Instrument¶

Base Classes and Calibration Tokens¶

Abstract base class for dispersers and calibration parameter tokens.

class unite.instrument.base.RScale(name=None, *, prior=None)[source]¶

Bases: Parameter

Multiplicative scale on the disperser resolving power R.

Nominal value is 1 (no correction). The model applies R_eff(λ) = R_nominal(λ) * r_scale.

Parameters:

namestr, optional: Human-readable label. When attached to a Disperser, the site name is auto-derived as 'r_scale_{disperser_name}' if not provided.
priorPrior, optional: Prior on the R scale factor. Defaults to Fixed(1.0) (fixed at nominal).

Parameters:

name (str | None)
prior (Prior | None)

class unite.instrument.base.FluxScale(name=None, *, prior=None)[source]¶

Bases: Parameter

Multiplicative flux normalisation between dispersers.

Nominal value is 1. The model divides observed flux by flux_scale, allowing relative flux calibration across multiple gratings.

Parameters:

namestr, optional: Human-readable label. When attached to a Disperser, the site name is auto-derived as 'flux_scale_{disperser_name}' if not provided.
priorPrior, optional: Prior on the flux scale factor. Defaults to Fixed(1.0) (fixed at nominal).

Parameters:

name (str | None)
prior (Prior | None)

class unite.instrument.base.PixOffset(name=None, *, prior=None)[source]¶

Bases: Parameter

Pixel displacement of the spectrum on the detector relative to the wavelength calibration.

Nominal value is 0 (no displacement). A positive value indicates the spectrum is displaced toward longer wavelengths on the detector: the model subtracts pix_offset * dlam_dpix from the calibrated pixel-edge wavelengths, shifting them blueward to compensate.

For example, if a disperser consistently returns redshifts that are too high compared to a reference, the spectrum is displaced redward by some number of pixels — set pix_offset to that (positive) number to correct the wavelength solution.

Parameters:

namestr, optional: Human-readable label. When attached to a Disperser, the site name is auto-derived as 'pix_offset_{disperser_name}' if not provided.
priorPrior, optional: Prior on the pixel offset. Defaults to Fixed(0.0) (no displacement).

Parameters:

name (str | None)
prior (Prior | None)

class unite.instrument.base.Disperser(unit, *, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: ABC

Abstract base class for dispersive optical elements.

A disperser maps wavelength coordinates to instrumental quantities such as resolving power and plate scale. Every concrete subclass must implement R() and dlam_dpix(), and must carry a unit attribute that records the wavelength unit the disperser expects.

Calibration is encoded by optional tokens (RScale, FluxScale, PixOffset):

r_scale — multiplicative scale on resolving power (R).
flux_scale — multiplicative flux normalisation.
pix_offset — pixel displacement of the spectrum on the detector (positive = redward; wavelength grid is corrected blueward).

None on any slot means that parameter is absent from the model entirely (equivalent to a fixed nominal value but without a token). To create a token that is fixed at its nominal value, pass e.g. r_scale=RScale() — the default prior is Fixed(1.0).

Sharing: two dispersers that reference the same token instance share a single parameter in the model (identity-based, like FWHM/ Redshift on lines).

Parameters:

unitastropy.units.UnitBase: The wavelength unit that this disperser operates in (e.g. u.Angstrom, u.nm, u.um). All wavelength values passed to R() and dlam_dpix() are assumed to be in this unit.
namestr, optional: Human-readable label (e.g. 'G235H'). Used in repr and as the default Spectrum.name when this disperser is attached.
r_scaleRScale, optional: Token for the resolving-power scale. None → not in model.
flux_scaleFluxScale, optional: Token for the flux normalisation. None → not in model.
pix_offsetPixOffset, optional: Token for the detector pixel displacement. None → not in model.

Parameters:

unit (u.UnitBase)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

abstractmethod R(wavelength)[source]¶

Return the resolving power at the given wavelengths.

