A New Look at the TeV Sky with the HAWC Gamma Ray ... - APS
Transcript of A New Look at the TeV Sky with the HAWC Gamma Ray ... - APS
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A New Look at the TeV Sky with theHAWC Gamma Ray Observatory
APS Mid-Atlantic Senior Physicists GroupFeb 15, 2017Jordan GoodmanUniversity of Maryland
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J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Talk Overview
• TeV Radiation– Sources/ Techniques– IACTs/ Air Showers
• HAWC– Design– Construction– Performance
• The HAWC Catalog• Other HAWC results
– Transients - AGN, IceCube Event– Dark Matter Limits– Anisotropy
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
The HAWC Collaboration
Michigan State UniversityUniversity of RochesterUniversity of California Santa Cruz MexicoInstituto Nacional de Astrofísica,
Óptica y Electrónica (INAOE) Universidad Nacional Autónoma
de México (UNAM)Instituto de FísicaInstituto de AstronomíaInstituto de GeofísicaInstituto de Ciencias Nucleares
United StatesUniversity of MarylandLos Alamos National LaboratoryUniversity of WisconsinUniversity of UtahUniv. of California, IrvineUniversity of New HampshirePennsylvania State UniversityUniversity of New MexicoMichigan Technological UniversityNASA/Goddard Space Flight CenterGeorgia Institute of TechnologyColorado State University
Universidad Politécnica de PachucaBenemérita Universidad Autónoma de PueblaUniversidad Autónoma de ChiapasUniversidad Autónoma del Estado de HidalgoUniversidad de GuadalajaraUniversidad Michoacana de San Nicolás de HidalgoCentro de Investigación y de Estudios AvanzadosInstituto Politécnico NacionalCentro de Investigación en Computación - IPNEuropeMax-Planck Institute for Nuclear PhysicsIFJ-PAN, Krakow, Poland
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J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
GeV Gamma-Rays from Space
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Swift
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
TeV Gamma Ray Sources
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tevcat.uchicago.edu
179 known TeV gamma-ray sources (as of October 2016)
Galactic:
Supernova Remnants Binary systems
Extragalactic:
AGNsGRBs (GeV)
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Complementarity of Gamma-Ray Detectors
FermiAGILEEGRET
HAWCARGO
Milagro VERITAS
HESSMAGIC
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Wide-field/Continuous Operation TeV Sensitivity
• Space-based detectors - continuous full-sky coverage in GeV• Ground-based detectors have TeV sensitivity
• IACTs (pointed) excellent energy and angle resolution• HAWC has 24-hour >1/2 sky coverage
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Imaging Atmospheric Cherenkov Telescopes
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HESS - Nambia
CTA - Future
VERITAS Arizona
MAGIC - La Palma
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Imaging Atmospheric Cherenkov Telescopes
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VERITAS (KICP) Arizona
~5o field of view.
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J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
What can you do with a wide-field instrument?
• Gamma Ray Astrophysics– Galactic Gamma-Ray Sources - Survey
• Discovery of Pulsars, PWNs, Binaries -especially extended sources
• Study of high energy behavior - source of galactic cosmic rays
• Morphology of sources• Galactic Diffuse and Fermi Bubbles
– Transients• Gamma Ray Bursts - high energy behavior• AGN - Continuous monitoring• IceCube, LIGO multimessenger observations
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• Particle Physics– Dark Matter - can look for places with
no visible signal – Primordial Black Holes – Violations of Lorentz Invariance– Look for sources of positron excess
• Cosmic Ray Anisotropy
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J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
HAWC Science Goals
• Gamma Ray Astrophysics– Galactic Gamma-Ray Sources • Pulsars, PWNs, Binaries • Galactic Diffuse and Fermi Bubbles
– Extragalactic Gamma-Ray Sources• Gamma-ray bursts• Active Galactic Nuclei
– Inter Galactic Magnetic Fields (IGMF)• Particle Physics– Dark Matter– Primordial Black Holes– Violations of Lorentz Invariance– Q-Balls
• Cosmic Ray Anisotropy• Solar Physics 11
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
High Energy View of our Galaxy
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HAWC 1—100 TeV, 1 year
Fermi LAT 0.05 — 2 TeV, >6 years
HESS >1TeV, 10 years
Credits: NASA/DOE/Fermi LAT Collaboration
credit: NASA / CXC / SAO / F. D. Seward, W. H. Tucker, R. A. Fesen
Pulsar Wind NebulaeSupernova Remnants TeV Binaries
Mirabel, Science, 312, 1759
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J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Cosmic Ray Discovery
• Physikalische Zeitschrift: “The results of these observations seem best explained by a radiation of great penetrating power entering our atmosphere from above.”
