SYNOPSIS

gyoto [--silent|--quiet|--verbose[=N]|--debug]
      [--no-sigfpe]
      [--help] [--list]
      [--ispec=i0:i1:di] [--jspec=j0:j1:dj]
      ([--imin=i0] [--imax=i1] [--di=di])
      ([--jmin=j0] [--jmax=j1] [--dj=dj])
      [--time=tobs] [--tmin=tmin]
      [--fov=angle] [--resolution=npix] [--distance=dist]
      [--paln=Omega] [--inclination=i] [--argument=theta]
      [--nthreads=nth] [--nprocesses=nprocs]
      [--plugins=pluglist]
      [--impact-coords[=fname.fits]]
      [--unit[=unit]]
      [--parameter=Path::Name[=value]]
      [--xmlwrite=output.xml]
      [--] input.xml output.fits

DESCRIPTION

Gyoto is a framework for computing geodesics in curved space-times. The gyoto utility program uses this framework to compute images of astronomical objects in the vicinity of compact objects (e.g. black-holes). Such images are distorted by strong gravitational lensing.

gyoto takes a scenery description in XML format (input.xml), computes this scenery using relativistic ray-tracing, and saves the result in FITS format.

A companion program, gyotoy(1), can be used to interactively visualize a single geodesic in any Gyoto metric (the trajectory of a single photon or massive particle).

Ray-tracing can be very time consuming. It is possible to interrupt the process at any time by hitting ^C, which will save the already-computed part of the image before exiting the program. You can then compute the rest of the image later using the --jmin option.

OPTIONS

The gyoto program accepts many options. Most have a long name (e.g. --parameter) and a short name (e.g. -E). When an option takes an argument, this argument must follow immediately the short option (e.g. -EPath::Name) and be separated from the long option by exactly the character "=" (e.g. --parameter=Path::Name). Long options can be abbreviated as long as the abbreviation is unambiguous (e.g. --par=Path::Name). Most options can appear several times and are processed in the order they appear in the command line. The two positional parameters (input.xml and output.fits) can appear anywhere in the command line, except if they start with a minus character (-) in which case they must appear last, after the option --.

Getting help

--help

-h

Print help summary. Although not as verbose as this manual page, the output of gyoto -h may be more complete and up to date. Then exit the program, unless --list below has only been specified.

--list

-l

Print list of currently registered Astrobj, Metric etc., then exit the program. This occurs after loading input.xml (if provided), so that any plug-in specified in the input file have already been loaded.

Setting the verbosity level

Those options are processed separately from the other and take effect early in the program execution.

--silent

-s

No output.

--quiet

-q

Minimal output.

--verbose[=N]

-v[N]

Verbose mode. Verbosity level N may be specified.

--debug

-d

Insanely verbose.

--no-sigfpe

Do not try to raise SIGFPE upon arithmetic exceptions. This option is meaningful only if fenv.h support is built in. Else this option is a no-op as SIGFPE is never raised.

Loading plug-ins

--plugins[=[nofail:]plug1[,[nofail:]plug2][...]]

-p[[nofail:]plug1[,[nofail:]plug2][...]]

Comma-separated list of Gyoto plugins to load. Overrides GYOTO_PLUGINS environment variable below. Only the last occurence matters.

Selecting a region

It is possible to ray-trace only part of the scenery by providing the pixel coordinates of the bottom-left (i0, j0) and top-right (i1, j1) corners of the region. The bottom-left pixel of the complete image has coordinates i=1 and j=1. The step in each direction (di, dj) can also be specified.

--ispec=[i0]:[i1]:[di]

-i[i0]:[i1]:[di]

--jspec=[j0]:[j1]:[dj]

-j[j0]:[j1]:[dj]

Default values: x0: 1; x1: npix (see option --resolution below); dx: 1.

--ispec=N

-iN

--jspec=N

-jN

Set both x0 and x1 to N.

Alternate region-selection options:

Those options are still supported for backward compatibility. They are deprecated in favour of --ispec and --jspec above:

--imin=i0

Default value: 1.

--imax=i1

Default value: npix

(see option --resolution below).

--di=di

Default value:1.

--jmin=j0

Default value: 1.

--jmax=j1

Default value: npix

(see option --resolution below).

--dj=dj

Default value:1.

Setting the camera position

The following parameters are normally provided in the Screen section of input.xml but can be overridden on the command line for instance to make a movie (by calling gyoto for each movie frame, changing only the option --time).

--time=tobs

The observing time in geometrical units.

--fov=angle

The field-of-view of the camera, in radians.

--resolution=npix

-rnpix

Number of rows and columns in the output image.

--distance=dist

(Coordinate) distance from the observer to the center of the coordinate system, in geometrical units.

--paln=Omega

Position angle of the line of nodes, in radians, East of North. The is the angle between the North direction and the line of nodes (see below).

