# SuperNOVAS
The NOVAS C astrometry library, made better. - [API documentation](https://smithsonian.github.io/SuperNOVAS/doc/html/files.html) - [SuperNOVAS pages](https://smithsonian.github.io/SuperNOVAS) on github.io [SuperNOVAS](https://github.com/Smithsonian/SuperNOVAS/) is a C/C++ astronomy software library, providing high-precision astrometry such as one might need for running an observatory, a precise planetarium program, or for analyzing astronomical datasets. It started as a fork of the Naval Observatory Vector Astrometry Software ([NOVAS](https://aa.usno.navy.mil/software/novas_info)) C version 3.1, but since then it has grown into its own, providing bug fixes, tons of new features, and a much improved API compared to the original NOVAS. __SuperNOVAS__ is easy to use and it is very fast, providing 3--5 orders of magnitude faster position calculations than [astropy](https://www.astropy.org/) 7.0.0 in a single thread (see the [benchmarks](#benchmarks)), and its performance will scale with the number of CPUs when calculations are performed in parallel threads. __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. And, despite it being a light-weight library, it fully supports the IAU 2000/2006 standards for microarcsecond-level position calculations. This document has been updated for the `v1.5` and later releases. ## Table of Contents - [Introduction](#introduction) - [Fixed NOVAS C 3.1 issues](#fixed-issues) - [Compatibility with NOVAS C 3.1](#compatibility) - [Building and installation](#installation) - [Building your application with SuperNOVAS](#integration) - [Celestial coordinate systems (old vs. new)](#methodologies) - [Example usage](#examples) - [Incorporating Solar-system ephemeris data or services](#solarsystem) - [Notes on precision](#precision) - [Tips and tricks](#tips) - [Runtime debug support](#debug-support) - [Representative benchmarks](#benchmarks) - [SuperNOVAS added features](#supernovas-features) - [Release schedule](#release-schedule) ----------------------------------------------------------------------------- ## Introduction __SuperNOVAS__ is a fork of the The Naval Observatory Vector Astrometry Software ([NOVAS](https://aa.usno.navy.mil/software/novas_info)). (It is not related to the separate NOVA / libnova library.) The primary goal of __SuperNOVAS__ is to improve on the original NOVAS C library via: - Fixing [outstanding issues](#fixed-issues). - Improved [API documentation](https://smithsonian.github.io/SuperNOVAS/doc/html/files.html). - [Faster calculations](#benchmarks). - [New features](#added-functionality). - [Refining the API](#api-changes) to promote best programming practices. - [Thread-safe calculations](#multi-threading). - [Debug mode](#debug-support) with informative error tracing. - [Regression testing](https://codecov.io/gh/Smithsonian/SuperNOVAS) and continuous integration on GitHub. 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 _build-time_ replacement for NOVAS in your application without having to change existing (functional) code you may have written for NOVAS C. __SuperNOVAS__ is really quite easy to use. Its new API is just as simple and intuitive as that of __astropy__ (or so we strive for it to be), and it is similarly well documented also (see the [API documentation](https://smithsonian.github.io/SuperNOVAS/doc/html/files.html)). You can typically achieve the same results with [similar lines of code](https://github.com/Smithsonian/SuperNOVAS/blob/main/doc/SuperNOVAS_vs_astropy.md) with __SuperNOVAS__ as with __astropy__, notwithstanding a little more involved error handling at every step (due to the lack of `try / except` style constructs in 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 Kovács](https://github.com/attipaci) at the Center for Astrophysics \| Harvard & Smithsonian, and it is available through the [Smithsonian/SuperNOVAS](https://github.com/Smithsonian/SuperNOVAS) repository on GitHub. Outside contributions are very welcome. See [how you can contribute](https://smithsonian.github.io/SuperNOVAS/doc/CONTRIBUTING.html) on how you can make __SuperNOVAS__ even better. ### Related links - [NOVAS](https://aa.usno.navy.mil/software/novas_info) home page at the US Naval Observatory. - [CALCEPH C library](https://calceph.imcce.fr) for integrating Solar-system ephemerides from JPL and/or in INPOP 2.0/3.0 format. - [NAIF SPICE toolkit](https://naif.jpl.nasa.gov/naif/toolkit.html) for integrating Solar-system ephemerides from JPL. - [Smithsonian/cspice-sharedlib](https://github.com/Smithsonian/cspice-sharedlib) for building CSPICE as a shared library for dynamic linking. - [IAU Minor Planet Center](https://www.minorplanetcenter.net/iau/mpc.html) provides up-to-date orbital elements for asteroids, comets, and near-Earth objects (NEOs), including newly discovered objects. ----------------------------------------------------------------------------- ## Fixed NOVAS C 3.1 issues __SuperNOVAS__ fixes a number of outstanding issues with NOVAS C 3.1:
- Fixes the [sidereal_time bug](https://aa.usno.navy.mil/software/novas_faq), whereby the `sidereal_time()` function
had an incorrect unit cast. This was a documented issue of NOVAS C 3.1.
- Fixes the [ephem_close bug](https://aa.usno.navy.mil/software/novas_faq), whereby `ephem_close()` in
`eph_manager.c` did not reset the `EPHFILE` pointer to NULL. This was a documented issue of NOVAS C 3.1.
- Fixes antedating velocities and distances for light travel time in `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.
- Fixes bug in `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()`.
- Fixes accuracy switching bug in `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.
- Fixes multiple bugs related to using cached values in `cio_basis()` with alternating CIO location reference
systems. This affected many CIRS-based position calculations downstream.
- Fixes bug in `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.
- Some remainder calculations in NOVAS C 3.1 used the result from `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.
- Fixes `aberration()` returning NaN vectors if the `ve` argument is 0. It now returns the unmodified input vector
appropriately instead.
- Fixes unpopulated `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.
- Fixes potential string overflows and eliminates associated compiler warnings.
- Nutation series used truncated expressions for the fundamental arguments, resulting in μas-level errors in when
dozens or more years away from the reference epoch of J2000.
- [__v1.1__] Fixes division by zero bug in `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.
- [__v1.1__] The NOVAS C 3.1 implementation of `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.
- [__v1.4__] The NOVAS C 3.1 implementation of `cel2ter()` / `ter2cel()` was such that if both `xp` and `yp`
parameters were zero, then no wobble correction was applied, not even for the TIO longitude (s'). The error from
this omission is very small, at just a few μas (microarcseconds) within a couple of centuries of J2000.
-----------------------------------------------------------------------------
## Compatibility with NOVAS C 3.1
__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 the libraries (e.g. the static
`libnovas.a`, or the shared `libnovas.so`), 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` option arguments used in 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.
-----------------------------------------------------------------------------
## Building and installation
- [Build SuperNOVAS using GNU make](#gnu-build)
- [Build SuperNOVAS using CMake](#cmake-build)
- [Install SuperNOVAS via `vcpkg`](#vcpkg-port)
- [Linux packages](#linux-packages)
- [Homebrew package](#homebrew)
### Build SuperNOVAS using GNU make
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, Mac OS X, BSD, Cygwin or WSL -- using
[GNU `make`](https://www.gnu.org/software/make/).
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:
- [CALCEPH](https://www.imcce.fr/recherche/equipes/asd/calceph/) C library integration is automatic on Linux if
`ldconfig` can locate the `libcalceph` shared library. You can also control CALCEPH integration manually, e.g. by
setting `CALCEPH_SUPPORT = 1` in `config.mk` or in the shell prior to the build. CALCEPH integration will require
an accessible installation of the CALCEPH development files (C headers and unversioned static or shared libraries
depending on the needs of the build).
- [NAIF CSPICE Toolkit](https://naif.jpl.nasa.gov/naif/toolkit.html) integration is automatic on Linux if `ldconfig`
can locate the `libcspice` shared library. You can also control CSPICE integration manually, e.g. by setting
`CSPICE_SUPPORT = 1` in `config.mk` or in the shell prior to the build. CSPICE integration will require an
accessible installation of the CSPICE development files (C headers, under a `cspice/` subfolder 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](https://github.com/Smithsonian/cspice-sharedlib) repository for
building CSPICE as a shared library.
- If your compiler does not support the C11 standard and it is not GCC >=3.3, but provides some nonstandard
support for declaring thread-local variables, you may want to pass the keyword to use to declare variables as
thread local via `-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`.)
Additionally, you may set number of environment variables to futher customize the build, such as:
- `CC`: The C compiler to use (default: `gcc`).
- `CPPFLAGS`: C preprocessor flags, such as externally defined compiler constants.
- `CFLAGS`: Flags to pass onto the C compiler (default: `-g -Os -Wall`). Note, `-Iinclude` will be added
automatically.
