Parameters
Select which parameters you want to examine:
 Object parameters (e.g.  'P001', 'P002', etc. tables)
 POSS I Field parameters ('plates' table)
 Astrometric Fit Parameters ('astrom' table)
 Photometric Fit Parameters ('photom' table)
 Photometric Standards ('standards' table)
 POSS I scanned data removed from MAPS Catalog ('cuts' table)
 All the parameters in the MAPS Catalog database (list all of the above)
'photom' Table Parameters
The 'photom' database table stores information describing the photometric fits performed (both for 'stellar' and 'integrated' magnitudes) for each POSS I plate in the MAPS Catalog. The following photometric fit parameters are stored for each field in the MAPS Catalog:
Field Name  Definition 

possfield  MAPS POSS I Field Name 
possnumber  MAPS POSS I Field Number 
emul  The emulsion of the plate. Either 'O' for the bluesensitive Kodak 103aO emulsion and 'E' for the redsensitive Kodak 103aE emulsion. The plot below shows the spectral response of these emulsions versus UBVRI filters. 
sb0, r0, beta, rm, gamma  These are the values of the coefficients used in the fit
of the diametermagnitude relation used to determine the magnitude of a
pointlike (nonextended) object. The function fit was a variant of the King and Kormendy form of the PSF functions (King (1971) and Kormendy (1973)) and has the form: mag(diam) = SB0 + 2.5 log10[(1+(diam/R0)^2)^BETA + (diam/RM)^GAMMA]where "diam" is the "areal" diameter in EREs (By "areal" diameter, we mean the diameter determined by taking the surface area of the scanned object in square EREs, and then computing the diameter of a circle with the same area.). The five parameters fit to the data are SB0, BETA, R0, GAMMA, and RM. This fit is accomplished via a nonlinear least squares fit and is done independently for the O and E plates. 
Nstars  Number of stars used in the fit 
Nflag  Number of stars flagged and not used in the fit 
calsrc  Photometric calibration sources on the O and E plates, respectively.

mindia, maxdia  The "areal" diameters (in ERE) of the smallest and largest stars used in the fit 
rms  The RMS of the entire fit for the diametermagnitude relation. If undefined, its value is set to "99.9000". 
rms_08_14  The RMS of fit for the diametermagnitude relation between 8th and 14th magnitude. If undefined, its value is set to "99.9000". 
rms_14_20  The RMS of fit for the diametermagnitude relation between 14th and 20th magnitude. If undefined, its value is set to "99.9000". 
rms_20_22  The RMS of fit for the diametermagnitude relation between 20th and 22th magnitude. If undefined, its value is set to "99.9000". 
D_sky  The photographic grain density of the sky determined from a lowresolution background scan of the plate. 
D_max, alpha_DI, beta_DI, gamma_DI  The densitytointensity relation used to compute the integrated
magnitudes of nonstellar (galactic) images is fit by a function developed by
Greg Aldering The densitytointensity function is assumed to have
a form:
D(I) = D_MAX*(1  exp[ALPHA*(I^(BETA*(I^GAMMA)))])motivated by a physical model for response of photographic grains to incoming photons. Note that in addition to the four parameters fit (ALPHA, BETA, GAMMA, and D_MAX), the intensity I in the above equation is (I_STAR+I_SKY)/I_REF, so I_SKY is another parameter to be fit. As before, the fit is performed independently on the O and E plates. This allows a check of the DtoI transformation using the fit I_SKY. 
I_sky  Estimate of the sky intensity based the sky density and the fit of D(I).
This sky intensity cooresponds to flux per square ERE on the and so one could convert this to sky surface brightness, mu_sky, in mag/arcsecond^2, can be computed from this intensity using the relation:
mu_sky = 2.5*log10(I_sky/(ERE^2/arcsecond^2))where (ERE^2/arcsecond^2) = (0.0245 ERE/arcsecond)^2. 
I_ref  Estimate of the reference intensity. 
I_thresh  Estimate of the threshold intensity. 
seeing  The seeing of the sky are determined by the PSF of stars used in fitting the densitytointensity relation. 