BibTex format
@inproceedings{Abarr:2025:10.22323/1.501.0976,
author = {Abarr, Q and Allison, P and Alvarez-Muñiz, J and Yebra, JA and Anderson, T and Basharina-Freshville, A and Beatty, JJ and Beaufore, L and Besson, DZ and Bose, R and Braun, D and Chamanbahar, B and Chen, P and Chen, Y and Clem, JM and Coakley, T and Connolly, A and Cremonesi, L and Cummings, A and Dasgupta, P and Deaconu, C and Flaherty, J and Gorham, PW and Hornhuber, C and Hoffman, J and Hughes, K and Hynous, A and Jung, A and Kofman, A and Ku, Y and Kuo, CY and Linton, P and Lisalda, L and Liu, TC and Luszczak, W and Mackey, SC and Martin, Z and McBride, K and Miki, C and Nam, J and Nichol, RJ and Novikov, A and Nozdrina, A and Oberla, E and Prohira, S and Pumphrey, H and Radomski, D and Rauch, BF and Scrandis, R and Seckel, D and Seikh, MFH and Shiao, J and Simburger, G and Vieregg, AG and Wang, SH and Welling, C and Wissel, SA and Xie, C and Yao, J and Young, R and Zas, E and Zeolla, A},
doi = {10.22323/1.501.0976},
title = {Searching for Ultrahigh Energy Neutrinos with PUEO},
url = {http://dx.doi.org/10.22323/1.501.0976},
year = {2025}
}
RIS format (EndNote, RefMan)
TY - CPAPER
AB - PUEO, the Payload for Ultrahigh Energy Observations, is a long duration balloon-borne experiment with the primary science goal of detecting the impulsive Askaryan emission from ultrahigh energy (UHE, >1 EeV) neutrinos interacting in the ice sheet of Antarctica. The ultrahigh energy neutrino flux is yet to be detected, and so a successful measurement by PUEO will give us information about the where and how these neutrinos are produced; this may be through a process called the GZK effect when ultrahigh energy cosmic rays interact with the cosmic microwave background, or it may be directly within the environment of cosmic ray accelerators. In order to detect radio Askaryan emission, PUEO consists of a broadband interferometric radio detector of 96 antennas which point down at the ice. Additionally, it has a drop-down low-frequency subsystem which will deploy after launch. This improves PUEO’s ability to detect tau neutrinos and charged cosmic rays, which can both produce geomagnetic air shower emission. This contribution will outline PUEO’s science case, present its expected sensitivity, and share status updates from our preparation to launch PUEO from McMurdo Station, Antarctica in December 2025.
AU - Abarr,Q
AU - Allison,P
AU - Alvarez-Muñiz,J
AU - Yebra,JA
AU - Anderson,T
AU - Basharina-Freshville,A
AU - Beatty,JJ
AU - Beaufore,L
AU - Besson,DZ
AU - Bose,R
AU - Braun,D
AU - Chamanbahar,B
AU - Chen,P
AU - Chen,Y
AU - Clem,JM
AU - Coakley,T
AU - Connolly,A
AU - Cremonesi,L
AU - Cummings,A
AU - Dasgupta,P
AU - Deaconu,C
AU - Flaherty,J
AU - Gorham,PW
AU - Hornhuber,C
AU - Hoffman,J
AU - Hughes,K
AU - Hynous,A
AU - Jung,A
AU - Kofman,A
AU - Ku,Y
AU - Kuo,CY
AU - Linton,P
AU - Lisalda,L
AU - Liu,TC
AU - Luszczak,W
AU - Mackey,SC
AU - Martin,Z
AU - McBride,K
AU - Miki,C
AU - Nam,J
AU - Nichol,RJ
AU - Novikov,A
AU - Nozdrina,A
AU - Oberla,E
AU - Prohira,S
AU - Pumphrey,H
AU - Radomski,D
AU - Rauch,BF
AU - Scrandis,R
AU - Seckel,D
AU - Seikh,MFH
AU - Shiao,J
AU - Simburger,G
AU - Vieregg,AG
AU - Wang,SH
AU - Welling,C
AU - Wissel,SA
AU - Xie,C
AU - Yao,J
AU - Young,R
AU - Zas,E
AU - Zeolla,A
DO - 10.22323/1.501.0976
PY - 2025///
TI - Searching for Ultrahigh Energy Neutrinos with PUEO
UR - http://dx.doi.org/10.22323/1.501.0976
ER -