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Simultaneous intensive photometry and high resolution spectroscopy of delta Scuti stars. IV. An improved picture of the pulsational behaviour of X Caeli
The delta Scuti star X Caeli has been the target of a simultaneousphotometric (14 consecutive nights) and spectroscopic campaign (8consecutive nights). From the analysis of light curves we were able topick up 17 frequency components, most of which were already detected intwo previous campaigns. The comparison with the results of the previouscampaigns shows that while some terms are rather stable (in particularthe dominant mode at 7.39 cd-1 ) others have conspicuousamplitude variations. 14 photometric terms have been also detected inthe radial velocity curve or in the analysis of the line profilevariations. There are no spectroscopic terms without photometriccounterparts, and this means that there are no high-degree modes asobserved in other delta Scuti stars. The simultaneous fit of light andline profile variations has allowed the estimation of the inclination ofrotational axis (about 70o) and the l,m identification formany modes. In particular there is clear evidence that the two shortestperiod modes are retrograde. Rather reliable results were found for thedominant mode which has l=1, m=-1. The resulting physical parameters ofits pulsation are in good agreement with the prediction of theoreticalmodels and suggest for this star a mixing length parameter of about 0.5.Finally the fundamental stellar physical parameters and their refinementare discussed in the light of the identification of the 7.47cd-1 term as a radial mode. Based on observations collectedat European Southern Observatory(Proposal 58.E-0278)
| Radial velocities of HIPPARCOS southern B8-F2 type stars
Radial velocities have been determined for a sample of B8-F2 type starsobserved by the Hipparcos satellite. Observations were obtained withinthe framework of an ESO key-program. Radial velocities have beenmeasured using a cross-correlation method, the templates being a grid ofsynthetic spectra. The obtained precision depends on effectivetemperature and projected rotational velocity of the star as well as ona possible asymmetry of the correlation peak generally due to secondarycomponents. New spectroscopic binaries have been detected from theseasymmetries and the variability of the measured radial velocity.Simulations of binary and triple systems have been performed. Forbinaries our results have been compared with Hipparcos binary data.Adding the variable radial velocities, the minimum binary fraction hasbeen found 60% for physical systems. Radial velocities have beendetermined for 581 B8-F2 stars, 159 being new. Taking into accountpublished radial velocities, 39% south A-type stars with V magnitudelower than 7.5 have a radial velocity. Based on observations obtained atthe European Southern Observatory (ESO, La Silla, Chile) and on datafrom the ESA Hipparcos astrometry satellite.}\fnmsep \thanks{Tables 7, 8and 9 are only available in electronic form at the CDS via anonymous ftpto cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Simultaneous intensive photometry and high resolution spectroscopy of δ Scuti stars. II. X Caeli: a star with unusual spectral features.
Simultaneous photometric B, V (14 consecutive nights; 100 hours ofobservations) and high resolution spectroscopic observations (4consecutive nights; 27 hours) were performed on the δ Scuti star XCaeli at La Silla Observatory in 1992. The photometric data allow thedetection of 14 pulsation terms, some of which coincide in frequencywith the second harmonics or the non-linear coupling terms of the lowerfrequency components. Possible excitation by resonance is suggested. Thecomparison with our previous observations of 1989 shows that while theamplitude of the strongest term (ν=7.39c/d) is very stable, a fewother terms have changed their amplitudes. From the study of lineprofiles and their variations we derive vsin i=70km/s,65deg<=i<=90deg, and that the dominant photometric term is aprograde mode with m=-1 and l=1 or 2. The other terms are probably nonradial p modes with l=2+/-1. There is no evidence of the presence ofhigh-degree sectorial modes with l=|m|. The stellar spectral lines havea narrow absorption core which could be due to the presence of acircumstellar shell.
| Ca II H and K Filter Photometry on the UVBY System. II. The Catalog of Observations
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995AJ....109.2828T&db_key=AST
| Red supergiants in the southern Milky Way. I - Search and classification techniques
A detailed description of a continuing survey for distant, coolsupergiants near the Galactic plane in the southern hemisphere ispresented. Candidate stars are found on near-IR objective-prism plates,and confirming observations are made with near-IR narrowband photometryand medium-resolution CCD spectroscopy. The fluxes of 36 southern andequatorial standard stars for the eight-color narrowband system aregiven. The way in which stars are classified in temperature andluminosity type, and the way the photometry is used to derive distancesand reddening are shown. Plate centers of the near-IR survey, propertiesof interference filters, fluxes of faint standard stars, and extinctioncoefficients for Cerro Tobolo are presented.
| 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.
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