the hawc ( high altitude water cherenkov) observatory
DESCRIPTION
The HAWC ( High Altitude Water Cherenkov) Observatory. The HAWC Collaboration. Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE) : Alberto Carramiñana, Eduardo Mendoza, Luis Carrasco, William Wall, Daniel Rosa, Guillermo Tenorio Tagle, Sergey Silich - PowerPoint PPT PresentationTRANSCRIPT
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The HAWC(High Altitude Water
Cherenkov) Observatory
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The HAWC CollaborationThe HAWC CollaborationUniversity of Maryland: Jordan Goodman, Andrew Smith,
Greg Sullivan, Jim Braun, David Berley
Los Alamos National Laboratory: Gus Sinnis, Brenda Dingus, John Pretz
University of Wisconsin: Teresa Montaruli, Stefan Westerhoff, Segev Ben Zvi, Juanan Aguilar, Dan Wahl
University of Utah: Dave Kieda, Wayne Springer
Univ. of California, Irvine: Gaurang Yodh’
Michigan State University: Jim Linnemann, Kirsten Tollefson, Dan Edmunds
George Mason University: Robert Ellsworth
Colorado State University: Miguel Mustafa, Dave Warner
University of New Hampshire: James Ryan
Pennsylvania State University: Tyce DeYoung, Patrick Toale, Kathryne Sparks
University of New Mexico: John Matthews, William Miller
Michigan Technical University: Petra Hüntemeyer
NASA/Goddard Space Flight Center: Julie McEnery, Elizabeth Hays, Vlasios Vasileiou
Georgia Institute of Technology: Ignacio Taboada, Andreas Tepe
HAWC Technical Staff: Michael Scheinder, Scott Delay
Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE): Alberto Carramiñana, Eduardo Mendoza, Luis Carrasco, William Wall, Daniel Rosa, Guillermo Tenorio Tagle, Sergey Silich
Universidad Nacional Autónoma de México (UNAM): Instituto de Astronomía: Octavio Valenzuela, V ladimir Avila-Reese, Marco Martos, Maria Magdalena Gonzalez, Sergio Mendoza, Dany Page, William Lee, Hector Hernández, Deborah Dultzin, Erika Benitez Instituto de Física: Arturo Menchaca, Rubén Alfaro, Varlen Grabski, Andres Sandoval, Ernesto Belmont. Arnulfo Matinez-Davalos Instituto de Ciencias Nucleares: Lukas Nellen, Gustavo Medina-Tanco, Juan Carlos D’Olivo Instituto de Geofísica: José Valdés Galicia, Alejandro Lara, Rogelio Caballero
Benemérita Universidad Autónoma de Puebla:Humberto Salazar, Arturo Fernández, Caupatitzio Ramirez, Oscar Martínez, Eduardo Moreno, Lorenzo Diaz, Alfonso Rosado,
Universidad Autónoma de Chiapas: Cesar Álvarez, Eli Santos Rodriguez, Omar Pedraza
Universidad de Guadalajara: Eduardo de la Fuente
Universidad Michoacana de San Nicolás de Hidalgo: Luis Villaseñor, Umberto Cotti, Ibrahim Torres, Juan Carlos Arteaga Velazquez
Centrode Investigacion y de Estudios Avanzados: Arnulfo Zepeda
Universidad de Guanajuato: David Delepine, Gerardo Moreno, Edgar Casimiro Linares, Marco Reyes, Luis Ureña, Mauro Napsuciale, Victor Migenes
USAMexico
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The HAWC CollaborationThe HAWC CollaborationUniversity of Maryland: Jordan Goodman, Andrew Smith,
Greg Sullivan, Jim Braun, David Berley
Los Alamos National Laboratory: Gus Sinnis, Brenda Dingus, John Pretz
University of Wisconsin: Teresa Montaruli, Stefan Westerhoff, Dan Wahl
University of Utah: Dave Kieda, Wayne Springer
Univ. of California, Irvine: Gaurang Yodh
Michigan State University: Jim Linnemann, Kirsten Tollefson, Dan Edmunds
George Mason University: Robert Ellsworth
University of New Hampshire: James Ryan
Pennsylvania State University: Tyce DeYoung, Patrick Toale, Kathryne Sparks
University of New Mexico: John Matthews, William Miller
Michigan Technical University: Petra Hüntemeyer
NASA/Goddard Space Flight Center: Julie McEnery, Elizabeth Hays, Vlasios Vasileiou
Georgia Institute of Technology: Ignacio Taboada, Andreas Tepe
