The 2QZ is affected by incompleteness is a number of different ways.
These are discussed in detail by Croom
et al (2003) (Paper XII). Here we outline these completeness issues
and supply the data and software required to make these corrections.
We define four separate causes of incompleteness which are:
We discuss each of these in turn below. In several cases we specify
completeness on a sector-by-sector basis where a sector is as a unique
area defined by the interesection of a number of circular 2dF fields.
Morphological completeness. This describes our effectiveness
at differentiating between point sources and extended soruces on UKST plates,
and also the possible effect of the QSO host galaxies on morphology at
Photometric completeness. This attempts to take into account any
QSOs which may have fallen outside of our colour selection limits.
Coverage completeness (or coverage). We define the coverage
as a fraction of 2QZ catalogue sources which have spectroscopic observations.
Spectroscopic completeness. This is the fraction of 2QZ spectroscopic
observations which have the specified quality of spectrum (below we consider
quality 1 identifications).
This falls into two catagories. The first concerns objects that are
truly point sources but which have been mis-classified by the APM analysis
software. The fraction of sources missed in this fashion is found
The second form of incompleteness, due to the effect of the AGN host
galaxies is much harder to model, however we note that even the largest
host galaxies (re~10 kpc) will have angular sizes of less that
2 arcsec at z>0.4. So at redshifts above z~0.4 we do not expect this
to be an important issue. Due to the uncertainty in the properties
of the host galaxies we choose not to make any specific correction for
incompleteness due to this affect.
We derive the incompleteness due to QSOs moving out of our colour selection
boundaries using a semi-empirical model which makes use of the mean colours
of QSOs as a function of redshift and the measured dispersion in colour
of the 2QZ QSOs. Full details are given in Croom
et al (2003) (Paper XII).
The resulting completeness map is a function of redshift and apparent
bJ magnitude and is shown below:
The photometric completeness countours are plotted at 10 percent (solid
lines) and 5 percent (dotted lines) intervals. This completeness
map is given in tabular form here.
A fortran program to read in the array
and calculate completeness values is also provided.
The coverage is defined as the fraction of 2QZ targets that were observed
spectroscopically. A map of this, pixelized on a scale of 1 arcmin
is available, as is the code required to produce the map (mask_mask.f).
The full coverage maps for the two 2QZ survey strips are shown below (top
NGP; bottom SGP):
Spectroscopic completeness is a function of both area, magnitude and redshift.
We first define the spectroscopic completeness across the 2QZ strips using
a similar pixelized map to the coverage map above. This is also generated
by the make_mask.f code. The combined
coverage and spectroscopic completeness mask for the two stips is shown
Spectroscopic completeness is also a function of magnitude, being lower
at the faintest apparent magnitudes observed. In a given sector the
magnitude dependent spectroscopic completeness is by:
Where A=20.388+-0.77 and B=-0.919+-0.052. fs(theta) is
the spectroscopic completeness as a function of angular position (i.e.
sector) described by the maps shown above. The combined spectroscopic
completeness is then
The ratio Nobs/Nest is also generated by the mask
making code make_mask.f.
Finally there is also a redshift dependent component to the completeness
such that full spectroscopic completeness is described by
The function R(z) is given in tabular form
in intervals on 0.1 in redshift, and can be found here.
We note that there are significant random errors on the calculation of
The above area masks are defined on a sector-by-sector basis and then pixelized
in 1x1 arcmin pixels. We provide both basic masks for the full catalogue
and the mask making software that will allow masks with varying completeness
thresholds to be made.
Originally the catalogue was defined in the the B1950 system.
Subsequently revised positions have been obtained in the J2000 system tied
to to the TYCHO-II reference frame. However, as all the field centres,
holes and plate edges are defined in the B1950 system it makes sense to
derive the completeness masks in this system also. For this reason
the final released catalogue contains both B1950 and J2000 coordinates.
The maps for the full catalogue (without any cut in sector completeness)
are available below. We have three separate mask files, containing
the coverage completeness (the fraction of objects observed), the spectroscopic
completeness (the fraction of observed objects with good IDs) and an estimate
of the Nobs/Nest ratio described in the equations
above. They are all in the same format, with the resulting masks
being pixelized in 1'x1' bins (4510x320 pixels).
The files containing the masks contain six lines of header information:
||centre of the first array element in RA (degrees)
||centre of the first array element in Dec (degrees)
||number of RA pixels
||number of Dec pixels
||RA step size (degrees)
||Dec step size (degrees)
The remainder of the file contains a 4510x320 real*4 array. There
are two versions available, both written out as FORTRAN arrays. The
first is an unformatted FORTRAN file that can be read using the following:
Alternatively, there is a text file which can be read using:
There are separate coverage maps for the NGP (or equatorial) and SGP
strips. Because the original 2QZ catalogue selection was based
on B1950 coordinates, the maps are specified in B1950 coordinates:
NGP coverage map (B1950): unformatted
SGP coverage map (B1950): unformatted
NGP completeness map (B1950): unformatted
SGP completeness map (B1950): unformatted
NGP Nobs/Nest ratio map (B1950): unformatted
SGP Nobs/Nest ratio map (B1950): unformatted
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The 2QZ team (July 2003)