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OPSIM-1171: Updates for Document 20160 #6

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OPSIM-1171: Updates for Document 20160 #6

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19 changes: 10 additions & 9 deletions index.md
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Expand Up @@ -11,7 +11,7 @@ information on the expected LSST camera and telescope components.

The appropriate methodology to calculate SNR values for PSF-optimized
photometry is outlined in the LSST Change Controlled Document
[LSE-40](http://ls.st/lse-40), and partially summarized below. Note
[LSE-40](https://ls.st/lse-40), and partially summarized below. Note
that LSE-40 was written with outdated throughput curves and
with an outdated understanding of the PSF profile which means the
actual numerical values calculated in that document are should not be used.
Expand Down Expand Up @@ -128,7 +128,7 @@ of the LSST mirors and focal plane and atmosphere, as well as
observations from existing telescopes, indicate that the PSF for point
sources should be similar to a von Karman profile. The details of the profile
depend independently on the size of the atmospheric IQ and the
hardware IQ. The conversion factors are described in the [Document 20160](http://ls.st/document-20160)
hardware IQ. The conversion factors are described in the [Document 20160](https://ls.st/document-20160)
by Bo Xin, George Angeli, and Zeljko Ivezic.

Because the SNR calculation only depends on the number of pixels
Expand Down Expand Up @@ -207,8 +207,8 @@ and airmass distributions, median expected m5 depths diverge from those above. (

### Useful github repositories

The algorithms described in [LSE-40](http://ls.st/lse-40) are implemented in the LSST
[rubin_sim.photUtils](http://github.com/lsst/rubin_sim) package,
The algorithms described in [LSE-40](https://ls.st/lse-40) are implemented in the LSST
[rubin_sim.photUtils](https://github.com/lsst/rubin_sim) package,
available on github. In particular, the
[SignalToNoise](https://github.com/lsst/rubin_sim/blob/main/rubin_sim/phot_utils/signaltonoise.py)
module calculates signal to noise ratios and limiting magnitudes (m5)
Expand Down Expand Up @@ -321,17 +321,18 @@ $C_m^{inf}$ and $C_m$ is $dC_m^{inf}$.
## Data Sources and References

Change controlled documents:
: - LSE-40 : "Photon Rates and SNR Calculations" <http://ls.st/lse-40> (useful for SNR eqns, but do not use the outdated values from this document)
- LSE-29 : "LSST System Requirements" <http://ls.st/lse-29>
- LSE-30 : "Observatory System Specifications" <http://ls.st/lse-30>
- LSE-59 : "Camera Subsystem Requirements" <http://ls.st/lse-59>
: - LSE-40 : "Photon Rates and SNR Calculations" <https://ls.st/lse-40> (useful for SNR eqns, but do not use the outdated values from this document)
- LSE-29 : "LSST System Requirements" <https://ls.st/lse-29>
- LSE-30 : "Observatory System Specifications" <https://ls.st/lse-30>
- LSE-59 : "Camera Subsystem Requirements" <https://ls.st/lse-59>

Official project documents not under change control -
: - The LSST Overview Paper <http://ls.st/document-5462>
- LSST Key Numbers <http://lsst.org/scientists/keynumbers>
- LSST-PST Syseng_throughputs components git repository <https://github.com/lsst-pst/syseng_throughputs>
- SMTN-002 <https://smtn-002.lsst.io> (this documnent)
- SMTN-002 <https://smtn-002.lsst.io> (this document)
- PSTN-054 <https://pstn-054.lsst.io>
- Atmospheric and Delivered Image Quality in OpSim <https://ls.st/document-20160>

| Additional Data | Value | Reference |
|:---------------------------------------------------------|------:|---------------:|
Expand Down
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