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V. F. Hess. Über Beobachtungen der durchdringenden Strahlung bei sieben Freiballonfahrten. Physikalische Zeitschrift, 13:1084-1091, November 1912.
Victor Franz Hess
Elevation Rate
Ground 121km 102 km 12
3.5 km 155 km 27
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J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016 14
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J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
• The flux charged cosmic rays follows nearly a single power law over:
• 10 decades in energy • 30 decades in flux
• Single particles have been observed with energies above 1020eV!
• There are several “kinks” in the spectrum where the exponent changes, steepening at the “knee” and flattening at the “ankle”.
• The source of the high-energy cosmic rays remains elusive.
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Direct Measurements in Space
Air Showersfrom the Ground
Cosmic Rays
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J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
More than 100 Years Later
• We know a lot about Cosmic Rays– We have found sources of high energy photons (gamma rays)– We have a number of ideas of how particles can be accelerated to high energies
• But we still don’t know the origin of the high energy Cosmic Rays!– Gamma-rays (and neutrinos) can point to the sources!
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Binary Neutron Star Coalescing
Spinning Neutron Star powering a relativistic wind
Super Massive Black Hole
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J. Goodman — Physics Olympics 2016 Spring 2016J. Goodman — Physics Olympics 2016 Spring 2016
Why Not Cosmic Ray Astronomy?
• Charged Particles are bent in the magnetic fields of our galaxy and local cluster
• Energy of >1019eV needed to point back to even galactic sources• Very high energy photons interact with light when traveling long
distances
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Washington
We need another messenger!
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Particle Astrophysics – Univ. of Maryland Fall 2016Particle Astrophysics – Univ. of Maryland Fall 2016
Candidate accelerators
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Large radius
Large magnetic field
Kotera, K; Olinto AV. 2011 Annu. Rev. Astron. Astrophy. 49:119-53
Hillas Plot
2T
B⊕
R⊕ 1AU
p=0.3 Brp in Gev/cB in Teslar in meters
B=2T r=1.5x1011mp=1011 GeV/c
=1020 eV/c
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman – Univ. of Maryland
Active Galactic Nuclei (AGN)
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Particle Astrophysics – Univ. of Maryland Fall 2016Particle Astrophysics – Univ. of Maryland Fall 2016
Hubble AGN M87
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Particle Astrophysics – Univ. of Maryland Fall 2016Particle Astrophysics – Univ. of Maryland Fall 2016
GRBs
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GRBs are now seen to produce gamma rays up to nearly 100 GeV
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Extensive Air Shower Development
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Physics Olympics - J. Goodman 2016
Proton - 100 TeV
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Gamma Shower 2 TeV (movies by Miguel Morales)
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Blue – Electrons Muons – Yellow Pions – Green Nucleons – Purple
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Proton Shower 2 TeV (movies by Miguel Morales)
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Blue – Electrons Muons – Yellow Pions – Green Nucleons – Purple
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J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Milagro
• In the mountains above Los Alamos at 2650m • In an existing pond
– 60m x 80m x 8m– 175 outriggers– 20,000 m2
• Operated from 2000- 2008• 1st wide-field TeV Observatory
29J. Goodman -
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J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Milagro
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J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J. Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Milagro
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Background Rejection in Milagro
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Proton MC Proton MC
Data DataγMC γMC
Use bottom layer of Milagro to detect penetrating particles (primarily muons) which are more prevalent in cosmic-ray (hadronic) showers than gamma-ray (electromagnetic) showers
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Milagro TeV Sources
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
VERITAS Observation of 2019+37
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Energy >1 Tev
>600 GeV <1 Tev
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
IceCube
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IceCubeAstrophysicalNeutrino
CosmicRay
AirShower
AtmosphericNeutrino
