WFCAM Catalogues


Document Number: VDF-SPE-IOA-00009-0001  Version 3


Author: Mike Irwin


Changes

The main changes from the previous versions of this document are: a slightly refined set of radii for the larger aperture sizes (the previous ones extended to an optimistically large final aperture which was similar size to the the background following algorithm ie. too big); a hopefully clearer definition of the aperture radii used; renaming and redefinition of the radius of the FWHM total flux estimator to avoid confusion with the aperture 3 flux; and additional descriptions of further header content mostly relating to derived Data Quality Control (DQC) information. Finally a note has been added describing the user-selectable parameters that determine how the software is run.


Preamble

The derived object catalogues are stored in multi-extension FITS files as FITS binary tables, one for each image extension with a dummy primary header unit. Each catalogue header contains a copy of the relevant telescope FITS header content in addition to detector-specific information.

Each detected object has an attached set of descriptors, forming the columns of the binary table and summarising derived position, shape and intensity information. During further processing stages ancilliary information such as the sky properties, seeing and so on are derived from the catalogues and stored in the FITS headers attached to each catalogue extension.

The catalogue format was derived from similar APM/SuperCOSMOS/INT WFC/CIRSI analysis which produced 32 4-byte parameters per detected object. This has been enhanced for WFCAM to an 80 4-byte parameter set to include extra parameters for flux estimation and error estimates.


The following tables cover the WFCAM standard and further processing pipeline output catalogues, where for simplicity all derived parameters are stored as floating point numbers even though some of them are more naturally integers.

Columns content description

No. ¯ Isophotal flux...... ¯ Description No.  Name  Description

1  Seq. no.   running number for ease of reference, in strict order of image detections
2  Isophotal flux   standard definition of summed flux within detection isophote, apart from
   detection filter is used to define pixel connectivity and hence which
   pixels to include. This helps to reduce edge effects for all isophotally
   derived parameters.
3  X coord   intensity-weighted isophotal centre-of-gravity in X
4  Error in X  estimate of centroid error
5  Y coord   intensity-weighted isophotal centre-of-gravity in Y
6  Error in Y  estimate of centroid error

7  Gaussian sigma   these are derived from the three general intensity-weighted second moments
8  Ellipticity   the equivalence between them and a generalised elliptical Gaussian
9  Position angle   distribution is used to derive Gaussian sigma = (sa2+sb2)1/2
   ellipticity = 1.0-sa/sb
   position angle = angle of ellipse major axis wrt x axis

10  Areal profile 1   number of pixels above a series of threshold levels relative to local sky.
11  Areal profile 2   levels are set at T, 2T, 4T, 8T ... 128T where T is the threshold. These
12  Areal profile 3   can be thought of as a sort of poor man's radial profile. Note that for now
13  Areal profile 4   deblended, i.e. overlapping images, only the first areal profile is computed
14  Areal profile 5   and the rest are set to -1 flagging the difficulty of computing accurate
15  Areal profile 6   profiles.
16  Areal profile 7  
17  Areal profile 8  for blended images this parameter is used to flag the start of the sequence
  of the deblended components by setting the first in the sequence to 0

18  Peak height   in counts relative to local value of sky - also zeroth order aperture flux
19  Error in pkht  

20  Aperture flux 1   These are a series of different radii soft-edged apertures designed to
   adequately sample the curve-of-growth of the majority of images and to
   provide fixed-sized aperture fluxes for all images. The scale size for
   these apertures is selected by defining a scale radius < FWHM >
   for site+instrument. In the case of WFCAM this ``core'' radius (rcore) has
   been fixed at 1.0 arcsec for convenience in inter-comparison with other
   datasets. A 1.0 arcsec radius is equivalent to 2.5 pixels for non-interleaved
   data, 5.0 pixels for 2x2 interleaved data, and 7.5 pixels for 3x3 interleaved
   data. In 1 arcsec seeing an rcore-radius aperture contains roughly
   2/3 of the total flux of stellar images. [In general the rcore parameter
   is user specifiable and hence is recorded in the output catalogue FITS
   header.]
   The aperture fluxes are sky-corrected integrals (summations) with a
   soft-edge (ie. pro-rata flux division for boundary pixels). However,
   for overlapping images they are more subtle than this since they are in
   practice simultaneously fitted top-hat functions, to minimise the effects
   of crowding. Images external to the blend are also flagged and not
   included in the large radius summations.
21  Error in flux  
22  Aperture flux 2  
23  Error in flux  
24  Aperture flux 3   Recommended if a single number is required to represent the flux for ALL
25  Error in flux  images - this aperture has a radius of rcore.
26  Aperture flux 4  
27  Error in flux   Starting with parameter 20 the radii are:
   1/2× rcore, 1/2× rcore, rcore, 2× rcore, 2× rcore,
   22× rcore, 4× rcore, 5× rcore, 6× rcore, 7× rcore,
28  Aperture flux 5  8× rcore, 10× rcore, 12× rcore
29  Error in flux  

