HMIMap¶

class sunpy.map.sources.HMIMap(data, header, **kwargs)[source]¶

Bases: sunpy.map.mapbase.GenericMap

HMI Image Map.

HMI consists of a refracting telescope, a polarization selector, an image stabilization system, a narrow band tunable filter and two 4096 pixel CCD cameras. It observes the full solar disk in the Fe I absorption line at 6173 Angstrom with a resolution of 1 arc-second. HMI takes images in a sequence of tuning and polarizations at a 4-second cadence for each camera. One camera is dedicated to a 45 s Doppler and line-of-sight field sequence while the other to a 90 s vector field sequence.

References

Notes

A number of the properties of this class are returned as two-value named tuples that can either be indexed by position ([0] or [1]) or be accessed by the names (.x and .y) or (.axis1 and .axis2). Things that refer to pixel axes use the .x, .y convention, where x and y refer to the FITS axes (x for columns y for rows). Spatial axes use .axis1 and .axis2 which correspond to the first and second axes in the header. axis1 corresponds to the coordinate axis for x and axis2 corresponds to y.

This class makes some assumptions about the WCS information contained in the meta data. The first and most extensive assumption is that it is FITS-like WCS information as defined in the FITS WCS papers.

Within this scope it also makes some other assumptions.

In the case of APIS convention headers where the CROTAi/j arguments are
provided it assumes that these can be converted to the standard PCi_j notation using equations 32 in Thompson (2006).
If a CDi_j matrix is provided it is assumed that it can be converted to a
PCi_j matrix and CDELT keywords as described in Greisen & Calabretta (2002)
The ‘standard’ FITS keywords that are used by this class are the PCi_j
matrix and CDELT, along with the other keywords specified in the WCS papers. All subclasses of this class must convert their header information to this formalism. The CROTA to PCi_j conversion is done in this class.

Warning

This class currently assumes that a header with the CDi_j matrix information also includes the CDELT keywords, without these keywords this class will not process the WCS. Also the rotation_matrix does not work if the CDELT1 and CDELT2 keywords are exactly equal. Also, if a file with more than two dimensions is feed into the class, only the first two dimensions (NAXIS1, NAXIS2) will be loaded and the rest will be discarded.

Attributes Summary

`bottom_left_coord`	The physical coordinate at the center of the bottom left ([0, 0]) pixel.
`carrington_latitude`	Observer Carrington latitude.
`carrington_longitude`	Observer Carrington longitude.
`center`	Return a coordinate object for the center pixel of the array.
`cmap`	Return the `matplotlib.colors.Colormap` instance this map uses.
`coordinate_frame`	An `astropy.coordinates.BaseCoordinateFrame` instance created from the coordinate information for this Map, or None if the frame cannot be determined.
`coordinate_system`	Coordinate system used for x and y axes (ctype1/2).
`data`	The stored dataset.
`date`	Image observation time.
`date_average`	Average time of the image acquisition.
`date_end`	Time of the end of the image acquisition.
`date_start`	Time of the beginning of the image acquisition.
`detector`	Detector name.
`dimensions`	The dimensions of the array (x axis first, y axis second).
`dsun`	Observer distance from the center of the Sun.
`dtype`	The `numpy.dtype` of the array of the map.
`exposure_time`	Exposure time of the image.
`fits_header`	A `Header` representation of the `meta` attribute.
`heliographic_latitude`	Observer heliographic latitude.
`heliographic_longitude`	Observer heliographic longitude.
`instrument`	Instrument name.
`latex_name`	LaTeX formatted description of the Map.
`mask`	Mask for the dataset, if any.
`measurement`	Returns the measurement type.
`meta`	The map metadata.
`name`	Human-readable description of the Map.
`ndim`	The value of `numpy.ndarray.ndim` of the data array of the map.
`nickname`	An abbreviated human-readable description of the map-type; part of the Helioviewer data model.
`observatory`	Returns the observatory.
`observer_coordinate`	the property method being decorated
`processing_level`	Returns the FITS processing level if present.
`quantity`	Unitful representation of the map data.
`reference_coordinate`	Reference point WCS axes in data units (i.e.
`reference_pixel`	Pixel of reference coordinate.
`rotation_matrix`	Matrix describing the rotation required to align solar North with the top of the image.
`rsun_meters`	Assumed radius of observed emission from the Sun center.
`rsun_obs`	Angular radius of the observation from Sun center.
`scale`	Image scale along the x and y axes in units/pixel (i.e.
`shifted_value`	The total shift applied to the reference coordinate by past applications of `shift`.
`spatial_units`	Image coordinate units along the x and y axes (i.e.
`timeunit`	The `Unit` of the exposure time of this observation.
`top_right_coord`	The physical coordinate at the center of the the top right ([-1, -1]) pixel.
`uncertainty`	Uncertainty in the dataset, if any.
`unit`	Unit of the map data.
`wavelength`	Wavelength of the observation.
`waveunit`	The `Unit` of the wavelength of this observation.
`wcs`	the property method being decorated

