Gran Sasso Science Institute - February 25, 2020 The High ......Excellent background rejection Large...

The High Altitude Water Cherenkov

Observatory

Gran Sasso Science Institute - February 25, 2020

Miguel Alejandro MostafáProfessor of P hysics, Astronomy and Astrophysics

Introduction & Motivation

The HAWC Observatory

Recent results

Outlook

Outline

2

3

4

1

Introduction

Cosmic Ray Flux

•At low E, solar magnetic fields strongly influence CR propagation

•At high E, the minimally deflected CRs are far less intense and thus much harder to detect.

UHECRs

Duldig, Science 314 (2006) 429-430

1 EeV ≝ 1018 eV

Fang & Murase, Nature Physics 14 (2018) 396–398

UHECR detection

Pierre Auger ObservatoryPublic Event Explorer

Page hosted by the Auger group atColorado State University

Size of the Pierre Auger Observatory

See Auger superimposed over LHC, Geneva GO

Recenter Auger in the current view.

Imagery ©2009 TerraMetrics, Map data ©2009 Tele Atlas -

UHECR detection

UHECR detection

0.38

0.42

0.46

km

-2 sr-1 y

r -1

-90

90

360 0

UHECR sky map

E > 8 EeV; 45° smoothing

Auger Collaboration, Science 357 (2017) 1266-1270

0.38

0.42

0.46

km

-2 sr

-1 y

r-1

-90

90

360 0

Supernova Remnants

•First resolved TeV γ-ray image of a Shell type SNR (Resolution ~10 arcmin)

•Acceleration source of cosmic rays, but is it evidence of protons?

H.E.S.S. Collaboration, Nature 432 (2004) 75

Supernova Remnants

Leptonic Hadronicvs.

Tanaka et al., The Astrophysical Journal 685 (2008) 988

Scientific Motivation

•Constrain the origin of cosmic rays by measuring gamma-ray spectra to 100 TeV.

•Probe particle acceleration in astrophysical jets with wide field of view, high duty factor observations.

•Explore new physics with an unbiased survey of the TeV sky.

Experimental Techniques

Space-based detectors Low energy threshold EGRET, Fermi-LAT

✓ Background free

✓ Large duty cycle

✓ Large aperture

- Small area


Imaging Atmospheric Cherenkov Telescopes High sensitivity HESS, MAGIC, VERITAS

✓ Large effective area

✓ Excellent background rejection

- Small aperture

- Low duty cycle


Ground array of air-shower particle detectors Large aperture + High duty cycle Milagro, Tibet, ARGO, HAWC

✓ Large aperture

✓ Excellent background rejection

✓ Large duty cycle

- Moderate area

HAWC

• 2nd generation water Cherenkov

•Wide instantaneous field of view (2 sr)

•High duty cycle (> 90%)

• Large area (22,000 m2)

A second generation wide-field γ-ray detector

10 parsecs

Main Features

•Most bright Galactic GeV sources extend to TeV

•Best instrument for hard spectrum and extended sources

The HAWC Observatory

300 - 7 m x 5 m steel Water Cherenkov Detectors (a.k.a. tanks) with 4 PMTs at 4,100 m a.s.l. in Mexico

Water Cherenkov Detectors

300 - 7 m x 5 m steel Water Cherenkov Detectors (a.k.a. tanks) with 4 PMTs at 4,100 m a.s.l. in Mexico

Dedicated laser calibration system


Dedicated laser calibration system

Effect of the laser calibration on the observation of the shadow of the Moon


deflection matches 2 TeV median energy angular resolution < shadow width of 1.2° position verifies pointing

HAWC site

HAWC site

Pico de Orizaba (18,500 ft)

LMT (4,600 m)

4,100 m a.s.l.

