Observation of the Forbush decrease of 22 th June 2015 with the LAGO - - PowerPoint PPT Presentation

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Observation of the Forbush decrease of 22 th June 2015 with the LAGO - - PowerPoint PPT Presentation

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Observation of the Forbush decrease of 22 th June 2015 with the LAGO detector in Brazil Anderson Campos Fauth 1 , Henrique Vieira de Souza 1 for the LAGO Collaboration 2 1 Instituto de Fsica Gleb Wataghin - Unicamp, Brazil 2 full list of members

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Observation of the Forbush decrease of 22th June 2015 with the LAGO detector in Brazil

Anderson Campos Fauth1, Henrique Vieira de Souza1 for the LAGO Collaboration2

1Instituto de Física Gleb Wataghin - Unicamp, Brazil

2full list of members and institutions at lagoproject.org/collab.html

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What is LAGO?

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  • The Latin American Giant Observatory (LAGO) is an extended

cosmic ray observatory composed of water-Cherenkov detectors (WCDs) placed throughout Latin America

  • The study of the space weather through the solar modulation
  • f galactic cosmic rays
  • A collaborative and non-centralized network of institutions

from ten countries (Argentina, Bolivia, Brazil, Colombia, Ecuador, Guatemala, Mexico, Peru, Venezuela and Spain)

  • 28 institutions, 113 members
  • Developments, expertise and data are shared across the LAGO

network

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The LAGO sites

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Geomagnetic rigidity cut-off (GV) The LAGO collaboration uses single or small arrays of detectors located at different altitude sites and covering a large range of geomagnetic rigidity cut-offs

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Chacaltaya, Bolivia

Some LAGO detectors

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Sierra Negra, Mexico Antarctica, by Argentina Bariloche, Argentina

Merida, Venezuela

Guatemala

Campina Grande, Brazil

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What is TANCA?

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University of Campinas TANCA Campinas, SP, Brazil 22º 54’ S, 47º 03 N 650 meters a.s.l.

TANCA is a nickname for the TANk detector of CAmpinas, the LAGO water-Cherenkov detector at University of Campinas, Brazil.

South Atlantic Anomaly

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The TANCA detector

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  • 3 PMT 9” Photonis XP1805
  • Liner Tyvek
  • 11400 liters of pure water
  • Areavertical = 10 m2

50ns; 10mV

Muon pulse Photonis XP1805

Voltage-divider, HV power supply

Water level height 1.14 m

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The TANCA DAq

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CAMAC/NIM modules: LeCroy Scaler 2551 (100 MHz); Logic Unit CAEN; Discriminator CAEN; Dual Gate Generator LeCroy 2323A; DAC CAEN

HV1=1075V HV2=1125V; HV3=1250V; Limiares: L=-22mV; TC=300ns ms CK S1 S2 S3 D12 D13 D23 TRI 2016 08 30 00 00 00 039 1472515200039 M 2016 08 29 23 56 1 2016 08 29 20 50 941 23.1 48.8 0.0 23.9 135 0.0 01 1472515201125 4996 2136 2174 2372 1860 1911 1924 1813 1472515202170 4996 2024 2055 2263 1727 1768 1817 1682 1472515203215 4996 2143 2199 2404 1882 1902 1965 1830

Precise (0.02sec) gate for the 1 sec time interval of the counts, future GLE detection?

Atmosferic date every 10 minutes

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TANCA muon count efficiency

Vertical muon (VM) 𝜗 = 𝑊𝑁 + 𝑢𝑏𝑜𝑙 𝑊𝑁

8 threshold = -30 mV

(95.7 ± 0.8) % Pulse amplitude histogram Two small, 40x38cm2, plastic scintillators used to select vertical muons Trigger: an other PMT with a threshold of 15mV The three PMTs calibrated to have the same gain

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Barometric coefficient

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𝑒𝑂 𝑂 = − 𝛾 𝑒𝑄 ln 𝑂 𝑂0 = − 𝛾 𝑄 − 𝑄0 𝛾 = (0.108 ± 0.06)%/𝑛𝑐𝑏𝑠 The flux of muons depends on the barometric pressure and this correlation can be approximated with an exponential behavior 𝐽 = 𝐽0 𝑓−𝛾(𝑄−𝑄0) The Forbush analyses are done with data corrected by the barometric coefficient.

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Five CMEs detected by SOHO/LASCO. WSA-Enlil simulation of the three first CMEs.

CME list: https://cdaw.gsfc.nasa.gov/CME_list/UNIVERSAL/2015_06/univ2015_06.html CME score board: NASA GSFC Community Coordinated Modeling Center (CCMC), https://kauai.ccmc.gsfc.nasa.gov/CMEscoreboard/

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Toward the Earth

TANCA registered a Forbush decrease June 2015 Coronal Mass Ejections

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Dst, Kp and TANCA during Forbush event

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The dashed vertical lines shows the CMEs arrivel time on Earth. The CMs and its magnetic interactions generated a strong geomagnetic storm Kp=8 Kp=6 Dst=-204nT The Dst index correlates well with the TANCA variations in muon counts.

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Forbush detection by TANCA, McMurdo and Auger Scaler Mode

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The Auger Scaler Mode (single particle technique) is 15 minutes time averaged data from the Pierre Auger Observatory surface detectors. It is placed at Malargue, Argentina The McMurdo neutron monitor is located at the Southh Pole and has a very low geomagnetic cut-off. McMurdo and Auger Scaler Mode correlate well with the TANCA result.

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Summary

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  • The TANCA detector is installed, calibrated and now is

taking data continuously

  • The TANCA is detecting Forbush decreases and a new

step will be analyzing these events together with

  • thers LAGO detectors
  • The TANCA detector is ready to detect a future muon

short –term GLE

  • LAGO collaboration is helping a regional integration in

Latin America

  • Using this WCD Brazilian students are learning about

muon decay, detector physics and interaction of radiation with matter

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Thank you for your attention

Anderson Fauth fauth@g.unicamp.br

We acknowledge the Pierre Auger Observatory, the University of Delaware and the Kyoto University for their open data policy making their data freely available through their web sites

This work is supported by FAPESP, CNPq and Unicamp.

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Extra slides

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LAGO sites

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