Unraveling the Structure in the ISM Through Radio Polarimetry

Details Unraveling the Structure in the ISM Through Radio Polarimetry Unraveling the Structure in the ISM Through Radio Polarimetry

Feb 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004mim..proc...81h&link_type=abstract

The Magnetized Interstellar Medium, Proceedings of the conference, held in Antalya, Turkey, September 8 - 12, 2003, Eds: B. Uyan

Computer Science

1

Scientific paper

We present two models of the Galactic warm interstellar gas to study depolarization and derive properties of the interstellar medium (ISM). First, a single-cell-size model of the ISM including magnetic fields and thermal and relativistic electrons is used to derive the magnetic field strength and typical scale of structure in the ISM. The polarized radiation in the model is compared to observations of the polarized synchrotron background at 350 MHz, taken with the Westerbork Synthesis Radio Telescope (WSRT). The modeling yields a random magnetic field component Bran ≈ 1-3 μG, a regular magnetic field component Breg ≈ 2-4 μG directed almost perpendicular to the line of sight, and a typical scale of the structure d ≈ 15 pc. A three-dimensional magnetohydrodynamical model of a Faraday screen is used to estimate the effect of beam depolarization on diffuse polarization observations. It suggests that sharp gradients in RM are a common feature in the warm ISM, and that the depolarization canals in the WSRT observations are most likely caused by beam depolarization. The additional error in RM in these observations introduced by beam depolarization is estimated to be ˜ 20%.

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