Legacy Survey Files

Top level directory for web access:: https://portal.nersc.gov/cfs/cosmo/data/legacysurvey/dr6/
Top level directory local to NERSC computers (for collaborators):: /global/cfs/cdirs/cosmo/data/legacysurvey/dr6/

FITS binary table with the RA, DEC bounds of each geometrical "brick" on the sky. This includes all bricks on the sky, not just the ones in our footprint or with coverage in DR6. For that information, see the next file description.

Column	Type	Description
`BRICKNAME`	char[8]	Name of the brick.
`BRICKID`	int32	A unique integer with 1-to-1 mapping to `brickname`.
`BRICKQ`	int16	A "priority" factor used for processing.
`BRICKROW`	int32	Dec row number.
`BRICKCOL`	int32	Number of the brick within a Dec row.
`RA`	float64	RA of the center of the brick.
`DEC`	float64	Dec of the center of the brick.
`RA1`	float64	Lower RA boundary.
`RA2`	float64	Upper RA boundary.
`DEC1`	float64	Lower Dec boundary.
`DEC2`	float64	Upper Dec boundary.

survey-bricks-dr6.fits.gz

A FITS binary table with information that summarizes the contents of each brick for DR6.

Column	Type	Description
`brickname`	char[8]	Name of the brick
`ra`	float64	RA of the center of the brick
`dec`	float64	Dec of the center of the brick
`nexp_g`	int16	Median number of exposures in the unique area (i.e. `BRICK_PRIMARY` area) of the brick in g-band
`nexp_r`	int16	Median number of exposures in the unique area of the brick in r-band
`nexp_z`	int16	Median number of exposures in the unique area of the brick in z-band
`nexphist_g`	int32[6]	Histogram of number of pixels in the unique brick area with 0, 1, 2, 3, 4, or > 5 exposures in g
`nexphist_r`	int32[6]	Histogram of number of pixels in the unique brick area with 0, 1, 2, 3, 4, or > 5 exposures in r
`nexphist_z`	int32[6]	Histogram of number of pixels in the unique brick area with 0, 1, 2, 3, 4, or > 5 exposures in z
`nobjs`	int16	Total number of `BRICK_PRIMARY` objects in this brick, of all types
`npsf`	int16	Total number of `BRICK_PRIMARY` objects in this brick, of type `PSF`
`nsimp`	int16	Total number of `BRICK_PRIMARY` objects in this brick, of type `SIMP` (there should be 0 such objects)
`nrex`	int16	Total number of `BRICK_PRIMARY` objects in this brick, of type `REX`
`nexp`	int16	Total number of `BRICK_PRIMARY` objects in this brick, of type `EXP`
`ndev`	int16	Total number of `BRICK_PRIMARY` objects in this brick, of type `DEV`
`ncomp`	int16	Total number of `BRICK_PRIMARY` objects in this brick, of type `COMP`
`psfsize_g`	float32	Median PSF size, in arcsec, evaluated at the `BRICK_PRIMARY` objects in this brick in g-band
`psfsize_r`	float32	Median PSF size, in arcsec, evaluated at the `BRICK_PRIMARY` objects in this brick in r-band
`psfsize_z`	float32	Median PSF size, in arcsec, evaluated at the `BRICK_PRIMARY` objects in this brick in z-band
`psfdepth_g`	float32	5-sigma PSF detection depth in \(g\)-band (AB mag), using PsfEx PSF model
`psfdepth_r`	float32	5-sigma PSF detection depth in \(r\)-band (AB mag), using PsfEx PSF model
`psfdepth_z`	float32	5-sigma PSF detection depth in \(z\)-band (AB mag), using PsfEx PSF model
`galdepth_g`	float32	5-sigma galaxy (0.45" round exp) detection depth in \(g\)-band (AB) mag
`galdepth_r`	float32	5-sigma galaxy (0.45" round exp) detection depth in \(r\)-band (AB) mag
`galdepth_z`	float32	5-sigma galaxy (0.45" round exp) detection depth in \(z\)-band (AB) mag
`ebv`	float32	Median SFD dust map E(B-V) extinction, in magnitudes, evaluated at `BRICK_PRIMARY` objects in this brick
`trans_g`	float32	Median Milky Way dust transparency in \(g\)-band, based on `ebv`. See also `MW_TRANSMISSION_G`
`trans_r`	float32	Median Milky Way dust transparency in \(g\)-band, based on `ebv`. See also `MW_TRANSMISSION_R`
`trans_z`	float32	Median Milky Way dust transparency in \(z\)-band, based on `ebv`. See also `MW_TRANSMISSION_Z`
`ext_g`	float32	Extinction in \(g\)-band
`ext_r`	float32	Extinction in \(r\)-band
`ext_z`	float32	Extinction in \(z\)-band
`wise_nobs`	int16[4]	Number of images that contributed to WISE calculations in each filter (not profile-weighted)
`trans_wise`	float32[4]	Median Milky Way dust transparency in WISE bands, based on `ebv`. See also, e.g., `MW_TRANSMISSION_W1`
`ext_w1`	float32	Extinction in \(W1\)-band
`ext_w2`	float32	Extinction in \(W2\)-band
`ext_w3`	float32	Extinction in \(W3\)-band
`ext_w4`	float32	Extinction in \(W4\)-band