Return type:

Parameters:

wavelengthArrayLike: Wavelength values in the unit specified by self.unit.

Returns:

ArrayLike: Resolving power R = λ / Δλ evaluated at each wavelength.

Parameters:

abstractmethod dlam_dpix(wavelength)[source]¶

Return the linear dispersion (wavelength per pixel).

Return type:

Parameters:

wavelengthArrayLike: Wavelength values in the unit specified by self.unit.

Returns:

ArrayLike: Dispersion dλ/dpix evaluated at each wavelength.

Parameters:

property has_calibration_params: bool¶: True if any calibration token is attached.

Instrument Configuration¶

Instrument configuration: disperser models with calibration tokens.

InstrumentConfig collects one Disperser per observing configuration. Each disperser carries optional RScale / FluxScale / PixOffset tokens (r_scale, flux_scale, pix_offset) for shared calibration parameters.

Degeneracy warning¶

A multi-disperser fit is only identified if at least one disperser has flux_scale=None (flux anchor) and at least one has pix_offset=None (pixel-offset anchor). validate() issues UserWarning when these conditions are not met. Validation is called automatically when this object is passed to Configuration.

Serialization¶

to_dict() hoists all unique calibration tokens to a top-level calib_params section keyed by token name. Disperser entries reference tokens by name. Shared tokens round-trip correctly — the same object is reconstructed for both entries.

Examples¶

>>> from unite.instrument import InstrumentConfig, RScale, FluxScale
>>> from unite.instrument.nirspec import G235H, G395H
>>> from unite.prior import TruncatedNormal
>>> r = RScale(prior=TruncatedNormal(1.0, 0.05, 0.8, 1.2))
>>> flux_0 = FluxScale(prior=TruncatedNormal(1.0, 0.1, 0.5, 2.0))
>>> cfg = InstrumentConfig([
...     G235H(r_scale=r),
...     G395H(r_scale=r, flux_scale=flux_0),
... ])
>>> cfg.names
['G235H', 'G395H']

class unite.instrument.config.InstrumentConfig(dispersers)[source]¶

Bases: object

Configuration for a multi-disperser spectral dataset.

An ordered collection of Disperser objects, one per observing disperser. Each disperser carries optional CalibParam tokens for calibration parameters.

The configuration is data-free: it describes which dispersers are used and how they are calibrated. Actual spectral data arrays are attached later via make_spectrum().

Parameters:

disperserssequence of Disperser: One entry per disperser. Names (disperser.name) must be unique.

Raises:

ValueError: If any disperser names are duplicated or empty.

Parameters:

dispersers (Sequence[Disperser])

validate()[source]¶

Check for flux and pixel-offset degeneracies.

Issues a UserWarning for each calibration axis (flux, dispersion) where no disperser is anchored (token None).

Return type:: None

property names: list[str]¶: Names of all dispersers in this configuration.

to_dict()[source]¶

Serialize to a YAML-safe dictionary.

Shared CalibParam tokens are hoisted to a top-level calib_params section. Disperser entries reference tokens by name, so sharing is preserved on round-trip.

Return type:

dict

Returns:

dict: Contains 'calib_params' and 'entries' keys.

classmethod from_dict(d)[source]¶

Deserialize from a dictionary.

Return type:

InstrumentConfig

Parameters:

ddict: As produced by to_dict().

Returns:

InstrumentConfig

Parameters:

d (dict)

to_yaml()[source]¶

Serialize to a YAML string.

Return type:

str

Returns:

str

classmethod from_yaml(text)[source]¶

Deserialize from a YAML string.

Return type:

InstrumentConfig

Parameters:

textstr: YAML string as produced by to_yaml().

Returns:

InstrumentConfig

Parameters:

text (str)

save(path)[source]¶

Save to a YAML file.

Return type:

None

Parameters:

pathstr or Path: Output file path.

