WFC3/IR G102 calibration and reference files
The configuration and calibration files presented in this page are in the correct format to be used with the aXe extraction software and the aXeSIM simulation software. The files linked here are based on the latest available calibrations. Older files can be found in the WFC3 FTP directory. To use these calibration products with aXe and aXeSIM, copy them into a directory and set your AXE_CONFIG_PATH environment variable to point to that directory.
Download All Files
All Files: WFC3.IR.G102.cal.V4.32.tar.gz
|Reference Filter||Configuration File|
v2.0 Configuration file calibrated to the F098M direct image: WFC3.IR.G102.V2.0.conf
Senstitivity, Flat Field, Master Sky Files
|Master Sky Image:||WFC3.IR.G102.sky.V1.0.fits.gz|
Additional information on the grism sky subtraction is provided on the WFC3 grism master sky page.
Calibrations are derived based on object positions determined from F098M direct imaging. Offsets from WFC3 ISR 2010-12 should be applied if positions are determined from imaging in other filters.
The master sky image should only be applied to data reprocessed using calwf3 v2.0 or later. It is also necessary to use them together with the aXe configuration file WFC3.IR.G102.V1.0.conf or later. WFC3 ISR 2011-01 gives details of how the master sky images were created.
Feb 5, 2016: Updated configuration files are now avaialble for a range of grism-filter combinations. Details on the data analysis will be provided in an upcoming ISR (Pirzkal et al., 2016).
Jan 24, 2011: Updated G102 sensitivity, flat-field, and configuration files are available, based on additional analysis of standard star data obtained in Cycle 17. The new files are designated as version 2. Note that the zeroth-order sensitivity file remains at version 1. Details of the data analysis are given in WFC3 ISR 2011-05.
Nov 23, 2010: An updated G102 configuration file (V1.5) is available, which contains changes to fix a problem encountered when using the 'fluxcube' method in aXe to produce a contamination image. It was noticed that the zeroth-order spectra were not showing up in the contamination image and therefore that order was being neglected when estimating the contamination in spectra. The V1.5 configuration files contain appropriate changes to the definitions for the zeroth-order spectra (BEAM B) to fix this problem.