Deployment status

From2011to2015

x15 more sensitive than Milagro

Design improvements

Design improvements

Fermi-LATskysmoothedmapE>50GeV(Pass8-6yearsofdata)(courtesyofM.Ajello)

Design improvements

Fermi-LATskysmoothedmapE>50GeV(Pass8-6yearsofdata)(courtesyofM.Ajello)

PreliminaryHAWCsmoothedmapE>500GeV(~1yearofdata)Fullarray

Science ResultsPenn State HAWCers in Mexico (2017)

The Crab

Multi-TeV sky

Abeysekara et al [HAWC] ApJ 843 (2017) 39

first HAWC catalog



first HAWC catalogcoincident with VER J1930+188 SNR G54.1+00.3 — PSR J1930+1852 TeV emission was reported to be point-like and likely from PWN nearby molecular CO cloud

2HWC J1930+188

NEW

NEW

2HWC J1928+178coincident with PSR J1928+1746 tail towards unidentified source 3FGL J1925.4+1727 VERITAS pt-src upper limit ~1.4% of Crab

2HWC J1927+187*associated with 2HWC J1930+188? ongoing analysis on spatial morphology

first HAWC catalog


2HWC J1953+294VERITAS confirms HAWC detection nearby PWN likely counterpart

first HAWC catalog


2HWC J1953+294VERITAS confirms HAWC detection nearby PWN likely counterpart

[VERITAS+Fermi-LAT+HAWC!] ApJ 866 (2018) 24

first HAWC catalog

NEW


first HAWC catalog

NEW

0.041 0.08 0.12 0.16 0.2 0.24 0.28 0.32 0.36 0.4 0.44

70:00:00.072:00:00.074:00:00.076:00:00.078:00:00.080:00:00.082:00:00.0

-2:00:00.0-1:00:00.0

0:00:00.0

1:00:00.0

2:00:00.0

3:00:00.0

4:00:00.0

5:00


Geminga

Abeysekara et al [HAWC] Science 6365 (2017) 911-914

Extended emission

Positron excess from nearby pulsars?


Extended emission

surface brightness

10°3 10°2 10°1 100 101

Energy [TeV]

10°3

10°2

10°1

100

101

102

E3

J(E

)[G

eV2

m°

2s°

1sr

°1]

±=0.33 (base)±=0.31±=0.35ø=3.6£104yr

ø=4£103yrFit param. syst.3æ range (base)AMS-02 e+

10°310°2

10°110

010

1

Energy [TeV]

10°3

10°2

10°1

100

101

102

E3J(E)[GeV

2m

°2s

°1sr°

1 ]

±=0.33 (base)±=0.31±=0.35ø=3.6£104yr

ø=4£103yrFit param. syst.3æ range (base)AMS-02 e+


Extended emission

Estimated positron energy flux at Earth

SS 433

VHE emission from the jets of a microquasar

Abeysekara et al [HAWC] Nature 562 (2018), 82-85

Penn State HAWC group at home (2018)

Recent Developments

The Crab

Multi-TeV sky


, a.k.a. Kelly’s thesis

𝜸-ray sky above 56 TeV

Abeysekara et al [HAWC] Phys. Rev. Lett. 124 (2020) 021102

E > 1 TeV

E > 10 TeVE > 56 TeV

Abeysekara et al [HAWC] Phys. Rev. Lett. 124 (2020) 021102

The highest energy sources

FIG. 3 of the PRL

Outlook: Outriggers

60◦80◦100◦120◦

Galactic Longitude

−12◦

−6◦

+0◦

+6◦

+12◦

Ga

lact

icL

ati

tud

e 3FH

LJ0

240.

5+61

13

3FH

LJ0

205.

5+64

49

3FH

LJ0

057.

9+63

25

3FH

LJ0

025.

5+64

07

3FH

LJ2

238.

4+59

01

3FH

LJ2

229.

0+61

14

3FH

LJ2

102.

3+47

03

3FH

LJ2

056.

7+49

40

3FH

LJ2

032.

2+41

27

3FH

LJ2

028.

6+41

10e

3FH

LJ2

021.

5+40

26

3FH

LJ2

021.

0+40

31e

3FH

LJ2

018.

5+38

51

3FH

LJ2

021.

1+36

51

3FH

LJ2

015.

9+37

12

3FH

LJ2

004.

2+33

39

3FH

LJ1

952.

8+32

53

3FH

LJ1

954.

