Status of the project E xtreme E nergy E vents area of Bari Prof. F. Romano - Politecnico di Bari &...
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Transcript of Status of the project E xtreme E nergy E vents area of Bari Prof. F. Romano - Politecnico di Bari &...
Status of the project Status of the project EExtreme xtreme EEnergy nergy EEventsvents
area 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
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 2008
ActivityShifts control of the students and LogbookRemote control and monitoringWeather stationLessons on cosmic raysEEE Conference on the activity: 26 May 2011
Data acquired130 days in 2010 155 days in 2011100 days up to April 2012
The telescope is in acquisition!
Altamura
Construction MRPC May 2009
Installing telescope: 2011
Acquired 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 2009
Installing telescope: 2011
Acquired first event: 1 March 2012
ActivityLogbookRemote control and monitoring Lessons on cosmic rays
Bari
Monitor and control
HV-LV system
DAQ & online analysis
Room control
Data 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
Program for the future
Study efficiency of the detectors as a
function of temperature and
pressure
Determining a correction coefficient
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 …