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Package is "python-sunpy" Sun Apr 26 21:11:37 2026 rev:41 rq:1349306 version:7.1.2 Changes: -------- --- /work/SRC/openSUSE:Factory/python-sunpy/python-sunpy.changes 2026-04-18 21:34:29.696966313 +0200 +++ /work/SRC/openSUSE:Factory/.python-sunpy.new.11940/python-sunpy.changes 2026-04-26 21:14:18.796775592 +0200 @@ -1,0 +2,7 @@ +Sat Apr 25 22:05:45 UTC 2026 - Dirk Müller <[email protected]> + +- update to 7.1.2: + * Fixed a bug where SIP distortion information in a Map WCS was + ignored. + +------------------------------------------------------------------- Old: ---- sunpy-7.1.1.tar.gz New: ---- sunpy-7.1.2.tar.gz ++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++ Other differences: ------------------ ++++++ python-sunpy.spec ++++++ --- /var/tmp/diff_new_pack.WMSA9V/_old 2026-04-26 21:14:19.376799289 +0200 +++ /var/tmp/diff_new_pack.WMSA9V/_new 2026-04-26 21:14:19.380799453 +0200 @@ -19,7 +19,7 @@ %{?sle15_python_module_pythons} %define skip_python311 1 Name: python-sunpy -Version: 7.1.1 +Version: 7.1.2 Release: 0 Summary: SunPy core package: Python for Solar Physics License: Apache-2.0 AND BSD-2-Clause AND BSD-3-Clause AND MIT ++++++ sunpy-7.1.1.tar.gz -> sunpy-7.1.2.tar.gz ++++++ diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/.cruft.json new/sunpy-7.1.2/.cruft.json --- old/sunpy-7.1.1/.cruft.json 2026-03-26 10:58:57.000000000 +0100 +++ new/sunpy-7.1.2/.cruft.json 2026-04-19 23:08:51.000000000 +0200 @@ -1,6 +1,6 @@ { "template": "https://github.com/sunpy/package-template";, - "commit": "93c8bc491584f214226a039a35d0cbebe305cd31", + "commit": "6436220cebd96b3638682023e7149eb78e012fdc", "checkout": null, "context": { "cookiecutter": { @@ -33,7 +33,7 @@ ".github/workflows/sub_package_update.yml" ], "_template": "https://github.com/sunpy/package-template";, - "_commit": "93c8bc491584f214226a039a35d0cbebe305cd31" + "_commit": "6436220cebd96b3638682023e7149eb78e012fdc" } }, "directory": null diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/CHANGELOG.rst new/sunpy-7.1.2/CHANGELOG.rst --- old/sunpy-7.1.1/CHANGELOG.rst 2026-03-26 10:58:57.000000000 +0100 +++ new/sunpy-7.1.2/CHANGELOG.rst 2026-04-19 23:08:51.000000000 +0200 @@ -1,3 +1,12 @@ +7.1.2 (2026-04-19) +================== + +Bug Fixes +--------- + +- Fixed a bug where SIP distortion information in a Map WCS was ignored. (`#8573 <https://github.com/sunpy/sunpy/pull/8573>`__) + + 7.1.1 (2026-03-26) ================== diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/PKG-INFO new/sunpy-7.1.2/PKG-INFO --- old/sunpy-7.1.1/PKG-INFO 2026-03-26 10:59:06.566252200 +0100 +++ new/sunpy-7.1.2/PKG-INFO 2026-04-19 23:09:02.227515200 +0200 @@ -1,6 +1,6 @@ Metadata-Version: 2.4 Name: sunpy -Version: 7.1.1 +Version: 7.1.2 Summary: SunPy core package: Python for Solar Physics Author-email: The SunPy Community <[email protected]> License-Expression: BSD-3-Clause @@ -56,7 +56,7 @@ Requires-Dist: reproject>=0.13.0; extra == "map" Requires-Dist: scipy>=1.12.0; extra == "map" Provides-Extra: opencv -Requires-Dist: opencv-python>=4.8.0.74; extra == "opencv" +Requires-Dist: opencv-python!=4.13.0.*,>=4.8.0.74; extra == "opencv" Provides-Extra: net Requires-Dist: beautifulsoup4>=4.13.1; extra == "net" Requires-Dist: drms>=0.7.1; extra == "net" @@ -120,12 +120,15 @@ Requires-Dist: astroquery>=0.4.6; extra == "docs-gallery" Requires-Dist: jplephem>=2.19; extra == "docs-gallery" Requires-Dist: pillow; extra == "docs-gallery" +Requires-Dist: exifread; extra == "docs-gallery" Provides-Extra: dev Requires-Dist: sunpy[docs,tests]; extra == "dev" Dynamic: license-file +``sunpy`` +========= + SunPy core package: Python for Solar Physics -============================================ |SunPy Logo| diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/README.rst new/sunpy-7.1.2/README.rst --- old/sunpy-7.1.1/README.rst 2026-03-26 10:58:57.000000000 +0100 +++ new/sunpy-7.1.2/README.rst 2026-04-19 23:08:51.000000000 +0200 @@ -1,5 +1,7 @@ +``sunpy`` +========= + SunPy core package: Python for Solar Physics -============================================ |SunPy Logo| diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/examples/showcase/artemis-ii-eclipse.py new/sunpy-7.1.2/examples/showcase/artemis-ii-eclipse.py --- old/sunpy-7.1.1/examples/showcase/artemis-ii-eclipse.py 1970-01-01 01:00:00.000000000 +0100 +++ new/sunpy-7.1.2/examples/showcase/artemis-ii-eclipse.py 2026-04-19 23:08:51.000000000 +0200 @@ -0,0 +1,514 @@ +""" +======================== +Artemis-II Solar Eclipse +======================== + +This example demonstrates how to process a solar eclipse image taken by the +Artemis-II crew using a digital camera onboard the spacecraft during their +Lunar flyby on April 7, 2026. Due to the relative positions of the Artemis II +spacecraft and the Moon, this eclipse provided nearly 54 minutes of totality, +far exceeding what is possible on Earth. This example walks through turning +one of those crew photos, a plain JPEG with EXIF metadata and no pointing +information, into a `~sunpy.map.Map` with a Helioprojective WCS. Starting from +raw JPEG images with EXIF metadata, the observation time is