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SuperNOVAS v1.2
The NOVAS C library, made better
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SuperNOVAS v1.2
The NOVAS C library, made better
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The NOVAS C astrometry library, made better.
SuperNOVAS is a C/C++ astronomy software library, providing high-precision astrometry such as one might need for running an observatory or a precise planetarium program. It is a fork of the Naval Observatory Vector Astrometry Software (NOVAS) C version 3.1, providing bug fixes, tons of extra features, while making it easier (and safer) to use also.
SuperNOVAS is entirely free to use without licensing restrictions. Its source code is compatible with the C99 standard, and hence should be suitable for old and new platforms alike. It is light-weight and easy to use, with full support for the IAU 2000/2006 standards for sub-microarcsecond position calculations.
This document has been updated for the v1.2 and later releases.
SuperNOVAS is a fork of the The Naval Observatory Vector Astrometry Software (NOVAS).
The primary goal of SuperNOVAS is to improve on the stock NOVAS C library via:
At the same time, SuperNOVAS aims to be fully backward compatible with the intended functionality of the upstream NOVAS C library, such that it can be used as a drop-in, build-time replacement for NOVAS in your application without having to change existing (functional) code you may have written for NOVAS C.
SuperNOVAS is currently based on NOVAS C version 3.1. We plan to rebase SuperNOVAS to the latest upstream release of the NOVAS C library, if new releases become available.
SuperNOVAS is maintained by Attila Kovacs at the Center for Astrophysics | Harvard & Smithsonian, and it is available through the Smithsonian/SuperNOVAS repository on GitHub.
Outside contributions are very welcome. See how you can contribute to make SuperNOVAS even better.
The SuperNOVAS library fixes a number of outstanding issues with NOVAS C 3.1. Here is a list of issues and fixes provided by SuperNOVAS over the upstream NOVAS C 3.1 code:
sidereal_time() function had an incorrect unit cast. This was a documented issue of NOVAS C 3.1.ephem_close() in eph_manager.c did not reset the EPHFILE pointer to NULL. This was a documented issue of NOVAS C 3.1.ephemeris(). When getting positions and velocities for Solar-system sources, it is important to use the values from the time light originated from the observed body rather than at the time that light arrives to the observer. This correction was done properly for positions, but not for velocities or distances, resulting in incorrect observed radial velocities or apparent distances being reported for spectroscopic observations or for angular-physical size conversions.ira_equinox() which may return the result for the wrong type of equinox (mean vs. true) if the equinox argument was changing from 1 to 0, and back to 1 again with the date being held the same. This affected routines downstream also, such as sidereal_time().cio_basis(), cio_location(), ecl2equ(), equ2ecl_vec(), ecl2equ_vec(), geo_posvel(), place(), and sidereal_time(). All these functions returned a cached value for the other accuracy if the other input parameters are the same as a prior call, except the accuracy.cio_basis() with alternating CIO location reference systems. This affected many CIRS-based position calculations downstream.equ2ecl_vec() and ecl2equ_vec() whereby a query with coord_sys = 2 (GCRS) has overwritten the cached mean obliquity value for coord_sys = 0 (mean equinox of date). As a result, a subsequent call with coord_sys = 0 and the same date as before would return the results in GCRS coordinates instead of the requested mean equinox of date coordinates.fmod() unchecked, which resulted in angles outside of the expected [0:2π] range and was also the reason why cal_date() did not work for negative JD values.aberration() returning NaN vectors if the ve argument is 0. It now returns the unmodified input vector appropriately instead.az output value in equ2hor() at zenith. While any azimuth is acceptable really, it results in unpredictable behavior. Hence, we set az to 0.0 for zenith to be consistent.d_light() if the first position argument is the ephemeris reference position (e.g. the Sun for solsys3.c). The bug affects for example grav_def(), where it effectively results in the gravitational deflection due to the Sun being skipped.rad_vel() has a number of issues that produce inaccurate results. The errors are typically at or below the tens of m/s level for objects not moving at relativistic speeds.SuperNOVAS strives to maintain API compatibility with the upstream NOVAS C 3.1 library, but not binary (ABI) compatibility.
If you have code that was written for NOVAS C 3.1, it should work with SuperNOVAS as is, without modifications. Simply (re)build your application against SuperNOVAS, and you are good to go.
The lack of binary compatibility just means that you cannot drop-in replace your compiled objects (e.g. novas.o, or the static libnovas.a, or the shared libnovas.so) libraries, from NOVAS C 3.1 with those from SuperNOVAS. Instead, you will have to build (compile) your application referencing the SuperNOVAS headers and/or libraries from the start.
This is because some function signatures have changed, e.g. to use an enum argument instead of the nondescript short int argument of NOVAS C 3.1, or because we added a return value to a function that was declared void in NOVAS C 3.1. We also changed the object structure to contain a long ID number instead of short to accommodate JPL NAIF codes, for which 16-bit storage is insufficient.
The SuperNOVAS distribution contains a GNU Makefile, which is suitable for compiling the library (as well as local documentation, and tests, etc.) on POSIX systems such as Linux, BSD, MacOS X, or Cygwin or WSL. (At this point we do not provide a similar native build setup for Windows, but speak up if you would like to add it yourself!)
