From 70edc9a86108e9ef0b713ece034992a22e97be0e Mon Sep 17 00:00:00 2001 From: github-actions Date: Thu, 16 Jan 2025 05:20:46 +0000 Subject: [PATCH] [automated site update] --- apidoc/html/index.html | 83 +++++++++--------- apidoc/html/md_CHANGELOG.html | 41 +++++---- apidoc/html/md_CONTRIBUTING.html | 2 +- apidoc/html/md_LEGACY.html | 20 ++--- apidoc/html/navtreedata.js | 145 ++++++++++++++++--------------- apidoc/html/navtreeindex0.js | 140 ++++++++++++++--------------- apidoc/html/navtreeindex1.js | 4 +- apidoc/html/navtreeindex2.js | 4 +- apidoc/html/navtreeindex3.js | 1 + apidoc/html/search/all_0.js | 20 ++--- apidoc/html/search/all_1.js | 20 ++--- apidoc/html/search/all_10.js | 16 ++-- apidoc/html/search/all_11.js | 10 +-- apidoc/html/search/all_12.js | 14 +-- apidoc/html/search/all_13.js | 34 ++++---- apidoc/html/search/all_14.js | 26 +++--- apidoc/html/search/all_15.js | 16 ++-- apidoc/html/search/all_16.js | 48 +++++----- apidoc/html/search/all_17.js | 36 ++++---- apidoc/html/search/all_18.js | 11 +-- apidoc/html/search/all_19.js | 8 +- apidoc/html/search/all_1a.js | 6 +- apidoc/html/search/all_1c.js | 2 +- apidoc/html/search/all_2.js | 16 ++-- apidoc/html/search/all_3.js | 4 +- apidoc/html/search/all_5.js | 48 +++++----- apidoc/html/search/all_6.js | 8 +- apidoc/html/search/all_7.js | 30 +++---- apidoc/html/search/all_8.js | 10 +-- apidoc/html/search/all_9.js | 16 ++-- apidoc/html/search/all_a.js | 20 ++--- apidoc/html/search/all_d.js | 18 ++-- apidoc/html/search/all_e.js | 4 +- apidoc/html/toc.xml | 139 ++++++++++++++--------------- apidoc/man/man3/md_CHANGELOG.3 | 3 + doc/CHANGELOG.md | 6 ++ doc/README.md | 2 + 37 files changed, 525 insertions(+), 506 deletions(-) diff --git a/apidoc/html/index.html b/apidoc/html/index.html index 69e6c6ec..12dc20eb 100644 --- a/apidoc/html/index.html +++ b/apidoc/html/index.html @@ -114,7 +114,8 @@
SuperNOVAS
-

The NOVAS C astrometry library, made better.

+

DOI

+

The NOVAS C astrometry library, made better.

  • API documentation.
  • SuperNOVAS pages on github.io
    • @@ -122,7 +123,7 @@

    SuperNOVAS is a C/C++ astronomy software library, providing high-precision astrometry such as one might need for running an observatory or a precise planetarium program. It is a fork of the Naval Observatory Vector Astrometry Software (NOVAS) C version 3.1, providing bug fixes, tons of extra features, while making it easier (and safer) to use also.

    SuperNOVAS is entirely free to use without licensing restrictions. Its source code is compatible with the C99 standard, and hence should be suitable for old and new platforms alike. It is light-weight and easy to use, with full support for the IAU 2000/2006 standards for sub-microarcsecond position calculations.

    This document has been updated for the v1.2 and later releases.

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    Table of Contents

    -

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    Introduction

    SuperNOVAS is a fork of the The Naval Observatory Vector Astrometry Software (NOVAS).

    The primary goal of SuperNOVAS is to improve on the stock NOVAS C library via:

    @@ -157,7 +158,7 @@

    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 at the Center for Astrophysics | Harvard & Smithsonian, and it is available through the Smithsonian/SuperNOVAS repository on GitHub.

    Outside contributions are very welcome. See how you can contribute to make SuperNOVAS even better.

    -

    +

    Related links

    • NOVAS home page at the US Naval Observatory.
      • @@ -168,7 +169,7 @@

    -

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    Fixed NOVAS C 3.1 issues

    The SuperNOVAS library fixes a number of outstanding issues with NOVAS C 3.1. Here is a list of issues and fixes provided by SuperNOVAS over the upstream NOVAS C 3.1 code:

      @@ -188,7 +189,7 @@

    -

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    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.