extracted. Then, +the known positions of the Moon, Sun, and planets are retrieved from JPL +Horizons via `sunpy.coordinates.get_horizons_coord` to build an initial +Helioprojective WCS using `sunpy.map.header_helper.make_fitswcs_header`. +The camera roll angle is refined by comparing the predicted and detected pixel +positions of Saturn, Mars, and Mercury, identified automatically. + +Finally, the residual radial barrel distortion is modelled using a single +`Simple Imaging Polynomial (SIP) <https://fits.gsfc.nasa.gov/registry/sip>`_ +3rd order coefficient derived from the planets positions. With the resulting +calibrated `sunpy.map.Map` it is straightforward to overplot some space-based +coronagraph data on top of the eclipse image. + +Image credit: NASA/Artemis II crew + +""" +from pathlib import Path + +import exifread +import hvpy +import matplotlib +import numpy as np +import requests +from hvpy.datasource import DataSource +from matplotlib import pyplot as plt +from matplotlib.patches import Circle +from scipy.signal import medfilt2d +from skimage import transform +from skimage.color import rgb2gray +from skimage.feature import canny, peak_local_max +from skimage.transform import hough_circle, hough_circle_peaks + +import astropy.units as u +from astropy.coordinates import CartesianRepresentation, SkyCoord, solar_system_ephemeris +from astropy.time import Time +from astropy.wcs import WCS + +import sunpy.map +from sunpy.coordinates import Helioprojective, SphericalScreen, get_horizons_coord +from sunpy.map import Map +from sunpy.map.header_helper import make_fitswcs_header +from sunpy.util.config import get_and_create_download_dir + +# Accurate planetary ephemeris from JPL Horizons +solar_system_ephemeris.set('de440s') + +############################################################################### +# Get and Convert the Raw Image +# ============================= +# The starting point is a single JPEG hosted in the NASA image library. It +# has no WCS, no pointing solution, or plate scale, we only have the raw +# image data. +# +# We first download and read in the raw image data directly taken by the crew +# on Artemis-II and convert the RGB jpeg data to a grayscale image. + +url = "https://images-assets.nasa.gov/image/art002e009301/art002e009301~orig.jpg"; +filename = url.split("/")[-1] +with requests.get(url, stream=True) as res: + res.raise_for_status() + with open(filename, "wb") as f: + for chunk in res.iter_content(chunk_size=8192): + f.write(chunk) + +artemis_image_rbg = np.flipud(matplotlib.image.imread(filename)) +artemis_image = rgb2gray(artemis_image_rbg) + +############################################################################### +# Let's downsample the image to reasonable size for processing and +# visualization. The original frame is very large, so for this example we +# downsample by a factor of 6. This can be set to `False` if running locally +# for full resolution analysis. + +downsampled = True +if downsampled: + artemis_image = transform.rescale(artemis_image, 1/6, anti_aliasing=True) + +############################################################################### +# And now let's plot the raw image. + +fig, ax = plt.subplots() +ax.imshow(artemis_image_rbg, origin="lower") +ax.set_axis_off() +# Reduce memory usage on RTD build +del artemis_image_rbg + +############################################################################### +# Extract Metadata +# ================ +# +# Let's now extract metadata stored in the JPEG image, in particular the date +# and time the image was taken. The time stamp of the image is the key +# information we need, as from this we can query JPL horizons for the positions +# of Artemis II, the Sun, the Moon and the planets. + +with Path(filename).open("rb") as f: + tags = exifread.process_file(f) + +obsdate, obstime= tags['EXIF DateTimeDigitized'].values.split(" ") +obsdate = obsdate.replace(":", "-") +obstime = Time(f"{obsdate}T{obstime}") +print(obstime) + +hours, _ = [int(part) for part in tags['EXIF OffsetTime'].values.split(":")] +offset = hours*u.hour + +# obstime = obstime + offset # It seems like the timezone or offset is set incorrectly + +############################################################################### +# Get Coordinates +# =============== +# +# To get the coordinates of the Artemis II spacecraft, the Sun, the Moon, and +# the planets at the observation time, we query JPL Horizons. +# Here we use the NAIF IDs for the bodies for the query. + +NAIF_IDS = { + "artemis_ii": -1024, + "moon": 301, + "sun": 10, + "mercury": 199, + "venus": 299, + "earth": 399, + "mars": 499, + "jupiter": 599, + "saturn": 699, + "uranus": 799, + "neptune": 899 +} + +coords = {name: get_horizons_coord(str(id), obstime) for name, id in NAIF_IDS.items()} + +############################################################################### +# Find and Fit Moon's Limb and Center +# =================================== +# +# While we now know where the Moon is on the sky, we still need to know where +# it is in the image. Fitting the Moon's limb gives us that pixel location, and +# combined with the Moon's known angular size, we