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• W4384133715 abstract "Abstract We present the analysis of the magnetic field ( B -field) structure of galaxies measured with far-infrared (FIR) and radio (3 and 6 cm) polarimetric observations. We use the first data release of the Survey of extragALactic magnetiSm with SOFIA of 14 nearby ( <?CDATA $lt 20$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:mo><</mml:mo> <mml:mn>20</mml:mn> </mml:math> Mpc) galaxies with resolved ( <?CDATA $5^{primeprime} mbox{--}18^{primeprime} ;$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:mn>5</mml:mn> <mml:mo accent=false>″</mml:mo> <mml:mo>–</mml:mo> <mml:mn>18</mml:mn> <mml:mo accent=false>″</mml:mo> <mml:mo>;</mml:mo> </mml:math> 90 pc–1 kpc) imaging polarimetric observations using SOFIA/HAWC+ from 53 to 214 μ m. We compute the magnetic pitch-angle ( <?CDATA ${{rm{Psi }}}_{B}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:msub> <mml:mrow> <mml:mi mathvariant=normal>Ψ</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>B</mml:mi> </mml:mrow> </mml:msub> </mml:math> ) profiles as a function of the galactocentric radius. We introduce a new magnetic alignment parameter ( ζ ) to estimate the disordered-to-ordered ratio of spiral B -fields. We find FIR and radio wavelengths to not generally trace the same B -field morphology in galaxies. The <?CDATA ${{rm{Psi }}}_{B}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:msub> <mml:mrow> <mml:mi mathvariant=normal>Ψ</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>B</mml:mi> </mml:mrow> </mml:msub> </mml:math> profiles tend to be more ordered across all galactocentric radii in radio ( <?CDATA ${zeta }_{6mathrm{cm}},=,0.93pm 0.03$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:msub> <mml:mrow> <mml:mi>ζ</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>6</mml:mn> <mml:mi>cm</mml:mi> </mml:mrow> </mml:msub> <mml:mspace width=0.25em /> <mml:mo>=</mml:mo> <mml:mspace width=0.25em /> <mml:mn>0.93</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.03</mml:mn> </mml:math> ) than in FIR ( <?CDATA ${zeta }_{154mu {rm{m}}}=0.84pm 0.14$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:msub> <mml:mrow> <mml:mi>ζ</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>154</mml:mn> <mml:mi>μ</mml:mi> <mml:mi mathvariant=normal>m</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>0.84</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.14</mml:mn> </mml:math> ). For spiral galaxies, FIR B -fields are 2%–75% more turbulent than the radio B -fields. For starburst galaxies, we find that FIR polarization is a better tracer of the B -fields along the galactic outflows than radio polarization. Our results suggest that the B -fields associated with dense, dusty, turbulent star-forming regions (those traced at FIR) are less ordered than warmer, less dense regions (those traced at radio) of the interstellar medium. The FIR B -fields seem to be more sensitive to the activity of the star-forming regions and molecular clouds within a vertical height of a few hundred parsecs in the disk of spiral galaxies than the radio B -fields." @default.
• W4384133715 created "2023-07-14" @default.
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• W4384133715 date "2023-07-01" @default.
• W4384133715 modified "2023-10-18" @default.
• W4384133715 title "Extragalactic Magnetism with SOFIA (SALSA Legacy Program). V. First Results on the Magnetic Field Orientation of Galaxies" @default.
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