Note that, for the nexphist rows, pixels that are masked by the NOIRLab Community Pipeline as, e.g., cosmic rays or saturation, do NOT count toward the number of exposures. More information about the morphological types and MW_TRANSMISSION can be found on the catalogs page.

survey-ccds-*fits.gz

FITS binary table with almanac information about each individual CCD image in each band. There is one file for each of:

90prime-g: BASS \(g\)-band
90prime-r: BASS \(r\)-band
mosaic-z: MzLS \(z\)-band
dr6plus: Additional MzLS CCDs

These files contain information regarding the photometric and astrometric zero points for each CCD of every image that is part of the DR6 data release. Photometric zero points for each CCD are computed by identifying stars and comparing their instrumental magnitudes to color-selected stars in the PanSTARRS "qz" catalog.

The photometric zeropoints (zpt, ccdzpt, etc) are magnitude-like numbers (e.g. 25.04), and indicate the magnitude of a source that would contribute one count per second to the image. For example, in an image with zeropoint of 25.04 and exposure time of 30 seconds, a source of magnitude 22.5 would contribute \(30 * 10^{((25.04 - 22.5) / 2.5)} = 311.3\) counts.

Column	Type	Description
`image_filename`	char[55]	Path to FITS image, eg "decam/CP20140810_g_v2/c4d_140815_235218_ooi_g_v2.fits.fz"
`image_hdu`	int16	FITS HDU number in the `image_filename` file where this image can be found
`camera`	char[7]	The camera that took this image
`expnum`	int32	Exposure number, eg 348224
`ccdname`	char[4]	CCD name (see Legacy Survey camera layout), eg "N10", "S7"
`object`	char[24]	Name listed in the object tag from the CCD header
`propid`	char[10]	Proposal ID of the program that took this image, eg "2014B-0404"
`filter`	char[1]	Filter used for observation, eg "\(g\)", "\(r\)", "\(z\)"
`exptime`	float32	Exposure time in seconds, eg 30
`mjd_obs`	float64	Date of observation in MJD (in UTC system), eg 56884.99373389
`fwhm`	float32	FWHM of observation
`width`	int16	Width in pixels of this image, eg 2046
`height`	int16	Height in pixels of this image, eg 4096
`ra_bore`	float64	Telescope boresight RA of this exposure (deg)
`dec_bore`	float64	Telescope boresight Dec of this exposure (deg)
`crpix1`	float32	Astrometric header value: X reference pixel
`crpix2`	float32	Astrometric header value: Y reference pixel
`crval1`	float64	Astrometric header value: RA of reference pixel
`crval2`	float64	Astrometric header value: Dec of reference pixel
`cd1_1`	float32	Astrometric header value: transformation matrix
`cd1_2`	float32	Astrometric header value: transformation matrix
`cd2_1`	float32	Astrometric header value: transformation matrix
`cd2_2`	float32	Astrometric header value: transformation matrix
`ra`	float64	Approximate RA center of this CCD (deg)
`dec`	float64	Approximate Dec center of this CCD (deg)
`skyrms`	float32	Sky rms for the entire image (in counts)
`sig1`	float32	Median per-pixel error standard deviation, in nanomaggies
`ccdzpt`	float32	Zeropoint for the CCD (AB mag)
`zpt`	float32	Median zero point for the entire image (median of all CCDs of the image), eg 25.0927
`ccdraoff`	float32	Median astrometric offset for the CCD <Gaia-Legacy Survey> in arcsec
`ccddecoff`	float32	Median astrometric offset for the CCD <Gaia-Legacy Survey> in arcsec
`ccdskycounts`	float32	Mean sky count level per pixel in the CP-processed frames measured (with iterative rejection) for each CCD in the image section [500:1500,1500:2500]
`ccdrarms`	float32	rms in astrometric offset for the CCD <Gaia-Legacy Survey> in arcsec
`ccddecrms`	float32	rms in astrometric offset for the CCD <Gaia-Legacy Survey> in arcsec
`ccdphrms`	float32	Photometric rms for the CCD (in mag)
`ccd_cuts`	int32	(ignore)

survey-ccds-dr6plus.kd.fits

As for the survey-ccds-*.fits.gz files but limited by the depth of each observation. This file contains all of the CCDs actually used for the DR6 reductions. Columns are the same as for survey-ccds-*.fits.gz files.