Parameters:

path (str | Path)

classmethod load(path)[source]¶

Load from a YAML file.

Return type:

InstrumentConfig

Parameters:

pathstr or Path: Path to a YAML file written by save().

Returns:

InstrumentConfig

Parameters:

path (str | Path)

Generic Implementations¶

Generic disperser implementations.

These are the building blocks for custom instruments.

Import from this module directly:

from unite.instrument.generic import GenericDisperser, SimpleDisperser

The Spectrum class lives in unite.spectrum.

class unite.instrument.generic.GenericDisperser(R_func, dlam_dpix_func, unit, *, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: Disperser

A disperser defined by user-supplied, JAX-jittable callables.

This is the most flexible concrete disperser: you provide arbitrary functions for R(λ) and dλ/dpix(λ) and they are forwarded directly.

Parameters:

R_funcCallable[[ArrayLike], ArrayLike]: A JAX-jittable function that returns the resolving power for a given array of wavelengths.
dlam_dpix_funcCallable[[ArrayLike], ArrayLike]: A JAX-jittable function that returns the linear dispersion for a given array of wavelengths.
unitastropy.units.UnitBase: The wavelength unit the functions expect.
namestr, optional: Human-readable label.
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the pixel shift.

Parameters:

R_func (Callable[[ArrayLike], ArrayLike])
dlam_dpix_func (Callable[[ArrayLike], ArrayLike])
unit (u.UnitBase)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

Examples

>>> import jax.numpy as jnp
>>> from astropy import units as u
>>> d = GenericDisperser(
...     R_func=lambda w: jnp.full_like(w, 2700.0),
...     dlam_dpix_func=lambda w: w / 2700.0,
...     unit=u.Angstrom,
... )
>>> d.R(jnp.array([5000.0]))
Array([2700.], dtype=float32)

R(wavelength)[source]¶

Return the resolving power by evaluating the stored callable.

Return type:: Array | ndarray | bool | number | bool | int | float | complex
Parameters:: wavelength (Array | ndarray | bool | number | bool | int | float | complex)

dlam_dpix(wavelength)[source]¶

Return the linear dispersion by evaluating the stored callable.

Return type:: Array | ndarray | bool | number | bool | int | float | complex
Parameters:: wavelength (Array | ndarray | bool | number | bool | int | float | complex)

class unite.instrument.generic.SimpleDisperser(wavelength, *, R=None, dlam=None, dvel=None, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: Disperser

A disperser defined on a pixel-sampled wavelength grid.

The wavelength array is interpreted as a sequence of pixel centers so that dλ/dpix is computed directly from the spacing of the array (via jnp.gradient).

The resolving power is derived from exactly one of three keyword arguments:

R — resolving power, scalar or array matching wavelength.
dlam — spectral resolution element Δλ (same unit as wavelength).
dvel — velocity fwhm in km/s. Converted via R = c / dvel.

A scalar value produces a constant R, Δλ, or Δv across the grid (and the corresponding resolving-power array is derived accordingly). An array value must have the same length as wavelength.

Parameters:

wavelengthu.Quantity: Pixel-center wavelengths. Must be 1-D.
RArrayLike, optional: Resolving power (scalar or per-pixel array).
dlamu.Quantity, optional: Spectral resolution Δλ, must be in wavelength units (scalar or per-pixel array)
dvelu.Quantity, optional: Velocity resolution in velocity units (scalar or per-pixel array).
namestr, optional: Human-readable label.
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the pixel shift.

Raises:

ValueError: If zero or more than one of R, dlam, dvel is provided, or if an array argument has the wrong length.

Parameters:

wavelength (u.Quantity)
R (ArrayLike | None)
dlam (u.Quantity | None)
dvel (u.Quantity | None)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

Notes

When R() or dlam_dpix() is called at wavelengths that differ from the stored grid, the values are linearly interpolated with jnp.interp.

