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Roche tomography of cataclysmic variables - III. Star-spots on AE Aqr
We present a Roche tomography reconstruction of the secondary star inthe cataclysmic variable AE Aqr. The tomogram reveals several surfaceinhomogeneities that are due to the presence of large, cool star-spots.In addition to a number of lower latitude spots, the maps also show thepresence of a large, high-latitude spot similar to that seen in Dopplerimages of rapidly rotating isolated stars, and a relative paucity ofspots at a latitude of 40°. In total, we estimate that some 18 percent of the Northern hemisphere of AE Aqr is spotted.We have also applied the entropy landscape technique to determineaccurate parameters for the binary system. We obtain optimal massesM1 = 0.74Msolar, M2 =0.50Msolar, a systemic velocity γ = -63kms-1and an orbital inclination i = 66°.Given that this is the first study to successfully image star-spots onthe secondary star in a cataclysmic variable, we discuss the role thatfurther studies of this kind may play in our understanding of thesebinaries.
| Few Skewed Disks Found in First Closure-Phase Survey of Herbig Ae/Be Stars
Using the three-telescope IOTA interferometer on Mount Hopkins, wereport results from the first near-infrared (λ=1.65 μm)closure-phase survey of young stellar objects (YSOs). These closurephases allow us to unambiguously detect departures from centrosymmetry(i.e., skew) in the emission pattern from YSO disks on the scale of ~4mas, expected from generic ``flared disk'' models. Six of 14 targetsshowed small, yet statistically significant nonzero closure phases, withlargest values from the young binary system MWC 361-A and the(pre-main-sequence?) Be star HD 45677. Our observations are quitesensitive to the vertical structure of the inner disk, and we confrontthe predictions of the ``puffed-up inner wall'' models of Dullemond,Dominik, & Natta (DDN). Our data support disk models with curvedinner rims because the expected emission appears symmetricallydistributed around the star over a wide range of inclination angles. Incontrast, our results are incompatible with the models possessingvertical inner walls because they predict extreme skewness (i.e., largeclosure phases) from the near-IR disk emission that is not seen in ourdata. In addition, we also present the discovery of mysterious H-band``halos'' (~5%-10% of light on scales 0.01"-0.50") around a few objects,a preliminary ``parametric imaging'' study for HD 45677, and the firstastrometric orbit for the young binary MWC 361-A.
| Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters
The availability of the Hipparcos Catalogue has triggered many kinematicand dynamical studies of the solar neighbourhood. Nevertheless, thosestudies generally lacked the third component of the space velocities,i.e., the radial velocities. This work presents the kinematic analysisof 5952 K and 739 M giants in the solar neighbourhood which includes forthe first time radial velocity data from a large survey performed withthe CORAVEL spectrovelocimeter. It also uses proper motions from theTycho-2 catalogue, which are expected to be more accurate than theHipparcos ones. An important by-product of this study is the observedfraction of only 5.7% of spectroscopic binaries among M giants ascompared to 13.7% for K giants. After excluding the binaries for whichno center-of-mass velocity could be estimated, 5311 K and 719 M giantsremain in the final sample. The UV-plane constructed from these datafor the stars with precise parallaxes (σπ/π≤20%) reveals a rich small-scale structure, with several clumpscorresponding to the Hercules stream, the Sirius moving group, and theHyades and Pleiades superclusters. A maximum-likelihood method, based ona Bayesian approach, has been applied to the data, in order to make fulluse of all the available stars (not only those with precise parallaxes)and to derive the kinematic properties of these subgroups. Isochrones inthe Hertzsprung-Russell diagram reveal a very wide range of ages forstars belonging to these groups. These groups are most probably relatedto the dynamical perturbation by transient spiral waves (as recentlymodelled by De Simone et al. \cite{Simone2004}) rather than to clusterremnants. A possible explanation for the presence of younggroup/clusters in the same area of the UV-plane is that they have beenput there by the spiral wave associated with their formation, while thekinematics of the older stars of our sample has also been disturbed bythe same wave. The emerging picture is thus one of dynamical streamspervading the