This tutorial provides information for the system efficiency Health Check monitoring. It is based on the measurement of QC1 parameters of STD_STAR calibration data once per night, weather and scheduling conditions allowing. Each STD_STAR OB makes a single observation of a spectrophotometric standard star in a specific instrument and wavelength setup, thus allowing evaluation of the instrument+telescope+atmosphere efficiency.
efficiency value at wave_c (QC1 database table uves_std, column max_effic)
This QC parameter is calculated by the QC report scripts, not by the pipeline.
Flux standard stars (STD) are observed on a regular basis with UVES on Paranal. Their purpose is to monitor the overall instrument efficiency (DQE; telescope+instrument+detectors) and to provide a measurement of the spectral response. They are taken with the slit width set to 5 or 10 arcseconds.
The flux standard table was delivered as part of the data package. It is also included in the calSelector data sets. It can be downloaded as flxstd.tfits.Z (576 kB). It is based on the ESO library of standard stars. The extinction table (also delivered) can be downloaded here.
Strategy for acquisition
Two kinds of standard star observations exist: daily measurements close to morning or evening twilight and long-term measurements during night-time.
Daily measurements: Standard stars are observed in three dichroic settings (346+580, 390+564, and 437+860, 1x1 binning), independently of the settings used for science observations during the night. These three dichroic settings are measured every night with science data. They are acquired close to twilight, with standards taken from a small set of stars with few spectral features. They are used for daily performance checks and as input to create master response curves for flux calibration of science spectra.
Long-term measurements: In addition, a dedicated set of standard stars is observed about twice a month during night-time under photometric and dark conditions and at low airmass. The reason for this strategy is to avoid the large intrinsic scatter (see below) of the daily measurements taken close to twilight. These measurements are used for long-term trending of the overall instrument efficiency.
QC1 parameters: chromatic efficiency
The pipeline processes the raw STD data (de-bias, flatten, average extraction), divides the flux table into the result and finally transforms into a fractional efficiency (where 0.1 means 10% of all incoming photons are registered on the CCD). The pipeline delivers an efficiency table (called UV_PEFC). Find more about the reduction of STD files here.
The efficiency table can be plotted, per order, over wavelength. The blaze wavelength of each order and the corresponding efficiency value there is written as QC1 parameter into the FITS header. The corresponding numbers for the central order are stored in the QC1 database uves_std as wave_c and max_effic (see here). The max_effic parameter is used for trending, assuming that all efficiency curves per setting are similar apart from a scaling factor. Their trending with time primarily reflects efficiency variations of instrument components.
The max_effic values for all standard settings are used to
The proper selection of input data is crucial. Accepting all max_effic values as produced by the pipeline creates a large scatter. Reasons for this are:
High-airmass data have the spectrum in the blue exposures shifted off-center which, especially in combination with a high sky level, brings the pipeline algorithm to assume an unrealistic background, with odd results for the efficiency. The same effect is observed under bad seeing since then the SKY level is unreliable as well. Stars with a rich absorption line spectrum tend to produce a larger scatter since max_effic is monochromatic.
See the current plots for the long-term trending of monochromatic efficiencies.
The UVES efficiency curve is monitored here.
The UVES pipeline produces response curves from STD calibration frames. Each exposure produces an individual response curve. Under ideal conditions (night is photometric, airmass is low, wide slit) each response curve provides a flux calibration for science data taken at the same setting and slit width.
Realistically, the individual response curves are not always of ideal quality. A careful selection of these curves would yield master response curves of better quality. For certain periods in the past, they were created. This set can be used for flux calibration of the reduced science data.
The careful selection of these curves turned out to be quite manpower intensive, and therefore it could not be supported in the long term. These curves only exist for the period between 2001-10-01 and 2004-11-30. Please also note that some of the following information is heritage information and comes without any claim for completeness.
Current response curves
With the upgrade of one of the red CCDs in 2009 it became obviously wrong to apply the old master reponse curves to the post-2009 UVES data.Unfortunately this was not immediately recognized on the QC side, and therefore the master response curves from 2004 were still applied for flux calibration until October 2011. Apart from the wrong usage of the response curve for the old red CCD, the application of the other two response curves for flux calibration was tolerable since the changes in the response curves are minor and slow.
With the termination of science processing the association of the response curves to the science data has been modified:
It is likely that chosing a response curve processed from a recent STD star exposure (i.e. a single one instead of a master one) is fully sufficient to obtain a reasonable flux calibration.
After 2005, master response curves have not been updated due to manpower constraints. They are expected to slowly evolve with time. The user may prefer to create, from STD star measurements, selected individual response curves around the date of the science observations and apply them for flux calibration. See also the link below.
To give an idea about the impact of the flux correction on the large-scale spectral slope, and about the precision that can be achieved, we have prepared a tutorial about flux calibration. Here you can also find a description of how to flux-calibrate your UVES data.