========================================================================== J/A+A/446/583 Journal of all RVs of eps Per primary (Libich+, 2006) The following files can be converted to FITS (extension .fit .fgz or .fiZ) table1.dat sources.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/A+A/446/583 ==========================================================================
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Beginning of ReadMe : J/A+A/446/583 Journal of all RVs of eps Per primary (Libich+, 2006) ================================================================================ The new orbital elements and properties of epsilon Persei Libich J., Harmanec P., Vondrak J., Yang S., Hadrava P., Aerts C., De Cat P., Koubsky P., Skoda P., Slechta M., Uytterhoeven K., Mathias P. <Astron. Astrophys. 446, 583 (2006)> =2006A&A...446..583L ================================================================================ ADC_Keywords: Binaries, spectroscopic ; Radial velocities Keywords: stars: binaries: early-type - stars: binaries: spectroscopic - Abstract: A detailed analysis of a large collection of electronic spectra from three observatories, together with radial velocities published earlier, were used to derive a new ephemeris and improved orbital elements for the eps Per binary. Observations covering a time interval of about 37000-days (101.3-years) can be reconciled with a constant orbital period of (14.0691+/-0.00004)-days. The high orbital eccentricity of 0.555+/-0.009 was also confirmed. New spectral observations confirm that there is a periodic variation of the systemic velocity. Together with new evidence from astrometric observations (also analyzed here), they confirm the existence of a third body in the system with an orbital period of about 9600-days (26.3-years), rather than 4156-days, as reported earlier. Application of the disentangling technique to the H alpha spectra with good S/N ratios did not allow detection of spectral lines of either the secondary or tertiary components. For plausible inclinations between 30 and 90 deg, the observed mass function implies a mass of the secondary M_2_=0.85-1.77M_sun_, if a primary mass is adopted of (13.5+/-2.0)M_sun_. Attempts to detect the third body via interferometric observations should continue in spite of this first negative result. Description: Radial velocities of epsilon Persei primary component are presented. They are from 15 various sources (observatories, instruments). The journal of data sources in details is in our paper, see Table 2. Each source is designated by number in column 3. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 03 57 51.2 +40 00 37 eps Per = ADS 2888 A ----------------------------------------------------------
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