30  Aperture flux 6  Note 4× rcore, ensures ~ 99% of PSF flux
31  Error in flux  
32  Aperture flux 7  extras for generalised galaxy photometry further spaced
33  Error in flux  
34  Aperture flux 8  in radius to ensure reasonable sampling further out.
35  Error in flux  
36  Aperture flux 9  
37  Error in flux  
38  Aperture flux 10  Note these are all corrected for pixels from overlapping neighbouring images
39  Error in flux  
40  Aperture flux 11  
41  Error in flux  
42  Aperture flux 12  
43  Error in flux  
44  Aperture flux 13  The biggest with radius 12× rcore ie. 24 arcsec diameter
45  Error in flux   The aperture fluxes can be combined with later-derived aperture
   corrections for general purpose photometry and together with parameter 18
   (the peak flux) give a simple curve-of-growth measurement which forms
   the basis of the morphological classification scheme


46  Petrosian radius  rp as defined in Yasuda et al. 2001 AJ 112 1104
47  Kron radius  rk as defined in Bertin and Arnouts 1996 A&A Supp 117 393
48  Hall radius  rh image scale radius eg. Hall & Mackay 1984 MNRAS 210 979
49  Petrosian flux  flux within circular aperture to k ×rp ; k = 2
50  Error in flux  
51  Kron flux  flux within circular aperture to k ×rk ; k = 2
52  Error in flux  
53  Hall flux  flux within circular aperture to k ×rh ; k = 5; alternative total flux
54  Error in flux  
55  Error bit flag  bit pattern listing various processing error flags

56  Sky level  local interpolated sky level from background tracker
57  Sky rms  local estimate of variation in sky level around image
58  Child/parent  flag for parent or part of deblended deconstruct
  (redundant since only deblended images are kept)

  The following are accreted after standard catalog generation

59  RA   RA and Dec explicitly put in columns for overlay programs that cannot,
60  Dec   in general, understand astrometric solution coefficients - note r*4
   storage precision accurate only to 50mas. Astrometry can
   be derived more precisely from WCS in header and XY in parameters 5 & 6

61  Classification   Flag indicating most probable morphological classification:
  eg. -1 stellar, +1 non-stellar, 0 noise, -2 borderline stellar, -9 saturated
62  Statistic   An equivalent N(0,1) measure of how stellar-like an image is, used in
   deriving parameter 61 in a `necessary but not sufficient' sense.
   Derived mainly from the curve-of-growth of flux using the well-defined
   stellar locus as a function of magnitude as a benchmark
   (see Irwin et al. 1994 SPIE 5493 411 for more details).

  From the further processing pipeline after deriving a suitable PSF

63  PSF flux  fitted flux from PSF
64  Error in flux  
65  X coord  updated PSF-fitted X centre
66  Error in X coord  
67  Y coord  updated PSF-fitted Y centre
68  Error in Y coord  
69  PSF fit c2  standard normalised variance of fit
70  nPSF  no. of degrees of freedom for PSF fit

71  1D Sersic flux  fitted flux for Sersic profile
72  Scale length  scale factor of fit
73  Power index  power law index of fit
74  Error in fit  standard normalised variance of fit
75  nS1  no. of degrees of freedom for 1D Sersic fit
76  2D Sersic flux  fitted flux for PSF-deconvolved 2D Sersic fit
77  Scale length  scale factor of fit
78  Power index  power law index of fit
79  Error in fit  standard normalised variance of fit
80  nS2  no. of degrees of freedom for 1D Sersic fit

 [For numerical stability the Sersic fits will use the previously derived x-y coordinates]

Note:- a more formal mathematical definition of many of these parameters, together with a corresponding definition of the image processing steps is given in the VDFS Data Reduction Library Design document VIS-SPE-IOA-20000-0010, and references therein, available on
http://www.ast.cam.ac.uk/vdfs/docs/. Although this particular document is specific to VISTA, the formalism is generally applicable and the processing steps and catalogue parameters are expected to be almost identical.



