Before using the 2MASS extended mission 6x data products, users are strongly encouraged to familiarize themselves with the Cautionary Notes to the All-Sky Data Release data products in 1.6. The 2MASS 6x observations were made using the same facilities and the same basic strategy as the main survey, and the 6x data were reduced with a software pipeline very similar to that used for the main survey. Therefore, most of the characteristics and limitations associated with the All-Sky Release data products will apply to the 6x data products.
The sections below describe features and caveats that are unique to the 6x data products and highlight a few of the important features that are common to the 6x and main survey data products. These sections are intended to supplement the Cautionary Notes to the All-Sky Data Release but not to replace them.
Section A3.1.d.i presents general Cautionary Notes, and A3.1.d.ii,
A3.1.d.iii and A3.1.d.iv provide essential information for
the 6x point and extended source Working Databases, Catalogs
and Atlas Images, respectively.
i. General 6x Notes
Although the objective of the 2MASS Extended Mission is to produce Databases, Catalogs and an Image Atlases that meet the same standards of reliability and quality as those of the main survey, the 2MASS 6x data products have not received the same level of scrutiny as the All-Sky Release products. The 6x data were obtained with same well-characterized facilities as the main survey and reduced with essentially the same processing software that incorporates multiple levels of quality assurance. The 6x release data products were generated using similar criteria and best practices developed to produce the 2MASS All-Sky Catalogs and Image Atlas. However, the reliability of the 6x products has not been thoroughly validated. Consequently, users are encouraged to use the 6x databases, catalogs and images with care, and to follow these recommendations:
Unlike the main survey, 2MASS 6x observations covered only approximately 589 deg2 distributed among 30 different fields containing targets of astronomical interest (see Figure 1 in A3.2). Most of the 6x area is contained in two large regions covering the Large and Small Magellanic Clouds, in which 383 deg2 and 127 deg2 are surveyed, respectively. The remaining ~80 deg2 is in 28 fields, the largest of which is the Lockman Hole in which 28.3 deg2 were observed.
The 6x fields are made up of a set of predefined 6° and 1° long (in declination) tiles, analogous to those used for the main survey and survey calibration observations, respectively. Duplicate tile numbers were incorrectly assigned to several scans in the Chameleon 2 and Hydra 6x fields that did not cover the same region of sky. Therefore, caution should be used when selecting or searching for observations according to tile number in those fields. See the Chameleon 2 and Hydra field description pages linked to Figure 1 in A.3.2.b for details.
Within individual 6x fields, there may be gaps in coverage for two reasons. First, some tiles were not scanned because of scheduling considerations, or were not observed in photometric conditions. Second, a telescope commanding script error caused the starting position of some 1° 6x scans to be displaced in declination from their nominal locations. This resulted in coverage gaps between adjacent declination bands of tiles ranging from a few arcseconds to as much as 4°. The Lupus 6x field scan coverage map shown in Figure 1 illustrates gaps from both missing scans scan offsets at the declination boundary
Observations of the Chameleon II, Hydra Abell 754 and Abell 3420 6x fields were most severely affected by the 1°-scan starting point problem. Coverage in those fields is extremely fragmented, and is split into two distinct regions separated by large distances in declination. Coverage in the northern and southern sections of these fields can also be irregular. Users should consult the sky coverage maps before using data from the Chameleon 2, Hydra, Abell 754 and Abell 3420 fields.
Effective Coverage of the Catalogs
The 6x-PSC and 6x-XSC cover slightly smaller areas than shown in the sky coverage maps for each field because Catalog sources were required to lie >10´´ and >15´´ away from Tile edges, respectively (A3.6.c). This tile-edge safety boundary minimizes edge-effects that include non-three-band coverage due to slight misalignments of the focal plane arrays, distortion at the edges of focal planes, and partial coverage of extended sources close to tile edges.
As in the main survey, coverage area is also lost in the 6x Catalogs due to the presence of bright stars and the influence of their bright image wings, ghosts images, diffractions spikes, latent images and other image artifacts (A.3.5.e). Extractions made near bright stars are carried in the 6x Working Databases, but are generally flagged as spurious detections of artifacts and therefore not passed to the reliable Catalogs. This has the effect of masking out an area around bright stars that scales with the star brightness. Figure 2 shows the spatial distribution of 6x-PSC sources in the Lupus field, illustrating the impact of bright star masking.
Between two and three square degrees of effective coverage was omitted from the 6x Catalogs because scans in several 6x fields were incorrectly labeled with the same tile numbers even though they did not cover the same region of sky (see A3.6.b). Because only one scan of tiles apparently observed more than once were selected for the catalogs, this duplicate labeling caused several scans and parts of scans with unique sky coverage to be excluded from the Catalogs. The extracted point and extended source information for the omitted area is still accessible in the 6x WDBs.
|Figure 1 - Sky map showing the outlines of 6x scans covering the Lupus field (blue lines), and the distribution of 6x-PSWDB extractions (red dots). Note the coverage gaps at the declination boundaries between some tiles, and the missing scans in the eastern half of the southern band of tiles.||Figure 2 - Sky map showing the outlines of 6x Lupus field scans (blue lines) and distribution of 6x-PSC sources (red dots). Note the effective masking of 6x-PSWDB extractions around several bright stars in the northern portion of the field.|
For the 6x observations, the READ2 integration time was increased from 1.3 s to 7.8 s, but the READ1 integration time remained at 51 ms, the same as in the main survey (A3.4.a). The brightest unsaturated sources in the main survey's 1.3 s READ2-READ1 images were also detectable as the faintest sources in the 51 ms READ1 frames. This photometric overlap was essential for providing contiguous and internally consistent magnitude coverage across the dynamic range of the survey. The 6x observations do not necessarily have overlapping READ1 and READ2-READ1 photometry because of the increased READ2 integration time. Thus, many saturated sources in the 6x READ2-READ1 exposures are too faint to be detected in the 51 ms READ1 frames, or are detected only at very low SNR levels. The resulting incompleteness and/or faint detections in the 8-11 mag READ1/READ2-READ1 boundary introduces artificial features in source counts and color-magnitude diagrams that are discussed below.
