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| Mon, June 2 | Tues, June 3 | Wed, June 4 | Thurs, June 5 | Fri, June 6 | |
|---|---|---|---|---|---|
| 8:00 | Breakfast | Breakfast | Breakfast | Breakfast | Breakfast |
| 9:00 | The Galactic Center at TeV Energies - Karl Kosack | Fermi GBM and GBM Burst Catalog - Adam Goldstein | Pulsar Observations - Elizabeth Ferrara | HAWC - Miguel Mostafa (pdf) | Final Wrap-up |
| 10:00 | Pulsars from a Theoretical Perspective - Alice Harding | GRBs in the Fermi LAT - Judy Racusin | Cosmic Rays from an Observational Perspective - Scott Wakely (pdf) | CTA and the Future - Karl Kosack | Project Results and Feedback |
| 11:00 | Break | Break | Break | Break | Break |
| 11:30 | GRBs from a Theoretical Perspective - Chuck Dermer (pdf)(ppt) | Student Talks | Cosmic-rays and Balloon-based Instrumentation - Scott Wakely (pdf) | Workshop Close Out | |
| 12:30 | Lunch | Lunch | Lunch | Lunch | Lunch |
| 1:30 | Multiwavelength Analysis Tutorial - Judy Racusin Hardware Topics - Jamie Holder Advanced Topics
| Free | Advanced Topics | TevCat Tutorial - Scott Wakely Advanced Topics | |
| BBQ |
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Frederic Jaron --- A new gamma-ray feature in LS I +61°303. Abstract
SlidesToggle Cloak Cloak LS I +61°303 is a stellar binary system consisting of a rapidly rotating Be star and a compact object in an eccentric orbit. It presents periodic emission from radio to gamma-rays and is one of a handful of known gamma-ray binaries. The presence of two periodicities in the radio emission sets this source apart from the other gamma-ray binaries. One is the orbital period P1 = 26.4960 +/- 0.0028 days, and the other is a superorbital modulation of the radio outbursts with period Plong = 1667 +/- 8 days. Recently, the long-term modulation has also been found in the Fermi-LAT gamma-ray light curve. We present our latest results. Annika Kreikenbohm --- Multiwavelength observations of the γ-NLS1 galaxy PKS2004-447. Abstract
Toggle Cloak Cloak The five most enigmatic members of the class of narrow-line Seyfert 1 galaxies are objects which exhibit both, bright radio and gamma-ray emission (hereafter γ-NLS1s). This demonstrates the existence of powerful relativistic jets similar to blazars and radio galaxies. But whether γ-NLS1s really define a distinct sub-class of active galaxies is still under debate. As the radio-loudest of all γ-NLS1s, PKS 2004−447 plays a key role in settling this debate. I present results from radio and X-ray observations of PKS 2004-447: the TANAMI VLBI program finds a high brightness-temperature core and a one-sided parsec-scale jet while Swift and XMM-Newton observations reveal a moderately variable unobscured X-ray spectrum, which is dominated by a flat power-law component. Furthermore, the γ-ray properties of PKS2004-447 are briefly reviewed and results are put in context with the other four known γ-NLS1. Xilu Wang --- Gamma Ray Emission From Starburst Galaxies. Abstract
Toggle Cloak Cloak In star-forming galaxies, gamma rays are mainly produced through the collision of high-energy protons in cosmic rays and protons in the interstellar medium (ISM) (i.e. cosmic ray- induced pi0-radiation ). For a "normal" star-forming galaxy like the Milky Way, most cosmic rays escape the Galaxy before such collisions, but in starburst galaxies with dense gas and huge star formation rate, most cosmic rays do suffer these interactions. We construct a "thick-target" model for starburst galaxies, in which cosmic rays are accelerated by supernovae, and escape is neglected. This model gives an upper limit to the gamma-ray emission and tests the calorimetry relation between gamma rays and cosmic rays for starbursts. Only two free parameters are involved in the model: cosmic-ray proton acceleration energy rate from supernova and the proton injection spectral index. We apply the model to five observed starburst galaxies: M82, NGC 253, NGC 1068, NGC 4945 and Circinus, and find the calorimetric relation holds for most of the starbursts, but for Circinus, other gamma-ray sources must be presented to explain for its GeV excess. The pionic gamma-ray emission is calculated from 10 MeV to 10 TeV, which covers the Fermi Gamma-ray Space Telescope (Fermi) energy range.
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