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3D mapping of the dense interstellar gas around the Local Bubble
We present intermediate results from a long-term program of mapping theneutral absorption characteristics of the local interstellar medium,motivated by the availability of accurate and consistent parallaxes fromthe Hipparcos satellite. Equivalent widths of the interstellar NaID-line doublet at 5890 Å are presented for the lines-of-sighttowards some 311 new target stars lying within ~ 350 pc of the Sun.Using these data, together with NaI absorption measurements towards afurther ~ 240 nearby targets published in the literature (for many ofthem, in the directions of molecular clouds), and the ~ 450lines-of-sight already presented by (Sfeir et al. \cite{sfeir99}), weshow 3D absorption maps of the local distribution of neutral gas towards1005 sight-lines with Hipparcos distances as viewed from a variety ofdifferent galactic projections.The data are synthesized by means of two complementary methods, (i) bymapping of iso-equivalent width contours, and (ii) by densitydistribution calculation from the inversion of column-densities, amethod devised by Vergely et al. (\cite{vergely01}). Our present dataconfirms the view that the local cavity is deficient in cold and neutralinterstellar gas. The closest dense and cold gas ``wall'', in the firstquadrant, is at ~ 55-60 pc. There are a few isolated clouds at closerdistance, if the detected absorption is not produced by circumstellarmaterial.The maps reveal narrow or wide ``interstellar tunnels'' which connectthe Local Bubble to surrounding cavities, as predicted by the model ofCox & Smith (1974). In particular, one of these tunnels, defined bystars at 300 to 600 pc from the Sun showing negligible sodiumabsorption, connects the well known CMa void (Gry et al. \cite{gry85}),which is part of the Local Bubble, with the supershell GSH 238+00+09(Heiles \cite{heiles98}). High latitude lines-of-sight with the smallestabsorption are found in two ``chimneys'', whose directions areperpendicular to the Gould belt plane. The maps show that the LocalBubble is ``squeezed'' by surrounding shells in a complicated patternand suggest that its pressure is smaller than in those expandingregions.We discuss the locations of several HI and molecular clouds. Usingcomparisons between NaI and HI or CO velocities, in some cases we areable to improve the constraints on their distances. According to thevelocity criteria, MBM 33-37, MBM 16-18, UT 3-7, and MBM 54-55 arecloser than ~ 100 pc, and MBM 40 is closer than 80 pc. Dense HI cloudsare seen at less than 90 pc and 85 pc in the directions of the MBM 12and MBM 41-43 clouds respectively, but the molecular clouds themselvesmay be far beyond. The above closest molecular clouds are located at theneutral boundary of the Bubble. Only one translucent cloud, G192-67, isclearly embedded within the LB and well isolated.These maps of the distribution of local neutral interstellar NaI gas arealso briefly compared with the distribution of both interstellar dustand neutral HI gas within 300 pc.Tables 1 and 2 are 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/411/447
| The mass ratio distribution of B-type visual binaries in the Sco OB2 association
A sample of 115 B-type stars in the Sco OB2 association is examined forexistence of visual companions in the J and K_s bands, using the ADONISnear-infrared adaptive optics system and coronograph. Practically allthe components in the separation range 0farcs3 -6farcs4 (45-900 AU) andmagnitudes down to K = 16 were detected. The K and J - K photometry ofthe primaries and differential photometry and astrometry of the 96secondaries are presented. Ten secondaries are new physical components,as inferred from the photometric and statistical criteria, while therest of the newly detected objects are faint background stars. After asmall correction for detection incompleteness and a conversion of thefluxes into masses, an unbiased distribution of the components massratio q was derived. The power law f(q)~ q-0.5 fits theobservations well, whereas a q-1.8 distribution, whichcorresponds to a random pairing of stars, is rejected. The companionstar fraction is 0.20+/-0.04 per decade of separation which iscomparable to the highest measured binary fraction among low-mass PMSstars and ~ 1.6 times higher than the binary fraction of low-mass dwarfsin the solar neighborhood and in open clusters in the same separationrange. Based on observations collected at the European SouthernObservatory, La Silla, Chile (ESO programme 65.H-0179). Tables 1, 3 andthe full version of Table 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/cgi-bin/qcat?J/A+A/382/92
| Short-period line profile variations in the Be star μ Centauri
We present new intensive photometric observations of the Be star μCen for several seasons which support a period close to 1d. We alsopresent high-resolution spectroscopic data consisting of 302 spectra in1999 and 864 spectra in 2000, all obtained within a two-week observingrun in each season. We use stacked grey-scale plots of spectra, fromwhich the mean line profile has been removed, to examine the profilevariations. We find that most nights show one residual absorptionfeature, moving from blue to red, visible in all helium and metal linesand also clearly visible in Hα and other lines formed in thecircumstellar environment. We therefore conclude that this feature is ofcircumstellar origin. In addition, a residual absorption feature movingfrom red to blue is sometimes seen at irregular intervals. We find thatthe residual absorption feature frequently strays outside the projectedrotational velocity limit and that on occasions it remains well withinthis limit. The radial velocity data reproduce only two of the sixfrequencies previously found in the star. We point out that this by nomeans implies that the star is a multiperiodic, non-radial pulsator.Photometric data obtained over several seasons indicate a period veryclose to 1d and not the 0.5-d period found from the radial velocities.We describe an outburst which occurred during the run and which resultedin increased Hα emission two nights later. It is clear thatoutbursts in Be stars are localized events and that the gas released byoutbursts is probably responsible for localized increased absorption,resulting in periodic light and line profile variations.