ccds-annotated-*.fits.gz

Versions of each of the survey-ccds-*.fits.gz file with additional information gathered during calibration pre-processing before running the Tractor reductions. One each for

90prime-g: BASS \(g\)-band
90prime-r: BASS \(r\)-band
mosaic-z: MzLS \(z\)-band
mosaic-dr6plus: Additional MzLS images

Includes all of the columns in the survey-ccds-*.fits.gz file plus the following:

Column	Type	Description
`annotated`	boolean	(ignore)
`good_region`	int16[4]	If only a subset of the CCD images was used, this array of x0,x1,y0,y1 values gives the coordinates that were used, [x0,x1), [y0,y1). -1 for no cut (most CCDs)
`ra0`	float64	RA coordinate of pixel (1,1)...Note that the ordering of the CCD corners is detailed here
`dec0`	float64	Dec coordinate of pixel (1,1)
`ra1`	float64	RA coordinate of pixel (1,H)
`dec1`	float64	Dec coordinate of pixel (1,H)
`ra2`	float64	RA coordinate of pixel (W,H)
`dec2`	float64	Dec coordinate of pixel (W,H)
`ra3`	float64	RA coordinate of pixel (W,1)
`dec3`	float64	Dec coordinate of pixel (W,1)
`dra`	float32	Maximum distance from RA,Dec center to the edge midpoints, in RA
`ddec`	float32	Maximum distance from RA,Dec center to the edge midpoints, in Dec
`ra_center`	float64	RA coordinate of CCD center
`dec_center`	float64	Dec coordinate of CCD center
`meansky`	float32	Our pipeline (not the CP) estimate of the sky level, average over the image, in ADU.
`stdsky`	float32	Standard deviation of our sky level
`maxsky`	float32	Max of our sky level
`minsky`	float32	Min of our sky level
`pixscale_mean`	float32	Pixel scale (via sqrt of area of a 10x10 pixel patch evaluated in a 5x5 grid across the image), in arcsec/pixel.
`pixscale_std`	float32	Standard deviation of pixel scale
`pixscale_max`	float32	Max of pixel scale
`pixscale_min`	float32	Min of pixel scale
`psfnorm_mean`	float32	PSF norm = 1/sqrt of N_eff = sqrt(sum(psf_i^2)) for normalized PSF pixels i; mean of the PSF model evaluated on a 5x5 grid of points across the image. Point-source detection standard deviation is `sig1 / psfnorm`.
`psfnorm_std`	float32	Standard deviation of PSF norm
`galnorm_mean`	float32	Norm of the PSF model convolved by a 0.45" exponential galaxy.
`galnorm_std`	float32	Standard deviation of galaxy norm.
`psf_mx2`	float32	PSF model second moment in x (pixels^2)
`psf_my2`	float32	PSF model second moment in y (pixels^2)
`psf_mxy`	float32	PSF model second moment in x-y (pixels^2)
`psf_a`	float32	PSF model major axis (pixels)
`psf_b`	float32	PSF model minor axis (pixels)
`psf_theta`	float32	PSF position angle (deg)
`psf_ell`	float32	PSF ellipticity 1 - minor/major
`humidity`	float32	Percent humidity outside
`outtemp`	float32	Outside temperate (deg C).
`tileid`	int32	tile number, 0 for data from programs other than MzLS or DECaLS
`tilepass`	uint8	tile pass number, 1, 2 or 3, if this was an MzLS or DECaLS observation, or 0 for data from other programs. Set by the observers (the meaning of `tilepass` is on the status page)
`tileebv`	float32	Mean SFD E(B-V) extinction in the tile, 0 for data from programs other than BASS, MzLS or DECaLS
`plver`	char[6]	Community Pipeline (CP) PLVER version string
`ebv`	float32	SFD E(B-V) extinction for CCD center
`decam_extinction`	float32[6]	Extinction for optical filters \(ugrizY\)
`wise_extinction`	float32[4]	Extinction for WISE bands W1,W2,W3,W4
`psfdepth`	float32	5-sigma PSF detection depth in AB mag, using PsfEx PSF model
`galdepth`	float32	5-sigma galaxy (0.45" round exp) detection depth in AB mag
`gausspsfdepth`	float32	5-sigma PSF detection depth in AB mag, using Gaussian PSF approximation (using `seeing` value)
`gaussgaldepth`	float32	5-sigma galaxy detection depth in AB mag, using Gaussian PSF approximation

Note that two columns have different formats between the survey-ccds-*.fits.gz and ccds-annotated-*.fits.gz files. The camera column is char[6] and the object column is char[37].

dr6-depth.fits.gz

A concatenation of the depth histograms for each brick, from the coadd/*/*/*-depth.fits tables. HDU1 contains histograms that describe the number of pixels in each brick with a 5-sigma AB depth in the given magnitude bin. HDU2 contains the bin edges of the histograms.

