HAWC Status & Galactic Science
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1 HAWC Status & Galactic Science HAWC photo from March Currently 243 of 300 tanks are built, " 192 are filled with water, and 143 are taking data nearly continuously.! Brenda Dingus, LANL US Spokesperson 5/7/2014 1!
2 Gamma-Ray Detectors HAWC is a wide field of view (~2sr), continuously operating (>90% duty cycle), TeV observatory.! Unbiased search for transients to initiate multi messenger observations! Highest energy observations with ~100 km 2 hr exposure after 5 years operation! Wide Field of View, Continuous Operations! TeV Sensitivity! Fermi AGILE EGRET! HAWC ARGO Milagro VERITAS HESS MAGIC 2!
3 HAWC Design 300 close packed water tanks (7.3m dia x 4.5 m deep of 200,000 liters) each with 4 upward facing photomultiplier tubes at the bottom! 180 meters 3!
4 HAWC Site Location in Mexico High Altitude Site of 4100 m with temperate climate and existing infrastructure 17 R.L. of atmospheric overburden vs 27 R.L. at sea level Latitude of 19 deg N HAWC Large Millimeter Telescope (50m dia. dish) Pico de Orizaba 5600 m (18,500 ) 4!
5 The HAWC Collaboration Los Alamos National Laboratory Univ. of Maryland Michigan State Univ. University of Wisconsin Pennsylvania State Univ. Univ, of Utah Univ. California Irvine George Mason University University of New Hampshire University of New Mexico Michigan Technological University NASA/Goddard Space Flight Center Georgia Institute of Technology University of Alabama Colorado State Univ. Univ. California Santa Cruz Instituto Nacional de Astrofísica Óptica y Electrónica Universidad Nacional Autónoma de México Instituto de Física Instituto de Astronomía Instituto de Geofisica Instituto de Ciencias Nucleares Benemérita Universidad Autónoma de Peubla Universidad Autónoma de Chiapas Universidad Autónoma del Estado de Hidalgo Universidad de Guadalajara Universidad Michoacana de San Nicolás de Hidalgo Centro de Investigacion y de Estudios Avanzados Universidad de Guanajuato ~100 Members Mexico USA 5!
6 Timeline 13M USD project funding began Feb 2011 Operations with 111 water Cherenkov detectors began Aug 2013 Currently, 243 water Cherenkov detectors have been built. Construction will be complete by end of 2014 Nov 2010! Feb 2012! Aug 2012! May 2013! Jan 2014! 6!
7 HAWC-30 Completed Sept 2012 HAWC 30 Events and! Observation of cosmic-ray shadow of Moon with 70 days of data! 7!
8 HAWC 100 Preliminary Sky Mrk 421# Crab >10 σ# Galactic Plane# Galactic Plane! Began operations Aug 2013 with ~1/3 of the array while still constructing! 8!
9 HAWC Sensitivity Differential Sensitivity per Quarter Decade of Energy! Astroparticle Physics 2013 Details coming in John Pretz s talk 9!
10 HAWC Simulated Performance vs Milagro Increased efficiency at lower energies 10!
11 Extensive Air Shower Development 4100m 2600m Higher Altitude means fewer radiation lengths and more particles (~5x) for same primary energy
12 HAWC Sensitivity Angular Resolution Hadron Rejection 12!
13 Gammas 8 TeV at ϴ= Hit PMTs 21 TeV at ϴ= Hit PMTs 24 TeV at ϴ= Hit PMTs Protons 118 TeV at ϴ= Hit PMTs 7 Brian Baughman - HAWC Collaboration - ICRC 2013 Rio Energy deposited away from core 13!
14 HAWC s Field Of View Known sources are shown, but most of the high latitude sky has not been observed at TeV energies Sources from TeVCAT.uchicago.edu 14!
15 Milagro Significance for Fermi GeV Bright Sources Abdo et al., ApJ Lett 2009! Bright GeV pulsars are coincident with TeV emission.!! HAWC will observe Galactic GeV sources with approximately the same significance as Fermi.! 15!
16 Highest Energy Sources For example, MGRO J SED peaks >10 TeV.! HAWC will likely discover new higher energy peaked sources.!! Aliu, et al. 2014, Spatially resolving MGR with VERITAS! Need HAWC-VERITAS joint spectral fits.!! 16!