R(wavelength)[source]¶

Return the resolving power, interpolated onto wavelength.

Return type:: Array | ndarray | bool | number | bool | int | float | complex
Parameters:: wavelength (Array | ndarray | bool | number | bool | int | float | complex)

dlam_dpix(wavelength)[source]¶

Return the linear dispersion, interpolated onto wavelength.

Return type:: Array | ndarray | bool | number | bool | int | float | complex
Parameters:: wavelength (Array | ndarray | bool | number | bool | int | float | complex)

NIRSpec Dispersers¶

JWST NIRSpec disperser implementations.

This module provides NIRSpec, a generic Disperser for any NIRSpec grating/prism configuration. Two resolving-power calibrations are available:

"uniform" or "uniformly-illuminated" — the official JDOX tabulated R(λ) curves shipped with the package as FITS files. This calibration is for uniformly illuminated sources.
"point" or "point-source" — polynomial R(λ) fits from de Graaff et al. (2025). This calibration is tailored for point-source observations.

Both calibrations share the same JDOX linear-dispersion (dλ/dpix) tables.

In addition to the generic NIRSpec class, named subclasses are provided for each grating:

PRISM
G140M, G140H
G235M, G235H
G395M, G395H

These fix the grating name while still accepting r_source and calibration token kwargs.

class unite.instrument.nirspec.disperser.G140H(r_source='point', *, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: NIRSpec

NIRSpec G140H disperser.

Convenience subclass of NIRSpec with the grating fixed to "g140h". Only r_source and calibration tokens need to be specified.

Parameters:

r_source"uniform", "uniformly-illuminated", "point", or "point-source", optional: Which resolving-power calibration to use (default "point").
namestr, optional: Human-readable label. Defaults to "G140H".
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the detector pixel displacement.

Parameters:

r_source (RSource)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

Examples

>>> d = G140H()
>>> d.grating
'g140h'

class unite.instrument.nirspec.disperser.G140M(r_source='point', *, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: NIRSpec

NIRSpec G140M disperser.

Convenience subclass of NIRSpec with the grating fixed to "g140m". Only r_source and calibration tokens need to be specified.

Parameters:

r_source"uniform", "uniformly-illuminated", "point", or "point-source", optional: Which resolving-power calibration to use (default "point").
namestr, optional: Human-readable label. Defaults to "G140M".
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the detector pixel displacement.

Parameters:

r_source (RSource)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

Examples

>>> d = G140M()
>>> d.grating
'g140m'

class unite.instrument.nirspec.disperser.G235H(r_source='point', *, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: NIRSpec

NIRSpec G235H disperser.

Convenience subclass of NIRSpec with the grating fixed to "g235h". Only r_source and calibration tokens need to be specified.

Parameters:

r_source"uniform", "uniformly-illuminated", "point", or "point-source", optional: Which resolving-power calibration to use (default "point").
namestr, optional: Human-readable label. Defaults to "G235H".
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the detector pixel displacement.

Parameters:

r_source (RSource)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

Examples

>>> d = G235H()
>>> d.grating
'g235h'

class unite.instrument.nirspec.disperser.G235M(r_source='point', *, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: NIRSpec

NIRSpec G235M disperser.

Convenience subclass of NIRSpec with the grating fixed to "g235m". Only r_source and calibration tokens need to be specified.

Parameters:

r_source"uniform", "uniformly-illuminated", "point", or "point-source", optional: Which resolving-power calibration to use (default "point").
namestr, optional: Human-readable label. Defaults to "G235M".
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the detector pixel displacement.

Parameters:

r_source (RSource)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

Examples

>>> d = G235M()
>>> d.grating
'g235m'

class unite.instrument.nirspec.disperser.G395H(r_source='point', *, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: NIRSpec

NIRSpec G395H disperser.

Convenience subclass of NIRSpec with the grating fixed to "g395h". Only r_source and calibration tokens need to be specified.

