From Nothing to Everything BBH and the Next Generation of GW Detectors Matthew Evans, MIT

From Nothing to Everything We recently detected our first GW from BBHs All detections have been at low red-shift What does the future hold for ground-based GW detection? How do we go from the local universe to high-z? May 8, 2017 Matthew Evans at BHI

LIGO Noise: Progress Previous best Present Upgrade Design Phys. Rev. Lett. 116, 131103 May 8, 2017 Matthew Evans at BHI

Incredible Isolation Big Scary Laser Massive Superoptics May 8, 2017 Matthew Evans at BHI

Big Scary Laser Advanced LIGO still has a lot of unexplored potential. There is almost a factor of 3 more sensitivity to gain with the Advanced LIGO design. Much of what is left to be done comes down to using all of the available laser power, and resolving technical problems that arise along the way. May 8, 2017 Matthew Evans at BHI

LIGO Noise: “Range” Previous best BBH 400Mpc Present BBH 4Gpc Upgrade Design Upgrade Phys. Rev. Lett. 116, 131103 May 8, 2017 Matthew Evans at BHI

Advanced LIGO Sensitive Volume Rate roughly 50 BBH mergers each year in a volume of 1 Gpc3 About 10 million galaxies per Gpc3 Advanced LIGO range now ~ 0.1 to 1 Gpc, depending on system mass We expect several more BBH events in the current observing. Initial Range Advanced Range Initial Range Advanced Range May 8, 2017 Matthew Evans at BHI

LIGO Noise: Progress Previous best Present Upgrade Design Phys. Rev. Lett. 116, 131103 May 8, 2017 Matthew Evans at BHI

May 8, 2017 Matthew Evans at BHI

Future Improvements (i.e., how I spend my time at MIT) Research aimed at making better detectors is on going in labs at MIT and elsewhere in the world The next upgrade will involve the use of squeezed states of light to reduce quantum noise in the interferometer Thermal noise can be reduced with better materials and cryogenic operation The next big leap in sensitivity will come from a longer interferometer…work in progress! May 8, 2017 Matthew Evans at BHI

Future Detectors May 8, 2017 Matthew Evans at BHI

Over the next 20 years… Sensitivity progression from the present (O1 and O2) to potential detectors of the 2030s. May 8, 2017 Matthew Evans at BHI

~106 “detectable” “detectable” “high SNR” ~103 “high SNR” M3: high natal kicks “detectable” “high SNR” ~103 “high SNR” M1: standard M10: MBH < 50 Mo May 8, 2017 Matthew Evans at BHI

M1 model 2 3 4 “detectable” “high SNR” May 8, 2017 2 3 4 M1 model “detectable” “high SNR” May 8, 2017 Matthew Evans at BHI

Compact Binaries from Everywhere! credit: John Miller (MIT) BNS NSBH BBH POP3? First Stars Formed High SNR Signals! CE PBH? May 8, 2017 Matthew Evans at BHI

The Message Advanced LIGO detection rate may reach ~1 per week mostly BBH z < 1 Near-term upgrades will increase the range by 2 rate may be ~1 per day Next generation detectors will reach high-z BBH and BNS detection rate will be mostly determined by astrophysical population, not detector sensitivity (peak near z ~ 3?) Many high SNR events with available for precision tests May 8, 2017 Matthew Evans at BHI