Methods Summary

`contour`(level, **kwargs)	Returns coordinates of the contours for a given level value.
`draw_contours`(levels[, axes])	Draw contours of the data.
`draw_grid`([axes, grid_spacing, annotate])	Draws a coordinate overlay on the plot in the Heliographic Stonyhurst coordinate system.
`draw_limb`([axes, resolution])	Draws the solar limb as seen by the map's observer.
`draw_quadrangle`(bottom_left, *[, width, ...])	Draw a quadrangle defined in world coordinates on the plot using Astropy's `Quadrangle`.
`is_datasource_for`(data, header, **kwargs)	Determines if header corresponds to an HMI image
`max`(args, *kwargs)	Calculate the maximum value of the data array.
`mean`(args, *kwargs)	Calculate the mean of the data array.
`min`(args, *kwargs)	Calculate the minimum value of the data array.
`peek`([draw_limb, draw_grid, colorbar])	Displays a graphical overview of the data in this object for user evaluation.
`pixel_to_world`(x, y)	Convert a pixel coordinate to a data (world) coordinate.
`plot`([annotate, axes, title, autoalign, ...])	Plots the map object using matplotlib, in a method equivalent to `imshow()` using nearest neighbor interpolation.
`quicklook`()	Display a quicklook summary of the Map instance using the default web browser.
`reproject_to`(target_wcs[, algorithm, ...])	Reproject the map to a different world coordinate system (WCS)
`resample`(dimensions[, method])	Resample to new dimension sizes.
`rotate`([angle, rmatrix, order, scale, ...])	Returns a new rotated and rescaled map.
`save`(filepath[, filetype])	Saves the SunPy Map object to a file.
`shift`(axis1, axis2)	Returns a map shifted by a specified amount to, for example, correct for a bad map location.
`std`(args, *kwargs)	Calculate the standard deviation of the data array.
`submap`(bottom_left, *[, top_right, width, ...])	Returns a submap defined by a rectangle.
`superpixel`(dimensions[, offset, func])	Returns a new map consisting of superpixels formed by applying 'func' to the original map data.
`world_to_pixel`(coordinate)	Convert a world (data) coordinate to a pixel coordinate.

Attributes Documentation

bottom_left_coord¶: The physical coordinate at the center of the bottom left ([0, 0]) pixel.

carrington_latitude¶: Observer Carrington latitude.

carrington_longitude¶: Observer Carrington longitude.

center¶

Return a coordinate object for the center pixel of the array.

If the array has an even number of pixels in a given dimension, the coordinate returned lies on the edge between the two central pixels.

cmap¶: Return the matplotlib.colors.Colormap instance this map uses.

coordinate_frame¶: An astropy.coordinates.BaseCoordinateFrame instance created from the coordinate information for this Map, or None if the frame cannot be determined.

coordinate_system¶

Coordinate system used for x and y axes (ctype1/2).

If not present, defaults to (HPLN-TAN, HPLT-TAN), and emits a warning.

data¶

The stored dataset.

Type: ndarray-like

date¶

Image observation time.

For different combinations of map metadata this can return either the start time, end time, or a time between these. It is recommended to use date_average, date_start, or date_end instead if you need one of these specific times.

