================================
The individual fits files are named as

1D signal > [FMOS_ID]_[date(UT)]_[grating]_1d.fits
1D noise  > [FMOS_ID]_[date(UT)]_[grating]_1d_no.fits
2D signal > [FMOS_ID]_[date(UT)]_[grating]_2d.fits
2D noise  > [FMOS_ID]_[date(UT)]_[grating]_2d_nosq.fits


Note:
 The spectral values are in the unit of [micro Jy].
 The wavelength in [Angstrom, calibrated for vacuum].
 The date of observation is UT (not Hawaii time).
 2D noise spectra have noise^2.
 Noise is given in unit of micro Jy, thus need to scale x1.25 to match the noise per pixel.  
 Caution! "CRVAL1" (the wavelength value of the first pixel) varies among observations.
 IMPORTANT: fluxes and noise were scaled to correct for offsets between IRS1 and IRS2 (see  Section 4.4 of Kashino et al. 2019, ApJS, 241, 10; https://ui.adsabs.harvard.edu/abs/2019ApJS..241...10K/abstract).

2019-03-17 Daichi Kashino
================================


#mask obs_date grating


sf4A   20120313   hl
sf1A   20120314   hl
sf2A   20120315   hl
sf1B   20120316   hl
sf3A   20120317   hl
sf1C   20120318   hs
j1     20120319   jl
j2     20121229   jl
sf3B   20130119   hl
sf4B   20130120   hl
j3     20130121   jl
j4     20130122   jl
HR2B   20131229   hl
ex1    20140122   hl
ex2    20140124   hl
HR3C   20140125   hl
HR1D   20140126   hl
HR4C   20140127   hl
j1B    20140208   jl
j4BC   20140209   jl
ex3    20140211   hl
j1E    20140307   jl
ex5    20141203   hl
COSMOS1_Hsp 20150207 hs
COSMOS2_Hsp 20150207 hs
COSMOS3_Hsp 20150208 hs
COSMOS4_Hsp 20150208 hs
HR7A   20150209   hl
HR7B   20150212   hl
HR6A   20150213   hl
HR5A   20150411   hl
HR5B   20150412   hl
HR8E   20160116   hl
HR4E   20160117   hl
HR1E   20160118   hl
HRC0   20160119   hl
HR6E   20160120   hl
j7E    20160121   jl
j1C    20160325   jl
j2B    20160327   jl
j4D    20160328   jl
j3B    20160330   jl
HR7E   20160331   hl
j1EB   20160420   jl
j6E    20160421   jl
j1D    20160422   jl
j3C    20160423   jl
j2C    20160424   jl
j8E    20160425   jl