The Astrophysical Journal (Jan 2024)

Extragalactic Magnetism with SOFIA (SALSA Legacy Program). VII. A Tomographic View of Far-infrared and Radio Polarimetric Observations through MHD Simulations of Galaxies

  • Sergio Martin-Alvarez,
  • Enrique Lopez-Rodriguez,
  • Tara Dacunha,
  • Susan E. Clark,
  • Alejandro S. Borlaff,
  • Rainer Beck,
  • Francisco Rodríguez Montero,
  • Seoyoung L. Jung,
  • Julien Devriendt,
  • Adrianne Slyz,
  • Julia Christine Roman-Duval,
  • Evangelia Ntormousi,
  • Mehrnoosh Tahani,
  • Kandaswamy Subramanian,
  • Daniel A. Dale,
  • Pamela M. Marcum,
  • Konstantinos Tassis,
  • Ignacio del Moral-Castro,
  • Le Ngoc Tram,
  • Matt J. Jarvis

DOI
https://doi.org/10.3847/1538-4357/ad2e9e
Journal volume & issue
Vol. 966, no. 1
p. 43

Abstract

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The structure of magnetic fields in galaxies remains poorly constrained, despite the importance of magnetism in the evolution of galaxies. Radio synchrotron and far-infrared (FIR) polarization and polarimetric observations are the best methods to measure galactic scale properties of magnetic fields in galaxies beyond the Milky Way. We use synthetic polarimetric observations of a simulated galaxy to identify and quantify the regions, scales, and interstellar medium (ISM) phases probed at FIR and radio wavelengths. Our studied suite of magnetohydrodynamical cosmological zoom-in simulations features high-resolutions (10 pc full-cell size) and multiple magnetization models. Our synthetic observations have a striking resemblance to those of observed galaxies. We find that the total and polarized radio emission extends to approximately double the altitude above the galactic disk (half-intensity disk thickness of h _I radio ∼ h _PI radio = 0.23 ± 0.03 kpc) relative to the total FIR and polarized emission that are concentrated in the disk midplane ( h _I FIR ∼ h _PI FIR = 0.11 ± 0.01 kpc). Radio emission traces magnetic fields at scales of ≳300 pc, whereas FIR emission probes magnetic fields at the smallest scales of our simulations. These scales are comparable to our spatial resolution and well below the spatial resolution (<300 pc) of existing FIR polarimetric measurements. Finally, we confirm that synchrotron emission traces a combination of the warm neutral and cold neutral gas phases, whereas FIR emission follows the densest gas in the cold neutral phase in the simulation. These results are independent of the ISM magnetic field strength. The complementarity we measure between radio and FIR wavelengths motivates future multiwavelength polarimetric observations to advance our knowledge of extragalactic magnetism.

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