Taken from, in order of preference:

The DATE-OBS FITS keyword
date_average
date_start
date_end
The current time

date_average¶

Average time of the image acquisition.

Taken from the DATE-AVG FITS keyword if present, otherwise halfway between date_start and date_end if both peices of metadata are present.

date_end¶

Time of the end of the image acquisition.

Taken from the DATE-END FITS keyword.

date_start¶

Time of the beginning of the image acquisition.

Taken from the DATE-BEG FITS keyword.

detector¶

dimensions¶: The dimensions of the array (x axis first, y axis second).

dsun¶: Observer distance from the center of the Sun.

dtype¶: The numpy.dtype of the array of the map.

exposure_time¶

Exposure time of the image.

This is taken from the ‘EXPTIME’ FITS keyword.

fits_header¶: A Header representation of the meta attribute.

heliographic_latitude¶: Observer heliographic latitude.

heliographic_longitude¶: Observer heliographic longitude.

instrument¶: Instrument name.

latex_name¶: LaTeX formatted description of the Map.

mask¶

Mask for the dataset, if any.

Masks should follow the numpy convention that valid data points are marked by False and invalid ones with True.

Type: any type

measurement¶: Returns the measurement type.

meta¶

The map metadata.

This is used to intepret the map data. It may have been modified from the original metadata by sunpy. See the added_items, removed_items and modified_items properties of MetaDict to query how the metadata has been modified.

name¶: Human-readable description of the Map.

ndim¶: The value of numpy.ndarray.ndim of the data array of the map.

nickname¶: An abbreviated human-readable description of the map-type; part of the Helioviewer data model.

observatory¶: Returns the observatory.

observer_coordinate¶

the property method being decorated

Type: prop

processing_level¶

Returns the FITS processing level if present.

This is taken from the ‘LVL_NUM’ FITS keyword.

quantity¶: Unitful representation of the map data.

reference_coordinate¶: Reference point WCS axes in data units (i.e. crval1, crval2). This value includes a shift if one is set.

reference_pixel¶

Pixel of reference coordinate.

The pixel returned uses zero-based indexing, so will be 1 pixel less than the FITS CRPIX values.

rotation_matrix¶

Matrix describing the rotation required to align solar North with the top of the image.

The order or precendence of FITS keywords which this is taken from is: - PC*_* - CD*_* - CROTA*

rsun_meters¶

Assumed radius of observed emission from the Sun center.

This is taken from the RSUN_REF FITS keyword, if present. If not, and angular radius metadata is present, it is calculated from rsun_obs and dsun. If neither pieces of metadata are present, defaults to the standard photospheric radius.

rsun_obs¶

Angular radius of the observation from Sun center.

This value is taken (in order of preference) from the ‘RSUN_OBS’, ‘SOLAR_R’, or ‘RADIUS’ FITS keywords. If none of these keys are present, the angular radius is calculated from rsun_meters and dsun.

scale¶: Image scale along the x and y axes in units/pixel (i.e. cdelt1, cdelt2).

shifted_value¶: The total shift applied to the reference coordinate by past applications of shift.

spatial_units¶: Image coordinate units along the x and y axes (i.e. cunit1, cunit2).

timeunit¶

The Unit of the exposure time of this observation.

Taken from the “TIMEUNIT” FITS keyword, and defaults to seconds (as per) the FITS standard).

top_right_coord¶: The physical coordinate at the center of the the top right ([-1, -1]) pixel.

uncertainty¶

Uncertainty in the dataset, if any.

Should have an attribute uncertainty_type that defines what kind of uncertainty is stored, such as 'std' for standard deviation or 'var' for variance. A metaclass defining such an interface is NDUncertainty but isn’t mandatory.

Type: any type

unit¶

Unit of the map data.

This is taken from the ‘BUNIT’ FITS keyword. If no ‘BUNIT’ entry is present in the metadata then this returns None. If the ‘BUNIT’ value cannot be parsed into a unit a warning is raised, and None returned.

wavelength¶

Wavelength of the observation.

This is taken from the ‘WAVELNTH’ FITS keywords. If the keyword is not present, defaults to None. If ‘WAVEUNIT’ keyword isn’t present, defaults to dimensionless units.

waveunit¶

The Unit of the wavelength of this observation.