can estimate the plate scale. +# +# Here we use canny edge detection and circular Hough filtering to obtain the +# Moon's limb and center. +# +# First pass on a downscaled version is used to get an estimate, which is +# used to extract the region of interest (ROI) for full resolution pass. + +print("starting low res pass") +scale = 0.5 if downsampled else 0.1 +down_scaled = transform.rescale(artemis_image, scale, anti_aliasing=True) + + # Edge detection +edges = canny(down_scaled, sigma=2) + + # Radius range in scaled image (diameter ~1/3 of image height) +h, w = down_scaled.shape +radii = np.arange(0.25*h, 0.4*h, 10) + + # Hough +hough_res = hough_circle(edges, radii) +accums, cx, cy, rad = hough_circle_peaks(hough_res, radii, total_num_peaks=1) +del hough_res + + # Scale back to original resolution +moon_x = int(cx[0] / scale) +moon_y = int(cy[0] / scale) +moon_r = rad[0] / scale +roi_ext = int(1.05*moon_r) + +slice_y = slice(moon_y-roi_ext, moon_y+roi_ext) +slice_x = slice(moon_x-roi_ext, moon_x+roi_ext) +print(f"Low res pass moon_x: {moon_x}, moon_y: {moon_y}, moon_r: {moon_r}") + +############################################################################### +# Full resolution pass within ROI +# ------------------------------- +# +# Let's now re-run the limb fitting on the full resolution within the cropped +# ROI. + +roi = artemis_image[slice_y, slice_x] + +edges = canny(roi, sigma=2) + +hough_radii = np.linspace(edges.shape[0] / 2.5, edges.shape[0] / 2, 30) +hough_res = hough_circle(edges, hough_radii).astype(np.float32) # reduce peak memory usage + +accums, cx, cy, radii = hough_circle_peaks(hough_res, hough_radii, total_num_peaks=1) + +print(f"High res pass moon_x: {cx[0] + slice_x.start}, moon_y: {cy[0]+slice_y.start}, moon_r: {radii}") + +############################################################################### +# Plot edge detection and Hough filtering results +# ----------------------------------------------- + +fig, ax = plt.subplots(ncols=3, nrows=1, figsize=(9, 3)) +ax[0].imshow(artemis_image[slice_y, slice_x]) +ax[0].set_title("Original") +ax[1].imshow(edges) +ax[1].set_title("Canny") +circ = Circle( + np.hstack([cx, cy]), radius=radii[0], facecolor="none", edgecolor="red", + linewidth=2, linestyle="dashed", label="Hough fit") +ax[2].imshow(artemis_image[slice_y, slice_x]) +ax[2].add_patch(circ) +ax[2].set_title("Original with fit") +fig.legend() + + +############################################################################### +# Create metadata +# ================ +# +# Build up the metadata required to make a `sunpy.map.Map` +# Here we calculate the reference pixel, and plate scale. + +im_cx = (cx[0] + slice_x.start) * u.pix +im_cy = (cy[0] + slice_y.start) * u.pix +im_radius = radii[0] * u.pix + +moon = SkyCoord(coords['moon'], observer=coords['artemis_ii']) +R_moon = 0.2725076 * u.R_earth # IAU mean radius +dist_moon = SkyCoord(coords['artemis_ii']).separation_3d(moon) +moon_obs = np.arcsin(R_moon / dist_moon).to("arcsec") +print(moon_obs) + +plate_scale = moon_obs / im_radius +print(plate_scale) + +############################################################################### +# Make a Map +# ========== +# +# Make a `sunpy.map.Map` using the metadata obtained so far using +# `sunpy.map.header_helper.make_fitswcs_header`. + +frame = Helioprojective(observer=coords['artemis_ii'], obstime=obstime) +moon_hpc = coords['moon'].transform_to(frame) + +header = make_fitswcs_header( + artemis_image, + moon_hpc, + reference_pixel=u.Quantity([im_cx, im_cy]), + scale=u.Quantity([plate_scale, plate_scale]) +) + +artemis_map = Map(artemis_image, header) + +############################################################################### +# Reusable plot helper + +def plot_artemis_map(amap, moon_coord, planets, reset_lim=True, legend=True, figsize=(9,4), **kwargs): + fig, ax = plt.subplots(1, 1, subplot_kw={"projection": amap}, figsize=figsize, **kwargs) + amap.plot(axes=ax) + amap.draw_limb(axes=ax, label='Sun') + ax.coords[0].set_format_unit(u.deg) + ax.coords[1].set_format_unit(u.deg) + + ax.plot_coord(moon_coord, 'b+', label="Lunar Center") + theta = np.linspace(0, 360, 100) * u.deg + lunar_limb = np.vstack([moon_hpc.Tx + np.sin(theta) * moon_obs, moon_hpc.Ty + np.cos(theta) * moon_obs]) + with SphericalScreen(amap.observer_coordinate): + ax.plot_coord(SkyCoord(*lunar_limb, frame=amap.coordinate_frame), label="Lunar Limb") + + xlim = ax.get_xlim() + ylim = ax.get_ylim() + for name, coord in planets.items(): + ax.plot_coord(coord, 'o', markerfacecolor='none', label=name.title()) + if reset_lim: + ax.set_xlim(xlim) + ax.set_ylim(ylim) + if legend: + ax.legend(bbox_to_anchor=(1.05, 1), loc='upper left', borderaxespad=0) + return fig, ax + +############################################################################### +# Plot map and positions of planets to see what should be visible + +planets = {name: coord for name, coord in coords.items() if name not in ["sun", "moon", "artemis_ii"]} + +fig, ax = plot_artemis_map(artemis_map, moon_hpc, planets, reset_lim=False) +fig.tight_layout() + +############################################################################### +# Mercury, Mars, Saturn