UN ESPERIMENTO CON NEUTRINI DEL TEV PRODOTTI DA LHC - CDS INFN BOLOGNA , 5/6/2019 - INFN ...
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Un esperimento con
neutrini del TeV prodotti da LHC
CdS INFN Bologna , 5/6/2019
!1
!2
X Section of Energetic Neutrinos (XSEN) project
G.M.Dallavalle, G.De Lellis, A. Di Crescenzo, D. Lazic, F.L.Navarria, Z.Szillasi
• http://arxiv.org/abs/1903.06564 “Physics Potential of an Experiment using LHC Neutrinos” March 5, 2019 (subm.
to J. of Phys. G)
• https://edms.cern.ch/ui/file/2022399/1.0/LHC-XSEN-EC-0002-1-0.pdf September 5, 2018
• http://arxiv.org/abs/1804.04413 April 12, 2018
• https://edms.cern.ch/ui/file/1908776/1.0/LHC-XSEN-EC-0001-1-0.pdf March 19, 2018.
LHC IP1 and IP5 are intense sources of 2500
PYTHIA MonteCarlo
neutrinos (all flavours, tau included) 2000 b, c production
GeV
1500
E
—> neutrinos reach TeV energies at large η
neutrino
—> LHC is a unique laboratory for measuring for the first
1000
time the νN Xsections in the 500 GeV - 2 TeV range 500
Favorable site exists with low
0
0 1 2 3 4 5 6 7 8 9 10
neutrino |η|
machine backgrounds F N VN
LHC
—> studied sites Very Near, Near, Far, Very Far
from IP5, IP1 CMS IP
—> VF qualifies as host for a neutrino detector: VF
at junction of the TI18 unused tunnel with LHC
—> TI18 has similar features to TI12 (FASER) at
opposite end of IP1: advantage of LHC ATLAS IP
magnetic bend and of a 30 m layer of rock LHCdN/dE_nu vs eta Noacc
Noacc_ENUvsETANU
GeV Entries 147230
Mean x 6.135
3 Mean y 176.6
10
Std Dev x 0.9412
Std Dev y 247.7
10 2
10
5 6 7 8 9 10
abs_etaCenter for Cosmology and AstroParticle Physics (CCAPP),
The Ohio State University, Columbus, OH 43210, USA
XSEN project !3
3
Department of Physics, The Ohio State University, Columbus, OH 43210, USA
(Dated: January 12, 2019)
Detector: Neutrinos are key to probing the deep structure of matter and the high-energy Universe. Yet, until
—> low mass recently,
(3 tonstheir
max): high energy
interactions had onlyneutrinos
been measured favoured since
at laboratory νΝ up
energies Χsection grows
to about 350 GeV.
:1711.11043v2 [astro-ph.HE] 12 Jan 2019
An opportunity to measure their interactions at higher energies opened up with the detection of
proportionally high-energy
to E neutrinos in IceCube, partially of astrophysical origin. Scattering o↵ matter inside the
—> 2 sectionsEarth
covering η ranges
a↵ects the with
distribution different
of their average
arrival directions energy
— from this, we( extract
0.7, 1.2the TeV )
neutrino-nucleon
—> slightly offcross
the section at energies from 18 TeV to 2 PeV, in four energy bins, in spite of uncertainties in the
beam axis prolongation from IP1 : to favour neutrinos from b,c (5%
neutrino flux. Using six years of public IceCube High-Energy Starting Events, we explicitly show
tau
neutrinos) for the first time that the energy dependence of the cross section above 18 TeV agrees with the
•
NO modifications to TI18 (checked
predicted softer-than-linear dependence,with
andCERN
reaffirm civil engineering)
the absence
p
the cross section rise sharply, up to a center-of-mass energy s ⇡ 1 TeV.
of new physics that would make
—> nuclear emulsions:
• efficient for vertex reconstruction (tau decay) Bustamante M., Connolly A., arXiv:1711.11043, Jan. 12, 2019
•ble,exposure
Introduction.— Neutrino interactions, though fee-
and analysis proved to stand
are important for particle physics and astrophysics. PILOT projection
105 provide precise2 tests
tracks/cm (i.e. of
~30the/fb in TI18) 100 RUN3 projection
1]
They Standard Model [1–3],
•probes
modularof newblocks, easy and
physics [4–6], to install
windows to otherwise
nucleon
veiled regions of the Universe. Yet, at neutrino energies DIS
Experiment: above 350 GeV there had been no measurement of their
interactions. This changed recently when the IceCube
accelerator data
1
>
—> Collaboration found
measurement in that
LHC theRUN3
neutrino-nucleon cross sec-
cm2 GeV
tion from 6.3 to 980 TeV agrees with predictions [7].