This is taken from the ‘WAVEUNIT’ FITS keyword. If the keyword is not present, defaults to None

wcs¶

the property method being decorated

Type: prop

Methods Documentation

contour(level, **kwargs)¶

Returns coordinates of the contours for a given level value.

For details of the contouring algorithm see skimage.measure.find_contours.

Parameters

level (float, astropy.units.Quantity) – Value along which to find contours in the array. If the map unit attribute is not None, this must be a Quantity with units equivalent to the map data units.
kwargs – Additional keyword arguments are passed to skimage.measure.find_contours.

Returns

contours (list of (n,2) SkyCoord) – Coordinates of each contour.

Examples

>>> import astropy.units as u
>>> import sunpy.map
>>> import sunpy.data.sample  
>>> aia = sunpy.map.Map(sunpy.data.sample.AIA_171_IMAGE)  
>>> contours = aia.contour(50000 * u.ct)  
>>> print(contours[0])  
    <SkyCoord (Helioprojective: obstime=2011-06-07T06:33:02.770, rsun=696000.0 km, observer=<HeliographicStonyhurst Coordinate (obstime=2011-06-07T06:33:02.770, rsun=696000.0 km): (lon, lat, radius) in (deg, deg, m)
(-0.00406308, 0.04787238, 1.51846026e+11)>): (Tx, Ty) in arcsec
[(719.59798458, -352.60839064), (717.19243987, -353.75348121),
...

See also

None

draw_contours(levels, axes=None, **contour_args)¶

Draw contours of the data.

Parameters

levels (Quantity) – A list of numbers indicating the contours to draw. These are given as a percentage of the maximum value of the map data, or in units equivalent to the unit attribute.
axes (matplotlib.axes.Axes) – The axes on which to plot the contours. Defaults to the current axes.

Returns

cs (list) – The QuadContourSet object, after it has been added to axes.

Notes

Extra keyword arguments to this function are passed through to the contour function.

draw_grid(axes=None, grid_spacing: Unit("deg") = <Quantity 15. deg>, annotate=True, **kwargs)¶

Draws a coordinate overlay on the plot in the Heliographic Stonyhurst coordinate system.

To overlay other coordinate systems see the WCSAxes Documentation

Parameters

axes (axes or None) – Axes to plot limb on, or None to use current axes.
grid_spacing (Quantity) – Spacing for longitude and latitude grid, if length two it specifies (lon, lat) spacing.
annotate (bool) – Passing False disables the axes labels and the ticks on the top and right axes.

Returns

overlay (CoordinatesMap) – The wcsaxes coordinate overlay instance.

Notes

Keyword arguments are passed onto the sunpy.visualization.wcsaxes_compat.wcsaxes_heliographic_overlay function.

draw_limb(axes=None, *, resolution=1000, **kwargs)¶

Draws the solar limb as seen by the map’s observer.

The limb is a circle for only the simplest plots. If the coordinate frame of the limb is different from the coordinate frame of the plot axes, not only may the limb not be a true circle, a portion of the limb may be hidden from the observer. In that case, the circle is divided into visible and hidden segments, represented by solid and dotted lines, respectively.

Parameters

axes (axes or None) – Axes to plot limb on or None to use current axes.
resolution (int) – The number of points to use to represent the limb.

Returns

visible (Polygon or Circle) – The patch added to the axes for the visible part of the limb (i.e., the “near” side of the Sun).
hidden (Polygon or None) – The patch added to the axes for the hidden part of the limb (i.e., the “far” side of the Sun).

Notes

Keyword arguments are passed onto the patches.

If the limb is a true circle, visible will instead be Circle and hidden will be None. If there are no visible points (e.g., on a synoptic map any limb is fully) visible hidden will be None.

To avoid triggering Matplotlib auto-scaling, these patches are added as artists instead of patches. One consequence is that the plot legend is not populated automatically when the limb is specified with a text label. See Composing Custom Legends in the Matplotlib documentation for examples of creating a custom legend.

draw_quadrangle(bottom_left, *, width: (Unit('deg'), Unit('pix')) = None, height: (Unit('deg'), Unit('pix')) = None, axes=None, top_right=None, **kwargs)¶

Draw a quadrangle defined in world coordinates on the plot using Astropy’s Quadrangle.