Before compiling the library take a look a config.mk and edit it as necessary for your needs, or else define the necessary variables in the shell prior to invoking make. For example:
earth_sun_calc() set BUILTIN_SOLSYS3 = 1 and/or for planet_ephem_provider() set BUILTIN_SOLSYS_EPHEM = 1. You can then specify these functions (or others) as the default planet calculator for ephemeris() in your application dynamically via set_planet_provider().CALCEPH_SUPPORT = 1 in config.mk or in the shell prior to the build. When enabled it will build libsolsys-calceph.so[.1] and/or .a supplemental libraries, depending on the build target. The build of the modules requires an accessible installation of the CALCEPH development files (C headers and unversioned static or shared libraries depending on the needs of the build).CSPICE_SUPPORT = 1 in config.mk or in the shell prior to the build. When enabled it will build libsolsys-cspice.so[.1] and/or .a supplemental libraries, depending on the build target. The build of the modules requires an accessible installation of the CSPICE development files (C headers, under a cspice/ sub-folder in the header search path, and unversioned static or shared libraries depending on the needs of the build). You might want to check out the Smithsonian/cspice-sharedlib repository for building CSPICE as a shared library.solarsystem() implementation for ephemeris() calls by setting DEFAULT_SOLSYS to 1 – 3 for solsys1.c trough solsys3.c, respectively. If you want to link your own solarsystem() implementation(s) against the library, you should not set DEFAULT_SOLSYS (i.e. delete or comment out the corresponding line or else set DEFAULT_SOLSYS to 0).readeph() implementation, by setting DEFAULT_READEPH. (The default setting uses the dummy readeph0.c which simply returns an error). Note, that a readeph() implementation is a relic of NOVAS C and not always necessary. You can provide a superior ephemeris reader implementation at runtime via the set_ephem_provider() call or equivalent (e.g. novas_use_calceph() or novas_use_cspice(), if they are available).cio_location(), you can specify the path to the CIO locator file (e.g. /usr/local/share/supernovas/CIO_RA.TXT) on your system e.g. by setting the CIO_LOCATOR_FILE shell variable prior to calling make. (The CIO locator file is not necessary for the functioning of the library, unless you specifically require CIO positions relative to GCRS.)-DTHREAD_LOCAL=... added to CFLAGS. (Don't forget to enclose the string value in escaped quotes in config.mk, or unescaped if defining the THREAD_LOCAL shell variable prior to invoking make.)Now you are ready to build the library:
will compile the shared (e.g. lib/libsupernovas.so) libraries, produce a CIO locator data file (e.g. tools/data/cio_ra.bin), and compile the API documentation (into apidoc/) using doxygen (if available). Alternatively, you can build select components of the above with the make targets shared, and local-dox respectively. And, if unsure, you can always call make help to see what build targets are available.
After building the library you can install the above components to the desired locations on your system. For a system-wide install you may simply run:
Or, to install in some other locations, you may set a prefix and/or DESTDIR. For example, to install under /opt instead, you can:
Or, to stage the installation under a 'build root' first:
Provided you have installed the SuperNOVAS headers into a standard location, you can build your application against it very easily. For example, to build myastroapp.c against SuperNOVAS, you might have a Makefile with contents like:
If you have a legacy NOVAS C 3.1 application, it is possible that the compilation will give you errors due to missing includes for stdio.h, stdlib.h, ctype.h or string.h. This is because these were explicitly included in novas.h in NOVAS C 3.1, but not in SuperNOVAS (at least not by default), as a matter of best practice. If this is a problem for you can 'fix' it in one of two ways: (1) Add the missing #include directives to your application source explicitly, or if that's not an option for you, then (2) set the -DCOMPAT=1 compiler flag when compiling your application:
If your application uses optional planet or ephemeris calculator modules, you may need to specify the appropriate optional shared library also:
The NOVAS C way to handle planet or other ephemeris functions was to link particular modules to provide the solarsystem() / solarsystem_hp() and readeph() functions. This approach is discouraged in SuperNOVAS, since we now allow selecting different implementations at runtime, but the old way is supported for legacy applications, nevertheless.
To use your own existing default solarsystem() implementation in this way, you must build the library with DEFAULT_SOLSYS unset (or else set to 0) in config.mk (see section above), and your applications Makefile may contain something like:
The same principle applies to using your specific readeph() implementation (only with DEFAULT_READEPH being unset in config.mk).
Note, a better way to recycle your old planet and ephemeris calculator modules may be to rename solarsystem() / solarsystem_hp() functions therein to e.g. my_planet_calculator() / my_planet_calculator_hp() and then in your application can specify these functions as the provider at runtime:
For readeph() implementations, it is recommended that you change both the name and the footprint to e.g.:
and then then apply it in your application as:
While it requires some minimal changes to the old code, the advantage of this preferred approach is (a) that you do not need to re-build the library with the DEFAULT_SOLSYS and DEFAULT_READEPH options disabled, and (b) you can switch between different planet and ephemeris calculator functions at will, during runtime.
The IAU 2000 and 2006 resolutions have completely overhauled the system of astronomical coordinate transformations to enable higher precision astrometry. (Super)NOVAS supports coordinate calculations both in the old (pre IAU 2000) ways, and in the new IAU standard method. Here is an overview of how the old and new methods define some of the terms differently:
| Concept | Old standard | New IAU standard |
|---|---|---|
| Catalog coordinate system | FK4, FK5, HIP... | International Celestial Reference System (ICRS) |
| Dynamical system | True of Date (TOD) | Celestial Intermediate Reference System (CIRS) |
| Dynamical R.A. origin | equinox of date | Celestial Intermediate Origin (CIO) |
| Precession, nutation, bias | separate, no tidal terms | IAU 2006 precession/nutation model |
| Celestial Pole offsets | dψ, dε | dx, dy |
| Earth rotation measure | Greenwich Sidereal Time (GST) | Earth Rotation Angle (ERA) |
| Fixed Earth System | WGS84 | International Terrestrial Reference System (ITRS) |
See the various enums and constants defined in novas.h, as well as the descriptions on the various NOVAS routines on how they are appropriate for the old and new methodologies respectively.
