Diffuse flux update AWG visioconf m s 26102012

Diffuse flux update AWG visioconf m. s. 26/10/2012 1

• “Accelerate” of the Diffuse flux analysis (16/10/2012) visioconference • Ice. Cube have 'indication' of a signal in the diffuse flux, both in muons and showers. • We should advance our diffuse analyses as much as possible to remain competitive and be able to answer the inevitable question 'what do we see'. • As reported during the meeting, the ANTARES sensitivity improvement is expected to decrease from 5. 3 10^-8 Ge. V cm-2 s-1 sr-1 down to about 2. 5 10^-8 Ge. V (same units) in the mu channel • Analyses on the shower channel started • Care should of course be taken that the usual 'quality control‘ on data is maintained. 2

• • • Different energy estimators for the muon energy R, d. Edx very well documented (Int. memo) Jutta promised a memo on the ANN estimator Simone reported that the R distribution looks strange (see analysis ELOG 684). The problem was caused by how ROOT files were created with the rootwriter project in Sea. Tray Both R and the Fabian's d. Ed. X estimator (ANN? ) inserted in the ant. DST; new production started. At present, the Rb. R v 2. 0, 2. 2 do not contain the new OM acceptance and the latest version of KM 3. A new MC 'test' production for the runs ending with '0' for both neutrinos and muons will be made to see if there are significant differences Jutta-Erlangen will use the ANN estimator, and Bologna people R (or d. Edx) (Fabian-Saclay? ) Sparking OM selection The (ambitious!!!) goal is to have results in time for the ERC/FRB 3 rd dec 3

New plot for diffuse flux limit 4

News • Mail inter-change with IC diffuse flux conveners • ROOT Macro used for the plot (starting from an old Robert Lahmann input) • Update of the IC results 5

Questions • Too many “ice” lines? • Dashed lines below the atmospheric neutrino region? • Include theoretical models? • W&B limits reduced? (see red section in the caption and last page) • Include my MACRO root in public pages? • Public? 6

Caption • • ANTARES upper limit (90% C. L. ) for a E− 2 diffuse high energy muon-neutrino flux ([1], red line), compared with upper limits from other experiments. The MACRO [2], Amanda-II [3], IC 40 [4], IC 56 [5] limits refer to νμ. The Baikal NT 200 [6] and Ice. Cube 40 νx [7] refer to neutrinos of all-flavors, and are divided by 3. For reference, the W&B [8] (with and without evolution) and the MPR for transparent sources [9] limits are also shown. They are divided by two, to take into account neutrino oscillations. The original bounds [8], [9] assumes a local energy generation rate for CRs (assuming protons) of E^2 d. N(E)/d. E = 10^44 erg/Mpc^3 yr. The recent Auger and Hi. Res data show that the assumed rate was a factor 2 to 3 too high. § § § § § [1] J. A. Aguilar et al. , Phys. Lett. B 696 (2011) 16. [2] M. Ambrosio et al. Astrop. Phys. 19 (2003) 1. [3] A. Achterberg et al. Phys. Rev. D 76 (2007) 042008. [4] R. Abbasi et al. , Physical Review D 84 (2011) 082001 [5] G. W. Sullivan , Neutrino 2012 (Nucl. Phys. B, Proc. Supp. XX (2012) xx) [6] A. V. Avrorin et al. Astronomy Letters 35 (2009) 651. [7] ar. Xiv: 1111. 2736 (Search for astrophysical neutrino-induced cascades using Ice. Cube-40) [8] E. Waxman and J. Bahcall. Phys. Rev. D 59 (1998) 023002 -1; J. Bahcall, E. Waxman. Phys. Rev. D 64 (2001) 023002 -1. [9] K. Mannheim, R. J. Protheroe, J. P. Rachen. Phys. Rev. D 63 (2000) 023003. 7

Old Plot 8

Ice. Cube plot (in the Sullivan proc of Neutrino 2012) 9

New normalization factor for W&B http: //arxiv. org/pdf/1101. 1155 v 1. pdf Value assumed in the W&B upper bound 10