HDU1

Column	Type	Description
`counts_ptsrc_g`	int32[50]	Histogram of pixels for point source depth in \(g\) band
`counts_gal_g`	int32[50]	Histogram of pixels for canonical galaxy depth in \(g\) band
`counts_ptsrc_r`	int32[50]	Histogram of pixels for point source depth in \(r\) band
`counts_gal_r`	int32[50]	Histogram of pixels for canonical galaxy depth in \(r\) band
`counts_ptsrc_z`	int32[50]	Histogram of pixels for point source depth in \(z\) band
`counts_gal_z`	int32[50]	Histogram of pixels for canonical galaxy depth in \(z\) band
`brickname`	char[8]	Name of the brick

HDU2

Column	Type	Description
`depthlo`	float32	Lower bin edge for each histogram in HDU1 (5-sigma AB depth)
`depthhi`	float32	Upper bin edge for each histogram in HDU1 (5-sigma AB depth)

dr6-depth-summary.fits.gz

A summary of the depth histogram of the whole DR6 survey. FITS table with the following columns:

Column	Type	Description
`depthlo`	float32	Lower limit of the depth bin
`depthhi`	float32	Upper limit of the depth bin
`counts_ptsrc_g`	int64	Number of pixels in histogram for point source depth in \(g\) band
`counts_gal_g`	int64	Number of pixels in histogram for canonical galaxy depth in \(g\) band
`counts_ptsrc_r`	int64	Number of pixels in histogram for point source depth in \(r\) band
`counts_gal_r`	int64	Number of pixels in histogram for canonical galaxy depth in \(r\) band
`counts_ptsrc_z`	int64	Number of pixels in histogram for point source depth in \(z\) band
`counts_gal_z`	int64	Number of pixels in histogram for canonical galaxy depth in \(z\) band

The depth histogram goes from magnitude of 20.1 to 24.9 in steps of 0.1 mag. The first and last bins are "catch-all" bins: 0 to 20.1 and 24.9 to 100, respectively. The histograms count the number of pixels in each brick's unique area with the given depth. These numbers can be turned into values in square degrees using the brick pixel area of 0.262 arcseconds square. These depth estimates take into account the small-scale masking (cosmic rays, edges, saturated pixels) and detailed PSF model.

External Files

The Legacy Survey photometric catalogs have been matched to the following external spectroscopic files from the SDSS, which can be accessed through the web at:: https://portal.nersc.gov/cfs/cosmo/data/legacysurvey/dr6/external/
Or on the NERSC computers (for collaborators) at:: /global/cfs/cdirs/cosmo/data/legacysurvey/dr6/external/

Each row of each external-match file contains the full record of the nearest object in our Tractored survey imaging catalogs, matched at a radius of 1.0 arcsec. The structure of the imaging catalog files is documented on the catalogs page. If no match is found, then OBJID is set to -1.

In addition to the columns from the Tractor catalogs, we have added columns from the SDSS files that can be used to track objects uniquely. These are typically some combination of PLATE, FIBER, MJD (or SMJD) and, in some cases, RERUN.

survey-dr6-specObj-dr14.fits

HDU1 (the only HDU) contains Tractored survey photometry that is row-by-row-matched to the SDSS DR14 spectrosopic pipeline file such that the photometric parameters in row "N" of survey-dr6-specObj-dr14.fits matches the spectroscopic parameters in row "N" of specObj-dr14.fits. The spectroscopic file is documented in the SDSS DR14 data model for specObj-dr14.fits.

survey-dr6-dr14Q_v4_4.fits

HDU1 (the only HDU) contains Tractored survey photometry that is row-by-row-matched to the SDSS DR14 (partially) visually inspected quasar catalog (Paris et al. 2018) such that the photometric parameters in row "N" of survey-dr6-dr14Q_v4_4.fits matches the spectroscopic parameters in row "N" of DR14Q_v4_4.fits. The spectroscopic file is documented in the SDSS DR14 data model for DR14Q_v4_4.fits.

survey-dr6-dr12Q.fits

HDU1 (the only HDU) contains Tractored survey photometry that is row-by-row-matched to the SDSS DR12 visually inspected quasar catalog (Paris et al. 2017) such that the photometric parameters in row "N" of survey-dr6-dr12Q.fits matches the spectroscopic parameters in row "N" of DR12Q.fits. The spectroscopic file is documented in the SDSS DR12 data model for DR12Q.fits.