- `LDFLAGS`: Extra linker flags (default is _not set_). Note, `-lm` will be added automatically.
- `CSTANDARD`: Optionally, specify the C standard to compile for, e.g. `c99` to compile for the C99 standard. If
defined then `-std=$(CSTANDARD)` is added to `CFLAGS` automatically.
- `WEXTRA`: If set to 1, `-Wextra` is added to `CFLAGS` automatically.
- `FORTIFY`: If set it will set the `_FORTIFY_SOURCE` macro to the specified value (`gcc` supports values 1
through 3). It affords varying levels of extra compile time / runtime checks.
- `CHECKEXTRA`: Extra options to pass to `cppcheck` for the `make check` target
- `DOXYGEN`: Specify the `doxygen` executable to use for generating documentation. If not set (default), `make` will
use `doxygen` in your `PATH` (if any). You can also set it to `none` to disable document generation and the
checking for a usable `doxygen` version entirely.
Now you are ready to build the library:
```bash
$ make
```
will compile the shared (e.g. `lib/libsupernovas.so`) libraries, and compile the API documentation (into `doc/`)
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.
To build __SuperNOVAS__ as static libraries, use `make static`.
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:
```bash
$ sudo make install
```
Or, to install in some other locations, you may set a prefix and/or `DESTDIR`. For example, to install under `/opt`
instead, you can:
```bash
$ sudo make prefix="/opt" install
```
Or, to stage the installation (to `/usr`) under a 'build root':
```bash
$ make DESTDIR="/tmp/stage" install
```
> [!TIP]
> On BSD, you will need to use `gmake` instead of `make`.
> [!NOTE]
> if you want to build __SuperNOVAS__ for with your old NOVAS C applications you might want to further customize the
> build. See Section(s) on [legacy application](#legacy-application) further below.
### Build SuperNOVAS using CMake
As of v1.5, __SuperNOVAS__ can be built using [CMake](https://cmake.org/) (many thanks to Kiran Shila). CMake allows
for greater portability than the regular GNU `Makefile`. Note, however, that the CMake configuration does not support
all of the build options of the GNU `Makefile`, such as automatic CALCEPH and CSPICE integration on Linux, supporting
legacy NOVAS C style builds, and code coverage tracking.
The basic build recipe for CMake is:
```bash
$ cmake -B build
$ cmake --build build
```
The __SuperNOVAS__ CMake build supports the following options (in addition to the standard CMake options):
- `BUILD_SHARED_LIBS=ON|OFF` (default: OFF) - Build shared libraries instead of static
- `BUILD_DOC=ON|OFF` (default: ON) - Compile HTML documentation. Requires `doxygen`.
- `BUILD_EXAMPLES=ON|OFF` (default: ON) - Build the included examples
- `BUILD_TESTING=ON|OFF` (default: ON - Build regression tests
- `BUILD_BENCHMARK=ON|OFF` (default: OFF - Build benchmarking programs
- `ENABLE_CALCEPH=ON|OFF` (default: OFF) - Optional CALCEPH ephemeris plugin support. Requires `calceph` package.
- `ENABLE_CSPICE=ON|OFF` (default: OFF) - Optional CSPICE ephemeris plugin support. Requires `cspice` library
installed.
For example, to build __SuperNOVAS__ as shared libraries with
[CALCEPH](https://calceph.imcce.fr) integration for ephemeris support:
```bash
$ cmake -B build -DCMAKE_BUILD_TYPE=Release -DBUILD_SHARED_LIBS=ON -DENABLE_CALCEPH=ON
$ cmake --build build
```
If a `CMAKE_BUILD_TYPE` is not set, the build will only use the `CFLAGS` (if any) that were set in the environment.
This is ideal for those who want to have full control of the compiler flags used in the build. Specifying
`Release` or `Debug` will append a particular set of appropriate compiler options which are suited for the given
build type. (If you want to use the MinGW compiler on Windows, you'll want to set
`-DCMAKE_C_COMPILER=gcc -G "MinGW Makefiles"` options also.)
After a successful build, you can install the `Runtime` (libraries), and `Development` (headers, CMake config, and
`pkg-config`) components, e.g. under `/usr/local`, as:
```bash
$ cmake --build build
```
Or, on Windows (Microsoft Visual C) you will want:
```bash
$ cmake --build build --config Release
```
After the build, you can install the __SuperNOVAS__ files in the location of choice (e.g. `/usr/local`):
```bash
$ cmake --install build --prefix /usr/local
```
You can also use the `--component` option to install just the selected components. For example to install just
the `Runtime` component:
```bash
$ cmake --install build --component Runtime --prefix /usr/local
```
### Install SuperNOVAS via `vcpkg`
As of version 1.5, SuperNOVAS is available through the [vcpkg](https://vcpkg.io/en/) registry. The `vcpkg` port
supports a wide range of platforms, including Linux, Windows, MacOS, and Android -- for both `arm64` and `x64`
architectures (and in case of Windows also `x86`). It is effectively the same as the CMake build (above), only with
more simplicity, convenience, and dependency resolution.
You can install the core SuperNOVAS library with `vcpkg` as:
```bash
$ vcpkg install supernovas
```
Or, including the `solsys-calceph` plugin library as:
```bash
$ vcpkg install supernovas[solsys-calceph]
```
The latter will also install the `calceph` library dependency, as needed.
### Linux packages
SuperNOVAS is packaged for both Debian and Fedora / EPEL Linux distributions, and derivatives based on these (Ubuntu,
Mint, RHEL, CentOS Stream, Alma Linux, Rocky Linux, Oracle Linux...).
On Debian-based platforms you might install all components via:
```bash
$ sudo apt-get install libsupernovas1 libsolsys-calceph1 libsupernovas-doc libsupernovas-dev
```
And or Fedora / EPEL based distributions as:
```bash
$ sudo dnf install supernovas supernovas-solsys-calceph supernovas-doc supernovas-devel
```
In both cases the first package is the runtime library, the second is the runtime library for the `solsys-calceph`
plugin, the third is documentation, and the last one is the files needed for application development.
> [!NOTE] The turnaround time for Debian packages is quite slow, and typically follows the 6-month Debian release
> cycle, whereas the Fedora / EPEL packages are usually fully up-to-date (i.e. in `stable`) within a week of a new
> SuperNOVAS release. Somewhat newer Debian versions may be found in `testing`, but even that tends to lag behind the
> `stable` Fedora / EPEL updates.
### Homebrew package
As of version 1.5, there is also a [Homebrew](https://brew.sh/) package through the maintainer's own Tap, which
includes the `solsys-calceph` plugin by default.
```bash
$ brew tap attipaci/pub
$ brew install supernovas
```
-----------------------------------------------------------------------------
## Building your application with SuperNOVAS
There are a number of ways you can build your application with __SuperNOVAS__. See which of the options suits your
needs best:
- [Using a GNU `Makefile`](#makefile-application)
- [Using CMake](#cmake-application)
- [Deprecated API](#deprecations)
- [Legacy linking `solarsystem()` and `readeph()` modules](#legacy-application)
- [Legacy modules: a better way](#preferred-legacy-application)
### Using a GNU `Makefile`
Provided you have installed the __SuperNOVAS__ headers and (static or shared) libraries into a standard location, you
can build your application against it easily. For example, to build `myastroapp.c` against __SuperNOVAS__, you might
have a `Makefile` with contents like:
```make
myastroapp: myastroapp.c
$(CC) -o $@ $(CFLAGS) $^ -lm -lsupernovas
```
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`, because these headers were implicitly included with
`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` compiler flag when compiling your
application:
```make
myastroapp: myastroapp.c
$(CC) -o $@ $(CFLAGS) -DCOMPAT $^ -lm -lsupernovas
```
If your application uses optional planet or ephemeris calculator modules, you may need to specify the additional
shared libraries also:
```make
myastroapp: myastroapp.c
$(CC) -o $@ $(CFLAGS) $^ -lm -lsupernovas -lsolsys-calceph -lcalceph
```
### Using CMake
Add the appropriate bits from below to the `CMakeLists.txt` file of your application (`my-application`):
```cmake
find_package(supernovas REQUIRED)
target_link_libraries(my-application PRIVATE supernovas)
```
Or, to include ephemeris support via the CALCEPH library (`solsys-calceph` component) also:
```cmake
find_package(supernovas REQUIRED COMPONENTS solsys-calceph)
target_link_libraries(my-application PRIVATE supernovas solsys-calceph)
```
Similarly, for ephemeris support via CSPICE you can use the `solsys-cspice` component.
### Deprecated API
__SuperNOVAS__ began deprecating some NOVAS C functions, either because they are no longer needed; or are not easy to
use and have better alternatives around; or are internals that should never have been exposed to end-users. The
deprecations are marked in the inline and HTML API documentations, suggesting also alternatives.
