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Detecting Air Showers on the Ground

Published byAdela Stevenson Modified over 9 years ago

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Presentation on theme: "Detecting Air Showers on the Ground"— Presentation transcript:

1 Detecting Air Showers on the Ground
Outline Air Shower Physics Extensive Air Showers Gamma/Hadron sep. Why use EAS Detectors Detecting showers on the ground Water Cherenkov - Milagro RPCs – ARGO Milagro Jordan Goodman University of Maryland

2 University of Maryland
Extensive Air Shower Development Jordan Goodman University of Maryland

3 University of Maryland
From Ralph Engel Jordan Goodman University of Maryland

4 University of Maryland
Extensive Air Shower Jordan Goodman University of Maryland

5 University of Maryland
Effect of Altitude ARGO Milagro Low Energy Threshold Requires High Altitude Jordan Goodman University of Maryland

6 University of Maryland
Cascade Development ARGO Milagro 1 TeV 10 TeV Jordan Goodman University of Maryland

7 Gamma Shower 2 TeV (movies by Miguel Morales)
Blue – Electrons Muons – Yellow Pions – Green Nucleons – Purple Jordan Goodman University of Maryland

8 Proton Shower 2 TeV (movies by Miguel Morales)
Blue – Electrons Muons – Yellow Pions – Green Nucleons – Purple Jordan Goodman University of Maryland

9 University of Maryland
Gamma Shower Content Ngammas Nelectrons Primary Energy (GeV) Jordan Goodman University of Maryland

10 Lateral distribution of EM energy and muons
EM energy from 500 GeV g Muons from 500 GeV Proton Muons from 500 GeV Proton EM energy from 500 GeV g Jordan Goodman University of Maryland

11 Techniques in TeV Astrophysics
Non-pointed instruments Pointed instruments High energy threshold Moderate background rejection Large field of view (~2sr) High duty cycle (>90%) Good for all sky monitor and for investigation of transient and diffuse sources. Low energy threshold Good background rejection Small field of view Low duty cycle Good for sensitive studies of known point sources. Jordan Goodman University of Maryland

12 University of Maryland
Jordan Goodman University of Maryland

13 University of Maryland
Sampling the Shower Water Tanks Scintillators Jordan Goodman University of Maryland

14 University of Maryland
Cherenkov Radiation When a charged particle moves through transparent media faster than speed of light in that media. Cherenkov radiation Cone of light Jordan Goodman University of Maryland

15 University of Maryland
Cherenkov Radiation Jordan Goodman University of Maryland

16 University of Maryland
Jordan Goodman University of Maryland

17 University of Maryland
Auger Jordan Goodman University of Maryland

18 University of Maryland
EAS g - Tibet Jordan Goodman University of Maryland

19 University of Maryland
IceTop Jordan Goodman University of Maryland

20 University of Maryland
ARGO Jordan Goodman University of Maryland

21 Limited Streamer Tubes
Jordan Goodman University of Maryland

22 University of Maryland
ARGO Design Jordan Goodman University of Maryland

23 RPC Satisfied the Requirements on Element of Carpet
Resistive Plate Chamber Low cost , high efficiency, high space & time resolution (<1ns), easy access to any part of detector, robust assembling, easy to achieve >90% coverage, mounting without mechanical supports. RPC PAD STRIP Jordan Goodman University of Maryland 2850x1258mm2

24 University of Maryland
ARGO Building Jordan Goodman University of Maryland

25 University of Maryland
DAQ RPC Jordan Goodman University of Maryland

26 University of Maryland
ARGO Events ARGO will be a very capable detector when completed in several years! Jordan Goodman University of Maryland

27 University of Maryland
Milagro 450 Top Layer 8” PMTs 273 Bottom Layer 8” PMTs 8 m 80m 50m Jordan Goodman University of Maryland