This draws a quadrangle that has corners at (bottom_left, top_right), and has sides aligned with the coordinate axes of the frame of bottom_left, which may be different from the coordinate axes of the map.

If width and height are specified, they are respectively added to the longitude and latitude of the bottom_left coordinate to calculate a top_right coordinate.

Parameters

bottom_left (SkyCoord or Quantity) – The bottom-left coordinate of the rectangle. If a SkyCoord it can have shape (2,) and simultaneously define top_right. If specifying pixel coordinates it must be given as an Quantity object with pixel units (e.g., pix).
top_right (SkyCoord or Quantity, optional) – The top-right coordinate of the quadrangle. If top_right is specified width and height must be omitted.
width (astropy.units.Quantity, optional) – The width of the quadrangle. Required if top_right is omitted.
height (astropy.units.Quantity) – The height of the quadrangle. Required if top_right is omitted.
axes (matplotlib.axes.Axes) – The axes on which to plot the quadrangle. Defaults to the current axes.

Returns

quad (Quadrangle) – The added patch.

Notes

Extra keyword arguments to this function are passed through to the Quadrangle instance.

Examples

classmethod is_datasource_for(data, header, **kwargs)[source]¶: Determines if header corresponds to an HMI image

max(*args, **kwargs)¶: Calculate the maximum value of the data array.

mean(*args, **kwargs)¶: Calculate the mean of the data array.

min(*args, **kwargs)¶: Calculate the minimum value of the data array.

peek(draw_limb=False, draw_grid=False, colorbar=True, **matplot_args)¶

Displays a graphical overview of the data in this object for user evaluation. For the creation of plots, users should instead use the plot method and Matplotlib’s pyplot framework.

Parameters

draw_limb (bool) – Whether the solar limb should be plotted.
draw_grid (bool or Quantity) – Whether solar meridians and parallels are plotted. If Quantity then sets degree difference between parallels and meridians.
colorbar (bool) – Whether to display a colorbar next to the plot.
**matplot_args (dict) – Matplotlib Any additional imshow arguments that should be used when plotting.

pixel_to_world(x: Unit('pix'), y: Unit('pix'))¶

Convert a pixel coordinate to a data (world) coordinate.

Parameters

x (Quantity) – Pixel coordinate of the CTYPE1 axis. (Normally solar-x).
y (Quantity) – Pixel coordinate of the CTYPE2 axis. (Normally solar-y).

Returns

coord (astropy.coordinates.SkyCoord) – A coordinate object representing the output coordinate.

plot(annotate=True, axes=None, title=True, autoalign=False, clip_interval: Unit('%') = None, **imshow_kwargs)¶

Plots the map object using matplotlib, in a method equivalent to imshow() using nearest neighbor interpolation.

Parameters

annotate (bool, optional) – If True, the data is plotted at its natural scale; with title and axis labels.
axes (Axes or None) – If provided the image will be plotted on the given axes. Else the current Matplotlib axes will be used.
title (str, bool, optional) – The plot title. If True, uses the default title for this map.
clip_interval (two-element Quantity, optional) – If provided, the data will be clipped to the percentile interval bounded by the two numbers.
autoalign (bool or str, optional) – If other than False, the plotting accounts for any difference between the WCS of the map and the WCS of the WCSAxes axes (e.g., a difference in rotation angle). If pcolormesh, this method will use pcolormesh() instead of the default imshow(). Specifying True is equivalent to specifying pcolormesh.
**imshow_kwargs (dict) – Any additional imshow arguments are passed to imshow().

Examples

>>> # Simple Plot with color bar
>>> aia.plot()   
>>> plt.colorbar()   
>>> # Add a limb line and grid
>>> aia.plot()   
>>> aia.draw_limb()   
>>> aia.draw_grid()   

Notes

The autoalign functionality is computationally intensive. If the plot will be interactive, the alternative approach of preprocessing the map (e.g., de-rotating it) to match the desired axes will result in better performance.