--inclination=i

Angle between the plane of the sky and the equator of the coordinate system. The intersection of those two planes is the line of nodes.

--argument=theta

Angle in the equatorial plane between the line of nodes and one of the main axes of the coordinate system.

Miscellaneous

Unsorted option(s):

--

Ends option processing, in case either

input.xml or output.fits starts with "-".

--nthreads=nth

-Tnth

Number of parallel threads to use. For instance, on a dual-core machine, --nthreads=2 should yield the fastest computation. This option is silently ignored if Gyoto was compiled without POSIX threads support. Note that the metric and object are replicated for each thread which can lead to a decrease in performance if either is memory-intensive. Setting this option to 0 is equivalent to setting it to 1.

--nprocesses=nprocs

-Pnprocs

Number of MPI processes to spawn for parallel ray-tracing, in addition to the main gyoto process which remains for managing the computation. Ignored if gyoto was compiled without MPI support. nprocs is the number of workers spawned. -P0 disables MPI multi-processing, whild -P1 uses two processes: the manager and one worker. If nprocs is >0, --nthreads is ignored. Note that the MPI environment usually needs to be set-up using some variant of mpirun. You should only launch one instance of gyoto and let it spawn its workers:

mpirun -np 1 gyoto -Pnprocs input.xml output.fits

--impact-coords[=impactcoords.fits]

In some circumstances, you may want to perform several computations in which the computed geodesics end up being exactly identical. This is the case for instance if you want to experiment changing the spectrum of a star or when making a movie of a rotating, optically thick disk. This option provides a mechanism to not recompute the geodesics in the most simple case:

• the Screen is always at the same position;
• the Metric is always exactly the same;
• the Astrobj is optically thick (no radiative transfer processing is necessary);
• the location and shape of the Astrobj is always the same.

If --impact-coords is passed without specifying impactcoords.fits, the 8-coordinate vectors of the object and photon at impact point are saved for each point of the Screen. Missing data (no impact) are set to DBL_MAX. These data are saved as a supplementary image HDU in the FITS file which is identified by its EXTNAME: "Gyoto Impact Coordinates". The FITS keyword "HIERARCH Gyoto Observing Date" of this HDU holds the observing date (in geometrical unit).

If impactcoords.fits is specified, the above mentioned data are read back from this file. The ray-tracing is not performed, but the Gyoto::Astrobj::Generic::processHitQuantities() method is called directy, yielding the same result if the four conditions above are met. The observing date stored in the FITS keyword "HIERARCH Gyoto Observing Date" is compared to the date specified in the screen or using the --time option and the impact coordinates are shifted in time accordingly.

It is also possible to set the two versions of this option at the same time:

--impact-coords=impactcoords.fits --impact-coords

In this case, the impact coordinates are read from impactcoords.fits, shifted in time, and saved in output.fits.

--unit[=unit]

-u[unit]

Specify unit to use for allowing instances of --parameter, untill next instance of --unit.

--parameter=Path::Name[=value]

-EPath::Name[=value]

Set arbitray parameter by name. Parameters can be set in the Astrobj, Metric etc. using the Path componenent. For instance,

For instance, assuming the Astrobj in star.xml has a property named "Radius" that can be set in unit "km", and a property named "Spectrum" which has a property named "Temperature", we can set the radius, temperature and the quantities to compute (a property in the Scenery itself) with:

gyoto -EQuantities=Spectrum \

      -ukm -EAstrobj::Radius=3 \

      -u -EAstrobj::Spectrum::Temperature=1000 \

      star.xml star.fits

gyoto --parameter=Quantities=Spectrum \

      --unit=km --parameter=Astrobj::Radius=3 \

      --unit="" --param=Astrobj::Spectrum::Temperature=1000 \

      star.xml star.fits

--xmlwrite=output.xml

-Xoutput.xml

Write back scenery to an XML file. The new file will contain additional default parameters and reflect the effect of --(astrobj|metric|scenery|screen|spectrometer)-parameter that appear before --xmlwrite. Can appear several times, e.g. to generate several XML files with different settings.

FILES

input.xml

A gyoto input file in XML format. Several examples are provided in the source doc/examples directory. Depending on how you installed

gyoto, they may be installed on your system in a place such as /usr/share/doc/libgyoto/examples/. It goes beyond the scope of this manpage to document the XML file format supported by Gyoto, please refer to the library documentation which may be distributed by your package manager, can be compiled from the Gyoto source, and can be consulted online at http://gyoto.obspm.fr/.

output.fits

The output image in FITS format.

gyoto will not overwrite output.fits unless it is prefixed with an (escaped) "!": "gyoto in.xml \!out.fits". This file may actually consist in a stack of images depending on the Gyoto Quantities and on the Spectrometer specified in input.xml. For further information on the FITS format, see http://fits.gsfc.nasa.gov/.

AUTHOR

Thibaut Paumard <[email protected]> wrote this manual.