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Mr.IITIAN007

gud point by Mr.Jack .In fact, for 1 universe ->

#1) Of the 500,000,000,000 galaxies in the universe, 10% are suitable for life in regard to galaxy-cluster density.
This leaves 50,000,000,000 galaxies in which life could occur.

#2) Of the 50,000,000,000 galaxies left in #1, 10% are also of suitable size.
This leaves 5,000,000,000 galaxies in which life could occur.

#3) Of the 5,000,000,000 galaxies left in #2, 10% are also spiral types.
This leaves 500,000,000 galaxies in which life could occur.

#4) Of the 500,000,000 galaxies left in #3, 20% have suitable mass-distribution.
This leaves 100,000,000 galaxies in which life could occur.

#5) Of the 100,000,000 galaxies left in #4, 10% have suitable galaxy locations.
This leaves 10,000,000 galaxies in which life could occur.

#6) Of the 10,000,000 galaxies left in #5, 10% have a suitable galaxy-cluster size.
This leaves 1,000,000 galaxies in which life could occur.

#7) Of the 1,000,000 galaxies left in #6, 10% have a suitable galaxy-cluster location.
This leaves 100,000 galaxies in which life could occur.

#8) Of the 100,000 galaxies left in #7, 20% have a suitable central bulge size.
This leaves 20,000 galaxies in which life could occur.

#9) Of the 20,000 galaxies left in #8, 10% have a suitable galaxy-cluster size.
This leaves 2,000 galaxies in which life could occur.

#10) Of the 2,000 galaxies left in #9, 10% have a suitable galaxy-cluster size.
This leaves 200 galaxies in which life could occur.

#11) Of the 2,000 galaxies left in #10, 5% have a suitably low rate of gamma-ray bursts.
This leaves 10 galaxies in which life could occur.

#12) Of the 10 galaxies left in #11, 10% have a suitable dwarf galaxy absorption rate.
This leaves 1 galaxy in which life could occur.

My god , I don't believe I just typed them ...what the hell just happened .Well to be more practical , the above parameters are not all the qualities and situations which may seriously limit the suitability of planets within those galaxies to support life. There are many more, such as the density of giant galaxies in the early universe; the masses of stars which become hypernovae; the frequency (& closeness) of hypernovae eruptions; the frequency (& closeness) of supernovae eruptions; the number (& closeness) of white dwarf binaries; the timing of solar nebula formation; the density of nearby quasars; the decay rate of cold dark matter particles; and the amount of silicate dust annealing by nebular shocks.

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