That said, the deprecated parts of the API are NOT removed, nor we plan on removing them for the foreseeable future.
Instead, they serve as a gentle reminder to users that perhaps they should stay away from these features for their own
good.
However, you have the option to force yourself to avoid using the deprecated API if you choose to do so, by compiling
your application with `-D_EXCLUDE_DEPRECATED`, or equivalently, by defining `_EXCLUDE_DEPRECATED` in your source code
_before_ including `novas.h`. E.g.:
```c
// Include novas.h without the deprecated definitions
#define _EXCLUDE_DEPRECATED
#include
To use your own existing default `solarsystem()` implementation in the NOVAS C way, you will have to build
__SuperNOVAS__ with `SOLSYS_SOURCE` set to the source file(s) of the implementation (`config.mk` or the environment).
The same principle applies to using your specific legacy `readeph()` implementation, except that you must set
`READEPH_SOURCE` to the source file(s) of the chosen implementation when building __SuperNOVAS__).
(You might have to also add additional include directories to `CPPFLAGS`, e.g. `-I/my-path/include` for you custom
sources for their associated headers).
### Legacy modules: a better way
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.
E.g.:
```c
set_planet_calculator(my_planet_calculator);
set_planet_calculator(my_planet_calculator_hp);
```
(You might also change the `short` type parameters to the SuperNOVAS enum types while at it, to conform to the
SuperNOVAS `novas_planet_provider` / `novas_planet_provider_hp` types.)
For `readeph()` implementations, it is recommended that you change both the name and the footprint to e.g.:
```c
int my_ephem_provider(const char *name, long id, double jd_tdb_high, double jd_tdb_low,
enum novas_origin *origin, double *pos, double *vel);
```
and then then apply it in your application as:
```c
set_ephem_provider(my_ephem_provider);
```
While all of that requires some minimal changes to your old code, the advantage of this preferred approach is that
you do not need to re-build the library with `USER_SOLSYS` and/or `USER_READEPH` defined.
-----------------------------------------------------------------------------
## Celestial coordinate systems (old vs. new)
|  |
|:--:|
| __Figure 1.__ SuperNOVAS Coordinate Systems and Conversions. Functions indicated in bold face are available in NOVAS C also. All other functions are available in SuperNOVAS only. SuperNOVAS also adds efficient [matrix transformations](#transforms) between the equatorial systems. |
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. The table below provides an overview of how the old and new methods define
some of the terms differently:
| Concept | Old standard | New IAU standard |
|:-------------------------- | ----------------------------- | ------------------------------------------------- |
| Catalog coordinate system | MOD (e.g. 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 | no tidal terms | IAU 2000/2006 precession/nutation model |
| Celestial Pole offsets | dψ, dε (for TOD) | _x_p, _y_p (for ITRS) |
| Earth rotation measure | Greenwich Sidereal Time (GST) | Earth Rotation Angle (ERA) |
| Pseudo Earth-fixed system | PEF | Terrestrial Intermediate Reference System (TIRS) |
| Earth rotation origin | Greenwich Meridian | Terrestrial Intermediate Origin (TIO) |
| Earth-fixed 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. Figure 1 also shows the relation of the
various old and new coordinate systems and the (Super)NOVAS functions for converting position / velocity vectors among
them.
> [!NOTE]
> In NOVAS, the barycentric BCRS and the geocentric GCRS systems are effectively synonymous to ICRS, since the origin
> for positions and for velocities, in any reference system, is determined by the `observer` location. Aberration and
> gravitational deflection correction included for apparent places only (as seen from the observer location,
> regardless of where that is), but not for geometric places.
> [!TIP]
> Older catalogs, such as J2000 (FK5), HIP, B1950 (FK4) or B1900 are just special cases of MOD (mean-of-date)
> coordinates for the J2000, J1991.25, B1950, and B1900 epochs, respectively.
> [!CAUTION]
> Applying residual polar offsets (Δdψ, Δdε or _x_p, _y_p) to the
> TOD equator (via `cel_pole()`) is discouraged. Instead, the sub-arcsecond level corrections to Earth orientation
> (_x_p, _y_p) should be used only for converting between the pseudo Earth-fixed (PEF or TIRS)
> and ITRS, and vice-versa (e.g. with `novas_make_frame()` or `wobble()`).
> [!NOTE]
> WGS84 has been superseded by ITRS for higher accuracy definitions of Earth-based locations. WGS84 matches ITRS to
> the 10m level globally, but it does not account for continental drifts and crustal motion. In (Super)NOVAS all
> Earth-base locations are presumed ITRS. ITRS longitude, latitude, and altitude coordinates are referenced to the
> GRS80 ellipsoid, whereas GPS locations are referenced to the WGS84 ellipsoid. __SuperNOVAS__ offers ways to convert
> between the two if needed.
-----------------------------------------------------------------------------
## Example usage
- [Calculating positions for a sidereal source](#sidereal-example)
- [Calculating positions for a Solar-system source](#solsys-example)
- [Coordinate and velocity transforms (change of coordinate system)](#transforms)
__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).
> [!NOTE]
> You may find an equivalent legacy example showcasing the original NOVAS method in
> [`NOVAS-legacy.md`](https://github.com/Smithsonian/SuperNOVAS/blob/main/doc/NOVAS-legacy.md).
### Calculating positions for a sidereal source
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.
- [Specify the object of interest](#specify-object)
- [Specify the observer location](#specify-observer)
- [Specify the time of observation](#specify-time)
- [Set up the observing frame](#observing-frame)
- [Calculate an apparent place on sky](#apparent-place)
- [Calculate azimuth and elevation angles at the observing location](#horizontal-place)
- [Going in reverse...](#reverse-place)
- [Calculate rise, set, and transit times](#rise-set-transit)
- [Coordinate and velocity transforms (change of coordinate system)](#transforms)
#### Specify the object of interest
First, you must provide the astrometric parameters (coordinates, and optionally radial velocity or redshift, proper
motion, and/or parallax or distance also). Let's assume we pick a star for which we have B1950 (i.e. FK4) coordinates.
We begin with the assigned name and the R.A. / Dec coordinates.
```c
cat_entry star; // Structure to contain information on sidereal source
// Let's assume we have B1950 (FK4) coordinates of
// 16h26m20.1918s, -26d19m23.138s
novas_init_cat_entry(&star, "Antares", 16.43894213, -26.323094);
```
If you have coordinates as strings in decimal or HMS / DMS format, you might use `novas_str_hours()` and/or
`novas_str_degrees()` to convert them to hours/degrees for `novas_init_cat_entry()`, with a fair bit of flexibility on
the particulars of the representation, e.g.:
```c
novas_init_entry(&star, "Antares",
novas_str_hours("16h 26m 20.1918s"), // e.g. using h,m,s and spaces as separators
novas_str_degrees("-26:19:23.138")); // e.g. using colons to separate components
```
Next, if it's a star or some other source within our own Galaxy, you'll want to specify its proper motion (in the same
reference system as the above coordinates), so we can calculate its position for the epoch of observation.
```c
// Now, let's add proper motion of 12.11, -23.30 mas/year.
novas_set_proper_motion(&star, -12.11, -23.30);
```
For Galactic sources you will also want to set the parallax using `novas_set_parallax()` or equivalently the distance
(in parsecs) using `novas_set_distance()`, e.g.:
```c
// Add parallax of 5.89 mas
novas_set_parallax(&star, 5.89);
```
Finally, for spectroscopic applications you will also want to set the radial velocity. You can use
`novas_set_ssb_vel()` if you have standard radial velocities defined with respect to the Solar System Barycenter; or
`novas_set_lsr_vel()` if the velocity is relative to the Local Standard of Rest (LSR); or else `novas_set_redshift()`
if you have a redshift measure (as is typical for distant galaxies and quasars). E.g.:
```c
// Add a radial velocity of -3.4 km/s (relative to SSB)
novas_set_ssb_vel(&star, -3.4);
```
Alternatively, if you prefer, you may use the original NOVAS C `make_cat_entry()` to set the astrometric parameters
above all at once.