survey-dr6-superset-dr12Q.fits

HDU1 (the only HDU) contains Tractored survey photometry that is row-by-row-matched to the superset of all SDSS DR12 spectroscopically confirmed objects that were visually inspected as possible quasars (Paris et al. 2017) such that the photometric parameters in row "N" of survey-dr6-Superset_dr12Q.fits matches the spectroscopic parameters in row "N" of Superset_DR12Q.fits. The spectroscopic file is documented in the SDSS DR12 data model for Superset_DR12Q.fits.

survey-dr6-dr7Q.fits

HDU1 (the only HDU) contains Tractored survey photometry that is row-by-row-matched to the SDSS DR7 visually inspected quasar catalog (Schneider et al. 2010) such that the photometric parameters in row "N" of survey-dr6-dr7Q.fits matches the spectroscopic parameters in row "N" of DR7qso.fit. The spectroscopic file is documented on the DR7 quasar catalog description page.

Tractor Catalogs

In the file listings outlined below:

brick names (<brick>) have the format <AAAa>c<BBB> where A, a and B are digits and c is either the letter m or p (e.g. 1126p222). The names are derived from the (RA, Dec) center of the brick. The first four digits are \(int(RA \times 10)\), followed by p to denote positive Dec or m to denote negative Dec ("plus"/"minus"), followed by three digits of \(int(Dec \times 10)\). For example the case 1126p222 corresponds to (RA, Dec) = (112.6°, +22.2°).
<brickmin> and <brickmax> denote the corners of a rectangle in (RA, Dec). Explicitly, <brickmin> has the format <AAA>c<BBB> where <AAA> denotes three digits of the minimum \(int(RA)\) in degrees, <BBB> denotes three digits of the minimum \(int(Dec)\) in degrees, and c uses the p/m ("plus"/"minus") format outlined in the previous bullet point. The convention is similar for <brickmax> and the maximum RA and Dec. For example 000m010-010m005 would correspond to a survey region limited by \(0^\circ \leq RA < 10^\circ\) and \(-10^\circ \leq Dec < -5^\circ\).
sub-directories are listed by the RA of the brick center, and sub-directory names (<AAA>) correspond to RA. For example 002 corresponds to brick centers between an RA of 2° and an RA of 3°.
<filter> denotes the \(g\), \(r\) or \(z\) band, using the corresponding letter.

Note that it is not possible to go from a brick name back to an exact (RA, Dec) center (the bricks are not on 0.1° grid lines). The exact brick center for a given brick name can be derived from columns in the survey-bricks.fits.gz file (i.e. brickname, ra, dec).

tractor/<AAA>/tractor-<brick>.fits

FITS binary table containing Tractor photometry, documented on the catalogs page.

Users interested in database access to the Tractor Catalogs can contact the Astro Data Lab [1] at datalab@noirlab.edu.

Sweep Catalogs

sweep/6.0/sweep-<brickmin>-<brickmax>.fits

The sweeps are light-weight FITS binary tables (containing a subset of the most commonly used Tractor measurements) of all the Tractor catalogs for which BRICK_PRIMARY==T in rectangles of RA, Dec. In addition to the columns listed below, the columns pertaining to optical data also have \(U\), \(I\) and \(Y\)-band entries (e.g. FLUX_U, FLUX_I, FLUX_Y), but, in DR6, these extra columns contain only zeros.