Derived catalogue FITS header contents

Examples of extra FITS header items derived from the catalogues or during catalogue creation, one set for each extension.

SKYLEVEL=             91.8     / Median sky brightness (counts/pixel)     

An automatic 2D background-following algorithm is used to track and "remove" slowly varying background features such as image gradients etc.. The default scale size for background tracking (NBSIZE) is currently set to 64 pixels, coupled with a smidge of non-linear filtering this gives a background tracking scale of order 100 pixels. (A bilinear interpolator is used to generate pixel resolution background maps internally).

SKYNOISE=              6.0     / Pixel noise at sky level (counts)           

Robust MAD estimator for noise scaled to equivalent Gaussian rms value ie. = MAD x 1.48 after removing large scale sky background variations. MAD = Median of the Absolute Deviations about the median

THRESHOL=              9.0     / Isophotal analysis threshold (counts)   

User-selectable parameter, the default is to set this to 1.5 skynoise as a compromise between detecting close to the limit of the data and not being swamped by spurious sources. It is possible to push the data limit fainter but at the expense of a large increase in spurious sources. LSBG detection requires a more subtle add-on to the catalogue and could be added given suitable demand.

MINPIX  =                4     / Minimum size for images (pixels)       

User-selectable parameter, in conjunction with the threshold above this determines how deep and how small ``real'' images can be. This default precludes many of the few pixel-hit cosmic rays from being considered since ``real'' images must have 4 contiguous simply-connected pixels in the union of the detection filter and data domains. For more details on image detection and parametersiation see the papers in http://www.ast.cam.ac.uk/vdfs/publications.html .

CROWDED =                1     / Crowded field analysis flag (0 none, 1 active)

User-selectable parameter, detection algorithm tried to disentangle overlapping images or images supperposed on the ``slowly'' varying background of other large images (default) otherwise just straighforward isophotal detection.

RCORE   =             3.50     / Core radius for default profile fit (pixels) 

User-selectable parameter, aperture flux designed to match median seeing of survey data. It is straighforward to show that if rcore = FWHM then for typical profiles encountered the rcore flux estimate has between 80-90idealised perfectly known PSF model method.

SEEING  =             2.95     / Average FWHM (pixels)                     

An average realistic FWHM estimated directly from the stellar images on the frame. Mutiply by pixel scale size to convert to arcsec (eg. *0.400 WFCAM; *0.333 INT WFC).

ELLIPTIC=             0.04     / Average stellar ellipticity (1-b/a)          

A direct estimate of the average stellar ellipticity, useful for spotting trailed frames usw.. Should not average much above 0.15 for "normal" frames.

CLASSIFD=                    T / Classified 

Has image morphological classifier been run ? if so an object classification flag and a stellarness index is included in the binary table columns.

SATURATE=          41593.8     / Average saturation level in frame            

An estimate directly from saturated images on the frame at what level image saturation occurs, including sky. This varies from detector to detector depending on the relative gains applied to bring them to a uniform flatfield reponse etc..

Photometric Information

APCORPK =            2.812     / Stellar aperture correction - peak height    
APCOR1  =            0.635     / Stellar aperture correction - core1 flux      
APCOR2  =            0.114     / Stellar aperture correction - core2 flux      
APCOR3  =            0.028     / Stellar aperture correction - core3 flux      
APCOR4  =            0.000     / Stellar aperture correction - core4 flux      
APCOR5  =            0.000     / Stellar aperture correction - core5 flux      
APCOR6  =            0.000     / Stellar aperture correction - core6 flux      
APCOR7  =            0.000     / Stellar aperture correction - core7 flux      

Aperture corrections in magnitudes needed to correct the assorted aperture-like measures produced in the catalogues onto the equivalent of a total flux stellar system. These constitute the components of a curve-of-growth analysis contained within the catalogues with radii defined in the previous table; t o be used in the sense that
corrected photometry = 2.5*log10(flux) + apcor
(1)
They also work well as a first order seeing correction for faint galaxies. Larger aperture corrections are not included.

