-
Notifications
You must be signed in to change notification settings - Fork 6
/
Copy pathChangeLog
146 lines (105 loc) · 5.51 KB
/
ChangeLog
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
19
20
21
22
23
24
25
26
27
28
29
30
31
32
33
34
35
36
37
38
39
40
41
42
43
44
45
46
47
48
49
50
51
52
53
54
55
56
57
58
59
60
61
62
63
64
65
66
67
68
69
70
71
72
73
74
75
76
77
78
79
80
81
82
83
84
85
86
87
88
89
90
91
92
93
94
95
96
97
98
99
100
101
102
103
104
105
106
107
108
109
110
111
112
113
114
115
116
117
118
119
120
121
122
123
124
125
126
127
128
129
130
131
132
133
134
135
136
137
138
139
140
141
142
143
144
145
146
- Development version (ver. 1.4.0)
+ A new component to accout for the [OIII]4959 blue wing is
available. The name is `line_oiii_4959_bw`. It is disabled by
default, enable it with `!QSFIT_OPT.oiii_4959_bluewing = 1`;
+ Component `line_oiii_bw` has been renamed to `line_oiii_5007_bw`;
+ Bugfix in reducing data for the [OIII] blue wing component;
- Mar. 11, 2019 (ver. 1.3.0)
+ The code has been largely refactored to implement the new
features, performance has improved, and a couple of emission lines
have been added, hence the results may be different from the v1.2.4
Catalog, although they are typically compatible within the quoted
uncertainties. In some case of strong correlation among fitting
parameters the results may be significantly different;
+ QSFit now supports fitting of absorption lines but their
location can not be automatically determined, and a first guess
for the rest frame wavelength must be manually provided. See the
USAGE file for an example.
+ Emission lines can now have a Lorentzian profile (rather than a
Gaussian one). See the USAGE file for an example.
+ The calling sequence has changed to accomodate the possibility to fit
multiple spectra simultaneously. See the USAGE file for an example.
+ Lower limit for EW iron UV is 1. Iron UV is disabled if
MIN(wavelength) > 2900. The `ironuv_fixed_max_z` configuration
option has beenn drooped;
+ The `tied` field of the parameter structure has been renamed to
`expr`, and its purpose changed: when used with `fixed=0` it
allows to specify a mathematical expression (possibly involving
other parameters) evaluated before passing the result to the
component function. When used with `fixed=1` it is used to tie
the value to other parameters (old behaviour);
+ New emission line components: CII] 2326 and [OIII]5007 blue
wing. The latter accountsfor the [OIII]5007 blue wing. It is
constrained to have a FWHM larger than the main [OIII]5007 by an
amount in the range 100:1000 km/s, and a blue velocity shift in
the range 0:2000 km/s with the respect to the main line. The name
of this new component is `line_oiii_bw`;
- Mar. 03, 2018 (ver. 1.2.4)
+ All calculations are now forced to be done with DOUBLE precision.
This ensure the reproducibility of the results regardless of the
data type of the redshift and color excess input parameters;
+ Added support for three more emission lines: NV 1241, OI 1306
and CII 1335;
+ Bugfix: the QSFit software used to create the first published
catalog (v1.2) had a bug in the code which freezes/thaws the iron
template component at optical wavelengths. This bug affected only
the spectral estimates for the sources with z < 0.4.
+ Bugfix: in very few cases QSFit computed the wrong spectral
coverage for the emission lines, enabling their corresponding
components instead of disabling them;
+ Minor bugfix
+ The whole QSFit catalog has been re-created using this QSFit
version. The results are available at the following address:
http://qsfit.inaf.it/cat_1.24/
- Dec. 09, 2017 (ver. 1.2.3)
+ QSFit now accept the `z=0` keyword, implying that the input data
are already given in emitted luminosity (rather than observed
flux), and the wavelengths are already in the source rest frame;
+ We added the !QSFIT_OPT.min_wavelength option, to specify the
minimum wavelength (in AA) to be considered in the fit. Smaller
wavelengths are ignored;
+ We added the !QSFIT_OPT.accept_line_res option to specify the
minimum emission line resolution (in km s^-1) to consider the line
in the fit. If the resolution of a line is smaller the whole line
range is ignored;
+ Minor bug fix.
- Nov 02, 2017 (ver. 1.2.2)
+ QSFit is now able to read data from an ASCII text file (rather
than from a SDSS DR10 FITS file): simply pass the `input='ASCII``
keyword to `qsfit`;
- Jul 20, 2017 (ver. 1.2.1)
+ QSFit is now able to fit a set of (manually added) absorption
lines. The list of absorption wavelengths must be specified
through the !QSFIT_OPT.abslines_wavelengths global variable.
- Jul 19, 2017 (ver. 1.2)
+ QSFit now defines a global variable upon initialization, named
`!QSFIT_OPT`, containing several settings to customize the fitting
behavior. Check the qsfit_prepare_options for further details;
+ The default host galaxy template is now SWIRE_ELL5
(http://www.iasf-milano.inaf.it/~polletta/templates/swire_templates.html);
+ By default, the continuum is now modeled with a single power law
instead of a smoothly broken power law. To restore the old
behaviour set `continuum.dalpha.fixed = 0`;
+ The four parts of the UV iron template are now joined in a
single component;
+ QSFit now estimates the equivalent widths for the iron and
emission line components;
+ A Monte Carlo resampling method has been implemented to
accurately estimate the parameter uncertainties. See the
corresponding section in the reference paper;
+ A new component to model the Balmer continuum and
pseudo-continuum (blending of high order Balmer lines) has been
added.
- May 29, 2017 (ver. 1.1)
Minor updates to improve performances, accuracy of results and
functionalities:
+ QSFit: initial value for the continuum component slope is now
-1.5 (in ver. 1.0 was -2);
+ QSFit: emission lines rest frame wavelengths have been
corrected;
+ QSFit: solved the error occurring when the number of "unknown"
emission lines was 0;
+ QSFit components sbpowerlaw and emline: improved performances;
+ Default gnuplot terminal is qt (in ver. 1.0 was wxt);
- Dec. 5, 2016 (ver. 1.0)
First commit of QSFit package