24-007 The Study of Quasar Polarization in The Hwo

il y a 2 semaines

Strasbourg, Grand Est, France CNES - Centre National d'Etudes Spatiales Temps plein
Doctorat, 36 mois

  • Temps plein
  • Aucune expérience exigée
  • Maitrise, IEP, IUP, Bac+
  • Astronomy, Astrophysics

Mission:


Active galactic nuclei (AGN) are extra-galactic objects observable from the nearby Universe out to cosmological distances thanks to their unmatched brightness among non-transient sources.

The tremendous amount of photons emitted by an AGN arise from mass accretion onto a central supermassive black hole (SMBH).

Matter falling into the SMBH potential well produces radiation from the far ultraviolet (UV) to the near-infrared (NIR), with photons originating from a region not larger that a few hundred/thousand astronomical units.

AGN are also powerful sources of high-energy (X-rays and gamma-ray) radiation, thermal-infrared re-emission by dust up to a hundred microns and, depending on the existence of a kiloparsec-scale jet of collimated material, synchrotron radio emission.

Although the global AGN picture seems rather understood, the details of AGN physics are still poorly constrained.

The key role of AGN and the growth of SMBH in galaxy evolution is now recognized, but the small size of the central engine (less than a parsec) makes it challenging to spatially resolve the innermost regions of an AGN and its host galaxy with current spatial-resolution capabilities.

Significant progress in understanding the precise mechanisms of matter and energy transfer and SMBH growth was achieved thanks to the advent of high-resolution spectrometers, high-angular resolution (+adaptive optics) imaging, timing and interferometry.

Yet, all these techniques are intrinsically limited by their lack of sensitivity to the morphology of the emitting/reprocessing regions and the intensity and configuration of the magnetic field.

Polarimetry, on the other hand, is extremely sensitive to the geometry and magnetic-field properties, and provides information about matter composition, temperature, and velocity, which complements that obtainable via other techniques.

Hence, new polarimetric observations using state-of-the-art polarimeters promise us the strongest constraints on the physical parameters controlling SMBH growth, AGN radiative outputs and their impact on galaxy evolution.

POLLUX will be such a state-of-the-art polarimeter. It is a high-resolution, broadband spectropolarimeter proposed for the Habitable Words Observatory (HWO).

HWO is the future large space telescope that the NASA plans to develop after the Nancy-Grace-Roman Space Telescope (launch planned for 2027) projects.

This telescope, equipped with a primary mirror whose diameter would be between 6.5 and 8 meters, would carry out its observations in the UV/optical/NIR.

The French spatial agency is currently working on the implementation of POLLUX in HWO.

The instrument Phase 0 study is led by the Laboratoire d'Astrophysique de Marseille (LAM) and the Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA) with the support of the CNES and a consortium of European scientists.


The AGN science case for HWO/POLLUX is currently lead by Frédéric Marin, in the Strasbourg astronomical observatory, who is the proponent of this thesis.

The goal of his team (and of the thesis) will be to characterize the performances of POLLUX (wavelength coverage, spectral resolution, polarimetric sensitivity, etc.) necessary to probe AGNs and therefore to contribute to the multi-thematic specifications of the instrument for the engineers in charge of POLLUX's development.

To do so, a PhD student is of fundamental importance in order to upgrade and use the Monte Carlo radiative transfer code STOKES (Goosmann & Gaskell 2007, Marin et al.

2012, 2015, This code is fine-tuned for the 3D modeling of AGNs from 1 microns to 200 keV, but lacks a number of critical physical processes that are necessary to understand and predict AGN observations.

Among them are all the polarization mechanisms arising from light/dust interactions that are crucial to understand the physics of dust within the AGN (torus, winds ), around the AGN (interaction of AGN light/matter with the interstellar medium) and along the observer's line-of-sight (galactic magnetic fields, dust within the Milky Way).

The scientific objectives of the thesis are as follows:

  • taking charge of the pre-existing C++ STOKES code
- implementation of thermal re-emission by dust;
- implementation of dichroic polarizing mechanisms (extinction, diffusion, absorption);
- implementation of new emission sources (black body, synchrotron, starlight, etc.);
- comparison of the code to other existing codes (which are limited to unique/simple/monoenergetic mechanisms) for benchmarking;
- fit of data (already acquired) from the VLT/FORS2 (optical spectropolarimetry);
- online release of the code (open-access) with its user manual;
- participation/lead in the writing of proposals for observations with ground instruments (VLT, Subaru );
- characterization of POLLUX's technological needs for finalizing the

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