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MOS Data Reduction
Michael BaloghUniversity of Durham
Outline
1. (Automatic) identification of slits and galaxies2. Distortion correction3. Background subtraction4. Wavelength calibration5. Flat fields and flux calibration
Data Reduction software
1. IRAF: Can deal with multiobject spectroscopy, but handles the following inelegantly:
• wavelength calibration• distortion corrections
2. Dan Kelson’s recently public software: http://www.ociw.edu/~kelson/
• designed for use with MOS data• handles wavelength calibration and distortion corrections
easily• Employs new technique for optimal background subtraction• But is somewhat obscure
Note: neither software package deals easily with ultraplex data
MOS data: the spectra
MOS data: flats
MOS data: arc lamps
Ultraplex data
Identification of Objects
Identification of Objects: IRAF
Interactively identify object(s) in each slit
Specify extent to extract in 1D spectrum
Can be tricky for faint spectra because optimal columns to extract will vary from slit to slit (in some cases will hit bright sky lines, in other cases miss bright part of spectrum)
Identification of Objects: IRAF
Kelson 2003
Identify slits in flat field image
Laplacian filter helps define slit edges
Pick object location on 2D image (using ds9, for example)
Identification of Objects: Kelson
Distortion correction
Spectra are usually curved, due to instrument distortions
NIRSPEC: Kelson 2003
Distortion correction
Two options:1. Rectify image before extracting spectra. Makes reduction easier, but introduces residuals in sky subtraction.
2. Measure distortion, but extract spectra from original frame and map to rectified coordinate frame.
Distortion correction: IRAF
d dCurvature in spatial direction is tricky to correct; not easily implemented.
Curvature in spectral direction can be traced when extracting spectrum. Must be done interactively and probably not used when extracting arc spectrum
Need to be able to see the spectrum…
Distortion Corrections: Kelson
1. Trace slits in flat field to map distortion in spectral direction
2. For each slit, trace sky lines (or arc lines) to map distortion in spatial direction
Kelson 2003
Background Correction
Background CorrectionUsual procedure:
Define backgroundregion on either side of object
Fit polynomial across dispersion
Assumes no distortion in spatial direction, so must correct first
Background CorrectionRebinning: introduces correlated noise, smears bad pixels, produces artifacts/residuals, and forces sky spectrum to have common pixelization
Instead: perform least-squares fit to sky spectrum in original coordinates. This provides better sampling in rectified coordinates.
Kelson, PASP, in press
Background CorrectionRebinning: introduces correlated noise, smears bad pixels, produces artifacts/residuals, and forces sky spectrum to have common pixelization
Instead: perform least-squares fit to sky spectrum in original coordinates. This provides better sampling in rectified coordinates.
Kelson, PASP, in press
Background Subtraction
2D LRIS spectrum
Spectrum profile in rectified coordinates
Compare smoothed version of above with profile from single pixel width
Kelson, PASP in press
Background Correction
1. Define sky regions (either directly, or using -clipping techniques)
2. Fit bivariate B-spline (Dierckx 1993) as a function of rectified coordinates
• Essentially approximates an interpolating spline along the wavelength coordinate, but with much finer sampling than available in a single CCD row
3. Can generalize further and fit simultaneously to all spectra in a frame. Thus get improved resolution even if distortions are small.
Kelson, PASP, in press
Kelson, PASP, in press
LRIS Raw
Sky model
Backgroundsubtracted
rms-smoothed,divided by noise: no residuals!
Kelson, PASP, in press
NIRSPEC Raw
Sky model
Backgroundsubtracted
rms-smoothed,divided by noise: no residuals!
Wavelength calibration
Extract arc lamp spectrum for each slit
IRAF: identify a few lines and fit low-order function.
Then easy to use this fit to find more lines and improve quality of the fit.
Task reidentify to find arc lines in other slits on same image does not work well. Usually have to do each slit separately.
Not clear to me if this uses trace information from spectrum.
Wavelength calibration I
Wavelength calibration II
Kelson (2003) softwareAutomatically identify lines in all slits, and computes pixel-wavelength transformation
Don’t know how it works, but it does! Can do in minutes what used to take me days with IRAF.
Flat fielding
Flat fielding
1. Remove the “slit function”: variation in sensitivity along the slit
Needed to correct for uneven slits
Flat fielding
2. Remove the “blaze”: variation in sensitivity in dispersion direction
Needed for flux calibration, unless star observed in every slit
Flat fielding
3. Remove pixel-to-pixel sensitivity variations.
Usually introduces a lot of noise
Flux Calibration
1. Observe photometric standard through one (or more) slits
2. Reduce normally, and flat field (remove “blaze” function)
3. Divide by known spectral shape to get detector response as function of wavelength.
Conclusions
For LDSS2 spectra, I find both give similar quality results
IRAF Kelson
Advantages • Lots of documentation• Most parameters are easily understood and located
• For well-behaved data, wavelength calibrations and distortion corrections are easy• Potential for improved background subtraction• Allows easy production of 2-dimensional reduced images• Little interaction => fast processing
Disadvantages • Wavelength calibration and distortion corrections are difficult and time consuming• Cannot easily produce 2-D calibrated images
• Very little documentation• Non-trivial to install (uses Python, VTK, other software)