When combining autoalign functionality with Helioprojective coordinates, portions of the map that are beyond the solar disk may not appear, which may also inhibit Matplotlib’s autoscaling of the plot limits. The plot limits can be set manually. To preserve the off-disk parts of the map, using the assume_spherical_screen() context manager may be appropriate.

quicklook()¶

Display a quicklook summary of the Map instance using the default web browser.

Notes

The image colormap uses histogram equalization.

Clicking on the image to switch between pixel space and coordinate space requires Javascript support to be enabled in the web browser.

Examples

>>> from sunpy.map import Map
>>> import sunpy.data.sample  
>>> smap = Map(sunpy.data.sample.AIA_171_IMAGE)  
>>> smap.quicklook()  

(which will open the following content in the default web browser)

<sunpy.map.sources.sdo.AIAMap object at 0x7f40b623d490>

Observatory	SDO
Instrument	AIA 3
Detector	AIA
Measurement	171.0 Angstrom
Wavelength	171.0 Angstrom
Observation Date	2011-06-07 06:33:02
Exposure Time	0.234256 s
Dimension	[1024. 1024.] pix
Coordinate System	helioprojective
Scale	[2.402792 2.402792] arcsec / pix
Reference Pixel	[511.5 511.5] pix
Reference Coord	[3.22309951 1.38578135] arcsec

Image colormap uses histogram equalization
Click on the image to toggle between units

reproject_to(target_wcs, algorithm='interpolation', return_footprint=False, **reproject_args)¶

Reproject the map to a different world coordinate system (WCS)

Note

This method requires the optional package reproject to be installed.

Additional keyword arguments are passed through to the reprojection function.

Parameters

target_wcs (dict or WCS) – The destination FITS WCS header or WCS instance
algorithm (str) – One of the supported reproject algorithms (see below)
return_footprint (bool) – If True, the footprint is returned in addition to the new map. Defaults to False.

Returns

outmap (GenericMap) – The reprojected map
footprint (ndarray) – Footprint of the input arary in the output array. Values of 0 indicate no coverage or valid values in the input image, while values of 1 indicate valid values. Intermediate values indicate partial coverage. Only returned if return_footprint is True.

Notes

The reprojected map does not preserve any metadata beyond the WCS-associated metadata.

The supported reproject algorithms are:

‘interpolation’ for reproject_interp()
‘adaptive’ for reproject_adaptive()
‘exact’ for reproject_exact()

See the respective documentation for these functions for additional keyword arguments that are allowed.

resample(dimensions: Unit('pix'), method='linear')¶

Resample to new dimension sizes.

Uses the same parameters and creates the same co-ordinate lookup points as IDL’’s congrid routine, which apparently originally came from a VAX/VMS routine of the same name.

Parameters

dimensions (Quantity) – Output pixel dimensions. The first argument corresponds to the ‘x’ axis and the second argument corresponds to the ‘y’ axis.
method (str) –
Method to use for resampling interpolation.
- 'neighbor' - Take closest value from original data.
- 'nearest' and 'linear' - Use n x 1-D interpolations using scipy.interpolate.interp1d.
- 'spline' - Uses piecewise polynomials (splines) for mapping the input array to new coordinates by interpolation using scipy.ndimage.map_coordinates.

Returns

out (GenericMap or subclass) – Resampled map

References

Rebinning

rotate(angle: Unit('deg') = None, rmatrix=None, order=4, scale=1.0, recenter=False, missing=0.0, use_scipy=False)¶

Returns a new rotated and rescaled map.

Specify either a rotation angle or a rotation matrix, but not both. If neither an angle or a rotation matrix are specified, the map will be rotated by the rotation angle in the metadata.

The map will be rotated around the reference coordinate defined in the meta data.

This method also updates the rotation_matrix attribute and any appropriate header data so that they correctly describe the new map.

