II. User's Guide to the 2MASS All-Sky Data Release

2. Point Source Catalog (PSC):

a. Point Source Catalog Column Descriptions

b. How to Use the 2MASS PSC - A PSC Practical User's Guide

c. PSC Source Selection Criteria:

The All-Sky Release PSC contains accurate astrometry and photometry for 470,992,970 near-infrared sources extracted from scans of 59,731 Tiles covering 99.998% of the sky.

Sources in the PSC were drawn from a Working Database of all detections in these Tiles, using the selection criteria described in Section V.3 and summarized in Table 1. The point source Working Database contains approximately a factor of two more detections than are in the PSC; a significant fraction of these are detections of noise and image artifacts. The source detection thresholds in 2MASS pipeline data processing are set intentionally low to insure completeness. The demanding reliability requirements for the 2MASS PSC were achieved by applying the selection criteria listed below.

Users are recommended to review the Cautionary Notes for the PSC in Section I.6.b for known features of and problems in the catalog.

The PSC is a Composite Catalog

The PSC generated with the selection criteria above is a composite release that has two distinct components contained in a single database. The first component consists of a higher SNR, high reliability Catalog that meets or surpasses all of the 2MASS Level 1 Requirements in unconfused regions of the sky. Very bright stars that saturate the shortest 2MASS exposures are included in this set even though they do not satisfy the photometric accuracy requirements of the Survey. The second component of the PSC is a lower signal to noise extension that primarily contains sources that reach 0.5-1.0 mag fainter J<15.8, H<15.1 and K_s<14.3 mag levels, where the PSC is >99% complete. The completeness, reliability and uniformity of the extension sources are not as good as the high-reliability Catalog subset of the PSC, and may not satisfy all of the specifications described in the Level 1 Requirements. They are included in the PSC because, when used with some care, they can be a valuable resource for certain classes of investigations in which homogeneous, statistical datasets are not necessary.

The criteria for selecting the high-reliability Catalog sources in the full PSC are listed in Table 2. The criteria are meant to be applied band-by-band, so technically PSC sources that satisfy the Catalog requirements in one band may not satisfy them all bands. These criteria are discussed in detail in I.6.b.

• Number of Objects:     Full PSC:   470,992,970         Catalog:   341,317,908



• Number of Detections in Each Band:
  
  

  Table 3

  Band	Full PSC	High SNR Catalog
  J	455,371,014	321,117,915
  H	436,797,138	269,533,860
  Ks	375,248,502	210,729,664




• Band-Detection Combinations (Full PSC):
  
  

  Table 4

  Band-Combination	Number	Percentage of Total
  JHKs	359,919,450	76.4
  JH	64,724,153	13.7
  HKs	7,603,506	1.6
  JKs	4,257,125	0.9
  J	26,470,286	5.6
  H	4,550,029	1.0
  Ks	3,468,421	0.7




• Sky Coverage

The nominal sky coverage of the PSC is 99.997%, slightly less than the 99.998% of the sky covered by the scans of the Survey Tiles. The additional lost area lost is caused by the Tile Edge Boundaries used for PSC source selection (V.3). There are 43 gaps in the PSC coverage encompassing a total of 1.15 deg². Their locations are given in III.2.c.

Much larger than the area lost due to coverage gaps in the PSC is the area effectively masked by the scattered light halos, diffraction spikes and latent images around very bright stars. The sky coverage of the PSC lost in the glare of bright stars is 106.2, 156.2 and 177.9 deg² in J, H and K_s, respectively.



• Distribution of PSC Sources With Galactic Latitude
  
  

  Figure 1 shows a 3-color map of average PSC source counts in 5´ × 5´ bins in a galactic aitoff projection, where J-band counts are mapped into blue, H-band into green and K_s-band into red. The density enhancement towards the Galactic Plane and in the bulge of the Milky Way is apparent. Note also the enhancements associated with the Large and Small Magellanic Clouds, and the extinction filaments running through and near the Galactic Plane. In Figure 2 is shown the differential distribution of PSC source counts as a function of galactic latitude. Counts for the full PSC and for the Catalog subset are shown in black and red, respectively. The PSC cumulative source counts as a function of galactic latitude are shown in Figure 3, and summarized in Table 5. 90% of all PSC sources fall within the half of the sky with |b|<30°.

