Monday, September 29
Theoretical Astrophysics Seminars – no TAC seminar today
Physics Department Colloquium
Location: UCB, 1 Le Conte Hall – 4:15 p.m.
Speaker: Bill Press (U. of Texas)
Title: “Eight Dimensions is Big Enough: Surprises in the Prisoner’s Dilemma Game”
Tuesday, September 30
Location: UCB – 402 Old Le Conte, 3:40 p.m.
Speaker: Aninda Dey (U. of Texas)
Title: “Field Theory on Gibbons-Hawking Spaces”
Wednesday, October 1
Location: LBNL – 50B-4205 – noon
Particle Theory Seminar
Location: LBNL – 50A-5132, 2:00 p.m.
Speaker: Kiel Howe (Stanford)
Title: “Maximally Natural SUSY and its Natural New Signatures”
String Group Meeting
Location: UCB – 402 Old LeConte, 3:40 p.m.
Location: LBNL, 50-5026, 3:30 p.m.
Thursday, October 2
Astronomy Lunch – tba
Location: UCB, 2 LeConte Hall, 4:10 p.m.
Speaker: Hannah Jang-Condell (U. of Wyoming)
Title: “Using Young Disks as Laboratories for Studying Planet Formation”
Abstract: Exoplanets have been discovered in orbits as close as 0.05 AU, and as distant as hundreds of AU. Hence, exoplanets are a hot topic, but they are also pretty cool. How do such disparate planetary systems arise? The best way to learn is to directly study planets while they are forming in young circumstellar disks. Gas-rich protoplanetary disks represent early stages of planet formation, when gas giants are still forming, while gas-free debris disks represent later stages of planet formation, when terrestrial planets could still be forming and dynamical interactions shape the system. In this talk, I will discuss some of the signatures of planets forming in disks, and show how the observations of these signatures informs our understanding of where, when, and how planets form.
Physics Research Progress Meeting
Location: LBNL – 50A-5132, 4:00 p.m.
Speaker: Pat McDonald (LBNL)
Title: “The Dark Energy Spectroscopic Instrument”
Friday, October 3
Location: LBNL 50-5026 – 12 p.m.
Speaker: Yin Li, Chicago
Title: “The power spectrum super-sample effect”
Abstract: The impact of density fluctuations with wavelengths larger than a survey must be considered when extracting cosmological information from power spectrum measurements. These modes change the power spectrum in the same way as a change in the cosmological background does. Using a handful of separate universe simulations, we accurately capture this effect in terms of response of the matter power spectrum to a single mode — the mean density fluctuation in the survey volume. The unknown amplitude of this mean density mode contributes to a (typically dominant) error in the matter power spectrum estimators. Alternatively, it can also be simply included in parameter estimation and forecasts by treating the mean density fluctuation as an additional cosmological parameter. Parameter degeneracies arise since the response of the power spectrum to the mean density mode and cosmological parameters share similar properties in changing the growth of structure and dilating the scale of features.
Location: SSL Addition Conference Room (#105) – 3:00 p.m.
Speaker: Claire Poppett, LBNL
Title: “Dark Energy Spectroscopic Instrument: Probing dark energy with optical fibers and 5000 robots”