Primordial Black Holes and Cosmological Phase Transitions Report ...

PBHs and Cosmological Phase Transitions 186
log 10Βtk
log 10Βtk
log 10Βtk
0
-20
-40
-60
-80
0
-20
-40
-60
-80
0
-20
-40
-60
-80
a n1.56, log 10t1s0
-3 -2 -1 0 1 2
log10 tk
1 s
c n1.54, log 10t1s1
-1 -0.5 0 0.5 1 1.5
log10 tk
1 s
e n1.60, log 10t1s2
-0.5 0 0.5 1 1.5 2 2.5 3
log10 tk
1 s
log 10Βtk
log 10Βtk
log 10Βtk
0
-20
-40
-60
-80
0
-20
-40
-60
-80
0
-20
-40
-60
-80
b n1.62, log 10t1s0
-3 -2 -1 0 1 2
log10 tk
1 s
d n1.66, log 10t1s1
-2 -1 0 1 2 3
log10 tk
1 s
f n1.68, log 10t1s2
-1 0 1 2 3 4
log10 tk
1 s
Figure 101: The fraction of the universe going into PBHs in a universe with a
running–tilt power spectrum when: (a) n+ =1.52 and t+ = 1 s; (b) n+ =1.62
and t+ = 1 s; (c) n+ =1.54 and t+ = 10 s; (d) n+ =1.66 and t+ = 10 s;
(e) n+ = 1.60 and t+ = 100 s; (f) n+ = 1.68 and t+ = 100 s. The dark
curve represents the radiation contribution and the cyan curve represents the
contribution from the electron–positron annihilation epoch. Also shown (top of
figure, in maroon) is the observational limit.