PoS(ICRC2019)681 http://pos.sissa.it/ , [email protected] , 120 days after the trigger time, we derive and report the corresponding up- ∼ † ; Nissim Fraija and M. Magdalena González ∗ [email protected] Speaker. For collaboration list, see PoS(ICRC2019) 1177. The detection of the gravitationalastronomy. wave For GW170817 the defined first a time, breakthrough aGravitational-Wave Observatory in gravitational (LIGO) wave multi-messenger and transient Virgo interferomter detected was by associated the withtromagnetic a Laser gamma-ray faint Interferometer elec- counterpart reported byon the the Gamma-ray Fermi satellite. Burst Monitor GRBcovering 170817A (GBM) was a aboard followed large up fraction by of anHigh enormous the Altitude observational Water electromagnetic Cherenkov campaign (HAWC) spectrum. gamma-ray observatory In to(VHE) TeV search this photons for in work, very-high-energy coincidence with we the use X-raywere emission the observed from up GRB data 170817A. to Since from no counts per limits in the energywith range similar from features proposed 1 by to A. 100 von TeV. Kienlin. In addition, we extend the analysis to GRBs † ∗ Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 36th International Cosmic Ray Conference -ICRC2019- July 24th - August 1st, 2019 Madison, WI, U.S.A. [email protected] Antonio Galván The HAWC Collaboration https://www.hawc-observatory.org/collaboration/icrc2019.php Instituto de Astronomía, UNAM. E-mail: Search for very-high-energy emission with HAWC from GW170817 event PoS(ICRC2019)681 ] after 3 , identi- 1 < 5 s, the ]. For this 2s [ 90 20 T ∼ , Antonio Galván 19 , 18 , 17 (J2000.0). Immediately, , ◦ 16 30 , discussion and results are , 4 − 15 ] emissions 9 and 16 days after 8 = δ and ] by the LIGO and Virgo observatories. m 2 , 20 1 h ] and radio [ 7 we present the bursts studied here. In Section ]. In general, TeV photons are likely generated 12 , 2 6 = 14 1 , α 13 , for an energy range of 4 - 100 TeV was derived. 12 1 , − s 11 2 ], using the data from the Fermi-GBM 10 yr catalog , ] analyzed the GBM catalog looking for similarities with other − 21 10 21 , 9 ergcm 10 − 10 × ]. Since the detection of the prompt emission, several of optical telescopes on 7 . 4 120 days after the trigger time. Different models based on external shocks have been -ray observatories: the High Energy Stereoscopic System (H.E.S.S.) Telescope and the γ ∼ 10 hours after the merger. The most interesting detection to the purposes of TeV counterpart FERMIGBRST - Fermi GBM Burst Catalog GRB 170817A triggered Fermi GBM at 2017 September 17 12:41:20 UTC. The Fermi GBM The GW170917/GRB 170817A event a few hours later entered the field of view of two of Recently von Kienlin et. al. [ The paper is arranged as follows. In Section Recently, A. von Kienlin in [ One of the events defining a breakthrough in the multi-messenger astronomy is the detection 1 ∼ we describe briefly the analysis performed. Finally, in Section ] 5 localization constrained this burst to a region at the TeV presented. 2. Follow-up to GRB 170817A and sGRBs alike. GRB 170817A was followed up bythe a electromagnetic massive spectrum. observational In campaign X-ray coveringNewton bands, a satellites, large this fraction burst in of was optical detected bands, byTelescope and the non-thermal in Chandra observations radio, and was bands XMM- at revealed 3 by and the 6 Hubble GHz were Space identified by the Very Large Array (VLA). HAWC observatory. Observations with the HAWC experimentUTC started and on finished 2017 August 2.03 17 hr at later.an 20:53 Although upper limit no of significant 1 excess of counts was detected by HAWC, sGRBs. These authors proposed a sampleThis of is sGRBs derived with from similar the characteristics GBM to data GRB by 170817A. applying cuts on the observable features (e.g. 3 the prompt emission, respectively. For the firstreached time in GRBs astronomy, the maximumdeveloped fluxes to were explain this burst [ reason, in this work we search for TeV emission up to thefied, time applying of a the