Parameters

angle (Quantity) – The angle (degrees) to rotate counterclockwise.
rmatrix (array-like) – 2x2 linear transformation rotation matrix.
order (int) – Interpolation order to be used. Must be in the range 0-5. When using scikit-image this parameter is passed into skimage.transform.warp() (e.g., 4 corresponds to bi-quartic interpolation). When using scipy it is passed into scipy.ndimage.affine_transform() where it controls the order of the spline. Faster performance may be obtained at the cost of accuracy by using lower values. Default: 4
scale (float) – A scale factor for the image, default is no scaling
recenter (bool) – If True, position the axis of rotation at the center of the new map Default: False
missing (float) – The numerical value to fill any missing points after rotation. Default: 0.0
use_scipy (bool) – If True, forces the rotation to use scipy.ndimage.affine_transform(), otherwise it uses the skimage.transform.warp(). Default: False, unless scikit-image can’t be imported

Returns

out (GenericMap or subclass) – A new Map instance containing the rotated and rescaled data of the original map.

See also

sunpy.image.transform.affine_transform: The routine this method calls for the rotation.

Notes

This function will remove old CROTA keywords from the header. This function will also convert a CDi_j matrix to a PCi_j matrix.

See sunpy.image.transform.affine_transform() for details on the transformations, situations when the underlying data is modified prior to rotation, and differences from IDL’s rot().

save(filepath, filetype='auto', **kwargs)¶

Saves the SunPy Map object to a file.

Currently SunPy can only save files in the FITS format. In the future support will be added for saving to other formats.

Parameters

filepath (str) – Location to save file to.
filetype (str, optional) – Any supported file extension, defaults to auto".
hdu_type (ExtensionHDU instance or class, optional) – By default, a FITS file is written with the map in its primary HDU. If a type is given, a new HDU of this type will be created. If a HDU instance is given, its data and header will be updated from the map. Then that HDU instance will be written to the file.
kwargs – Any additional keyword arguments are passed to write_file.

shift(axis1: Unit('deg'), axis2: Unit('deg'))¶

Returns a map shifted by a specified amount to, for example, correct for a bad map location. These values are applied directly to the reference_coordinate. To check how much shift has already been applied see shifted_value

Parameters

axis1 (Quantity) – The shift to apply to the Longitude (solar-x) coordinate.
axis2 (Quantity) – The shift to apply to the Latitude (solar-y) coordinate

Returns

out (GenericMap or subclass) – A new shifted Map.

std(*args, **kwargs)¶: Calculate the standard deviation of the data array.

submap(bottom_left, *, top_right=None, width: (Unit('deg'), Unit('pix')) = None, height: (Unit('deg'), Unit('pix')) = None)¶

Returns a submap defined by a rectangle.

Any pixels which have at least part of their area inside the rectangle are returned. If the rectangle is defined in world coordinates, the smallest array which contains all four corners of the rectangle as defined in world coordinates is returned.

Parameters

bottom_left (astropy.units.Quantity or SkyCoord) – The bottom-left coordinate of the rectangle. If a SkyCoord it can have shape (2,) and simultaneously define top_right. If specifying pixel coordinates it must be given as an Quantity object with units of pixels.
top_right (astropy.units.Quantity or SkyCoord, optional) – The top-right coordinate of the rectangle. If top_right is specified width and height must be omitted.
width (astropy.units.Quantity, optional) – The width of the rectangle. Required if top_right is omitted.
height (astropy.units.Quantity) – The height of the rectangle. Required if top_right is omitted.

Returns

out (GenericMap or subclass) – A new map instance is returned representing to specified sub-region.

Notes

When specifying pixel coordinates, they are specified in Cartesian order not in numpy order. So, for example, the bottom_left= argument should be [left, bottom].

Examples

>>> import astropy.units as u
>>> from astropy.coordinates import SkyCoord
>>> import sunpy.map
>>> import sunpy.data.sample  
>>> aia = sunpy.map.Map(sunpy.data.sample.AIA_171_IMAGE)  
>>> bl = SkyCoord(-300*u.arcsec, -300*u.arcsec, frame=aia.coordinate_frame)  
>>> tr = SkyCoord(500*u.arcsec, 500*u.arcsec, frame=aia.coordinate_frame)  
>>> aia.submap(bl, top_right=tr)   
<sunpy.map.sources.sdo.AIAMap object at ...>
SunPy Map
---------
Observatory:         SDO
Instrument:          AIA 3
Detector:            AIA
Measurement:         171.0 Angstrom
Wavelength:          171.0 Angstrom
Observation Date:    2011-06-07 06:33:02
Exposure Time:       0.234256 s
Dimension:           [335. 335.] pix
Coordinate System:   helioprojective
Scale:               [2.402792 2.402792] arcsec / pix
Reference Pixel:     [126.5 125.5] pix
Reference Coord:     [3.22309951 1.38578135] arcsec
...

