天体物理学报lgo引力波探测器释疑.pptxVIP

LIGO: Initiating the Advanced Detector Era for Gravitational Wave Astrophysics;Outline;LIGO Addresses Fundamental Questions in Physics and Astronomy;The LIGO Scientific Collaboration;Albert Einstein;Existence proof: PSR 1913+16;Gravitational Waves;LIGO Interferometry;The LIGO Laboratory Sites;S6 – Last Science Run of Initial LIGO Era ;LIGO Astrophysics;Binary CoalescencesS5/S6 all-sky blind searchTightest rate limits from LIGO Observations;D ~ 6500 light-years Young and rapidly spinning down Spin frequency nEM = 29.8 Hz ? nGW = 2 nEM = 59.6 Hz Spin down due to: electromagnetic braking? particle acceleration? GW emission? Observed luminosity of the Crab nebula accounts for 1/2 spin down power S6 results: Astrophys. J. 785 (2014) 119 h 1.6 x 10-25 9X below the EM spin down limit (using restricted priors on orientation) GW energy upper limit:  1.2% of radiated energy is in GWs Ellipticity upper limit: e 8.6x 10-5 ;EFST, Shanghai, China 13 October 2014;Advanced LIGO Upgrade;Advanced LIGO:A 2nd generation detector;Advanced LIGO:A 2nd generation detector;Advanced LIGO:A 2nd generation detector;Recent snapshot of interferometer performance - LLO;Operated as a phased array – aperture synthesis GW astronomy: - Enhance detection confidence - Localize sources - Decompose the polarization of gravitational waves;Localization:International Array of GW Interferometers;Summary;NASA/WMAP;4km @ Washington + 4km @ Lousiana + 4km @ India + 3km @ Italy;LIGO’s mission;LIGO Addresses Fundamental Questions in Physics and Astronomy;An interferometer is really a microphone;How to make a very sensitive interferometer(with suspended mirrors);LIGO limiting noise floor;e;S5: Triggered GRB searches