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| Tues, May 29 | Wed, May 30 | Thurs, May 31 | Fri, June 1 | Sat, June 2 | |
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| 8:15 | Breakfast | Breakfast | Breakfast | Breakfast | Breakfast |
| 9:00 | Welcome and Introduction (ppt) - Liz | Intro to Fermi LAT - Regina Caputo | Detectors for LAT - Regina | GRB Science - Judy Racusin | Cosmic Rays and Shocks - Pierre Cristofari |
| 10:00 | Intro to the Fermi Mission and Sky - Julie McEnery | Intro to Fermi GBM - Michelle Hui | IACTs - Marcos Santander | Transients with HAWC - Michelle | Shock accel and expansion of SNRs - Pierre |
| 11:00 | Break | Break | Break | Break (Photo!) | Break |
| 11:30 | Air Showers - Pat Harding | HAWC Science - Pat | The Basics of AGN & their High-Energy Emission - Eileen Meyer | Student Talks / 1 Slide Summaries | Calculating and using Upper Limits - Eileen |
| 12:30 | Lunch | Lunch | Lunch | Lunch | Lunch |
| 1:30 | Tour of Fermi Resources Getting Started with Maximum Likelihood Analysis - Pat Harding Getting Started with Fermi: Students choose a source for analysis. | Getting started with Likelihood Analysis in LAT - Jeremy Perkins Quiz tool link: kahoot.it
| Generating LAT XML Models - Elizabeth Ferrara instructions for using make3FGLxml.py script Advanced Likelihood/fermiPy (data.tgz) PDG Statistics review pdf (deltaLL values in Table 38.2 on page 29) | Likelihood Examples/Advanced Topics
Student Projects | Advanced Topics: Upper Limits? Getting started with Burst Analysis Michelle/Judy (Or in 2nd week)
Student Projects
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| 4:45 | End of the Day Tagup | End of the Day Tagup | End of the Day Tagup | End of the Day Tagup | End of the Day Tagup |
| Crab Feast |
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Resonant Shattering Flares (RSFs) are expected to occur during the inspiral phase for some NS- NS and NS-BH mergers. They result from the resonant tidal excitation of the NS crust-core interface mode fracturing the crust and sparking a relativistic pair-photon fireball, emitted seconds before the merger. RSFs are prompt, bright, and isotropic, allowing detection and triggering from well beyond the LIGO-horizon and may be an important source for detectable electromagnetic counterparts to GW mergers. When a GRB is present, they appear as pre-cursors to the main flare, while for off- axis systems they should appear as isolated under-luminous GRBs with extremely short duration. I will discuss the physics and detectable emissions for RSFs compared to other counterparts, as well as afterglow, detection, and triggering strategies. |
Milena Crnogorčević Crnogorčević - "Searching for axion-like particles in core-collapse supernovae using the Fermi-LAT and GBM" - abstract
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