In NOVAS, the barycentric BCRS and the geocentric GCRS systems are effectively synonymous to ICRS. The origin for positions and for velocities, in any reference system, is determined by the observer location in the vicinity of Earth (at the geocenter, on the surface, or in Earth orbit).
SuperNOVAS v1.1 has introduced a new, more intuitive, more elegant, and more efficient approach for calculating astrometric positions of celestial objects. The guide below is geared towards this new method. However, the original NOVAS C approach remains viable also (albeit often less efficient). You may find an equivalent example usage showcasing the original NOVAS method in LEGACY.md.
A sidereal source may be anything beyond the solar-system with 'fixed' catalog coordinates. It may be a star, or a galactic molecular cloud, or a distant quasar.
First, you must provide the coordinates (which may include proper motion and parallax). Let's assume we pick a star for which we have B1950 (i.e. FK4) coordinates:
We must convert these coordinates to the now standard ICRS system for calculations in SuperNOVAS, first by calculating equivalent J2000 coordinates, by applying the proper motion and the appropriate precession. Then, we apply a small adjustment to convert from J2000 to ICRS coordinates.
(Naturally, you can skip the transformation steps above if you have defined your source in ICRS coordinates from the start.) Once the catalog entry is defined in ICRS, you can proceed wrapping it in a generic source structure (which handles both catalog and ephemeris sources).
Next, we define the location where we observe from. Here we can (but don't have to) specify local weather parameters (temperature and pressure) also for refraction correction later (in this example, we'll skip the weather):
Similarly, you can also specify observers in Earth orbit, in Sun orbit, at the geocenter, or at the Solar-system barycenter.
Next, we set the time of observation. For a ground-based observer, you will need to provide SuperNOVAS with the UT1 - UTC time difference (a.k.a. DUT1), and the current leap seconds. Let's assume 37 leap seconds, and DUT1 = 0.114, then we can set the time of observation, for example, using the current UNIX time:
Alternatively, you may set the time as a Julian date in the time measure of choice (UTC, UT1, TT, TDB, GPS, TAI, TCG, or TCB):
or, for the best precision we may do the same with an integer / fractional split:
Next, we set up an observing frame, which is defined for a unique combination of the observer location and the time of observation:
Here dx and dy are small diurnal (sub-arcsec level) corrections to Earth orientation, which are published in the IERS Bulletins. They are needed when converting positions from the celestial CIRS frame to the Earth-fixed ITRS frame. You may ignore these and set zeroes if sub-arcsecond precision is not required.
The advantage of using the observing frame, is that it enables very fast position calculations for multiple objects in that frame. So, if you need to calculate positions for thousands of sources for the same observer and time, it will be significantly faster than using the low-level NOVAS C routines instead. You can create derivative frames for different observer locations, if need be, via novas_change_observer().
Note that without a proper ephemeris provider for the major planets, you are invariably restricted to working with NOVAS_REDUCED_ACCURACY frames, providing milliarcsecond precision only. To create NOVAS_FULL_ACCURACY frames, with sub-μas precision, you will you will need a high-precision ephemeris provider for the major planets (beyond the low-precision Earth and Sun calculator included by default), to account for gravitational bending around massive planets. Without it, μas accuracy cannot be ensured, in general. Therefore, attempting to construct high-accuracy frames without an appropriate high-precision ephemeris provider will result in an error from the requisite ephemeris() call.
Now we can calculate the apparent R.A. and declination for our source, which includes proper motion (for sidereal sources) or light-time correction (for Solar-system bodies), and also aberration corrections for the moving observer and gravitational deflection around the major Solar System bodies. You can calculate an apparent location in the coordinate system of choice (ICRS/GCRS, CIRS, J2000, MOD, or TOD):
Apart from providing precise apparent R.A. and declination coordinates, the sky_pos structure also provides the x,y,z unit vector pointing in the observed direction of the source (in the designated coordinate system). We also get radial velocity (for spectroscopy), and apparent distance for Solar-system bodies (e.g. for apparent-to-physical size conversion).
Note, that if you want geometric positions (and/or velocities) instead, without aberration and gravitational deflection, you might use novas_geom_posvel() instead. And regardless, which function you use you can always easily and efficiently change the coordinate system in which your results are expressed by creating an appropriate transform via novas_make_transform() and then using novas_transform_vector() or novas_transform_skypos().
If your ultimate goal is to calculate the azimuth and elevation angles of the source at the specified observing location, you can proceed from the sky_pos data you obtained above (in whichever coordinate system!) as:
Above we converted the apparent coordinates, assuming they were calculated in CIRS, to refracted azimuth and elevation coordinates at the observing location, using the novas_standard_refraction() function to provide a suitable refraction correction. We could have used novas_optical_refraction() instead to use the weather data embedded in the frame's observer structure, or some user-defined refraction model, or else NULL to calculate unrefracted elevation angles.
Solar-system sources work similarly to the above with a few important differences.
