1. GW150914 – the first GW detection ! Is it a start of GW astronomy ? If “yes” then which ? «Счастлив, кто посетил сей мир в его минуты роковые !...» Ф.Тютчев (ст. «Цицерон») Руденко В.Н., ГАИШ, ОАС 19 фев. 2016 (9дней после NSF пресс конференции)

2. Frequency Range: (50 – 1500) Hz Blind All Sky Searching Sources: - compact binary systems evolution (inspiral, merging, ring down) - supernova collapse events - continuous GW radiation (Pulsars) - stochastic GW background - Triggered Search ( Astro-gravity associations)

3. Non modeled Bursts outputs of two GW detectors: vectors a, b total energy : E = normalized and integrated at the it is reduced to variables: Burst’s Excess Power: Burst’s Cross Power: Basic searching algorithms

4. Sine-gaussian waveform

5. Wavelet transform

7. Results of the all-sky search for gravitational wave burst signals are presented for the first joint LIGO (S5) and Virgo VSR1 runs in 2006-2007.  The analysis has been performed with three different search algorithms in a wide frequency band between 50-6000 Hz. No plausible GW candidates have been identified.  As a result, a limit on the rate of burst GW signals (combined with the LIGO results from the first S5 year) has been established: less than 2 events per year at 90% confidence level with sensitivity in the range 6-20 × 10 −22 Hz −1/2  This rate limit is increased by more than an order of magnitude compared to the previous LIGO runs. S.Klimenko, GWDAW14, January 26, 2010, Rome, LIGO-G1000033-v8

9. GW-experiment: News Fig. 1. Advanced Virgo sensitivity curve compared with Virgo and LIGO design and current bar sensitivity. Violin modes are not displayed for clarity

10. 10 Coalescing Binaries Source: coalescence of compact binary stars (BNS, BBH, NS/BH)‏ – Waveform accurately modelled in the first and last phase Allows matched filtering – Less known in the “merger” phase Interesting physics here, for instance for BNS – Rate very uncertain A few events/year could be accessible to the LSC-Virgo network chirp

11. PRL_116, 061.102 (2016) FIG2

12. event GW150914 Sept. 14, 2015 at 09:50:45 UTC. all time series are filtered with a 35–350 Hz band-pass filter and band-reject filters to remove the strong instrumental spectral lines ; GW150914 arrived first at L1 and ~ 6.9 ms later at H1; (for a visual comparison, the H1 data are also shown, shifted in time by this amount and inverted to account for the detectors’ relative orientations); second row: solid lines show a numerical relativity waveform for a system with parameters consistent with those recovered from GW150914 third row: residuals after subtracting the numerical relativity waveform from the filtered detector time series. bottom row: a time-frequency representation of the strain data, showing the signal frequency increasing over time.

13. 35 Hz  150 Hz,   0.2 sec, orbital frequency 75 Hz M  30M 0 m 1 +m 2  70 M 0 2GM / c 2  210 km NS –NS, BH-NS are rejected Chirp mass SNR ~ 24 (!), h ~ 2 10^{-21}, D ~ 400 Mpc (!)

15. Advanced LIGO vs. Initial LIGO 15 15-20 Mpc BNS inspiral range ~200 Mpc BNS inspiral range

16. Detection of Neutron Star Binaries Coalescence LIGO program 2015 - 2022 Neutron Star Binaries: Advanced LIGO: ~ 200 Mpc “Detection rate” ~ 10/year Class. Quant. Grav. 27, 173001 (2010) (Initial LIGO: ~15 Mpc, Rate ~1/50years)

17. Expected Science with GW info channel Fundamental Physics Is the nature of gravitational radiation as predicted by Einstein? Is Einstein theory the correct theory of gravity? Are black holes in nature black holes of GR? Are there naked singularities? Astrophysics What is the nature of gravitational collapse? What is the origin of gamma ray bursts? What is the structure of neutron stars and compact objects? Cosmology How did massive black BH at galactic nuclei form and evolve? What is dark energy? What phase transitions took place in the early Universe? What were the physical conditions at the big bang? Moriond, March 2011 Key strategy  multi-messengers astronomy

18. Historical Periods for US GW Detectors Initial LIGO! » 1983 MIT and Caltech jointly present results of the km-scale interferometer study to NSF. Receive endorsement by NSF committee on new large programs in physics. ! » 1990 The US National Science Board (NSB) approves the LIGO construction proposal, which envisions Initial LIGO followed by Advanced LIGO.! » 1994-1995 Site construction begins at the Hanford and Livingston locations.! » 2002 The first coincident operation of Initial LIGO interferometers with the GEO600 interferometer.! » 2006 Initial LIGO design sensitivity achieved. ! Advanced LIGO! » 1999 The LSC Concept Paper for Advanced LIGO completed.! » 2003 LIGO Laboratory submits proposal to NSF for Advanced LIGO proposal.! » 2006 NSF conducts review of Advanced LIGO Construction. ! » 2008 Advanced LIGO Construction is funded by NSF.! » 2014 Advanced LIGO Construction completed.! » 2015 Advanced LIGO begins science operations! D.Reitz, ET7 conf. Florence 2-3 Feb 2016

19. The Terrain in the Next Few Years The advanced detectors should make detections in the 2016-2018 frame! The nature of the classes of detected sources will provide valuable input (but not completely dictated) the science case for a 3G detector network! More importantly, the window of GW astronomy will open into the arenas of frontier strong field physics, high energy astrophysics, multi-messenger astronomy! The case for proposing a 3G detecto r will never be as good as it is in the next few years! Start with rough estimates of the costs! » Guess: Upgrades of detectors in current facilities: $100-$150M (in 2016 $) ! » Guess: New facilities with new detectors: $1- 1.5B (in 2016 $)! A new observatory with 10 or 20 or 40 km arm lengths will require a new site! R&D themes are common for Voyager and Cosmic Explorer Given time scales and costs (Voyager $150M funding in 2020; CE $1.5B in 2030), optimistically it might be possible to do both ! D.Reitz, ET7 conf. Florence 2-3 Feb 2016

20. Let’s hope that GW150914 will be not the unique event ! Thanks for attention.