3+28

35

3FH

LJ1

925.

3+16

17

3FH

LJ1

923.

2+14

08e

3FH

LJ1

943.

9+21

17

3FH

LJ1

958.

1+24

37

3FH

LJ1

958.

6+28

46

3FH

LJ2

023.

3+31

54

3FH

LJ2

027.

0+33

43

3FH

LJ2

026.

7+34

49

3FH

LJ2

111.

4+46

05

3FH

LJ2

229.

4+53

49

3FH

LJ2

301.

9+58

55e

3FH

LJ2

323.

4+58

48

3FH

LJ2

329.

7+61

01

3FH

LJ0

014.

9+61

18

3FH

LJ0

035.

9+59

50

3FH

LJ0

131.

1+61

20

320◦340◦0◦20◦40◦−12◦

−6◦

+0◦

+6◦

+12◦

Ga

lact

icL

ati

tud

e 3FH

LJ1

911.

0+09

05

3FH

LJ1

907.

0+07

13

3FH

LJ1

855.

3+07

51

3FH

LJ1

857.

7+02

46e

3FH

LJ1

855.

5+01

42

3FH

LJ1

849.

4-00

56

3FH

LJ1

840.

9-05

32e

3FH

LJ1

839.

4-05

53

3FH

LJ1

838.

9-05

37

3FH

LJ1

836.

5-06

51e

3FH

LJ1

834.

1-07

06e

3FH

LJ1

824.

3-06

21

3FH

LJ1

823.

3-13

39

3FH

LJ1

813.

4-12

45

3FH

LJ1

804.

7-21

44e

3FH

LJ1

803.

1-21

48

3FH

LJ1

753.

8-25

37

3FH

LJ1

748.

0-24

46

3FH

LJ1

744.

5-26

09

3FH

LJ1

741.

8-25

36

3FH

LJ1

747.

2-28

22

3FH

LJ1

746.

2-28

52

3FH

LJ1

745.

6-29

00

3FH

LJ1

731.

7-30

03

3FH

LJ1

732.

6-31

31

3FH

LJ1

718.

0-37

26

3FH

LJ1

714.

0-38

11

3FH

LJ1

714.

4-38

29

3FH

LJ1

703.

4-41

45

3FH

LJ1

641.

1-46

19

3FH

LJ1

640.

6-46

33

3FH

LJ1

636.

3-47

31e

3FH

LJ1

633.

0-47

46e

3FH

LJ1

631.

6-47

56e

3FH

LJ1

626.

3-49

15

3FH

LJ1

620.

7-49

28

3FH

LJ1

603.

8-49

03

3FH

LJ1

616.

2-50

54e

3FH

LJ1

553.

8-53

25e

3FH

LJ1

534.

0-52

31

3FH

LJ1

427.

9-60

54

3FH

LJ1

443.

0-62

27e

3FH

LJ1

507.

9-62

28e

3FH

LJ1

459.

4-60

52

3FH

LJ1

509.

5-58

51

3FH

LJ1

514.

2-59

09e

3FH

LJ1

524.

8-59

04

3FH

LJ1

600.

3-58

11

3FH

LJ1

552.

7-56

11e

3FH

LJ1

615.

3-51

46e

3FH

LJ1

619.

7-50

59

3FH

LJ1

639.

3-51

45

3FH

LJ1

650.

3-50

45

3FH

LJ1

622.

9-50

04

3FH

LJ1

655.

5-47

37e

3FH

LJ1

652.

2-46

33e

3FH

LJ1

657.

6-46

56

3FH

LJ1

648.

5-46

10

3FH

LJ1

709.

7-44

29

3FH

LJ1

733.

4-39

42

3FH

LJ1

713.

5-39

45e

3FH

LJ1

745.

8-30

28e

3FH

LJ1

747.

2-29

59

3FH

LJ1

748.

1-29

03

3FH

LJ1

748.

6-28

16

3FH

LJ1

801.

5-24

50

3FH

LJ1

800.

5-23

43e

3FH

LJ1

800.

7-23

57

3FH

LJ1

809.