First, You will have to provide one or more functions to obtain the barycentric ICRS positions for your Solar-system source(s) of interest for the specific Barycentric Dynamical Time (TDB) of observation. See section on integrating External Solar-system ephemeris data or services with SuperNOVAS. You can specify the functions that will handle the respective ephemeris data at runtime before making the NOVAS calls that need them, e.g.:
Or, if you have the CALCEPH library installed on your system, and you have built SuperNOVAS with CALCEPH_SUPPORT = 1, then you might call:
Next, instead of make_cat_object() you define your source as an object with an name or ID number that is used by the ephemeris service you provided. For major planets you might want to use make_planet(), if they use a novas_planet_provider function to access ephemeris data with their NOVAS IDs, or else make_ephem_object() for more generic ephemeris handling via a user-provided novas_ephem_provider. E.g.:
As of version 1.2 you can also define solar system sources with orbital elements (such as the most up-to-date ones provided by the Minor Planet Center for asteroids, comets, etc.):
Note, that even with orbital elements, you will, in general, require a planet calculator, to provide precise positions for the Sun or planet, around which the orbit is defined.
Other than that, it's the same spiel as before, e.g.:
When one does not need positions at the microarcsecond level, some shortcuts can be made to the recipe above:
NOVAS_REDUCED_ACCURACY instead of NOVAS_FULL_ACCURACY for the calculations. This typically has an effect at the milliarcsecond level only, but may be much faster to calculate.If accuracy below the milliarcsecond level is not required NOVAS_REDUCED_ACCURACY mode offers faster calculations, in general.
Some of the calculations involved can be expensive from a computational perspective. For the most typical use case however, NOVAS (and SuperNOVAS) has a trick up its sleeve: it caches the last result of intensive calculations so they may be re-used if the call is made with the same environmental parameters again (such as JD time and accuracy).
A direct consequence of the caching of results in NOVAS is that calculations are generally not thread-safe as implemented by the original NOVAS C 3.1 library. One thread may be in the process of returning cached values for one set of input parameters while, at the same time, another thread is saving cached values for a different set of parameters. Thus, when running calculations in more than one thread, the results returned may at times be incorrect, or more precisely they may not correspond to the requested input parameters.
While you should never call NOVAS C from multiple threads simultaneously, SuperNOVAS caches the results in thread local variables (provided your compiler supports it), and is therefore safe to use in multi-threaded applications. Just make sure that you:
config.mk or in your equivalent build setup.The NOVAS API has been using conventional units (e.g. AU, km, day, deg, h) typically for its parameters and return values alike. Hence, SuperNOVAS follows the same conventions for its added functions and data structures also. However, when interfacing SuperNOVAS with other programs, libraries, or data files, it is often necessary to use quantities that are expressed in different units, such as SI or CGS. To facilitate such conversions, novas.h provides a set of unit constants, which can be used for converting to/from SI units (and radians). For example, novas.h contains the following definitions:
You can use these, for example, to convert quantities expressed in conventional units for NOVAS to standard (SI) values, by multiplying NOVAS quantities with the corresponding unit definition. E.g.:
And vice-versa: to convert values expressed in standard (SI) units, you can divide by the appropriate constant to 'cast' an SI value into the particular physical unit, e.g.:
Finally, you can combine them to convert between two different conventional units, e.g.:
Many of the (Super)NOVAS functions take an accuracy argument, which determines to what precision quantities are calculated. The argument can have one of two values, which correspond to typical precisions around:
enum novas_accuracy value | Typical precision |
|---|---|
NOVAS_REDUCED_ACCURACY | ~ 1 milli-arcsecond (mas) |
NOVAS_FULL_ACCURACY | below 1 micro-arcsecond (μas) |
Note, that some functions will not support full accuracy calculations, unless you have provided a high-precision ephemeris provider for the major planets (and any Solar-system bodies of interest), which does not come with SuperNOVAS out of the box. In the absense of a suitable high-precision ephemeris provider, some functions might return an error if called with NOVAS_FULL_ACCURACY.
The SuperNOVAS library is in principle capable of calculating positions to sub-microarcsecond, and velocities to mm/s, precision for all types of celestial sources. However, there are certain prerequisites and practical considerations before that level of accuracy is reached.