E.g.:
```c
make_cat_entry("Antares", "FK4", 1,
novas_str_hours("16h 26m 20.1918s"),
novas_str_degrees("-26:19:23.138"),
-12.11, -23.30, 5.89, -3.4, &star);
```
Next, we wrap that catalog source into a generic celestial `object` structure. (An `object` handles various
Solar-system sources also, as you'll see further below). Whereas the catalog source may have been defined in any epoch
/ catalog system, the `object` structure shall define ICRS coordinates always (no exceptions):
```c
object source; // Encapsulates a sidereal or a Solar-system source
// Use the B1950 astrometric parameters to set up the observables in ICRS...
make_cat_object_sys(&star, "B1950", &source);
```
Alternatively, for high-_z_ sources you might simply use the 1-step `make_redshifted_object_sys()` e.g.:
```c
object quasar;
// 12h29m6.6997s +2d3m8.598s (ICRS) z=0.158339
make_redshifted_object_sys("3c273", 12.4851944, 2.0523883, "ICRS", 0.158339, &quasar);
```
#### Specify the observer location
Next, we define the location where we observe from. Let's assume we have a GPS location:
```c
observer obs; // Structure to contain observer location
// Specify the location we are observing from, e.g. a GPS / WGS84 location
// 50.7374 deg N, 7.0982 deg E, 60m elevation
make_gps_observer(50.7374, 7.0982, 60.0, &obs);
```
> [!TIP]
> You might use `make_itrf_observer()` instead if the location is defined on the GRS80 reference ellipsoid, used e.g.
> for ITRF locations. Or, if you have geocentric Cartesian coordinates, you could use `make_xyz_site()` and then
> `make_observer_at_site()`.
Again you might use `novas_str_degrees()` for typical string representations of the longitude and latitude coordinates
here, such as:
```c
make_gps_observer(
novas_str_degrees("50.7374N"),
novas_str_degrees("7.0982 deg E"),
60.0,
&obs);
```
Alternatively, you can also specify airborne observers, or observers in Earth orbit, in heliocentric orbit, at the
geocenter, or at the Solar-system barycenter. The above also sets default, mean annual weather parameters based on
the location and a global model based on Feulner et al. (2013).
You can, of course, set actual weather values _after_, as appropriate, if you need them for the refraction models,
e.g.:
```c
obs.on_surf.temperature = 12.4; // [C] Ambient temperature
obs.on_surf.pressure = 973.47; // [mbar] Atmospheric pressure
obs.on_surf.humidity = 48.3; // [%] relative humidity to use for refraction.
```
#### Specify the time of observation
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. You can obtain suitable values for DUT1 from
IERS, and for the highest precision, interpolate for the time of observations. For the example, let's assume 37 leap
seconds, and DUT1 = 0.042,
```c
int leap_seconds = 37; // [s] UTC - TAI time difference
double dut1 = 0.042; // [s] UT1 - UTC time difference
```
Then we can set the time of observation, for example, using the current UNIX time:
```c
novas_timespec obs_time; // Structure that will define astrometric time
// Set the time of observation to the precise UTC-based UNIX time
novas_set_current_time(leap_seconds, dut1, &obs_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):
```c
double jd_tai = ... // TAI-based Julian Date
novas_set_time(NOVAS_TAI, jd_tai, leap_seconds, dut1, &obs_time);
```
or, for the best precision we may do the same with an integer / fractional split:
```c
long ijd_tai = ... // Integer part of the TAI-based Julian Date
double fjd_tai = ... // Fractional part of the TAI-based Julian Date
novas_set_split_time(NOVAS_TAI, ijd_tai, fjd_tai, leap_seconds, dut1, &obs_time);
```
Or, you might use string dates, such as an ISO timestamp:
```c
novas_set_str_time(NOVAS_UTC, "2025-01-26T22:05:14.234+0200", leap_seconds, dut1, &obs_time);
```
Note, that the likes of `novas_set_time()` will automatically apply diurnal corrections to the supplied UT1-UTC time
difference for libration and ocean tides. Thus, the supplied values should not include these. Rather you should pass
`dut1` directly (or interpolated) from the IERS Bulletin values for the time of observation.
#### Set up the observing frame
Next, we set up an observing frame, which is defined for a unique combination of the observer location and the time of
observation:
```c
novas_frame obs_frame; // Structure that will define the observing frame
double xp = ... // [mas] Earth polar offset x, e.g. from IERS Bulletin A.
double yp = ... // [mas] Earth polar offset y, from same source as above.
// Initialize the observing frame with the given observing parameters
novas_make_frame(NOVAS_REDUCED_ACCURACY, &obs, &obs_time, xp, yp, &obs_frame);
```
Here `xp` and `yp` are small (sub-arcsec level) corrections to Earth orientation. Values for these are are published
in the [IERS Bulletins](https://www.iers.org/IERS/EN/Publications/Bulletins/bulletins.html). These values should be
interpolated for the time of observation, but should NOT be corrected for libration and ocean tides
(`novas_make_frame() will apply such corrections as appropriate for full accuracy frames). The Earth orientation
parameters (EOP) are needed only when converting positions from the celestial CIRS (or TOD) frame to the Earth-fixed
ITRS (or PEF) frames. You may ignore these and set zeroes if not interested in Earth-fixed calculations or 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 (see the [benchmarks](#benchmarks)), since all sources in a frame have well-defined, fixed, topological
positions on the celestial sphere. It is only a matter of expressing these positions as coordinates (and velocities)
in a particular coordinate system. 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()`.
> [!IMPORTANT]
> Without a proper ephemeris provider for the major planets, you are invariably restricted to working with
> `NOVAS_REDUCED_ACCURACY` frames, providing milliarcsecond precision at most. Attempting to construct high-accuracy
> frames without an appropriate high-precision ephemeris provider will result in an error from the requisite
> `ephemeris()` calls.
> [!TIP]
> `NOVAS_FULL_ACCURACY` frames require a high-precision ephemeris provider for the major planets, e.g. to account
> for the gravitational deflections. Without it, μas accuracy cannot be ensured, in general. See section on
> [Incorporating Solar-system ephemeris data or services](#solarsystem) further below.
#### Calculate an apparent place on sky
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 (in full accuracy mode). You can calculate an
apparent location in the coordinate system of choice (ICRS/GCRS, CIRS, J2000, MOD, TOD, TIRS, or ITRS) using
`novas_sky_pos()`. E.g.:
```c
sky_pos apparent; // Structure containing the precise observed position
novas_sky_pos(&source, &obs_frame, NOVAS_CIRS, &apparent);
```
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]
> If you want geometric positions (and/or velocities) instead, without aberration and gravitational deflection, you
> might use `novas_geom_posvel()`.
> [!TIP]
> Regardless, which reference system you have used in the calculations above, you can always easily and efficiently
> change the coordinate reference 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()`. More on
> [coordinate transforms](#transforms) further below.
#### Calculate azimuth and elevation angles at the observing location
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!):
```c
double az, el; // [deg] local azimuth and elevation angles to populate
// Convert the apparent position in CIRS on sky to horizontal coordinates
novas_app_to_hor(&obs_frame, NOVAS_CIRS, apparent.ra, apparent.dec, novas_standard_refraction,
&az, &el);
```
Above we converted the apparent coordinates, that 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.
#### Going in reverse...
Of course, __SuperNOVAS__ allows you to go in reverse, for example from an observed Az/El position all the way to
proper ICRS R.A./Dec coordinates.
E.g.:
```c
double az = ..., el = ...; // [deg] measured azimuth and elevation angles
double pos[3]; // [arb. u.] xyz position vector
double ra, dec; // [h, deg] R.A. and declination to populate
// Calculate the observer's apparent coordinates from the observed Az/El values,
// lets say in CIRS (but it could also be ICRS, for all that matters).
novas_hor_to_app(&obs_frame, az, el, novas_standard_refraction, NOVAS_CIRS, &ra, &dec);
// Convert apparent to ICRS geometric positions (no parallax)
novas_app_to_geom(&obs_frame, NOVAS_CIRS, ra, dec, 0.0, pos);
// Convert ICRS rectangular equatorial to R.A. and Dec
vector2radec(pos, &ra, &dec);
```
Voila! And, of course you might want the coordinates in some other reference systems, such as B1950. For that you can
simply add a transformation before `vector2radec()` above, e.g. as:
```c
...
// Transform position from ICRS to B1950
gcrs_to_mod(NOVAS_JD_B1950, pos, pos);
// Convert B1950 xyz position to R.A. and Dec
vector2radec(pos, &ra, &dec);
```
#### Calculate rise, set, and transit times
You may be interested to know when sources rise above or set below some specific elevation angle, or at what time they
appear to transit at the observer location. __SuperNOVAS__ has routines to help you with that too.
Given that rise, set, or transit times are dependent on the day of observation, and observer location, they are
effectively tied to an observer frame.
