Find here an overview of the spectral plots. This target is a telluric
standard star.
All spectra have been taken with the same instrumental parameters as the NGSL targets.
SPECTRA: This column links to full views with 30 or 50 A panels of the co-added spectra
(available also under "2| Detailed spectra").
RANGE: wavelength range of the spectra in A.
SETUP: CCD and central wavelength [in nm]. BLU stands for the blue
CCD, REDL is the lower RED, REDU the upper red CCD.
OB ID: Observing Block (OB) number. Each target has normally been
observed in two OBs, covering the whole wavelength range.
FILE: name of the product file plotted here ('_rvc' indicating that
pipeline products have been fluxed, averaged, and RV correct
ed).
HDR: header of first parent raw file.
N: number of single exposures co-added for the final spectrum.
EXPT: exposure time in seconds for single exposure.
TEXP: exposure time in seconds for co-added product (as
displayed here).
SLITW: slit width in arcsecs.
SEEING: Averaged DIMM seeing value from begin and end of first
exposure. n/a: no data available. An asterisk marks values
applicable for begin or end of exposure only.
AIRM: Averaged airmass value from begin and end of first
exposure.
RV_helio: Heliocentric radial velocity correction, in km/s. NOTE:
The telluric spectra are *not* RV corrected.
RV_shift: Radial velocity correction in km/s. NOTE: The telluric spectra are *not* RV corrected.
comm.: any comment.
The spectral plots above 5810 A have telluric lines marked by blue vertical bars. These lines have been identified from
the reference spectra. The line catalogue is limited in sensitivity by the S/N of these data. The telluric line list
plotted here is also the reference for all other spectral plots.
Catalog of telluric lines: 580U | 860L | 860U
The panel plots have flux in physical units, 1e-13 erg/s/cm**2/A. Data are
corrected for atmospheric extinction. The abscissa is in Angstroem.
The flux scale has been fine-tuned to minimize steps between setups. These are
likely to be due to slit losses.
Corrections have been anything between negligible and considerable, depending on the seeing during the exposures.
There have been cases with seeing much better than the slit width, but also cases with a considerable fraction of flux lost due to bad
seeing. Check columns 'SLITW' and 'SEEING'.
For details about the flux calibration with the UVES pipeline check out here.
The overview plot has
- the full spectrum (rebinned to 5 A) on top ('overview');
- a signal/noise plot based on the ratio spectrum/errorbar (the errorbar
spectrum as delivered by the pipeline) properly scaled by the number of
averaged spectra.