solar neighbourhood and travelling in the Galaxy withsimilar space velocities. The term dynamical stream is more appropriatethan the traditional term supercluster since it involves stars ofdifferent ages, not born at the same place nor at the same time. Theposition of those streams in the UV-plane is responsible for the vertexdeviation of 16.2o ± 5.6o for the wholesample. Our study suggests that the vertex deviation for youngerpopulations could have the same dynamical origin. The underlyingvelocity ellipsoid, extracted by the maximum-likelihood method afterremoval of the streams, is not centered on the value commonly acceptedfor the radial antisolar motion: it is centered on < U > =-2.78±1.07 km s-1. However, the full data set(including the various streams) does yield the usual value for theradial solar motion, when properly accounting for the biases inherent tothis kind of analysis (namely, < U > = -10.25±0.15 kms-1). This discrepancy clearly raises the essential questionof how to derive the solar motion in the presence of dynamicalperturbations altering the kinematics of the solar neighbourhood: doesthere exist in the solar neighbourhood a subset of stars having no netradial motion which can be used as a reference against which to measurethe solar motion?Based on observations performed at the Swiss 1m-telescope at OHP,France, and on data from the ESA Hipparcos astrometry satellite.Full Table \ref{taba1} is only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/430/165}
| Near-Infrared Interferometric Measurements of Herbig Ae/Be Stars
We have observed the Herbig Ae/Be sources AB Aur, VV Ser, V1685 Cyg (BD+40°4124), AS 442, and MWC 1080 with the Palomar TestbedInterferometer, obtaining the longest baseline near-IR interferometricobservations of this class of objects. All of the sources are resolvedat 2.2 μm with angular size scales generally <~5 mas, consistentwith the only previous near-IR interferometric measurements of HerbigAe/Be stars, by Millan-Gabet and collaborators. We determine the angularsize scales and orientations predicted by uniform-disk, Gaussian, ring,and accretion disk models. Although it is difficult to distinguishdifferent radial distributions, we are able to place firm constraints onthe inclinations of these models, and our measurements are the firstthat show evidence for significantly inclined morphologies. In addition,the derived angular sizes for the early-type Herbig Be stars in oursample, V1685 Cyg and MWC 1080, agree reasonably well with thosepredicted by the face-on accretion disk models used by Hillenbrand andcollaborators to explain observed spectral energy distributions. Incontrast, our data for the later-type sources AB Aur, VV Ser, and AS 442are somewhat inconsistent with these models and may be explained betterthrough the puffed-up inner disk models of Dullemond and collaborators.
| High-Precision Near-Infrared Photometry of a Large Sample of Bright Stars Visible from the Northern Hemisphere
We present the results of 8 yr of infrared photometric monitoring of alarge sample of stars visible from Teide Observatory (Tenerife, CanaryIslands). The final archive is made up of 10,949 photometric measuresthrough a standard InSb single-channel photometer system, principally inJHK, although some stars have measures in L'. The core of this list ofstars is the standard-star list developed for the Carlos SánchezTelescope. A total of 298 stars have been observed on at least twooccasions on a system carefully linked to the zero point defined byVega. We present high-precision photometry for these stars. The medianuncertainty in magnitude for stars with a minimum of four observationsand thus reliable statistics ranges from 0.0038 mag in J to 0.0033 magin K. Many of these stars are faint enough to be observable with arraydetectors (42 are K>8) and thus to permit a linkage of the bright andfaint infrared photometric systems. We also present photometry of anadditional 25 stars for which the original measures are no longeravailable, plus photometry in L' and/or M of 36 stars from the mainlist. We calculate the mean infrared colors of main-sequence stars fromA0 V to K5 V and show that the locus of the H-K color is linearlycorrelated with J-H. The rms dispersion in the correlation between J-Hand H-K is 0.0073 mag. We use the relationship to interpolate colors forall subclasses from A0 V to K5 V. We find that K and M main-sequence andgiant stars can be separated on the color-color diagram withhigh-precision near-infrared photometry and thus that photometry canallow us to identify potential mistakes in luminosity classclassification.
