V. Catalog Generation
2. Tile Selection
The 2MASS Second Incremental Release contains source and image
data drawn from observations of 27,493 Tiles, covering an area of
19,681 sq.deg. (~47%) of the sky.
The selection of Tiles for the Release uses the
the overall scan "quality" assigned during the
Quality Assurance process (cf. IV.10),
and several other criteria described in the following sections.
Tiles selected to be candidates for the Release
were those that were pipeline processed as of 1999 June 1, the date
Catalog Generation for the Release began. This includes dates
in the following range:
This period included 329 northern and 239 southern
nights that have at least one photometric period.
Tiles in the date ranges described above that were assigned
a photometric quality of 0.5 were candidates for the
Release. As described in IV.10, the photometric
quality is a combination of the photometric calibration assessment
for a night and the photometric sensitivity
based upon the measured average seeing and background conditions during
the observation.
While the overall photometric quality factor assigned a Tile
is a complex combination of parameters, a quality 0.5
usually indicates that the following conditions were met:
Candidate Tile observations for the Second Incremental Release
were required to have a measured average seeing FWHM
3.5´´.
Seeing conditions worse than this value generally lead to poor
photometric sensitivity and begin to compromise the completeness
achieved when trying to discriminate between small, faint extended
and stellar sources.
Candidate Tiles for the Second Incremental Release
can have no more than three Atlas Images in which the residual background
noise in the H-band exceeds the 5- noise
level predicted for the observed mean background level and source density.
A significant challenge to accurate H-band photometry of extended
sources in 2MASS processing is residual structure in the measured
sky background due to atmospheric OH airglow emission. When the
airglow emission varies on spatial scales smaller than
the scale over which the extended source processing
attempts to fit the Atlas Image backgrounds
(cf. IV.5),
the resulting background estimate and photometry will be compromised.
The
expected noise in a 2MASS Atlas Image can be predicted from
the detector characteristics, mean background illumination
and source density (confusion noise). A single 2MASS Atlas Image
can have post-fit residual noise levels larger than the predicted
values due to the presence of bright stars or galaxies. However,
empirical analysis has shown that when more than three Images
in a Tile have H-band residual noise greater than the predicted
level, the origin is invariably strong small-scale structure
in the airglow emission.
A number of Tiles have been observed more than once during
the course of Survey operations for engineering or validation purposes.
For the Release Catalogs, a single observation of each Tile is selected
for inclusion. The observation of a Tile that has the
best assessed quality, considering photometric accuracy, background
and seeing conditions, was selected for the Release.
All Tiles included in the 2MASS Second Incremental Release
must be part of a block of at least three RA-contiguous Tiles.
Blocks of one or two isolated Tiles will be included in later
releases when surrounding Tiles are available.
The achieved accuracy of 2MASS position reconstruction
(cf. IV.6) depends on the number
and distribution of ACT astrometric reference stars in each Tile.
In Tiles that contain very few or poorly distributed reference stars, the
astrometric solution can wander off the reference frame.
The global consistency of the astrometric solution for a particular
Tile relative to surrounding Tiles, that contain different
reference stars, is gauged by examining the repeatability of
positions of sources in Tile overlap regions. The positional
uncertainties quoted in the PSC are adjusted to reflect the global
consistency of
the astrometric solutions; sources in "ACT-challenged" Tiles
have larger uncertainties than those in Tiles with many and/or
well-distributed reference stars.
The three-contiguous Tile requirement is driven by the need
for accurate assessment of the astrometric uncertainties.
No Tiles in the declination bands closest to the equatorial poles
(|dec| > 84°) are included in the Second Incremental Data Release.
[Last Update: 14 February 2000, by R. Cutri and T. Chester]
a. Date Range
b. Photometric Quality
c. Average Seeing
d. Residual Background Structure
e. Multiple Tile Observations
f. Tile Contiguity
g. Other area considerations
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