42
Included code to catch incompatible compilation options.
Introduced
-DOUT_WL_CAT
and
-DWFE_OVERRIDE
options.
Added independent SNR cut for WL source galaxies.
Added finite line width smearing in BAO mode.
Added more realistic model for noise variance on NIR detectors (v6 and previous had
behavior equivalent to
mode==0
in
getNoiseTotal
, which was too optimistic).
Added thermal background model.
Version 8:
October 1, 2011
Added PZCAL mode.
Added updated CMC galaxy size distribution model (
j
=2), and correspondingly changed the
suggested command line input.
Changed
CCD_MODE
behavior to correspond to pixel parameters appropriate for a CCD
rather than HgCdTe detector.
Changed
WFE_OVERRIDE
behavior to switch off WL-‐specific inputs that are not used in
this mode.
Fixed bug in
n
eff
computation (v7 and previous were too pessimistic; typical changes are
~3%).
Version 9:
March 7, 2012
Changed detector options from macros to global variables set at the beginning of the run;
allows user to choose detector without recompiling.
Added
−
DWFE_HOPKINS_EXP
flag for alternative wavefront distribution.
Added support for completeness in the BAO mode.
Fixed bugs in error reporting.
Version 10:
March 28, 2012
Added the Sobral
et al
HαLF option.
Added output on photon counts per unit line flux in the BAO mode.
Added source continuum to the noise model.
Switched default BAO cuts to SNRo instead of SNRe (the latter is available as the
-DUSE_SNRE option
).
10. Acknowledgements
The development of this ETC has benefited from comparisons with other codes
and/or calculations by Ed Cheng, Jeff Kruk, and Michael Levi.
Peter Capak, Ed Cheng, Dave Content, Cliff Jackson, Jeff Kruk, Jason Rhodes, David
Sobral, and Yun Wang have been very helpful in providing input models, comments, and
feedback.
During the development of the ETC, Christopher Hirata has been supported by the
U.S. Department of Energy (DOE-‐FG03-‐92-‐ER40701), the National Science Foundation (NSF
AST-‐0807337), and the David & Lucile Packard Foundation.
