https://github.com/simonrw/ngts-error-contributions
For calculating the NGTS error contributions
https://github.com/simonrw/ngts-error-contributions
Last synced: over 1 year ago
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For calculating the NGTS error contributions
- Host: GitHub
- URL: https://github.com/simonrw/ngts-error-contributions
- Owner: simonrw
- Created: 2011-11-16T17:47:09.000Z (over 14 years ago)
- Default Branch: master
- Last Pushed: 2017-02-17T12:24:44.000Z (over 9 years ago)
- Last Synced: 2025-02-06T08:45:20.344Z (over 1 year ago)
- Language: Python
- Homepage:
- Size: 758 KB
- Stars: 1
- Watchers: 2
- Forks: 0
- Open Issues: 0
-
Metadata Files:
- Readme: README.mkd
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README
# README
Here I break down what the scripts in this directory do. I may unite them with some form of interface script which is a huge waste of time but will make me feel better.
The scripts can roughly be broken down into a few categories
* configuration
* Noise model
* Saturation estimation
* Field numbers
## Configuration
### Config.py
This is the settings file for any NGTS specific settings. This sets such things as the read time and sky background.
### ConfigWASP.py
This is the same as `Config.py` but with WASP specific settings
## Noise model
### ErrorContributions.py
This plots the noise model contributions for a given `Config`, by assuming an exposure time, calculating the noise contributions and binning up to a configurable total exposure (by default 3600 seconds, 1 hour).
The main configurable parameter is the magnitude, allowing an exposure time vs fractional error plot to be created.
usage: ErrorContributions.py [-h] [-o Filename] -m magnitude
[-s {bright,dark}] [-z ZEROPOINT] [-r RENDER]
optional arguments:
-h, --help show this help message and exit
-o Filename, --output Filename
Image filename
-m magnitude, --targetmag magnitude
Target magnitude
-s {bright,dark}, --skylevel {bright,dark}
Sky type (bright or dark
-z ZEROPOINT, --zeropoint ZEROPOINT
Custom zero point
-r RENDER, --render RENDER
Render tables file>
### TheoryNoiseWithBinning.py
(Also including `TheoryNoiseWithBinningWASP.py`)
This script takes the other slice dimension through the magnitude/exposure time/fractional error cube from `ErrorContributions.py` and takes an exposure time from the user and plots the more normal fractional rms type plot with the noise model and contributions.
usage: TheoryNoiseWithBinning.py [-h] [-t TOTALTIME] -e EXPTIME
[-s {bright,dark}] [-d DEVICE] [-w] [-n] [-S]
optional arguments:
-h, --help show this help message and exit
-t TOTALTIME, --totaltime TOTALTIME
Total integration time
-e EXPTIME, --exptime EXPTIME
Science exposure time
-s {bright,dark}, --skylevel {bright,dark}
Sky type (bright or dark
-d DEVICE, --device DEVICE
PGPLOT device
-w, --plotwasp Overlay some WASP staring data
-n, --plotngts Overlay some NGTS prototype data
-S, --satlimit Do not plot saturation limit
## Saturation estimation
### FractionVsCentre.py
Calculate the distribution of fractions in the centre pixel for a psf of given
size as the psf is moved away from the centre pixel
### OffsetDistribution.py
Monte-Carlo simulation using the techniques in `FractionVsCentre` to plot the distribution of central pixel flux fractions, to estimate a typical value used in the saturation estimation.
### SaturationVsExposure.py
Using the noise model, calculate the saturation magnitudes as a function of science exposure time.
## Field numbers
### HighPrecisionRange.py & PlotHighPrecisionRange.py
These calculate and plot (respectively) the high precision range, using data from `SaturationVsExposure` and the 1mmag point from `TheoryNoiseWithBinning` to produce the range at which an object is considered high precision but not saturated.
### NHighPrecisionObjects.py
This script takes the high precision range from `HighPrecisionRange` and applies it to three fields using NOMAD data stored in the NOMADFields subdirectory. It plots the fraction of high precision objects in each field as a function of exposure time.
### NSaturatedInField.py
Plots the number of saturated objects in the three fields used in this study. Dark and bright time are used.
### NumberOfExposures.py
This calculates the number of exposures we require over a number of years for a given exposure time, and calculates the storage requirements.
## Other
### BatchRun.py
This runs all scripts.