CUORE BOX Trigger thresholds 1. The 2TY dataset of CUORE underwent additional processing for low energy studies Low Energy Analyses with CUORE and a Search for Solar Axions Sensitivity optimizing detector selections Solar axion search • Use an Optimum Trigger (OT) on data processed through an Optimum Filter, a matched filter to optimize the signal to noise ratio • OT triggers are much lower than triggering on the derivative of raw waveforms (DT), enabling low energy searches Samantha Pagan1 on behalf of the CUORE Collaboration (samantha.pagan@yale.edu) CUORE: The Cryogenic Underground Observatory for Rare Events • 988 TeO2 crystal cryogenic calorimeters operated at ~15 mK, which convert deposited energy from particles into heat • Located at Laboratori Nazionali del Gran Sasso • Collected and analyzed over 2 tonne·yrs of TeO2 exposure Low energy analysis methods • 2 tonne·yr dataset of CUORE underwent additional processing for low-energy studies building off of CUORE-0 and CUORE techniques • Te x-rays from calibration data are a tool for optimizing many methods • Study pulse shape and events rate to select the best performing detectors of the array • Greatly increased exposure compared to previous methods x • Specific low-energy variables and event-level cuts developed for: • Multi-site events tagging • Dedicated pulse shape analysis to reject spurious events • Identifying pileup pulses WIMP search References 1Wright Laboratory, Department of Physics, Yale University [1] Lowering the energy threshold of large-mass bolometric detectors: S. Domizio et al. JINST 6 (2011) P02007 [2] Low energy analysis techniques for CUORE: EPJ C (2017) 77: 857 [3] Performance of the low threshold Optimum Trigger on CUORE data: A . Branca et al. Journal of Physics: Conference Series (2020) 1468(1):012118 [4] Search for 14.4 keV solar axions from M1 transition of 57Fe with CUORE crystals: JCAP05 (2013) 007 [2] [1] • Axions and Axion-like Particles (ALPs) are dark matter candidates • Multiple solar axion searches are possible with CUORE • Ongoing search for solar axions produced from an M1 transition of 57Fe in the sun and detected by the axio-electric effect noise power spectrum signal template Optimum Filter Acknowledgments The CUORE Collaboration thanks the directors and staff of the Laboratori Nazionali del Gran Sasso and the technical staff of our laboratories. This work was supported by the Istituto Nazionale di Fisica Nucleare (INFN); the National Science Foundation under Grant Nos. NSF-PHY-0605119, NSF-PHY-0500337, NSF-PHY-0855314, NSF-PHY-0902171, NSF-PHY-0969852, NSF-PHY-1307204, NSF-PHY-1314881, NSF-PHY-1401832, and NSF-PHY-1913374; Yale University, Johns Hopkins University, and University of Pittsburgh. This material is also based upon work supported by the US Department of Energy (DOE) Office of Science under Contract Nos. DE-AC02-05CH11231 and DE-AC52-07NA27344; by the DOE Office of Science, Office of Nuclear Physics under Contract Nos. DE-FG02-08ER41551, DE-FG03-00ER41138, DE- SC0012654, DE-SC0020423, DE-SC0019316; and the NSF Graduate Research Fellowship Program under Grant No. DGE-1752134. This research used resources of the National Energy Research Scientific Computing Center (NERSC). This work makes use of both the DIANA data analysis and APOLLO data acquisition software packages, which were developed by the CUORICINO, CUORE, LUCIFER, and CUPID-0 Collaborations. The authors acknowledge Advanced Research Computing at Virginia Tech for providing computational resources and technical support that have contributed to the results reported within this paper. • Exposures affected by temperature, vibrational controls and time of year • Candidate backgrounds and noise: 210Pb in TeO2 and Cu components, 125mTe, vibrational noise from microseism events • Energy resolution: ~ 2-3 keV FWHM at 30 keV Low energy spectrum for selected channels at 10 keV Preliminary 0 5 10 15 20 25 30 35 40 Analysis Threshold* [keV] 0 20 40 60 80 100 Detectors Selec