New functions for v1.3 #113
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Codecov ReportAll modified and coverable lines are covered by tests ✅
Additional details and impacted files@@ Coverage Diff @@
## main #113 +/- ##
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+ Coverage 99.70% 99.73% +0.02%
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Files 8 8
Lines 3054 3387 +333
Branches 576 649 +73
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+ Hits 3045 3378 +333
Partials 9 9
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Changes for the upcoming v1.3 feature release, expected around 1 May 2025.
Fixed
Physical vs projected motion of sidereal sources. #115: Modified
place()andnovas_geom_posvel()to use the specified SSB-based radial velocity, rather than projected movement, for calculating observer based radial velocities for sidereal sources.transform_cat()corrections to parallax when changing epochs. #116:transform_cat()to update parallax to the recalculated value when precessing or changing epochs.Added
LSR vs SSB-based radial velocities for
cat_entry#114: Newnovas_lsr_to_ssb_vel()can be used to convert velocity vectors referenced to the LSR to Solar-System Barycentric velocities. And,novas_ssb_to_lsr_vel()to provide the inverse conversion.New
novas_hms_hours(const char *str)andnovas_dms_degrees(const char *str)convenience functions to make it easier to parse HMS or DMS based time/angle values, returning the result in units of hours or degrees, appropriately for use in SuperNOVAS.New
novas_frame_lst()convenience function to readily return the Local (apparent) Sidereal Time for a given Earth-based observing frame.New
novas_rises_above()andnovas_sets_below()functions to return the date/time a source rises above or sets below a specific elevation on a given date. (Useful for Earth-based observers only).New
novas_helio_dist()function to calculate the heliocentric distance of a Solar-system body on a given date. Thenovas_solar_power()function can be used to estimate the incident Solar power on a Solar-system body, whilenovas_solar_illum()can be used to calculate the fraction of a spherical body that is illuminated by the Sun seen from the observer location.New
novas_hpa()andnovas_epa()functions to calculate the parallactic angle (a.k.a. vertical position angle) for a given location on sky, using the local horizontal coordinates, or else the equatorial position, respectively. The parallactic angle (PA) can be useful to convert local Cartesian offsets (e.g. from a flat image or detector array) between the local horizontal and equatorial orientations, e.g. via the newly addednovas_h2e_offset()ornovas_e2h_offset()functions. The conversion between offsets and absolute coordinates usually requires a WCS projections, such as described in Calabretta & Greisen 2002.New
novas_sep(),novas_equ_sep(), andnovas_object_sep()functions can be used to calculate the precise apparent distance between two spherical or equatorial locations, or between two sources, respectively.novas_sun_angle()andnovas_moon_angle()can be used to calculate the apparent angular distance of sources from the Sun and Moon, respectively.New
novas_observableandnovas_trackdata structures to provide second order Taylor series expansion of the apparent horizontal or equatorial positions, distances and redshifts for sources. They can be calculated with the newly addednovas_track_hor()ornovas_track_equ()functions. Such tracking values, including rates and accelerations can be directly useful for controlling telescope drives in horizontal or equatorial mounts to track sources (hence the name). You can also obtain instantaneous projected (extrapolated) positions from the tracking parameters vianovas_track_project()at low computational cost.New
novas_los_to_xyz()andnovas_xyz_to_los()functions to convert between polar-oriented (δφ, δθ, δr) vectors along a line of sight, and rectangular equatorial (δx, δy, δz) vectors.New
novas_xyz_to_uvw()function to convert ITRS Earth locations (absolute or differential) to equatorial projections along a line of sight in the direction of a source. Such projections are oft used in interferometry.