NOVAS_FULL_ACCURACY in the absense of a suitable high-precision planetary ephemeris provider.earth_sun_calc() in solsys3.c), but certainly not at the sub-microarcsecond level, and not for other solar-system sources. You will need to provide a way to interface SuperNOVAS with a suitable ephemeris source (such as the CSPICE toolkit from JPL or CALCEPH) if you want to use it to obtain precise positions for Solar-system bodies. See the section further below for more information how you can do that.cel_pole() and get_ut1_to_tt() functions to apply / use the published values from these to improve the astrometric precision of Earth-orientation based coordinate calculations. Without setting and using the actual polar offset values for the time of observation, positions for Earth-based observations will be accurate at the tenths of arcsecond level only.on_surface data structure that specifies the observer locations. Note, that refraction at radio wavelengths is notably different from the included optical model, and a standard radio refraction model is included as of version 1.1. In any case you may want to skip the refraction corrections offered in this library, and instead implement your own as appropriate (or not at all)._Thread_local or else the earlier GNU C >= 3.3 standard __thread modifier. You can also set the preferred thread-local keyword for your compiler by passing it via -DTHREAD_LOCAL=... in config.mk to ensure that your build is thread-safe. And, if your compiler has no support whatsoever for thread_local variables, then SuperNOVAS will not be thread-safe, just as NOVAS C isn't.novas_debug(NOVAS_DEBUG_ON) or novas_debug(NOVAS_DEBUG_EXTRA) to enable. When enabled, any error condition (such as NULL pointer arguments, or invalid input values etc.) will be reported to the standard error, complete with call tracing within the SuperNOVAS library, s.t. users can have a better idea of what exactly did not go to plan (and where). The debug messages can be disabled by passing NOVAS_DEBUF_OFF (0) as the argument to the same call. Here is an example error trace when your application calls grav_def() with NOVAS_FULL_ACCURACY while solsys3 provides Earth and Sun positions only and when debug mode is NOVAS_DEBUG_EXTRA (otherwise we'll ignore that we skipped the almost always negligible deflection due to planets): ephemeris() can be set at runtime via set_planet_provider(), and set_planet_provider_hp() (for high precision calculations). Similarly, if planet_ephem_provider() or planet_ephem_provider_hp() (defined in solsys-ephem.c) are set as the planet calculator functions, then set_ephem_provider() can set the user-specified function to use with these to actually read ephemeris data (e.g. from a JPL .bsp file).set_cio_locator_file() at runtime to specify the location of the binary CIO interpolation table (e.g. cio_ra.bin) to use, even if the library was compiled with the different default CIO locator path.nu2000k() can be replaced by another suitable IAU 2006 nutation approximation via set_nutation_lp_provider(). For example, the user may want to use the iau2000b() model or some custom algorithm instead.gcrs_to_cirs(), cirs_to_itrs(), and itrs_to_cirs(), cirs_to_gcrs().gcrs_to_j2000(), j2000_to_tod(), tod_to_itrs(), and itrs_to_tod(), tod_to_j2000(), j2000_to_gcrs().itrs_to_hor() and hor_to_itrs() to convert Earth-fixed ITRS coordinates to astrometric azimuth and elevation or back. Whereas tod_to_itrs() followed by itrs_to_hor() is effectively a just a more explicit 2-step version of the existing equ2hor() for converting from TOD to to local horizontal (old methodology), the cirs_to_itrs() followed by itrs_to_hor() does the same from CIRS (new IAU standard methodology), and had no prior equivalent in NOVAS C 3.1.ecl2equ() for converting ecliptic coordinates to equatorial, complementing existing equ2ecl().gal2equ() for converting galactic coordinates to ICRS equatorial, complementing existing equ2gal().refract_astro() complements the existing refract() but takes an unrefracted (astrometric) zenith angle as its argument.place() for simpler specific use: place_star(), place_icrs(), place_gcrs(), place_cirs(), and place_tod().radec_star() and radec_planet() as the common point for existing functions such as astro_star(), local_star(), virtual_planet(), topo_planet() etc.tt2tdb(), get_utc_to_tt(), and get_ut1_to_tt() make it simpler to convert between UTC, UT1, TT, and TDB time scales, and to supply ut1_to_tt arguments to place() or topocentric calculations.solarsystem() variants. It is possible to use the different solarsystem() implementations provided by solsys1.c, solsys2.c, solsys3.c and/or solsys-ephem.c side-by-side, as they define their functionalities with distinct, non-conflicting names, e.g. earth_sun_calc() vs planet_jplint() vs planet_eph_manager vs planet_ephem_provider(). See the section on Building and installation further above on including a selection of these in your library build.)novas_case_sensitive(int) to enable (or disable) case-sensitive processing of object names. (By default NOVAS object names are converted to upper-case, making them effectively case-insensitive.)make_planet() and make_ephem_object() to make it simpler to configure Solar-system objects.frames.c). A novas_frame object uniquely defines both the place and time of observation, with a set of pre-calculated transformations and constants. Once the frame is defined it can be used very efficiently to calculate positions for multiple celestial objects with minimum additional computational cost. The frames API is also more elegant and more versatile than the low-level NOVAS C approach for performing the same kind of calculations. And, frames are inherently thread-safe since post-creation their internal state is never modified during the calculations. The following new functions were added: novas_make_frame(), novas_change_observer(), novas_geom_posvel(), novas_geom_to_app(), novas_sky_pos(), novas_app_to_hor(), novas_app_to_geom(), novas_hor_to_app(), novas_make_transform(), novas_invert_transform(), novas_transform_vector(), and novas_transform_sky_pos().novas_timespec structure for the self-contained definition of precise astronomical time (timescale.c). You can set the time via novas_set_time() or novas_set_split_time() to a JD date in the timescale of choice (UTC, UT1, GPS, TAI, TT, TCG, TDB, or TCB), or to a UNIX time with novas_set_unix_time(). Once set, you can obtain an expression of that time in any timescale of choice via novas_get_time(), novas_get_split_time() or novas_get_unix_time(). And, you can create a new time specification by incrementing an existing one, using novas_increment_time(), or measure time differences via novas_diff_time(), novas_diff_tcg(), or novas_diff_tcb().novas_planet_bundle structure to handle planet positions and velocities more elegantly (e.g. for gravitational deflection calculations).obs_posvel() to calculate the observer position and velocity relative to the Solar System Barycenter (SSB).obs_planets() to calculate planet positions (relative to observer) and velocities (w.r.t. SSB).grav_undef() to undo gravitational bending of the observed light to obtain geometric positions from observed ones.grav_planets() and grav_undo_planets() functions to apply/ or undo gravitational deflection using a specific set of gravitating bodies.NOVAS_MOD (Mean of Date) which includes precession by not nutation and NOVAS_J2000 for the J2000 dynamical reference system.NOVAS_AIRBORNE_OBSERVER and NOVAS_SOLAR_SYSTEM_OBSERVER, and corresponding make_airborne_observer() and