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IRS products that come out of the engineering pipeline:
| File Type |
Name
SPITZER_S+module*_aorkey_expnum_ dcenum_version_type.suffix |
Format |
Description |
| Raw science data cube |
SPITZER_S1_9876540_96_0_1_raw.fits |
FITS image as 3-D cube with 16-bit integer,
128x128xn (n depends on the Spectral Exp Time)
Size: n x 32768 byte + header (typical/maximum value: 550 kbyte) |
Pixel values unchanged from the MIPL DCE, but header
keywords much reduced in number; some keywords are modified
using a keyword dictionary; the modifications include
renaming and averaging groups of keywords |
| Engineering data |
SPITZER_S1_9876540_96_0_1_pipe0.fits |
FITS image as 3-D cube with 32-bit real, 256/128x128xn
Size: 280 kbyte |
Output of the engineering pipeline, whose header is
then modified by the pointing transfer and the final product
generator (pipeline # 111); its header contains
now such things as proposer's and target names. |
| Peakup data |
SPITZER_S5_9876540_96_0_1_bcd.fits |
FITS image as 2-D image with 32-bit real, 128x128
Size: 65536 bytes + header |
Output of the engineering pipeline having been processed onboard
the spacecraft, whose header is
then modified by the pointing transfer and the final product
generator (pipeline # 111); its header contains
now such things as proposer's and target names. |
* S0, S1, S2, S3 correspond to short-low (SL), short-high (SH), long-low (LL), long-high (LH)
S5, S6 correspond to peakup only blue (PB), peakup only red (PR)
In cycle 2, PU imaging will be introduced and we will have:
S8, S9 correspond to peakup imaging blue (PBI), peakup imaging red (PRI)
IRS products that come out of the science pipeline:
| File Type |
Name
SPITZER_S+module_aorkey_expnum_ dcenum_version_type.suffix
or
SPITZER_S+module_aorkey_dcenum_ version_Enum*_type.suffix |
Format |
Description |
| BCD |
Earliest science archived pipeline product that is released (reduced 3D data cube):
1. SPITZER_S1_9876540_96_0_1_lnz.fits
1u. SPITZER_S1_9876540_96_0_1_lnzu.fits
Data corrected for detector behavior ("droop" effect):
2. SPITZER_S1_9876540_96_0_1_droop.fits
2u. SPITZER_S1_9876540_96_0_1_drunc.fits
Data with removed straylight/crosstalk, skipped in alternate path:
3. SPITZER_S1_9876540_96_0_1_rsc.fits
3u. SPITZER_S1_9876540_96_0_1_rscu.fits
Fully processed data (including flat fielding):
4. SPITZER_S1_9876540_96_0_1_bcd.fits
4fu. SPITZER_S1_9876540_96_0_1_func.fits
4du. SPITZER_S1_9876540_96_0_1_dbunc.fits
Alternate flat fielded data:
5. SPITZER_S1_9876540_96_0_1_f2ap.fits
5u. SPITZER_S1_9876540_96_0_1_f2unc.fits |
1,1u. FITS image as 3-D cube with 32-bit real, 128x128xn
(n depends on the Spectral Exp Time)
Size: n x 65536 byte + header (typcial value: 1.0 Mbyte)
2,3,5. FITS image with 32-bit real, 128x128
Size: 100 kbyte
4. FITS image with 32-bit real, 128x128
Size: 80 kbyte
2u,3u,4u,5u. FITS image with 32-bit real, 128x128
Size: 70 kbyte |
1. Product of the module "LINEARIZ" which linearizes the data according to
a model for each pixel.