two-step maximum selection X-ray supported13 flux. by sGRBs a with statistical similar criteria features using to GRBit bayesian 170817A. is block Since ideal analysis, HAWC and scans possible the to whole sky search continuously, for TeV emission in coincidence with these bursts. searches came from the observation of the X-ray [ ground started one of the mostdetection exhaustive follow of up the campaigns optical of counterparts the came[ modern from astronomy. the The Large first Binocular Telescope Observatory (LBT) by synchrotron self-Compton (SSC) emission from X-ray photons [ of the gravitational wave (therefore GW) GW170817 [ Follow up to GRB 170817A 1. Introduction This gravitational wave was identified aswas associated a with binary a system short consisting Gammathe of Ray neutron GW Burst stars. event. (from The now sGRB merger TheFermi or spacecraft GRB GRB) [ produced was detected by the Gamma-ray Burst Monitor (GBM) on board the PoS(ICRC2019)681 ]. 24 ]) and 3 is small. As ◦ Antonio Galván 45 ∼ . We have estimated a ]. Here, specific details 1 22 the transit duration and the 5 with a pivot energy of 1 . 1 2 ] shows. − 23 ]. Finally, for those bursts with unknown 25 0.009 (similar to the GRB170817A [ ∼ 2 ]. The maps are combined to cover consecutive time 22 ], only GRB 150101B, GRB 170111A and GRB 170817A . 21 1 . The optimal sensitivity of HAWC lies in the range of declination of ◦ 0.1 & and energies of 1 and 100 TeV. ] ◦ ] for a source like the crab nebula, it is expected that 90% of the signal arrives within 64 22 , ◦ 26 and the contribution from those events outside a cone with open angle of 4 central hours of the transit. The detection efficiency is not uniform and depends on the − From the GRBs identified by [ Sidereal day sky maps divided into 9 bins as a function of the multiplicity of the shower Unfortunately, there was no TeV emission found for any of the bursts studied here. In particu- The details on the adopted analysis in this work, such as event reconstruction, systematic The HAWC observatory is located next to the volcano Sierra Negra in the state of Puebla in Although HAWC continuously records extensive air showers in all directions over the horizon, ◦ [ ∼ ∈ intervals beginning at theconsecutive GW time trigger. intervals in For logarithmic thetook scale time case covering intervals of of a 1, GRB total 10 1701817APoisson of and distribution 100 120 we thus, days. days. have the The significance considered background For distribution fluctuationsUpper 10 other is are limits well well bursts approximated described of we by by the a a flux normal function are [ derived assuming a spectral index of theoretical prediction of SSC emission fromconstraining the as observed X-ray observed emission. in Figure The upper limits are not were within the HAWC’s field oftotal view exposure for time at for least each one of hour. these In bursts Table reported. redshift, we assume two characteristic values of z source declination. On the othersource hand, and the the energy spectral sensitivity index is of a the function source of as the the declination Figure of 10events the from are [ constructed as described in [ lar, the flux upper limits derived for GRB 170817A are presented in Figure the TeV on the GRBs location usingthe a Feldman-Cousins extragalactic confidence background interval light approach (EBL) and attenuation considering [ z=0.3 (an average value for sGRBs). 4. Results and Conclusions δ uncertainties, background subtraction and map making, are described in [ Mexico at an altitude of(WCDs) 4,100m as a.s.l. the main HAWC array ishighest and constituted energies. 