    @@ -196,7 +197,7 @@

    This is because some function signatures have changed, e.g. to use an enum argument instead of the nondescript short int argument of NOVAS C 3.1, or because we added a return value to a function that was declared void in NOVAS C 3.1. We also changed the object structure to contain a long ID number instead of short to accommodate JPL NAIF codes, for which 16-bit storage is insufficient.

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    Building and installation

    The SuperNOVAS distribution contains a GNU Makefile, which is suitable for compiling the library (as well as local documentation, and tests, etc.) on POSIX systems such as Linux, BSD, MacOS X, or Cygwin or WSL. (At this point we do not provide a similar native build setup for Windows, but speak up if you would like to add it yourself!)

    Before compiling the library take a look a config.mk and edit it as necessary for your needs, or else define the necessary variables in the shell prior to invoking make. For example:

    @@ -230,7 +231,7 @@

    $ make DESTDIR="/tmp/stage" install

    -

    +

    Building your application with SuperNOVAS

    Provided you have installed the SuperNOVAS headers 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:

    myastroapp: myastroapp.c
    @@ -241,14 +242,14 @@

    If your application uses optional planet or ephemeris calculator modules, you may need to specify the appropriate optional shared library also:

    myastroapp: myastroapp.c
    $(CC) -o $@ $(CFLAGS) $^ -lm -lsupernovas -lsolsys-calceph
    -

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Legacy linking <tt>solarsystem()</tt> and <tt>readeph()</tt> modules

The NOVAS C way to handle planet or other ephemeris functions was to link particular modules to provide the solarsystem() / solarsystem_hp() and readeph() functions. This approach is discouraged in SuperNOVAS, since we now allow selecting different implementations at runtime, but the old way is supported for legacy applications, nevertheless.

To use your own existing default solarsystem() implementation in this way, you must build the library with DEFAULT_SOLSYS unset (or else set to 0) in config.mk (see section above), and your applications Makefile may contain something like:

myastroapp: myastroapp.c my_solsys.c
$(CC) -o $@ $(CFLAGS) $^ -lm -lsupernovas

The same principle applies to using your specific readeph() implementation (only with DEFAULT_READEPH being unset in config.mk).

-

+

Legacy modules: a better way...

Note, a better way to recycle your old planet and ephemeris calculator modules may be to rename solarsystem() / solarsystem_hp() functions therein to e.g. my_planet_calculator() / my_planet_calculator_hp() and then in your application can specify these functions as the provider at runtime:

set_planet_calculator(my_planet_calculator);
@@ -263,7 +264,7 @@

While it requires some minimal changes to the old code, the advantage of this preferred approach is (a) that you do not need to re-build the library with the DEFAULT_SOLSYS and DEFAULT_READEPH options disabled, and (b) you can switch between different planet and ephemeris calculator functions at will, during runtime.

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Example usage

SuperNOVAS v1.1 has introduced a new, more intuitive, more elegant, and more efficient approach for calculating astrometric positions of celestial objects. The guide below is geared towards this new method. However, the original NOVAS C approach remains viable also (albeit often less efficient). You may find an equivalent example usage showcasing the original NOVAS method in LEGACY.md.

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Note on alternative methodologies

The IAU 2000 and 2006 resolutions have completely overhauled the system of astronomical coordinate transformations to enable higher precision astrometry. (Super)NOVAS supports coordinate calculations both in the old (pre IAU 2000) ways, and in the new IAU standard method. Here is an overview of how the old and new methods define some of the terms differently:

@@ -305,10 +306,10 @@

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. Dotted arrows indicate possible loss of precision due to the inadequacy of the old precession-nutation (Lieske et al. 1977) model.

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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.

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Specify the object of interest

First, you must provide the coordinates (which may include proper motion and parallax). Let's assume we pick a star for which we have B1950 (i.e. FK4) coordinates:

cat_entry star; // Structure to contain information on sidereal source
@@ -342,7 +343,7 @@

// 12h29m6.6997s +2d3m8.598s (ICRS) z=0.158339
make_redshifted_object("3c273", 12.4851944, 2.0523883, 0.158339, &quasar);
make_redshifted_object
int make_redshifted_object(const char *name, double ra, double dec, double z, object *source)
Definition super.c:1142
-

+

Specify the observer location

Next, we define the location where we observe from. Here we can (but don't have to) specify local weather parameters (temperature and pressure) also for refraction correction later (in this example, we'll skip the weather):

observer obs; // Structure to contain observer location
@@ -353,7 +354,7 @@

make_observer_on_surface
int make_observer_on_surface(double latitude, double longitude, double height, double temperature, double pressure, observer *obs)
Definition novas.c:6959
observer
Definition novas.h:999

Similarly, you can also specify observers in Earth orbit, in Sun orbit, at the geocenter, or at the Solar-system barycenter.

