*** Sensitivity Function for 00apr Night #2 ***
*** the IRAF way ***

05.24.00

1.  Get all the files you're gonna need.

lris0080.fits	int. flat longslit 150/7500, OG570
lris0081.fits   int. flat longslit 150/7500, OG570
lris0082.fits   int. flat longslit 150/7500, OG570
lris0083.fits   int. flat longslit 150/7500, OG570
lris0084.fits   int. flat longslit 150/7500, OG570
lris0085.fits	int. flat longslit 150/7500, clear
lris0086.fits	int. flat longslit 150/7500, clear
lris0087.fits	int. flat longslit 150/7500, clear
lris0088.fits	int. flat longslit 150/7500, clear
lris0089.fits	int. flat longslit 150/7500, clear
lris0090.fits	HeNeAr longslit 150/7500
lris0146.fits	Hiltner 600, clear
lris0148.fits	Hiltner 600, OG570
lris0220.fits	Wolf 1346, clear
lris0221.fits	Wolr 1346, OG570

2.  Fix CCD timing error with idl scripts (handle night 1 and night 2
    separately.

	e.g. lris0080 --> lris0080t

3.  Run twoamp on flats, lamp, and data.

	e.g. lris0080t --> lris0080tcb

4.  Make two flats: with filter and without.

	lris0080tcb			lris0085tcb
	lris0081tcb			lris0086tcb
	lris0082tcb --> flat_filt	lris0087tcb --> flat_clear
	lris0083tcb			lris0088tcb
	lris0084tcb			lris0089tcb

5.  Run response.

	flat_filt --> flat_filt_res	flat_clear --> flat_clear_res

6.  Flatten lamp, data using the write flat for the right stuff.

	e.g. lris0090tcb --> lris0080tcbf

7.  Cosmic ray zap data.

	e.g. lris0146tcbf --> lris0146tcbfz

8.  Extra and wavelength calibrate standard spectra.  The lamp calibration is a little
    bit sketch, since the arc lamps were taken only on night one, and I'm using data
    from night two.  The grangle changed by a very small amount (2/1000), so I don't think
    there can be that big of a difference.  Also, for the lamp extracted I used the clear
    hiltner and then the clear wolf extractions as references, and I'll calibrate each
    accordingly.

9.  Run standard on each of the lambda-calibrated spectra.  Set bandwith and bandsep
    to 20 (according to Tom and Doug and Josh).  In the interactive window, delete boxes
    that are clearly on absorption lines.  Do this for each spectrum.

        input = "hilt_clear.w"  Input image file root name
       output = "std.00apr"     Output flux file (used by SENSFUNC)
    star_name = "hilt600"       Star name in calibration list
      airmass =                 Airmass
      exptime =                 Exposure time (seconds)
          mag =                 Magnitude of star
      magband =                 Magnitude type
         teff =                 Effective temperature or spectral type
       answer = "y"             (no|yes|NO|YES|NO!|YES!)
    (samestar = yes)            Same star in all apertures?
 (beam_switch = no)             Beam switch spectra?
   (apertures = "")             Aperture selection list
   (bandwidth = 20.)            Bandpass widths
     (bandsep = 20.)            Bandpass separation
     (fnuzero = 3.6800000000000E-20) Absolute flux zero point
  (extinction = "onedstds$kpnoextinct.dat") Extinction file
      (caldir = "onedstds$spec50cal/") Directory containing calibration data
 (observatory = "keck")         Observatory for data
    (interact = yes)            Graphic interaction to define new bandpasses
    (graphics = "stdgraph")     Graphics output device
      (cursor = "")             Graphics cursor input
        (mode = "al")           

10. Run sensfunc.

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*** Sensitivity Function for 00apr Night #2 ***
*** the IDL way ***

05.26.00

1.  You need to reduce your data (as well as the standard star spectra)
    in the manner of the supernova guys.  That is, do a global sky subtraction
    in your 2D if it helps you to pick out faint continua, but actually do
    you extraction from the non-subtracted 2D.  This goes for the data
    and the standards.  (Also, recall that bogus did a crappy job on the flats.
    Reduce this stuff as you would longslit spectra, and use a order 21 spline3
    with low/hi rejection = 5 when making the response function.)

	a)  Get stuff.	

		lris0078.fits	wolf 1346 150l long, clear
		lris0079.fits   wolf 1346 150l long, OG570
		lris0080.fits	int flats 150l long, OG570
		lris0081.fits	int flats 150l long, OG570
		lris0082.fits	int flats 150l long, OG570
		lris0083.fits   int flats 150l long, OG570
		lris0084.fits	int flats 150l long, OG570
		lris0085.fits	int flats 150l long, clear
		lris0086.fits	int flats 150l long, clear
		lris0087.fits	int flats 150l long, clear
		lris0088.fits	int flats 150l long, clear
		lris0089.fits	int flats 150l long, clear
		lris0090.fits	arc lamps 150l long, clear
		lris0180.fits	hdf00ap2 spectroscopy
		lris0181.fits	hdf00ap2 spectroscopy
		lris0182.fits	hdf00ap2 spectroscopy
		lris0183.fits	int flats
		lris0184.fits	int flats
		lris0185.fits	int flats
		lris0186.fits	int flats
		lris0187.fits	HgKr
		lris0188.fits	NeAr
		lris0190.fits	hdf00ap2 spectroscopy
		lris0191.fits	hdf00ap2 spectroscopy
		lris0192.fits	hdf00ap2 spectroscopy
		lris0193.fits	int flats
		lris0194.fits	int flats
		lris0195.fits	int flats
		lris0196.fits	int flats

	b)  Fix timing error.  (lris0078 --> lris0078t)

	c)  Cut ser_yprime slit from spectra, lamps, and flats.

		e.g. imcopy lris0180[*,694:787] spec1
	
	d)  Run twoamp on everything.  (Remember to change y2=93 on data.)

	e)  Make flats.  Run response.

		flat_data1.fits		flat for hdf data, batch 1
		flat_data2.fits		flat for hdf data, batch 2
		flat_stdclr.fits	flat for wolf, clear
		flat_stdflt.fits	flat for wolf, OG570

	f)  Flatten.  (spec1cb --> spec1cbf)

	g)  Combine data frames.  (Don't background subtract; don't zap.)

2.  Extract and wavelength calibrate data and standards.  Name the wavelength
    calibrate spectra *.w.ms.fits.

3.  Start IDL.  Run mkfluxstar.  (May need to add keyword OBSERVAT = keck in
    image headers.  Also, put file mastersky.fits in working directory.)

4.  Run mkbstar.  Do same thing, sort of.

5.  Run calibrate; run final.