The Highest Energy Emission from Short GammaRay Bursts
The Highest Energy Emission from Short Gamma-Ray Bursts Pablo Saz Parkinson Santa Cruz Institute for Particle Physics, UCSC SCIPP Seminar, 9 March 2007
Outline Introduction: What is a short GRB? Motivation: Why search for HE emission? Milagro Search for VHE emission Future prospects Pablo Saz Parkinson. 9 March 2007 2
Gamma-Ray Bursts (GRBs) Large explosions of gamma rays discovered in late 60’s. First afterglow (and redshift) late 90’s. First short burst afterglow detected May 2005. Two types of GRBs: short (< 2 s) and long (> 2 s). Long bursts related to death of massive stars. Short bursts related to binary mergers. ‘Swift’ surprises: Bright X-ray flares, steep decays, shallow decays, … Pablo Saz Parkinson. 9 March 2007 3
Norris et al. (1984) Pablo Saz Parkinson. 9 March 2007 4
Kouveliotou et al. (1993) Distributions “overlap”. Duration alone cannot distinguish the two populations. In addition, bursts may have Extended emission (e. g. Lazzati et al. 2001, Norris et al. 2006) The first 2 s of a long burst is spectrally similar to short bursts (Ghirlanda et al 2004). Some bursts may look long but be “short”, and vice versa. There may be more than two populations … Pablo Saz Parkinson. 9 March 2007 5
A word about SGRs Boggs et al. 2006 The flare from SGR 1806 -20 was the brightest explosion ever detected Maybe some short GRBs are SGRs Estimates vary a great deal but can at most account for 20% This SGR outburst was at high zenith angle for Milagro (almost 70 degrees) Pablo Saz Parkinson. 9 March 2007 6
Another distinguishing feature (Norris et al. 2006) Pablo Saz Parkinson. 9 March 2007 7
Donaghy et al. (2006) Conclusion: The duration at which a burst is equally likely to be in the SPB class and the LPB class is found to be 5 seconds. Pablo Saz Parkinson. 9 March 2007 8
Characteristics of Short GRBs Shorter duration Harder spectrum Narrower pulses Good for testing QG No spectral lag (Amelino-Camelia 2005 Scargle et al. 2006) Less luminous Lower redshift Less absorption by EBL No associated supernova Location in galaxies with low SFR Pablo Saz Parkinson. 9 March 2007 9
So what causes short GRBs? Favorite model: Binary merger - Energetics is the right order of magnitude - Most have been found in low SFR regions - Time scales are consistent - No apparent SN association No conclusive evidence (waiting for LIGO) Pablo Saz Parkinson. 9 March 2007 10
Search for VHE emission from GRBs Experimental Motivation – EGRET (e. g. GRB 940217) – GRB 941017 (High Energy component) – Milagrito Burst (GRB 970417 a) Theoretical – Many models predict VHE emission (e. g. SSC) Why Milagro? – Large (1/6 sky) field of view and > 90% duty cycle – No need to point: search for prompt emission – Best current instrument for this type of search Pablo Saz Parkinson. 9 March 2007 11
EGRET GRB Spectrum Dingus (2003) d. N/d. E ~ E-1. 95 Pablo Saz Parkinson. 9 March 2007 12
High Energy emission from GRB 941017 GRB 940217 -18 -14 s 18 Ge. V! 14 -47 s 47 -80 s 80 -113 s 113 -211 s Hurley et al. , Nature 372, 652 (1994) Gonzalez et al. , Nature 424, 749 (2003) Pablo Saz Parkinson. 9 March 2007 13
Short GRB 930131? Note: EGRET deadtime ~ 100 ms T 90=14 s, fluence = 1. 2 x 10 -5 erg cm-2 Pablo Saz Parkinson. 9 March 2007 Credit: J. Norris 14
Theory of the high E component Shape of high energy component applies constraints to ambient densities and magnetic fields. Milagro has the sensitivity to observe the predicted emission or rule out the model. More GRBs with low redshift are needed. Pe’er & Waxman (Ap. JL 603, 1, L 1 -L 4, 2004) constrain source parameters for Inverse Compton emission of GRB 941017 Pablo Saz Parkinson. 9 March 2007 z=0. 5 z=0. 2 z=0. 02 15
Dermer et al. 1999 Te. V emission mirrors Me. V Measurement of time dependence Of the high energy emission can test the SSC model and the external shock scenario. Pablo Saz Parkinson. 9 March 2007 16
Razzaque and Meszaros model (Razzaque & Meszaros 2006) Pablo Saz Parkinson. 9 March 2007 17
Detecting Gamma Rays High Sensitivity HESS, MAGIC, CANGAROO, VERITAS Low Energy Threshold EGRET/GLAST Large Aperture/High Duty Cycle Milagro, Tibet, ARGO, HAWC? Large Effective Area Excellent Background Rejection (>99%) Space-based (small area) “Background Free” Moderate Area/Large Area (HAWC) Good Background Rejection Low Duty Cycle/Small Aperture Large Duty Cycle/Large Aperture High Resolution Energy Spectra Studies of known sources Unbiased Sky Survey (<300 Ge. V) AGN Physics Unbiased Sky Survey Extended sources Surveys of limited regions of sky Point source sensitivity Transients (GRBs) (<100 Ge. V) Transients (GRB’s) Solar physics/space weather Pablo Saz Parkinson. 9 March 2007 18
MAGIC response to GRBs Albert et al. (2006) Pablo Saz Parkinson. 9 March 2007 19