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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. Let's assume 37 leap seconds, and DUT1 = 0.114, then we can set the time of observation, for example, using the current UNIX time:

novas_timespec obs_time; // Structure that will define astrometric time
@@ -378,7 +379,7 @@

novas_set_split_time(NOVAS_TAI, ijd_tai, fjd_tai, 37, 0.114, &obs_time);
novas_set_split_time
int novas_set_split_time(enum novas_timescale timescale, long ijd, double fjd, int leap, double dut1, novas_timespec *time)
Definition timescale.c:114
-

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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:

novas_frame obs_frame; // Structure that will define the observing frame
@@ -393,7 +394,7 @@

Here dx and dy are small diurnal (sub-arcsec level) corrections to Earth orientation, which are published in the IERS Bulletins. They are needed when converting positions from the celestial CIRS frame to the Earth-fixed ITRS frame. You may ignore these and set zeroes if sub-arcsecond precision is not required.

The advantage of using the observing frame, is that it enables very fast position calculations for multiple objects in that frame. So, if you need to calculate positions for thousands of sources for the same observer and time, it will be significantly faster than using the low-level NOVAS C routines instead. You can create derivative frames for different observer locations, if need be, via novas_change_observer().

Note that without a proper ephemeris provider for the major planets, you are invariably restricted to working with NOVAS_REDUCED_ACCURACY frames, providing milliarcsecond precision only. To create NOVAS_FULL_ACCURACY frames, with sub-μas precision, you will you will need a high-precision ephemeris provider for the major planets (beyond the low-precision Earth and Sun calculator included by default), to account for gravitational bending around massive planets. Without it, μas accuracy cannot be ensured, in general. Therefore, attempting to construct high-accuracy frames without an appropriate high-precision ephemeris provider will result in an error from the requisite ephemeris() call.

-

+

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. You can calculate an apparent location in the coordinate system of choice (ICRS/GCRS, CIRS, J2000, MOD, or TOD):

sky_pos apparent; // Structure containing the precise observed position
@@ -404,7 +405,7 @@

sky_pos
Definition novas.h:1019

Apart from providing precise apparent R.A. and declination coordinates, the sky_pos structure also provides the x,y,z unit vector pointing in the observed direction of the source (in the designated coordinate system). We also get radial velocity (for spectroscopy), and apparent distance for Solar-system bodies (e.g. for apparent-to-physical size conversion).

Note, that if you want geometric positions (and/or velocities) instead, without aberration and gravitational deflection, you might use novas_geom_posvel() instead. And regardless, which function you use you can always easily and efficiently change the coordinate system in which your results are expressed by creating an appropriate transform via novas_make_transform() and then using novas_transform_vector() or novas_transform_skypos().

-

+

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!) as:

double az, el; // [deg] local azimuth and elevation angles to populate
@@ -417,7 +418,7 @@

sky_pos::dec
double dec
[deg] apparent, topocentric, or astrometric declination (degrees)
Definition novas.h:1022

Above we converted the apparent coordinates, assuming they were calculated in CIRS, to refracted azimuth and elevation coordinates at the observing location, using the novas_standard_refraction() function to provide a suitable refraction correction. We could have used novas_optical_refraction() instead to use the weather data embedded in the frame's observer structure, or some user-defined refraction model, or else NULL to calculate unrefracted elevation angles.

-

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Calculating positions for a Solar-system source

Solar-system sources work similarly to the above with a few important differences.

First, You will have to provide one or more functions to obtain the barycentric ICRS positions for your Solar-system source(s) of interest for the specific Barycentric Dynamical Time (TDB) of observation. See section on integrating External Solar-system ephemeris data or services with SuperNOVAS. You can specify the functions that will handle the respective ephemeris data at runtime before making the NOVAS calls that need them, e.g.:

@@ -477,7 +478,7 @@

NOVAS_TOD
@ NOVAS_TOD
Definition novas.h:386

-

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Tips and tricks

-

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Reduced accuracy shortcuts

When one does not need positions at the microarcsecond level, some shortcuts can be made to the recipe above:

-

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Multi-threaded calculations

Some of the calculations involved can be expensive from a computational perspective. For the most typical use case however, NOVAS (and SuperNOVAS) has a trick up its sleeve: it caches the last result of intensive calculations so they may be re-used if the call is made with the same environmental parameters again (such as JD time and accuracy).