Parameters:

r_source"uniform", "uniformly-illuminated", "point", or "point-source", optional: Which resolving-power calibration to use (default "point").
namestr, optional: Human-readable label. Defaults to "G395H".
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the detector pixel displacement.

Parameters:

r_source (RSource)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

Examples

>>> d = G395H()
>>> d.grating
'g395h'

class unite.instrument.nirspec.disperser.G395M(r_source='point', *, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: NIRSpec

NIRSpec G395M disperser.

Convenience subclass of NIRSpec with the grating fixed to "g395m". Only r_source and calibration tokens need to be specified.

Parameters:

r_source"uniform", "uniformly-illuminated", "point", or "point-source", optional: Which resolving-power calibration to use (default "point").
namestr, optional: Human-readable label. Defaults to "G395M".
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the detector pixel displacement.

Parameters:

r_source (RSource)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

Examples

>>> d = G395M()
>>> d.grating
'g395m'

class unite.instrument.nirspec.disperser.PRISM(r_source='point', *, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: NIRSpec

NIRSpec PRISM disperser.

Convenience subclass of NIRSpec with the grating fixed to "prism". Only r_source and calibration tokens need to be specified.

Parameters:

r_source"uniform", "uniformly-illuminated", "point", or "point-source", optional: Which resolving-power calibration to use (default "point").
namestr, optional: Human-readable label. Defaults to "PRISM".
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the detector pixel displacement.

Parameters:

r_source (RSource)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

Examples

>>> d = PRISM()
>>> d.grating
'prism'

class unite.instrument.nirspec.disperser.NIRSpec(grating, r_source='point', *, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: Disperser

Disperser for a JWST NIRSpec grating or prism configuration.

Parameters:

gratingstr: NIRSpec grating name. One of "prism", "g140m", "g140h", "g235m", "g235h", "g395m", "g395h" (case-insensitive).
r_source"uniform", "uniformly-illuminated", "point", or "point-source", optional: Which resolving-power calibration to use. "uniform" or "uniformly-illuminated" interpolates the tabulated JDOX R(λ) curve for uniformly illuminated sources; "point" or "point-source" (default) evaluates the polynomial fit from de Graaff et al. (2025), which is tailored for point-source observations.
namestr, optional: Human-readable label. Defaults to the grating name (upper-case).
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the detector pixel displacement.

Parameters:

grating (str)
r_source (RSource)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

Notes

The linear dispersion dλ/dpix is always taken from the JDOX dispersion tables regardless of the r_source choice.

All wavelengths are in microns (astropy.units.um).

Examples

>>> d = NIRSpec("g235h")
>>> d.grating
'g235h'
>>> d.r_source
'point'

>>> d_uniform = NIRSpec("prism", r_source="uniform")
>>> d_uniform.r_source
'uniform'

R(wavelength)[source]¶: Return the resolving power at the given wavelengths (µm).

dlam_dpix(wavelength)[source]¶: Return dλ/dpix in µm/pixel, interpolated from the JDOX table.

SDSS Disperser¶

SDSS spectrograph disperser implementation.

Provides SDSSDisperser, a concrete Disperser for SDSS optical spectra. The resolving power R(λ) is derived from the wdisp column (wavelength dispersion per pixel, in Angstroms) of standard SDSS spec-*.fits files at load time via from_sdss_fits().

Before data is loaded, the disperser can be constructed with default or placeholder R values, allowing calibration tokens to be configured and the disperser configuration to be serialized.

Examples¶

>>> from unite.instrument.sdss import SDSSDisperser
>>> d = SDSSDisperser()
>>> d.unit
Unit("Angstrom")

class unite.instrument.sdss.disperser.SDSSDisperser(name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: Disperser

Disperser for SDSS optical spectra.

