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The Tokyo PMC catalog 90-93: Catalog of positions of 6649 stars observed in 1990 through 1993 with Tokyo photoelectric meridian circle The sixth annual catalog of the Tokyo Photoelectric Meridian Circle(PMC) is presented for 6649 stars which were observed at least two timesin January 1990 through March 1993. The mean positions of the starsobserved are given in the catalog at the corresponding mean epochs ofobservations of individual stars. The coordinates of the catalog arebased on the FK5 system, and referred to the equinox and equator ofJ2000.0. The mean local deviations of the observed positions from theFK5 catalog positions are constructed for the basic FK5 stars to comparewith those of the Tokyo PMC Catalog 89 and preliminary Hipparcos resultsof H30.
| A new optical extinction law and distance estimate for the Taurus-Auriga molecular cloud This paper presents optical spectrophotometry of field stars projectedon the Taurus-Auriga molecular cloud. We derive extinction laws forheavily reddened stars in this sample and show that the reddening lawthrough the dark cloud is nearly identical to the standard law forlambda-lambda(3600-6100) and AV approximately less than 3mag. Our spectroscopic parallaxes suggest a distance of 140 +/- 10 pcfor the northern portion of the cloud and show no compelling evidencefor a substantial variation in distance across the leading edge of thecloud.
| Radial velocity measurements. IV - Ground-based accompaniment to the HIPPARCOS observation program The paper presents 396 radial velocities of stars distributed in 19fields of 4 x 4 degrees. The study employs the Fehrenbach objectiveprism method and the same measuring technique used in a previous paper(Fehrenbach et al., 1987).
| Infrared spectroscopy of dust in the Taurus dark clouds - Ice and silicates Low-resolution spectra of the 3 micron water-ice features of 22 starsand the 10 micron silicate dust features of 16 stars are presented forstars in the direction of the extensive dark cloud complex in Taurus,including both dust-embedded objects and background field stars seenthrough the cloud. A very close linear correlation is found between thepeak optical depth in the 3 micron feature and visual extinction, A(v),for field stars. The detection of ice in all cases where A(v) exceeds athreshold value of 3.3 + or - 0.1 mag serves as a basis for models ofvolatile mantle growth on grains in the dark cloud environment. Thesilicate feature is poorly correlated with A(v), and its relativeweakness per unit A(v) in the spectra of field stars with strong icebands may reflect the dilution of silicates as a fraction of total grainmass as mantles accrete in the dark cloud.
| Magnetic field structure in the Taurus dark cloud Optical and infrared polarimetry of sources in the direction of theTaurus cloud are obtained in order to study the magnetic field in thiscloud and its possible role in the cloud's evolution. Most of the starsare background giant stars whose light shines through the cloud and ispolarized by the cloud material. The transverse component of themagnetic field, as delineated by the polarization vectors, is generallyperpendicular to the galactic plane, and the stratified structure of thecloud could be due to the effect of the magnetic field during the earlystages of collapse. Three of the 13 embedded stars are stronglypolarized with position angles nearly perpendicular to those of nearbyfield stars. The polarization of these stars is most likely intrinsic,and the direction of polarization indicates that the materialsurrounding these stars may be magnetic i.e., that the magnetic field isfrozen in this material.
| Polarimetric investigation of background stars in the region of T and RY Tau Electropolarimetric observations of 97 background stars in the TTauri/RY Tauri region, obtained with the 40-cm Cassegrain telescope ofthe Biurakan Astrophysical Observatory in December 1982, are reportedand interpreted in terms of local-magnetic-field effects oncometary-nebula bending. The data are presented in a table, and thedependence of polarization position angle on declination is establishedin a graph and attributed to a continuous variation in the direction ofthe magnetic field. From the magnitude of the effect, however, it isconcluded that the observed bending of the cometary nebulae in theregion results from the combined influence of the local magnetic momentand the magnetic moment of the star itself (as proposed by Vardanian,1983) rather than from the local moment alone.
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Observation and Astrometry data
Constellation: | Taurus |
Right ascension: | 04h40m58.87s |
Declination: | +23°56'23.3" |
Apparent magnitude: | 9.397 |
Proper motion RA: | -0.8 |
Proper motion Dec: | -8.6 |
B-T magnitude: | 9.865 |
V-T magnitude: | 9.436 |
Catalogs and designations:
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