Note to users: the PHOTFLAM values provided in the image header for UVIS1 (sci,2 or ext4) are the correct values to use for both UVIS1 and UVIS2; they are calculated for an infinite aperture. Ignore the PHOTFLAM values given in the UVIS2 image headers. The values in these tables are slightly out of date compared to the PHOTFLAM value in the header, and differ from the header values by ~1% or so (depending on the filter).
For WFC3, zeropoints represent the magnitude corresponding to a (flat-field corrected) count rate of 1 e ⋅ s -1, and thus can be used to convert instrumental to astrophysical units. The tables below summarize results determined from a new reduction of all SMOV4, Cycle 17, and Cycle 18 observations of GD153, G191B2B, GD71, and P330E. The independent calibrations from the four stars agree to within 1% in most filters, and the photometric zeropoint is set to the average of the measurements. This is a substantial improvement over the previous calibration, where a filter-specific solution was not calculated (i.e., a smooth curve was across all wavelengths, ignoring small departures). For the first time, the new data sets have been processed using the new AstroDrizzle software and with the newly released WFC3 flat fields. For the UVIS camera, these flats are substantially better than the previous generation (i.e., more spatially stable given the removal of the "flare").
The results from this analysis will replace the existing calibration of the WFC3 photometric sensitivity in the file headers, and also define new throughput tables for synphot (e.g., the ETC) and CDBS. Changes in the zeropoints are less than 2% for most filters.
The methodology used to determine the zeropoints will be described in a forthcoming ISR.
Zeropoint tables after March 06, 2012:
For an infinite aperture:
For a 0.4 arcsec radius aperture:
Zeropoint tables prior to March 06, 2012:IR
Aperture Corrections and Encircled Energy CurvesAperture Corrections and EE curves for WFC3/UVIS
Aperture Corrections and EE curves for WFC3/IR
- VEGAmag : SYNPHOT standard magnitude system, for which Vega by definition has magnitude 0 at all wavelengths. The vega magnitude of a star with flux F is -2.5 log10 (F/F_vega) where F_vega is the calibrated spectrum of Vega in Synphot.
- STmag and ABmag:
both systems define an equivalent flux
density for a source, corresponding to the flux density of a source
of predefined spectral shape that would produce the observed count
rate, and convert this equivalent flux to a magnitude. The
conversion is chosen so that the magnitude in V corresponds roughly
to that in the Johnson system. In the STmag system, the flux density
is expressed per unit wavelength, and the reference spectrum is flat
in F_lam , while in the ABmag system, the flux density is expressed
per unit frequency , and the reference spectrum is flat in F_nu.
The definitions are:
- STmag = -2.5 Log F_lam -21.10
- ABmag = -2.5 Log F_nu - 48.6
Photometric Keywords in the SCI extention of WFC3 images:(keywords affected by the sensitivity curve update are highlighted)
- PHOTMODE: Observation configuration for photometric calibration.
- PHOTFLAM: inverse sensitivity (erg cm-2 s-1 Ang-1).
- PHOTZPT: ST magnitude zeropopint (= 21.10).
- PHOTPLAM: pivot wavelength.
- STMAG_ZEROPOINT = -2.5 Log (PHOTFLAM) - PHOTZPT = -2.5 Log (PHOTFLAM) - 21.10
- ABMAG_ZEROPOINT = -2.5 Log (PHOTFLAM) - 21.10 - 5 Log (PHOTPLAM) + 18.6921
Users performing photometry on non-drizzled _flt images may wish to read the description of the pixel area map.Created 09/09/2009 MJD
Modified 03/06/2012 by CMP