8-23

32

3FH

LJ1

801.

6-23

27

3FH

LJ1

811.

5-19

27

3FH

LJ1

830.

0-15

18

3FH

LJ1

826.

2-14

51

3FH

LJ1

824.

5-13

51e

3FH

LJ1

826.

1-12

56

3FH

LJ1

833.

6-10

34

3FH

LJ1

834.

5-08

46e

3FH

LJ1

838.

9-07

04e

3FH

LJ1

857.

0+00

59

3FH

LJ1

855.

9+01

21e

3FH

LJ1

911.

5+03

10

3FH

LJ1

907.

9+06

02

Fig.

13.—Adap

tivelysm

oothed

counts

map

show

ingthewhole

Galactic

plan

e0◦≤

l≤

360◦at

Galactic

latitudes

−14

◦≤

b≤

14◦divid

edin

fourpan

els.Thepan

elsare

centeredat

l=

90◦,

0◦,

270◦an

d180

◦,from

topto

bottom

.Detected

point

sources

aremarked

with

across

whereas

extended

sources

areindicated

with

their

extension

s.Only

sources

locatedat

−4◦≤

b≤

4◦are

labelled

,plustheCrab

Nebula.

36

60◦80◦100◦120◦

Galactic Longitude

−12◦

−6◦

+0◦

+6◦

+12◦

GalacticLatitude 3FH

LJ0240.5+6113

3FHL

J0205.5+6449

3FHL

J0057.9+6325

3FHL

J0025.5+6407

3FHL

J2238.4+5901

3FHL

J2229.0+6114

3FHL

J2102.3+4703

3FHL

J2056.7+4940

3FHL

J2032.2+4127

3FHL

J2028.6+4110e

3FHL

J2021.5+4026

3FHL

J2021.0+4031e

3FHL

J2018.5+3851

3FHL

J2021.1+3651

3FHL

J2015.9+3712

3FHL

J2004.2+3339

3FHL

J1952.8+3253

3FHL

J1954.3+2835

3FHL

J1925.3+1617

3FHL

J1923.2+1408e

3FHL

J1943.9+2117

3FHL

J1958.1+2437

3FHL

J1958.6+2846

3FHL

J2023.3+3154

3FHL

J2027.0+3343

3FHL

J2026.7+3449

3FHL

J2111.4+4605

3FHL

J2229.4+5349

3FHL

J2301.9+5855e

3FHL

J2323.4+5848

3FHL

J2329.7+6101

3FHL

J0014.9+6118

3FHL

J0035.9+5950

3FHL

J0131.1+6120

320◦340◦0◦20◦40◦−12◦

−6◦

+0◦

+6◦

+12◦

GalacticLatitude 3FH

LJ1911.0+0905

3FHL

J1907.0+0713

3FHL

J1855.3+0751

3FHL

J1857.7+0246e

3FHL

J1855.5+0142

3FHL

J1849.4-0056

3FHL

J1840.9-0532e

3FHL

J1839.4-0553

3FHL

J1838.9-0537

3FHL

J1836.5-0651e

3FHL

J1834.1-0706e

3FHL

J1824.3-0621

3FHL

J1823.3-1339

3FHL

J1813.4-1245

3FHL

J1804.7-2144e

3FHL

J1803.1-2148

3FHL

J1753.8-2537

3FHL

J1748.0-2446

3FHL

J1744.5-2609

3FHL

J1741.8-2536

3FHL

J1747.2-2822

3FHL

J1746.2-2852

3FHL

J1745.6-2900

3FHL

J1731.7-3003

3FHL

J1732.6-3131

3FHL

J1718.0-3726

3FHL

J1714.0-3811

3FHL

J1714.4-3829

3FHL

J1703.4-4145

3FHL

J1641.1-4619

3FHL

J1640.6-4633

3FHL

J1636.3-4731e

3FHL

J1633.0-4746e

3FHL

J1631.6-4756e

3FHL

J1626.3-4915

3FHL

J1620.7-4928

3FHL

J1603.8-4903

3FHL

J1616.2-5054e

3FHL

J1553.8-5325e

3FHL

J1534.0-5231

3FHL

J1427.9-6054

3FHL

J1443.0-6227e

3FHL

J1507.9-6228e

3FHL

J1459.4-6052

3FHL

J1509.5-5851

3FHL

J1514.2-5909e

3FHL

J1524.8-5904

3FHL

J1600.3-5811

3FHL

J1552.7-5611e

3FHL

J1615.3-5146e

3FHL

J1619.7-5059

3FHL

J1639.3-5145

3FHL

J1650.3-5045

3FHL

J1622.9-5004

3FHL