  Table 5 - Cumulative Source Counts

  	Full PSC		High SNR Catalog
  |b| <	Number	Percentage of Total	Number	Percentage of Total
  2°	64,860,852	0.138	52,127,949	0.152
  5°	171,536,055	0.364	134,110,427	0.392
  10°	285,981,079	0.607	214,860,387	0.628
  15°	347,566,169	0.738	256,977,785	0.751
  20°	382,750,070	0.813	281,232,441	0.822
  30°	421,458,546	0.895	308,171,925	0.900
  40°	442,833,953	0.940	323,026,991	0.944
  50°	455,114,841	0.966	331,516,768	0.969
  60°	462,673,352	0.982	336,675,553	0.984
  70°	467,397,538	0.992	339,852,389	0.993
  80°	470,076,205	0.999	341,633,227	0.998
  90°	470,992,970	1.000	342,237,326	1.000

  
  
  

  Figure 1	Figure 2	Figure 3

• Differential Source Counts and Detection Limits

  The 2MASS PSC is complete down to J<15.8, H<15.1 and K_s<14.3 mag, in the absence of confusion. Sources 0.5-1.0 mag fainter than these limits are included in the PSC, but with decreasing completeness. The source detection limit rises with increasing confusion level.

  The J, H and K_s differential PSC source counts, normalized by area, are shown in Figures 4 and 5 for a 702.8 deg² area with b>+75° and the 10°x10° area centered on l=55°,b=0°, respectively. In each figure, the blue line represents the J-band source density, the green line is H and the red line is K_s. Figure 4 shows that the high latitude PSC contains detections 0.5-1.0 magnitudes fainter than the nominal completeness limits. The turnover in the source counts in the Galactic plane field, shown in Figure 5, illustrates that the completeness limit of the PSC in high source density regions can be nearly 1 magnitude brighter than the north Galactic cap field because of confusion noise. The dependence of completeness with source density is illustrated in Figure 6 which shows an all-sky Galactic aitoff projection map of the K_s magnitude at which the differential source counts peak. The turnover in the source count curves is not a formal measure of completeness, but serves as a proxy to show the variation of the completeness across the sky. A detailed discussion of the variation of PSC source densities and counts is given in VI.7.





Figure 4	Figure 5	Figure 6

Photometry of point sources in 2MASS was done using different algorithms depending on how bright a source was relative to the saturation regimes of the Survey observations. The origin of the default magnitudes given for each source is specified by the rd_flg value. Sources that were not saturated on the 1.3 s "Read_2-Read_1" exposures, the vast majority of objects detected in the Survey, were measured using profile fit photometry. These have rd_flg="2" in the appropriate band. Sources that saturated the 1.3 s exposures, but not the 51 ms "Read_1" exposures where measured using aperture photometry on the short exposure frames, and are designated with rd_flg="1" in the appropriate bands. Sources that saturated even the 51 ms exposures have brightness estimates derived from 1-d radial profile fits of the non-saturated portions of their images on the 51 ms exposures. These sources have rd_flg="3" in the appropriate bands.

• Photometric Accuracy

  Figure 7 shows the average quoted J, H and K_s default magnitude measurement uncertainties in 0.2 mag bins plotted as a function of source magnitude for all PSC sources having b>+75°. The vertical error bars show the RMS dispersion in the mean uncertainties in each brightness bin and the dashed horizontal lines in each panel show the SNR=10 levels (<>=0.109 mag). The J-band panel is labeled with the rd_flg values in the appropriate brightness regimes.

  The measurement precision for bright, non-saturated sources (rd_flg="1" or "2") approaches a constant limit of 0.01-0.02 mags that is set by pixelization effects. The characteristic uncertainties increase towards fainter flux levels as background photon noise becomes important. The achieved SNR=10 levels in the north galactic pole field are on average fainter than the J=15.8, H=15.1 and K_s=14.3 mag specified in the Level 1 Requirements. The brightness estimates of the fully saturated sources (rd_flg="3") are of much poorer accuracy than non-saturated sources.