1u. Uncertainty file for lnz.fits
2. Most processing steps applied, except for straylight removal, cross talk
correction, flat fielding, pointing transfer, and final product generator
2u. Uncertainty file for droop.fits
3. Most processing steps applied, except for flat fielding, pointing transfer, and
final product generator
3u. Uncertainty file for rsc.fits
4. Collapsed (2-D) 128x128 slope image CORRECTED for straylight (SL) or
crosstalk (SH,LH), after division by the flatfield image
Obtained via ramp-slope estimation in the IRS pipeline
4fu. Uncertainty image for bcd.fits
4du. Uncertainty image associated with the product bcd.fits that comes
from the darkcal pipeline
5. Data image UNCORRECTED for either
crosstalk or straylight removal, after division by the flatfield image
5u. Uncertainty image for f2ap.fits |
| Coadded 2-D image |
1. SPITZER_S1_9876540_96_1_E012345_coa2d.fits
2. SPITZER_S1_9876540_96_1_A012345_c2unc.fits
3. SPITZER_S1_9876540_96_1_A012345_inlst.txt
4. SPITZER_S1_9876540_96_1_A012345_2dcoad.txt |
1. FITS image with 32-bit real, 128x128
Size: 90 kbyte
2. FITS image with 32-bit real, 128x128
Size: 70 kbyte
3-4. ASCII file
Size: a few hundred byte |
1. Image coadded according to
selected criteria and rules
2. Uncertainty image for coa2d.fits
3. List of input files for coadding
4. Gives statistical weight of input files for coadding |
| Mask files |
1. SPITZER_S1_9876540_96_0_1_bmask.fits
2. SPITZER_S1_9876540_96_0_1_dmask.fits
3. SPITZER_S1_9876540_96_1_A012345_c2msk.fits
4. SPITZER_S1_9876540_96_1_A012345_ibsmk.txt |
1,3. FITS image with 16-bit integer, 128x128
Size: 40 kbyte
2. FITS image as 3-D cube with 16-bit integer,
128x128xn (n depends on the Spectral Exp Time)
Size: n x 32768 byte + header (typical value: 530 kbyte)
4. ASCII file |
1. Mask file, associated with bcd.fits, used to store pixel status information that
is applicable to the individual collapsed (2-D) 128x128 slope image
(see bit definition)
2. Mask file associated with lnz.fits, flags individual reads up the ramp
3. Mask file associated with the coa2d.fits, flags pixels with few valid inputs
4. List of bmask files |
| Log file |
If associated with BCD product:
SPITZER_S1_9876540_96_0_1_out.pline
If associated with ensemble product:
SPITZER_S1_9876540_96_1_A012345_out.pline |
ASCII file
Size: several 10 kbyte |
Output log file from several pipelines |
* The letter "E" stands for "ensemble" product and "A" for "ancillary ensemble" product.
"Enum" is the ensemble number.
IRS products that come out of the extraction (post-BCD) pipeline:
| File Type |
Name
SPITZER_S+module_aorkey_expnum_ dcenum_version_type.suffix
or
SPITZER_S+module_aorkey_dcenum_ version_Enum*_type.suffix |
Format |
Description |
| Tuned spectrum table |
Extracted spectrum:
1. SPITZER_S1_9876540_96_0_1_spect.tbl
Extracted position table for extracted spectrum:
1r. SPITZER_S1_9876540_96_0_1_ridge.tbl
Alternate extracted spectrum:
2. SPITZER_S1_9876540_96_0_1_spec2.tbl
Extracted spectrum from coadded data (coa2d.fits):
3. SPITZER_S1_9876540_96_1_E012345_tune.tbl
Extracted position table for coadded data:
3r. SPITZER_S1_9876540_96_1_A012345_ridge.tbl |
1,2,3. ASCII table
Size: <= 200 kbyte
1r,3r. ASCII table
Size: <= 300 kbyte |
1. Table containing flux in Jy as a function of wavelength for each order
(BCD extraction)
1r. Table containing information about where the extraction was performed for
extracted spectrum
2. Table containing flux in Jy as a function of wavelength for each order
(alternate BCD extraction)
3. Table
containing flux in Jy as a function of wavelength for each order
(Extraction of coadd)
3r. Table containing information about where the extraction was performed for
the coadded data |
** The letter "E" stands for "ensemble" product and "A" for "ancillary ensemble" product.
"Enum" is the ensemble number.
