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I Taboada / Ga Tech 2nd Low Energy Workshop
Transient Source Searches with DeepCore
Ignacio Taboada Georgia Ins?tute of Technology
I Taboada / Ga Tech 2nd Low Energy Workshop
Neutrino Transients
GRB, AGNs, SGRs, … Decoupled neutrons in GRB Jets: 1-100 GeV
Choked GRBs / jets inside core-collapse SNe Typical energy: 10 GeV – 10 TeV High event rates for nearby SNe
I Taboada / Ga Tech 2nd Low Energy Workshop
Neutrino Transients
GRB, AGNs, SGRs, … Decoupled neutrons in GRB Jets: 1-100 GeV
Choked GRBs / jets inside core-collapse SNe Typical energy: 10 GeV – 10 TeV High event rates for nearby SNe
Taboada I. Phys. Rev. D 81, 083011 (2010)
I Taboada / Ga Tech 2nd Low Energy Workshop
Choked Jets in Core Collapse Supernovae
Evidence for choked jets / anisotropy
Correla?on between GRBs and Type Ic Sne: SN 2003dh / GRB 030329 Hjorth et al. Nature (2003)
SN 2008d Mazzali et al. Science (2008); Tanaka et al. ApJ. (2009) SN 2007gr Paragi et al. Nature (2010) SN 2009bb Soderberg et al. Nature (2010)
I Taboada / Ga Tech 2nd Low Energy Workshop
Neutrinos from Choked Jets in CC SNe
Ando & Beacom. Phys.Rev.Le]. (2005)
200 GeV 30 GeV
Razzaque, Mészáros and Waxman, Phys. Rev. Le]. (2004); (2005).
20 TeV 100 GeV
K p
IceCube
SN @ 10 Mpc
I Taboada / Ga Tech 2nd Low Energy Workshop
Neutrino-‐Ma]er interac?ons
ANIS: neutrino simula?on MMC: par?cle dE/dx near the detector
All the caveats men?on in this workshop apply
I Taboada / Ga Tech 2nd Low Energy Workshop
Effec?ve Area Calcula?on
R
H
n Cascade
nm Star?ng
Through going
E > 10 GeV H = 350 m R = 125 m
I Taboada / Ga Tech 2nd Low Energy Workshop
Effec?ve Areas
ne nm
nt
Supernova at 10 Mpc with default Ando & Beacom parameter choice:
11 nm with oscilla?ons 28 nm without oscilla?ons
(Oscilla?ons do not lead to 1:1:1)
IceCube
DeepCore
I Taboada / Ga Tech 2nd Low Energy Workshop
Event rates in Deep Core
ne nm
nt
Supernova at 10 Mpc with default Ando & Beacom parameter choice > 10 GeV: 0.6 ne ; 3.0 nm ; 0.4 nt
(Oscilla?ons included and it’s not 1:1:1)
kaon
I Taboada / Ga Tech 2nd Low Energy Workshop
What can we see?
Jet poin?ng prob. 10 – 20 % (???)
CC SN rate within 10 Mpc 1 – 2/yr
Ando, Beacom, Yuksel PRL (2005) Kistler, et al arXiv:0810.1959
Leo I group is just outside this box (~10.8 Mpc)
I Taboada / Ga Tech 2nd Low Energy Workshop
Supernova Explosion ?me
• Given (well sampled) core collapse SN lightcurves, explosion ?me can be determined to within ~0.5 days. Cowen et al. Astropart.Phys. (2010)
• DeepCore Neutrino rate is 300 / day, and 10 GeV neutrinos direc?on can’t be reconstructed (well enough)
I Taboada / Ga Tech 2nd Low Energy Workshop
IceCube CPU Nothern Hemisphere
Iridium
ROTSE III
SN/GRB
I Taboada / Ga Tech 2nd Low Energy Workshop
Op?cal follow up enhancement
Search for N (≥ 1) “TeV” event (IceCube) and M “10 GeV” events (DeepCore) in coincidence
RN,M = RNa RM
bΩa
2π
N−1 Ωb
2π
M ∆TM+N−1
(N − 1)!M !
I Taboada / Ga Tech 2nd Low Energy Workshop
Accidental rate examples Assume 105 nm/yr in IceCube ; 105 bckg/yr in DeepCore ; no angular resolu?on for DeepCore ; 100 s search window
1 IceCube nm & 2 DeepCore evts: 94 / year
1 IceCube nm & 3 DeepCore evts: 1.4 / year
I Taboada / Ga Tech 2nd Low Energy Workshop
What’s next?
• Calculate event rates using IceCube sovware (Jacob Daughhetee)
• Develop a filter, analyze data, etc: farther ahead
• Determine best search strategy. Example 1 >TeV nm and 1 > 100 GeV nm (4o resolu?on – search out to 17 Mpc)
I Taboada / Ga Tech 2nd Low Energy Workshop
Conclusions, Caveats, Comments
Example SN at 10 Mpc results in 4 DeepCore events.
For CC SNe, DeepCore is sensi?ve to the pion component of the spectrum and IceCube is sensi?ve to the kaon component
Sensi?vity to (at least) 10 Mpc – but probably higher due to fluctua?ons
I assumed 0.2:0.4:0.4 flavor ra?o at Earth, but an energy dependent calcula?on is needed
An IceCube sovware calcula?on is forthcoming
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