We present^{13}CO(
One of the cornerstone effects in spintronics is spin pumping by dynamical magnetization that is steadily precessing (around, for example, the
 NSFPAR ID:
 10441072
 Publisher / Repository:
 IOP Publishing
 Date Published:
 Journal Name:
 Journal of Physics: Materials
 Volume:
 6
 Issue:
 4
 ISSN:
 25157639
 Page Range / eLocation ID:
 Article No. 045001
 Format(s):
 Medium: X
 Sponsoring Org:
 National Science Foundation
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Abstract J = 1 → 0) observations for the EDGECALIFA survey, which is a mapping survey of 126 nearby galaxies at a typical spatial resolution of 1.5 kpc. Using detected^{12}CO emission as a prior, we detect^{13}CO in 41 galaxies via integrated line flux over the entire galaxy and in 30 galaxies via integrated line intensity in resolved synthesized beams. Incorporating our CO observations and optical IFU spectroscopy, we perform a systematic comparison between the line ratio and the properties of the stars and ionized gas. Higher ${\mathit{\ue23e}}_{12/13}\equiv I{[}^{12}\mathrm{CO}(J=1\to 0)]/I{[}^{13}\mathrm{CO}(J=1\to 0)]$ values are found in interacting galaxies compared to those in noninteracting galaxies. The global ${\mathit{\ue23e}}_{12/13}$ slightly increases with infrared color ${\mathit{\ue23e}}_{12/13}$F _{60}/F _{100}but appears insensitive to other hostgalaxy properties such as morphology, stellar mass, or galaxy size. We also present azimuthally averaged profiles for our sample up to a galactocentric radius of 0.4 ${\mathit{\ue23e}}_{12/13}$r _{25}(∼6 kpc), taking into account the^{13}CO nondetections by spectral stacking. The radial profiles of are quite flat across our sample. Within galactocentric distances of 0.2 ${\mathit{\ue23e}}_{12/13}$r _{25}, the azimuthally averaged increases with the star formation rate. However, Spearman rank correlation tests show the azimuthally averaged ${\mathit{\ue23e}}_{12/13}$ does not strongly correlate with any other gas or stellar properties in general, especially beyond 0.2 ${\mathit{\ue23e}}_{12/13}$r _{25}from the galaxy centers. Our findings suggest that in the complex environments in galaxy disks, is not a sensitive tracer for ISM properties. Dynamical disturbances, like galaxy interactions or the presence of a bar, also have an overall impact on ${\mathit{\ue23e}}_{12/13}$ , which further complicates the interpretations of ${\mathit{\ue23e}}_{12/13}$ variations. ${\mathit{\ue23e}}_{12/13}$ 
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