IRS calibration files:
| File Type |
Name
b+module*_type.suffix
or
b+module*_r+rampduration**_type.suffix |
Format |
Description |
| Flat data cube |
1. b0_flatfield.fits
2. b0_flatfield_cmask.fits |
1. FITS image as 3-D cube with 32-bit real, 128x128x2
Size: 170 kbyte
2. FITS image with single-precision floating-point values,
128x128
Size: 90 kbyte |
1. The first plane of data contains the flatfield image
and the second plane of data contains the corresponding sigmas
2. Mask file associated with flatfield.fits |
| Dark data cube |
1. b0_r6_dark.fits
2. b0_r6_dark_unc.fits
3. b0_r6_dark_cmask.fits |
1,2. FITS image as 3-D cube with 32-bit real,
128x128xn (n depends on the Spectral Exp Time)
Size: n x 65536 byte + header (typical value: 1.08 Mbyte)
3. FITS image as 3-D cube with 16-bit integer,
128x128xn (n depends on the Spectral Exp Time)
Size: n x 32768 byte + header (typical value: 530 kbyte) |
1. Dark calibration file: observation of a dark part of the sky
2. Uncertainty image associated with dark.fits
3. Mask file associated with dark.fits |
| Linearity data cube |
1. b0_lincal.fits
2. b0_lincal_cmask.fits |
1. FITS image as 3-D cube with 32-bit real,
128x128x3
Size: 200 kbyte
2. FITS image with 16-bit integer, 128x128
Size: 40 kbyte |
1. Data cube describing the linearity coefficient for each pixel:
The first plane contains the value of the linearity coefficient alpha (used in series expansion x+alpha*x^2);
the second plane contains the "soft saturation cutoff" for the lincal module;
the third plane contains the associated uncertainties of the first plane.
2. Mask file associated with lincal.fits |
| Flux |
b0_fluxcon.tbl |
ASCII file
Size: < 6 kbyte |
Flux conversion factors and order tuning coefficients.
The photometric tuning coefficients are determined by
polynomial fits (up to 5th order) to the ratios of
extracted spectra of standard star observations and
known spectral energy distributions (model).
|
| Wavelength calibration tables |
1. b0_wavsamp.tbl
2. b0_wavsamp_offset.fits
3. b0_wavsamp_wave.fits
4. b0_wavesamp_omask.fits |
1. ASCII table
Size: < 200 kbyte
2,3. FITS image with 32-bit real, 128x128
Size: 70 kbyte
4. FITS image with 16-bit integer, 128x128
Size: 40 kbyte |
1. Table
describing the pixel regions (can be fraction of a pixel) used in flatfielding and extraction.
Each row describes the pixels contributing flux to a given wavelength in the output spectrum.
2. Spatial offsets (in arcseconds) per pixel from the FOV center
3. The wavelength associated with each pixel
4. The spectral order associated with each pixel |
| Other Mask files |
1. b0_lmask.fits
2. b0_omask.fits
3. b0_pmask.fits
4. b0_umask.fits |
1-4. FITS image with 16-bit integer, 128x128
Size: 40 kbyte |
1. Mask identifying the unilluminated regions used in fitting the straylight correction
in the short-low module
2. Order mask file
3. Mask file containing the long-term pixel status
4. Mask file identifying unilluminated regions for droop and dark corrections
(different than lmask.fits for short-low) |
* b0, b1, b2, b3 correspond to short-low (SL), short-high (SH), long-low (LL), long-high (LH)
** The ramp duration in seconds of:
b0: 6,14,60,240
b1: 6,30,120,480
b2: 6,14,30,120
b3: 6,14,60,240
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