Back to LIST WG1B home.
Home of the SMBH source specification MLDC subgroup
- Here you can see some figures produced for m1=10^6, m2 = 2×10^6. In the (Fig1) I plot frequency as function of time, separation as function of time, average over inclination/postition SNR accumulated with time, accumulative SNR (a partucular choice of inclination and direction). In the (Fig2) I plot S(f) (from Shane’s sensitivity generation page, default params) and SPA for h, averaged over angles, optimal and for a particular direction and inclination. SNR^2 = 4\int (h_{spa})^2/S(f) df. For this system I have
z ~ 1.5 D_L = 10Gpc, <SNR> = 1086, for waveform truncated at 6M, and <SNR> = 798 for waveform trancated at 7M (more likely due to tapering)
- I have written code for random generation of parameters with the following range (”U” stands for uniform):
m1 U[1, 5]x10^6 solar mass, m2 = m1/x, where x is U[1,4]; inclination and theta_source : cos(...) is U[-1,1]; polarization and phi_source U[0, 2pi]; coalescence time U[178-20, 178+20] days;
- I have fixed distance to 10Gpc (all values quoted here are red shifted) and performed Monte Carlo simulation using 10000 random signals. SNR was estimated using stationary phase approximation and 0-generation (Cutler’98). In this figure (
), I plot m1 vs. m2 in units 10^6 solar mass; in this figure (
) I plot coalescence time as function of masses; in this figure (
) I plot initial frequency as function of masses, in this figure (
) I plot average SNR as function of masses; In this figure (
) I plot SNR for random signals; finally, in this figure (Fig8) I plot SNR of random signals as function of masses in order to show min SNR.
