2. Spectroscopic data
2.1. Optical and near IR spectroscopy
We have monitored BX Mon regularly with the CAT telescope and the Coudé Echelle spectrograph (CES) at the ESO observatory at La Silla, Chile. The observations were carried out remotely from Garching, Germany. The optical spectra were taken with a resolution and cover a spectral interval of . Spectra centered at have a resolution and cover . We complement our data with observations by van Winckel et al. (1993) who used the same telescope and instrument. A log of our optical observations is given in Table 1 and Table 2. The details of the CAT observations and data reduction are as described in Schmid et al. (1998, Paper III).
Table 1. Log of our ESO high resolution spectroscopy of BX Mon redwards of . We give the orbital phase (Eq. 1), the central wavelength , the heliocentric radial velocity derived from absorption lines, , the H emission line equivalent width, and the line flux (in scaled units, see Sect. 7.1).
Table 2. Log of our ESO high resolution observations of BX Mon bluewards of . We give the orbital phase (Eq. 1), the central wavelength and the heliocentric radial velocities from cross-correlation with an A-star spectrum, , and with an M-star spectrum, .
For the purpose of spectral classification we took a near IR spectrum with , covering the range on March 15, 1992 with the ESO telescope. For a description of this observation see Mürset & Schmid (1998).
2.2. UV data
We retrieved all the available low resolution IUE spectra of BX Mon from the final IUE archive. A log of the IUE observations is given in Table 3. The last entry in Table 3 refers to an observation, that suffered from scattered light caused by a problem with the IUE optics. The spectrum was corrected with the LWP 31623L sky exposure. No high resolution spectra of BX Mon have been taken by IUE.
Table 3. Log of IUE spectra of BX Mon. We give the orbital phase (Eq. 1), archive number, FES-magnitude and the integrated observed flux in  in the two intervals from 1800 to 1880 Å and from 3010 to 3090 Å , which are free of strong emission lines.
© European Southern Observatory (ESO) 1998
Online publication: July 20, 1998