  Although the default magnitudes for most non-saturated (rd_flg="2") PSC sources are derived from profile-fit photometry, aperture photometry magnitudes are also supplied. For isolated sources, aperture photometry yields better precision than profile-fit photometry in the high signal-to-noise regime because errors in the point source profile templates dominate the uncertainties in those cases. At lower signal-to-noise ratios (fainter sources), where photon noise dominates the measurement statistics, profile-fitting yields better accuracy. This is illustrated in in Figures 8, 9 and 10, which show the average quoted J, H and K_s photometric uncertainties, respectively, for the profile-fit and aperture photometry of all non-saturated (rd_flg="2") PSC sources with b>+75°. The cross-over points where profile-fit and aperture photomety produce similar uncertainties on average occur at J~14, H~13 and K_s~12.5 mag for this region of the sky.

  The point source photometric sensitivity achieved by 2MASS varied with sky conditions, including atmospheric transparency, seeing, and emissive backgrounds, and with the level of confusion noise (VI.2). Quality assurance standards ensured that only data taken under conditions known to meet the sensitivity requirements for the survey were accepted. Figure 11 shows the spatial distribution of the average K_s magnitudes at which the mean measurement uncertainty is ~0.109 mag (SNR=10) in a galactic aitoff projection. Away from the Galactic Center, the SNR=10 level is usually fainter than the minimum of K_s=14.3 mag required for the Survey. The impact of confusion on the extracted photometry is seen by the degraded SNR=10 levels in and around the Galactic Center.





Figure 7	Figure 8	Figure 9	Figure 10

Figure 11





• Band-Band Photometric Performance

  The J-H-K_s color-color diagrams for the north Galactic cap and Galactic plane fields described in Figures 4 and 5 are shown in Figures 12 and 13, respectively. In these figures, the color-coding signifies the density of sources in color bins, with red showing the highest density and blue the lowest. The density scaling shown in each figure is relative, and specific to each sample. The expected tracks for dwarf and giant stars from Koorneef (1983, A&A, 128, 84) and Bessell & Brett (1988, PASP, 100, 1134) are overlaid as solid and dashed lines, respectively. The small offset between the dwarf and giant tracks and the locus of 2MASS source colors is a result of differences in the photometric systems (see VI.4b).

  The high density locus of source colors in the north Galactic pole field follows closely that expected for dwarf stars, with peaks in density corresponding to early M-dwarfs (J-H~0.65, H-K_s~0.15) and mid-G-dwarfs (J-H~0.30, H-K_s~0.07). The broad spread of colors seen in lower density is due to the predominance of low SNR measurements. The locus of sources extending from to the upper right in the Galactic Plane field diagram follows the reddening vector in J-H-K_s space, illustrating that there is a significant amount of foreground extinction along this line of sight. Figure 14 shows a log-scaled all-sky map of the mean J-H color of all PSC sources with J<15.8 and H<15.1 mag in 5 arcminute bins in Galactic aitoff projection. The colors of sources are strongly affected by extinction associated with the Plane of the Milky Way. The filamentary color structure seen in Figure 14 traces the structure seen in the all-sky map of IRAS 100 micron emission, which is shown in Figure 15. The Large and Small Magellanic clouds also stand out in the color map shown in Figure 11 because luminous, late-type giants are preferentially detected by 2MASS at the distance of those galaxies.

Figure 12	Figure 13	Figure 14	Figure 15

f. Astrometric Properties:

2MASS PSC positions are reconstructed in the International Celestial Reference System (ICRS) via the Tycho 2 Catalog and are accurate to 70-80 mas over the magnitude range of 9 < K_s < 14 mag. The astrometric accuracy of brighter sources is approximately 120 mas. Fainter sources have astrometric accuracies that decrease monotonically with decreasing source brightness.

The astrometric performance of 2MASS is summarized in Figure 16 which shows RMS position residuals of PSC sources plotted versus K_s magnitude measured against several different references, as described below and discussed in detail in VI.5. In this figure, the two upper panels show the cross-scan (approximately RA) position residuals, and the bottom two panels show the in-scan (approximately Dec) residuals. Sources observed from the northern 2MASS observatory are shown in the two left plots, and those observed from the southern observatory are shown in the right pair of plots. In each panel, the mean positional uncertainty on each axis quoted for PSC sources are shown by the dotted black lines.

• Internal Repeatability of Reconstructed Positions

  Sources that fall in the overlap region between 2MASS Tiles may be independently detected and measured more than once during the Survey. The green curves shown in each panel of Figure 16 represent the RMS of the differences in 2MASS positions measured for all multiply-detected sources in the overlap regions. The positions of sources in the 9 < K_s < 14 mag range are repeatable to 40-50 mas on both axes. Brighter sources, which are extracted primarily from the 51 ms "Read_1" exposures, exhibit slightly higher position residuals because of the effects of seeing on the short exposures. Sources with K_s > 14 mag show increasing residuals as the SNR of the extraction decreases.




