Binary compact object coalescence rates: The role of elliptical galaxies
  We estimate binary compact object merger detection rates for LIGO, including
the binaries formed in ellipticals long ago. Specifically, we convolve hundreds
of model realizations of elliptical- and spiral-galaxy population syntheses
with a model for elliptical- and spiral-galaxy star formation history as a
function of redshift. Our results favor local merger rate densities of 4\times
10^{-3} {Mpc}^{-3}{Myr}^{-1} for binary black holes (BH), 3\times 10^{-2}
{Mpc}^{-3}{Myr}^{-1} for binary neutron stars (NS), and 10^{-2}
{Mpc}^{-3}{Myr}^{-1} for BH-NS binaries. Mergers in elliptical galaxies are a
significant fraction of our total estimate for BH-BH and BH-NS detection rates;
NS-NS detection rates are dominated by the contribution from spiral galaxies.
Using only models that reproduce current observations of Galactic NS-NS
binaries, we find slightly higher rates for NS-NS and largely similar ranges
for BH-NS and BH-BH binaries. Assuming a detection signal-to-noise ratio
threshold of 8 for a single detector (as part of a network), corresponding to
radii \Cv of the effective volume inside of which a single LIGO detector could
observe the inspiral of two 1.4 M_\sun neutron stars of 14 Mpc and 197 Mpc, for
initial and advanced LIGO, we find event rates of any merger type of 2.9*
10^{-2} -- 0.46 and 25-400 per year (at 90% confidence level), respectively. We
also find that the probability P_{detect} of detecting one or more mergers with
this single detector can be approximated by (i) P_{detect}\simeq 0.4+0.5\log
(T/0.01{yr}), assuming \Cv=197 {Mpc} and it operates for T years, for T between
2 days and 0.1 {yr}); or by (ii) P_{detect}\simeq 0.5 + 1.5 \log \Cv/32{Mpc},
for one year of operation and for $\Cv$ between 20 and 70 Mpc. [ABRIDGED]