The Milagro Te. V observatory • • • 2630 m above sea level in the Jemez Mountains, Los Alamos, New Mexico Operational since 2000 (with 8” PMTs with “baffles” outriggers since 2003) 2. 8 x 2. 8 m spacing Duty cycle greater than 90% ~ 2 sr field of view Top Layer: 450 PMTs, 1. 5 m deep Trigger rate 1. 5 -2 k. Hz Bottom Layer: 273 PMTs, 6. 5 m deep Angular resolution of 0. 45 degrees Outriggers: 175 black plastic tanks each Energy: ~ 100 Ge. V – 100 Te. V with a PMT, spread over 20, 000 m 2 (median ~ 2. 5 Te. V) Pablo Saz Parkinson. 9 March 2007 20
Event Reconstruction Real air shower event Monte Carlo gamma-ray shower Pablo Saz Parkinson. 9 March 2007 21
Milagro Effective Area Pablo Saz Parkinson. 9 March 2007 22
Why is GRB VHE emission elusive? Atmospheric Cerenkov Telescopes cannot search for prompt emission Primack et al. 05 Extragalactic Background Light (EBL) absorption High Energy+ EBL –> e+ e. I=I 0 e-t t=1 => ~ 0. 37 t=10 => ~ 4. 5 x 10 -5 Pablo Saz Parkinson. 9 March 2007 23
Why VHE emission is elusive (Cont’d) Most bursts are at high z ~ 20% of bursts with measured z have z < 0. 5 Milagro expects ~ 1/year in its FOV with z < 0. 5 Pablo Saz Parkinson. 9 March 2007 24
“triggered” vs “untriggered” Untriggered Search: – Real-time, all locations, instant notification – Many time scales (0. 25 msec to > 2 hr) – Drawback: LARGE number of trials Triggered Search: – Satellites provide time, location, and duration of burst -> more sensitive – Even limits on bursts with redshifts are important – Swift is greatly increasing our sample – Drawback: small number of bursts Pablo Saz Parkinson. 9 March 2007 25
The untriggered search: outputs Probability histograms No significant emission detected 0. 0251 s 0. 0398 s 0. 158 s -20 -10 log(P) Milagro can set model-dependent upper limits on VHE emission from GRBs. D. Noyes, Ph. D Thesis, 2005 Pablo Saz Parkinson. 9 March 2007 26
The triggered search More sensitive than untriggered search (know location and duration) Ideal GRB: bright, nearby, at a good zenith angle. Have not had such a burst. Swift could change this. Milagrito evidence for Te. V emission This was 1 of 54 bursts searched. The Milagro sample of bursts has only recently surpassed this number. GRB 970417 a had a post-trial probability of 1. 7 x 10 -3 (including the 54 bursts searched) Pablo Saz Parkinson. 9 March 2007 27
Short GRBs in Milagro’s FOV We define “short” to be 5 s 2000 -2007: 17 GRBs (15 well localized) 6 Swift GRBs 6 Inter-Planetary Network (IPN) 4 BATSE 1 HETE 3 firm redshifts (0. 55, 0. 86, 3. 91) 3 questionable redshifts (0. 001, 0. 225, 0. 41) Pablo Saz Parkinson. 9 March 2007 28
Search for a Te. V signal Light curve (T=0 trigger time) Number of events in 1. 6 degree bin Look at number of events in a given bin during the relevant time (e. g. T 90) Compute estimated Background in that bin using 2 hours of data around the burst Calculate significance Number of events expected from background Significance (GRB location at center) Pablo Saz Parkinson. 9 March 2007 29
Significances Pablo Saz Parkinson. 9 March 2007 30
Milagro Limits for Some Bursts GRB 050509 b: A short/hard burst (z=0. 225? ) – Eiso(ke. V) = 2 x 10 -8 ergs/cm 2 – Eiso(Te. V)/Eiso(ke. V) < 10 – 20 (GCN Circular 3411) – Razzaque et al. model would give ~0. 02 s-1 GRB 051103: A short/hard (0. 17 s) burst detected by the IPN – Eiso(ke. V) = 2. 34 x 10 -5 ergs/cm 2 – Eiso(Te. V)/Eiso(ke. V) < 1 (if z~0 -> M 81 < 4 Mpc) (GCN Circular 4249) GRB 060427 b: Another short (0. 2 s) IPN burst, z=? , 16 o zenith – Eiso(Te. V)/Eiso(ke. V) < 4 (for z=0. 5) (GCN Circular 5061) – Eiso(Te. V)/Eiso(ke. V) ~ 0. 1 for z=0 Pablo Saz Parkinson. 9 March 2007 31
Results Submitted to Ap. J Pablo Saz Parkinson. 9 March 2007 32
Future prospects: HAWC A low-cost successor to Milagro, reusing the PMTs and much of the instrumentation, optimized layout, at high altitude (~4500 m), with a potential increase in sensitivity of > 15. 841 PMTs (29 x 29) in one layer 5. 0 m spacing Single layer with 4 m depth Instrumented Area: 22, 500 m 2 1 year survey point source sensitivity of ~60 m. Crab Pablo Saz Parkinson. 9 March 2007 33
Future prospects: HAWC Milagro HAWC Pablo Saz Parkinson. 9 March 2007 34
Summary and Conclusions - Our knowledge of short GRBs is still in its infancy. - Short GRBs are good candidates for VHE emission. - Detection of VHE emission should constrain the numerous models and can also be used to probe deeper physics questions (e. g. QG) - No VHE emission from GRBs has been detected to date, but it cannot be definitely ruled out. Swift will continue to provide a number of potential candidates and blind searches will help to constrain such emission. - A future detector, HAWC, larger and at higher altitude (~4500 m) would significantly improve the prospects for detecting VHE emission from short GRBs. - GLAST, in conjunction with the ground-based Te. V detectors will put severe constraints on emission models. 35 Pablo Saz Parkinson. 9 March 2007
Thank You Pablo Saz Parkinson. 9 March 2007 36
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