AKARI IRC infrared 2.5-5 micron spectroscopy of a large sample of
  luminous infrared galaxies
  We present the results of our systematic infrared 2.5-5 micron spectroscopy
of 60 luminous infrared galaxies (LIRGs) with infrared luminosities L(IR) =
10^11-12 Lsun, and 54 ultraluminous infrared galaxies (ULIRGs) with L(IR) >
10^12 Lsun, using AKARI IRC. AKARI IRC slit-less spectroscopy allows us to
probe the full range of emission from these galaxies, including spatially
extended components. The 3.3 micron polycyclic aromatic hydrocarbon (PAH)
emission features, hydrogen recombination emission lines, and various
absorption features are detected and used to investigate the properties of
these galaxies. Because of the relatively small effect of dust extinction in
the infrared range, quantitative discussion of these dusty galaxy populations
is possible. For sources with clearly detectable Br beta (2.63 micron) and Br
alpha (4.05 micron) emission lines, the flux ratios are found to be similar to
that predicted by case B theory. Starburst luminosities are estimated from both
3.3 micron PAH and Br alpha emission, which roughly agree with each other. In
addition to the detected starburst activity, a significant fraction of the
observed sources display signatures of obscured AGNs, such as low PAH
equivalent widths, large optical depths of dust absorption features, and red
continuum emission. The energetic importance of optically elusive buried AGNs
in optically non-Seyfert galaxies tends to increase with increasing galaxy
infrared luminosity, from LIRGs to ULIRGs.