HAWC Technical Staff: Michael Scheinder, Scott Delay
Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE): Alberto Carramiñana, Eduardo Mendoza, Luis Carrasco, William Wall, Daniel Rosa, Guillermo Tenorio Tagle, Sergey Silich
Universidad Nacional Autónoma de México (UNAM): Instituto de Astronomía: Octavio Valenzuela, V ladimir Avila-Reese, Marco Martos, Maria Magdalena Gonzalez, Sergio Mendoza, Dany Page, William Lee, Hector Hernández, Deborah Dultzin, Erika Benitez Instituto de Física: Arturo Menchaca, Rubén Alfaro, Varlen Grabski, Andres Sandoval, Ernesto Belmont. Arnulfo Matinez-Davalos Instituto de Ciencias Nucleares: Lukas Nellen, Gustavo Medina-Tanco, Juan Carlos D’Olivo Instituto de Geofísica: José Valdés Galicia, Alejandro Lara, Rogelio Caballero
Benemérita Universidad Autónoma de Puebla:Humberto Salazar, Arturo Fernández, Caupatitzio Ramirez, Oscar Martínez, Eduardo Moreno, Lorenzo Diaz, Alfonso Rosado,
Universidad Autónoma de Chiapas: Cesar Álvarez, Eli Santos Rodriguez, Omar Pedraza
Universidad de Guadalajara: Eduardo de la Fuente
Universidad Michoacana de San Nicolás de Hidalgo: Luis Villaseñor, Umberto Cotti, Ibrahim Torres, Juan Carlos Arteaga Velazquez
Centrode Investigacion y de Estudios Avanzados: Arnulfo Zepeda
Universidad de Guanajuato: David Delepine, Gerardo Moreno, Edgar Casimiro Linares, Marco Reyes, Luis Ureña, Mauro Napsuciale, Victor Migenes
USA Mexico
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HAWC Collaboration April 2010
HAWC Science ObjectivesHAWC Science Objectives
• Discover the origin of cosmic rays by measuring gamma-ray spectra to 100 TeV
– Hadronic sources have unbroken spectra beyond 30-100 TeV– Galactic diffuse gamma rays probe the distant cosmic ray flux
• Understand particle acceleration in astrophysical jets with wide field of view, high duty factor observations.
– Trigger Multi-Messenger/Multi-Wavelength Observations of Flaring Active Galactic Nuclei (including TeV orphan flares)
– Detect Short and Long Gamma-Ray Bursts
• Explore new physics via HAWC’s unbiased survey of ½ the sky.
– Increase understanding of TeV sources to search for new physics.
– Study the local TeV cosmic rays and their anisotropy.
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HAWC ScienceHAWC 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.
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Comparison of Gamma-Ray Comparison of Gamma-Ray Detectors Detectors
Large Aperture/High Duty CycleMilagro, Tibet, ARGO, HAWC
Moderate Area
Excellent Background Rejection
Large Duty Cycle/Large Aperture
Unbiased Sky Survey
Extended sources
Transients (GRB’s) > 100 GeV
High Energies up to 100 TeV
Low Energy ThresholdEGRET/Fermi
Space-based (Small Area)
“Background Free”
Large Duty Cycle/Large Aperture
Sky Survey (< 10 GeV)
AGN Physics
Transients (GRBs) < 300 GeV
High SensitivityHESS, MAGIC, VERITAS
Large Effective Area
Excellent Background Rejection
Low Duty Cycle/Small Aperture
High Resolution Energy Spectra up to ~20 TeV
Studies of known sources
Surveys of limited regions of sky
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HAWC Collaboration April 2010
Milagro and HAWCMilagro 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)
IntroIntro
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HAWC Science ReviewsHAWC Science Reviews
• PASAG - October 2009 – HAWC is a moderate-priced initiative that will
carry out excellent astrophysics using a novel technique; there is also the possibility of surprising results of relevance for particle physics.
• NSF Review Panel December 2007: – “There is a strong case for HAWC as a wide
field of view survey instrument at the TeV scale.” They concluded the project is well understood and technically ready with a strong collaboration.