The 2MASS 6x data primarily exist to report the faint extension of the original survey results provided by the 6x increase in READ2 exposure time. Photometry of the brighter 7.8 s READ2 and 51 ms READ1 extractions are included in the 6x catalogs given their utility for variability and proper motion studies.
Photometry for bright sources that are near
to or brighter than the saturation level of
the 6x 7.8 s READ2 exposures should be obtained
from the 2MASS All-Sky Catalogs. In general, photometry
for any source with high SNR measurements in the All-Sky Catalogs
should take precedence over the 6x measurements because they
have received a greater level of review and validation
The raw 6x imaging data were reduced with a modified version of the 2MAPPS v3.0 software pipeline that was used for the main survey. The changes made to 2MAPPS are summarized in A3.5. Basic processing steps and pipeline output products remained essentially unchanged from main survey data processing.
Most modifications in the reduction software were designed
to accommodate the longer READ2 exposure times of the 6x data
and the resulting higher source and background count rates.
Secondary changes included corrections to software bugs that
were known to exist from main survey data processing, and
a small number that further improved data quality and brought final
output data formats closer to those of the release products.
Magnitudes reported in the 6x Point and Extended Source Working Databases and Catalogs are in the same natural 2MASS photometric system as the All-Sky PSC and XSC. The system bandpasses are described in III.1.b. Transformations between the 2MASS and selected other photometric systems, updated from the initial forms derived by Carpenter et al. (2001, AJ, 121, 2851), are given in VI.4.b.
Position reconstruction for the 6x observations (A3.5.b) used the 2MASS All-Sky PSC as the primary astrometric reference catalog, rather than the Tycho-2 Catalog that was used as the reference for the main survey.
The relatively high density of astrometric reference stars provided by the All-Sky PSC results in excellent global 6x astrometric performance relative to the All-Sky PSC and external catalogs, as documented in A3.2.c. For example, the mean radial offset between the reported positions of stars in the 6x-PSC source and the UCAC2 astrometric catalog is 95 mas which is essentially the same as measured between All-Sky PSC and UCAC astrometry. In addition, the software error that resulted in uncorrected distortion for Read_1 sources in the main survey data processing has been corrected for the 6x processing. Thus, there is no systematic bias with cross-scan position between READ1 and READ2-READ1 astrometry for 6x point sources.
ii. 6x Point Source Working Database and Catalog
The 6x-PSC is released as part of the 6x-PSWDB and not as a separate table as was done for the All-Sky Survey. The subset of rows in the 6x-PSWDB that comprise the 6x-PSC are identified as having a value of cat=1 in their source entry.
The 6x-PSWDB contains all extractions from all observations made in the long exposure mode These include one or more independent detections of real astrophysical sources, detections of low SNR noise excursions, and spurious detections of image artifacts and transient events such as cosmic ray strikes and meteor trails.
The 6x-PSC is comprised of the subset of 6x-PSWDB entries that define a uniform, complete and reliable list of near infrared sources. One unique detection of inertial near infrared sources is selected for objects observed multiple times, so the 6x-PSC can be thought of as a "snapshot" of the near infrared sky. The criteria used to select the 6x-PSC from the 6x-PSWDB are described in A3.6, and are analogous to those used to draw the 2MASS All-Sky PSC from the Survey Point Source Working Database.
The 6x-PSWDB contains a large number of spurious detections of faint noise excursions, image artifacts, and transient events such as cosmic ray strikes and meteor trails in addition to detections of real astrophysical sources. To help discriminate between real and spurious extractions, each 6x-PSWDB entry has been assigned a reliability flag value, rel, that is related to the probability that it is a detection of a real astrophysical object at the time of the 2MASS observation. The reliability flag is a single character in the range "A" to "F", with "A" representing sources with the highest reliability and "F" the lowest. Appendix 5 contains a description of the algorithm used to assign the reliability flag values and limitations of the estimator.
Users should use the 6x-PSC, or should select 6x-PSWDB sources having a reliability flag value of rel="A" to minimize the number of spurious extractions. Caution should be exercised when using any 6x-PSWDB source with a lower probability of reliability. When in doubt about the reliability of a 6x catalog or database entry, we strongly recommend examining the image of the source using the 6x Image Atlas.
Table 1 contains a breakdown of the 6x-PSWDB and 6x-PSC according to reliability flag value, and the probability of reliability associated with each value of rel. The 6x-PSC source selection criteria are designed to identify reliable sources in the 6x-PSWDB, so the number 6x-PSC entries declines rapidly with decreasing probability of reliability. There are still a small number of low reliability sources in the 6x-PSC. Visual examination of the 42 6x-PSC sources with rel="F" reveals that most (29) are in fact detections of real objects that are usually confused, in close multiple systems, or are measurements of brighter stars in the difficult READ1 and READ_2 sensitivity "gap." The remaining 13 rel="F" extractions in the 6x-PSC are spurious detections in the disks of large galaxies, in the halos of bright stars, and glints at the edge of images.
|rel Value||Number (6x-PSWDB)||Number (6x-PSC)||Probability of Reliability|
In general, unreliable database and catalog entries exhibit one or more of the characteristics described in Table 2. Users should scrutinize such sources carefully. However, possession of any one or more of these attributes does not necessarily guarantee that a detection is unreliable, only that it merits examination. We strongly advise examining images of any 6x-PSWDB or 6x-PSC entries whose reliability may be in question.
