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Proper motions of faint ROSAT WTT stars in the Chamaeleon region
We present proper motions of 59 stars of the ROSAT All-Sky Survey (RASS)located in direction of the Chamaeleon star forming region (SFR) in themagnitude range B=5.1 - 17 mag. Proper motions of the fainter stars werenewly derived utilizing survey Schmidt plates from the GSC II platearchive and from a set of special plates taken with the ESO Schmidttelescope. The vector point diagram (VPD) indicates that the certifiedWTT stars cluster away from the region occupied by the brighterpre-main-sequence stars (PMS) in Cha I. The distance to this newassociation is estimated at ~ 100 pc, sensibly smaller than the 150 pcgenerally assumed for the SFR. This yields an upper limit of 2 km s(-1)for the velocity dispersion of this new kinematic group. The de-reddenedCM diagram of the group members suggest the WTT stars are still PMSobjects, but older (3-30 Myr) and less massive than previousdeterminations. These revised age estimates, the newly derived grouppeculiar velocity, and current distance estimates to the Cha I/II/IIIcomplex would favour in-situ formation against that predicted by highvelocity cloud models. Finally, based on a redetermination of thepeculiar motions of stars and gas, we speculate that the whole SFRoriginated from the local Orion spur as a result of more classicalmechanisms like interactions with the spiral arms. Based on observationscollected at the European Southern Observatory (Chile) and on data fromthe Hipparcos astrometry satellite. Table~1 is available only inelectronic form at the CDS via anonymous ftp at 130.79.128.5.
| Searching for old neutron stars with ROSAT. II. Soft X-ray sources in galactic dark clouds
This is the second in a series of three papers constraining the numberof detectable old neutron stars in the Galaxy. Here, I present thestatistical analysis of a sample of X-ray sources coincident with areasof dark clouds in the Galactic plane. I compare this sample with allsources in the ROSAT All-Sky Survey bright source catalog within 20(deg)of the Galactic plane. I present the results of an identificationprogram of a subset of sources that are compatible with a soft, thermalX-ray spectrum and an effective source temperature of less than 70eV.The three brightest sources in this sample form an intriguing subgroup.One of them is a previously identified candidate for an accretingneutron star. I identify the other two sources with hot white dwarfstars. I find no new accreting neutron star candidate in this sample.Based on this result, I derive an upper limit to the space density ofaccreting neutron stars in fields of Galactic dark clouds of ~ 2sr(-1)at a count rate >0.05s(-1) .
| A study of the Chamaeleon star forming region from the ROSAT all-sky survey. I. X-ray observations and optical identifications.
We present the observations of the ROSAT all-sky survey (RASS) in thedirection of the Chamaeleon cloud complex, as well as the spectroscopicidentifications of the detected X-ray sources. The main purpose of thisidentification program was the search for low mass pre-main sequencestars. Sixteen previously known PMS stars were detected with highconfidence by ROSAT. Eight are classical T Tauri stars and eight areweak-line T Tauri stars, Seventy-seven new weak-line T Tauri stars wereidentified on the basis of the presence of strong Li λ 6707absorption, spectral type later than F0 and chromospheric emission. Wegive coordinates and count rates of the X-ray sources, and presentoptical spectra and finding charts for the sources identified opticallyas new pre-main sequence stars. Optical UBV(RI)_c_ and near-infraredJHKLM photometry for this sample of stars is also provided. In addition,6 new dKe-dMe candidates are found among the RASS sources.
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Observation and Astrometry data
| Constellation: | Chamaleon |
| Right ascension: | 11h55m57.09s |
| Declination: | -77°00'30.3" |
| Apparent magnitude: | 8.6 |
| Distance: | 46.948 parsecs |
| Proper motion RA: | -44.4 |
| Proper motion Dec: | 3.5 |
| B-T magnitude: | 9.464 |
| V-T magnitude: | 8.672 |
Catalogs and designations:
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