and Neptune are within the field of view, though +# Neptune is not visible as it is too distant and faint. + +planets = {name: coords[name] for name in ["mercury", "mars", "saturn"]} + +fig, ax = plot_artemis_map(artemis_map, moon_hpc, planets, reset_lim=False) +fig.tight_layout() + +############################################################################### +# Find roll angle +# =============== +# +# A clear roll is visible, so the positions of the planets are used to +# estimate the camera orientation. Use `skimage.feature.peak_local_max` to +# find the brightest peaks, which should correspond to the planets. + +if downsampled: + planets_pixels = peak_local_max(artemis_image, threshold_abs=0.9, num_peaks=3, min_distance=30) +else: + artemis_median_img = medfilt2d(artemis_image, kernel_size=5) + planets_pixels = peak_local_max(artemis_median_img, threshold_abs=0.9, num_peaks=3, min_distance=30) + del artemis_median_img + +planets_pix_x = planets_pixels[:,1] +planets_pix_y = planets_pixels[:,0] + +planet_coords = artemis_map.pixel_to_world(planets_pix_x * u.pix, planets_pix_y * u.pix) + +############################################################################### +# Verify we've correctly identified the planets. + +fig, ax = plot_artemis_map(artemis_map, moon_hpc, planets) +with SphericalScreen(coords["artemis_ii"]): + ax.plot_coord(planet_coords, 's', markerfacecolor='none') + +############################################################################### +# We need to determine which pixel positions correspond to which planets. +# From the map above, we can see that, in terms of distance from the Moon, +# the planets are Saturn, Mars, and Mercury, in that order. Therefore, we +# sort them by the separation angle from the Moon's center. + +# Saturn, Mars, Mercury +with SphericalScreen(coords["artemis_ii"]): + sep = moon_hpc.transform_to(planet_coords.frame).separation(planet_coords) +planet_index = np.argsort(sep) +actual_planets_pixel = CartesianRepresentation(planets_pix_x[planet_index], planets_pix_y[planet_index], [0] * 3) * u.pix + +moon_pixel = CartesianRepresentation(*artemis_map.wcs.world_to_pixel(moon_hpc), 0)*u.pix + +# to match the order of the actual_planets_pixel +planets_temp = SkyCoord([planets[name] for name in ["saturn", "mars", "mercury"]]) +planets_pixel = CartesianRepresentation(*artemis_map.wcs.world_to_pixel(planets_temp), 0) * u.pix + +vec_expected = planets_pixel - moon_pixel +vec_actual = actual_planets_pixel - moon_pixel +roll_angles = -np.arccos(vec_expected.dot(vec_actual) / (vec_expected.norm() * vec_actual.norm())) + +weights = sep[planet_index].to(u.deg).value +roll_angles_weighted = np.average(roll_angles, weights=weights) +print(roll_angles.to('deg')) +print(roll_angles.mean().to('deg')) +print(f"Weighted roll: {np.degrees(roll_angles_weighted):.4f} deg") + +############################################################################### +# Use derived roll and make new header and map + +header_roll = make_fitswcs_header( + artemis_image, + moon_hpc, + reference_pixel=u.Quantity([im_cx, im_cy]), + scale=u.Quantity([plate_scale, plate_scale]), + rotation_angle=-roll_angles_weighted.to('deg') +) + +artemis_map_roll = Map(artemis_image, header_roll) + +############################################################################### +# Let's now plot map and positions of Saturn, Mars, and Mercury to check if +# the WCS is correct. +# +# There seems to be some residual distortion that gets worse towards the edges. + +fig, ax = plot_artemis_map(artemis_map_roll, moon_hpc, planets) + +############################################################################### +# Correct Optical Distortion +# ========================== +# +# We can see that there is some optical distortion. Let's assume the distortion +# is due to the lens (e.g., barrel or pincushion), centered in the middle of +# the image, and derive the correction from the observed versus actual planet +# positions. + +cx, cy = artemis_map_roll.wcs.wcs.crpix +r_actual, r_predicted = [], [] +for i, name in enumerate(["saturn", "mars", "mercury"]): + hpc = planets[name].transform_to(artemis_map_roll.coordinate_frame) + px, py = artemis_map_roll.wcs.world_to_pixel(hpc) + ax, ay = planets_pix_x[planet_index][i], planets_pix_y[planet_index][i] + r_predicted.append(np.sqrt((px - cx)**2 + (py - cy)**2)) + r_actual.append(np.sqrt((ax - cx)**2 + (ay - cy)**2)) + +r_predicted = np.array(r_predicted) +r_actual = np.array(r_actual) + +k1_estimates = (r_actual/r_predicted - 1) / r_predicted**2 +weights = r_predicted # weight by distance — Mercury most reliable +k1 = np.average(k1_estimates, weights=weights) +print(f"k1 per planet: {k1_estimates}") +print(f"Weighted k1: {k1:.6e} pix^-2") + +# Use only Mars and Mercury — Saturn too close to center and fit error +k1_estimates_reliable = k1_estimates[1:] +r_reliable = r_predicted[1:] +k1 = np.average(k1_estimates_reliable, weights=r_reliable) +print(f"k1 (Mars+Mercury only): {k1:.6e} pix^-2") + +############################################################################### +# Create a SIP header, WCS and verify the SIP improve positions + +header_sip = artemis_map_roll.fits_header.copy() +header_sip['CTYPE1'] = 'HPLN-TAN-SIP' +header_sip['CTYPE2'] = 'HPLT-TAN-SIP' +header_sip['A_ORDER'] = 3 +header_sip['B_ORDER'] = 3 +header_sip['A_3_0'] = -k1 +header_sip['A_1_2'] = -k1 +header_sip['B_0_3'] = -k1 +header_sip['B_2_1'] = -k1 +header_sip['A_DMAX'] = 1.0 +header_sip['B_DMAX'] = 1.0 +wcs_sip = WCS(header_sip) + +for i, name in enumerate(["saturn", "mars", "mercury"]): + hpc = planets[name].transform_to(artemis_map_roll.coordinate_frame) + px_nosip = wcs_sip.wcs_world2pix([[hpc.Tx.to(u.deg).value, hpc.Ty.to(u.deg).value]], 0)[0] + px_sip = wcs_sip.all_world2pix([[hpc.Tx.to(u.deg).value, hpc.Ty.to(u.deg).value]], 0)[0] + ax, ay = planets_pix_x[planet_index][i], planets_pix_y[planet_index][i] + print(f"{name}: residual without SIP=({ax-px_nosip[0]:.1f}, {ay-px_nosip[1]:.1f}) " + f"with SIP=({ax-px_sip[0]:.1f}, {ay-px_sip[1]:.1f})") + +############################################################################### +# Final Map +# ========= +# +# Create a final version of the map with the SIP headers. + +artemis_map_final = Map((artemis_image, header_sip)) +fig, ax = plot_artemis_map(artemis_map_final, moon_hpc, planets) +ax.set_title(f"Artemis-II Solar Eclipse {obstime}") +fig.tight_layout() + +############################################################################### +# Overplotting Coronagraph Images +# =============================== +# In this section we will fetch images of the near corona from SOHO/LASCO +# and overplot them on the eclipse map. +# The Artemis II image shows the faint outer corona around the Moon, as the +# spacecraft was close to the moon during the flyby, so the apparent angular +# size is much larger than the Sun's, so it blocks not only the Sun's disk but +# a substantial region of the inner corona around it. +# +# By reprojecting and overplotting the LASCO images, we can overlap them inside +# the Moon's image, to produce a composite that extends from the inner corona +# outwards. +# +# First step is to fetch the images from Helioviewer. + +lasco_c2_file = hvpy.save_file(hvpy.getJP2Image(obstime.datetime, + DataSource.LASCO_C2.value), + filename=get_and_create_download_dir() + "/LASCO_C2.jp2", overwrite=True) +lasco_c2_map = Map(lasco_c2_file) +lasco_c3_file = hvpy.save_file(hvpy.getJP2Image(obstime.datetime, + DataSource.LASCO_C3.value), + filename=get_and_create_download_dir() + "/LASCO_C3.jp2", overwrite=True) +lasco_c3_map = Map(lasco_c3_file) + +############################################################################### +# Next we reproject the LASCO map to the same WCS as the Artemis eclipse map. + +with SphericalScreen(coords["artemis_ii"]): + c3_map_img = lasco_c3_map.reproject_to(artemis_map_final.wcs) + c2_map_img = lasco_c2_map.reproject_to(artemis_map_final.wcs) + + +############################################################################### +# As the final step we will crop the LASCO C3 image to the limb of the Moon +# and mask regions with no data. + +# Calculate coordinates for each pixel in the map. +all_hpc = sunpy.map.all_coordinates_from_map(c3_map_img) + +# Calculate the angular offset from the center of the moon for each pixel. +moon_cen_offsets = all_hpc.separation(coords['moon']) + +# Create a mask which is True for all offsets greater than the +# observed angular width of the moon. +c3_map_img.mask = np.logical_or( + moon_cen_offsets >= moon_obs, + # Also mask out the parts of the image with no data + c3_map_img.data < 10, +) +# Mask out the parts of the C2 image with no data +c2_map_img.mask = c2_map_img.data < 10 + +############################################################################### +# Now setup a new plot with the same distortion corrected eclipse image and +# reprojected, masked LASCO data. + +fig, ax = plot_artemis_map(artemis_map_final, moon_hpc, planets) + +# Overplot both LASCO images, with autoalign off as we already reprojected them. +c3_map_img.plot(axes=ax, autoalign=False) +c2_map_img.plot(axes=ax, autoalign=False) + +ax.set_title(f"Artemis-II Solar Eclipse {obstime}") +fig.tight_layout() + +# sphinx_gallery_thumbnail_number = -2 diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/examples/showcase/artemis-ii-trajectory.py new/sunpy-7.1.2/examples/showcase/artemis-ii-trajectory.py --- old/sunpy-7.1.1/examples/showcase/artemis-ii-trajectory.py 1970-01-01 01:00:00.000000000 +0100 +++ new/sunpy-7.1.2/examples/showcase/artemis-ii-trajectory.py 2026-04-19 23:08:51.000000000 +0200 @@ -0,0 +1,161 @@ +""" +===================== +Artemis II trajectory +===================== + +This example visualizes the trajectory of the Artemis II spacecraft. + +Artemis II was NASA's first crewed mission to the Moon since Apollo 17 in 1972, +flying four astronauts around the Moon on a ~10 day test flight in April 2026. +The trajectory is visualized in two different coordinate frames. The plots +also highlight the segment of the trajectory when Artemis II was in eclipse. +""" +import matplotlib.pyplot as plt +import numpy as np +from matplotlib.dates import DateFormatter + +import astropy.units as u +from astropy.constants import R_earth +from