|Single band detection||rd_flg="0" in two bands|
|Contamination or confusion flagging||cc_flg != "000"|
|Large value of profile-fit photometry 2 value||rd_flg="2" and [jhk]_psfchi >> 1|
|Low frame-detection count for SNR>7 sources||ndet[1,3,5] 1 and [jhk]_snr >7|
|READ1 detection that is fainter than the READ2 saturation limits||(rd_flg="1" and j_m>11) or (rd_flg="1" and h_m>10.5) or (rd_flg="1" and k_m>10)|
|Source is fragment of an extended source||gal_contam="2"||Source is associated with a solar system object||mp_flg="1"|
As was the case for the main survey, 6x point source photometry is measured differently for three brightness regimes. The J, H and Ks default magnitudes (j_m, h_m, k_m) listed for each object represent what are the best available measurements in each band, as determined by the automated processing. The rd_flg specifies the origin of the default magnitude in each band. Table 1 below contains the possible values of rd_flg, a description of the photometry algorithm corresponding to each value, and the number of instances of each value, by band, in the 6x-PSWDB and 6x-PSC.
Figures 3-5 show the J, H and Ks 6x-PSWDB differential source counts in the 6x Lockman Hole field, decomposed by rd_flg. The majority of detected sources are non-saturated in the 7.8 s READ2-READ1 6x exposures, and have default photometry from profile-fitting (rd_flg=2). The 6x counts extend approximately one magnitude fainter than in the main survey, and 6x READ2-READ1 saturation occurs at J>11, H>10.5 and Ks>10 mag, approximately two magnitudes fainter than in the main survey observations. For a small fraction of the non-saturated READ2-READ1 detections profile-fitting photometry fails, and curve-of-growth-corrected aperture photometry provides the default magnitude (rd_flg=4).
The default magnitudes for point sources in the brightness range 4.5<J<11, 4<H<10.5, 3.5<Ks<10 mag are taken from aperture photometry measurements made on the 51 ms READ1 exposures (rd_flg=1). Because the READ1 exposure time was not increased for the 6x observations, measurements of sources at the faint end of the READ1 regime will be of relatively low SNR. Higher precision measurements of such stars are provided by the All-Sky PSC wherein these objects were in the high SNR, non-saturated READ2-READ1 range.
Stars brighter than approximately J~4.5, H~4 and Ks~3.5 mag saturate even the 51 ms exposures. Photometry of such objects is performed using a 1-d radial profile fit to the azimuthally-averaged image profile on the READ1 exposures, and the rd_flg value for the appropriate band is "3". The boundary between rd_flg=1 and rd_flg=3 for the 6x data is the same as for the main survey and users should defer to the All-Sky PSC for fluxes and positions for these sources. Inclusion of these saturated observations in the 6x databases is largely to support variability and proper motion studies.
|Figure 3 - Differential 6x PSWDB J-band source counts for the Lockman Hole field. Counts are broken down into different rd_flg populations denoted by color..||Figure 4 - Differential 6x PSWDB H-band source counts for the Lockman Hole field. Counts are broken down into different rd_flg populations denoted by color..||Figure 5 - Differential 6x PSWDB Ks-band source counts for the Lockman Hole field. Counts are broken down into different rd_flg populations denoted by color..|
The origin and general quality of the default magnitude photometry listed in the 6x-PSWDB and 6x-PSC are summarized by a number of informative flags that accompany each source. It is essential that users refer to these flags when interpreting photometry for any source in the 6x Point Source products. The primary quality indicator flags include rd_flg, ph_qual, cc_flg and bl_flg. Each of these is comprised of three characters, each corresponding to one band; the first character is the J-band value, the second is the H value, and the third is the Ks value.
The rd_flg denotes the origin of and algorithm used to derive the quoted default magnitudes for each 2MASS 6x Point Source. Table 3 contains the possible values of rd_flg, their interpretation and the number of instances of each value in each band in the 6x point source tables.
|rd_flg Value||Source of Photometry||6x-PSWDB||6x-PSC|
|0||Not detected in this band. The default magnitude is the 95% confidence upper limit derived from a 4" radius aperture measurement taken at the position of the source on the 6x Atlas Image. The sky background is estimated in an annular region with inner radius of 14" and outer radius of 20". The uncertainty in the default magnitude, [jhk]_msig is null in these cases.||4002889||7551654||11487578||90851||1001170||2881445|
|1||"READ1" aperture photometry. The default magnitude is derived from aperture photometry (IV.4.a.i) measurements on the 51 ms "READ1" exposures. The aperture radius is 4", with the sky background measured in an annulus with an inner radius of 14" and an outer radius of 20". Used for sources that saturate one or more of the 7.8s "READ2" exposures, but are not saturated on at least one of the 51 ms "READ1" frames. The photometric uncertainty in these cases is the RMS variation of the measured flux from all frames on which a source falls. If the source was measured on only one frame, the [jhk]_msig value becomes a flag, and has a value of >8.0 mag in the appropriate band.||61596||78655||85856||35317||41590||46922|
|2||READ2-READ1 profile-fit photometry. The default magnitude is derived from a profile-fitting measurement (IV.4.b) made on the 7.8 sec "READ2" exposures. The profile-fit magnitudes are normalized to curve-of-growth-corrected aperture magnitudes. This is the most common type in the 6x-PSWDB, and is used for sources that have no saturated pixels in any of the 7.8 sec exposures. The uncertainties for the profile-fit measurements, [jhk]_msig, are derived from a goodness-of-fit metric that includes terms for uncertainties in the photon noise in the sky background reference, the noise in the source brightness, and how well the fitted profile matches the actual point-spread-function of the source.||19771707||15960573||11935820||8453862||7428661||5503591|
|3||Saturated in READ1. The default magnitude is derived from a 1-d radial profile fitting measurement made on the 51 ms "READ1" exposures. Used for very bright sources that saturate all of the 51 ms "READ1 1" exposures. The photometric uncertainty in these cases is the RMS variation of the measured flux from all frames on which a source falls. If the source was measured on only one frame, the [jhk]_msig value becomes a flag, and has a value of >8.0 mag in the appropriate band.||260||345||304||158||201||185|