• machine
Because therebackgrounds
is no artificial likely
neutrinotobeam
increase
at a TeV
¯
with
and HL-LHC
above, IceCube used atmospheric and astrophysi- 10 1
•
T2K (Fe) 14 GGM-SPS 81
calwith 150 /fb,
neutrinos, 1.5 tons,
the latter can by
discovered record
them upuptotoa 2000
few
38
T2K (CH) 14 GGM-PS 79
PeV [26, 31–38]. Refs. [4, 6, 39–42] showed that, because
HE neutrino interactions, up to 100 ν_tau
IceCube neutrinos interact significantly with matter in-
[10 T2K (C) 13
ArgoNeuT 14
IHEP-ITEP 79
IHEP-JINR 96
—> PILOT RUN
side Earth, in distribution
their 2021 in energy and arrival di-
ArgoNeuT 12 MINOS 10
CC /E
ANL 79 NOMAD 08 astrophysical data
• 0.4 tons,
rection carries25 /fb, 1.2 about
information TeV , ~ 100 HE
neutrino-nucleon ν
cross BEBC 79 NuTeV 06
N
BNL 82 SciBooNE 11
•
sections, which, like IceCube [7], we extract.
characterisation of thethe
However, Ref. [7] extracted background
cross section in a sin-
CCFR 97
CDHS 87
SKAT 79
IC HESE showers 17 (avg. of , ¯ )
• set-up
gle, and tune
wide energy emulsion
bin, so its energy handling
dependence in that 10 2
10 1 1 101 102 103 104 105 106
infrastructure
range andAanalysis
remains untested. significant deviation from the
Neutrino energy E [GeV]
predicted softer-than-linear dependence could signal the
presence of new physics, so we extract the cross sectionPROSSIMI PASSI: PERCORSI IN PARALLELO
Percorso 1 Percorso 2 (solo PILOT) Percorso 3 INFN
• EoI sottoposta a LHCC Chair • EoI sottoposta a LHCC • EoI da sottoporre a
Chair e a LMC Chair Presidente CSN1
• in discussione nella sessione
chiusa di Giugno
• presentazione nella • presentazione? richieste
sessione di Giugno del per PILOT in DOT1
• assegnazione dei referees TREX e discussione
• LoI da sottoporre entro metà • se PILOT approvato,
Luglio (allargare collaborazione, • se green light, apertura sigla? Oppure
garantire le risorse) discussione nella dopo approvazione
sessione di Giugno di LHCC? a Settembre?
LMC e decisione
• discussione coi referee,
presentazione e decisione nella
sessione di Settembre
Percorso 4
• se progetto approvato, TP per la
• Fondi europei?
sessione di Novembre e
decisione
• decisione finale del Research
Board a inizio 2020
!4le ISSUEs
XSEN WBS 2019-2021
XSEN WBS 2019 2019 2019 2020 2020 2020 2020 2021 2021 2021 2021
Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4
OK by cern civil engineering
Experiment design
LOI submission (early,final) to LHCC/LMC
Collaboration setting-up
fund raising
investigate EU funds
Technical Proposal submission (early,final)
CERN green light by ResearchBoard
find emulsion producer
order emulsions for 2021 run
emulsion production
R&D analysis tools
set-up development infrastructure
produce detector support mechanics
install detector
LHC recommissioning and Run3 start
2021 emulsion development (first, second batch)
brick layout Collaborazione in via di formazione
detector depth
emulsion procurement XSEN è un micro-OPERA; la sezione
emulsion development
analysis aveva il Know-how, e le attrezzatureYou can also read
