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Astron. Astrophys. 357, 951-956 (2000)

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2. Observations

HST observed RW Aur on 10 August 1993 (Program 3845) in 3 spectral bands with the Goddard High Resolution Spectrograph in medium resolution mode and Detector 2. Wavelength calibration lamp was used in nearly the same spectral bands. The start time of each observation, Archive Dataset name, grating designation, observed spectral band and number of independent exposures (RPTOBS+1 parameter) are presented in Table 1. The analyzed spectra were adopted from HST Archive, recalibrated using the most up-to-date reference files and processed with IRAF v2.11 and STSDAS/TABLES v2.0.2 software as recommended in Chap. 36 of "HST Data Handbook".


Table 1. Log of HST Program 3845 on 10 august 1993

The standard "pipeline" wavelength calibration was improved by using the STSDAS waveoff task and respective W_CAL observations - see Table 1. All wavelengths are corrected for the orbital motion of the HST and the Earth (i.e. they are heliocentric) and are presented for vacuum if [FORMULA] Å and for air otherwise. The Van Hoof (1999)electronic database was used to identify lines in RW Aur spectra. To improve the signal-to-noise (S/N) ratio we combined all independent exposures for each spectral band and additionally smoothed them via a 4-point running mean, so the resulting spectral resolution is near 15 km s-1. The five gaps in Figs. 1-3 are due to the "dead" diodes of the Detector 2.

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© European Southern Observatory (ESO) 2000

Online publication: June 5, 2000