New constraints on the primordial black hole number density from Galactic γ-ray astronomy

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Table 1:

Constraints on PBHs of mass $M_{\star }$ for different dark matter distributions^a.
DM distribution	$f(M_{\star})$	$\Omega_{\rm PBH}(M_{\star})$	$\beta(M_\star)$
Moore	$6.04 \pm 0.05\times 10^{-9}$	$1.38\times 10^{-9}$	$0.98\times 10^{-27}$
Moore $_{\rm c}$	$1.07 \pm 0.07\times 10^{-9}$	$0.24\times 10^{-9}$	$0.17\times 10^{-27}$
NFW	$6.70 \pm 0.05\times 10^{-9}$	$1.53\times 10^{-9}$	$1.08\times 10^{-27}$
NFW $_{\rm c}$	$1.93 \pm 0.08\times 10^{-9}$	$0.44\times 10^{-9}$	0.31 10^-27
isothermal	$11.62 \pm 0.04\times 10^{-9}$	$2.65\times 10^{-9}$	$1.87\times 10^{-27}$

^a f is the maximum fraction of dark matter in the form of PBHs, $\Omega_{\rm PBH}(M_{\star})$ is the corresponding cosmological density, and $\beta$ is the fraction of regions undergoing collapse when the mass enclosed within the cosmological horizon was $M_{\star }$ .

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