|4||READ2-READ1 aperture photometry. The default magnitude is derived from curve-of-growth-corrected 4" radius aperture photometry measurements (IV.4.c) on the 7.8 s "READ2" exposures. This is used for sources that are not saturated in any of the READ2 frames, but where the profile-fitting measurements fail to converge to a solution. These magnitudes are the same as the standard aperture magnitudes (j_m_stdap, h_m_stdap, k_m_stdap), but when they are the default magnitudes, it generally implies that they are low quality measurements. The photometric uncertainty in these cases is the RMS variation of the measured flux from all frames on which a source falls.||12542||9163||6940||56||36||29|
|6||Inconsistent deblend. The default magnitude is the 95% confidence upper limit derived from a 4" radius aperture measurement taken at the position of the source on the 6x Atlas Image. The sky background is estimated in an annular region with inner radius of 14" and outer radius of 20". This is used for pairs of sources which are detected and resolved in another band, but are detected and not resolved in this band. This differs from a rd_flg="0" because in this case there is a detection of the source in this band, but it is not consistently resolved across all bands. The [jhk]_msig value is null for these cases.||150997||400713||456392||57347||165206||205308|
|9||Detection at this location, but no useful brightness measurement possible. The default magnitude is the 95% confidence upper limit derived from a 4" radius aperture measurement taken at the position of the source on the 6x Atlas Image. The sky background is estimated in an annular region with inner radius of 14" and outer radius of 20". This is used for sources that were nominally detected in this band, but which could not have a useful brightness measurement from either profile fitting or aperture photometry. This often occurs in highly confused regions, or very near Tile edges where a significant fraction of the measurement aperture or sky annulus falls off the focal plane.||23711||22599||50812||3||730||114|
|ph_qual Value |
(1 per band)
|Z||Detection in this band is identified with an image artifact. The corresponding cc_flg value in this band is "C", "D", "G" or "P". Sources with ph_qual="Z" in any band are excluded from the 6x-PSC.||604809||471768||273603||0||0||0|
|X||There is a detection at this location, but no useful brightness estimate can be extracted using any algorithm. rd_flg=9 and default magnitude is null.||66||4165||32359||3||730||114|
|U||Upper limit on magnitude. Either source is not detected in this band (rd_flg=0), or it is detected, but not resolved in a consistent fashion with other bands (rd_flg=6). A value of ph_qual="U" does not necessarily mean that there is no flux detected in this band at the location. Whether or not flux has been detected can be determined from the value of rd_flg. When rd_flg="0", no flux has been detected. When rd_flg="6", flux has been detected at the location where the images in all three bands (JHKs) were not deblended consistently.||4150606||7944790||11937902||148198||1166376||3086753|
|F||This category includes rd_flg=1 or rd_flg=3 sources where a reliable estimate of the photometric error, [jhk]_msig, could not be determined. The uncertainties reported for these sources in [jhk]_msig and [jhk]_msigcom are flags and have numeric values >8.0.||3913||6773||9593||1658||3211||4325|
|E||This category includes detections of any brightness or SNR where: 1) the goodness-of-fit quality of the profile-fit photometry was very poor (rd_flg=2 and [jhk]_psf_chi10.0); or 2) where profile-fit photometry did not converge, and an aperture magnitude is reported (rd_flg=4); or 3) where the number of frames on which a source was detected was too small in relation the number of frames in which a detection was geometrically possible (rd_flg=1 or rd_flg=2). The 2 limit results in many relatively bright (SNR>>10) unresolved double stars being found in this category.||63602||53217||33655||29331||22287||12007|
|A||Detections in any brightness regime where valid measurements were made (rd_flg=1,2 or 3) with [jhk]_snr10 AND [jhk]_msig0.10857.||10429521||7098971||5016932||5919095||4055241||2843514|
|B||Detections in any brightness regime where valid measurements were made (rd_flg=1,2 or 3) with [jhk]_snr7 AND [jhk]_msig0.15510.||3987039||2759642||1736451||2148894||1600838||978771|
|C||Detections in any brightness regime where valid measurements were made (rd_flg=1,2 or 3) with [jhk]_snr5 AND [jhk]_msig0.21714.||2731914||3129174||2106271||362428||1455871||1083313|
|D||Detections in any brightness regime where valid measurements were made (rd_flg=1,2 or 3) with no [jhk]_snr or [jhk]_msig requirement.||2052232||2555202||2876936||27987||333040||628797|
In the 2MASS 6x-PSWDB, the cc_flg values identify extractions that are either real astrophysical sources whose measurements are confused and/or contaminated by other nearby sources or image artifacts, or that are spurious detections of image artifacts. The algorithms used to identify confused and/or contaminated sources and to set the values of the cc_flg during 6x data processing are discussed in A3.5.e. The encoding of the cc_flg is summarized in Table 5 below.
Users should select sources with cc_flg="000" if they need samples of sources that have the lowest probability of contamination. However, this constraint may compromise the completeness of source selection, particularly in crowded fields where a significant fraction of sources are affected by photometric confusion (cc_flg="c").
6x-PSWDB or 6x-PSC entries containing a cc_flg value other than "0" in any detected band should be viewed with caution. A cc_flg value of [C,D,G,P] indicates that the entry is associated with an image artifact. If the cc_flg has any of these values in all detected bands, then the WDB entry is most likely a spurious detection of the artifact. WDB entries with non-zero but lower case letter cc_flg values [b,c,d,p,s], or that have a capital letter cc_flg value in fewer than all detected bands, are probably real sources but with photometry that may be corrupted and/or biased by artifacts or confusion with nearby sources.