The remaining information necessary for photometric calibration may also be included in the following keywords:-

PERCORR =              -0.006  / Sky calibration correction (mags)             

this is a correction based on the median dark sky recorded in science frames compared to the median for all the detectors and as such is an ancillary correction to the gain correction derived from the flatfield (usually twilight flats) data. This correction is to be used in the same sense as before in that
corrected photometry = 2.5*log10(flux) + apcor + percorr
(2)

MAGZPT  =               22.10  / Photometric ZP (mags) for default extinction  

Derived detector zero-point in the sense of what magnitude object gives a total (corrected) flux of 1 count/s. These ZPs are appropriate for generating magnitudes in the natural detector+filter system based on Vega, see http://www.ast.cam.ac.uk/vdfs/docs/reports/ for more details on colour equations etc.. The ZPs have been derived from a robust average of all photometric standards observed on any particular set of frames, corrected for airmass but assuming the default extinction values listed later. For other airmass or other values of the extinction use
ZP ZP - [sec(z)-1]*extinct + extinct default - extinct
(3)

You can then make use of any of the assorted flux estimators to produce magnitudes via


Mag = ZP - 2.5*log10(flux/exptime) - apcor - percorr
(4)

Note that for the so-called total and isophotal flux options it is not possible to have a single-valued aperture correction

MAGZRR  =                0.15  / Photometric ZP error (mags)                   

error in the zero point. If good photometric night this error will be at the level of a few percent. Values of 0.05 and above indicate correspondingly non-photometric night and worse. [Currently set to -1 for WFCAM data.]

EXTINCT =                0.05  / Default extinction in passband

for WFCAM these are currently set to a constant clear night level, which within the current measuring error is the same for all passbands. Note that the frame-by-frame derived ZP from 2MASS automatically corrects for extinction variations, assuming they are uniform across the field of view.

To compute approximate errors in the fluxes you can also use the following:-


error2 = flux/gain + npixels*skynoise2
(5)

where npixels is either the effective area ie. p*rcore2 for the ``core'' measures or the no. of pixels above the detection isophote ie. areal profile1; gain is the final overall detector system gain. (see http://www.ast.cam.ac.uk/vdfs/docs/reports/sv for values); flux is whichever measure you are using but note that for ``total'' this formula is not accurate since ``total'' fluxes are derived using a rather convoluted curve-of-growth technique; average skynoise can be obtained from the catalogue fits header.

Astrometric Information

For a description of the World Coordinate System (WCS) see Calabretta & Greisen 2002 A&A 395 1077 and Greisen & Calabretta 2002 A&A 395 1061.

CTYPE1  = 'RA---ZPN'           / Zenithal polynomial projection 
CTYPE2  = 'DEC--ZPN'           / Zenithal polynomial projection 

CRPIX1  =              2999.40 / Reference pixel X on axis 1
CRPIX2  =              -940.32 / Reference pixel Y on axis 2

CRVAL1  =         112.45449231 / [deg] Right ascension at the reference pixel
CRVAL2  =          30.07196251 / [deg] Declination at the reference pixel     
CRUNIT1 = 'deg     '           / Unit of right ascension co-ordinates          
CRUNIT2 = 'deg     '           / Unit of declination co-ordinates              

CD1_1   =      -7.11999928E-08 / Transformation matrix element                
CD1_2   =       1.11427136E-04 / Transformation matrix element                
CD2_1   =       1.11433289E-04 / Transformation matrix element                 
CD2_2   =      -1.73270884E-07 / Transformation matrix element                

PV2_1   =                  1.0 / Pol.coeff. for pixel -> celestial coord       
PV2_3   =                -50.0 / Pol.coeff. for pixel -> celestial coord       
PROJP1  =                  1.0 / Old style ZPN projection keyword r term      
PROJP3  =                -50.0 / Old style ZPN projection keyword r**3 term   

NUMBRMS =                   87 / Number of standards used                     
STDCRMS =                0.089 / Astrometric fit error (arcsec)               




File translated from TEX by TTH, version 3.00.
On 4 Feb 2006, 17:23.