements secured.Simultaneously, 9,648 UBV measurements of 48 check stars (most of themof early spectral types) were obtained. A careful transformation of allobservations into the standard Johnson system allowed detection andmonitoring of even very mild long-term light and colour variations ofthese objects. Almost all early-type Be stars in the sample turned outto be variable. For several stars phase-locked light variations relatedto their binary nature were established. Sudden brightenings, on a timescale of a few days, were detected for o Cas and QR Vul. Tables 2 and 3are only available in electronic form at CDS via ftp tocdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html
| ICCD Speckle Observations of Binary Stars. XII. Measurements During 1984-1986 From the Perkins 1.8 M Telescope
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996AJ....111..393A&db_key=AST
| The ROSAT all-sky survey catalogue of optically bright OB-type stars.
For the detailed statistical analysis of the X-ray emission of hot starswe selected all stars of spectral type O and B listed in the Yale BrightStar Catalogue and searched for them in the ROSAT All-Sky Survey. Inthis paper we describe the selection and preparation of the data andpresent a compilation of the derived X-ray data for a complete sample ofbright OB stars.
| The photoelectric astrolabe catalogue of Yunnan Observatory (YPAC).
The positions of 53 FK5, 70 FK5 Extension and 486 GC stars are given forthe equator and equinox J2000.0 and for the mean observation epoch ofeach star. They are determined with the photoelectric astrolabe ofYunnan Observatory. The internal mean errors in right ascension anddeclination are +/- 0.046" and +/- 0.059", respectively. The meanobservation epoch is 1989.51.
| 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 determination of T_eff_ of B, A and F main sequence stars from the continuum between 3200 A and 3600 A.
A method of determination of the effective temperature of B, A and Fmain sequence stars is proposed, using the slope of the continuumbetween 3200A and 3600A. The effective temperature calibration is basedon a sample of stars with energy distributions known from UV to the red.We have determined the Balmer jump and the effective temperatures for235 main sequence stars. The temperatures found have been compared withthose derived by Underhill et al. (1979), Kontizas & Theodossiou(1980), Theodossiou (1985), Morossi & Malagnini (1985). Thecomparison showed good agreement for most of the stars in common. On theother hand, the temperatures derived from the reddening-free colourfactor QUV, from the colour index (m1965-V) and from (B-V), given inGulati et al. (1989), are systematically lower than our temperatures,however the differences are within one-sigma error.
| The Hα environment of T Tauri resolved by speckle interferometry.
T Tauri, the prototype of a class of low-mass pre-main sequence stars,was observed with the 3.6m Canada-France-Hawaii telescope (CFHT) and theCP40 photon-counting camera in November 1989. The data have beenanalysed using techniques of Speckle Interferometry to obtaindiffraction-limited information on the spatial extent of T Tauri innarrow passbands centered on the Hα line and the nearby redcontinuum. The object appears unresolved in the continuum passband,while it is resolved in Hα. The Hα emission is fitted with amodel consisting of two strongly flattened two-dimensional gaussians. Inthis model ~80% of the flux lies in a component (A) which is onlymarginally resolved, and ~20% lies in a component (B) with a semi-majoraxis FWHM of ~0.09". After subtraction of continuum, 2/3 of the Hαemission is spatially unresolved and 1/3 is resolved. The position angleof component B is 192deg+/-5deg, which approximates the direction of theperpendicular to the jet known in the [OI] and [SII] lines; this jetextends 30" westwards up to the Herbig-Haro object HH1555. Thecorresponding linear size of the Hα emitting region B is ~6 by15AU FWHM assuming a distance of T Tauri of d=140pc. We argue that thisemission arises either from the interaction between a weakly collimatedwind with a circumstellar flaring disc, or from the basis of thewestward jet which is seen on a larger scale.
| Short-term photometric variability of Psi Persei and Zeta Tauri
We report the short-term photometric periods and UBV light and coloramplitudes of the Be stars Psi Persei and Zeta Tauri, derived fromobservations made in Arizona and Hungary, as part of a multiwavelengthcampaign in 1991. The most likely periods are 1.021 and 0.665 days,respectively, with the period of Zeta Tauri being most uncertain. Theseare in satisfactory agreement with the periods obtained fromsimultaneous UV photometry and/or from previous ground-basedobservations.
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