Expected detection rate of gravitational wave estimated by Short Gamma-Ray Bursts

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1 Expected detection rate of gravitational wave estimated by Short Gamma-Ray Bursts Daisuke Yonetoku (Kanazawa Univ.), Tatsuya Sawano, Asuka Toyanago, Yasuaki Kagawa (Kanazawa U.) Takashi Nakamura (Kyoto U.), Keitaro Takahashi (Kumamoto U.) Kazumi Kashiyama (Penn S. U.), Kunihito Ioka (KEK) Experimental Part: Tatsuya Sawano, K. Yoshida, Yasuaki Kagawa, Masao Ina, Yu Endo, Satoshi Yagitani, Yoshiya Kasahara (Kanazawa U.) Atsushi Harayama and Hirokazu Ikeda (ISAS/JAXA) Special Thanks : Makoto Arimoto (TITech) 1. SGRB rate estimated with the Epeak brightness correlation arxiv: , ApJ, 789, 65 (2014) 2. Wide field X-ray monitor aboard micro satellite project Kanazawa-SAT 3 UNISEC: Gravitational Wave Physics and Astronomy Workshop 2015 (17 20 June, Osaka

2 Long & Short GRBs Short GRB Long GRB Number of Events NS-NS NS-BH Duration (sec) LGRBs (T > 2 sec) Massive star explosion (M>40M sun ) Associated with Supernovae (energetic Hypernovae) E = ergs Black Hole & relativistic jet SGRBs (T < 2 sec) Merging Neutron Star Binaries (?) E = ergs Black Hole & relativistic jet (?)

3 Gamma-Ray Spectrum Band et al α: low-energy spectral index β: high-energy spectral index E 0 :break energy E α Briggs et al Non-thermal spectrum Synchrotron radiation from accelerated electrons by the relativistic shock. Maybe νf ν E β Maximum of νf ν spectrum Peak energy (E peak ) Epeak

4 E peak Luminosity Correlation of LGRBs/SGRBs LGRBs SGRBs LGRB (DY et al. 2004, 2010) LL pp = 4ππdd LL 2 FF pp = AA[EE pp (1 + zz)] dd LL AA 1.6 = EE (1 + zz) 1.6 4ππFF pppppppp pp SGRB (Tsutsui et al. 2013) LL pp = 4ππdd LL 2 FF pp = BB[EE pp (1 + zz)] 1.6 DY et al. (2004, 2010) for LGRBs Tsutsui, DY + (2013) for SGRBs Epeak (1+z) [kev] 2 dd LL BB 1.6 (1 + zz) 1.6 = EE 4ππFF pppppppp pp We can use the correlation as the Luminosity/Distance indicator.

5 Event selection CGRO/BATSE current burst catalog (1) 100 brightest SGRBs with T 90 < 2 sec (2) Spectral parameters are obtained for 72 SGRBs. (for remaining 28, poor statistics and variable BGD condition) (3) We succeeded in calculating the pseudo-z for all 72 SGRBs. CGRO BATSE life time = 9.2 years Fraction of sky coverage = Trigger efficiency > % for F = 1 ph/cm2/s Effective life time = 4.4 years

6 64msec peak luminosity (10 52 erg/s) Redshift Distribution Flux limit F > 4x10-6 erg/cm 2 /s Redshift <θ j > ~ 6 degrees Absolute SGRB Rate (events/mpc 3 /yr) Cumulative Number N(>L) SGRB Luminosity Formation Function Rate with L > erg/sec Ψ(L) L -0.84±0.09 (1+z) 6.0±1.7 Luminosity Redshift (10(1+z) 52 erg/s) We used a non-parametric method. (Lynden-Bell 1971, Petrosian 1993, etc.) Local Rate x events/mpc 3 /yr Fong et al Local Rate including geometrical factor x 10-7 events/mpc 3 /yr

7 Expected Detection Rate of G-W Local Rate including geometrical factor x 10-7 events/mpc 3 /yr (Lower Limit) NS-NS binary ( R < 200 Mpc) events/yr NS-BH binary ( R < 680 Mpc) events/yr For M BH = 10 M sun & M NS = 1.4 M sun Factor of 4 There are many dimmer SGRBs, and the expectation rate will increase by a factor of 4 at least. Advanced-LIGO s first science run (from September 2015) NS-NS binary (80 Mpc) : ~ 1 events/yr NS-BH binary (270 Mpc) : ~ 27 events/yr

8 Establishment of gravitational wave astronomy with wide field X-ray monitor by Kanazawa-SAT 3 Daisuke Yonetoku Tatsuya Sawano Kazuki Yoshida, Yasuaki Kagawa, Masao Ina, Yu Endo, Asuka Toyanago (Kanazawa Univ.) A. Harayama and H. Ikeda (ISAS/JAXA) Satellite Bus System Satoshi Yagitani, Yoshiya Kasahara, Tomohiko Imachi, Yoshitaka Goto, Mitsunori Ozaki (Kanazawa U.) Special thanks : M. Arimoto (TITech)

9 Extended soft X-ray Emission Perley et al. (2009) Kagawa, DY, + (2015) Swift-BAT Swift-XRT Total energy of Extended X-ray Emission is comparable to the prompt impulse. Spectrum is softer than the short prompt. The ratio of SGRBs having E.E. is ~ 1/2.

10 Detector Configurations Sensitivity (8σ detection) Peak photon flux Detector Si strip detector x 2 Energy range Kanazawa-SAT cm kev Field of view Effective area Angular resolution Sensitivity 1 20 kev 1 str (full coded) Swift-BAT 5200 cm kev 50 cm 2 (for ½ aperture ratio) 30 arcmin (geometrical) < 10 arcmin (photon stat.) (3-7)x10-8 (erg/cm2/s) : rate ~ 10-8 (erg/cm2/s) : imaging 50µmt, 35µmt 1-dimensional random mask 0.30mm X 17cm 7cm 8cm 76.8 mm Y 256 strips D = 7cm Si strip d = 0.3mm pitch 10

11 X-ray Imaging Experiment ΔE = 1.3 kev 5.9 kev 55 Fe LD = 2.0 kev pedestal Radio Isotope 8.80 mm 7.46 mm Imaging experiment with Bread-Board Model Readout from 2.0 kev. (we will improve the design and performance of ASIC) X-ray image is obtained with radio isotopes and X-ray beam line. 11

12 Schedule FY Detector Proto-type Model Detector Flight Model Satellite Engineering Model Satellite Flight Model Hardware Verification Software development Hardware Verification Software development Hardware Integration Test Software development Hardware Software development launch Operation

13 Summaries We estimated the SGRB rate with Epeak Luminosity correlation Local rate is > 1.15 x 10-7 events/mpc 3 /yr (Lower Limit) NS-NS binary ( R < 200 Mpc) events/yr NS-BH binary ( R < 680 Mpc) events/yr We are developing the wide field X-ray imaging detector aboard the micro satellite (50cm cube, 50 kg) Kanazawa-SAT 3. We will launch Kanazawa-SAT 3 in We will support iwf-maxi project and contribute to establish the G-W astronomy to find X-ray counterparts.

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