28 University of Maryland
Milagro Site Jordan Goodman University of Maryland

29 University of Maryland
Milagro Jordan Goodman University of Maryland

30 University of Maryland
Milagro Outriggers Jordan Goodman University of Maryland

31 Shower hitting the pond at an angle
Jordan Goodman University of Maryland

32 2 Tev Proton Shower hitting the pond
Jordan Goodman University of Maryland

33 2 Tev E/M Shower hitting the pond
Jordan Goodman University of Maryland

34 University of Maryland
Angle Reconstruction For large showers, the angle can be reconstructed to better than 0.50o. (However, there are systematics associated with core location) Jordan Goodman University of Maryland

35 University of Maryland
Events Jordan Goodman University of Maryland

36 University of Maryland
Shower Curvature Jordan Goodman University of Maryland

37 University of Maryland
Conical shape from ARGO Jordan Goodman University of Maryland

38 Curvature Correction Curved Shower Front 7ns/100m
The shower front is not a plane, but is curved about the shower core Times of individual PMTs are adjusted based on the distance to the shower core Core Location Error vs True Core Distance from Center of Pond Without Outriggers Core Error (meters) Core Distance (meters) Curved Shower Front 7ns/100m With Outriggers Core Error (meters) Jordan Goodman University of Maryland Core Distance (meters)

39 Why Use EAS Detectors to Study Gammas
Transient Sources GRB’s Don’t know when or where to look Some indications of 2nd hard comp. Variable Sources Diffuse Sources Galactic Plane New Sources Jordan Goodman University of Maryland

40 Gamma – Hadron Separation
Jordan Goodman University of Maryland

41 University of Maryland
Tibet III + MUON 8,640 m2 Jordan Goodman University of Maryland

42 University of Maryland
miniHAWC g mini- High Altitude Water Cherenkov experiment Jordan Goodman University of Maryland

43 University of Maryland
Detector Layout Milagro: 450 PMT (25x18) shallow (1.4m) layer 273 PMT (19x13) deep (5.5m) layer 175 PMT outriggers Instrumented Area: ~40,000m2 PMT spacing: 2.8m Shallow Area: 3500m2 Deep Area: 2200m2 HAWC: 5625 or PMTs (75x75x(1 or 2)) Single layer at 4m depth or 2 layers at Milagro depths Instrumented Area: 90,000m2 PMT spacing: 4.0m Shallow Area: 90,000m2 Deep Area: 90,000m2 miniHAWC: 841 PMTs (29x29) 5.0m spacing Single layer with 4m depth Instrumented Area: 22,500m2 PMT spacing: 5.0m Shallow Area: 22,500m2 Deep Area: 22,500m2 Jordan Goodman University of Maryland

44 Gamma/Hadron Separation
Gammas Protons 30 GeV 70 GeV 230 GeV 20 GeV 270 GeV Size of miniHAWC Size of Milagro deep layer Jordan Goodman University of Maryland

45 University of Maryland
Curtains A high altitude version of Milagro would trigger at >10kHz. Need to control spurious triggers due to single muons. Install curtains to optically isolate the PMTs. Intrinsic Gamma hadron separation Jordan Goodman University of Maryland

46 University of Maryland
MiniHAWC  4m 5 m miniHAWC 170m 150m m 6m Jordan Goodman University of Maryland

47 University of Maryland
Tibet – 4300m ARGO Jordan Goodman University of Maryland

48 Comparison of Effective Areas
50 Tube Trigger Jordan Goodman University of Maryland

49 University of Maryland
The Diffuse Galactic Plane in miniHAWC and HAWC Use Neutral H map to trace out VHE Gamma-Ray flux. Normalize to Milagro observed TeV diffuse emission from the Galactic plane. Jordan Goodman University of Maryland

50 Conclusions on Air Shower Detectors
They are complimentary to ACTs Their features of wide field of view and continuous observation gives them the ability to: Observe transient sources Observe diffuse objects Discover new objects Jordan Goodman University of Maryland

51

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