<h3>?? June 2009 (Current release)</h3>
<p>
<a href="cmdfit.tar.gz">cmdfit.tar.gz</a>
</p>
<a href="cmdfit_mac.tar.gz">cmdfit_mac.tar.gz</a>
</p>
(1) The major change is that the age axis is now given in log10(yrs) rather
than Myr.
This makes things much easier when dealing with data which have a large
uncertainty in age, as this is a far more natural axis to use.<br>
(2) There are now "user" isochrones, which allow you to supply a file of
either (i) luminosity, effective temperature and gravity or (ii) colour
and magnitude for a given age.
Now interpolation in age is carried out on this files, allowing you to make
the choice as to how this interpolation is done is therefore yours.
The formats are dealt with in the section of the manual on isochrones.
</p>
</p>
<h3>29 October 2008 (Current release)</h3>
<p>
<a href="cmdfit.tar.gz">cmdfit.tar.gz</a>
</p>
Documentation fix for example 2.
</p>
<h3>15 October 2008</h3>
<p>
<a href="cmdfit.tar.gz_15-10-08">cmdfit.tar.gz_15-10-08</a>
</p>
<p>
To be on the safe side, I switched off the extraoplation of the 
colour-Teff relationships.
<h3>24 September 2008</h3>
</p>
<p>
This is a major update in techniques, which I hope to write up, but
for the moment should be quoted as Naylor (in prep).
(1) I use a new normalisation, which retains the mass function in the
grids, but then normalises the grid to sum to one between the brightest and
faintest datapoints.
This avoids the problem of the normalisation going infinite if the isochrone
is vertical.<br>
(2) To generate the uncertainties I now use the uncer method (replacing
bootstrap), for which there is a <a href="uncer.html">brief description</a>.
Its faster and more accurate.<br>
(3) The calculation of the expected value of tau^2 has been improved, and is
now done in a program called tau2, which replaces tau.
The old estimate became increasingly poor as the number of free parameters
increased.
</p>
<h3>19 February 2008</h3>
<p>
(1) A correction to Example 2.
The extra uncertainty to be added to the colour was given as 0.03, it
should be 0.042.
Both the web-page and the sample files have been updated to reflect this
change.<br>
</p>
<h3>21 August 2007</h3>
<p>
(1) V vs V-I for the Geneva isochrones.<br>
(2) V vs B-V for the Siess and Baraffe isochrones.<br>
(3) The option to use Bessell et al (1998) colour and bolometric corections.<br>
(4) Grid now imposes the upper limit on tau-squared to be the tau-squared of
the best fitting data point (i.e. that with the lowest tau-squared) plus
some value.
We do this so that if a different normalisation for tau-squared is used,
which efectively adds a constant to all the tau-squared values, the answer
remains the same.
With the chi-squared-like normalisation the lowest tau-squared value was
so close to zero this has little effect on the fits.<br>
</p>
<h3>05 June 2007</h3>
<p>
(1) The Padova option was using the z=0.004 tracks from the Cioni et
al (2006) papers, not as stated on the web pages Girardi et al (2002).
The code has been changed so the web page is correct, and the web
page now explicitly states its the z=0.019 models.<br>
</p>
<h3>03 October 2006</h3>
<p>
(1) Corrected a problem whereby if the mass-range you requested outran
that available in the isochrones for model numbers greater than 20
(i.e. those which come ready calibrated in colour and magnitude), you
got some strange low-level effects in the 2D ischrones.<br>
(2) Updated Example 1 so the numbers are correct for the new code (the
differences are within the uncertainties).<br>
(3) Added .in files to Example 1, which contain the precise inputs
needed to run the programs.<br>
</p>
<h3>30 September 2006 </h3>
<p>
(1) Corrected bundle so it includes files which are soft links on my 
machine.<br>
(2) Compiled all software statically, to improve portability.<br>
</p>
