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2009-04-23:
* MIRA 0.9.8 released.
* Changes to use OptimPack-1.3 and to display Fdata and Fprior.
* Complex visibilities can be fitted with (or without) Goodman
approximation.
2008-12-12:
* MIRA 0.9.7 released.
* Fixed oifits.i for empty ARRNAME or INSNAME.
2008-12-09:
* MIRA 0.9.6 released.
* Fixed a bug in oifits.i with oifits_new_* when master is provided
(thanks to Thibaut Paumard).
* Fixed a bug in mira_new_fft_xform with spatial frequencies exactly
equal to zero (thanks to Stéphanie Renard).
2008-10-03:
* MIRA 0.9.5 released.
* Fix bug when no target is specified in mira_add_oidata.
* In mira_add_oidata/mira_new, keyword cleanup_bad_data can be set
to 0, 1, 2 to achieve different levels of filtering of invalid data.
* Various fixes in oifits.i for creating/saving OI-FITS files (thanks
to Sylvestre Lacour).
2008-09-26:
* MIRA 0.9.4 released.
* Added the possibility to select the target in mira_new.
* Hack for FLAG column to deal with AMBER data.
2008-09-23:
* MIRA 0.9.3 released.
* Fixed a bug in __mira_build_coordinate_list__ which prevent to use
data files with central frequency (0,0) measured.
* New function mira_dirac.
2008-09-07:
* Massive rewrite of oifits.i to optimize the code, make it easier to read
and let the users create OI-FITS data on the fly and save it to a file.
2008-09-04:
* MIRA 0.9.2 released. This is the version used for the MIRA demonstration
(see mira-demo.i) at SPIE 2008 Conference in Marseille (France).
* Some change in plots.
2008-07-12:
* MIRA 0.9.1 released. This is the version used for the VLTI 2008 Summer
School at Keszthely (Hungary).
* Missing fft_utils.i is now part of the distribution.
2008-06-06:
* MIRA 0.9 released.
2008-05-02:
* MIRA 0.8 released.
2008-01-31:
* MIRA 0.7 released.
* Orientation of u-v and image coordinates fixed to match astronmical
conventions.
* Use OptimPack1.
* Noisy works again.
* New Monte-Carlo optimizer.
* Fix a bug in mira_add_oidata with loading of complex visibilities.
2007:
* Penalty with respect to data is now computed for cartesian representation
of a complex (not a polar).
* Huge rewrite of code: all data of given type are collected in a single
table (more compact representation and faster computation/plotting when a
lot of interferometric data-blocks are fitted).
* Wavelength selection is more flexible (you can specify the effective
wavelength and bandwidth to consider).
* Very fast approximation of the Fourier transform by means of FFT (or FFTW)
and spectral interpolation.
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