make_solar_system_observer() functions. Airborne observers have an Earth-fixed momentary location, defined by longitude, latitude, and altitude, the same way as for a stationary observer on Earth, but are moving relative to the surface, such as in an aircraft or balloon based observatory. Solar-system observers are similar to observers in Earth-orbit but their momentary position and velocity is defined relative to the Solar System Barycenter (SSB), instead of the geocenter.on_surface structure, e.g. for refraction calculations at radio wavelengths. The make_on_surface() function will set humidity to 0.0, but the user can set the field appropriately afterwards.novas_app_to_hor() / novas_hor_to_app() functions. The models novas_standard_refraction() and novas_optical_refraction() implement the same refraction model as refract() in NOVAS C 3.1, with NOVAS_STANDARD_ATMOSPHERE and NOVAS_WEATHER_AT_LOCATION respectively, including the reversed direction provided by refract_astro(). The user may supply their own custom refraction model also, and may make use of the generic reversal function novas_inv_refract() to calculate refraction in the reverse direction (observer vs astrometric elevations) as needed.novas_radio_refraction() based on the formulae by Berman & Rockwell 1976.cirs_to_tod() and tod_to_cirs() functions for efficient transformation between True of Date (TOD) and Celestial Intermediate Reference System (CIRS), and vice versa.make_cat_object() function to create a NOVAS celestial object structure from existing cat_entry data.novas_make_redshifted_object() to simplify the creation of distant catalog sources that are characterized with a redshift measure rather than a radial velocity value.novas_v2z(), novas_z2v(),grav_redshift(), redhift_vrad(), unredshift_vrad(), novas_z_add(), and novas_z_inv().novas_use_calceph() and/or novas_use_calceph_planets() to specify and use ephemeris data via CALCEPH for Solar-system sources in general, and for major planets specifically; and novas_calceph_use_ids() to specify whether object.number in NOVAS_EPHEM_OBJECT type objects is a NAIF ID (default) or else a CALCEPH ID number of the Solar-system body.novas_use_cspice(), novas_use_cspice_planets(), novas_use_cspice_ephem() to use the NAIF CSPICE library for all Solar-system sources, major planets only, or for other bodies only. NOVAS_EPHEM_OBJECTS should use NAIF IDs with CSPICE (or else -1 for name-based lookup). Also provides cspice_add_kernel() and cspice_remove_kernel().novas_to_naif_planet(), novas_to_dexxx_planet(), and naif_to_novas_planet().get_planet_provider() and get_planet_provider_hp().novas_planet_for_name() function to return the NOVAS planet ID for a given (case insensitive) name.object.type can now be set to NOVAS_ORBITAL_OBJECT, whose orbit can be defined by the set of novas_orbital, relative to a novas_orbital_system. You can initialize an object with a set of orbital elements using make_orbital_object(), and for planetary satellite orbits you might use novas_set_orbsys_pole(). For orbital objects, ephemeris() will call on the new novas_orbit_posvel() to calculate positions. While orbital elements do not always yield precise positions, they can for shorter periods, provided that the orbital elements are up-to-date. For example, the Minor Planer Center (MPC) publishes accurate orbital elements for all known asteroids and comets regularly. For newly discovered objects, this may be the only and/or most accurate information available anywhere.NOVAS_EMB (Earth-Moon Barycenter) and NOVAS_PLUTO_BARYCENTER to enum novas_planets to distinguish from the corresponding planet centers in calculations.gcrs_to_tod() / tod_to_gcrs() and gcrs_to_mod() / mod_to_gcrs() vector conversion functions for convenience.object initializer macros in novas.h for the major planets, Sun, Moon, and barycenters, e.g. NOVAS_EARTH_INIT or NOVAS_SSB_INIT. These wrap the parametric NOVAS_PLANET_INIT(num, name) macro, and can be used to simplify the initialization of NOVAS objects.novas.h.enums as their option arguments instead of raw integers. These enums are defined in novas.h. The same header also defines a number of useful constants. The enums allow for some compiler checking, and make for more readable code that is easier to debug. They also make it easy to see what choices are available for each function argument, without having to consult the documentation each and every time.errno set, usually to EINVAL) if the arguments supplied are invalid (unless the NOVAS C API already defined a different return value for specific cases. If so, the NOVAS C error code is returned for compatibility).errno so that users can track the source of the error in the standard C way and use functions such as perror() and strerror() to print human-readable error messages.const whenever the function does not modify the data content being pointed at. This supports better programming practices that generally aim to avoid unintended data modifications.NULL arguments, both for optional input values as well as outputs that are not required (see the API Documentation for specifics). This eliminates the need to declare dummy variables in your application code.NAN so that even if the caller forgets to check the error code, it becomes obvious that the values returned should not be used as if they were valid. (No more sneaky silent failures.)frame_tie(pos, J2000_TO_ICRS, pos) using the same pos vector both as the input and the output. In this case the pos vector is modified in place by the call. This can greatly simplify usage, and eliminate extraneous declarations, when intermediates are not required.struct layouts the same as NOVAS C thanks to alignment, thus allowing cross-compatible binary exchange of cat_entry records with NOVAS C 3.1.make_object() to retain the specified number argument (which can be different from the starnumber value in the supplied cat_entry structure).cio_location() will always return a valid value as long as neither output pointer argument is NULL. (NOVAS C 3.1 would return an error if a CIO locator file was previously opened but cannot provide the data for whatever reason).cel2ter() and ter2cel() can now process 'option'/'class' = 1 (NOVAS_REFERENCE_CLASS) regardless of the methodology (EROT_ERA or EROT_GST) used to input or output coordinates in GCRS.cio_array(), including I/O error checking.fund_args(), instead of the linear model in NOVAS C 3.1.era(), fund_args(), and planet_lon() by being more careful about the order in which terms are accumulated and combined, resulting in a small improvement on the few uas (micro-arcsecond) level.place() now returns an error 3 if and only if the observer is at (or very close, within ~1.5m) of the observed Solar-system object.grav_def() is simplified. It no longer uses the location type argument. Instead it will skip deflections due to a body if the observer is within ~1500 km of its center (which is below the surface for all major Solar system bodies).rad_vel() and place() will include gravitational corrections to radial velocity for light originating at the surface, and observed near Earth or at a large distance away.If you want to use SuperNOVAS to calculate positions for a range of Solar-system objects, and/or to do it with sufficient precision, you will have to interface it to a suitable provider of ephemeris data, such as JPL Horizons or the Minor Planet Center. Given the NOVAS C heritage, and some added SuperNOVAS flexibility in this area, you have several options on doing that. These are listed from the most practical (and preferred) to the least so (the old ways).
