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

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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