extract_1d step extracts a 1D signal from a 2D or 3D dataset and
writes spectral data to an “x1d” product. This works on all JWST spectroscopic
modes, including MIRI LRS (slit and slitless) and MRS, NIRCam WFSS and
TSGRISM, NIRISS WFSS and SOSS, and NIRSpec fixed-slit, IFU, and MOS.
An EXTRACT1D reference file is used for most modes to specify the location and size of the target and background extraction apertures. The EXTRACT1D reference file is not used for Wide-Field Slitless Spectroscopy data (NIS_WFSS or NRC_WFSS). For these modes the extraction region is instead taken to be the full size of the input 2D subarray or cutout for each source, or restricted to the region within which the world coordinate system (WCS) is defined in each cutout.
For slit-like 2D input data, source and background extractions are done using
a rectangular aperture that covers one pixel in the dispersion direction and
uses a height in the cross-dispersion direction that is defined by parameters in
the EXTRACT1D reference file.
For 3D IFU data, on the other hand, the extraction options differ depending on
whether the target is a point or extended source. For a point
source, the spectrum is extracted using circular aperture photometry,
optionally including background subtraction using a circular annulus.
For an extended source, rectangular aperture photometry is used, with
the entire image being extracted, and no background subtraction, regardless
of what was specified in the reference file or step arguments.
For both point or extended sources, photometric measurements make use of
the Astropy affiliated package
photutils to define an aperture
object and perform extraction. For 3D NIRSpec fixed slit rateints data, the
extract_1d step will be skipped as 3D input for the mode is not supported.
For most spectral modes an aperture correction will be applied to the extracted 1D spectral data (unless otherwise selected by the user), in order to put the results onto an infinite aperture scale. This is done by creating interpolation functions based on the APCORR reference file data and applying the interpolated aperture correction (a multiplicative factor between 0 and 1) to the extracted, 1D spectral data (corrected data include the “flux”, “surf_bright”, “flux_error”, “sb_error”, and all flux and surface brightness variance columns in the output table).
Calibrated and potentially resampled 2D images or 3D cubes. The format should be a CubeModel, SlitModel, IFUCubeModel, ImageModel, MultiSlitModel, or a ModelContainer. For some JWST modes this is usually a resampled product, such as the “s2d” products for MIRI LRS fixed-slit, NIRSpec fixed-slit, and NIRSpec MOS, or the “s3d” products for MIRI MRS and NIRSpec IFU. For other modes that are not resampled (e.g. MIRI LRS slitless, NIRISS SOSS, NIRSpec BrightObj, and NIRCam and NIRISS WFSS), this will be a “cal” product. For modes that have multiple slit instances (NIRSpec fixed-slit and MOS, WFSS), the SCI extensions should have the keyword SLTNAME to specify which slit was extracted, though if there is only one slit (e.g. MIRI LRS and NIRISS SOSS), the slit name can be taken from the EXTRACT1D reference file instead.
Normally the photom step should be applied before running
photom has not been run, a warning will be logged and the
extract_1d will be in units of count rate. The
converts data to units of either surface brightness (MegaJanskys per steradian) or,
for point sources observed with NIRSpec and NIRISS SOSS, units of flux density
The output will be in
MultiSpecModel format. For each input slit there will
be an output table extension with the name EXTRACT1D. This extension will
have columns WAVELENGTH, FLUX, FLUX_ERROR, FLUX_VAR_POISSON, FLUX_VAR_RNOISE,
FLUX_VAR_FLAT, SURF_BRIGHT, SB_ERROR, SB_VAR_POISSON, SB_VAR_RNOISE,
SB_VAR_FLAT, DQ, BACKGROUND, BKGD_ERROR, BKGD_VAR_POISSON, BKGD_VAR_RNOISE,
BKGD_VAR_FLAT and NPIXELS.
Some meta data will be written to the table header, mostly copied from the
The output WAVELENGTH data is copied from the wavelength array of the input 2D data,
if that attribute exists and was populated, otherwise it is calculated from the WCS.
FLUX is the flux density in Janskys; see keyword TUNIT2 if the data are
in a FITS BINTABLE. FLUX_ERROR is the error estimate for FLUX, and it has the
same units as FLUX. The error is calculated as the square root of the sum of the
three variance arrays: Poisson, read noise (RNOISE), and flat field (FLAT).
