QDeblend3D is a Graphical User Interface for integral field spectroscopic data with the specific aim to deblend the emission from an unobscured AGN and its underlying host galaxy. The algorithm uses the fact that the broad-line region of an AGN is appearing as a point-like source given its compact size <1pc. Thus, a point-spread function PSF can be easily computed and used to deblend point-like and extended emission. Since the narrow emission lines from the host galaxy are usually on top of the broad lines, spectral windows have to be carefully selected to map the broad line intensity across the IFU field. That is the reasons why a GUI is well suited for this task, so that the data can be inspected directly and spectral windows can be adjusted on the fly depending on the AGN host galaxy properties.

The basics of the deblending algorithm behind QDeblend3D is explained in more detail in the articles:

  1. Integral field spectroscopy of nearby QSOs - I. ENLR size-luminosity relation, ongoing star formation and resolved gas-phase metallicities,  Husemann et al. (2014)
  2. The properties of the extended warm ionised gas around low-redshift QSOs and the lack of extended high-velocity outflows, Husemann et al. (2013)

Any Publication using QDeblend3D should cite those two papers for reference.

The software will in particular be useful for IFU data of unobscured AGN obtained with the ongoing major surveys, like CALIFA, SAMI and MaNGA. I am currently updating the software to efficiently deal with the large data generated by the large VLT-MUSE instrument, and also enhance its capabilites in terms of a wavelength dependent PSF.

Please contact me directly if you have any question or suggestion related to the use of QDeblend3D.

Screenshot of the QDeblend3D GUI with real data from the MUSE instrument.