RHUL Physics Department TWiki> Public Web>UserList>StewartBoogert>StewartBoogertAstronomy>StewartBoogertMSciProjects>StewartBoogertSpectroscopy2015>20151118_MSciSpectrocopyMeeting (19 Nov 2015, JosephBayley) EditAttach

- Mapping wavelength\grating\position on camera
- add term to fit function so
- plot histogram of residuals instead of 3d plot, where
- histogram should follow Gaussian with , , is if all point lie above fit plane etc
- with , write down as well so can get per degrees of freedom.
- do a linear fit first, then add terms and see how varies.
- could also plot data points for each grating position with fit function
- put all lamps onto same plot

- Scan of peak across CCD
- Have the scan plot as parametric function
- then can see intrumental response
- similtaneous fit with r of circle fit
- fit with parabola

- Errors
- Take lots of 0.5s frames and look at the spread of the data
- normalise to the same area under curves, then see how individual point varies
- to normalise, divide each point by bin width and the total number of points in the distribution
- see how the varies with exposure time
- derive some error bar from this and compare it to the poisson error found before
- may follow students-t distribution not Gaussian

- Fit to line
- for background fit quadratic that is not to large so affects Gaussian
- add some skew to the Gaussian
- see if the skew is the same on both sides of the chip
- look up how to skew the Gaussian
- odd/even functions in the
- could use Gaussian as a function of where:
- if then its a normal Gaussian
- if or other function then can add skew

- Look at fourier transform of the ccd pixel readout

-- JosephBayley - 19 Nov 2015

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Topic revision: r1 - 19 Nov 2015 - JosephBayley

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