```c
novas_frame frame = ...; // Earth-based observer location and lower-bound time of interest.
object source = ...; // Source of interest
// UTC-based Julian day *after* observer frame, when source rises above 30 degrees of elevation
// next, given a standard optical refraction model.
double jd_rise = novas_rises_above(30.0, &source, &frame, novas_standard_refraction);
// UTC-based Julian day *after* observer frame, of next source transit
double jd_transit = novas_transit_time(&source, &frame);
// UTC-based Julian day *after* observer frame, when source sets below 30 degrees of elevation
// next, not accounting for refraction.
double jd_rise = novas_sets_below(30.0, &source, &frame, NULL);
```
Note, that in the current implementation these calls are not well suited sources that are at or within the
geostationary orbit, such as such as Low Earth Orbit satellites (LEOs), geostationary satellites (which never really
rise, set, or transit), or some Near Earth Objects (NEOs), which will rise set multiple times per day. For the latter,
the above calls may still return a valid time, only without the guarantee that it is the time of the first such event
after the specified frame instant. A future implementation may address near-Earth orbits better, so stay tuned for
updates.
### Calculating positions for a Solar-system source
Solar-system sources work similarly to the above with a few important differences at the start.
#### Planets and/or ephemeris type objects
Historically, NOVAS divided Solar-system objects into two categories: (1) major planets (including also the Sun, the
Moon, and the Solar-system Barycenter); and (2) 'ephemeris' type objects, which are all other Solar-system objects.
The main difference is the numbering convention. NOVAS major planets have definitive ID numbers (see
`enum novas_planet`), whereas 'ephemeris' objects have user-defined IDs. They are also handled by two separate adapter
functions (although __SuperNOVAS__ has the option of using the same ephemeris provider for both types of objects
also).
Thus, instead of `make_cat_object()` you define your source as a planet or ephemeris type `object` with a 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.:
```c
object mars, ceres; // Hold data on solar-system bodies.
// Mars will be handled by the planet provider function
make_planet(NOVAS_MARS, &mars);
// Ceres will be handled by the generic ephemeris provider function, which let's say
// uses the NAIF ID of 2000001 _or_ the name 'Ceres' (depending on the implementation)
make_ephem_object("Ceres", 2000001, &ceres);
```
> [!IMPORTANT]
> Before you can handle all major planets and other ephemeris objects this way, 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
> [Incorporating Solar-system ephemeris data or services](#solarsystem).
And then, it's the same spiel as before, e.g.:
```c
int status = novas_sky_pos(&mars, &obs_frame, NOVAS_TOD, &apparent);
if(status) {
// Oops, something went wrong...
...
}
```
#### Solar-system objects with Keplerian orbital parameters
As of version __1.2__ you can also define solar system sources with Keplerian orbital elements (such as the most
up-to-date ones provided by the [Minor Planet Center](https://minorplanetcenter.net/data) for asteroids, comets,
etc.):
```c
object NEA; // e.g. a Near-Earth Asteroid
// Fill in the orbital parameters (pay attention to units!)
novas_orbital orbit = NOVAS_ORBIT_INIT;
orbit.a = ...; // Major axis in AU...
... // ... and the rest of the orbital elements
// Create an object for that orbit
make_orbital_object("NEAxxx", -1, &orbit, &NEA);
```
> [!NOTE]
> Even with orbital elements, you will, in general, still require an ephemeris provider also, to obtain precise
> positions for the Sun, an Earth-based observer, or the planet, around which the orbit is defined.
#### Approximate planet and Moon orbitals
Finally, as of version __1.4__, you might generate approximate (arcmin-level) orbitals for the major planets (but not
Earth!), the Moon, and the Earth-Moon Barycenter (EMB) also. E.g.:
```c
double jd_tdb = ... // Time (epoch) for which to calculate orbital parameters
// Planet orbitals, e.g. for Mars
novas_orbital mars_orbit = NOVAS_ORBIT_INIT;
novas_make_planet_orbit(NOVAS_MARS, jd_tdb, &mars_orbit);
// Moon's orbital around Earth
novas_orbital moon_orbit = NOVAS_ORBIT_INIT;
novas_make_moon_orbit(jd_tdb, &moon_orbit);
```
While the planet and Moon orbitals are not suitable for precision applications, they can be useful for determining
approximate positions (e.g. via the `novas_approx_heliocentric()` and `novas_approx_sky_pos()` functions), and for
rise/set time calculations.
### Coordinate and velocity transforms (change of coordinate system)
__SuperNOVAS__ introduces matrix transforms (correctly since version __1.4__), which can take a position or velocity
vector (geometric or apparent), obtained for an observer frame, from one coordinate system to another efficiently.
E.g.:
```c
novas_frame frame = ... // The observer frame (time and location)
double j2000_vec[3] = ...; // IN: original position vector, say in J2000.
double tirs_vec[3] = {0.0}; // OUT: equivalent vector in TIRS we want to obtain
novas_transform T; // Coordinate transformation data
// Calculate the transformation matrix from J2000 to TIRS in the given observer frame.
novas_make_transform(&frame, NOVAS_J2000, NOVAS_TIRS, &T);
// Transform the J2000 position or velocity vector to TIRS...
novas_transform_vector(j2000_vec, &T, tirs_vec);
```
Transformations support all __SupeNOVAS__ reference systems, that is ICRS/GCRS, J2000, TOD, MOD, CIRS, TIRS, and ITRS.
The same transform can also be used to convert apparent positions in a `sky_pos` structure also, e.g.:
```c
...
sky_pos j2000_pos = ... // IN: in J2000, e.g. via novas_sky_pos()...
sky_pos tirs_pos; // OUT: equivalent TIRS position to calculate...
// Transform the J2000 apparent positions to TIRS....
novas_transform_sky_pos(&j2000_pos, &T, &tirs_pos);
```
-----------------------------------------------------------------------------
## Incorporating Solar-system ephemeris data or services
If you want to use __SuperNOVAS__ to calculate positions for a range of Solar-system objects, and/or to do it with
precision, you will have to interface it to a suitable provider of ephemeris data. The preferred ways to do that in
__SuperNOVAS__ enumerated below. (The legacy NOVAS C ways are not covered here, since they require specialized builds of
__SuperNOVAS__, which are covered [further above](#legacy-application).)
NASA/JPL provides [generic ephemerides](https://naif.jpl.nasa.gov/pub/naif/generic_kernels/spk/) for the major
planets, satellites thereof, the 300 largest asteroids, the Lagrange points, and some Earth orbiting stations. For
example, [DE440](https://naif.jpl.nasa.gov/pub/naif/generic_kernels/spk/planets/de440.bsp) 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](https://ssd.jpl.nasa.gov/horizons/) system (via the command-line / telnet or API interfaces) to
generate custom ephemerides (SPK/BSP) for just about all known solar systems bodies, down to the tiniest rocks.
- [CALCEPH integration](#calceph-integration)
- [NAIF CSPICE toolkit integration](#cspice-integration)
- [Universal ephemeris data / service integration](#universal-ephemerides)
### CALCEPH integration
The [CALCEPH](https://www.imcce.fr/recherche/equipes/asd/calceph/) library provides 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 (or for CMake
configure with the `-DENABLE_CALCEPH=ON`). Depending on the build target (or type), it will build
`libsolsys-calceph.so[.1]` (target `shared` or CMake option `-DBUILD_SHARED_LIBS=ON1`) or `libsolsys-calceph.a` (target
`static` or default CMake build) libraries or `solsys-calceph.o` (target `solsys`, no CMake equivalent), 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:
```c
#include
#include
// You can open a set of JPL/INPOP ephemeris files with CALCEPH...
t_calcephbin *eph = calceph_open_array(...);
// Then use them as your generic SuperNOVAS ephemeris provider
int status = novas_use_calceph(eph);
if(status < 0) {
// Oops something went wrong...
}
// -----------------------------------------------------------------------
// Optionally you may use a separate ephemeris dataset for major planets
// (or if planet ephemeris was included in 'eph' above, you don't have to)
t_calcephbin *pleph = calceph_open(...);
status = novas_use_calceph_planets(pleph);
if(status < 0) {
// Oops something went wrong...
}
```
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`), and link against the CALCEPH library
also (`-lcalceph`). That's all there is to it.
When using CALCEPH, ephemeris objects are referenced by their ID numbers (`object.number`), unless it is set to -1, in
which case name-based lookup will be used instead. ID numbers are assumed to be NAIF by default, but
`novas_calceph_use_ids()` can select between NAIF or CALCEPH numbering systems, if necessary.
### NAIF CSPICE toolkit integration
The [NAIF CSPICE Toolkit](https://naif.jpl.nasa.gov/naif/toolkit.html) 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 (or for CMake
configure with `-DENABLE_CSPICE=ON`). Depending on the build target, it will build `libsolsys-cspice.so[.1]` (target
`shared` or CMake option `-DBUILD_SHARED_LIBS=ON`) or `libsolsys-cspice.a` (target `static` or default CMake build)
libraries or `solsys-cspice.o` (target `solsys`, no CMake equivalent), 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](https://github.com/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:
```c
#include
#include
// You can load the desired kernels for CSPICE
// E.g. load DE440s and the Mars satellites:
int status;
status = cspice_add_kernel("/path/to/de440s.bsp");
if(status < 0) {
// oops, the kernels must not have loaded...
