The UVES pipeline delivers extracted spectra which are debiased, flattened, background subtracted, wavelength calibrated and extracted. These data come in non-physical units ('quasi-ADU'), with their large-scale slope determined by the ratio of stellar and flat field spectral slopes. For line profile studies this is sufficient. If however an object has been observed in different setups and should ultimately be merged into one single result spectrum, it is very useful to have a correction for the instrument response slope.

A standard star measurement is processed by the pipeline into the flat-fielded, extracted and wavelength-calibrated result, p_std. This pipeline product can be further processed (which includes extinction correction, normalization for exposure time, binning and gain) into the normalized standard star spectrum, f_std. This divided into the tabulated flux, F_std, of the standard star, finally yields the response curve, R:

R = F_std/f_std

where F_std is in physical units (erg/[s cm**2 A]) and f_std is in quasi-ADU.

Having determined a reasonable response curve R, it can readily be used to flux-calibrate any point-source object spectrum, f_obj:

F_obj = f_obj*R.

The precision of the flux calibration is limited by

• the flattening process: standard star spectra and science object should have been reduced with the same or at least comparable flat field spectra;
• differences in extinction law between standard and science target;
• slit losses: usually the science target will be observed with a slit smaller than the standard stars (10 arcs).

The daily standard star measurements are processed by the UVES pipeline into response curves. These products (being delivered as UV_PRSP files) in principle measure the ratio (physical flux distribution/registered counts) per standard star but are not directly suitable for flux calibration. The typical output has very strong remnants of the flat-fielding process (order-scale ripples) and often a bad background subtraction (since data are typically taken in the twilight). Also the data have often very high signal and are poorly extracted by the optimum extraction routine.

Furthermore the pipeline-delivered response curves lack

• correction for exposure time
• correction for extinction
• correction for binning and gain.

Here is an example which illustrates some of these problems with pipeline-processed response curves. Curves have already been corrected for exposure time, extinction, binning and gain, and they have been selected from good nights only. The scans in the middle panel show the typical order ripples, and also the strong Balmer absorption series (here visible as quasi-emission feature). The upper panel shows the flux distribution taken from the standard star table (16 A bins in this example).

To overcome these problems and provide a set of UVES response curves useful for science flux calibration purposes, a set of properly selected input frames has been defined. Selection criteria were:

• low to moderate airmass
• night known to have been photometric
• suitable standard star spectrum (poor in features)

These have been used to create master response curves which are binned to 50 A resolution. This avoids the quality problems of the high-resolution versions, and at the same time the problems of spectral features in the standard star data. The lower panel in the above figure shows the selected and corrected response curves for the setting 437BLUE (blue curves). The red curve is the averaged master response curve.

The final master response curves have been edited in spectral regions with strong emission or absorption features. The underlying assumption is that the real instrument response varies only slowly over 50 A scales.

They come per standard setting wavelength (346, 390, 437; 564, 580, 860 REDL and REDU).  No distinction is made between dichroics and non-dichroics.

Download and view master response curves

Extracted UVES science data can be flux calibrated using these master response curves. Here is a short summary of the steps required:

• take the reduced science spectrum (pipeline product RED_SCIENCE_ccd where ccd is any of BLUE/REDL/REDU)
• read the EXPTIME keyword from reduced and have norm = reduced/EXPTIME
• read the CONAD keyword and apply gain correction: norm_conad = norm*CONAD
• read the BINX keyword; apply correction norm_bin = norm_conad/BINX
• read the AIRMASS keyword; create image file extinction from extinction file atmoexan.tfits, with same stepsize as norm; apply extinction correction as norm_exti = norm_bin*10**(0.4*extinction*AIRMASS)
• convert proper MASTER_RESPONSE into image file response (same step size as norm)
• apply flux correction as fluxed_science = norm_exti*response

The product fluxed_science comes in physical units [10**(-16) erg/s/cm**2/A] vs. A.

As a check for this procedure, we have selected spectra of a flux standard star, HR5501. These data have been measured in all standard settings in the same night (2002-02-09). For the purpose of this test, they have  been processed by the pipeline as SCIENCE spectra. The following figure shows the pipeline-delivered extracted flux (red settings 564/580/860 REDL and REDU CCDs) and the master response curves (top) for these settings. Setting 580 is plotted red, the others in black.

In the next figure, we see the flux calibrated spectra, i.e. the product of the extracted spectra and the master response curves. These spectra have physical units (10e-16 erg/s/cm**2/A). The tabulated fluxes, in the same units, are overplotted as blue dots. The upper panel has the residual fluxes (measured divided by tabulated). These never exceed 10% in continuum regions. Strong line features of course produce larger deviations. The systematic shifts come from  differences between the master response curve used here (derived as average from several different input curves), and the individual response curves for HR5501.

In conclusion, (i) the master response curves can be reasonably precisely constructed from day-to-day response curves, with the corrections described; (ii) these master response curves can be used in a straightforward way to flux-calibrate the science spectra.

Of course one has to keep in mind the reservations made above about flat field, extinction and slit losses. The flattening process should be critical as long as the proper time range has been selected. Slit losses are likely to be monochromatic if the ADC has been used.

This is a very promising result in view of the fact that UVES is not specifically designed to provide high-quality flux calibrations.