CosmicRay
AtmosphericMuon
IcCube uses Atmospheric muons fromthe Southern Hemisphere
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Milagro & IceCube
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
SmallScaleAnisotropy
4821http://people.roma2.infn.it/~aldo/RICAP09_trasp_Web/Vernetto_ARGO_RICAP09ar.pdf
MilagroResults
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Cosmic Ray Anisotropy
R. Abbasi et al., ApJ 740:16 (2011), arXiv:1105.2326
Milagro 5 TeV
IceCube 20 TeV
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016 50
High Altitude Water Cherenkov
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
HAWC Design builds on Milagro
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Milagro “1st Generation” Water Cherenkov gamma-ray detector• 2650m (8600’) elevation near Los Alamos, NM• Covered pond of 4000 m2
• Operated 2000-2008• Detected new Galactic sources, Galactic plane,
cosmic ray anisotropy, and put upper limits on prompt emission from gamma-ray bursts
HAWC “2nd Generation” Water Cherenkov gamma-ray detector• 4100m (13500’) elevation near Puebla, Mexico• 300 water tanks spread over 20,000 m2
• Construction 2010-14, Operation 2015-2020(25)• ~15x Milagro’s sensitivity with ~10x lower
energy threshold
©Aurore Simonnet
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Gamma/Hadron Separation
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Gam
mas
Prot
ons
30 GeV 70 GeV 230 GeV
20 GeV 70 GeV 270 GeVSize of HAWC
Size of Milagro deep layer
Energy Distribution at ground level
Rejection factor ~ e-<μ>
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
The HAWC Site
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Latitude:18o59.7’NLongitude:97o18.6’W
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
HAWC
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HAWC
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
HAWC
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HAWC
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
HAWC Differential Sensitivity
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5 years of HAWC operations will give similar sensitivity at 10 TeV as 1 TeV for ACTs
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Fermi Observation of GRB 090510
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Fermi Observation of GRB 090510 with HAWC
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• Assume spectrum extends to 125 GeV and attenuation with EBL model of Gilmore
• HAWC: 200 events from GRB 090510 if near zenith~few background events
• Major Improvements!– Low-threshold DAQ– 10-inch PMTs
→ HAWC would observe 100s of events for spectrum to only 31 GeV
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Milagro/Fermi/HAWC Comparison
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•HAWC is ~15x more sensitive (sig/√bg) than Milagro•HAWC sees the Crab at ~6σ in a day - Milagro took 6 months to see 6σ
•Taking into account the Fermi exposure and signal vs Milagro we find that for galactic sources Fermi is ~15x more sensitive than Milagro. •HAWC at TeV has approximately the same sensitivity as Fermi has at GeV for galactic sources.
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
HAWC Tanks
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Tank Construction
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016–
Angle Reconstruction
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Photons convert to e+e- in the water
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
HAWC-250
HAWC-250: November, 2014 (~150Days)HAWC-111: Operations Begins: August 2013 (283 days)
HAWC Inauguration, HAWC-300: March, 2015
HAWC-11173
HAWC-30
HAWC-300
HAWC-30: Engineering Test of full detector
HAWC-300: March 2015 – Present : >95% uptime
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
300th WCD tank constructed/filled Jan 2015~3,900 tanker truck trips
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016 78
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Construction Video
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
HAWC Electronics
82
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J. Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J. Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
HAWC Data
• We read in every PMT hit all the time– Raw data rate - 500MB/s -10 VME Backplanes
• Trigger in Software– Trigger rate requiring ~30 hits in 300ns is ~25kHz
• Process in near real time• Rate to disk ~24MB/s -> ~2TB/day (everyday)• Data is moved by portable disk arrays to UNAM
– About once a week it’s driven to Mexico City– Moved over Internet II to UMD
• Raw Data plus processed data is stored in Mexico and Maryland – About a petabyte a year– Currently we have about 4 PB of storage at UMD
83
The Data Bus
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016–Energy deposited away from core7
Monte CarloSimulation
Gamma Hadron Separation (MC)
84
Gammas
Protons
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016–
HAWC-250 Data
85