| Binary systems with post-T Tauri secondaries
The identification of post-T Tauri (pTT) stars selected throughspectroscopic criteria by Pallavicini et al. (\cite{Pallavicini92}) andby Martín et al. (1992) among the candidates belonging to visualbinary systems is revisited in the present paper by studying theirposition in the HR diagram. These stars belong to the so-called Lindroosbinary sample (Lindroos \cite{Lindroos85}), i.e. to systems withearly-type primaries and late-type companions. If these binaries arephysical and not simply optical pairs, similar ages must be found forthe early-type primary and the late-type component of each system. Theages of these systems have been derived by Lindroos in 1986, by usingcalibrations of the uvbyβ indices. In this paper, we revisit theseages through the position of these stars among new evolutionary tracksin the HR diagram for pre- and post-main sequence stars. We derive newestimations of the ages of each system component, as well as theirmasses, using parallaxes of the early-type component derived fromHipparcos data and by forcing the late-type companion to be at the samedistance. Teff and log g of the early-type components havebeen computed using the calibrations of two independent photometricsystems: the uvbyβ photometry and the Geneva system. TheTeff of the late-type stars have been determined by usingvarious calibrations of several photometric systems: uvbyβ, UBV andVRI, in order to determine the uncertainties and systematic errors onthese parameters and consequently on the ages. Differences in the agesand masses obtained by using various sources of recent evolutionarymodels are considered and discussed. The consistency of the age of thelate type component with that of its early type primary is examined; thevalidity of this criterion for a selection of physical pairs isdiscussed. The accuracy of the observational and theoretical data arenot sufficient to assign stringent values to the age for several of theexamined systems. Nevertheless, in spite of the large error bars, wehave established that we could select a number of systems which,according to their position in the HR diagram, may be physicallyassociated. The selection of possible physically bounded systemsobtained with the present approach and that made by Pallavicini et al.(\cite{Pallavicini92}) or Martín et al. (1992) on the basis ofspectroscopic criteria are not always coincident. Spectroscopiccriteria, for example the presence of a strong Li feature, are morestringent conditions than that of coherent ages of primaries andsecondaries; however the Li I 6708 doublet is expected to fade in thelatest stages of the pre-main sequence life of a star, so that the``oldest" pTTs may not be detected by spectroscopy only. The differentresults so obtained are discussed for each system and we conclude thatthe present approach may be used as a powerful criterion to select newpTT candidates in visual binaries to be observed and analyzed with highresolution spectrographs and to select candidates that have almostreached the main sequence. Partly based on data from the ESA Hipparcosastrometric satellite. Tables 2, 5, 7 and 9 are only available inelectronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/379/162
| ADONIS observations of hard X-ray emitting late B-type stars in Lindroos systems
We present adaptive optics JHK_S imaging observations of threemain-sequence late B-type stars listed in the Lindroos Catalogue: HD123445, HD 127971 and HD 129791. Given their spectral types, these starsshould not be X-ray emitters. However, they have been detected by ROSATand their X-ray emission has been attributed to possible unresolvedlate-type companions. We have carried out near-IR observations withADONIS at the ESO 3.6 m but have not detected any late-type companionsclose to HD 127971 and HD 129791. This result leads us to conclude thateither (i) they are spectroscopic binaries with unresolved low-masscompanions, or (ii) they are intrinsic X-ray emitters. While the formercase would be consistent with the reported high multiplicity ofearly-type (A and B) stars, the latter would yield a revision of stellaractivity theories which do not predict X-ray emission from these