1 HAWC: Continuous, Wide Field of View Observations of the Very High Energy Sky Brenda Dingus, LANL HAWC US Spokesperson 14 Nov 2013

2 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/Microquasars ExtraGalactic Galactic

3 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   + +  o +…  e +  +  +… p +   + +  o +…  e +  +  +… Gamma-Rays Probe Accelerated Particles

4 Active Galactic Nuclei Massive Black Hole Accelerates Jet of Particles to Relativistic Velocities => Synchrotron Emission and Inverse Compton and/or Proton Cascades BeppoSAX MAGIC, CAT M. Hayashida Urry

5 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  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 minutes 5 hours

6 Fermi observation of GRB090510, z=0.9 Highest Observed Energy was 33 GeV with 16  -rays >1 GeV Constrained Lorentz Invariance at the Plank Mass scale HAWC would detect this GRB if it occurred in FOV. Gilmore& Taboada, (arXiv: ), predict 1.65 GRB/yr detected by HAWC Gamma-Ray Bursts

7 Wide Field of View, Continuous Operations Gamma-Ray Detectors Fermi AGILE EGRET TeV Sensitivity HAWC ARGO Milagro Tibet AS  VERITAS HESS MAGIC

8 Astroparticle Physics in press HAWC Sensitivity Differential Sensitivity per Quarter Decade of Energy

9 HAWC Sensitivity Angular ResolutionHadron Rejection

10 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

11 HAWC Design builds on the success of Milagro Milagro “1 st Generation” Water Cherenkov gamma-ray detector 2650m (8600’) elevation near Los Alamos, NM Covered pond of 4000 m 2 Operated HAWC “2 nd Generation” Water Cherenkov gamma-ray detector 4100m (13500’) elevation near Puebla, Mexico 300 water tanks spread over m 2 Construction , Operation x Milagro’s sensitivity with 10 x lower energy threshold ©Aurore Simonnet

12 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

13 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 Pico de Orizaba 5600 m (18,500’) Large Millimeter Telescope (50m dia. dish) HAWC

14 The HAWC Collaboration

15 The HAWC Collaboration Los 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 Barber Univ. of California, Irvine: Gaurang Yodh, Peter Karn Michigan State University: Jim Linnemann, Kirsten Tollefson, Dan Edmunds, Udara Abeysekara, Tilan Ukwatta George Mason University: Robert Ellsworth Colorado State University: Miguel Mostafa, Dave Warner, Megan Longo, Paco Salesa Grues, Michael Gussert University of New Hampshire: James Ryan Pennsylvania State University: Tyce DeYoung, Dmitry Zaborov, Kathryne Sparks University of Alabama: Patrick Toale University of New Mexico: John Matthews, Robert Lauer Michigan 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 Velazquez Universidad 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 Zepeda Universidad 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

16 11/ / / / /2013 Important Dates 13M USD project funding began Feb 2011 Operations with 100 water Cherenkov detectors in Aug 2013 Observatory complete in Aug 2014

17 HAWC on 4 Nov

18 DAQ, Analysis, & Archiving VME Backplane Front End Boards CAEN V1190 TDC 128 PMTs Readout Computer Trigger and Reconstruction Client Front End Boards CAEN V1190 TDC 128 PMTs Readout Computer Trigger and Reconstruction Client Trigger and Reconstruction Client Trigger and Reconstruction Client Analysis, Monitoring, Archiving Raw Data 500 MB/s Triggered Data 20 MB/s x10 24 Hour Raw Data 50 TB 2 Week Triggered Data 25 TB 1 Week Triggered 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

19 We’re detecting Gamma Rays!

20 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