Comments (5)
Looks good. I agree with the separate branches for space and ground, even if we primarily use only one branch.
Will all groups fit in a rectangular window (as opposed to a more complicated shape)? We may also want to include any mask information that fits inside the group footprint so we know when sources are expected to be chopped off.
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We need to look at Erin Sheldon's MEDS DES formalism for grouping objects. This is what LSST DM will likely build off of (private communication Jim Bosch).
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After contacting Erin he responded
Hi Guys -
That meds library (https://github.com/esheldon/meds) is currently only for
reading the files. The code that creates them is a C++ code located here:https://github.com/rmjarvis/deswl_shapelets/blob/master/src/MakeCutouts.cpp
It is C++ for historical reasons: we have a nice WCS class in C++ and I
leveraged that. I would do it in python now, and plan to rewrite it some
time soon.Anyway, some documentation is at the top of that file. I will also be
describing it in great detail in our upcoming DES shear catalog paper, which
is about 85% complete.I can send you a copy of that when it is cleared for release, or if you really
want to see it soon I could rip out that section and latex it up separately
(it is public information anyway, since you could figure it out from the code)Let me know if you have any questions.
-e
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Here are some questions we asked Erin along with his responses:
Q: It looks like you are using fits file format. I am guessing it is because
you can have the WCS header easily attached to the cutout images. Did you
consider any other file structures like HDF5?
A: The reason is to remove a heavy dependency like HDF. Also with the
fitsio python package (not pyfits), we get fast random access within
the data structure (all postage stamps are stored internally in one
large 1-d array). Note we fpack the files, which reduced the size by
a factor of 5 or so.
Q: Is there are reason you only have square cutouts and of fixed sizes?
A: The box sizes are chosen to faciliate FFTs. The sizes are in 2N or 3*2N.
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Based on the previous information we've decide to diverge from the MEDS format for the following reasons:
- HDF5 is not a "heavy" dependency in the frameworks we¹re already using.
- We'll be extremely lucky if we ever get to a regime where we're IO
limited! - A flat data structure sounds like a bookkeeping headache for the
hierarchical source models we¹ve been discussing. - And, of course, we don't need to compute FFTs of our cutouts because we're
forward modeling.
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Related Issues (20)
- Add spectral properties to the galaxy models using the galsim.Chromatic class HOT 1
- Create a script to plot hdf5 segments HOT 1
- Add filter throughput curves to hdf5 file HOT 4
- Single noise value or noise map HOT 1
- Create some model vs data plots function
- Use compound types for roaster output format HOT 2
- Fix MCMC sampling of Spergel `nu` parameters HOT 4
- Run DM Stack on the galsim_galaxy output
- Fix WCS of galsim_galaxy images HOT 2
- Add gain metadata to the galsim_galaxy hdf5 and fits file outputs HOT 1
- Output PSF fits image in galsim_galaxy.py
- Fix effective PSF for LSST in galsim_galaxy.py
- Output PSF hdf5 data in galsim_galaxy.py HOT 1
- Update/clone `sheller.py` to prepare GREAT3 data for input to JIF
- Debug multithreading in Roaster
- Define a GalSim noise model from GREAT3 inputs
- Demonstrate PSF marginalization for a single galaxy image HOT 5
- Enforce consistency between exposure times in noise and zeropoint calculations in galsim_galaxy.py
- Debug parameter optimization in Roaster
- Separate chromatic models into GalsimGalaxy sub-class
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