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Detection of gamma-rays emitted by radioactive isotopes synthesized instellar explosions can give important insights into the processes that powertransients such as supernovae, as well as providing a detailed census of theabundance of different isotope species relevant to the chemical evolution ofthe Universe. Observations of nearby supernovae have yielded observationalproof that $^{57}$Co powered the late-time evolution of SN1987A's lightcurve,and conclusive evidence that $^{56}$Ni and its daughter nuclei power the lightcurves of Type Ia supernovae. In this paper we describe the prospects fordetecting nuclear decay lines associated with the decay of $^{48}$V, thedaughter nucleus of $^{48}$Cr, which is expected to be synthesised in largequantities - $M_{\mathrm{Cr}}\sim1.9\times10^{-2}\,\mathrm{M_\odot}$ - intransients initiated by explosive helium burning ($\alpha$-capture) of a thickhelium shell. We calculate emergent gamma-ray line fluxes for a simulatedexplosion model of a thermonuclear explosion of carbon-oxygen white dwarf coreof mass $0.45\,M_{\odot}$ surrounded by a thick helium layer of mass$0.21\,M_{\odot}$. We present observational limits on the presence of $^{48}$Vin nearby SNe Ia 2014J using the \textit{INTEGRAL} space telescope, excluding a$^{48}$Cr production on the surface of more than $0.1\,\mathrm{M_{\odot}}$. Wefind that the future gamma-ray mission AMEGO will have an approximately 5 percent chance of observing $^{48}$V gamma-rays from such events during thecurrently-planned operational lifetime, based on our birthrate predictions offaint thermonuclear transients. We describe the conditions for a $3\sigma$detection by the gamma-ray telescopes \textit{INTEGRAL}/SPI, COSI and AMEGO.

Prospects of direct detection of $^{48}$V gamma-rays from thermonuclear supernovae