Hadron Shower (off source) Likely Gamma Shower (Crab event)
HAWCData
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016 86
hadronic event gamma ray-like eventgamma/hadron parameter
Gamma - Hadron Separation
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Photon rich sample from the Crab
1 in 104 Events Kept25% Efficiency for Photons
With Strong Photon Cut
88
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Shower Curvature
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J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016J Goodman — Particle Astrophysics – Univ. of Maryland Fall 2016
Significant Improvement
93
3σ/sqrt(day) 5.5σ sqrt(day)
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Moon Shadow
94
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
17 Months of Data
95
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
17 Months of Data
96
Galactic Plane
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
17 Months of Data
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Mrk 501 - 23σ
Mrk 421 - 33σ
Galactic Plane
Crab Nebula - 105σ
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
17 Months of Data
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
17 Months of Data
99
Crab Mrk 421 Mrk 501
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100
Skymap — Milagro, 8 years
Crab Mrk 421 Mrk 501
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Skymap — HAWC, 507 daysCrabMrk 421 Mrk 501
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017 105
TeVC
atHAW
CLabe
ls:
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017 107
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
HAWC view of the Galactic Plane
108
• ~40sourcesseeninfirstyear• 25%arenew
Pulsar~8kpc(26,000ly)awaySupernovaremnantwithveryenergeticpulsar
Associationunclear
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Survey Results
109
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
2HWC J1953+294 - 12 months of data
113
• No previously known TeV source.
• New analysis by VERITAS, archival plus new data, source confirmed.
• Possible association 3FGL J1951.6+2926 / PWN DA 495?
PreliminaryReported errors
are stat. only
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
2HWC J1953+294 - 17 months of data
114
• No previously known TeV source.
• New analysis by VERITAS, archival plus new data, source confirmed.
• Possible association 3FGL J1951.6+2926 / PWN DA 495?
PreliminaryReported errors
are stat. only
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Energy Estimation
116
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
High Energy Sky (>56 TeV) with 1º
117
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Pulsar Wind Nebulae - Geminga
118
• Closest (250 parsecs) known middle aged (300ky) pulsar• Possible nearby cosmic ray acceleration site — explanation for positron excess (Yuksel et al. 2009)
• Not seen by IACTs, extent maybe larger than IACT FOV.• Ongoing morphological and spectral studies
Milagro - Point Search
XMM, Pavlov et al. 2010
Yüksel, Kistler, Stanev PRL 2009
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017 119
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Transient Search - The Crab Nebula
124
•Crab flares, continue up to TeV?•No activity in radio, IR, and X-rays.•HAWC Pass 4 data from Nov 26 2014 to June 2016.•>105σ in 315 transits.•Lightcurve binned in sidereal day.•Consistent with constant flux.
MeV-GeV gamma ray
Credit: NASA/DOE/Fermi LAT/R. Buehler
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Transient Search - The Crab Nebula
125
On October 3rd, 2016, AGILE (GeV) reported enhanced emission from the Crab Nebula (ATEL #9586). The Fermi-LAT *GeV) confirmed the detection in ATEL #9588, with flux up to 1.8 times larger than typical.
HAWC online monitoring shows the Crab to be fully consistent with its usual expectation over the same time period in the TeV.
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Transient Search - Mrk 421 / Mrk 501
126
Mrk 421
Mrk 501
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Transient Search - Mrk 501
127
April 5, 2016
April 8, 2016
April 7, 2016
April 6, 2016
Astronomer’sTelegramtoimmediatelyalertcommunityofactivity.
Monitoringallgamma-raysourcesvisibletoHAWCeveryday.
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Mrk421 January 1-6, 2017
128
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J. Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J. Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Multi-wavelength / Multi-messenger
• We have follow-up agreements with:– Swift– Fermi-LAT– IACTs
• FACT• HESS• MAGIC• VERITAS
– AMON– IceCube– ANTARES– LIGO/VIRGO
129
IceCubeATel:#7856HAWCFollow-upATel:#7868
HAWCATel#8922onMrk501flare
HAWC-triggered:• New source candidates lists.• follow-up observations by IACTs such as VERITAS and MAGIC
from Pass 1 release.• Flares from known gamma-ray sources.
Externally triggered:• IceCube alert on high confidence neutrino event (highest energy
pointed astrophysical track-like).
• Fermi alerts on flaring activities.