A direct consequence of the caching of results in NOVAS is that calculations are generally not thread-safe as implemented by the original NOVAS C 3.1 library. One thread may be in the process of returning cached values for one set of input parameters while, at the same time, another thread is saving cached values for a different set of parameters. Thus, when running calculations in more than one thread, the results returned may at times be incorrect, or more precisely they may not correspond to the requested input parameters.

@@ -504,7 +505,7 @@

  • or else, set the appropriate non-standard keyword to use for declaring thread-local variables for your compiler in config.mk or in your equivalent build setup.

    • -

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    Physical units

    The NOVAS API has been using conventional units (e.g. AU, km, day, deg, h) typically for its parameters and return values alike. Hence, SuperNOVAS follows the same conventions for its added functions and data structures also. However, when interfacing SuperNOVAS with other programs, libraries, or data files, it is often necessary to use quantities that are expressed in different units, such as SI or CGS. To facilitate such conversions, novas.h provides a set of unit constants, which can be used for converting to/from SI units (and radians). For example, novas.h contains the following definitions:

    @@ -540,7 +541,7 @@

    NOVAS_AU
    #define NOVAS_AU
    Definition novas.h:144

    -

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    Notes on precision

    Many of the (Super)NOVAS functions take an accuracy argument, which determines to what precision quantities are calculated. The argument can have one of two values, which correspond to typical precisions around:

    @@ -552,7 +553,7 @@

    NOVAS_FULL_ACCURACY below 1 micro-arcsecond (μas)

    Note, that some functions will not support full accuracy calculations, unless you have provided a high-precision ephemeris provider for the major planets (and any Solar-system bodies of interest), which does not come with SuperNOVAS out of the box. In the absense of a suitable high-precision ephemeris provider, some functions might return an error if called with NOVAS_FULL_ACCURACY.

    -

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    Prerequisites to precise results

    The SuperNOVAS library is in principle capable of calculating positions to sub-microarcsecond, and velocities to mm/s, precision for all types of celestial sources. However, there are certain prerequisites and practical considerations before that level of accuracy is reached.

      @@ -566,14 +567,14 @@

    -

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    SuperNOVAS specific features

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    Newly added functionality

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    Added in v1.1

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    Added in v1.2

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    Refinements to the NOVAS C API

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    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. Given the NOVAS C heritage, and some added SuperNOVAS flexibility in this area, you have several options for going about it. These are listed from the most practical (and preferred) to the least so (the old ways).

    NASA/JPL provides generic ephemerides for the major planets, satellites thereof, the 300 largest asteroids, the Lagrange points, and some Earth orbiting stations. For example, DE440 covers the major planets, and the Sun, Moon, and barycenters for times between 1550 AD and 2650 AD. Or, you can use the JPL HORIZONS system (via the commnad-line / telnet or API interfaces) to generate custom ephemerides (SPK/BSP) for just about all known solar systems bodies, down to the tiniest rocks.

    @@ -678,7 +679,7 @@

  • Legacy linking of custom ephemeris functions

    • -

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    Optional CALCEPH integration

    The 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. Depending on the build target, it will build libsolsys-calceph.so[.1] (target shared) or libsolsys-calceph.a (target static) libraries or solsys-calceph.o (target solsys), which provide the novas_use_calceph() and novas_use_calceph_planets(), and novas_calceph_use_ids() functions.

    @@ -707,7 +708,7 @@

    novas_use_calceph_planets
    int novas_use_calceph_planets(t_calcephbin *eph)
    Definition solsys-calceph.c:420

    All modern JPL (SPK) ephemeris files should work with the solsys-calceph plugin. When linking your application, add -lsolsys-calceph to your link flags (or else link with solsys-calceph.o). That's all there is to it.

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    Optional NAIF CSPICE toolkit integration

    The NAIF CSPICE Toolkit is the canonical standard library for JPL ephemeris files from C/C++. As of version 1.2, we provide optional support for interfacing SuperNOVAS with CSPICE for handling Solar-system objects.