...
}
// Load additional kernels as needed...
status = cspice_add_kernel("/path/to/mar097.bsp");
...
// Then use CSPICE as your SuperNOVAS ephemeris provider
novas_use_cspice();
```
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`), and of course the CSPICE library also. That's all there is
to it.
When using CSPICE, ephemeris objects are referenced by their NAIF ID numbers (`object.number`), unless that number is
set to -1, in which case name-based lookup will be used instead.
### Universal ephemeris data / service integration
Possibly the most universal way to integrate ephemeris data with __SuperNOVAS__ is to write your own
`novas_ephem_provider` function.
```c
int my_ephem_reader(const char *name, long id, double jd_tdb_high, double jd_tdb_low,
enum novas_origin *restrict origin,
double *restric pos, double *restrict vel) {
// Your custom ephemeris reader implementation here
...
}
```
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()`:
```c
set_ephem_provider(my_ephem_reader);
```
By default, your custom `my_ephem_reader` function will be used for `NOVAS_EPHEM_OBJECT` type objects only (i.e.
anything other than the major planets, the Sun, Moon, Solar-system Barycenter...). But, you can use the same function
for the major planets (`NOVAS_PLANET` type objects) also via:
```c
set_planet_provider(planet_ephem_provider);
set_planet_provider_hp(planet_ephem_provider_hp);
```
The above simply instructs __SuperNOVAS__ to use the same ephemeris provider function for planets as what was set
for `NOVAS_EPHEM_OBJECT` type objects, 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.
## Notes on precision
Many of the (Super)NOVAS functions take an accuracy argument, which determines to what level of 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` | ~ 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 absence of a suitable high-precision ephemeris provider, some functions might
return an error if called with `NOVAS_FULL_ACCURACY`. (Click on the wedges next to each component to expand the
details...)
### Prerequisites to precise results
The __SuperNOVAS__ library is in principle capable of calculating positions to 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. (Click on the wedge next to each heading below to expand
the details.)
The IAU 2000/2006 conventions and methods
High precision calculations will generally require that you use __SuperNOVAS__ with the new IAU standard quantities and methods. The old ways were simply not suited for precision much below the milliarcsecond level. In particular, Earth orientation parameters (EOP) should be applied only for converting between TIRS and ITRS systems, and defined either with `novas_make_frame()` or else with `wobble()`. The old ways of incorporating (global) offsets in TOD coordinates via `cel_pole()` should be avoided.Gravitational effects
Calculations much below the milliarcsecond level will require accounting for gravitational bending around massive Solar-system bodies, and hence will require you to provide a high-precision ephemeris provider for the major planets. Without it, there is no guarantee of achieving precision below the milli-arcsecond level in general, especially when observing near the Sun or massive planets (e.g. observing Jupiter's or Saturn's moons, near conjunction with their host planet). Therefore, some functions will return with an error, if used with `NOVAS_FULL_ACCURACY` in the absence of a suitable high-precision planetary ephemeris provider.Solar-system ephemeris
Precise calculations for Solar-system sources requires precise ephemeris data for both the target object as well as for Earth, and the Sun. For the highest precision calculations you also need positions for all major planets to calculate gravitational deflection precisely. By default, __SuperNOVAS__ can only provide approximate positions for the Earth and Sun (see `earth_sun_calc()`) at the tens of arcsecond level. You will need to provide a way to interface __SuperNOVAS__ with a suitable ephemeris source (such as CALCEPH, or the CSPICE toolkit from JPL) to obtain precise positions for Solar-system bodies. See the [section further above](#solarsystem) for more information how you can do that.Earth orientation parameters (EOP)
Calculating precise positions for any Earth-based observations requires precise knowledge of Earth orientation parameters (EOP) at the time of observation. Earth's pole is subject to predictable precession and nutation, but also small irregular and diurnal variations in the orientation of the rotational axis and the rotation period (a.k.a. polar wobble). You can apply the EOP values in `novas_set_time()` (for UT1-UTC), and `novas_make_frame()` (_x_p and _y_p) to improve the astrometric precision of Earth based coordinate calculations. Without the EOP values, positions for Earth-based calculations will be accurate at the tenths of arcsecond level only. The [IERS Bulletins](https://www.iers.org/IERS/EN/Publications/Bulletins/bulletins.html) provide up-to-date measurements, historical data, and near-term projections for the polar offsets, the UT1-UTC time difference, and leap-seconds (UTC-TAI). For sub-milliarcsecond accuracy the values published by IERS should be interpolated before passing to the likes of `novas_set_time()` or `novas_make_frame()`. At the micro-arcsecond (μas) level, you will need to ensure also that the EOP values are provided for the same ITRF realization as the observer's location, e.g. via `novas_itrf_transform_eop()`.Atmospheric refraction model
Ground based observations are subject to atmospheric refraction. __SuperNOVAS__ offers the option to include refraction corrections with a set of atmospheric models. Estimating refraction accurately requires local weather parameters (pressure, temperature, and humidity), which may be be specified within the `on_surface` data structure alongside the observer location. A standard radio refraction model is included as of version __1.1__, as well as our implementation of the wavelength-dependent IAU refraction model (`novas_wave_refraction()` since version 1.4) based on the SOFA `iauRefco()` function. If none of the supplied options satisfies your needs, you may also implement your own refraction correction to use.
E.g.,
```c
char *pos = NULL; // We'll keep track of the string parse position here
enum novas_timescale scale; // We'll parse the timescale here (if we can)
// Parse the M/D/Y date up to the 'TAI' timescale specification...
double jd = novas_parse_date_format(NOVAS_GREGORIAN_CALENDAR, NOVAS_MDY,
"2/16/2025 20:08:49.082 TAI", &pos);
// Then parse the 'TAI' timescale marker, after the date/time specification
scale = novas_timescale_for_string(pos);
if(scale < 0) {
// Oops, not a valid timescale marker. Perhaps assume UTC...
scale = NOVAS_UTC;
}
// Now set the time for the given calendar, date format, and timescale of the
// string representation.
novas_set_time(scale, jd, leap_seconds, dut1, &time);
```
-----------------------------------------------------------------------------
## Runtime debug support
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.
When debug mode is 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_DEBUG_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):
```
ERROR! earth_sun_calc: invalid or unsupported planet number: 6 [=> 2]
@ earth_sun_calc_hp [=> 2]
@ ephemeris:planet [=> 12]
@ light_time2 [=> 22]
@ obs_planets [=> 12]
@ grav_def [=> 12]
```
-----------------------------------------------------------------------------
## Representative benchmarks
To get an idea of the speed of __SuperNOVAS__, you can use `make benchmark` on your machine. Figure 2 below
summarizes the single-threaded results obtained on an AMD Ryzen 5 PRO 6650U laptop. While this is clearly not the
state of the art for today's server class machines, it nevertheless gives you a ballpark idea for how a typical, not
so new, run-of-the-mill PC might perform.
|  |
|:--:|
| __Figure 2.__ SuperNOVAS apparent position calculation benchmarks, including proper motion, the IAU 2000 precession-nutation model, polar wobble, aberration, and gravitational deflection corrections, and precise spectroscopic redhift calculations. |
The tests calculate apparent positions (in CIRS) for a set of sidereal sources with random parameters, using either
the __SuperNOVAS__ `novas_sky_pos()` or the legacy NOVAS C `place()`, both in full accuracy and reduced accuracy
modes. The two methods are equivalent, and both include calculating a precise geometric position, as well as
aberration and gravitational deflection corrections from the observer's point of view.
| Description | accuracy | positions / sec |
|:----------------------------------- |:---------:| ---------------:|
| `novas_sky_pos()`, same frame | reduced | 3130414 |
| | full | 3149028 |
| `place()`, same time, same observer | reduced | 831101 |
| | full | 831015 |
| `novas_sky_pos()`, individual | reduced | 168212 |
| | full | 25943 |
| `place()`, individual | reduced | 167475 |
| | full | 25537 |
For reference, we also provide the reduced accuracy benchmarks from NOVAS C 3.1.
| Description | accuracy | positions / sec |
|:------------------------------------|:---------:|----------------:|
| NOVAS C 3.1 `place()`, same frame | reduced | 371164 |
| NOVAS C 3.1 `place()`, individual | reduced | 55484 |
For comparison, a very similar benchmark with [astropy](https://www.astropy.org/) (v7.0.0 on Python v3.13.1) on the
same machine, provides ~70 positions / second both for a fixed frame and for individual frames. As such,
__SuperNOVAS__ is a whopping ~40000 times faster than __astropy__ for calculations in the same observing frame, and
400--2000 times faster than __astropy__ for individual frames. (The __astropy__ benchmarking code is also provided
under the `benchmark/` folder in the __SuperNOVAS__ GitHub repository).
| Description | positions / sec |
|:------------------------------------------------|----------------:|
| __astropy__ 7.0.0 (python 3.13.1), same frame | 71 |
| __astropy__ 7.0.0 (python 3.13.1), individual | 70 |
As one may observe, the __SuperNOVAS__ `novas_sky_pos()` significantly outperforms the legacy `place()` function, when
repeatedly calculating positions for sources for the same instant of time and same observer location, providing 3--4
times faster performance than `place()` with the same observer and time. The same performance is maintained even when
cycling through different frames, a usage scenario in which the performance advantage over `place()` may be up to 2
orders of magnitude. When observing frames are reused, the performance is essentially independent of the accuracy. By
contrast, calculations for individual observing times or observer locations are generally around twice a fast if
reduced accuracy is sufficient.