SURF_BRIGHT is the surface brightness in MJy / sr, except that for point
sources observed with NIRSpec and NIRISS SOSS, SURF_BRIGHT will be set to
zero, because there’s no way to express the extracted results from those modes
as a surface brightness. SB_ERROR is the error estimate for SURF_BRIGHT, calculated
in the same fashion as FLUX_ERROR but using the SB_VAR arrays. While it’s expected
that a user will make use of the FLUX column for point-source data and the
SURF_BRIGHT column for an extended source, both columns are populated (except for
NIRSpec and NIRISS SOSS point sources, as mentioned above).
extract_1d step collapses the input data from 2-D to 1-D by summing
one or more rows (or columns, depending on the dispersion direction).
A background may optionally be subtracted, but
there are also other options for background subtraction prior to
For the case of input data in units of MJy / sr, the SURF_BRIGHT
and BACKGROUND columns are
populated by dividing the sum by the number of pixels (see the NPIXELS column,
described below) that were added together. The FLUX column is populated
by multiplying the sum by the solid angle of a pixel, and also multiplying
by 10^6 to convert from MJy to Jy.
For the case of input data in units of MJy (i.e. point sources,
NIRSpec or NIRISS SOSS), the SURF_BRIGHT column is set to zero, the
FLUX column is just multiplied by 10^6, and the BACKGROUND column is
divided by NPIXELS and by the solid angle of a pixel to convert to surface
brightness (MJy / sr).
NPIXELS is the number of pixels that were added together for the source extraction region. Note that this is not necessarily a constant, and the value is not necessarily an integer (the data type is float). BACKGROUND is the measured background, scaled to the extraction width used for FLUX and SURF_BRIGHT. BACKGROUND will be zero if background subtraction is not requested. BKGD_ERROR is calculated as the square root of the sum of the BKGD_VAR arrays. DQ is not populated with useful values yet.
Extraction for 2D Slit Data¶
The operational details of the 1D extraction depend heavily on the parameter
values given in the EXTRACT1D reference file.
Here we describe their use within the
Source Extraction Region¶
As described in the documentation for the
EXTRACT1D reference file,
the characteristics of the source extraction region can be specified in one
of two different ways.
The simplest approach is to use the
extract_width parameters. Note that all of these values are
zero-indexed integers, the start and stop limits are inclusive, and the values
are in the frame of the image being operated on (which could be a cutout of a
larger original image).
dispaxis=1, the limits in the dispersion direction are
xstop and the limits in the cross-dispersion direction are
dispaxis=2, the rolls are reversed.
extract_width is also given, that takes priority over
dispaxis=1) for the extraction width, but
ystop will still be used to define the centering of the extraction region
in the cross-dispersion direction. For point source data,
xstop values (dispaxis = 2) are shifted to account
for the expected location of the source. If dispaxis=1, then the
are modified. The offset amount is calculated internally. If it is not desired to apply this
offset, then set
use_source_posn = False. If the
use_source_posn parameter is None (default),
the values of
ystart/ystop in the
extract_1d reference file will be used
to determine the center position of the extraction aperture. If these values are not set in the
reference file, the
use_source_posn will be set internally to True for point source data
according to the table given in srctype.
Any of the extraction location parameters will be modified internally by the step code if the
extraction region would extend outside the limits of the input image or outside
the domain specified by the WCS.
A more flexible way to specify the source extraction region is via the
src_coeff is specified as a list of lists of floating-point
polynomial coefficients that define the lower and upper
limits of the source extraction region as a function of dispersion. This allows,
for example, following a tilted or curved spectral trace or simply
following the variation in cross-dispersion FWHM as a function of wavelength.
ystop values are given,
takes precedence. The
xstop values can still be used to
limit the range of the extraction in the dispersion direction. More details on
the specification and use of polynomial coefficients is given below.
Background Extraction Regions¶
One or more background extraction regions for a given aperture instance can
be specified using the
bkg_coeff parameter in the EXTRACT1D reference file.
This is directly analogous to the use of
src_coeff for specifying source
extraction regions and functions in exactly the same way. More details on the
use of polynomial coefficients is given in the next section.
Background subtraction will be done if and only if
bkg_coeff is given in
the EXTRACT1D reference file. The background is determined independently for
each column (or row, if dispersion is vertical), using pixel values from all
background regions within each column (or row).
Parameters related to background subtraction are
smoothing_lengthis specified, the 2D image data used to perform background extraction will be smoothed along the dispersion direction using a boxcar of width
smoothing_length(in pixels). If not specified, no smoothing of the input 2D image data is performed.
bkg_fitspecifies the type of background computation to be performed within each column (or row). The default value is None; if not set by the user, the step will search the reference file for a value. If no value is found,
bkg_fitwill be set to “poly”. The “poly” mode fits a polynomial of order
bkg_orderto the background values within the column (or row). Alternatively, values of “mean” or “median” can be specified in order to compute the simple mean or median of the background values in each column (or row). Note that using “bkg_fit=mean” is mathematically equivalent to “bkg_fit=poly” with “bkg_order=0”. If
bkg_fitis provided both by a reference file and by the user, e.g.
steps.extract_1d.bkg_fit='poly', the user-supplied value will override the reference file value.
bkg_orderis used to indicate the polynomial order to be used. The default value is zero, i.e. a constant.