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Abdo et al. ApJL (accepted)arXiv:0904.1018
15 TeV associations out
of 35 likely galactic sources
in our field of view
Milagro Results
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GeV Pulsars Produce TeV PWNGeV Pulsars Produce TeV PWN
GeV Emission is pulsed & due to rotation axis misaligned with Magnetic Dipole of ~1012 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
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Geminga (J0634.0+1745)Geminga (J0634.0+1745)
• 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
10 parsecs
68% PSFMilagro
HAWC Milagro sees Geminga at 30% of the Crab at ~20 TeVwhile IACTs have a limit of ~1% of the Crab at >200 GeV
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Geminga with HAWCGeminga with HAWC
• 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
10 parsecs
Milagro sees Geminga at 30% of the Crab at ~20 TeVwhile IACTs have a limit of ~1% of the Crab at >200 GeV
HAWC
68% PSFMilagro
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Milagro Spectrum of the CrabMilagro Spectrum of the Crab
HESS Crab data/fit
Energy reach from ~3TeV to >100 TeVPeak sensitivity for E-2 source at ~100 TeV
Milagro68%
HAWC
Milagro Results
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Milagro Spectrum of the Crab w/HAWCMilagro Spectrum of the Crab w/HAWC
Energy reach from ~3TeV to >100 TeVPeak sensitivity for E-2 source at ~100 TeV
Milagro68%
HAWC
HEGRA Crab data/fit
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In Milagro J2019+37 is 700 mCrabThe flux in γ/s >200 GeV is 95mCrab
HESS Crab fit:(Io =3.76x10-7,Γ=2.39,Ec=14.1 TeV)
MGRO J2019+37/ 0FGL J2020.8+3649MGRO J2019+37/ 0FGL J2020.8+3649
Milagro68%
HAWC
Milagro Results
This source is almost as bright as the Crab at Milagro’s energy
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In Milagro J2019+37 is 700 mCrabThe flux in γ/s >200 GeV is 95mCrab
HESS Crab fit:(Io =3.76x10-7,Γ=2.39,Ec=14.1 TeV)
MGRO J2019+37/ 0FGL J2020.8+3649MGRO J2019+37/ 0FGL J2020.8+3649
Milagro68%
HAWC
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MGRO J1908+06MGRO J1908+06
Ecut 14 40 (1σ56 (2σ
Milagro68%
HAWC
Milagro Results
A Milagro discovered source now seen by HESS and VERITASUsing 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)
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Milagro 3Milagro 3σσ source detected at 20 source detected at 20σσ HAWC (3months) HAWC (3months)HAWC Simulation
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HAWC Simulation
Milagro 3Milagro 3σσ source detected at 20 source detected at 20σσ HAWC (3months) HAWC (3months)
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HAWC Simulation
Milagro 3Milagro 3σσ source detected at 20 source detected at 20σσ HAWC (3months) HAWC (3months)
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Diffuse TeV ExcessDiffuse TeV Excess• Whether or not there is a GeV excess, Milagro sees a TeV excess.
• This excess could be due to unresolved sources or hadronic cosmic rays hitting matter near their source.
• If the TeV excess has a flat spectrum, it is likely hadronic in origin and may not be detectable at GeV energies.
– With help from ACTs and Fermi we will do a source subtraction
– This will allow us to measure the spectrum and morphology of the excess
• This study could point to regionsof the galaxy with a higher concentration of cosmic raysthan near earth - pointing to sites of acceleration.
Abdo et. al ApJ 2008
Milagro Results
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Active Galactic Nuclei Flares Active Galactic Nuclei Flares
• HAWC makes daily observations without weather, moon, or solar constraints. • HAWC’s 5 σ sensitivity for Mrk 421 is (10,1,0.1) Crab in (3 min, 5 hrs, 1/3 yr)
• HAWC will notify multiwavelength observers in real time of flaring AGN• Study correlations with x-rays, etc to determine emission mechanisms
• Discovery potential for orphan TeV flares producing neutrinos and UHECR
1 month
Milagro’s 9σ Mrk421
X-ray flux
Mila
gro
flux
Quadratic or Linear? Synchrotron Self
Compton or External Compton?
Crab Flux
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Distinguishing New Physics from AstrophysicsDistinguishing New Physics from Astrophysics
• Violation of Lorentz Invariance OR Energy Dependent Particle Acceleration– HAWC will detect multiple flaring extragalactic sources (AGN and
GRBs) to resolve redshift vs source mechanisms
• Cosmological Star Formation OR Spectral Cut-offs in the source– HAWC will trigger multiwavelength observations of flaring AGN to
obtain best measured and modeled TeV spectra
• Continuum Gamma-Ray Emission from Dark Matter Annihilation OR Astrophysical Source– HAWC will search for time variability which would imply an
astrophysical source
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Cosmic Ray ObservationsCosmic Ray Observations
• Milagro data show an unexpected anisotropy (PRL 101, 221101, 2008)
• No weighting or cutting.
• Map dominated by charged cosmic rays.
• 10o smoothing, looking for intermediate sized features.
• Two regions of excess 15.0σ and 12.7σ. Fractional excess of 6x10-4 (4x10-4) for region A(B).
HeliotailGeminga
Significance (σ’s)
Milagro Results
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21http://people.roma2.infn.it/~aldo/RICAP09_trasp_Web/Vernetto_ARGO_RICAP09ar.pdf
Milagro Results
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HAWC Collaboration April 2010
Cosmic Ray AnisotropyCosmic 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 gamma-hadron rejection can:– Measure the spectrum with much higher precision
– Measure the gamma-ray fraction
• Understanding this is important for Dark Matter Searches
Milagro Results
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HAWC Collaboration April 2010
Geminga as a Local Cosmic Ray SourceGeminga as a Local Cosmic Ray Source
• “If the observed cosmic ray excess does indeed arise from the Geminga SN explosion, the long–sought “smoking gun” connecting cosmic rays with supernovae would finally be at hand. - Salvati and Sacco (AA 09)
• 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
arXiv:0810.2784
PAMELA’s positron excess
Fit well given Milagro’s flux from Geminga