NASA/JPL provides generic ephemerides for the major planets, satellites thereof, the 300 largest asteroids, the Lagrange points, and some Earth orbiting stations. For example, DE440 covers the major planets, and the Sun, Moon, and barycenters for times between 1550 AD and 2650 AD. Or, you can use the JPL HORIZONS system to generate custom ephemeris data for pretty much all known solar systems bodies, down to the tiniest rocks.
The CALCEPH library provides an easy-to-use access to JPL and INPOP ephemeris files from C/C++. As of version 1.2, we provide optional support for interfacing SuperNOVAS with the the CALCEPH C library for handling Solar-system objects.
Prior to building SuperNOVAS simply set CALCEPH_SUPPORT to 1 in config.mk or in your environment. Depending on the build target, it will build libsolsys-calceph.so[.1] (target shared) or libsolsys-calceph.a (target static) libraries or solsys-calceph.o (target solsys), which provide the novas_use_calceph() and novas_use_calceph_planets(), and novas_calceph_use_ids() functions.
Of course, you will need access to the CALCEPH C development files (C headers and unversioned libcalceph.so or .a library) for the build to succeed. Here is an example on how you'd use CALCEPH with SuperNOVAS in your application code:
All modern JPL (SPK) ephemeris files should work with the solsys-calceph plugin. When linking your application, add -lsolsys-calceph to your link flags (or else link with solsys-calceph.o). That's all there is to it.
The NAIF CSPICE Toolkit is the canonical standard library for JPL ephemeris files from C/C++. As of version 1.2, we provide optional support for interfacing SuperNOVAS with CSPICE for handling Solar-system objects.
Prior to building SuperNOVAS simply set CSPICE_SUPPORT to 1 in config.mk or in your environment. Depending on the build target, it will build libsolsys-cspice.so[.1] (target shared) or libsolsys-cspice.a (target static) libraries or solsys-cspice.o (target solsys), which provide the novas_use_cspice(), novas_use_cspice_planets(), and novas_use_cspice_ephem() functions to enable CSPICE for providing data for all Solar-system sources, or for major planets only, or for other bodies only, respectively. You can also manage the active kernels with the cspice_add_kernel() and cspice_remove_kernel() functions.
Of course, you will need access to the CSPICE development files (C headers, installed under a cspice/ directory of an header search location, and the unversioned libcspice.so or .a library) for the build to succeed. You may want to check out the Smithsonian/cspice-sharedlib GitHub repository to help you build CSPICE with shared libraries and dynamically linked tools.
Here is an example on how you might use CSPICE with SuperNOVAS in your application code:
All JPL ephemeris data will work with the solsys-cspice plugin. When linking your application, add -lsolsys-cspice to your link flags (or else link with solsys-cspice.o). That's all there is to it.
Possibly the most universal way to integrate ephemeris data with SuperNOVAS is to write your own novas_ephem_provider, e.g.:
which takes an object ID number (such as a NAIF) an object name, and a split TDB date (for precision) as it inputs, and returns the type of origin with corresponding ICRS position and velocity vectors in the supplied pointer locations. The function can use either the ID number or the name to identify the object or file (whatever is the most appropriate for the implementation and for the supplied parameters). The positions and velocities may be returned either relative to the SSB or relative to the heliocenter, and accordingly, your function should set the value pointed at by origin to NOVAS_BARYCENTER or NOVAS_HELIOCENTER accordingly. Positions and velocities are rectangular ICRS x,y,z vectors in units of AU and AU/day respectively.
This way you can easily integrate current ephemeris data, e.g. for the Minor Planet Center (MPC), or whatever other ephemeris service you prefer.
Once you have your adapter function, you can set it as your ephemeris service via set_ephem_provider():
By default, your custom my_ephem_reader function will be used for 'minor planets' only (i.e. anything other than the major planets, the Sun, Moon, Solar-system Barycenter...). But, you can use the same function for the mentioned 'major planets' also via:
provided you compiled SuperNOVAS with BUILTIN_SOLSYS_EPHEM = 1 (in config.mk), or else you link your code against solsys-ephem.c explicitly. Easy-peasy.