    Prior to building SuperNOVAS simply set CSPICE_SUPPORT to 1 in config.mk or in your environment. Depending on the build target, it will build libsolsys-cspice.so[.1] (target shared) or libsolsys-cspice.a (target static) libraries or solsys-cspice.o (target solsys), which provide the novas_use_cspice(), novas_use_cspice_planets(), and novas_use_cspice_ephem() functions to enable CSPICE for providing data for all Solar-system sources, or for major planets only, or for other bodies only, respectively. You can also manage the active kernels with the cspice_add_kernel() and cspice_remove_kernel() functions.

    @@ -736,7 +737,7 @@

    cspice_add_kernel
    int cspice_add_kernel(const char *filename)
    Definition solsys-cspice.c:127

    All JPL ephemeris data will work with the solsys-cspice plugin. When linking your application, add -lsolsys-cspice to your link flags (or else link with solsys-cspice.o). That's all there is to it.

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    +

    Universal ephemeris data / service integration

    Possibly the most universal way to integrate ephemeris data with SuperNOVAS is to write your own novas_ephem_provider, e.g.:

    int my_ephem_reader(const char *name, long id, double jd_tdb_high, double jd_tdb_low,
    @@ -755,10 +756,10 @@

    planet_ephem_provider_hp
    short planet_ephem_provider_hp(const double jd_tdb[2], enum novas_planet body, enum novas_origin origin, double *position, double *velocity)
    Definition solsys-ephem.c:46

    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.

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    Legacy support for (older) JPL major planet ephemerides

    If you only need support for major planets, you may be able to use one of the modules included with the distribution. The legacy NOVAS modules solsys1.c and solsys2.c provide built-in support to older JPL ephemerides (DE200 to DE421), either via the eph_manager interface of solsys1.c or via the FORTRAN pleph interface with solsys2.c.

    -

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    Planets via <tt>eph_manager</tt>

    To use the eph_manager interface for planet 1997 JPL planet ephemeris (DE200 through DE421), you must either build SuperNOVAS with BUILTIN_SOLSYS1 = 1 in config.mk, or else link your application with solsys1.c and eph_manager.c from SuperNOVAS explicitly. If you want eph_manager to be your default ephemeris provider (the old way) you might also want to set DEFAULT_SOLSYS = 1 in config.mk. Otherwise, your application should set eph_manager as your planetary ephemeris provider at runtime via:

    set_planet_provider(planet_eph_manager);
    @@ -776,7 +777,7 @@

    ephem_close
    short ephem_close(void)
    Definition eph_manager.c:224

    Note, that at any given time eph_manager can have only one ephemeris data file opened. You cannot use it to retrieve data from multiple ephemeris input files at the same time. (But you can with CALCEPH or the CSPICE toolkit, either of which you can interface as discussed further above!)

    That's all, except the warning that this method will not work with newer JPL ephemeris data, beyond DE421.

    -

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    Planets via JPL's <tt>pleph</tt> FORTRAN interface

    To interface eith the JPL PLEPH library (FORTRAN) for planet ephemerides, you must either build SuperNOVAS with BUILTIN_SOLSYS2 = 1 in config.mk, or else link your application with solsys2.c and your appropriately modified jplint.f (from the examples sub-directory) explicitly, together with the JPL PLEPH library. If you want this to be your default ephemeris provider (the old way) you might also want to set DEFAULT_SOLSYS = 2 in config.mk. Otherwise, your application should set your planetary ephemeris provider at runtime via:

    set_planet_provider(planet_jplint);
    @@ -785,14 +786,14 @@

    planet_jplint
    short planet_jplint(double jd_tdb, enum novas_planet body, enum novas_origin origin, double *position, double *velocity)
    Definition solsys2.c:87

    Integrating JPL ephemeris data this way can be arduous. You will need to compile and link FORTRAN with C (not the end of the world), but you may also have to modify jplint.f (providing the intermediate FORTRAN jplint_() / jplihp_() interfaces to pleph_()) to work with the version of pleph.f that you will be using. Unless you already have code that relies on this method, you are probably better off choosing one of the other ways for integrating planetary ephemeris data with SuperNOVAS.

    -

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    Legacy linking of custom ephemeris functions

    Finally, if none of the above is appealing, and you are fond of the old ways, you may compile SuperNOVAS with the DEFAULT_SOLSYS option disabled (commented, removed, or else set to 0), and then link your own implementation of solarsystem() and solarsystem_hp() calls with your application.