stars.On the other hand, HD 123445 does indeed show visual companions, namelyan apparent subarcsecond faint (K_s ~ 10) binary system at a projectedseparation of 5\arcsec from the late-B type star. The JHK_S magnitudesand colors of the components are consistent with (i) a pair of Pre MainSequence (PMS) K-type stars at 140 pc (i.e. possible members of theUpper Centaurus Lupus association), (ii) a pair of Main Sequence M-typestars at 60 pc and (iii) a pair of K-type giants at 2.6 kpc. While inthe first case the reported X-ray emission can be ascribed to the newobjects, in the second and third case it cannot, and we have to assumethe late B-type star to be either a spectroscopic binary itself or asingle star with intrinsic X-ray emission. Spectroscopy is required toconfirm the possible PMS nature of the new binary and Chandra X-ray highspatial resolution (astrometric) imaging observations are required todefinitely determine the source of the X-ray emission. If the B9 starresults to be the X-ray emitter, near-IR spectroscopy can be used toinvestigate the presence of a T Tauri like spectroscopic companions.Based on observations collected at the European Southern Observatory, LaSilla, under project 65.H-0568(A).
| X-ray emission from Lindroos binary systems
We present a study of the X-ray emission from binary systems extractedfrom the Lindroos catalogue (Lindroos 1986) based on the ROSAT All-Skysurvey as well as ROSAT PSPC and HRI pointings. The studied sampleconsists of visual binary systems comprised of early-type primaries andlate-type secondaries. The ages of the systems were determined byLindroos (1985) from uvbybeta photometry of the primaries. These agesrange between 33 and 135 Myr, so if the late-type secondaries arephysically bound to the early-type primaries, they could be Post-T Tauristars (PTTS). We have found strong X-ray emission from severalsecondaries. This fact together with their optical and IR data, makethem bona fide PTTS candidates. We have also detected X-ray emissionfrom several early-type primaries and, in particular, from most of thelate-B type stars. Because their HRI hardness ratios are similar tothose from resolved late-type stars, the presence of an unresolvedlate-type companion seems to be the cause of this emission.
| High S/N Echelle spectroscopy in young stellar groups. II. Rotational velocities of early-type stars in SCO OB2.
We investigate the rotational velocities of early-type stars in the ScoOB2 association. We measure v.sin(i) for 156 established and probablemembers of the association. The measurements are performed with threedifferent techniques, which are in increasing order of expectedv.sin(i): 1) converting the widths of spectral lines directly tov.sin(i), 2) comparing artificially broadened spectra of low v.sin(i)stars to the target spectrum, 3) comparing the HeI λ4026 lineprofile to theoretical models. The sample is extended with literaturedata for 47 established members of Sco OB2. Analysis of the v.sin(i)distributions shows that there are no significant differences betweenthe subgroups of Sco OB2. We find that members of the binary populationof Sco OB2 on the whole rotate more slowly than the single stars. Inaddition, we find that the B7-B9 single star members rotatesignificantly faster than their B0-B6 counterparts. We test varioushypotheses for the distribution of v.sin(i) in the association. Theresults show that we cannot clearly exclude any form of randomdistribution of the direction and/or magnitude of the intrinsicrotational velocity vector. We also investigate the effects of rotationon colours in the Walraven photometric system. We show that positions ofB7-B9 single dwarfs above the main sequence are a consequence ofrotation. This establishes the influence of rotation on the Walravencolours, due primarily to surface gravity effects.
| 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.
| 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.
| Radio continuum emission from stars: a catalogue update.
An updated version of my catalogue of radio stars is presented. Somestatistics and availability are discussed.
| Simultaneous photometric and spectroscopic monitoring of rapid variations of the Be star η Centauri.