| The association of IRAS sources and 12CO emission in the outer Galaxy
We have revisited the question of the association of CO emission withIRAS sources in the outer Galaxy using data from the FCRAO Outer GalaxySurvey (OGS). The availability of a large-scale high-resolution COsurvey allows us to approach the question of IRAS-CO associations from anew direction - namely we examined all of the IRAS sources within theOGS region for associated molecular material. By investigating theassociation of molecular material with random lines of sight in the OGSregion we were able to construct a quantitative means to judge thelikelihood that any given IRAS-CO association is valid and todisentangle multiple emission components along the line of sight. Thepaper presents a list of all of the IRAS-CO associations in the OGSregion. We show that, within the OGS region, there is a significantincrease ( ~ 22%) in the number of probable star forming regions overprevious targeted CO surveys towards IRAS sources. As a demonstration ofthe utility of the IRAS-CO association table we present the results ofthree brief studies on candidate zone-of-avoidance galaxies with IRAScounterparts, far outer Galaxy CO clouds, and very bright CO clouds withno associated IRAS sources. We find that ~ 25% of such candidate ZOAGsare Galactic objects. We have discovered two new far outer Galaxystar-forming regions, and have discovered six bright molecular cloudsthat we believe are ideal targets for the investigation of the earlieststages of sequential star formation around HII regions. Finally, thispaper provides readers with the necessary data to compare othercatalogued data sets with the OGS data.Tables 1, 2 and A1 are only available in electronic form at the CDS viaanonymous ftp to\ cdsarc.u-strasbg.fr (130.79.128.5) or via\http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/399/1083
| The stellar mass ratio of GK Persei
We study the absorption lines present in the spectra of the long-periodcataclysmic variable GK Per during its quiescent state, which areassociated with the secondary star. By comparing quiescent data withoutburst spectra we infer that the donor star appears identical duringthe two states and the inner face of the secondary star is notnoticeably irradiated by flux from the accreting regions. We obtain newvalues for the radial velocity semi-amplitude of the secondary star,KK=120.5+/-0.7kms-1, a projected rotationalvelocity, VKsini=61.5+/-11.8kms-1, andconsequently a measurement of the stellar mass ratio of GK Per,q=MK/MWD=0.55+/-0.21. The inferred white dwarfradial velocities are greater than those measured traditionally usingthe wings of Doppler-broadened emission lines suspected to originate inan accretion disc, highlighting the unsuitability of emission lines formass determinations in cataclysmic variables. We determine mass limitsfor both components in the binary,MK>=0.48+/-0.32Msolar andMWD>=0.87+/-0.24Msolar.