    For Solar-system objects other than the major planets, you may also provide your own readeph() implementation. (In this case you will want to set DEFAULT_READEPH in config.mk to specify your source code for that function before building the SuperNOVAS library, or else disable that option entirely (e.g. by commenting or removing it), and link your application explicitly with your readeph() implementation.

    The downside of this approach is that your SuperNOVAS library will not be usable without invariably providing a solarsystem() / solarsystem_hp() and/or readeph() implementations for every application that you will want to use SuperNOVAS with. This is why the runtime configuration of the ephemeris provider functions is the best and most generic way to add your preferred implementations while also providing some minimum default implementations for other users of the library, who may not need your ephemeris service, or have no need for planet data beyond the approximate positions for the Earth and Sun.

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    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:

    @@ -808,7 +809,7 @@

    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.

    -

    +

    Release schedule

    A predictable release schedule and process can help manage expectations and reduce stress on adopters and developers alike.

    Releases of the library shall follow a quarterly release schedule. You may expect upcoming releases to be published around February 1, May 1, August 1, and/or November 1 each year, on an as-needed basis. That means that if there are outstanding bugs, or new pull requests (PRs), you may expect a release that addresses these in the upcoming quarter. The dates are placeholders only, with no guarantee that a new release will actually be available every quarter. If nothing of note comes up, a potential release date may pass without a release being published.

    diff --git a/apidoc/html/md_CHANGELOG.html b/apidoc/html/md_CHANGELOG.html index f631f2d7..c52c3e77 100644 --- a/apidoc/html/md_CHANGELOG.html +++ b/apidoc/html/md_CHANGELOG.html @@ -117,16 +117,19 @@

    All notable changes to the SuperNOVAS library will be documented in this file.

    The format is based on Keep a Changelog, and this project adheres to Semantic Versioning.

    +[Unreleased]

    +

    Upcoming bug fix release, targeted for 1 May 2025.

    +

    [1.2.0] - 2025-01-15

    Feature release. New easy to use adapter modules for CALCEPH or the NAIF CSPICE Toolkit to provide precise positions for Solar-system sources. Also, added support for Keplerian orbitals, such as the ones published by the IAU Minor Planet Center (MPC) for asteroids, comets, and Near-Earth-Objects (NEOs). And, many more fixes and improvements.

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    Fixed

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    [1.1.1] - 2024-10-28

    Bug fix release. Nothing too scary, mainly just a collection of smaller fixes and improvements.

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    [1.1.0] - 2024-08-04

    Feature release. Introducing a more efficient and elegant approach to position and velocity calculations using observer frames; versatile handling of astronomical timescales; and support for further observer locations, coordinate reference systems, and atmospheric refraction models. The release also fixes a number of bugs, of varying severity, which affected prior SuperNOVAS releases.

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    Fixed

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    [1.0.1] - 2024-05-13

    Bug fix release with minor changes.

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    [1.0.0] - 2024-03-01

    This is the initial release of the SuperNOVAS library. Changes are indicated w.r.t. the upstream NOVAS C 3.1 library from which SuperNOVAS is forked from.

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    Fixed

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    The SuperNOVAS library is for everyone. And, it is developers like you who can make it better. Whether there is a nagging issue you would like to fix, or a new feature you'd like to see, you can make a difference yourself. Make this project a little bit your own, by submitting pull requests with fixes and enhancement. When you are ready, here are the typical steps for contributing to the project:

    1. Old or new Issue? Whether you just found a bug, or you are missing a much needed feature, start by checking open (and closed) Issues. If an existing issue seems like a good match to yours, feel free to speak up, comment, or to offer help in resolving it. If you find no issues that match, go ahead and create a new one.
      2. diff --git a/apidoc/html/md_LEGACY.html b/apidoc/html/md_LEGACY.html index 8597b18c..a639ee0c 100644 --- a/apidoc/html/md_LEGACY.html +++ b/apidoc/html/md_LEGACY.html @@ -114,16 +114,16 @@
      Astrometric Positions the Old Way
    -

    As of version 1.1, the SuperNOVAS library offers a new, more versatile, more intuitive, and more efficient way to calculate the astrometric positions (and velocities) of celestial sources, via observing frames (see README.md). However the old approach of the NOVAS C library remain viable also. This document demonstrates calculating the astrometric places of sources the old way, without using the observing frames approach that is now preferred in SuperNOVAS.