The above benchmarks are all for single-threaded performance. Since __SuperNOVAS__ is generally thread-safe, you can
expect that performance shall scale with the number of concurrent CPUs used. So, on a 16-core PC, with similar single
core performance, you could calculate up to 32 million precise positions per second, if you wanted to. To put that into
perspective, you could calculate precise apparent positions for the entire Gaia dataset (1.7 billion stars) in under
one minute.
-----------------------------------------------------------------------------
## SuperNOVAS added features
- [Newly functionality highlights](#added-functionality)
- [Refinements to the NOVAS C API](#api-changes)
### New functionality highlights
Below is a non-exhaustive overview new features added by __SuperNOVAS__ on top of the existing NOVAS C API. See
[`CHANGELOG.md`](https://github.com/Smithsonian/SuperNOVAS/blob/main/CHANGELOG.md) for more details.
New in v1.0
- New runtime configuration: * The planet position, and generic Solar-system position calculator functions can be set at runtime, and users can provide their own custom implementations, e.g. to read ephemeris data, such as from a JPL `.bsp` file. * If CIO locations vs GCRS are important to the user, the user may call `set_cio_locator_file()` at runtime to specify the location of the binary CIO interpolation table (e.g. `CIO_RA.TXT` or `cio_ra.bin`) to use, even if the library was compiled with the different default CIO locator path. * The default low-precision nutation calculator `nu2000k()` can be replaced by another suitable IAU 2006 nutation approximation. For example, the user may want to use the `iau2000b()` model or some custom algorithm instead. - New constants, and enums -- adding more specificity and transparency to option switches and physical units. - Many new functions to provide more coordinate transformations, inverse calculations, and more intuitive usage.New in v1.1
- New observing-frame based approach for calculations (`frames.c`). A `novas_frame` object uniquely defines both the place and time of observation, with a set of precalculated 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. - New `novas_timespec` structure for the self-contained definition of precise astronomical time (`timescale.c`). You can set the time to a JD date in the timescale of choice (UTC, UT1, GPS, TAI, TT, TCG, TDB, or TCB), or to a UNIX time. Once set, you can obtain an expression of that time in any timescale of choice. And, you can create a new time specification by incrementing an existing one, or measure precise time differences. - New coordinate reference systems `NOVAS_MOD` (Mean of Date) which includes precession but not nutation and `NOVAS_J2000` for the J2000 dynamical reference system. - New observer locations `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. - New set of built-in refraction models to use with the frame-based functions, including a radio refraction model based on the formulae by Berman & Rockwell 1976. Users 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 (observed vs astrometric elevations as the input) as needed.New in v1.2
- New functions to calculate and apply additional gravitational redshift corrections for light that originates near massive gravitating bodies (other than major planets, or Sun or Moon), or for observers located near massive gravitating bodies (other than the Sun and Earth). - [CALCEPH integration](#calceph-integration) to specify and use ephemeris data via the CALCEPH library for Solar-system sources in general, and for major planets specifically. - [NAIF CSPICE integration](#cspice-integration) to use the NAIF CSPICE library for all Solar-system sources, or for major planets or other bodies only. - Added support for using orbital elements. `object.type` can now be set to `NOVAS_ORBITAL_OBJECT`, whose orbit can be defined by `novas_orbital`, relative to a `novas_orbital_system`. 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 Planet Center](https://www.minorplanetcenter.net/iau/mpc.html) (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. - Added `NOVAS_EMB` (Earth-Moon Barycenter) and `NOVAS_PLUTO_BARYCENTER` to `enum novas_planets` to distinguish from the corresponding planet centers in calculations. - Added more physical unit constants to `novas.h`.New in v1.3
- New functions to aid the conversion of LSR velocities to SSB-based velocities, and vice-versa. (Super)NOVAS always defines catalog sources with SSB-based radial velocities, but some catalogs provide LSR velocities. - New functions to convert dates/times and angles to/from their string representations. - New functions to convert between Julian Days and calendar dates in the calendar of choice (astronomical, Gregorian, or Roman/Julian). - New convenience functions for oft-used astronomical calculations, such as rise/set times, LST, parallactic angle (a.k.a. Vertical Position Angle), heliocentric distance, illumination fraction, or incident solar power, Sun and Moon angles, and much more. - New functions and data structures provide second order Taylor series expansion of the apparent horizontal or equatorial positions, distances, and redshifts for sources. These values, including rates and accelerations, can be directly useful for controlling telescope drives in horizontal or equatorial mounts to track sources. You can also use them to obtain instantaneous projected (extrapolated) positions at low computational cost.New in v1.4
- Updated nutation model from IAU2000 to IAU2006 (P03) model, by applying scaling factors (Capitaine et al. 2005) to match the IAU2006 precession model that was already implemented in NOVAS. - Approximate Keplerian orbital models for the major planets (Standish & Williams, 1992), EMB, and the Moon (Chapront et al. 2002), for when arcmin-scale accuracy is sufficient (e.g. rise or set times, approximate sky positions). - Moon phase calculator functions, based on above orbital modeling. - Improved support for expressing and using coordinates in TIRS (Terrestrial Intermediate Reference System) and ITRS (International Terrestrial Reference System). - Improvements to atmospheric refraction modeling.New in v1.5
- Simpler functions to calculate Greenwich Mean and Apparent Sidereal Time (GMST / GAST). - Functions to calculate corrections to the Earth orientation parameters published by IERS, to include the effect of libration and ocean tides. Such corrections are necessary to include if needing or using ITRS / TIRS coordinates with accuracy below the milliarcsecond (mas) level. - New functions to simplify the handling ground-based observing locations (GPS vs ITRF vs Cartesian locations), including setting default weather values, at least until actual values are specified if needed, and conversion between geodetic (longitude, latitude, altitude) and geocentric Cartesian (x, y, z) site coordinates using the reference ellipsoid of choice (e.g. GRS80 or WGS84). - Transformations of site coordinates and Earth orientation parameters between different ITRF realizations (e.g. ITRF2000 snd ITRF2014). - Functions to calculate the rate at which an observer's clock ticks differently from a standard astronomical timescale, due to the gravitational potential around the observer and the observer's movement. - No longer using a CIO vs GCRS locator data file in any way, thus eliminating an annoying external soft dependency. This change has absolutely zero effect on backward compatibility and functionality. - GNU `make` build support for Mac OS X and FreeBSD (co-authored with Kiran Shila). - CMake build support (co-authored with Kiran Shila).
- Changed to [support for calculations in parallel threads](#multi-threading) by making cached results thread-local.
This works using the C11 standard `_Thread_local`, or the C23 `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.
- __SuperNOVAS__ functions take `enum`s as their option arguments instead of raw integers. The enums allow for some
compiler checking (e.g. using the wrong enum), 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.
- All __SuperNOVAS__ functions check for the basic validity of the supplied arguments (Such as NULL pointers, or
empty strings) and will return -1 (with `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).
- All erroneous returns now set `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.
- __SuperNOVAS__ prototypes declare function pointer arguments as `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.
- Many __SuperNOVAS__ functions allow `NULL` arguments, both for optional input values as well as outputs that are
not required (see the [API Documentation](https://smithsonian.github.io/SuperNOVAS/doc/html/) for specifics).
This eliminates the need to declare dummy variables in your application code.
- Many output values supplied via pointers are set to clearly invalid values in case of erroneous returns, such as
`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.)
- All __SuperNOVAS__ functions that take an input vector to produce an output vector allow the output vector argument
be the same as the input vector argument. For example, `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.