Name	Type	Units	Description
`RELEASE`	int32		Unique integer denoting the camera and filter set used (RELEASE is documented here)
`BRICKID`	int32		Brick ID [1,662174]
`BRICKNAME`	char[8]		Name of brick, encoding the brick sky position, eg "1126p222" near RA=112.6, Dec=+22.2
`OBJID`	int32		Catalog object number within this brick; a unique identifier hash is `BRICKID,OBJID`; `OBJID` spans [0,N-1] and is contiguously enumerated within each blob
`TYPE`	char[4]		Morphological model: "PSF"=stellar, "REX"="round exponential galaxy" = round EXP galaxy with a variable radius, "EXP"=exponential, "DEV"=deVauc, "COMP"=composite. Note that in some FITS readers, a trailing space may be appended for "PSF ", "EXP " and "DEV " since the column data type is a 4-character string
`RA`	float64	deg	Right ascension at equinox J2000
`DEC`	float64	deg	Declination at equinox J2000
`RA_IVAR`	float32	1/deg²	Inverse variance of `RA` (no cosine term!), excluding astrometric calibration errors
`DEC_IVAR`	float32	1/deg²	Inverse variance of `DEC`, excluding astrometric calibration errors
`DCHISQ`	float32[5]		Difference in χ² between successively more-complex model fits: PSF, REX, DEV, EXP, COMP. The difference is versus no source.
`EBV`	float32	mag	Galactic extinction E(B-V) reddening from SFD98, used to compute `MW_TRANSMISSION`
`FLUX_G`	float32	nanomaggies	model flux in \(g\)
`FLUX_R`	float32	nanomaggies	model flux in \(r\)
`FLUX_Z`	float32	nanomaggies	model flux in \(z\)
`FLUX_W1`	float32	nanomaggies	WISE model flux in \(W1\)
`FLUX_W2`	float32	nanomaggies	WISE model flux in \(W2\)
`FLUX_W3`	float32	nanomaggies	WISE model flux in \(W3\)
`FLUX_W4`	float32	nanomaggies	WISE model flux in \(W4\)
`FLUX_IVAR_G`	float32	1/nanomaggies²	Inverse variance of `FLUX_G`
`FLUX_IVAR_R`	float32	1/nanomaggies²	Inverse variance of `FLUX_R`
`FLUX_IVAR_Z`	float32	1/nanomaggies²	Inverse variance of `FLUX_Z`
`FLUX_IVAR_W1`	float32	1/nanomaggies²	Inverse variance of `FLUX_W1`
`FLUX_IVAR_W2`	float32	1/nanomaggies²	Inverse variance of `FLUX_W2`
`FLUX_IVAR_W3`	float32	1/nanomaggies²	Inverse variance of `FLUX_W3`
`FLUX_IVAR_W4`	float32	1/nanomaggies²	Inverse variance of `FLUX_W4`
`MW_TRANSMISSION_G`	float32		Galactic transmission in \(g\) filter in linear units [0,1]
`MW_TRANSMISSION_R`	float32		Galactic transmission in \(r\) filter in linear units [0,1]
`MW_TRANSMISSION_Z`	float32		Galactic transmission in \(z\) filter in linear units [0,1]
`MW_TRANSMISSION_W1`	float32		Galactic transmission in \(W1\) filter in linear units [0,1]
`MW_TRANSMISSION_W2`	float32		Galactic transmission in \(W2\) filter in linear units [0,1]
`MW_TRANSMISSION_W3`	float32		Galactic transmission in \(W3\) filter in linear units [0,1]
`MW_TRANSMISSION_W4`	float32		Galactic transmission in \(W4\) filter in linear units [0,1]
`NOBS_G`	int16		Number of images that contribute to the central pixel in \(g\): filter for this object (not profile-weighted)
`NOBS_R`	int16		Number of images that contribute to the central pixel in \(r\): filter for this object (not profile-weighted)
`NOBS_Z`	int16		Number of images that contribute to the central pixel in \(z\): filter for this object (not profile-weighted)
`NOBS_W1`	int16		Number of images that contribute to the central pixel in \(W1\): filter for this object (not profile-weighted)
`NOBS_W2`	int16		Number of images that contribute to the central pixel in \(W2\): filter for this object (not profile-weighted)
`NOBS_W3`	int16		Number of images that contribute to the central pixel in \(W3\): filter for this object (not profile-weighted)
`NOBS_W4`	int16		Number of images that contribute to the central pixel in \(W4\): filter for this object (not profile-weighted)
`RCHISQ_G`	float32		Profile-weighted χ² of model fit normalized by the number of pixels in \(g\)
`RCHISQ_R`	float32		Profile-weighted χ² of model fit normalized by the number of pixels in \(r\)
`RCHISQ_Z`	float32		Profile-weighted χ² of model fit normalized by the number of pixels in \(z\)
`RCHISQ_W1`	float32		Profile-weighted χ² of model fit normalized by the number of pixels in \(W1\)
`RCHISQ_W2`	float32		Profile-weighted χ² of model fit normalized by the number of pixels in \(W2\)
`RCHISQ_W3`	float32		Profile-weighted χ² of model fit normalized by the number of pixels in \(W3\)
`RCHISQ_W4`	float32		Profile-weighted χ² of model fit normalized by the number of pixels in \(W4\)
`FRACFLUX_G`	float32		Profile-weighted fraction of the flux from other sources divided by the total flux in \(g\) (typically [0,1])
