Examples

You can try the examples with your own data cube, but you can also download the exact same cubes I used here.

http://celeste.phy.ulaval.ca/files/new_orb3_cubes_examples/

If you experience any problem with the download please send me a message (thomas.martin.1@ulaval.ca).

First basic examples

These examples show the basic usage of ORCS

• Getting started
• How precise must be the input velocity parameter ?
• Make a fit over an entire region of the field
• Differences between fitting a sincgauss model and two sinc lines

Automatic velocity and flux estimation (complete examples)

• Automatic estimation of the flux and velocity and double sinc fit
• Multiple components fitting with automatic velocity estimate

Bayesian fitting vs. classical fitting

Here are more advanced examples that show step-by-step the differences between a classical fit and a Bayesian fit on a model spectrum. You will thus first learn how to model a spectrum and then fit a model spectrum with one line, two resolved lines and two unresolved lines: this is when the bayesian fitting algorithm becomes intersting ;)

• Modelling and fitting a single line spectrum
• Modelling and fitting a spectrum with two resolved lines
• Modelling and fitting two unresolved emission lines with a bayesian approach

Calibrating your data

A data cube can be recalibrated using mode specific algorithm which depends on the type of data you have observed. You might want to give a try to these examples to see if you can get a better calibration for your data.

• Wavelength recalibration with the sky lines (Mendel OH bands)
• Image registration
• Flux Calibration Example Using HST image

Advanced fitting

These examples show advanced fitting procedures.

• Constraining line ratios
• Various notes on fitting emission lines

Other Tools

• Automatic source detection
• Radial Velocity Correction
• How to use the computed correction