Accretion disks around supermassive black holes are promising sites for stellar mass black hole mergers detectable with LIGO .
Here we present the results of Monte-Carlo simulations of black hole mergers within 1-d AGN disk models .
For the spin distribution in the disk bulk , key findings are : ( 1 ) The distribution of \chi _ { eff } is naturally centered around \tilde { \chi } _ { eff } \approx 0.0 , ( 2 ) the width of the \chi _ { eff } distribution is narrow for low natal spins .
For the mass distribution in the disk bulk , key findings are : ( 3 ) mass ratios \tilde { q } \sim 0.5 - 0.7 , ( 4 ) the maximum merger mass in the bulk is \sim 100 - 200 M _ { \odot } , ( 5 ) \sim 1 \% of bulk mergers involve BH > 50 M _ { \odot } with ( 6 ) \simeq 80 \% of bulk mergers are pairs of 1st generation BH .
Additionally , mergers at a migration trap grow an IMBH with typical merger mass ratios \tilde { q } \sim 0.1 .
Ongoing LIGO non-detections of black holes > 10 ^ { 2 } M _ { \odot } puts strong limits on the presence of migration traps in AGN disks ( and therefore AGN disk density and structure ) as well as median AGN disk lifetime .
The highest merger rate occurs for this channel if AGN disks are relatively short-lived ( \leq 1 Myr ) so multiple AGN episodes can happen per Galactic nucleus in a Hubble time .