Results of the simultaneous monitoring of line-profile and light andcolour variations of the bright southern Be star ηCen in May-June1992 are reported. The new data were analyzed along with numerousearlier b and uvby observations of the star, secured between 1987 and1991. The brightness of ηCen varies on three distinct time scalesbut only rapid variations on a time scale of hours to days are analyzedhere. They can be described as a superposition of a periodic componentwith period 0.6424241d, which is secularly stable over the wholesix-year interval covered by our data, and systematic but obviouslyaperiodic cycle-to-cycle disturbances. The 0.6424-d light curve isslightly non-sinusoidal (light minima occur 0.64^P^ after light maxima)and has an average peak-to-peak amplitude of 0.05mag in y, b and v andabout 0.10mag in u. The u-b and 1 indices also vary with the sameperiod, with full amplitudes of 0.04mag and 0.03mag, respectively, whilethe variations of b-y and .1mag - if present - are within 0.01mag only.During light maximum, the star is bluest in u-b. The radial velocity ofSi III 455.26nm as measured in the outer wings of the profile exhibits anearly sinusoidal variation with the 0.6424-d period and definitivelyexcludes the triple-wave photometric period of 1.927d consideredearlier. For variations of other line-profile parameters of the Si III455.26 nm line, the most significant periods differ by up to +/-5% fromthe 0.6424-d period. More extended spectroscopic material will be neededto confirm our preliminary conclusion that this disparity is ofstochastic nature only and that the entire line-profile variability maybe reconciled with the photometric period. The exactly simultaneousmonitoring shows that radial velocity, first moment, equivalent width,and line depth of the Si III 455.26nm line increase when the star isgetting brighter and bluer. Very pronounced higher-order line-profilevariations of the Si III line were also detected. They have thecharacter of apparent absorption or emission bumps, which move acrossthe line profile from blue to red. Most of them disappear close to theline center. The analysis of their radial velocities leads to asuper-period, which is close to the photometric one. Occurrence andstrength of the bumps also seem to follow the same period. The light,colour, radial-velocity and equivalent-width variations can only be dueto the low-order line profile variations or duplicity. The observedradial-velocity amplitude seems to be larger than expected for therotational modulation and nonradial pulsation models. Theequivalent-width variation cannot be understood unless a phase-dependentmicroturbulent velocity is assumed in both models. Available data cannotalso exclude a model of a contact binary with 0.6-day orbital period.
| ROSAT detections of X-ray emission from young B-type stars
We present first results of a series of pointings of the Rosat HRI atvisual binaries consisting of a B-star with a later-type companion. Thebinaries selected for this study are very likely physical pairs. Datingof the B-type stars with respect to the zero-age main sequence, as wellas spectroscopic observations of the late-type stars, provides evidencefor the extreme youth of these systems with ages typically near or below10 exp 8 yr. Surprisingly, the late-B component was in many casesdetected as an X-ray source, in contrast to previous findings that X-rayemission among late-B field stars is rather uncommon.
| A homogeneous catalog of new UBV and H-beta photometry of B- and A-type stars in and around the Scorpius-Centaurus OB association
B- and A-type stars in and near the Sco-Cen OB association areinvestigated with UBV and H-beta photometry to acquire data relevant tothe luminosity function of Sco-Cen. The measurements generally consistof two 10-s integrations of U, B, V, (W, N) filters, and theobservations are corrected iteratively for atmospheric extinction andinstrumental response. The data presented give the mean V magnitude,mean B-V, mean U-B, and the estimated uncertainties for these values.The catalog provides a homogeneous catalog of data for a large fieldwith stellar objects delineating membership to the association Sco-Cenand that affect the luminosity function of the aggregate.
| X-ray emission from age-dated post-T Tauri stars.
Not Available
| Walraven photometry of nearby southern OB associations
Homogeneous Walraven (VBLUW) photometry is presented for 5260 stars inthe regions of five nearby southern OB associations: Scorpio Centaurus(Sco OB2), Orion OB1, Canis Major OB1, Monoceros OB1, and Scutum OB2.Derived V and (B - V) in the Johnson system are included.
| Intensive photometry of southern Be variables. I - Winter objects
Results are presented from an intensive photometric campaign on somebright southern Be stars to search for periodic light variations. Inorder to obtain good phase coverage, observations were conducted fromtwo sites with different longitude: ESO and SAAO. Most of the starsobserved are indeed variable with periods close to one day. Results forwinter objects are given.
| A photometric survey of the bright southern Be stars
Repeated UBV photometric measurements were made of the 86 bright Bestars south of declination -20 deg, and a network of comparison starswas set up. From a statistical study of the differential photometry itwas found that short- or intermediate-term variability seems to beoccurring in about half of the Be stars, and to be more evident in thestars of earlier spectral type. It was also possible to identify 11individual short- or intermediate-term variables. Four of these (all ofearly B spectral type) appear to exhibit significant variability on atime-scale of a day or less. More intensive observations of one of thesestars, 28 Omega CMA, indicate short-term variations consistent with thepublished spectroscopic period of 1.37 day.
