Found 2 talks width keyword ISM magnetic fields
I will review the status of the QUIJOTE (Q-U-I JOint TEnerife) experiment, a project led from the IAC with the aim of characterising the polarisation of the Cosmic Microwave Background (CMB) and other galactic or extragalactic physical processes that emit in microwaves in the frequency range 10-42GHz, and at large angular scales (1 degree resolution). QUIJOTE consists of two telescopes and three instruments operating from the Teide Observatory, and started operations about 10 years ago, in November 2012.
I will discuss the status of the project, and I will present the latest scientific results associated with the wide survey carried out with the first QUIJOTE instrument (MFI) at 11, 13, 17 and 19GHz, covering approximately 29000 deg$^2$ with polarisation sensitivities in the range of 35-40 $\mu$K/deg. These MFI maps provide the most accurate description we have of the polarization of the emission of the Milky Way in the microwave range, in a frequency domain previously unexplored by other experiments. These maps provide a unique view of the Galactic
magnetic field as traced by the synchrotron emission. These results have been presented in an initial series of 6 scientific articles published on January 12th, 2023.
Finally, I will describe the prospects for future CMB observations from the Teide Observatory.
I will present an extensive analysis of the 850 microns (353 GHz) polarization maps of the SCUBA Polarimeter Legacy (SCUPOL) Catalogue produced by Matthews et al., focusing on the molecular clouds and star-forming regions. The first half of the presentation will concern the several methods used in order to analyze and characterize the observed polarization maps and a statistical analysis of the results will be presented. The second half of the talk will focus on a method used for describing the turbulent regimes of the four well sampled regions, S106, OMC-2/3, W49, and DR21, based on comparisons with three-dimensional magnetohydrodynamics (MHD) numerical simulations scaled to the observed polarization maps. It will be shown how this method can be used for constraining the values of the inclination angle of the mean magnetic field with respect to the line of sight. Consistency of the results obtained from the comparison of the information extracted from the analysis of the observed and simulated maps with results obtained from independent observation data analysis by other authors will be discussed. Conclusions regarding how simple, ideal, isothermal, and non-self-gravitating MHD simulations may be sufficient in order to describe the large-scale observed physical properties of some molecular cloud envelopes will be given.
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