Radial measurements of IMF-sensitive absorption features in two massive
  ETGs
  We make radial measurements of stellar initial mass function (IMF) sensitive
absorption features in the two massive early-type galaxies NGC 1277 and IC 843.
Using the Oxford Short Wavelength Integral Field SpecTrogaph (SWIFT), we obtain
resolved measurements of the NaI0.82 and FeH0.99 indices, among others, finding
both galaxies show strong gradients in NaI absorption combined with flat FeH
profiles at $\sim0.4$\AA. We find these measurements may be explained by radial
gradients in the IMF, appropriate abundance gradients in [Na/Fe] and [Fe/H], or
a combination of the two, and our data is unable to break this degeneracy. We
also use full spectral fitting to infer global properties from an integrated
spectrum of each object, deriving a unimodal IMF slope consistent with Salpeter
in IC 843 ($x=2.27\pm0.17$) but steeper than Salpeter in NGC 1277
($x=2.69\pm0.11$), despite their similar FeH equivalent widths. Independently,
we fit the strength of the FeH feature and compare to the E-MILES and CvD12
stellar population libraries, finding agreement between the models. The IMF
values derived in this way are in close agreement with those from spectral
fitting in NGC 1277 ($x_{\mathrm{CvD}}=2.59^{+0.25}_{-0.48}$ ,
$x_{\mathrm{E-MILES}}=2.77\pm0.31$), but are less consistent in IC 843, with
the IMF derived from FeH alone leading to steeper slopes than when fitting the
full spectrum ($x_{\mathrm{CvD}}=2.57^{+0.30}_{-0.41}$,
$x_{\mathrm{E-MILES}}=2.72\pm0.25$). This work highlights the importance of a
large wavelength coverage for breaking the degeneracy between abundance and IMF
variations, and may bring into doubt the use of the Wing-Ford band as an IMF
index if used without other spectral information.
