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Algorithms
Apart from reading this page, you should also refer to the
EDR paper
, the
list of changes from the EDR to DR1
, the
changes from DR1 to DR2
, and,
what's new for DR3
. The
Data products
page contains an introduction on how to use the data.
Imaging
Spectroscopy
Magnitudes
Fiber
Model
cModel
Petrosian
PSF
Radial Profiles
Which magnitude should I use?
Classification & Morphology
Star/Galaxy Separation
Model Fits
Surface Brightnesses
Ellipticities
Adaptive Moments
Isophotal Quantities
Photometric processing flags
IMPORTANT!
Photometric flux calibration
Assessment of photometric calibration
Converting SDSS counts to SDSS (asinh) magnitudes
(and
vice versa
)
Converting SDSS to AB magnitudes
Converting SDSS asinh magnitudes to fluxes.
Astrometric calibration
Flat-field creation and quality
Sky measurement
Centroiding and psf determination (see
how to reconstruct the PSF at any position
).
Deblending
Resolve:
making sure an object from overlapping observations is only included in a catalogue once.
Creation of imaging masks
Target selection
Main Galaxy Sample
Luminous Red Galaxies (LRG)
Quasars
Stars
ROSAT All-Sky Survey sources
Serendipity
Tiling
(assigning fibers & plate centers)
Reduction of spectroscopic data
Extraction of 1d spectra
Wavelength calibration
Flux calibration:
spectrophotometry
Continuum fits and line measurements
Spectral type determination and redshift measurement
Cross-correlation templates
Velocity dispersion measurements
Last modified: Fri Mar 5 13:43:06 CST 2004
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