6x-PSWDB entries that are identified as artifacts
(cc_flg = [C,D,G,P]) in any band are not passed to the
6x-PSC. However, the 6x-PSC does contain sources that may
be contaminated by artifacts or confusion (cc_flg = [b,c,d,p,s])
in one or more bands.
|cc_flg Value |
(1 per band)
|0||Real source unaffected by artifacts, or not detected in that band||19068694||20954202||22383866||6764368||7387179||8002265|
|p||Real source whose photometry may be contaminated by a persistence (latent) image of a bright star||108966||122566||42175||30689||56385||12142|
|c||Real source whose photometry may be biased because of confusion with nearby brighter source||3692108||2121811||1132896||1607010||1036306||541756|
|d||Real source whose photometry may be contaminated by a diffraction spike||6068||1027||10083||2755||4654||4629|
|s||Real source whose photometry may be contaminated by a horizontal "stripe" (electronic cross-talk) due to a bright star||492934||303268||150718||232664||152899||76543|
|b||Real source that is confused in the bandmerging process because of a nearby source||1319||2598||1629||108||171||259|
|P||Spurious detection of a Persistence (Latent) image of a bright star||286063||292724||103307||0||0||0|
|C||Spurious detection in the Confusion "halo" around a bright star||154010||103995||77539||0||0||0|
|D||Spurious detection on a Diffraction spike from a nearby bright star||91575||98060||70611||0||0||0|
|G||Spurious detection of a dichroic Glint||121965||16074||50878||0||0||0|
The photometric uncertainties given in the [jhk]_msig columns in the 6x-PSWDB and 6x-PSC are equivalent to the "corrected" uncertainties in the [jhk]_cmsig columns in the All-Sky PSC and Survey Point Source Reject File for profile-fit photometry.
One of the modifications made to the
data reduction pipeline for 6x data processing was a change to
the profile-fitting photometry error model to compensate for the
overestimation of photometric uncertainties that affected
the main survey point source photometry.
As a result, there was no need to apply the
a posteriori corrections
to the 6x photometric uncertainties that were applied to the main survey data.
There are no [jhk]_cmsig
columns in the 6x PSWDB and 6x-PSC.
While the 2MASS 6x observations probe one magnitude deeper than the main survey on average, the actual sensitivity achieved by individual scans varied with the atmospheric transparency, seeing and background emission levels. Histograms of the estimated magnitudes at which point source SNR=10 for all northern and southern observatory 6x scans are shown in Figure 6. As with the main survey, the achieved sensitivities range by nearly +0.5 mag in the extreme depending on the atmospheric conditions.
The point source sensitivity of the 6x observations are also constrained by source confusion noise. Differential source counts from the Lockman Hole and Cygnus 6x fields are compared with the counts from the same areas of the main survey in Figures 7 and 8, respectively. The 6x counts in the high galactic latitude Lockman Hole field turn over approximately one magnitude fainter than those in the All-Sky PSC, near J=17.6, H=16.9 and Ks=16.1 mag. The improvement relative to the All-Sky PSC is not as great in the Cygnus field, which has an order of magnitude higher source density than the Lockman Hole region.
|Figure 6 - Distribution of the estimated SNR=10 magnitudes for all photometric 6x scans, based on atmospheric transparency, seeing and background. These estimates do not take into account the effects of confusion.||Figure 7 - Area-normalized 6x-PSC and 6x-XSC differential source counts in the Lockman Hole 6x field, compared with those in the same area in the All-Sky PSC and XSC. 6x-PSC and 6x-XSC counts are shown by the red and blue lines, respectively. All-Sky PSC and XSC counts are shown in the grey and cyan shaded regions.||Figure 8 - Same as Figure 7, but for the Cygnus 6x field region.|
The effective sensitivity "gap" between the 51 ms READ1 and 7.8s READ2 6x exposures results in photometric biases between 6x and All-Sky PSC data, and can produce artifacts in source count curves and color-magnitude diagrams generated using 6x point source data. Differential point source counts from the Lockman Hole 6x field are shown in Figure 9. The small discontinuities near 10.5-11 mag range are caused by the incompleteness and systematic flux overestimation of low SNR measurements in the READ1 exposures. The same effects cause the horizontal discontinuity of points near Ks=10.5 mag in the 6x color-magnitude diagram from the same field shown in Figure 10.
Photometry for bright sources that are near to
or brighter than the saturation level of
the 6x 7.8 s READ2 exposures
should be obtained from the 2MASS All-Sky PSC.
In addition, photometry for any point source with high SNR measurements
in the All-Sky Catalogs should take precedence over the 6x measurements
because they have received a greater level of review and validation
|Figure 9 - Differential point source counts from the 6x Lockman Hole observations showing the discontinuities at the READ1/READ2-READ1 boundaries.||Figure 10 - Color-magnitude diagram for point (red) and extended source (green) extractions 6x WDBs in the Lockman Hole field. The black contours trace the density of point sources. The horizontal discontinuity near Ks=10.5 mag is at the READ1/READ2-READ1 sensitivity boundary.|
Point source photometry from the 6x-PSWDB/PSC and All-Sky PSC typically agree on average to within 1-2%. However, there are systematic deviations from this agreement in certain brightness regimes that are caused by flux overestimation in both the 6x and survey data and possible non-linearity in the 6x measurements.
Diagrams showing the photometric differences between the 6x and All-Sky PSC point source photometry plotted as a function of 6x magnitude are included in the detailed field summary pages linked to Figure 1 in A3.2.b. An example of one such diagram from the Abell 3558 6x field is shown in Figure 11. Several features can be seen in this diagram that highlight biases in the the 6x photometry relative to the main survey measurements:
In certain high source density 6x fields, such as Cygnus shown in Figure 12, the 6x point source photometry for sources in the range 12-15 mag becomes systematically brighter than the that from the All-Sky PSC photometry, up to ~5%, until the flux overestimation in the faint All-Sky PSC dominates. The origin of this bias is not understood. It is not the same in all bands, nor is it seen in all high density fields.