    +

    As of version 1.1, the SuperNOVAS library offers a new, more versatile, more intuitive, and more efficient way to calculate the astrometric positions (and velocities) of celestial sources, via observing frames (see README.md). However the old approach of the NOVAS C library remain viable also. This document demonstrates calculating the astrometric places of sources the old way, without using the observing frames approach that is now preferred in SuperNOVAS.

    -

    +

    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

    First, you must provide the coordinates (which may include proper motion and parallax). Let's assume we pick a star for which we have B1950 (i.e. FK4) coordinates:

    cat_entry source; // Structure to contain information on sidereal source
    @@ -145,7 +145,7 @@

    CHANGE_J2000_TO_ICRS
    @ CHANGE_J2000_TO_ICRS
    Definition novas.h:570
    CHANGE_EPOCH
    @ CHANGE_EPOCH
    The combined equivalent of PROPER_MOTION and PRECESSION together.
    Definition novas.h:566

    (Naturally, you can skip the transformation steps above if you have defined your source in ICRS coordinates from the start.)

    -

    +

    Spefify the observer location

    Next, we define the location where we observe from. Here we can (but don't have to) specify local weather parameters (temperature and pressure) also for refraction correction later (in this example, we'll skip the weather):

    observer obs; // Structure to contain observer location
    @@ -155,7 +155,7 @@

    make_observer_on_surface(50.7374, 7.0982, 60.0, 0.0, 0.0, &obs);
    make_observer_on_surface
    int make_observer_on_surface(double latitude, double longitude, double height, double temperature, double pressure, observer *obs)
    Definition novas.c:6959
    observer
    Definition novas.h:999
    -

    +

    Specify the time of observation

    We also need to set the time of observation. Our clocks usually measure UTC, but for astrometry we usually need time measured based on Terrestrial Time (TT) or Barycentric Time (TDB) or UT1. For a ground-based observer, you will often have to provide NOVAS with the TT - UT1 time difference, which can be calculated from the current leap seconds and the UT1 - UTC time difference (a.k.a. DUT1):

    // The current value for the leap seconds (UTC - TAI)
    @@ -174,7 +174,7 @@

    julian_date
    double julian_date(short year, short month, short day, double hour)
    Definition novas.c:6591
    get_ut1_to_tt
    double get_ut1_to_tt(int leap_seconds, double dut1)
    Definition super.c:74
    get_utc_to_tt
    double get_utc_to_tt(int leap_seconds)
    Definition super.c:46
    -

    +

    Specify Earth orientation parameters

    Next, you may want to set the small diurnal (sub-arcsec level) corrections to Earth orientation, which are published in the IERS Bulletins. The obvious utility of these values comes later, when converting positions from the celestial CIRS frame to the Earth-fixed ITRS frame. Less obviously, however, it is also needed for calculating the CIO location for CIRS coordinates when a CIO locator file is not available, or for calculations sidereal time measures etc. Therefore, it's best to set the pole offsets early on:

    // Current polar offsets provided by the IERS Bulletins (in arcsec)
    @@ -184,7 +184,7 @@

    cel_pole(jd_tt, POLE_OFFSETS_X_Y, dx, dy);
    cel_pole
    short cel_pole(double jd_tt, enum novas_pole_offset_type type, double dpole1, double dpole2)
    Definition novas.c:3143
    POLE_OFFSETS_X_Y
    @ POLE_OFFSETS_X_Y
    Offsets are dx, dy pairs (IAU 2006 precession-nutation model)
    Definition novas.h:514
    -

    +

    Calculate apparent positions on sky

    Now we can calculate the precise apparent position (CIRS or TOD) of the source, such as it's right ascension (R.A.) and declination, and the equatorial x,y,z unit vector pointing in the direction of the source (in the requested coordinate system and for the specified observing location). We also get radial velocity (for spectroscopy), and distance (e.g. for apparent-to-physical size conversion):

    sky_pos pos; // We'll return the observable positions (in CIRS) in this structure
    @@ -203,7 +203,7 @@

    sky_pos
    Definition novas.h:1019

    The placement of the celestial target in the observer's frame includes appropriate aberration corrections for the observer's motion, as well as appropriate gravitational deflection corrections due to the Sun and Earth, and for other major gravitating solar system bodies (in full precision mode and if a suitable planet provider function is available).

    The calculated sky_pos structure contains all the information needed about the apparent position of the source at the given date/time of observation. We may use it to get true apparent R.A. and declination from it, or to calculate azimuth and elevation at the observing location. We'll consider these two cases separately below.

