  We present results obtained from near-infrared JHK spectroscopic observations
of novae V2491 Cyg and V597 Pup in the early declining phases of their 2007 and
2008 outbursts respectively. In both objects, the spectra displayed emission
lines of HI, OI, HeI and NI. In V597 Pup, the HeI lines were found to
strengthen rapidly with time. Based on the observed spectral characteristics,
both objects are classified as He/N novae. We have investigated the possibility
of V2491 Cyg being a recurrent nova as has been suggested. By studying the
temporal evolution of the line widths in V2491 Cyg it appears unlikely that the
binary companion is a giant star with heavy wind as in recurrent novae of the
RS Oph type. Significant deviations from that of recombination case B
conditions are observed in the strengths of the HI lines. This indicates that
the HI lines, in both novae, are optically thick during the span of our
observations. The slope of the continuum spectra in both cases was found to
have a \lambda^-(3-3.5) dependence which deviates from a Rayleigh-Jeans
spectral distribution. Both novae were detected in the post-outburst super-soft
X-ray phase; V2491 Cyg being very bright in X-rays has been the target of
several observations. We discuss and correlate our infrared observations with
the observed X-ray properties of these novae.
