Such as generated by make_spectral_flats(). Pixel-by-pixel sensitivity correction map (i.e., flat field), Slitloss correction map (i.e., for slits of nonuniform width), Name into which final, calibrated file should be written. INPUTS:ДЇilename of raw, uncalibrated science frame (in ADUs, not electrons) outfn : str Note that the dispersion direction should be вЂhorizontalвЂ™ Non-uniform slit widths (which cause non-smooth backgrounds) Pixel-to-pixel nonuniformities (i.e., traditional flat-fielding) calibrate_stared_mosfire_spectra ( scifn, outfn, skycorrect, pixcorrect, subreg_corners, **kw ) В¶ Correct non-dithered WIDE-slit MOSFIRE spectral frames for: 15:51 IJMC: Converted to Python, with some unit conversionsД®mpty object container. Section 4.3 of GreenвЂ™s вЂњSpherical AstronomyвЂќ (1985). The dispersion for each wavelength is derived from PROCEDURE:Д¬omputes the difference between the dispersion at two Returns the atmospheric disperion in arcseconds. KEYWORD PARAMETERS:Д¬ANCEL - Set on return if there is a problem OUTPUTS: Water - water vapor pressure in mm of Hg.ДЇco2 - relative concentration of CO2 (by pressure) Temp - atmospheric temperature in degrees C OPTIONAL INPUTS: Pressure - atmospheric pressure in mm of Hg Spectroscopy CALLING SEQUENCE: result = atmosdisp(wave,wave_0,za,pressure,temp,$ Compute the atmosperic dispersion relative to lambda_0.

Pyfits getdata