    -

    +

    A. True apparent R.A. and declination

    If you want to know the apparent R.A. and declination coordinates from the sky_pos structure you obtained, then you can follow with:

    double ra, dec; // [h, deg] We'll return the apparent R.A. [h] and declination [deg] in these
    @@ -216,7 +216,7 @@

    If, however, you calculated the position in CIRS with the more precise IAU 2006 methodology (as we did in the example above), you have one more step to go still. The CIRS equator is the true equator of date, however its origin (CIO) is not the true equinox of date. Thus, we must correct for the difference of the origins to get the true apparent R.A.:

    ra = cirs_to_app_ra(jd_tt, NOVAS_FULL_ACCURACY, ra);
    cirs_to_app_ra
    double cirs_to_app_ra(double jd_tt, enum novas_accuracy accuracy, double ra)
    Definition super.c:621
    -

    +

    B. Azimuth and elevation angles at the observing location

    If your goal is to calculate the astrometric azimuth and zenith distance (= 90° - elevation) angles of the source at the specified observing location (without refraction correction), you can proceed from the sky_pos data you obtained from place_star() as:

    double itrs[3]; // ITRS position vector of source to populate
    @@ -237,7 +237,7 @@

    NOVAS_STANDARD_ATMOSPHERE
    @ NOVAS_STANDARD_ATMOSPHERE
    Definition novas.h:478
    observer::on_surf
    on_surface on_surf
    Definition novas.h:1004

    -

    +

    Calculating positions for a Solar-system source

    Solar-system sources work similarly to the above with a few important differences.

    First, You will have to provide one or more functions to obtain the barycentric ICRS positions for your Solar-system source(s) of interest for the specific Barycentric Dynamical Time (TDB) of observation. See section on integrating External Solar-system ephemeris data or services with SuperNOVAS. You can specify the functions that will handle the respective ephemeris data at runtime before making the NOVAS calls that need them, e.g.:

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- - - - - - - - + + + + + + + + + - - - - - - - - - + + + + + + + + + - + - - - - + + + + - - + + - - - - + + + + - + - - - - - - - + + + + + + + - + - - + + - - - - + + + + + - - - + + + - - - - + + + + - - - - + + + + - - - - - + + + + + - - - - - - - - + + + + + + + + - + diff --git a/apidoc/man/man3/md_CHANGELOG.3 b/apidoc/man/man3/md_CHANGELOG.3 index 27cc8394..10c34ed6 100644 --- a/apidoc/man/man3/md_CHANGELOG.3 +++ b/apidoc/man/man3/md_CHANGELOG.3 @@ -7,6 +7,9 @@ md_CHANGELOG \- Changelog All notable changes to the \fCSuperNOVAS\fP library will be documented in this file\&. .PP The format is based on \fCKeep a Changelog\fP, and this project adheres to \fCSemantic Versioning\fP\&. +.SH "[Unreleased]" +.PP +Upcoming bug fix release, targeted for 1 May 2025\&. .SH "[1\&.2\&.0] - 2025-01-15" .PP Feature release\&. New easy to use adapter modules for CALCEPH or the NAIF CSPICE Toolkit to provide precise positions for Solar-system sources\&. Also, added support for Keplerian orbitals, such as the ones published by the IAU Minor Planet Center (MPC) for asteroids, comets, and Near-Earth-Objects (NEOs)\&. And, many more fixes and improvements\&. diff --git a/doc/CHANGELOG.md b/doc/CHANGELOG.md index c0cefc60..957d4fc3 100644 --- a/doc/CHANGELOG.md +++ b/doc/CHANGELOG.md @@ -7,6 +7,12 @@ The format is based on [Keep a Changelog](https://keepachangelog.com/en/1.1.0/), [Semantic Versioning](https://semver.org/spec/v2.0.0.html). +## [Unreleased] + +Upcoming bug fix release, targeted for 1 May 2025. + + + ## [1.2.0] - 2025-01-15 Feature release. New easy to use adapter modules for CALCEPH or the NAIF CSPICE Toolkit to provide precise positions diff --git a/doc/README.md b/doc/README.md index a88373b6..9261f683 100644 --- a/doc/README.md +++ b/doc/README.md @@ -1,5 +1,7 @@ CfA logo
    +[![DOI](https://zenodo.org/badge/748170057.svg)](https://doi.org/10.5281/zenodo.14584983) + The NOVAS C astrometry library, made better. - [API documentation](https://smithsonian.github.io/SuperNOVAS/apidoc/html/files.html).