• LIGO/VIRGO gravitation wave event follow-up
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J. Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J. Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
LIGOEvents• Responding to LIGO events
– Sent Private GCN on first event– It was below our horizon
• Developed algorithm to look in a region– Analysis searches for excess counts over the steady-state cosmic-ray
background using 4 sliding time windows (0.1, 1, 10, and 100 seconds) shifted forward in time by 10% their width over the course of the entire day.
130
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017 131
Candidate1:RA:28.628(+01h54m30.63s)J2000Dec:+1.200(+01d11'59.1")J2000Error:+1.15(squareregion,halfside)Duration:10secondsPre-trialsp-value:2.55e-07Post-trialsp-value:0.08
Boxing Day Event
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2.6 ± 0.3 PeV
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J. Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J. Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
IceCube >2.6 PeV Muon Neutrino
• HAWC-111 live. Several hours out of HAWC’s FOV.
• Searches:– Integrated dataset (Steady, Aug 2013-May
2015 dataset)– Next Day / Prior Day– ±2 and ±5 days around the event.
• All searches consistent with cosmic-ray background.
133
IceCube Error Circle
HAWC-250 Integrated Data
IceCube ATel: #7856HAWC Follow-up ATel: #7868
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Transients: Gamma Ray Bursts
135
GRB 130427AHAWC-30zenith 57°scaler DAQ
[Astr
ophy
s. J. 8
00 (2
015)
, 78]
[K. S
park
s Woo
dle]
TITLE: GCN CIRCULAR NUMBER: 19423SUBJECT: GRB 160509A: non-observation of VHE emission with HAWCDATE: 16/05/11 17:27:37 GMT
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Dark Matter
136
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
HAWC: Dark Matter
Preliminary
• HAWC has sensitivity to indirect detection of TeV WIMPs in:- Satellite galaxies, the Galactic
Center, and galaxy clusters• Cosmological simulations predict
more satellite galaxies than observed– 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
137
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017–
Dark Matter - Segue-1
139102
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Dark Matter Limits
140
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
HAWC Data - no gamma ray cut
143
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Large Scale Anisotropy
144
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Anisotropy
145
Fitdipole+quadrupole+octupoletomapfor24-hrbackgroundestimationSubtractedfitrelativeintensityfrom24-hrmap
RegionsA,BandCaretheonlystatisticallysignificantexcesses(>5σpost-trials)
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~2 TeV
~5 TeV
~13.5 TeV
~45 TeV
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
HAWC IceCube Joint Fit
147
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Large-scale structures e.g. Fermi Bubbles
149
NASA / DOE / Fermi LAT / D. Finkbeiner & others
Credits: NASA's Goddard Space Flight Center
• Large scale, non-uniform structures extending above and below the Galactic center.• Edges line up with X-ray features.• Correlate with microwave excess (WMAP haze)• Both hadronic and leptonic model fit Fermi LAT data.
Leptonic model can explain both gamma ray and microwave excess.• First limits in TeV, hard spectrum is highly unlikely.
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Diffuse Emission
150
No Cut-off 150 GeV Cut-off
Fermi Bubbles
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
HAWC 90%CL upper limits
152
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Outriggers
- HAWCSparseOutriggerArray:EnhancedSensitivityabove10TeV- Accuratelydeterminecorepositionforshowersoffthemaintankarray.
- Increaseeffectiveareaabove10TeVby3-4x- FundedbyLANL/Mexico.- 2500litertanks:1/80th sizeofHAWCtanks.
117
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J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017J Goodman — Particle Astrophysics – Univ. of Maryland Winter 2017
Storm on the 13-14 January 2016
155
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Storm on the 19th of August
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Popocatépetl
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Outlook
• The HAWC observatory began full-scale operation in March 2015.
• It is now providing a nearly contiuous view of the transient TeV sky• Catalog of first year full operation is in prep (2HWC), with new TeV sources!
• Diverse science results, stay tuned!• Upgrade to expand the array to enhance effective area >10 TeV by 3-4x is
currently under installation.
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HAWC is now operationalIt is giving a new wide-field view of the TeV skyIt is synergistic with other instruments:
MOUs with VERITAS, IceCube, MAGIC, HESS, FermiIt is now providing a nearly contiuous view of the transient TeV sky
Summary