`FRACFLUX_R`	float32		Profile-weighted fraction of the flux from other sources divided by the total flux in \(r\) (typically [0,1])
`FRACFLUX_Z`	float32		Profile-weighted fraction of the flux from other sources divided by the total flux in \(z\) (typically [0,1])
`FRACFLUX_W1`	float32		Profile-weighted fraction of the flux from other sources divided by the total flux in \(W1\) (typically [0,1])
`FRACFLUX_W2`	float32		Profile-weighted fraction of the flux from other sources divided by the total flux in \(W2\) (typically [0,1])
`FRACFLUX_W3`	float32		Profile-weighted fraction of the flux from other sources divided by the total flux in \(W3\) (typically [0,1])
`FRACFLUX_W4`	float32		Profile-weighted fraction of the flux from other sources divided by the total flux in \(W4\) (typically [0,1])
`FRACMASKED_G`	float32		Profile-weighted fraction of pixels masked from all observations of this object in \(g\), strictly between [0,1]
`FRACMASKED_R`	float32		Profile-weighted fraction of pixels masked from all observations of this object in \(r\), strictly between [0,1]
`FRACMASKED_Z`	float32		Profile-weighted fraction of pixels masked from all observations of this object in \(z\), strictly between [0,1]
`FRACIN_G`	float32		Fraction of a source's flux within the blob in \(g\), near unity for real sources
`FRACIN_R`	float32		Fraction of a source's flux within the blob in \(r\), near unity for real sources
`FRACIN_Z`	float32		Fraction of a source's flux within the blob in \(z\), near unity for real sources
`ANYMASK_G`	int16		Bitwise mask set if the central pixel from any image satisfies each condition in \(g\)
`ANYMASK_R`	int16		Bitwise mask set if the central pixel from any image satisfies each condition in \(r\)
`ANYMASK_Z`	int16		Bitwise mask set if the central pixel from any image satisfies each condition in \(z\)
`ALLMASK_G`	int16		Bitwise mask set if the central pixel from all images satisfy each condition in \(g\)
`ALLMASK_R`	int16		Bitwise mask set if the central pixel from all images satisfy each condition in \(r\)
`ALLMASK_Z`	int16		Bitwise mask set if the central pixel from all images satisfy each condition in \(z\)
`WISEMASK_W1`	uint8		W1 bright star bitmask, \(2^0\) \((2^1)\) for southward (northward) scans
`WISEMASK_W2`	uint8		W2 bright star bitmask, \(2^0\) \((2^1)\) for southward (northward) scans
`PSFSIZE_G`	float32	arcsec	Weighted average PSF FWHM in the \(g\) band
`PSFSIZE_R`	float32	arcsec	Weighted average PSF FWHM in the \(r\) band
`PSFSIZE_Z`	float32	arcsec	Weighted average PSF FWHM in the \(z\) band
`PSFDEPTH_G`	float32	1/nanomaggies²	For a \(5\sigma\) point source detection limit in \(g\), \(5/\sqrt(\mathrm{PSFDEPTH\_G})\) gives flux in nanomaggies and \(-2.5[\log_{10}(5 / \sqrt(\mathrm{PSFDEPTH\_G})) - 9]\) gives corresponding magnitude
`PSFDEPTH_R`	float32	1/nanomaggies²	For a \(5\sigma\) point source detection limit in \(g\), \(5/\sqrt(\mathrm{PSFDEPTH\_R})\) gives flux in nanomaggies and \(-2.5[\log_{10}(5 / \sqrt(\mathrm{PSFDEPTH\_R})) - 9]\) gives corresponding magnitude
`PSFDEPTH_Z`	float32	1/nanomaggies²	For a \(5\sigma\) point source detection limit in \(g\), \(5/\sqrt(\mathrm{PSFDEPTH\_Z})\) gives flux in nanomaggies and \(-2.5[\log_{10}(5 / \sqrt(\mathrm{PSFDEPTH\_Z})) - 9]\) gives corresponding magnitude
`GALDEPTH_G`	float32	1/nanomaggies²	As for `PSFDEPTH_G` but for a galaxy (0.45" exp, round) detection sensitivity
`GALDEPTH_R`	float32	1/nanomaggies²	As for `PSFDEPTH_R` but for a galaxy (0.45" exp, round) detection sensitivity
`GALDEPTH_Z`	float32	1/nanomaggies²	As for `PSFDEPTH_Z` but for a galaxy (0.45" exp, round) detection sensitivity
`WISE_COADD_ID`	char[8]		unWISE coadd file name for the center of each object
`FRACDEV`	float32		Fraction of model in deVauc [0,1]
`FRACDEV_IVAR`	float32		Inverse variance of `FRACDEV`
`SHAPEDEV_R`	float32	arcsec	Half-light radius of deVaucouleurs model (>0)
`SHAPEDEV_R_IVAR`	float32	1/arcsec	Inverse variance of `SHAPEDEV_R`
`SHAPEDEV_E1`	float32		Ellipticity component 1
`SHAPEDEV_E1_IVAR`	float32		Inverse variance of `SHAPEDEV_E1`
`SHAPEDEV_E2`	float32		Ellipticity component 2
`SHAPEDEV_E2_IVAR`	float32		Inverse variance of `SHAPEDEV_E2`
`SHAPEEXP_R`	float32	arcsec	Half-light radius of exponential model (>0)
`SHAPEEXP_R_IVAR`	float32	1/arcsec2	Inverse variance of `SHAPEEXP_R`
`SHAPEEXP_E1`	float32		Ellipticity component 1
`SHAPEEXP_E1_IVAR`	float32		Inverse variance of `SHAPEEXP_E1`
`SHAPEEXP_E2`	float32		Ellipticity component 2
`SHAPEEXP_E2_IVAR`	float32		Inverse variance of `SHAPEEXP_E2`

