Detection probability of light compact binary mergers in future observing runs of the current ground-based gravitational wave detector network

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Table 1.

GW detector network observing run information used in this article.

Index ^(a)	Run	Duration	BNS range ^(b)			V_lT_l
l		(days)	(Mpc)			(10⁻³ Gpc³ yr)
			H	L	V
0	O1	130	70	60	–	0.43
1	O2	268	60	85	25	1.5
2	O3a	183	105	135	45	7.7
3	O3b	147	115	135	50	7.4
4	O4a	235	140	150	–	15
5	O4b	294	155	170	50	23
6	O4c1	63	155	170	50	5.4
7	O4c2	160	155	170	50	14
8	O5 ^(c)	1000	330	330	150	940

Notes.

^(a)

The index l is included to ease the comparison with Eq. (18).

^(b)

Relative to a representative chirp mass, m_c = 1.22 M_⊙.

^(c)

Projection.

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