Magnetic fields are now widely recognized as critical at many scales to galactic dynamics and structure, including multiphase pressure balance, dust processing, and star formation. Using imposed magnetic fields cannot reliably model the interstellar medium's (ISM) dynamical structure nor phase interactions. Dynamos must be modeled. ISM models exist of turbulent magnetic fields using smallscale dynamo (SSD). Others model the largescale dynamo (LSD) organizing magnetic fields at the scale of the disk or spiral arms. Separately, neither can fully describe the galactic magnetic field dynamics nor topology. We model the LSD and SSD together at a sufficient resolution to use the low explicit Lagrangian resistivity required. The galactic SSD saturates within 20 Myr. We show that the SSD is quite insensitive to the presence of an LSD and is even stronger in the presence of a largescale shear flow. The LSD grows more slowly in the presence of SSD, saturating after 5 Gyr versus 1–2 Gyr in studies where the SSD is weak or absent. The LSD primarily grows in warm gas in the galactic midplane. Saturation of the LSD occurs due to
 Award ID(s):
 1804048
 NSFPAR ID:
 10402209
 Date Published:
 Journal Name:
 Monthly Notices of the Royal Astronomical Society
 Volume:
 517
 Issue:
 1
 ISSN:
 00358711
 Page Range / eLocation ID:
 526 to 542
 Format(s):
 Medium: X
 Sponsoring Org:
 National Science Foundation
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