Galactic Sources with Milagro and HAWC. Jordan Goodman for the HAWC and Milagro Collaborations

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1 Galactic Sources with Milagro and HAWC Jordan Goodman for the HAWC and Milagro Collaborations Snowpack 2010

2 Milagro and HAWC Milagro was a first generation wide-field gamma-ray telescope: Proposed in 1990 Operations began in 2001/04 Developed /h separation Discovered: more than a dozen TeV sources diffuse TeV emission from the Galactic plane a surprising directional excess of cosmic rays Showed that most bright galactic GeV sources extend to the TeV Best instrument for hard spectrum and extended sources HAWC is the next logical step It will be 15x more sensitive than Milagro It can be running in 3 yrs (with Fermi) Intro HAWC Collaboration April 2010

3 How do you make Milagro better?

4 From Milagro to HAWC Move it to higher altitude Improve optical isolation Cover more area with water Milagro 2350m asl One big pond Pond area 4,000 m 2 HAWC 4150m asl Individual tanks Tank area ~20,000 m 2

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6 HAWC m x4.3m Steel Tanks with 3 PMTs at 4100m asl in Mexico HAWC Collaboration

7 Pico de Orizaba and Sierra Negra HAWC Collaboration

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9 Full size prototype

10 Light-tight tight Bladder

11 Much Better Low Energy Response HAWC HAWC Performance Much Better Background Rejection Milagro Milagro w / -h cut Milagro HAWC Milagro Milagro Much Better Angular Resolution HAWC Better Energy Resolution HAWC HAWC Collaboration April 2010

12 HAWC Science Gamma Astronomy with wide FoV and high duty cycle: Understand particle acceleration in AGN and GRB jets through the discovery of short and long GRBs at > 100 GeV energies and MWL Target of Opportunity programs on flares; Understand the sources of Galactic CRs through the observation of galactic sources including extended ones (SNRs in molecular clouds, superbubbles) Studies on EBL and diffuse gamma emissions. Hadronic Astronomy: find evidence of proton acceleration in Galactic CR sources (eg understanding Milagro regions with larger statistics) Exotic phenomena photon oscillations in axion-like particles through EBL studies; Lorentz invariance; Slow Monopoles and Q-balls.

13 Milagro Results 15 TeV associations out of 35 likely galactic sources in our field of view Abdo et al. ApJL (accepted) arxiv:

14 Milagro/Fermi/HAWC Comparison Taking into account the Fermi exposure and signal vs Milagro we find that for galactic sources Fermi is ~15x more sensitive than Milagro. HAWC will be ~15 times more sensitive than Milagro HAWC will have approximately the same sensitivity as Fermi for hard spectrum galactic sources at ~10 4 times the energy. HAWC Collaboration April 2010

15 GeV Pulsars Produce TeV PWN GeV Emission is pulsed & due to rotation axis misaligned with Magnetic Dipole of ~10 12 G TeV Emission is produced by particles further accelerated in the shock interacting with the ambient medium. IMPLICATIONS TeV PWN are prevalent with GeV pulsars GeV emission has broad beam

16 Geminga (J ) 10 parsecs 68% PSF Milagro Brightest GeV source of 34 searched is Geminga Old (300 kyr) PWN and nearby (250 pc) ~10 parsec extent is similar to HESS observations of more distant PWN HAWC Milagro sees Geminga at 30% of the Crab at ~20 TeV while IACTs have a limit of ~1% of the Crab at >200 GeV

17 Geminga with HAWC 10 parsecs 68% PSF Milagro Brightest GeV source of 34 searched is Geminga Old (300 kyr) PWN and nearby (250 pc) ~10 parsec extent is similar to HESS observations of more distant PWN HAWC

18 Milagro Results Milagro Spectrum of the Crab Milagro 68% HAWC Energy reach from ~3TeV to >100 TeV Peak sensitivity for E -2 source at ~100 TeV HESS Crab data/fit

19 HESS/HEGRA/Milagro Crab Spectra HESS HEGRA

20 If you use the fit to 2.75 we find a ~80 25 TeV cutoff If you constrain the fit to 2.65 at lower energies we find a ~65 TeV cutoff Crab Cut-off

21 Milagro Spectrum of the Crab w/hawc Milagro 68% HAWC Energy reach from ~3TeV to >100 TeV Peak sensitivity for E -2 source at ~100 TeV HEGRA Crab data/fit

22 Milagro Results MGRO J / 0FGL J Milagro 68% HAWC In Milagro J is 700 mcrab The flux in s >200 GeV is 95mCrab HESS Crab fit: (Io =3.76x10-7, =2.39, Ec=14.1 TeV) This source is almost as bright as the Crab at Milagro s energy

23 HAWC View Milagro 68% HAWC In Milagro J is 700 mcrab The flux in /s >200 GeV is 95mCrab HESS Crab fit: (Io =3.76x10-7, =2.39, Ec=14.1 TeV)

24 Milagro Results MGRO J Milagro 68% HAWC Ecut (1 56 (2 A Milagro discovered source now seen by HESS and VERITAS Using HESS spectrum of -2.1 as input, Milagro requires a cut-off at <40(56) TeV (N.B. Milagro measures a larger flux, possibly because we are integrating over a larger area than HESS)

25 Energy Discrimination Normal Weighting Low Energy Weighting

26 Boomerang Milagro Veritas

27 Milagro/Veritas Comparison

28 HAWC Simulation Milagro 3 3 source detected at 20 HAWC (3months) HESS

29 HAWC Simulation Milagro 3 3 source detected at 20 HAWC (3months) HESS

30 HAWC Simulation Milagro 3 3 source detected at 20 HAWC (3months)

31 Milagro Results Cosmic Ray Observations Significance ( s) Geminga Heliotail Milagro data show an unexpected anisotropy (PRL 101, , 2008) No weighting or cutting. Map dominated by charged cosmic rays. 10 o smoothing, looking for intermediate sized features. Two regions of excess 15.0 and Fractional excess of 6x10-4 (4x10-4 ) for region A(B).

32 Milagro Results 21

33 Milagro Results Cosmic Ray Anisotropy Data are not consistent with: Mostly gamma-rays > data looks hadronic with cosmic ray spectrum > flatter, with ~10 TeV cutoff HAWC with better energy resolution and gammahadron rejection can: Measure the spectrum with much higher precision Measure the gamma-ray fraction Understanding this is important for Dark Matter Searches HAWC Collaboration April 2010

34 Conclusions Milagro was a first generation wide field detector It showed that many bright galactic GeV sources extend to TeV energies Many sources are extended in TeV It found a surprising anisotropy in TeV Cosmic Rays HAWC will Have 15x the sensitivity of Milagro It will measure spectra out to 100 TeV Snowpack 2010

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