| A study of visual double stars with early-type primaries. V - Post-T Tauri secondaries
In an ongoing study of companions of O and B type primaries, themajority of the secondaries are found to be of spectral type F, G, or K.Their properties are investigated in relation to their evolutionarystatus. The ages of the systems have been determined from uvby-betaphotometry of the primaries and it is found that all are younger than150 million years and half are less than 30 million years old.Thirty-seven secondaries have ages less than the expected contractiontime to the zero-age-main sequence (ZAMS). More than 50 percent of theF, G, and K secondaries exhibit spectroscopic features (Ca II H, K andH-alpha emission and strong Li absorption) typical of young stars andreminiscent of T Tauri stars although not as conspicuous. It isappropriate to classify them as post-T Tauri stars. The lifetime of somefeatures characteristic of early stellar evolution is discussed.
| A study of visual double stars with early type primaries. IV Astrophysical data
Astrophysical parameters (MK class, color excess, absolute magnitude,distance, effective temperature, mass, and age) are derived fromcalibrations of the uvby-beta indices for the members of 253 doublestars with O or B type primaries and faint secondaries. The photometricspectral classification is compared to the MK classes, and the agreementis very good. The derived data together with spectroscopic and JHKL dataare used for deciding which pairs are likely to be physical and whichare optical, and it is shown that 98 (34 percent) of the secondaries arelikely to be members of physical systems. For 90 percent of the physicalpairs the projected separation between the components is less than25,000 AU. A majority of the physical secondaries are late-type stars,and 50 percent of them are contracting towards the zero-agemain-sequence. Also presented are new uvby-beta data for 43 secondariesand a computer program for determining astrophysical parameters fromuvby-beta data.
| The local system of early type stars - Spatial extent and kinematics
Published uvby and H-beta photometric data and proper motions arecompiled and analyzed to characterize the structure and kinematics ofthe bright early-type O-A0 stars in the solar vicinity, with a focus onthe Gould belt. The selection and calibration techniques are explained,and the data are presented in extensive tables and graphs and discussedin detail. The Gould belt stars of age less than 20 Myr are shown togive belt inclination 19 deg to the Galactic plane and node-lineorientation in the direction of Galactic rotation, while the symmetricaldistribution about the Galactic plane and kinematic properties (purecircular differential rotation) of the belt stars over 60 Myr oldresemble those of fainter nonbelt stars of all ages. The unresolveddiscrepancy between the expansion observed in the youngest nearby starsand the predictions of simple models of expansion from a point isattributed to the inhomogeneous distribution of interstellar matter.
| A study of visual double stars with early type primaries. II - Photometric results
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1983A&AS...51..161L&db_key=AST
| A study of visual double stars with early type primaries. I - Spectroscopic results
Attention is given to spectral peculiarities found in data on thespectral classes of 486 stars in 254 visual doublet or multiplet systemswith O or B type primaries, in order to isolate a group of very youngstars that may serve for the study of early stellar evolutioncharacteristics. It is noted that the material contains a substantialfraction of secondaries that are likely to be physical, and that severalof these may be in the premain-sequence phase of stellar evolution, orhave reached the zero-age main sequence.
| Intermediate band photometry of early-type stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977PASP...89..205E&db_key=AST
| Radial velocities of Southern B stars determined at the Radcliffe Observatory - VIII. Stars with HD spectral types B8 and B9
Not Available
| Line strengths for southern OB stars-II. Observations with moderate dispersion
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969MNRAS.144...31B&db_key=AST
| Line strengths for southern OB stars-I, Spectrograms with high dispersion
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969MNRAS.144....1B&db_key=AST
| Radial velocities of southern OB stars and supergiants
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969MNRAS.143....1B&db_key=AST
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| Csillagkép: | Kentaur |
| Rektaszcenzió: | 14h35m31.50s |
| Deklináció: | -41°31'02.0" |
| Vizuális fényesség: | 5.87 |
| Távolság: | 109.89 parszek |
| RA sajátmozgás: | -21.9 |
| Dec sajátmozgás: | -23.3 |
| B-T magnitude: | 5.772 |
| V-T magnitude: | 5.86 |
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