J1655.5-4737e

3FHL

J1652.2-4633e

3FHL

J1657.6-4656

3FHL

J1648.5-4610

3FHL

J1709.7-4429

3FHL

J1733.4-3942

3FHL

J1713.5-3945e

3FHL

J1745.8-3028e

3FHL

J1747.2-2959

3FHL

J1748.1-2903

3FHL

J1748.6-2816

3FHL

J1801.5-2450

3FHL

J1800.5-2343e

3FHL

J1800.7-2357

3FHL

J1809.8-2332

3FHL

J1801.6-2327

3FHL

J1811.5-1927

3FHL

J1830.0-1518

3FHL

J1826.2-1451

3FHL

J1824.5-1351e

3FHL

J1826.1-1256

3FHL

J1833.6-1034

3FHL

J1834.5-0846e

3FHL

J1838.9-0704e

3FHL

J1857.0+0059

3FHL

J1855.9+0121e

3FHL

J1911.5+0310

3FHL

J1907.9+0602

Fig.13.—

AdaptivelysmoothedcountsmapshowingthewholeGalacticplane0 ◦≤l≤360 ◦atGalactic

latitudes−14◦≤b≤14◦dividedinfourpanels.Thepanelsarecenteredatl=90◦,0 ◦,270 ◦and180 ◦,from

toptobottom.Detectedpointsourcesaremarkedwithacrosswhereasextendedsourcesareindicatedwith

theirextensions.Onlysourceslocatedat−4 ◦≤b≤4 ◦arelabelled,plustheCrabNebula.

36

Outlook: HAWC South

H.E.S.S.

Fermi-LAT

HAWC

Galactic Center

Conclusions• Extended regions, transient

events, highest energies

Main results

• Dark matter, extended regions, diffuse emission, cosmic rays, …

• EBL, solar physics, …

Other results



Main results



Other results

Multi-wavelength physics

• MoUs with IceCube, IACTs, etc • AMON • HAWC alerts



Main results



Other results

Multi-wavelength physics

• MoUs with IceCube, IACTs, etc • AMON • HAWC alerts

Outlook• Array of Outriggers • Southern Observatory



Main results

Thank you very muchThe HAWC Collaboration

Recent HAWC publications• “Multiple Galactic Sources with Emission Above 56 TeV Detected by HAWC,”

Physical Review Letters 124 (2020) 021102

• “Measurement of the Crab Nebula Spectrum Past 100 TeV with HAWC,” The Astrophysical Journal 881 (2019) 134

• “Searching for dark matter sub-structure with HAWC,” Journal of Cosmology and Astroparticle Physics 07 (2019) 022

• “MAGIC and Fermi-LAT gamma-ray results on unassociated HAWC sources,” Monthly Notices of the Royal Astronomical Society 485, 356 (2019)

• “All-sky Measurement of the Anisotropy of Cosmic Rays at 10 TeV and Mapping of the Local Interstellar Magnetic Field,” The Astrophysical Journal 871, 96 (2019)

• “Very-high-energy particle acceleration powered by the jets of the microquasar SS 433,” Nature 562, 82-85 (2018)

• “Constraints on spin-dependent dark matter scattering with long-lived mediators from TeV observations of the Sun with HAWC,” Physical Review D 98, 123012 (2018)

Gran Sasso Science Institute - February 25, 2020 The High ......Excellent background rejection Large...

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Transcript of Gran Sasso Science Institute - February 25, 2020 The High ......Excellent background rejection Large...