17 Cygnus: A Complicated Region MGRO J :! - Collocated extended emission detected by IACTs, Milagro, and ARGO! - Spectrum appears to line up with the Fermi cocoon cosmic ray acceleration model can explain the diffuse emission in the cocoon! Milagro contours on Fermi counts map M. Hui! 17!
18 Geminga: a Nearby Positron Source Milagro s(detec>on(of(an(extended( excess(coincident(with(geminga( PAMELA s(positron(excess(is(well(fit( given(milagro s(flux(from(geminga( ~ 10 parsec! The confirmed presence of a nearby, ancient source of high-energy electrons and positrons immediately suggests an explanation for the positron excess. -Yüksel, Kistler, Stanev Phys Rev Lett 2009 HAWC will detect Geminga with >50σ to map diffusion near source. 18!
19 TeV Galactic Diffuse Emission! Milagro flux exceeds GALPROP predictions!! BUT are there unresolved sources???! HAWC will resolve more sources and can detect the GALPROP flux! Abdo, 2008 ApJ! From Petra Huentemeyer s APS 2014 Talk, " Hot News from the HAWC Gamma-Ray Observatory! 19!
20 HAWC Diffuse Sky Prediction after 3 Years GALPROP assumption! 4 deg smoothing! From Petra Huentemeyer s APS 2014 Talk, " Hot News from the HAWC Gamma-Ray Observatory!
21 Active Galactic Nuclei Flares HAWC will monitor AGN within 2/3 of the sky with 20% duty cycle/day (5 hrs) regardless of sun, moon, or weather VERITAS follow up observations to HAWC s prompt notifications will result in shorter time variability in new and known TeV sources. Worldwide Dataset of TeV Observations by IACTs of Mrk421 HAWC 5 minutes! 1 month HAWC 5 hours! Tluczykont et al. 2010! 21!
22 Fermi observation of GRB090510, z=0.9 Highest Observed Energy was 33 GeV with 16 γ-rays >1 GeV Constrained Lorentz Invariance at the Plank Mass scale HAWC would detect this GRB if it occurred in FOV HAWC will promptly search satellite notifications and will promptly notify community of detections. Fermi spectra allows HAWC to constrain max energy. VERITAS follow up could likely detect TeV afterglow. Gamma-Ray Bursts 22!
23 Dark Matter HAWC has sensitivity to indirect detection of multi-tev WIMPs in satellite galaxies, the Galactic Center, and galaxy clusters Cosmological simulations predict more satellite galaxies than observed Recently higher M/L galaxies have been found by Sloan Deep Survey HAWC will observe all M/L galaxies in half the sky, even if L=0 Solid lines are 5 sigma sensitivity.! Dashed lines show sensitivity with the expected Sommerfeld enhancement due to additional resonances.! Horizontal line is the cross section for thermal production of WIMPs.! Preliminary! HAWC-VERITAS-Fermi complement each other by ruling out different mass scales and channels. VERITAS deep observations of HAWC unidentified high lat sources would reveal spectral and spatial signatures. 23!
24 The Unexpected Milagro Discovered an Anisotropy of 10 TeV Cosmic Rays (PRL, 2009) Confirmed in Northern Hemisphere by ARGO and now HAWC, and in Southern Hemisphere by Ice Cube Gyroradius of 10TeV proton in 2µG field is parsecs=1000 AU No known sources within this distance Annihilation in protons of nearby Dark Matter? (Harding, astroph/ ) Strangelets (stable quark matter)? (Kotera, Perez-Garcia, Silk astroph/ v1) Any ideas on how VERITAS can help? 24!
25 Summary: HAWC & VERITAS Coordinated observations are important Joint analysis is needed Spectral, Spatial, Temporal, Scientific HAWC observations are just beginning with a plan of operating for 5 years with the full detector HAWC detects Crab>10σ# 25!
26 BACKUP 26!
27 Fermi Bubbles? 27!
28 Much Better Low Energy Response HAWC Performance Much Better Background Rejection HAWC Milagro (a) HAWC (b) Milagro Milagro HAWC Milagro (d) Much Better Angular Resolution Better Energy Resolution (c) HAWC
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