Because of the potential bias between 6x and survey point source photometry in the transition region between 51 ms READ1 and 7.8s READ2 measurements from the 6x exposures, high SNR measurements from the 2MASS All-Sky PSC should always take precedence over 6x measurements of the same objects. The 2MASS All-Sky PSC has also benefited from greater validation and scrutiny.
|Figure 11 - Differences between 6x and main survey default point source photometry as a function of 6x source default magnitude in the Abell 3558 6x field. Black contours trace the density of individual sources that are shown as light grey points. The large blue points and error bars show the trimmed average and RMS of the 6x-survey magnitude differences for all sources in 0.25 magnitude wide bins.||Figure 12 - Differences between 6x and main survey default point source photometry as a function of 6x source default magnitude in the Cygnus 6x field. Black contours trace the density of individual sources that are shown as light grey points. The large blue points and error bars show the trimmed average and RMS of the 6x-survey magnitude differences for all sources in 0.25 magnitude wide bins.|
A detailed analysis of 2MASS-6x point source astrometry based on comparisons with the 2MASS All-Sky PSC, Tycho 2 and UCAC2 catalogs is presented in A3.2.c. The overall astrometric precision of the 2MASS-6x point source measurements is on par with that of the 2MASS All-Sky PSC. For example, the mean radial offset between positions of stars reported in the All-Sky PSC and the UCAC2 catalog is 95 mas.
The quoted position uncertainties for 6x point sources not saturated on the 7.8 s READ2-READ1 exposures (rd_flg="2") are approximately 20% larger than expected based on comparisons with the external catalogs. The uncertainty overestimation is most likely the result of an overly conservative correction for systematic errors in the 2MASS All-Sky PSC astrometric reference catalog. The quoted uncertainties for sources in the READ1 (rd_flg="1") brightness regime have are lower than expected from the same comparisons.
An error in how frame distortion corrections were applied in survey data processing was corrected for the reduction of 6x observation data (A3.5.b.ii). As a result, the small (±50 mas) position bias between sources in the READ1 and READ2-READ1 regimes that is present in the All-Sky PSC is not seen in the 6x-PSWDB astrometry.
The 6x-PSWDB contains the point source extractions from all 2MASS 6x observations. Sources falling in regions that were scanned more than once may have multiple, independent measurements in the database. Consequently, source counts derived from the 6x-PSWDB may overestimate the true distributions because of the presence of redundant source detections. Use the 6x-PSC, in which duplicate detections have been removed, to avoid this error.
and sdet columns in the 6x-PSWDB
give the number of scans that covered the position of a source
and the number of unique scans in which the source was detected,
respectively. The average positions and photometry are
available for sources detected more than once in the
The 6x-PSC Catalog Generation process selected one, unique apparition of sources in scan overlap regions that have multiple detections present in the 6x-PSWDB. There are approximately 1000 cases in the 6x-PSC where this multiple detection resolution process failed and two detections of the same source from different scans were promoted to the Catalog. These failures were caused by confusion that ensued when one or more of the multiply-detected sources were themselves artificially split within their respective scans because of blending with nearby objects or noise excursions. The sources involved are often faint and/or complex, such as small extended edge-on galaxies that trigger multiple point source detections.
Figure 13 shows a histogram of radial separations between pairs of 6x-PSC sources in scan overlap regions. The roll-off in number of pairs with separations less than 5-6" is a result of the effective resolution limit of the 2MASS telescope and camera system. The sharp drop below 2" separation is caused by the 2" match window using in the multiple detection resolution process, and the the pairs with separations <2" are those that were not properly dealt with by the multiple detection resolution process. A similar population of small separation source pairs exists in the All-Sky PSC, as seen in Figure 14 in I.6.b.ix.
|Figure 13 - Histogram of separations between pairs of 6x-PSC sources in the scan overlap regions. There are ~1000 pairs with separations <2" that are a result of errors in the multiple detection resolution process.|
No attempt was made to remove non-inertially fixed sources from the
6x-PSWDB or 6x-PSC. Sources that are at the positions of known asteroids,
comets, planets or planetary satellites at the time of the 6x observations
are flagged by having mp_flg="1"
These are positional associations and are not necessarily identifications,
so they remain in the 6x source lists. Some fraction of the putative
detections are chance superpositions of the predicted solar system
object positions with background sources. This is particularly likely
at low Galactic latitudes, where the density of background stars is large.
All 6x point source extractions were positionally correlated with the Tycho 2 and USNO-A2.0 optical catalogs. 2MASS 6x sources that have optical catalog counterparts within ~5´´ have listed in the 6x-PSWDB and 6x-PSC source records the optical catalog identifier (a="T" or "U"), blue and visual-or-red magnitudes, the 2MASS/optical position separation (dist_opt) and position angle (phi_opt). Matches with the Tycho 2 catalog take precedence over the USNO-A2.0 matches in the listing.
These are positional associations, and not necessarily identifications. The positional accuracy of 2MASS and the optical catalogs is sufficiently high that inertial sources should have positions that match to within ~1´´. Optical associations with separations dist_opt >1´´ are either proper motion candidates, or possible cases of chance alignments with the IR sources.
The optical magnitudes listed for the optical associations in the 6x-PSWDB are derived from the Tycho 2 and USNO-A2.0 values. In the case of Tycho 2 associations, the optical magnitudes listed are Johnson B and V magnitudes and are derived from the Tycho blue (BT) and visual (VT) magnitudes using the transformations given by (Høg et al. 2000):
V = VT - 0.090*(BT - VT)
B-V = 0.850*(BT - VT)
For USNO-A2.0 associations, the optical magnitudes are the photographic blue and red magnitudes taken explicitly from the USNO-A2.0 Catalog.
