Status of the project Status of the project EExtreme xtreme EEnergy nergy EEventsventsarea of area of BariBari

Prof. F. Romano - Politecnico di Bari & INFN Bari

Dott. M. Abbrescia – Ricercatore Università di Bari

Dott.ssa A. Regano - Centro Fermi

Seconda Conferenza dei Progetti del CENTRO FERMI, Roma 19-20 Aprile 2012

Extreme Energy Events - La scienza nelle scuole

Stations coordinated by Bari INFN section

Average distance: 65 km

LC "Cagnazzi" Altamura

IISS “Staffa” – Trinitapoli [II fase]

LS "Scacchi" Bari [II fase]

Construction MRPC 2006Installing telescope: May 2008Acquired first event: 30 May 2008ActivityShifts control of the students and LogbookRemote control and monitoringWeather stationLessons on cosmic raysEEE Conference on the activity: 26 May 2011Data acquired130 days in 2010 155 days in 2011100 days up to April 2012

The telescope is in acquisition!

Altamura

Construction MRPC May 2009Installing telescope: 2011Acquired first event: 5 November 2011

ActivityLogbookRemote control and monitoringWeather stationLessons on cosmic raysMagazine Ipogei06

The telescope is in acquisition!

Trinitapoli

The telescope is in acquisition!

Construction MRPC June 2009Installing telescope: 2011Acquired first event: 1 March

2012

ActivityLogbookRemote control and monitoring Lessons on cosmic rays

Bari

Monitor and control

HV-LV systemDAQ & online analysisRoom controlData transfer

All remotely controlled or almost!

Specifications of telescopes LV system classic trigger electronic card: model Catania-

CERN GPS electronic card: Hytec MRPC plane distance: 60cm Average rate: 38Hz LV system: model Lecce trigger electronic card: model Catania-

CERN GPS electronic card: Hytec MRPC plane distance: 59cm Average rate: 20Hz LV system: model Lecce trigger electronic card: model Bologna GPS electronic card: missing MRPC plane distance: 67cm Average rate: 12Hz

Bari

Trinitapoli

Altamura

Flare recorded by the Solar Dynamics

Observatory (SDO) on the night between

14th and 15th February 2011. 

It is a solar flare, of category X2, followed by an important Coronary Mass Emission (CME)

This kind of flares are constantly monitored since they can have relevant consequences on Earth

Valentine’s Day Solar Flare

Counts of cosmic rays - Altamura telescope

Decrease ForbushThe Valentine’s Day solar flare

as observed by the EEE Altamura telescope

March 2012 Sun activity

Approximate Flare Maximum: 05-03-2012 0410 UT at Flux X 1.1

Approximate Flare Maximum: 07-03-2012 0024 UT at Flux X 5.4

Forbush March 2012

Second solar flare observed by the EEE Altamura telescope

Preliminary!

Weather – Altamura March 2012

Program for the future

Study efficiency of the detectors as a

function of temperature and

pressure

Determining a correction coefficient

It is a known effect on the RPC detector...

Temperature

Pressure

In practice

During the data acquisition the efficiency of the

stations EEE  varies

Vary the frequency of counts μ

The objective is to study how the efficiency varies by comparing it with a small telescope scintillators

ConclusionsThe EEE experiment in the area of Bari:

3 active telescopes EEE

The Altamura telescope acquire data almost continuosly from 3 years

First school to observe two Forbush decrease

In the near future, with 3 telescopes, we want …… to study detector performance under varying weather conditions… look for coincidences in the middle distance… continue the observation of cosmics phenomena

EEE produces physics and …

… the students' enthusiasm