How to obtain physical variables from Mg II h&k lines using \(IRIS^{2}\) inversions

Edited by A. Sainz Dalda, V. Hansteen, M. Gošić, and B. De Pontieu.

e-mail: asainz.solarphysics@gmail.com or bdp@lmsal.com

Last updated on Jun 24, 2020.

Contents:

• 1. IRIS²: IRIS Inversion based on Representative profiles Inverted by STiC
  • 1.1. Quick start to invert IRIS Mg II h&k lines with IRIS²
  • 1.2. Limitations of IRIS² inversions
  • 1.3. Understanding the quality of the IRIS² results
    • 1.3.1. The weights and the weighting windows: \(w_i\)
    • 1.3.2. The quality of the fit: \(\chi^2\)
    • 1.3.3. The uncertainty: \(\sigma_p\)
  • 1.4. IRIS² elements in SolarSoft
  • 1.5. Acknowledging \(IRIS^{2}\)
• 2. IRIS² in SolarSoft
  • 2.1. Standalone installation
  • 2.2. Inversion of IRIS Mg II h&k lines with iris2
  • 2.3. Inversion of a large raster file, a region of interest, or a masked area
  • 2.4. The function iris2
    • 2.4.1. IRIS² Tutorial Videos: inverting IRIS Mg h&k lines with iris2
  • 2.5. Inspecting the IRIS² model atmosphere (and beyond)
    • 2.5.1. The IRIS2 3D Model Inspector window
    • 2.5.2. The IRIS2 Model Atmosphere window
    • 2.5.3. The IRIS2 Fit window
    • 2.5.4. The \(\chi^2\)-map, map_index_db, and map_mu_db maps
  • 2.6. The function show_iris2model
    • 2.6.1. IRIS² Tutorial Videos: inspecting the inversion results with show_iris2model
• 3. IRIS² and deepIRIS² in python
• 4. Hands-on tutorial of IRIS² in IDL.
  • 4.1. Installation of minimal IRIS SolarSoft branch (including \(IRIS^{2}\))
  • 4.2. Verifying the minimal \(IRIS^{2}\) SolarSoft and the temporary \(IRIS^{2}\) code installation
  • 4.3. First \(IRIS^{2}\) inversion
    • 4.3.1. Calibration of IRIS Level 2 data
    • 4.3.2. Inspecting the Mg II h&k data cube
    • 4.3.3. Loading the \(IRIS^{2}\) database
    • 4.3.4. Lookind for the closest RP in the \(IRIS^{2}\) database
    • 4.3.5. Inversion of Mg II h&k lines based in RPs inverted by STiC