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Astron. Astrophys. 336, 637-647 (1998)

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2. Spectroscopic data

2.1. Optical and near IR spectroscopy

We have monitored BX Mon regularly with the CAT [FORMULA] 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 [FORMULA] and cover a spectral interval of [FORMULA]. Spectra centered at [FORMULA] have a resolution [FORMULA] and cover [FORMULA]. 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]

Table 1. Log of our ESO high resolution spectroscopy of BX Mon redwards of [FORMULA]. We give the orbital phase [FORMULA] (Eq. 1), the central wavelength [FORMULA], the heliocentric radial velocity derived from absorption lines, [FORMULA], the H[FORMULA] emission line equivalent width, [FORMULA] and the line flux [FORMULA] (in scaled units, see Sect. 7.1).
Notes:
[FORMULA] Observation from Van Winckel et al. (1993)
[FORMULA] Low signal to noise



[TABLE]

Table 2. Log of our ESO high resolution observations of BX Mon bluewards of [FORMULA]. We give the orbital phase [FORMULA] (Eq. 1), the central wavelength [FORMULA] and the heliocentric radial velocities from cross-correlation with an A-star spectrum, [FORMULA], and with an M-star spectrum, [FORMULA].
Notes:
[FORMULA] Observation from Van Winckel et al. (1993)
[FORMULA] No measurable absorption lines from the hot component


For the purpose of spectral classification we took a near IR spectrum with [FORMULA], covering the range [FORMULA] on March 15, 1992 with the ESO [FORMULA] 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]

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 [[FORMULA]] in the two intervals [FORMULA] from 1800 to 1880 Å and [FORMULA] from 3010 to 3090 Å , which are free of strong emission lines.
Notes:
[FORMULA] No reliable FES value available (scattered light)


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© European Southern Observatory (ESO) 1998

Online publication: July 20, 1998
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