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HAWC:Continuous, Wide Field of View Observations of the Very High Energy Sky

Brenda Dingus, LANLHAWC US Spokesperson14 Nov 2013

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Nature’s Particle Accelerators:Gamma-Ray Sources

HST Image of M87

Active Galactic Nuclei:Black Hole producing

relativistic jet of particles

Short Gamma-Ray Burst:

Binary Neutron Star Coalescing

Artist Conception of Short GRBs

Long Gamma-Ray Burst:Massive Star Collapsing

into a Black Hole

Pulsar Wind Nebula:Spinning Neutron Star powering a relativistic

wind

Chandra Image of Crab

HESS TeV

+ x-ray

Supernova Remnant

X-ray Binaries/Microquas

ars

Ext

raG

alac

tic

G

alac

tic

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Electrons:Synchrotron Emission•Probes Magnetic Field, Electron Energy

Inverse Compton Scattering•Probes Photon Field, Electron Energy

Synchrotron Self Compton•If photon field is synchrotron, then electron energies are determined•Quadratic relation between variability of TeV (IC) and X-rays (synch)

Hadrons:p + p -> p+ + po +… -> e + n + g +…

p + g -> p+ + po +… -> e + n + g +…

Gamma-Rays Probe Accelerated Particles

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Active Galactic Nuclei

Massive Black Hole Accelerates Jet of Particles to Relativistic Velocities=> Synchrotron Emission and Inverse Compton and/or Proton Cascades

BeppoSAXMAGIC, CAT

M. HayashidaUrry

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Active Galactic Nuclei Flares~40 known TeV AGN

• IACT observations of <<1% duty cycle/AGN detect no flaring in most HAWC’s will monitor all Northern AGN with 20% duty cycle/day (5 hrs) regardless of sun, moon, or weather

HAWC’s 5 s sensitivity is (10,1,0.1) Crab in (3 min, 5 hrs, 1/3 yr)

Worldwide Dataset of TeV Observations by IACTs of Mrk421

1 month

Tluczykont et al. 2010

3 minutes

5 hours

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Fermi observation of GRB090510, z=0.9

• Highest Observed Energy was 33 GeV with 16 g-rays >1 GeV

• Constrained Lorentz Invariance at the Plank Mass scale

HAWC would detect this GRB if it occurred in FOV.

Gilmore& Taboada, (arXiv:1306.1127), predict 1.65 GRB/yr detected by HAWC

Gamma-Ray Bursts

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Wide Field of View, Continuous Operations

Gamma-Ray Detectors

FermiAGILEEGRET

TeV Sensitivity

HAWCARGO

Milagro Tibet AS

VERITASHESS

MAGIC

8http://arxiv.org/abs/1306.5800 Astroparticle Physics in press

HAWC SensitivityDifferential Sensitivity per Quarter Decade of Energy

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HAWC Sensitivity

Angular Resolution Hadron Rejection

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Known sources are shown, but most of the high latitude sky has not been observed at TeV energies

HAWC’s Field Of View

Sources from TeVCAT.uchicago.edu

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HAWC Design builds on the success of Milagro

Milagro “1st Generation” Water Cherenkov gamma-ray detector• 2650m (8600’) elevation near Los

Alamos, NM• Covered pond of 4000 m2 • Operated 2000-2008HAWC “2nd Generation” Water Cherenkov gamma-ray detector• 4100m (13500’) elevation near Puebla,

Mexico• 300 water tanks spread over 25000 m2

• Construction 2010-14, Operation 2013-19

• 15 x Milagro’s sensitivity with 10 x lower energy threshold

©Aurore Simonnet

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HAWC Design

180 meters

140

meters

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

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HAWC Site Location in Mexico

• High Altitude Site of 4100 m with temperate climate and existing infrastructure

• 17 R.L. of atmospheric overburdenvs 27 R.L. at sea level

• Latitude of 19 deg N

Pico de Orizaba 5600 m

(18,500’)

Large Millimeter Telescope

(50m dia. dish)

HAWC

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The HAWC Collaboration

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The HAWC CollaborationLos Alamos National Laboratory: Brenda Dingus (US

spokesperson), : Gus Sinnis, John Pretz, Patrick Younk, Gerd Kunde, Pat Harding

University of Maryland: Jordan Goodman, Andrew Smith, Jim Braun, David Berley, Brian Baughman, Josh Wood

University of Wisconsin: Stefan Westerhoff, Segev BenZvi, Mike Duvernois, Zig Hampel-Arias, Dan Fiorino, Ian Wisher, Asif Imran, Tom Weisgarber

University of Utah: Dave Kieda, Wayne Springer, Ahron BarberUniv. of California, Irvine: Gaurang Yodh, Peter KarnMichigan State University: Jim Linnemann, Kirsten Tollefson,

