DR6 Release - October 13th 2009 (GPS added Jan 8th 2010)
DR6 does not currently contain UDS detection/source data.
Please see UKIDSSDR5PLUS for UDS data.
The charts linked below show the status of the UKIDSS surveys in this
release. This 6th release, like the DR5plus release, only contains one
database, UKIDSSDR6plus, which contains all the data, i.e. includes
data from fields
that have incomplete waveband coverage as prescribed by a given survey.
The WSA DR6plus release contains views of the survey source tables that allow
users to easily target their queries at only those areas that have complete
waveband coverage. The names of the source table views are
lasYJHKsource, gpsJHKsource, gcsZYJHKsource and
dxsJKsource. These names reflect the required waveband coverage.
They appear in the schema browser under
both the table and view sections. The UDS being only one field that now has
coverage in J, H and K does not require a view.
A description of the data and how it is held in the archive is given in the
DR6 Release Summary
||No. of multiframes
||No. of objects in
|No. of sources in
||Y=20.2, J=19.6, H=18.8, K=18.2
||J=19.8, H=19.0, K=18.1
||Z=20.4, Y=20.1, J=19.6, H=18.8, K=18.2
New in DR6:
Particular attention should be given to any notes detailing limitations
and known issues - see below,
known issues and
The deblending error for extended source photometry described in known issues has now been fixed.
The LAS now has second-epoch observations in the J filter in some fields. The
detections from both epochs are merged into the
lasSource table using attributes J_1 and J_2.
The DXS has some new attributes in the dxsVariability table: jMinMag, jMaxMag,
jNGt3sig, etc, which give the minimum and maximum magnitude of the individual
observations of a source and the number of observations that are more than
3 standard deviations from the mean. These are calculated for each filter. In
the dxsVarFrameSetInfo table, the attributes aStrat, bStrat and cStrat which
gave the parameters for the best fit to the photometric noise as a function
of magnitude have been replaced by aStratPht, bStratPht and cStratPht and the
equivalent attributes for the astrometric noise (aStratAst, bStratAst,
cStratAst) have been added. However, the astrometric fit has not yet been
calculated, so the astrometric noise attributes are set to defaults.
The DXS deep stacks have been processed with the correct smoothing function
at the time of extraction, resulting in fewer false detections at the faint
Data from intermediate stacks with one or more deprecated extensions are now
used in the stacking. These extensions are given a weighting of 0 during
stacking. The totalExpTime attribute in MultiframeDetector is calculated on an
extension by extension basis and takes into account missing exposure from
If there is only one observation of a DXS field in a particular pointing and
band, then a deep stack is no longer created, and the intermediate stack is
used in the dxsMergeLog table instead. We have added the productID and
releaseNum attributes to ProgrammeFrame to track which deep or intermediate
stacks correspond to which product in RequiredStack.
WFAU, Institute for Astronomy,
Royal Observatory, Blackford Hill
Edinburgh, EH9 3HJ, UK