The SDSS spectrographs use a log-linear wavelength grid. The resolving power and linear dispersion are set from data at spectrum load time (from_sdss_fits()), but the disperser can also be pre-constructed with calibration tokens for serialization.

Parameters:

wavelengthArrayLike, optional: Pixel-center wavelengths in Angstroms. When not provided, R() and dlam_dpix() return placeholder values (constant R=2000, dlam_dpix=1.0).
wdispArrayLike, optional: Wavelength dispersion per pixel (Angstroms/pixel) from the SDSS wdisp column. Same length as wavelength. The resolving power is computed as R(λ) = λ / (2.355 * wdisp) (since wdisp is sigma in wavelength units per pixel, and FWHM = 2.355 * sigma).
namestr, optional: Human-readable label. Defaults to 'SDSS'.
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the pixel shift.

Parameters:

name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

R(wavelength)[source]¶

Return the resolving power at the given wavelengths (Angstrom).

Return type:

Parameters:

wavelengthArrayLike: Wavelength values in Angstroms.

Returns:

ArrayLike: Resolving power R at each wavelength.

Parameters:

dlam_dpix(wavelength)[source]¶

Return dλ/dpix in Angstrom/pixel.

Return type:

Parameters:

wavelengthArrayLike: Wavelength values in Angstroms.

Returns:

ArrayLike: Linear dispersion at each wavelength.

Parameters:

DESI Disperser¶

DESI spectrograph disperser implementation.

Provides DESIDisperser, a concrete Disperser for DESI optical spectra. The resolving power R(λ) is derived from the banded LSF resolution matrix stored in native DESI spectra-*.fits files at load time via from_desi_fits().

Before data is loaded, the disperser can be constructed with placeholder values, allowing calibration tokens to be configured.

Examples¶

>>> from unite.instrument.desi import DESIDisperser
>>> d = DESIDisperser('B')
>>> d.unit
Unit("Angstrom")
>>> d.arm
'B'

class unite.instrument.desi.disperser.DESIDisperser(arm, name='', r_scale=None, flux_scale=None, pix_offset=None)[source]¶

Bases: Disperser

Disperser for a single DESI spectrograph arm.

The DESI focal-plane spectrograph splits each spectrum into three arms: B (blue, 3600-5800 Angstrom), R (red, 5760-7620 Angstrom), and Z (near-IR, 7520-9824 Angstrom). The resolving power and linear dispersion are set from data at spectrum load time (from_desi_fits()), but the disperser can also be pre-constructed with calibration tokens for serialization.

Parameters:

arm{‘B’, ‘R’, ‘Z’}: Spectrograph arm to model.
namestr, optional: Human-readable label. Defaults to the lower-case arm letter.
r_scaleRScale, optional: Token for the resolving-power scale.
flux_scaleFluxScale, optional: Token for the flux normalisation.
pix_offsetPixOffset, optional: Token for the pixel shift.

Parameters:

arm (str)
name (str)
r_scale (RScale | None)
flux_scale (FluxScale | None)
pix_offset (PixOffset | None)

ARMS: tuple[str, ...] = ('B', 'R', 'Z')¶

R(wavelength)[source]¶

Return the resolving power at the given wavelengths (Angstrom).

Return type:

Parameters:

wavelengthArrayLike: Wavelength values in Angstroms.

Returns:

ArrayLike: Resolving power R at each wavelength.

Parameters:

dlam_dpix(wavelength)[source]¶

Return dλ/dpix in Angstrom/pixel.

Return type:

Parameters:

wavelengthArrayLike: Wavelength values in Angstroms.

Returns:

ArrayLike: Linear dispersion at each wavelength.

Parameters:

Instrument¶

Base Classes and Calibration Tokens¶

Instrument Configuration¶

Sharing tokens¶

Degeneracy warning¶

Serialization¶

Examples¶

Generic Implementations¶

NIRSpec Dispersers¶

SDSS Disperser¶

Examples¶

DESI Disperser¶

Examples¶