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Possibly could be done by artificially shifting the spectra from different instruments to non-overlapping wavelengths (w/ appropriate scalings) and constraining the common features for the fitting. T…
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I really enjoy tinkering with ddsp. It would be a bit more approachable if we could experiment more easily with 44.1kHz or the other standard audio formats. Could you perhaps make it more straightforw…
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Hello,
First and foremost, thank you for all of the excellent work that's done here! `brms` is an excellent package and really helps decrease dependence on working in base `stan`, which is helpful …
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These grids are not available automatically in spectral_data/bosz2024_grids. I see that there was a function to call the download of these files `download_BOSZ_2024`, but because this isn't run automa…
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Hi,
Currently DESI applies heliocentric corrections based on the ra,dec of the center of the field, as opposed to star by star.
The difference between those can be computed easily:
![image](ht…
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From Satellite Team product development:
![image](https://cloud.githubusercontent.com/assets/2837257/24120397/e25156ea-0d8a-11e7-907a-76ee055007a7.png)
See:
- [Satellite Team - Google Drive](…
bbest updated
7 years ago
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A common situation in X-ray astronomy is to fit the same model to multiple datasets, e.g. in XMM, we get 5 simultaneous spectra (RGS1, RGS2, MOS1, MOS2, PN), in Chandra we get up to three (HEG, MEG, a…
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When the source amplitude is much higher than the background (ex. broken power law source with norm=3e-1 & power law background with norm=1 created using source_injector.ipynb), get_log_like returns n…
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This looks like a good survey
Community detection and stochastic block models:
recent developments by Emmanuel Abbe 2017
https://arxiv.org/pdf/1703.10146.pdf
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**Context**: I am using CAFE to extract attenuation information in ~4500 MIRI/MRS spaxels. To minimize the runtime over such a large dataset, I’ve turned emission line fitting off so I can do my own G…