Dan Edmunds, Udara Abeysekara, Tilan UkwattaGeorge Mason University: Robert EllsworthColorado State University: Miguel Mostafa, Dave Warner,

Megan Longo, Paco Salesa Grues, Michael GussertUniversity of New Hampshire: James RyanPennsylvania State University: Tyce DeYoung, Dmitry Zaborov,

Kathryne Sparks University of Alabama: Patrick ToaleUniversity of New Mexico: John Matthews, Robert LauerMichigan Technical University: Petra Hüntemeyer, Emanuele

Bonamente, Nathan Kelley-Hoskins, Michelle Hui, Hugo Ayala, Hao Zhou

NASA/Goddard Space Flight Center: Julie McEnery, Elizabeth Hays, Vlasios Vasileiou

Georgia Institute of Technology: Ignacio Taboada, Andreas Tepe, Dirk Lennarz

HAWC Technical Staff: Michael Schneider, Scott Delay

Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE): Alberto Carramiñana (Mexico Spokesperson), Eduardo Mendoza,

Luis Carrasco, William Wall, Daniel Rosa, Ibrahim Torres, Sergey Silich, Jason Walters

Universidad Nacional Autónoma de México (UNAM): Instituto de Astronomía; Maria Magdalena Gonzalez, Marco Martos, Sergio Mendoza, Dany Page, William Lee, Hector Hernández, Deborah Dultzin, Erika Benitez Instituto de Física: Rubén Alfaro Molina,

Varlen Grabski, Andres Sandoval Espinosa, Ernesto Belmont Moreno, Saul Aguilar Slazar Institudo de Ciencias Nucleares; Lukas Nellen, Gustaov Medina Tanco, Jaun Carlos D’Olivo Institudo de Geofísica:

José Valdés Galicia, Alejandro Lara, Rogelio Caballero Benemérita Universidad Autónoma de Puebla: Humberto Salazar

Ibarguen, Arturo Fernández, Caupatitzio Ramirez, Oscar Martínez, Eduardo Moreno Barbosa, Lorenzo Diaz, Alfonso Rosado

Universidad Autónoma de Chiapas: Cesar Álvarez Ochoa, Eli Santos Rodriguez, Roberto Arceo Reyes, Jorge Jara Jiménez

Universidad de Guadalajara: Eduardo de la Fuente, Enrique VelazquezUniversidad Michoacana de San Nicolás de Hidalgo: Luis Villaseñor,

Umberto Cotti, Juan Carlos Arteaga Velazquez, Pedro A. Miranda-Romagnoli, Roberto Noriega Papaqui, Eucario Gonzalo

Centrode Investigacion y de Estudios Avanzados: Arnulfo ZepedaUniversidad de Guanajuato: David Delepine, Gerardo Moreno, Edgar

Casimiro Linares, Marco Reyes, Luis Ureña, Mauro Napsuciale, Victor Migenes

CIC Instituto Politécnico Nacional: Jesus Martinez

USA: 16 institutions,

57 people

Mexico:15 institutions,

54 people

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11/2010

02/2012

08/2012

01/2013

05/2013

Important Dates13M USD project

funding began Feb 2011

Operations with 100 water Cherenkov detectors in Aug 2013

Observatory complete in Aug 2014

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HAWC on 4 Nov 2013

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DAQ, Analysis, & Archiving

VM

E B

ack

pla

ne

VM

E B

ack

pla

ne

Front EndBoards

CAENV1190TDC

128 PMTs

ReadoutComputer

Trigger andReconstruction

Client

Front EndBoards

CAENV1190TDC

128 PMTs

ReadoutComputer

Trigger andReconstruction

Client

Trigger andReconstruction

Client

Trigger andReconstruction

Client

Analysis, Monitoring,

Archiving

Raw Data500 MB/s

Triggered Data20 MB/s

x10

24 Hour Raw Data

50 TB

2 WeekTriggered Data

25 TB

1 WeekTriggered Data Portable Disk

• DAQ and Monitoring from off site with internet connection

• Reconstruction, analysis, and transient search performed on site

• Prompt receipt and notification of transients via internet to GCN, IAU, AMON, . . .

• Each week data is hand carried to Mexico City for transfer via internet to US (@ 50 MB/sec)

• 4 PB/year of data is archived in both US and Mexico

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We’re detecting Gamma Rays!

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• Operations began last summer with 1/3 of full detector

• HAWC Construction will be complete by the end of 2014

• Current work on calibration, reconstruction, and analysis algorithms is progressing well

• HAWC has detected known TeV sources of Crab, Mrk 421, and Mrk 501already

• New TeV sources coming soon!

Summary