NEW!!! Travel schedule for return trip
Week 1
Tues, May 26 | Wed, May 27 | Thurs, May 28 | Fri, May 29 | Sat, May 30 | |
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8:15 | Breakfast | Breakfast | Breakfast | Breakfast | Breakfast |
9:00 | The Fermi Mission - Julie McEnery | Particle Acceleration - Markos | Dark Matter Searches in the LAT - Andrea pdf | Gamma-ray Generation - Markos | Gamma-ray Detective Work - Reshmi |
10:00 | Radiation Processes - Markos Georganopoulos | The Fermi Large Area Telescope - Andrea Albert pdf | History and Techniques of Imaging Atmospheric Cherenkov Telescopes - Jamie Holder pdf | The Fermi LAT Catalogs - Seth Digel | Astroparticle Physics at the South Pole - Detecting high-energy neutrinos with IceCube - Naoko Neilson |
11:00 | Break | Break | Break | Break | Break |
11:30 | Pulsars - Tyrel Johnson | Student Talks / 1 Slide Summaries | Blazars - the Observational Perspective - Reshmi Mukherjee | ||
12:30 | Lunch | Lunch | Lunch | Lunch | Lunch |
1:30 | The Likelihood Method - Liz Hays Steve's sample code: Instructions for installing the Fermi Virtual Machine Science Tools Intro and Data Exploration (includes VM shared folder setup ) - Elizabeth Ferrara Students choose a source for analysis. | Likelihood Tutorial – Jeremy Perkins Poll students for use of scripted analysis. | Generating LAT XML Models - Elizabeth Ferrara instructions for using make3FGLxml.py script Advanced Likelihood (cover convergence, 3 basic scripting tools, minor update) Data: PDG Statistics review pdf (deltaLL values in Table 38.2 on page 29) | IRFs Tutorial (Tyrel) Useful scripts: Line Analysis with the LAT - Andrea
| 1 Slide Summaries (cont) Advanced Topic: Summed likelihood tutorial, summed likelihood analysis files summedLikeFiles.tgz
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Crab Feast TBD |
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Mon, June 1 | Tues, June 2 | Wed, June 3 | Thurs, June 4 | Fri, June 5 | |
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8:15 | Breakfast | Breakfast | Breakfast | Breakfast | Breakfast |
9:00 | Cosmic Background Radiation - Yoshi Inoue (Lecture notes) | Cosmic Gamma-ray Background - Yoshi | Cosmic Infrared/Optical background - Yoshi | Future MeV - Liz | Final Wrap-up |
10:00 | Diffuse Emission - Seth | Data Analysis with IACTs - Jamie | Overview of HAWC Science - Ignacio Taboada | GRB Theory Observations and Analysis - J. Michael | Project Results and Feedback |
11:00 | Break | Break | Break | Break | Break |
11:30 | Fundamental Physics from High Energy Observations - Julie | Trip to Wallops | GRB Theory and Analysis - J. Michael Burgess | Data Analysis with HAWC - Ignacio | Workshop Close Out |
12:30 | Lunch | Lunch | Lunch | Lunch | Lunch |
1:30 | Advanced Topics: Working groups
| Trip to Wallops |
Advanced Topics | HAWC sensitivity tutorial - Ignacio Effective Area script: EffArea.C Advanced Topics: | |
Virden Hosted BBQ |
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The GCT’s camera for the Cherenkov Telescope Array - Andrea De FrancoToggle Cloak Cloak The Gamma Cherenkov Telescope’s (GCT) camera is a development project involving UK, US, Japanese, French, Australian and Dutch institutes for the dual-mirror Small-Sized Telescopes (SST-2M) of the Cherenkov Telescope Array (CTA). Two GCT camera prototypes are fully funded. The first will be based on multi-anode photomultipliers (MAPMs) and the second on silicon photomultipliers (SiPMs). The camera is designed to record flashes of Cherenkov light lasting from a few to a hundred nanoseconds, with typical RMS image width and length of ~0.2° x 0.1° and has a 9° field of view. The physical camera geometry is dictated by the GCT telescope optics: a curved focal surface with radius of curvature 1 m and diameter 35 cm is required. The first prototype is now assembled and under extensive lab testing and meant to commissioned on field in the third quarter of this year. The SiPM based camera will follow shortly.
TeV pulsed emission from the Crab detected by MAGIC - Daniel GalindoToggle Cloak Cloak How and where pulsars accelerate particles have been long standing questions. The Crab pulsar, hosted inside its nebula, has been a test bench for any proposed pulsar emission scenario. The discovery of a power-law spectral component, above the cutoff measured by the LAT detector, on board of the Fermi satellite, and extending up to 400 GeV, has challenged the consensus view of the high-energy pulsars. The latest results obtained by the MAGIC collaboration, with more than 300 hours of observations, report the most energetic, ever detected, pulsed gamma rays coming from an astrophysical source, namely the Crab pulsar. The energy spectrum of the Crab pulsar extends up to ~2 TeV, connecting smoothly with the spectral points above 10 GeV measured by Fermi- LAT. Above 400 GeV the detected emission mainly comes from the interpulse, showing a pulse peak at a level of 6.5 sigma. The spectra of the two peaks follow two distinct power-law functions. These results imply that such energetic gamma rays are produced via Inverse Compton scattering in the vicinity of the light cylinder radius by an underlying particle population with Lorentz factors higher than 10^6. The exact site of gamma-ray production cannot be unequivocally assigned, given that none of the existing theories can reproduce all aspects of the observed measurements.
X-ray and gamma-ray studies of the supernova remnant (SNR) CTB 37B hosting a young magnetar - Harsha KumarToggle Cloak Cloak The supernova remnant (SNR) CTB 37B, located in a complicated region of CTB 37, is associated with the 3.82 s magnetar CXOU J171405.7-381031. We present a high-resolution study of the remnant using all available Chandra and XMM-Newton observations in order to characterize the spatial and spectral properties of the diffuse emission, to address the debated age of the SNR, as well as to infer the supernova explosion properties. Observations of the CTB 37 complex performed with the H.E.S.S. telescope array revealed HESS J1713-381, the first TeV source coincident with a magnetar. The origin of the TeV emission has been attributed primarily to the SNR shell, although it has been also suggested that the magnetar may contribute to the HESS source. The source has not yet been detected in any previous studies with the Fermi Large Array Telescope (LAT) that has allowed for successful detections of several SNRs in the MeV- GeV energy range. A further investigation using additional Fermi data to date would help reveal any possible gamma ray emission from this region in the GeV regime, as well as shed light on the nature of its multi-wavelength emission.
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Glossary of Fermi and related jargon
Example ipython notebook from Eric Charles' lecture for statistics in astronomy grad course: Guest Lecture of Applications in Astro Statistics id 17506
Things to do and Eat
These are places we've gone in the past for food:
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