Two 2MAPPS software errors that affected the optical associations in the main survey data reduction were corrected in 6x data processing:
iii. 6x Extended Source Working Database and Catalog
The 6x-XSC is released as part of the 6x-XSWDB and not as a separate table as was done for the All-Sky Survey. The subset of rows in the 6x-XSWDB that comprise the 6x-XSC are identified as having a value of cat=1 in their source entry.
The 6x-XSWDB contains all extractions of sources believed to be extended relative to the instantaneous point-spread-function (PSF) in all observations made in the 2MASS long exposure mode. These include one or more independent detections of real extended astrophysical sources such as galaxies and galactic nebulae, and detections of single and multiple stars and spurious image artifacts that have extended source signatures.
The 6x-XSC is comprised of the subset of 6x-XSWDB entries
that define a uniform, complete and reliable list of extended near infrared
sources. One unique detection of each source
is selected for objects observed multiple times,
so the 6x-XSC can be thought of as a "snapshot" of the near infrared sky.
The criteria used to select the 6x-XSC from the 6x-PSWDB
are described in A3.6, and are
analogous to those used to draw the 2MASS All-Sky XSC from the
Survey Extended Source Working Database.
2MASS 6x extended source processing (see A3.5.d) attempts to identify all sources that are not well-fit by a single PSF. Therefore, the 6x-XSWDB includes true extended sources, such as galaxies and nebulae. Because the algorithms are not perfect, the 6x-XSWDB also contains detections of close multiple stars and spurious detections of artifacts produced by background gradients around bright stars.
To help discriminate between real extended sources and multiple stars and spurious extractions, each 6x-XSWDB entry has been assigned a reliability flag value, rel, that is related to the probability that it is a detection of a real, extended astrophysical object at the time of the 2MASS observation. The reliability flag is a single character in the range "A" to "F", with "A" representing sources with the highest reliability and "F" the lowest. Appendix 5 contains a description of the algorithm used to assign the reliability flag values and limitations of the estimator.
Table 6 contains a breakdown of the 6x-XSWDB and 6x-XSC according to reliability flag value, and the probability of reliability associated with each value of rel. The 6x-XSC source selection criteria are designed to identify reliable sources in the 6x-XSWDB, so the number 6x-XSC entries declines rapidly with decreasing probability of reliability. There are still a small number of low reliability sources in the 6x-XSC. The single 6x-XSC source with rel="F" is a compact red object superimposed on diffuse nebulosity in the IC1396 6x Field. It was classified as "ambiguous" in visual examination (see below).
Use the 6x-XSC, or select 6x-XSWDB sources having a reliability flag value of rel="A" to minimize the number of spurious extended sources. Caution should be exercised when using any 6x-XSWDB source with a lower probability of reliability. When in doubt about the reliability of a 6x catalog or database entry, we strongly recommend examining the image of the source using the 6x Image Atlas.
|rel Value||Number (6x-XSWDB)||Number (6x-XSC)||Probability of Reliability|
Images of a large number of candidate extended sources in the 6x-XSWDB were examined visually as part of the reliability scoring. The results of these examinations are encoded in the visual classification score (vc) database parameter. The possible values of vc and frequency of occurrence in the 6x-XSWDB and 6x-XSC are listed in Table 7. Note that objects that were visually classified to be not truly extended (i.e. single or multiple stars) or image artifacts (vc=2) where not selected for the 6x-XSC.
|-2||Unknown. Sources that were examined but could not be unambiguously classified. These objects are usually faint and compact.||16016||5156|
|-1||Not examined visually.||120714||39152|
|1||Galaxy or galactic extended source.||78477||39733|
|2||Not true extended source (i.e. single or multiple star or artifact.||31884||0|
The cc_flg is used to highlight 6x-XSWDB and 6x-XSC entries that have some probability of being artifacts or contaminated by nearby large galaxies.
Users should select extended sources with cc_flg="0" if they need samples that have the lowest probability of contamination.
Sources flagged as artifacts (cc_flg="A") include those corrupted by a bright stars and those that are outright spurious detections of image artifacts produced by bright stars. These sources were identified as such by visual inspection of their images. They are not selected for the 6x-XSC.
Table 8 summarizes the possible values of cc_flg and the number of occurrences of each value in the 6x-XSWDB and 6x-XSC. Note that the 6x cc_flg encoding is slightly different than used for the All-Sky XSC.
|cc_flg Value||Nature of Source||Number|
|0||Nominal. Unaffected by artifacts.||213698||84040|
|A||Artifact or unreliable||31884||0|
|z||Fragment of a large galaxy or nebula. Extracted information is generally not useful.||1508||0|
|X||Associated with large galaxy.||1||1|
The 2MASS 6x XSWDB may contain multiple measurements of the same object. Some of these multiple detections are independent measurements of objects in regions observed more than once during 2MASS 6x observations, and some are duplicate source entries from the overlapping 6x Atlas Image declination boundaries within the same scan and are not independent. Because of this "over-completeness," the 6x-XSWDB is not suitable for studies based on source count statistics. Use the 2MASS All-Sky XSC and 6x XSC for this type of inquiry.
Because the 6x-XSWDB contains extractions of all extended source candidates from all 2MASS 6x observations taken under photometric conditions, it may contain more than one independent measurement of objects in regions that were scanned multiple times. The number of duplicate source detections varies across the 6x fields, depending on 6x tile overlap geometry and the number of times 6x tiles were scanned. See A3.2 for a description of the coverage of the 6x observations.
The 6x Merged Extended Source Information Table provides combined position, brightness and shape information for multiply-detected extended sources in the 6x observations, and statistics on source brightness that are useful for identifying variables. Source confirmation statistics from the Merged Source Information table is also contained in the 6x-XSWDB: the spos and sdet columns in the 6x-XSWDB give the number of scans that covered the position of a source and the number of unique scans in which the source was detected as an extended source, respectively.
