High Energy Emission. Brenda Dingus, LANL HAWC

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1 High Energy Emission from GRBs Brenda Dingus, LANL HAWC

2 What are GRBs? Cosmological distance Typical observed z>1 Energy released is up to few times the rest mass of Sun (if isotropic) in a few seconds => narrow beam Most of the energy is emitted in rays Relativistically expanding fireball Shocks between shells of different velocity Shocks created when fireball decelerates into external medium Central Engine Collapse of massive, rotating star? (long GRBs) Coalescence of binary neutron stars? (short GRBs) Final Product is Black Hole (probably) 2

3 High Energy Emission from GRB (Past) EGRET observations of delayed HE gamma ray emissions It is not straightforward to explain by conventional electron synchrotron models Proton acceleration? Origin of UHECR? Gonzalez et al. Nature 2003 BATSE s EGRET/TASC 14 47s Hurley et al. Nature s Two γ 18 GeV ~T0+75 min s s 3 /22

4 Fermi LAT Detected Bursts Granot, astroph

5 Highest Energy Requires Large Bulk Lorentz Factor Gamma Rays attenuated at the source by + > e + e + peak cross section when E 1 E 2 ~ 4 m e 2 c 4 / (1 cos ) Density of photons is high as inferred from source distance & rapid variability No attenuation if emission is from fireball with large bulk Lorentz factor Decrease Energy of Gamma Rays Reduce Number of Photons Increase the source size Bulk Lorentz factor,, required to give opacity of 1 for the highest E -ray observed For reference, AGN jets have Lithwick & Sari Mar 10 dingus@lanl.gov 5

6 GRB Bulk Lorentz Factors > ~1000

7 Extragalactic ray Absorption High energy gamma rays pair produce with the infrared to UV extragalactic background light (EBL) EBL not well constrained by direct measurements due to zodiacal light, but is constrained by galaxy and star formation history Low ray absorption possibly explained by axions? e - ~TeV e + ~ev

8 EBL evolves with redshift Kneiske, et al A&A

9 Optical Depth evolves with redshift

10 Highest Energy Gamma Rays vs EBL models , 13 GeV , 33 GeV , 31 GeV

11 Fundamental Physics with rays Test of Lorentz Invariance which is predicted by some quantum gravity theories v = c(1 ± E /E QG + O[(E /E QG ) 2 ]) E QG ~ Planck mass ~ GeV Compare light curve at different energies Need several sources at different redshift to disentangle effects of ray production in the source However, a single observation can give a limit on E QG If E QG = M Planck, then a light seconds, and E = 100 GeV=10-17 M Planc should arrive 1 s late.

12 GRB This short GRB rules out theories of violation of Lorentz invariance which are linear in E /E QG where E QG < m planck

13 Going to Higher Energies from the Ground Atmospheric Cherenkov Telescopes (VERITAS, HESS, MAGIC) Low duty cycle of 5 10% due to moonless, cloud free night time observations Require notification to look in direction of GRB Prompt Localizations by Fermi GBM have larger uncertainty than the field of view of the ACT Slew times of tens of seconds are too long for short GRBs + Excellent sensitivity to lower energies Extensive Air Shower Observatories (Milagro, ARGO, HAWC) Worse sensitivity at lower energies + 24 hours/day, 7 days/week operation with > 95% duty factor + Large field of view of 2sr (~1/6 the sky) + Online analysis to send alerts if transient source is detected

14 HAWC High Altitude Water Cherenkov

15 HAWC Sensitivity is 15x Better than Milagro s (a) Larger Effective Area at Lowest Energies (b) Improved Background Rejection (c) Better Angular Resolution => x improvement in flux sensitivity => (10 15) 2 = x faster to observe same flux

16 HAWC s Low Energy Response Monte Carlo Simulation which has been confirmed with Milagro observations. Gamma ray air showers with angular reconstruction better than 1.5 degrees.

17 Extensive Air Shower Development 4100m 2600m Higher Altitude means fewer radiation lengths and more particles Fluctuations in first interaction means more particles For example 5% of events (e -3 =5%) will have 5 x more particles

18 HAWC & Fermi > 10 GeV Sensitivity Source Spectrum is dn/de = E 2 and is cutoff by absorption with the EBL model of Gilmore, 2009

19 HAWC s Field of View = 2.6 sr = 1.8 sr

20 HAWC GRB Capability GRB Z=0.9 Highest Observed Energy 33 GeV HAWC will detect with 5 sigma significance if spectrum extends to 50 GeV If spectrum extends to 125 GeV (and is attenuated by EBL model of Gilmore), then HAWC would detect 200 gammarays

21 Measuring the Max Energy with HAWC + Fermi

22 Future Prospects are Exciting More GRBs from Fermi to come (~1/month) Possible Afterglow or Long GRB detection by ACTs Likely Detection of Prompt Emission by HAWC HAWC is ready to go 1 st Tank Site is Ready

23 Active Galactic Nuclei Flares Correlations with x-rays, optical, radio to determine emission mechanisms Discovery potential for orphan TeV flares producing neutrinos and UHECR Milagro s 9 Mrk421 Milagro flux Quadratic or Linear? Synchrotron Self 1 month Compton or External Compton? Crab Flux X-ray flux

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