During source extraction, the background fit is evaluated at each pixel within the source extraction region for that column (row), and the fitted values will be subtracted (pixel by pixel) from the source count rate.
Source and Background Coefficient Lists¶
The interpretation and use of polynomial coefficients to specify source and
background extraction regions via
bkg_coeff is the same.
The coefficients are specified as a list of an even number of lists (an
even number because both the lower and upper limits of each extraction region
must be specified). The source extraction coefficients will normally be
a list of just two lists, the coefficients for the lower limit function
and the coefficients for the upper limit function of one extraction
region. The limits could just be constant values,
e.g. [[324.5], [335.5]]. Straight but tilted lines are linear functions:
[[324.5, 0.0137], [335.5, 0.0137]]
Multiple regions may be specified for either the source or background, or both. It will be common to specify more than one background region. Here is an example for specifying two background regions:
[[315.2, 0.0135], [320.7, 0.0135], [341.1, 0.0139], [346.8, 0.0139]]
This is interpreted as follows:
[315.2, 0.0135]: lower limit for first background region
[320.7, 0.0135]: upper limit for first background region
[341.1, 0.0139]: lower limit for second background region
[346.8, 0.0139]: upper limit for second background region
Note: If the dispersion direction is vertical, replace “lower” with “left” and “upper” with “right” in the above description.
Notice especially that
bkg_coeff contain floating-point
values. For interpreting fractions of a pixel, the convention used here
is that the pixel number at the center of a pixel is a whole number. Thus,
if a lower or upper limit is a whole number, that limit splits the pixel
in two, so the weight for that pixel will be 0.5. To include all the
pixels between 325 and 335 inclusive, for example, the lower and upper
limits would be given as 324.5 and 335.5 respectively.
The order of a polynomial is specified implicitly to be one less than the number of coefficients. The number of coefficients for a lower or upper extraction region limit must be at least one (i.e. zeroth-order polynomial). There is no predefined upper limit on the number of coefficients (and hence polynomial order). The various polynomials (lower limits, upper limits, possibly multiple regions) do not need to have the same number of coefficients; each of the inner lists specifies a separate polynomial. However, the independent variable (wavelength or pixel) does need to be the same for all polynomials for a given slit.
Polynomials specified via
bkg_coeff are functions of either wavelength
(in microns) or pixel number (pixels in the dispersion direction, with respect to
the input 2D slit image), which is specified by the parameter
The default is “pixel”. The values of these polynomial functions are pixel numbers in the
direction perpendicular to dispersion.
Extraction for 3D IFU Data¶
In IFU cube data, 1D extraction is controlled by a different set of EXTRACT1D reference file parameters. For point source data the extraction aperture is centered at the RA/DEC target location indicated by the header. If the target location is undefined in the header, then the extraction region is the center of the IFU cube. For extended source data, anything specified in the reference file or step arguments will be ignored; the entire image will be extracted, and no background subtraction will be done.
For point sources a circular extraction aperture is used, along with an optional
circular annulus for background extraction and subtraction. The size of the extraction
region and the background annulus size varies with wavelength.
The extraction related vectors are found in the asdf extract1d reference file.
For each element in the
wavelength vector there are three size components:
outer_bkg. The radius vector sets the extraction size; while
outer_bkg specify the
limits of an annular background aperture. There are two additional vectors in the reference file,
axis_pa, which are placeholders for possible future functionality.
The extraction size parameters are given in units of arcseconds and converted to units of pixels
in the extraction process.
The region of overlap between an aperture and a pixel can be calculated by
one of three different methods, specified by the
method parameter: “exact”
(default), limited only by finite precision arithmetic; “center”, the full value
in a pixel will be included if its center is within the aperture; or “subsample”,
which means pixels will be subsampled N x N and the “center” option will be used
for each sub-pixel. When
method is “subsample”, the parameter
is used to set the resampling value. The default value is 10.
For IFU cubes the error information is contained entirely in the ERR array, and is not broken out into the
VAR_POISSON, VAR_RNOISE, and VAR_FLAT arrays. As such,
extract_1d only propagates this
non-differentiated error term. Note that while covariance is also extremely important for IFU data cubes
(as the IFUs themselves are significantly undersampled) this term is not presently computed or taken
into account in the
extract_1d step. As such, the error estimates should be taken as a rough
approximation that will be characterized and improved as flight data become available.