>>> aia.submap([0,0]*u.pixel, top_right=[5,5]*u.pixel)   
<sunpy.map.sources.sdo.AIAMap object at ...>
SunPy Map
---------
Observatory:         SDO
Instrument:          AIA 3
Detector:            AIA
Measurement:         171.0 Angstrom
Wavelength:          171.0 Angstrom
Observation Date:    2011-06-07 06:33:02
Exposure Time:       0.234256 s
Dimension:           [6. 6.] pix
Coordinate System:   helioprojective
Scale:               [2.402792 2.402792] arcsec / pix
Reference Pixel:     [511.5 511.5] pix
Reference Coord:     [3.22309951 1.38578135] arcsec
...

>>> width = 10 * u.arcsec
>>> height = 10 * u.arcsec
>>> aia.submap(bl, width=width, height=height)   
<sunpy.map.sources.sdo.AIAMap object at ...>
SunPy Map
---------
Observatory:         SDO
Instrument:          AIA 3
Detector:            AIA
Measurement:         171.0 Angstrom
Wavelength:          171.0 Angstrom
Observation Date:    2011-06-07 06:33:02
Exposure Time:       0.234256 s
Dimension:           [5. 5.] pix
Coordinate System:   helioprojective
Scale:               [2.402792 2.402792] arcsec / pix
Reference Pixel:     [125.5 125.5] pix
Reference Coord:     [3.22309951 1.38578135] arcsec
...

>>> bottom_left_vector = SkyCoord([0, 10]  * u.deg, [0, 10] * u.deg, frame='heliographic_stonyhurst')
>>> aia.submap(bottom_left_vector)   
<sunpy.map.sources.sdo.AIAMap object at ...>
SunPy Map
---------
Observatory:         SDO
Instrument:          AIA 3
Detector:            AIA
Measurement:         171.0 Angstrom
Wavelength:          171.0 Angstrom
Observation Date:    2011-06-07 06:33:02
Exposure Time:       0.234256 s
Dimension:           [70. 69.] pix
Coordinate System:   helioprojective
Scale:               [2.402792 2.402792] arcsec / pix
Reference Pixel:     [1.5 0.5] pix
Reference Coord:     [3.22309951 1.38578135] arcsec
...

superpixel(dimensions: Unit("pix"), offset: Unit("pix") = <Quantity [0., 0.] pix>, func=<function sum>)¶

Returns a new map consisting of superpixels formed by applying ‘func’ to the original map data.

Parameters

dimensions (tuple) – One superpixel in the new map is equal to (dimension[0], dimension[1]) pixels of the original map. The first argument corresponds to the ‘x’ axis and the second argument corresponds to the ‘y’ axis. If non-integer values are provided, they are rounded using int.
offset (tuple) – Offset from (0,0) in original map pixels used to calculate where the data used to make the resulting superpixel map starts. If non-integer value are provided, they are rounded using int.
func – Function applied to the original data. The function ‘func’ must take a numpy array as its first argument, and support the axis keyword with the meaning of a numpy axis keyword (see the description of sum for an example.) The default value of ‘func’ is sum; using this causes superpixel to sum over (dimension[0], dimension[1]) pixels of the original map.

Returns

out (GenericMap or subclass) – A new Map which has superpixels of the required size.

References

Summarizing blocks of an array using a moving window

world_to_pixel(coordinate)¶

Convert a world (data) coordinate to a pixel coordinate.

Parameters

coordinate (SkyCoord or BaseCoordinateFrame) – The coordinate object to convert to pixel coordinates.

Returns

x (Quantity) – Pixel coordinate on the CTYPE1 axis.
y (Quantity) – Pixel coordinate on the CTYPE2 axis.