astropy.coordinates import solar_system_ephemeris +from astropy.time import Time + +from sunpy.coordinates import get_horizons_coord, sun +from sunpy.time import parse_time + +############################################################################## +# First, define times spanning the Artemis II mission, with higher resolution +# across eclipse transitions (i.e., the four contacts). The contact times are +# approximate. + +t_start = parse_time("2026-Apr-02 01:58:33") +t_c1 = parse_time("2026-Apr-07 00:32:46") # start of partial eclipse +t_c2 = parse_time("2026-Apr-07 00:34:28") # start of total eclipse +t_c3 = parse_time("2026-Apr-07 01:28:55") # end of total eclipse +t_c4 = parse_time("2026-Apr-07 01:31:03") # end of partial eclipse +t_end = parse_time("2026-Apr-10 23:54:22") + +time_spans = [(t_start, t_c1 - 10*u.s, 5*u.min), + (t_c1 - 30*u.s, t_c2 + 30*u.s, 5*u.s), + (t_c2 + 30*u.s, t_c3 - 30*u.s, 5*u.min), + (t_c3 - 30*u.s, t_c4 + 30*u.s, 5*u.s), + (t_c4 + 30*u.s, t_end, 5*u.min)] +times = Time(np.concatenate([np.arange(t1.jd, t2.jd, dt.to_value(u.day)) + for t1, t2, dt in time_spans]), format='jd') + +############################################################################## +# Use JPL Horizons via :func:`~sunpy.coordinates.get_horizons_coord` to +# retrieve relevant coordinates, and then use the coordinate framework to +# convert to ecliptic coordinates. There is no convenient coordinate frame +# for the Earth-Moon system, so convert to a heliocentric frame for now. + +# Use a JPL ephemeris because astropy's built-in ephemeris is not accurate enough +solar_system_ephemeris.set('de440s') + +# Get the Artemis II coordinate in Heliocentric Mean Ecliptic +artemis = get_horizons_coord("Artemis II", times).heliocentricmeanecliptic + +# Get other relevant coordinates +# Specify NAIF IDs for Earth and Moon due to multiple matches for string input +earth = get_horizons_coord(399, times).heliocentricmeanecliptic +moon = get_horizons_coord(301, times).heliocentricmeanecliptic +em_barycenter = get_horizons_coord("Earth-Moon Barycenter", times).heliocentricmeanecliptic + +############################################################################## +# Determine when Artemis II was in eclipse using :func:`sunpy.coordinates.sun.eclipse_amount`. +# When the eclipse percentage is greater than 0, at least part of the Sun is +# eclipsed by the Moon. Be aware that this function assumes a uniform lunar +# radius, but features of the lunar terrain may be comparable to the apparent +# size of the Sun as seen from Artemis II, so the calculation is only an +# approximation. + +eclipse_percentage = sun.eclipse_amount(artemis) +eclipsed = np.flatnonzero(eclipse_percentage > 0) # at least partially eclipsed + +############################################################################## +# Plot the eclipse percentage when transitioning in an out of eclipse. + +fig, axs = plt.subplots(1, 2, layout="constrained") + +axs[0].plot(times.datetime64, eclipse_percentage, '.-') +axs[0].set_xlim((t_c1 - 1*u.min).datetime64, (t_c2 + 1*u.min).datetime64) +axs[0].set_title("Entering eclipse") + +axs[1].plot(times.datetime64, eclipse_percentage, '.-') +axs[1].set_xlim((t_c3 - 1*u.min).datetime64, (t_c4 + 1*u.min).datetime64) +axs[1].set_title("Exiting eclipse") + +for ax in axs: + ax.grid() + ax.xaxis.set_major_formatter(DateFormatter('%m-%d %H:%M')) + ax.tick_params('x', rotation=90) + ax.set_ylabel("Eclipse percentage") + +############################################################################## +# Shift the coordinates to have the Earth-Moon barycenter as the origin, +# convert to units of Earth radii, and keep only the X and Y components for +# later plotting. + +artemis_x, artemis_y, _ = ((artemis.cartesian - em_barycenter.cartesian).xyz / R_earth).decompose() +earth_x, earth_y, _ = ((earth.cartesian - em_barycenter.cartesian).xyz / R_earth).decompose() +moon_x, moon_y, _ = ((moon.cartesian - em_barycenter.cartesian).xyz / R_earth).decompose() + +############################################################################## +# Plot the Artemis II trajectory in fixed ecliptic X-Y coordinates. The motion +# of the Earth relative to the Earth-Moon barycenter is not discernible on +# this plot. The segment of the trajectory when Artemis II was in eclipse is +# highlighted. + +fig, ax = plt.subplots() + +ax.plot(earth_x, earth_y, ls='dashed', color='b', label='Earth') +ax.plot(earth_x[-1], earth_y[-1], '.', color='b') + +ax.plot(moon_x, moon_y, ls='dashed', color='g', label='Moon') +ax.plot(moon_x[-1], moon_y[-1], '.', color='g') + +ax.plot(artemis_x, artemis_y, color='k', label='Artemis II') +ax.plot(artemis_x[-1], artemis_y[-1], '.', color='k') +ax.plot(artemis_x[eclipsed], artemis_y[eclipsed], color='m', lw=3, label='eclipse') + +ax.set_title('Fixed coordinate frame') +ax.set_xlabel('Ecliptic X (Earth radii)') +ax.set_ylabel('Ecliptic Y (Earth radii)') +ax.set_aspect('equal') +ax.legend(loc='center right') + +############################################################################## +# Transform the X and Y components so that the we are in the frame co-rotating +# with the Moon's orbital motion. + +angle = np.arctan2(moon_y, moon_x) +c, s = np.cos(-angle), np.sin(-angle) + +artemis_xp, artemis_yp = artemis_x * c - artemis_y * s, artemis_x * s + artemis_y * c +earth_xp, earth_yp = earth_x * c - earth_y * s, earth_x * s + earth_y * c +moon_xp, moon_yp = moon_x * c - moon_y * s, moon_x * s + moon_y * c + +############################################################################## +# Plot the Artemis II trajectory in coordinates co-rotating with the Moon's +# orbital motion. + +fig, ax = plt.subplots() + +ax.plot(earth_xp, earth_yp, ls='dashed', color='b', label='Earth') +ax.plot(earth_xp[-1], earth_yp[-1], '.', color='b') + +ax.plot(moon_xp, moon_yp, ls='dashed', color='g', label='Moon') +ax.plot(moon_xp[-1], moon_yp[-1], '.', color='g') + +ax.plot(artemis_xp, artemis_yp, color='k', label='Artemis II') +ax.plot(artemis_xp[-1], artemis_yp[-1], '.', color='k') +ax.plot(artemis_xp[eclipsed], artemis_yp[eclipsed], color='m', lw=3, label='eclipse') + +ax.set_title('Coordinate frame co-rotating with the Moon') +ax.set_xlabel('X (Earth radii)') +ax.set_ylabel('Y (Earth radii)') +ax.set_aspect('equal') +ax.legend(loc='center') + +plt.show() + +# sphinx_gallery_thumbnail_number = 3 diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/pyproject.toml new/sunpy-7.1.2/pyproject.toml --- old/sunpy-7.1.1/pyproject.toml 2026-03-26 10:58:57.000000000 +0100 +++ new/sunpy-7.1.2/pyproject.toml 2026-04-19 23:08:51.000000000 +0200 @@ -68,7 +68,7 @@ "reproject>=0.13.0", "scipy>=1.12.0", ] -opencv = ["opencv-python>=4.8.0.74"] +opencv = ["opencv-python>=4.8.0.74,!=4.13.0.*"] net = [ "beautifulsoup4>=4.13.1", "drms>=0.7.1", @@ -147,6 +147,7 @@ "astroquery>=0.4.6", "jplephem>=2.19", "pillow", + "exifread", ] dev = ["sunpy[docs,tests]"] diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/sunpy/_version.py new/sunpy-7.1.2/sunpy/_version.py --- old/sunpy-7.1.1/sunpy/_version.py 2026-03-26 10:59:06.000000000 +0100 +++ new/sunpy-7.1.2/sunpy/_version.py 2026-04-19 23:09:01.000000000 +0200 @@ -18,7 +18,7 @@ commit_id: str | None __commit_id__: str | None -__version__ = version = '7.1.1' -__version_tuple__ = version_tuple = (7, 1, 1) +__version__ = version = '7.1.2' +__version_tuple__ = version_tuple = (7, 1, 2) -__commit_id__ = commit_id = 'g5984e5d5b' +__commit_id__ = commit_id = 'gd6d084921' diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/sunpy/map/mapbase.py new/sunpy-7.1.2/sunpy/map/mapbase.py --- old/sunpy-7.1.1/sunpy/map/mapbase.py 2026-03-26 10:58:57.000000000 +0100 +++ new/sunpy-7.1.2/sunpy/map/mapbase.py 2026-04-19 23:08:51.000000000 +0200 @@ -674,6 +674,11 @@ # Set the shape of the data array w2.array_shape = self.data.shape + # Unlike Astropy we only use SIP distortions if it is in the CTYPE. + if any(t.endswith("-SIP") for t in self.coordinate_system): + sip_wcs = astropy.wcs.WCS(header=self.meta) + w2.sip = sip_wcs.sip + # Validate the WCS here. w2.wcs.set() return w2 diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/sunpy/map/sources/tests/test_hmi_source.py new/sunpy-7.1.2/sunpy/map/sources/tests/test_hmi_source.py --- old/sunpy-7.1.1/sunpy/map/sources/tests/test_hmi_source.py 2026-03-26 10:58:57.000000000 +0100 +++ new/sunpy-7.1.2/sunpy/map/sources/tests/test_hmi_source.py 2026-04-19 23:08:51.000000000 +0200 @@ -112,11 +112,15 @@ # We use our sample HMI image to test memory mapping because it is large (8 MB data array) @pytest.mark.remote_data def test_memmap(): + from sunpy.data.sample import HMI_LOS_IMAGE + + # Burn in base memory usage associated with Map instantiation + _ = Map(HMI_LOS_IMAGE) + process = psutil.Process() initial = process.memory_info() - from sunpy.data.sample import HMI_LOS_IMAGE hmi_map = Map(HMI_LOS_IMAGE) instantiated = process.memory_info() diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/sunpy/map/tests/test_mapbase.py new/sunpy-7.1.2/sunpy/map/tests/test_mapbase.py --- old/sunpy-7.1.1/sunpy/map/tests/test_mapbase.py 2026-03-26 10:58:57.000000000 +0100 +++ new/sunpy-7.1.2/sunpy/map/tests/test_mapbase.py 2026-04-19 23:08:51.000000000 +0200 @@ -107,6 +107,41 @@ assert pv_values[6] == (2, 10, 0.1) +def test_wcs_sip(aia171_test_map): + wcs1 = aia171_test_map.wcs + header_sip = wcs1.to_header() + k1 = -7e-12 + + header_sip["CTYPE1"] = header_sip["CTYPE1"] + "-SIP" + header_sip["CTYPE2"] = header_sip["CTYPE2"] + "-SIP" + header_sip['A_ORDER'] = 3 + header_sip['B_ORDER'] = 3 + header_sip['A_3_0'] = -k1 + header_sip['A_1_2'] = -k1 + header_sip['B_0_3'] = -k1 + header_sip['B_2_1'] = -k1 + header_sip['A_DMAX'] = 1.0 + header_sip['B_DMAX'] = 1.0 + + sip_map = sunpy.map.Map(aia171_test_map.data, header_sip) + + sip_wcs = sip_map.wcs + assert sip_wcs.sip is not None + + # The SIP distortion shouldn't affect the ref pixel + ref1 = aia171_test_map.wcs.pixel_to_world(*aia171_test_map.reference_pixel) + ref2 = sip_map.wcs.pixel_to_world(*aia171_test_map.reference_pixel) + + assert u.allclose(ref1.Tx, ref2.Tx) + assert u.allclose(ref1.Ty, ref2.Ty) + + # Pixels away from the ref should be distorted + edge1 = aia171_test_map.wcs.pixel_to_world(1020, 1020) + edge2 = sip_map.wcs.pixel_to_world(1020, 1020) + + assert not u.allclose(edge1.Tx, edge2.Tx) + assert not