• Reconstructed Precision of the Astrometric Reference Stars

  In Figure 17 are shown histograms of cross-scan (RA - left panel) and in-scan (Dec - right panel) offsets between reconstructed 2MASS positions and Tycho 2 catalog positions. The residual distributions are shown separately for Tycho 2 stars that were in the original Tycho 1 catalog (denoted by the black lines and Tycho 2(1)), and those for stars that are new to the Tycho 2 catalog (denoted by the red lines and Tycho 2(2)). The standard deviations of the 2MASS-Tycho 2(1) position offsets are 81 and 88 mas, along the cross-scan and in-scan axes, respectively. The residuals with respect to the stars new to Tycho 2 are slightly higher, 145 and 133 mas.

  The black and blue curves in Figure 16 show the RMS of 2MASS-Tycho-2(1) and 2MASS-Tycho-2(2) position differences, respectively, plotted versus K_s magnitude. 2MASS positions for stars with K_s > 9 mag show in-scan and cross-scan residuals of ~60 mas with respect to Tycho-2(1). Brighter stars have residuals of ~100 mas. The 2MASS-Tycho-2(2) residuals for fainter stars are systematically higher than the Tycho-2(1) residuals and with the UCAC residuals, as discussed below.

  Comparison with the Tycho 2 catalog is not the best assessment of 2MASS astrometric performance, though, because Tycho 2 was the primary astrometric reference for 2MASS, and because Tycho 2 stars are brighter than the vast majority of 2MASS sources.




• Astrometric Accuracy with Respect to UCAC

A better gauge of the 2MASS astrometric performance is provided by comparison with the U.S. Naval Observatory CCD Astrograph Catalog (UCAC). UCAC contains stars significantly fainter than Tycho 2, better sampling the 2MASS brightness range, and was not used in any way for 2MASS position reconstruction. UCAC has reported astrometric precision of 20 mas for stars with 10 < R < 14 mag, and ~70 mas for stars at the limiting magnitude of R=16 mag.

Figure 18 shows histograms of the in-scan (RA) and cross-scan (Dec) position differences between 2MASS and UCAC for nearly 5.2 million stars common to both catalogs. The standard deviation of 2MASS-UCAC position differences are 80 mas and 82 mas in the in-scan and cross-scan axes, respectively, which is consistent with the net residuals measured for Tycho-2(1). The red curves in Figure 16 show the RMS residuals between 2MASS and UCAC positions plotted as a function of 2MASS K_s magnitude. Stars in the range 9 < K_s < 14 mag have residuals of 70-80 mas. Brighter stars show residuals of 100-120 mas. The position residuals for stars fainter than K_s~14 mag begin to increase, indicating that the 2MASS astrometric accuracy is dominated by extraction uncertainties rather than uncertainties in mapping into the ICRS reference frame beyond this magnitude.

• Number of Possible Known Solar System Object Detections Identified in Catalog:     15,964

  The 2MASS All-Sky Release PSC contains 15,964 sources that are positionally associated with the predicted positions of known minor planets, comets, planets and planetary satellites. A number of these objects appear in the PSC multiple times because they moved to a region of sky covered by observations of a different Tile at a different time. For example, (52) Europa appears in the PSC five times, its position having been scanned on September 19 and 25, 1998 UT, twice on February 25, 2000 UT, and once again on March 14, 2000 UT. Some fraction of PSC sources associated with solar system objects are actually chance superpositions of the predicted positions with background sources, and not actual detections of the source. This is particularly likely at low Galactic latitudes where the density of background stars is large. Association with solar system objects is discussed in IV.9.

  2MASS is essentially a single-epoch survey, so systematic identification of previously uncatalogued asteroids was not possible. A comparison of the 2MASS PSC with the Sloan Digital Sky Survey Early Data Release sources (VI.1.ii) found that ~0.09% of the high-quality PSC sources are suspected uncatalogued asteroids in the 126 deg² searched. Extrapolating to the full sky suggests that there may be ~8,800 previously unknown asteroids in the PSC. However, this is likely an upper limit since the field used in the comparison is on the ecliptic plane.