If you only need support for major planets, you may be able to use one of the modules included in the SuperNOVAS distribution. The modules solsys1.c and solsys2.c provide built-in support to older JPL ephemerides (DE200 to DE421), either via the eph_manager interface of solsys1.c or via the FORTRAN pleph interface with solsys2.c.
To use the eph_manager interface for planet 1997 JPL planet ephemeris (DE200 through DE421), you must either build SuperNOVAS with BUILTIN_SOLSYS1 = 1 in config.mk, or else link your application with solsys1.c and eph_manager.c from SuperNOVAS explicitly. If you want eph_manager to be your default ephemeris provider (the old way) you might also want to set DEFAULT_SOLSYS = 1 in config.mk. Otherwise, your application should set eph_manager as your planetary ephemeris provider at runtime via:
Either way, before you can use the ephemeris, you must also open the relevant ephemeris data file with ephem_open():
And, when you are done using the ephemeris file, you should close it with
Note, that at any given time eph_manager can have only one ephemeris data file opened. You cannot use it to retrieve data from multiple ephemeris input files at the same time. (But you can with the CSPICE toolkit, which you can integrate as discussed further above!)
That's all, except the warning that this method will not work with newer JPL ephemeris data, beyond DE421.
To interface eith the JPL PLEPH library (FORTRAN) for planet ephemerides, you must either build SuperNOVAS with BUILTIN_SOLSYS2 = 1 in config.mk, or else link your application with solsys2.c and your appropriately modified jplint.f (from the examples sub-directory) explicitly, together with the JPL PLEPH library. If you want this to be your default ephemeris provider (the old way) you might also want to set DEFAULT_SOLSYS = 2 in config.mk. Otherwise, your application should set your planetary ephemeris provider at runtime via:
Integrating JPL ephemeris data this way can be arduous. You will need to compile and link FORTRAN with C (not the end of the world), but you may also have to modify jplint.f (providing the intermediate FORTRAN jplint_() / jplihp_() interfaces to pleph_()) to work with the version of pleph.f that you will be using. Unless you already have code that relies on this method, you are probably better off choosing one of the other ways for integrating planetary ephemeris data with SuperNOVAS.
Finally, if none of the above is appealing, and you are fond of the old ways, you may compile SuperNOVAS with the DEFAULT_SOLSYS option disabled (commented, removed, or else set to 0), and then link your own implementation of solarsystem() and solarsystem_hp() calls with your application.
For Solar-system objects other than the major planets, you may also provide your own readeph() implementation. (In this case you will want to set DEFAULT_READEPH in config.mk to specify your source code for that function before building the SuperNOVAS library, or else disable that option entirely (e.g. by commenting or removing it), and link your application explicitly with your readeph() implementation.
The downside of this approach is that your SuperNOVAS library will not be usable without invariably providing a solarsystem() / solarsystem_hp() and/or readeph() implementations for every application that you will want to use SuperNOVAS with. This is why the runtime configuration of the ephemeris provider functions is the best and most generic way to add your preferred implementations while also providing some minimum default implementations for other users of the library, who may not need your ephemeris service, or have no need for planet data beyond the approximate positions for the Earth and Sun.
You can enable or disable debugging output to stderr with novas_debug(enum novas_debug_mode), where the argument is one of the defined constants from novas.h:
novas_debug_mode value | Description |
|---|---|
NOVAS_DEBUG_OFF | No debugging output (default) |
NOVAS_DEBUG_ON | Prints error messages and traces to stderr |
NOVAS_DEBUG_EXTRA | Same as above but with stricter error checking |
The main difference between NOVAS_DEBUG_ON and NOVAS_DEBUG_EXTRA is that the latter will treat minor issues as errors also, while the former may ignore them. For example, place() will return normally by default if it cannot calculate gravitational bending around massive planets in full accuracy mode. It is unlikely that this omission would significantly alter the result in most cases, except for some very specific ones when observing in a direction close to a major planet. Thus, with NOVAS_DEBUG_ON, place() go about as usual even if the Jupiter's position is not known. However, NOVAS_DEBUG_EXTRA will not give it a free pass, and will make place() return an error (and print the trace) if it cannot properly account for gravitational bending around the major planets as it is expected to.
A predictable release schedule and process can help manage expectations and reduce stress on adopters and developers alike.
Releases of the library shall follow a quarterly release schedule. You may expect upcoming releases to be published around February 1, May 1, August 1, and/or November 1 each year, on an as-needed basis. That means that if there are outstanding bugs, or new pull requests (PRs), you may expect a release that addresses these in the upcoming quarter. The dates are placeholders only, with no guarantee that a new release will actually be available every quarter. If nothing of note comes up, a potential release date may pass without a release being published.
Feature releases (e.g. 1.x.0 version bumps) are provided at least 6 months apart, to reduce stress on adopters who may need/want to tweak their code to integrate these. Between feature releases, bug fix releases (without significant API changes) may be provided as needed to address issues. New features are generally reserved for the feature releases, although they may also be rolled out in bug-fix releases as long as they do not affect the existing API – in line with the desire to keep bug-fix releases fully backwards compatible with their parent versions.
In the weeks and month(s) preceding releases one or more release candidates (e.g. 1.0.1-rc3) will be published temporarily on GitHub, under Releases, so that changes can be tested by adopters before the releases are finalized. Please use due diligence to test such release candidates with your code when they become available to avoid unexpected surprises when the finalized release is published. Release candidates are typically available for one week only before they are superseded either by another, or by the finalized release.
Copyright (C) 2024 Attila Kovács
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