u.allclose(edge1.Ty, edge2.Ty) + def test_wcs_cache(aia171_test_map): wcs1 = aia171_test_map.wcs wcs2 = aia171_test_map.wcs diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/sunpy/tests/figure_hashes_mpl_382_astropy_702_animators_121.json new/sunpy-7.1.2/sunpy/tests/figure_hashes_mpl_382_astropy_702_animators_121.json --- old/sunpy-7.1.1/sunpy/tests/figure_hashes_mpl_382_astropy_702_animators_121.json 1970-01-01 01:00:00.000000000 +0100 +++ 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"sunpy.visualization.tests.test_drawing.test_draw_prime_meridian_aia171": "8c3600762afc1dbf5cf05e79651bd715767ebaeb615c1b788390df6f9bb27bde", - "sunpy.visualization.tests.test_drawing.test_heliographic_equator_prime_meridian": "3cb195a44e899ef46de7365bd0a0c580b7ea69662bdc560a1bbb1686c2ad48cf", - "sunpy.visualization.tests.test_visualization.test_show_hpr_impact_angle": "b6cdb96de7411476a395f41c30877ff48db6f17a2f72a3d05b5d8406144072f3" -} diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/sunpy/tests/helpers.py new/sunpy-7.1.2/sunpy/tests/helpers.py --- old/sunpy-7.1.1/sunpy/tests/helpers.py 2026-03-26 10:58:57.000000000 +0100 +++ new/sunpy-7.1.2/sunpy/tests/helpers.py 2026-04-19 23:08:51.000000000 +0200 @@ -90,10 +90,9 @@ import mpl_animators animators_version = "dev" if (("dev" in mpl_animators.__version__) or ("rc" in mpl_animators.__version__)) else mpl_animators.__version__.replace('.', '') - ft2_version = f"{mpl.ft2font.__freetype_version__.replace('.', '')}" mpl_version = "dev" if (("dev" in mpl.__version__) or ("rc" in mpl.__version__)) else mpl.__version__.replace('.', '') astropy_version = "dev" if (("dev" in astropy.__version__) or ("rc" in astropy.__version__)) else astropy.__version__.replace('.', '') - return f"figure_hashes_mpl_{mpl_version}_ft_{ft2_version}_astropy_{astropy_version}_animators_{animators_version}.json" + return f"figure_hashes_mpl_{mpl_version}_astropy_{astropy_version}_animators_{animators_version}.json" def figure_test(test_function): diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/sunpy.egg-info/PKG-INFO new/sunpy-7.1.2/sunpy.egg-info/PKG-INFO --- old/sunpy-7.1.1/sunpy.egg-info/PKG-INFO 2026-03-26 10:59:06.000000000 +0100 +++ new/sunpy-7.1.2/sunpy.egg-info/PKG-INFO 2026-04-19 23:09:01.000000000 +0200 @@ -1,6 +1,6 @@ Metadata-Version: 2.4 Name: sunpy -Version: 7.1.1 +Version: 7.1.2 Summary: SunPy core package: Python for Solar Physics Author-email: The SunPy Community <[email protected]> License-Expression: BSD-3-Clause @@ -56,7 +56,7 @@ Requires-Dist: reproject>=0.13.0; extra == "map" Requires-Dist: scipy>=1.12.0; extra == "map" Provides-Extra: opencv -Requires-Dist: opencv-python>=4.8.0.74; extra == "opencv" +Requires-Dist: opencv-python!=4.13.0.*,>=4.8.0.74; extra == "opencv" Provides-Extra: net Requires-Dist: beautifulsoup4>=4.13.1; extra == "net" Requires-Dist: drms>=0.7.1; extra == "net" @@ -120,12 +120,15 @@ Requires-Dist: astroquery>=0.4.6; extra == "docs-gallery" Requires-Dist: jplephem>=2.19; extra == "docs-gallery" Requires-Dist: pillow; extra == "docs-gallery" +Requires-Dist: exifread; extra == "docs-gallery" Provides-Extra: dev Requires-Dist: sunpy[docs,tests]; extra == "dev" Dynamic: license-file +``sunpy`` +========= + SunPy core package: Python for Solar Physics -============================================ |SunPy Logo| diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/sunpy.egg-info/SOURCES.txt new/sunpy-7.1.2/sunpy.egg-info/SOURCES.txt --- old/sunpy-7.1.1/sunpy.egg-info/SOURCES.txt 2026-03-26 10:59:06.000000000 +0100 +++ new/sunpy-7.1.2/sunpy.egg-info/SOURCES.txt 2026-04-19 23:09:02.000000000 +0200 @@ -212,6 +212,8 @@ examples/saving_and_loading_data/genericmap_in_fits.py examples/saving_and_loading_data/load_adapt_fits_into_map.py examples/showcase/README.txt +examples/showcase/artemis-ii-eclipse.py +examples/showcase/artemis-ii-trajectory.py examples/showcase/eclipse_amount.py examples/showcase/hmi_cutout.py examples/showcase/los_simulation_box_intersection.py @@ -701,8 +703,8 @@ sunpy/sun/tests/test_constants.py sunpy/sun/tests/test_models.py sunpy/tests/__init__.py -sunpy/tests/figure_hashes_mpl_382_ft_261_astropy_702_animators_121.json -sunpy/tests/figure_hashes_mpl_dev_ft_261_astropy_dev_animators_dev.json +sunpy/tests/figure_hashes_mpl_382_astropy_702_animators_121.json +sunpy/tests/figure_hashes_mpl_dev_astropy_dev_animators_dev.json sunpy/tests/helpers.py sunpy/tests/mocks.py sunpy/tests/self_test.py diff -urN '--exclude=CVS' '--exclude=.cvsignore' '--exclude=.svn' '--exclude=.svnignore' old/sunpy-7.1.1/sunpy.egg-info/requires.txt new/sunpy-7.1.2/sunpy.egg-info/requires.txt --- old/sunpy-7.1.1/sunpy.egg-info/requires.txt 2026-03-26 10:59:06.000000000 +0100 +++ new/sunpy-7.1.2/sunpy.egg-info/requires.txt 2026-04-19 23:09:01.000000000 +0200 @@ -51,6 +51,7 @@ astroquery>=0.4.6 jplephem>=2.19 pillow +exifread [image] scipy>=1.12.0 @@ -78,7 +79,7 @@ zeep>=4.3.0 [opencv] -opencv-python>=4.8.0.74 +opencv-python!=4.13.0.*,>=4.8.0.74 [s3] fsspec[s3]>=2023.6.0
![https://images-assets.nasa.gov/image/art002e009301/art002e009301~orig.jpg"](https://images-assets.nasa.gov/image/art002e009301/art002e009301~orig.jpg"){kind=link}