- Catalog names can be up to 6 bytes (including termination), up from 4 in NOVAS C, while keeping `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.
- Changed `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.
- More efficient paging (cache management) for `cio_array()`, including I/O error checking.
- IAU 2000A nutation model uses higher-order Delaunay arguments provided by `fund_args()`, instead of the linear
model in NOVAS C 3.1.
- IAU 2000 nutation made a bit faster, reducing the the number of floating-point multiplications necessary by
skipping terms that do not contribute. Its coefficients are also packed more frugally in memory, resulting in a
smaller footprint.
- Changed the standard atmospheric model for (optical) refraction calculation to include a simple model for the
annual average temperature at the site (based on latitude and elevation). This results is a slightly more educated
guess of the actual refraction than the global fixed temperature of 10 °C assumed by NOVAS C 3.1 regardless of
observing location.
- [__v1.1__] Improved the precision of some calculations, like `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.
- [__v1.1__] `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.
- [__v1.1__] `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).
- [__v1.1.1__] For major planets (and Sun and Moon) `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 from
the source.
- [__v1.3__] In reduced accuracy mode apply gravitational deflection for the Sun only. In prior versions, deflection
corrections were applied for Earth too. However, these are below the mas-level accuracy promised in reduced
accuracy mode, and without it, the calculations for `place()` and `novas_sky_pos()` are significantly faster.
- [__v1.3__] `julian_date()` and `cal_date()` now use astronomical calendar dates instead of the fixed Gregorian
dates of before. Astronomical dates are Julian/Roman calendar dates prior to the Gregorian calendar reform of 1582.
- [__v1.3__] Use C99 `restrict` keyword to prevent pointer argument aliasing as appropriate.
- [__v1.4.2__] Nutation models have been upgraded from the original IAU2000 model to IAU2006 (i.e. IAU2000A R06),
making them dynamically consistent with the implemented IAU2006 (P03) precession model.
- [__v1.5__] Faster IAU2000A (R06) nutation series and `ee_ct()` calculations, with a ~2x speedup.
- [__v1.5__] Weaned off using CIO locator file internally (but still allowing users to access them if they want to).
-----------------------------------------------------------------------------
## Release schedule
A predictable release schedule and process can help manage expectations and reduce stress on adopters and developers
alike.
__SuperNOVAS__ will try to 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.
New features are generally reserved for the feature releases (e.g. __1.x.0__ version bumps), 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](https://github.com/Smithsonian/SuperNOVAS/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) 2025 Attila Kovács
SuperNOVAS-1.5.0/benchmark/ 0000775 0000000 0000000 00000000000 15076473367 0015376 5 ustar 00root root 0000000 0000000 SuperNOVAS-1.5.0/benchmark/.gitignore 0000664 0000000 0000000 00000000026 15076473367 0017364 0 ustar 00root root 0000000 0000000 benchmark*
!*.c
!*.py
SuperNOVAS-1.5.0/benchmark/CMakeLists.txt 0000664 0000000 0000000 00000001636 15076473367 0020144 0 ustar 00root root 0000000 0000000 # Additional CMake configuration file for building the benchmarking programs
# of the SuperNOVAS library.
#
# To invoke simply configure the cmake build in the supernovas directory with
# the -DBUILD_BENCHMARK=ON option.
#
# Author: Attila Kovacs
# List of benchmarking programs to build
set(BENCHMARK_PROGRAMS
benchmark-nutation
benchmark-place
)
include_directories(${supernovas_INCLUDE_DIRS})
# Build each example
foreach(BENCHMARK ${BENCHMARK_PROGRAMS})
set(BENCHMARK_SOURCE ${BENCHMARK}.c)
if(EXISTS ${CMAKE_CURRENT_SOURCE_DIR}/${BENCHMARK_SOURCE})
add_executable(${BENCHMARK} ${BENCHMARK_SOURCE})
# Link against the supernovas library
target_link_libraries(${BENCHMARK} PRIVATE
supernovas::core
${MATH}
)
else()
message(WARNING "Source file ${BENCHMARK_SOURCE} not found - ${BENCHMARK} will not be built")
endif()
endforeach()
SuperNOVAS-1.5.0/benchmark/Makefile 0000664 0000000 0000000 00000002001 15076473367 0017027 0 ustar 00root root 0000000 0000000 # Part of SuperNOVAS
#
# Generates headless README.md and HTML documentation
#
# Author: Attila Kovacs
# Use the definitions project definitions
include ../config.mk
BENCHMARKS = benchmark-nutation benchmark-place
CPPFLAGS += -I../include
LDFLAGS += -L../$(LIB) -lsupernovas
.PHONY: all
all: build run
.PHONY: build
build: $(BENCHMARKS)
.PHONY: run
run: build
@for prog in $(BENCHMARKS) ; do $(LIB_PATH_VAR)=../$(LIB) ./$${prog} ; done
.PHONY: clean
clean:
.PHONY: distclean
distclean: clean
@rm -f $(BENCHMARKS)
benchmark-%: benchmark-%.c
$(CC) -o $@ $(CPPFLAGS) $(CFLAGS) $< $(LDFLAGS)
# Built-in help screen for `make help`
.PHONY: help
help:
@echo
@echo "Syntax: make [target]"
@echo
@echo "The following targets are available:"
@echo
@echo " all (default) builds and runs benchmarks."
@echo " build Builds benchmarks."
@echo " run Runs benchmarks."
@echo " clean Removes intermediate products."
@echo " distclean Deletes all generated files."
@echo
SuperNOVAS-1.5.0/benchmark/benchmark-astropy.py 0000664 0000000 0000000 00000005054 15076473367 0021405 0 ustar 00root root 0000000 0000000 # astropy benchmark for position calculations, matching the SuperNOVAS
# benchmarks in `benchmark-place.c`
#
# It calculates CIRS positions for an Earth based observer for a number of
# random sidereal sources. The first benchmark calculates positions for a
# fixed observing frame (time and observer location), while the second test
# calculates positions for individual observing frames.
#
# Author: Attila Kovacs
# Date: 2025-01-25
# ----------------------------------------------------------------------------
import astropy
import random
import time
import astropy.units as u
from astropy.coordinates import SkyCoord, EarthLocation, Longitude, Latitude, CIRS
# ----------------------------------------------------------------------------
# main program entry point
# Number of sources / iterations to test with
N = 300
# ----------------------------------------------------------------------------
# Set up a source 'catalog' with the desired number of sources and random
# properties
sources = []
for i in range(0, N):
# Generate random source properties
ra = Longitude(360.0 * (random.random() - 0.5) * u.degree)
dec = Latitude(180.0 * (random.random() - 0.5) * u.degree)
d = (1.0 + 1000.0 * random.random()) * u.pc
pmra = 100.0 * (random.random() - 0.5) * u.mas / u.yr
pmdec = 100.0 * (random.random() - 0.5) * u.mas / u.yr
rv = 1000.0 * (random.random() - 0.5) * u.km / u.s
sc = SkyCoord(ra, dec, d, pm_ra_cosdec=pmra, pm_dec=pmdec, radial_velocity=rv)
sources.append(sc)
# ----------------------------------------------------------------------------
# Benchmark 1: calculating positions in the same frame
# Set up a fixed observing frame...
tim = astropy.time.Time("2025-01-25T15:32:00")
loc = EarthLocation.from_geodetic(lon=Longitude(6.16 * u.degree), lat=Latitude(42.7 * u.degree), height=2500.0)
frame = CIRS(obstime=tim, location=loc)
start = time.time()
for source in sources :
source.transform_to(frame)
end = time.time()
print("same frame " + str(N / (end - start)))
# ----------------------------------------------------------------------------
# Benchmark 2: calculating positions in individual frames
start = time.time()
for source in sources :
tim = astropy.time.Time("2025-01-25T15:32:00") - 365.0 * random.random() * u.day
lon = Longitude(360.0 * random.random() * u.degree)
lat = Latitude(180.0 * (random.random() - 0.5) * u.degree)
loc = EarthLocation.from_geodetic(lon, lat, height=2500.0)
frame = CIRS(obstime=tim, location=loc)
source.transform_to(frame)
end = time.time()
print("individual frame " + str(N / (end - start)))
SuperNOVAS-1.5.0/benchmark/benchmark-nutation.c 0000664 0000000 0000000 00000004104 15076473367 0021332 0 ustar 00root root 0000000 0000000 /**
* @file
*
* @date Created on Jan 26, 2025
* @author Attila Kovacs
*/
/**
* @file
*
* @date Created on Jan 24, 2025
* @author Attila Kovacs
*/
#define _POSIX_C_SOURCE 199309L ///< for clock_gettime()
#include