Image Stacks

Image stacks are on tangent-plane (WCS TAN) projections, 3600 × 3600 pixels, at 0.262 arcseconds per pixel.

coadd/<AAA>/<brick>/legacysurvey-<brick>-ccds.fits

FITS binary table with the list of CCD images that were used in this brick. Contains the same columns as survey-ccds-dr6plus.kd.fits, and also contains the additional columns:

Column	Type	Description
`ccd_cuts`	int32	(ignore)
`ccd_x0`	int16	Minimum x image coordinate overlapping this brick
`ccd_y0`	int16	Minimum y image coordinate overlapping this brick
`ccd_x1`	int16	Maximum x image coordinate overlapping this brick
`ccd_y1`	int16	Maximum y image coordinate overlapping this brick
`brick_x0`	int16	Minimum x brick image coordinate overlapped by this image
`brick_x1`	int16	Maximum x brick image coordinate overlapped by this image
`brick_y0`	int16	Minimum y brick image coordinate overlapped by this image
`brick_y1`	int16	Maximum y brick image coordinate overlapped by this image
`psfnorm`	float32	Same as `psfnorm` in the ccds-annotated- file
`galnorm`	float32	Same as `galnorm` in the ccds-annotated- file
`plver`	char[4]	Community Pipeline (CP) version
`skyver`	char[19]	Git version of the sky calibration code
`wcsver`	char[1]	Git version of the WCS calibration code
`psfver`	char[12]	Git version of the PSF calibration code
`skyplver`	char[4]	CP version of the input to sky calibration
`wcsplver`	char[4]	CP version of the input to WCS calibration
`psfplver`	char[4]	CP version of the input to PSF calibration

coadd/<AAA>/<brick>/legacysurvey-<brick>-image-<filter>.fits
Stacked image centered on a brick location covering 0.25° × 0.25°. The primary HDU contains the coadded image (inverse-variance weighted coadd), in units of nanomaggies per pixel.
- NOTE: These are not the images used by Tractor, which operates on the single-epoch images.
- NOTE: that these images are resampled using Lanczos-3 resampling.
coadd/<AAA>/<brick>/legacysurvey-<brick>-invvar-<filter>.fits
Corresponding stacked inverse variance image based on the sum of the inverse-variances of the individual input images in units of 1/(nanomaggies)² per pixel.
- NOTE: These are not the inverse variance maps used by Tractor, which operates on the single-epoch images.
coadd/<AAA>/<brick>/legacysurvey-<brick>-model-<filter>.fits.gz
Stacked model image centered on a brick location covering 0.25° × 0.25°.
- The Tractor's idea of what the coadded images should look like; the Tractor's model prediction.
coadd/<AAA>/<brick>/legacysurvey-<brick>-chi2-<filter>.fits

Stacked χ² image, which is approximately the summed χ² values from the single-epoch images.
coadd/<AAA>/<brick>/legacysurvey-<brick>-depth-<filter>.fits.gz
Stacked depth map in units of the point-source flux inverse-variance at each pixel.
- The 5σ point-source depth can be computed as \(5 / \sqrt(\mathrm{depth\_ivar})\) .
coadd/<AAA>/<brick>/legacysurvey-<brick>-galdepth-<filter>.fits.gz
Stacked depth map in units of the canonical galaxy flux inverse-variance at each pixel. The canonical galaxy is an exponential profile with effective radius 0.45" and round shape.
- The 5σ galaxy depth can be computed as \(5 / \sqrt(\mathrm{galdepth\_ivar})\) .
coadd/<AAA>/<brick>/legacysurvey-<brick>-nexp-<filter>.fits.gz

Number of exposures contributing to each pixel of the stacked images.
coadd/<AAA>/<brick>/legacysurvey-<brick>-image.jpg

JPEG image of calibrated image using the \(g,r,z\) filters as the colors.
coadd/<AAA>/<brick>/legacysurvey-<brick>-model.jpg

JPEG image of the Tractor's model image using the \(g,r,z\) filters as the colors.
coadd/<AAA>/<brick>/legacysurvey-<brick>-resid.jpg

JPEG image of the residual image (data minus model) using the \(g,r,z\) filters as the colors.

Raw Data

See the raw data page.

Footnotes