Extended sources were detected and characterized on the 6x Atlas Images during 2MASS 6x data processing. Because the Atlas Images within each 6x scan were constructed with 54 pixels (54") of declination overlap between adjacent images, objects that fall in the overlap region between images, or that span more than one image in a scan may have been extracted more than once. All extended source detections in each scan, including the "in-scan duplicates," were loaded into the 6x XSWDB. Because they are based on the same image data, the in-scan duplicates are not independent measurements and thus they are different than the multiple detections of extended sources that were scanned repeated times.
In-scan duplicate detections can be identified in the
6x XSWDB as two extended source entries from the same observation
(e.g. with the same
scan_key value) that also
have nearly the same position and possibly magnitudes,
but that have different values of the
coadd_key which identifies the
Atlas Image from which the source was extracted.
The 2MASS 6x-XSWDB and 6x-XSC contain some extended sources that are truncated by Atlas Image edges, and consequently have distorted position, flux and shape measurements. Use the measurements of any extended source that lies within approximately 1' of a scan or image edge with caution. Refer to the All-Sky XSC for the best available measurements of any objects on scan or image boundaries.
2MASS extended source processing detected and characterized objects on a single Atlas Image. Sources that are truncated by image edges were not accurately measured. Although detections of truncated objects are contained in the 6x XSWDB, they typically have underestimate fluxes, positions that are biased away from the image edge, and incorrect size and shape attributes.
The overlap size between 2MASS 6x tiles and between the declination boundaries of Atlas Images was designed in part so that objects up to approximately one arcminute in diameter would be fully covered by at least one scan. Small extended objects in the 6x XSWDB that lie on Atlas Image edges may have a duplicate entry from another scan if there is an adjacent overlapping scan. Because of the finite size of the 6x fields, though, many scans do not have overlapping scans.
Extended sources larger than one arcminute in diameter
that are truncated by scan or image edges may not always
be fully contained on a single Atlas Image, and may therefore
not have an accurate measurement available in any 2MASS extended
source table (survey, 6x or calibration). The largest objects
detected in 2MASS survey observations were characterized using special
post-processing for the
Galaxy Atlas (LGA; Jarrett et al. AJ, 125, 525),
and the LGA entries are contained in the All-Sky XSC.
However, the LGA is not complete for objects smaller than a few
arcminutes, so care should be taken when using any extended source
measurement in close proximity to a scan edge.
The 2MASS 6x-XSWDB and 6x-XSC do not contain accurate flux, position or size measurements for objects that are large relative to the size of a 6x Atlas Image, or that span more than one Atlas Image. Consult the 2MASS All-Sky XSC or Large Galaxy Atlas for measurements of galaxies that are larger than a few arminutes in diameter, or that are truncated by the boundaries of a 6x Atlas Image.
2MASS extended source processing detected and characterized objects on a single Atlas Image. Extended sources that are large with respect to the size of an Atlas Image were often artificially "shredded" into multiple components which generally have misleading flux, position and shape measurements. Even when very large objects were correctly detected as a single source, their positions and photometry were usually biased due to incorrect background subtraction and/or because sections of the objects are missing from the image. Because the 2MASS 6x XSWDB contains the default processing output for large extended objects, they should not be used to obtain information about objects with very large size or that are partially truncated by scan edges. Many large galaxy/nebula segments in the 6x extended source tables are flagged by the confusion and contamination flag and have values of cc_flg='z' or 'Z'.
Special post-processing was used to
to characterize very large objects detected in 2MASS survey observations.
This processing utilized measurements on image mosaics that
fully contained the large sources, and from which accurate
background fitting could be performed. The resulting
Large Galaxy Atlas
(LGA; Jarrett et al. 2003 AJ, 125, 525) entries
were added to the 2MASS All-Sky XSC to insure the catalog's
bright source completeness. Comparable LGA post-processing was not
carried out for the 6x data. Therefore, the All-Sky XSC
should be consulted for the best available measurements for
the 6x-XSWDB or 6x-XSC.
iv. 6x Image Atlas
The 6x Atlas Images preserve the observed background sky levels measured relative to camera dark frames with the shutter closed. The mean background level is normally largest in the Ks band, although it can be larger in the H-band due to atmospheric OH airglow emission.
The only background compensation that is made during 6x Atlas Image construction is to adjust the individual frame backgrounds by a constant to produce seamless combined images. Because the OH airglow (especially at H-band) often contains structure on scales at or below the 2MASS frame size, the resulting Atlas Images sometimes show large background spatial variations. Th low frequency airglow structure can be seen in the mosaic constructed from the 6x Atlas Images of the IC1396 field shown in Figure 14.
|Figure 14 - 6x J+H+Ks image mosaic showing the field containing IC1396 (the Elephant Trunk nebula). The green-hued background structure is caused by time-variable atmospheric airglow emission that is strongest in the H-band.|
No correction for saturation is made during Atlas Image construction.
Saturation occurs in the READ2-READ1 frames from which the 6x Atlas Images
are constructed approximately two magnitudes brighter than in the main
at J<11, H<10.5 and Ks<10.0. Saturation
is handled correctly during source photometry in 6x pipeline processing.
Therefore, users are advised to defer to the 6x Catalogs
for photometry of bright point and extended sources.
Because some regions of the sky were observed more than once during 6x observations, the 6x Image Atlas may contain more than one independent image covering a particular location on the sky. When examining the image of a particular source selected from the 6x-PSWDB/PSC or 6x-XSWDB/XSC, it is important to select the 6x Atlas Image from the same scan in which the source was detected.
Image Services allow specification of a particular date, observatory
(hemisphere) and scan number
when requesting images from the 6x Atlas. If these
are not specified, you may not receive the
image from the correct scan.
[Last Updated: 2008 March 13; by R. Cutri]