Interface for spectra, images and cubes (mpdaf.obj
)¶
The mpdaf.obj
package provides a way to load a MUSE cube created by the MUSE
pipeline (i.e. a 3GB FITS data cube of approximately 300x300x3680 pixels) into a
Python object that manages spatial world-coordinates, wavelength world
coordinates, pixel variances and bad pixel information.
It is then relatively easy to extract smaller cubes, narrow-band images or spectra from the cube. The world coordinates, associated variances and bad-pixel masks are propagated into these extracted cubes, images, and spectra. Many useful operations like masking, interpolation, re-sampling, smoothing and profile fitting are also provided.
Contents:
Reference/API¶
mpdaf.obj Package¶
Functions¶
UnitArray (array, old_unit, new_unit) |
|
UnitMaskedArray (mask_array, old_unit, new_unit) |
|
axis_increments_from_cd (cd) |
Return the angular increments of pixels along the Y and X axes of an image array whose coordinates are described by a specified FITS CD matrix. |
bounding_box (form, center, radii, shape[, …]) |
Return Y-axis and X-axis slice objects that bound a rectangular image region that just encloses either an ellipse or a rectangle, where the rectangle has a specified center position, Y-axis and X-axis radii, and a given rotation angle relative to the image axes. |
deg2dms (x) |
Transform degrees to degrees:arcminutes:arcseconds strings. |
deg2hms (x) |
Transform degrees to hours:minutes:seconds strings. |
deg2sexa (x) |
Transform equatorial coordinates from degrees to sexagesimal strings. |
determine_refframe (phdr) |
Determine the reference frame and equinox in standard FITS WCS terms. |
dms2deg (x) |
Transform degrees:arcminutes:arcseconds strings to degrees. |
flux2mag (flux, err_flux, wave) |
Convert flux from erg. |
gauss_image ([shape, wcs, factor, gauss, …]) |
Create a new image from a 2D gaussian. |
hms2deg (x) |
Transform hours:minutes:seconds strings to degrees. |
image_angle_from_cd (cd[, unit]) |
Return the rotation angle of the image. |
is_float (x) |
Test if x is a float number. |
is_int (x) |
Test if x is an int number. |
is_number (x) |
Test if x is a number. |
iter_ima (cube[, index]) |
An iterator over the images of successive spectral pixels in a Cube |
iter_spe (cube[, index]) |
An iterator over the spectra of successive image pixels in a Cube |
mag2flux (mag, wave) |
Convert flux from AB mag to erg. |
moffat_image ([shape, wcs, factor, moffat, …]) |
Create a new image from a 2D Moffat function. |
sexa2deg (x) |
Transform equatorial coordinates from sexagesimal strings to degrees. |
Classes¶
Cube ([filename, hdulist, data, mask, var, …]) |
This class manages Cube objects, which contain images at multiple wavelengths. |
CubeList (files[, scalelist, offsetlist]) |
Manages a list of cubes and handles the combination. |
CubeMosaic (files, output_wcs, **kwargs) |
Manages a list of cubes and handles the combination to make a mosaic. |
DataArray ([filename, hdulist, data, mask, …]) |
Parent class for Cube , Image and Spectrum . |
Gauss1D (lpeak, peak, flux, fwhm, cont, …) |
This class stores 1D Gaussian parameters. |
Gauss2D (center, flux, fwhm, cont, rot, peak, …) |
This class stores 2D gaussian parameters. |
Image ([filename, ext, wcs, data, var, unit, …]) |
Manage image, optionally including a variance and a bad pixel mask. |
Moffat2D (center, flux, fwhm, cont, n, rot, …) |
This class stores 2D moffat parameters. |
SpatialFrequencyLimits (fmax, rot) |
Allow to keep track of the spatial frequency limits of an image. |
Spectrum ([filename, hdulist, data, mask, …]) |
Spectrum objects contain 1D arrays of numbers, optionally accompanied by corresponding variances. |
WCS ([hdr, crpix, crval, cdelt, deg, rot, …]) |
The WCS class manages the world coordinates of the spatial axes of MPDAF images, using the pywcs package. |
WaveCoord ([hdr, crpix, cdelt, crval, cunit, …]) |
WaveCoord class manages world coordinates in spectral direction. |