| Spatially Resolved Circumstellar Structure of Herbig AE/BE Stars in the Near-Infrared
We have conducted the first systematic study of Herbig Ae/Be stars usingthe technique of long baseline stellar interferometry in thenear-infrared, with the objective of characterizing the distribution andproperties of the circumstellar dust responsible for the excessnear-infrared fluxes from these systems. The observations for this workhave been conducted at the Infrared Optical Telescope Array (IOTA). Theprincipal result of this paper is that the interferometer resolves thesource of infrared excess in 11 of the 15 systems surveyed. A newbinary, MWC 361-A, has been detected interferometrically for the firsttime. The visibility data for all the sources has been interpretedwithin the context of four simple models which represent a range ofplausible representations for the brightness distribution of the sourceof excess emission: a Gaussian, a narrow uniform ring, a flat blackbodydisk with a single temperature power law, and an infrared companion. Wefind that the characteristic sizes of the near-infrared emitting regionsare larger than previously thought (0.5-5.9 AU, as given by the FWHM ofthe Gaussian intensity). A further major result of this paper is thatthe sizes measured, when combined with the observed spectral energydistributions, essentially rule out accretion disk models represented byblackbody disks with the canonical T(r)~r-3/4 law. We alsofind that, within the range observed in this study, none of the sources(except the new binary) shows varying visibilities as the orientation ofthe interferometer baseline changes. This is the expected behavior forsources which appear circularly symmetric on the sky, and for thesources with the largest baseline position angle coverage (AB Aur, MWC1080-A) asymmetric brightness distributions (such as inclined disks orbinaries) become highly unlikely. Taken as an ensemble, with no clearevidence in favor of axisymmetric structure, the observations favor theinterpretation that the circumstellar dust is distributed in sphericalenvelopes (the Gaussian model) or thin shells (the ring model). Thisinterpretation is also supported by the result that the measured sizes,combined with the excess near-infrared fluxes, imply emission of finiteoptical depth, as required by the fact that the central stars areoptically visible. The measured sizes and brightnesses do not correlatestrongly with the luminosity of the central star. Moreover, in twocases, the same excess is observed from circumstellar structures thatdiffer in size by more than a factor of 2 and surround essentiallyidentical stars. Therefore, different physical mechanisms for thenear-infrared emission may be at work in different cases, oralternatively, a single underlying mechanism with the property that thesame infrared excess is produced on very different physical scales.
| Absolute proper motions of open clusters. I. Observational data
Mean proper motions and parallaxes of 205 open clusters were determinedfrom their member stars found in the Hipparcos Catalogue. 360 clusterswere searched for possible members, excluding nearby clusters withdistances D < 200 pc. Members were selected using ground basedinformation (photometry, radial velocity, proper motion, distance fromthe cluster centre) and information provided by Hipparcos (propermotion, parallax). Altogether 630 certain and 100 possible members werefound. A comparison of the Hipparcos parallaxes with photometricdistances of open clusters shows good agreement. The Hipparcos dataconfirm or reject the membership of several Cepheids in the studiedclusters. Tables 1 and 2 are only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Solving the kilosecond quasi-periodic oscillation problem of the intermediate polar GK Persei
We detect the likely optical counterpart to previously reported X-rayQPOs in spectrophotometry of the intermediate polar GK Per during the1996 dwarf nova outburst. The characteristic time-scales range between4000 and 6000 s. Although the QPOs are an order of magnitude longer thanthose detected in the other dwarf novae we show that a new QPO model isnot required to explain the long time-scale observed. We demonstratethat the observations are consistent with oscillations being the resultof normal time-scale QPOs beating with the spin period of the whitedwarf. We determine the spectral class of the companion to be consistentwith its quiescent classification and find no significant evidence forirradiation over its inner face. We detect the white dwarf spin periodin line fluxes, V/R ratios and Doppler-broadened emission profiles.
| 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 Use of Near Infrared Spectroscopy to Reclassify HR:8881
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1994MNRAS.266..678H&db_key=AST
| UBV photometry of stars whose positions are accurately known. VI
Results are presented from UBV photometric observations of 1000 stars ofthe Bright Star Catalogue and the faint extension of the FK5.Observations were carried out between July 1987 and December 1990 withthe 40-cm Cassegrain telescope of the Kvistaberg Observatory.
| Photometric Data for the Bright Stars
Not Available
| Etude cinematique et photometrique d'une region de Cas.
Not Available
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Observation and Astrometry data
| Constellation: | Cassiopeia |
| Right ascension: | 23h20m14.30s |
| Declination: | +61°58'12.0" |
| Apparent magnitude: | 6.45 |
| Distance: | 289.017 parsecs |
| Proper motion RA: | 6.9 |
| Proper motion Dec: | -5.3 |
| B-T magnitude: | 8.59 |
| V-T magnitude: | 6.584 |
Catalogs and designations:
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