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A Galactic Scale Magnetized Wind Around a Normal Star-Forming Galaxy by Matthews, A. M.; Cotton, W. D.; Peters, W. M.; Marchetti, L.; Jarrett, T. H.; Condon, J. J.; van der Hulst, J. M.; Moloko, M. is a scholarly article available to read on EtoBox.

What is A Galactic Scale Magnetized Wind Around a Normal Star-Forming Galaxy about?

Galaxy formation theory identifies superwinds as a key regulator of star formation rates, galaxy growth, and chemical enrichment. Thermal and radiation pressure are known to drive galactic-scale winds in dusty starbursting galaxies (e.g. M82), but modern numerical simulations have recently highlighted that cosmic-ray (CR) driven winds may be especially important in normal galaxies with modest star formation rate surface densities. However, CR-driven winds have yet to be conclusively observed -- leaving significant uncertainty in their detailed microphysics. We present MeerKAT radio continuum and HI spectral-line observations of one such normal galaxy, NGC 1532; a nearby ($D\sim15\,\mathrm{Mpc}$) and edge-on ($i \gtrsim 80^{\circ}$) spiral galaxy tidally interacting with its smaller elliptical companion, NGC 1531. We find magnetized, highly-ordered radio continuum loops extending $\sim10$ kpc above and below the disk; visibly connecting discrete star-forming regions in the disk with the nucleus. The deep MeerKAT HI observations place an upper limit on the column density of neutral gas coincident with the outflow to $N_\mathrm{HI} \lesssim 3 \times 10^{19}\,\mathrm{cm}^{-2}$. Unlike

Author

Matthews, A. M.; Cotton, W. D.; Peters, W. M.; Marchetti, L.; Jarrett, T. H.; Condon, J. J.; van der Hulst, J. M.; Moloko, M.

Published

2024

Language

EN