345 by smaller HAWC 300 has detectors Waterangular an to Cherenkov resolution instantaneous improve Detectors its field sensitivity of to view showers of of 2 the sr, a duty cycle > 95% and an its effective area is a function of< the 45 zenith angle of the primary gamma-ray. It is optimal for values Follow up to GRB 170817A main pulse was followed by afor soft TeV tail emission emission, at etc). long Those time bursts scales are as clearly in interesting GRB to 170817A. search 3. Analysis relevant to our analysis are presented. shown by [ PoS(ICRC2019)681 Antonio Galván ]. Redshift (2017) . Multi-messenger 21506 1710.05833 (hr) [ Exposure Time GRB Coordinates Network, Circular , (2017) L12 848 (hr) ApJ 3 , Transit duration (2017) . (deg) Error 21505 Dec (deg) General characteristics of the short GRBs used in this study. LIGO/Virgo G298048: Fermi GBM trigger 524666471/170817529: LIGO/Virgo LIGO/Virgo G298048: Fermi GBM trigger 170817.529 and LIGO single IFO RA (deg) Table 1: GRB Coordinates Network, Circular Service, No. 21506, (2017) , Identification of a possible gravitational-wave counterpart Service, No. 21505, (2017) trigger Observations of a Binary Neutron Star Merger We acknowledge the support from: the US National Science Foundation (NSF) the US De- As observed, even though GRB 150101B has the highest redshift observed, the derived flux HAWC continuously monitors the whole sky in order to search for VHE emission from sGRBs GRB NAME GRB 150101BGRB 188.0 170111B -11.0 270.9 63.7 0 6.7 4.51 0.99 464.58 96.467 0.134 - GRB 170817A 197.5 -23.4 0 2.01 205.27 0.009 [1] R. Clasey Essick, [2] V. Connaughton, [3] B. P. Abbott, R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, C. Adams et al., 5. Acknowledgements partment of Energy Office of High-Energyopment (LDRD) Physics; program the of Laboratory Los Directed Alamos National Researchnología Laboratory; and (CONACyT), Consejo México Devel- Nacional (grants de 271051, Ciencia 232656, y 260378,258865, Tec- 179588, 239762, 243290, 254964, 271737, 132197, 281653)(Cátedrasrayos gamma; 873, L’OREAL Fellowship 1563, for 341), Women inUNAM Laboratorio (grants Science AG100317, 2014; Nacional IN111315, Red IN111716-3, HAWC HAWC, IA102715, México; de IN111419,VIEP-BUAP; DGAPA- IA102019, PIFI IN112218); 2012, 2013, PROFOCIE 2014,search 2015; Foundation; the the University Institute of of WisconsinNational Geophysics, Alumni Laboratory; Polish Re- Planetary Science Physics, Centre grant and DEC-2014/13/B/ST9/945, Signatures DEC-2017/27/B/ST9/02272; Coordinación at de Los la Alamos Investigación Científica deton Advanced la Fellowship Universidad 180385. Michoacana; Thanks Royal to Societytechnical Scott support. - Delay, New- Luciano Díaz and Eduardo Murrieta for References upper limit is comparable withThe the best one obtained flux for upper GRB limitlow 170111A exposure. is assuming obtained a The for redshift flux GRB ofconsequence upper 0.009. of 170817A limit the because for very of GRB low 170111A their exposurefunction when time. closeness of time assuming and The is a decreasing medium a redshift behavior clear of of consequence the of 0.3 flux the is upper increasing also time limits a in window. as timescales a from seconds to days.of In this view work, of we HAWC present and the associated most or interesting possible sGRBs associated in to the field gravitational waves. Follow up to GRB 170817A PoS(ICRC2019)681 Antonio Galván GRB , ]. The X-ray counterpart to the (2017) . 21520 1710.05433 GRB Coordinates Network, Circular [ , (2017) 71 4 GRB 170817A: Fermi GBM detection. 551 Nature , (2017) . 22763 GW170817/GRB170817A: LBT optical detection. Upper limits derived by HAWC using 10 slide windows. The solid line is the SSC prediction at gravitational-wave event GW170817 Service, No. 22763, (2017) Coordinates Network, Circular Service, No. 21520, #1 (2017) [4] A. von Kienlin, C. Meegan and A. Goldstein, [6] E. Troja, L. Piro, H. van Eerten, R. T. Wollaeger, M. Im, O. D. Fox et al., [5] A. Rossi, 40 TeV. Figure 1: Follow up to GRB 170817A PoS(ICRC2019)681 ]. ApJ , The Short Antonio Galván A radio Late time The 1711.11573 A mildly relativistic . ]. ]. (2017) [ (2019) 200 (2019) arXiv:1906.00502 871 1710.05435 [ ApJ 1710.05431 ArXiv e-prints ]. , [ , arXiv e-prints , (2017) 1579 Light Curves of a Shock-breakout Material and a 5 (2017) L20 358 1712.03237 848 Science ApJ , , (2017) [ ArXiv e-prints , ]. . 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