Workshops & Events, 2013
Supernova Hub hosts the JLA (SDSS+SNLS) collaboration meeting
May 15 - 17, 2013 | Chicago, IL
The Supernava Hub at the KICP will host a joint meeting of the SDSS+SNLS (JLA) collaboration which takes place May 15-17 2013 at the University of Chicago. The meetings will start Wed morning at the Temporary Astronomy & Astrophysics Center(TAAC). The Wednesday talks are each 30 minutes to include plenty of time for discussion. The Thursday & Friday discussions can include short presentations as needed. Note that there will be no food at the meeting locations.

Wednsday May 15 (TAAC 67, all day)
1. 09:45 am: introduction/welcome
2. 10:00 am: overview of cosmology analysis (Marc)
3. 10:30 am: General PS1 updates (Sclonic)
4. 11:00 am: Break
5. 11:30 am: calibration summary (Marc)
6. noon - 2pm: lunch
7. 2:00 pm: training systematics (Jennifer)
8. 2:30 pm: intrinsic scatter (Rick)
9. 3:00 pm: sources of intrinsic scatter (Scolnic/PS1)
10. 3:30 pm: break
11. 4:00 pm: add SDSS into the training (Rahul)
12. 4:30 pm: SDSS data release update (Masao)

Thursday May 16 (TAAC 67 from 9am to 1pm, LASR East from 2-5pm)
1. Finish talk(s) from Monday
2. discussion of papers in prep (includes short presentations)
3. u band anomaly
4. simulated mu bias
5. host properties
6. selection requirements
7pm: dinner in South Loop
9:30pm: Buddy Guy's Legends

Friday May 17 (TAAC 67 from 9-1pm, BSLC rm 240 from 1-5pm)
1. future strategies for final cosmology results
2. results with photometric sample
3. extension of the SALT training sample + SN database : Patrick
4. project of SALT training vs host galaxy properties : Nicolas

First Annual GMT Community Science Meeting: "Cosmology in the Era of Extremely Large Telescopes"
June 10 - 12, 2013 | University of Chicago's Gleacher Center, Chicago, IL

The Kavli Institute for Cosmological Physics (KICP) at the University of Chicago and GMTO are planning a joint workshop to be held in Chicago on June 10-12, 2013. The goal of the conference is to examine the role of galaxies as probes of cosmology, both today and in the future as large galaxy surveys and the next generation of large telescopes, in space and on the ground, come into being. We will bring together theorists and observers to discuss contemporary problems in cosmology and galaxy evolution as well as the opportunities offered by a new generation of facilities and surveys.

The conference will be organized into five half-day sessions. Keynote speakers will provide an overview of the state of theory and observation in each subfield. Contributed lectures will delve into the details of front-line research issues. The first session will review relevant surveys and facilities, including the GMT, large imaging surveys such as the Dark Energy Survey, LSST, and Euclid among others, and upcoming missions, such as the James Webb Space Telescope. This will be followed by sessions on First-Light and Reionization of the Universe, Galaxy Formation and Assembly, Intergalactic and Circumgalactic Gas, and Galaxies & the Intergalactic medium as probes of Dark Matter and Dark Energy. The conference will be held in downtown Chicago at the University of Chicago's Gleacher Center. A gala conference banquet will be held at the Adler Planetarium looking out on to Lake Michigan.

Yeunjin Kim: "The effect of the nuclear burning during the deflagration on the final observables in Supernovae type Ia"
July 15, 2013 | TAAC 67
PhD Committee members: Don Lamb, Joshua Frieman, Fausto Cattaneo

Thesis Abstract: A common model of the explosion mechanism of type Ia supernovae is based on a delayed detonation of a white dwarf (WD) in which deflagration precedes detonation. We study one of the delayed detonation models, Gravitationally Confined Detonation (GCD), in two-dimensional simulations, and we discuss a range of the final theoretical observables that can plausibly account for the variety of observed events. Furthermore, we probe the pulsational character of the WD due to the deflagration and its effect on the final observables in one-dimensional studies.

Two-dimensional GCD models with different ignition conditions, parametrized by the number of ignition bubbles and their locations relative to the center of the WD, were performed. The initial ignition led to the development of the subsonic burning flame which in turn generated nuclear burning energy from C and O burning. Depending on the unique initial condition, different amount of nuclear burning energy was released during the deflagration, and at large the star detonated as either a Classical GCD or a Pulsationally-assisted GCD. Furthermore, we have shown a correlation between the amount of nuclear burning that occurs during the deflagration phase and the final abundances of intermediate mass elements such as Si-group. Lastly, the distribution of the ejecta during the homologous phase was studied for each model.

In addition, we create simplified one-dimensional models that test mainly the effects of the pre-detonation stellar internal velocity profile and the post-detonation velocity of expansion on the production of alpha-particle nuclei, including 56Ni. We observe two distinct post-detonation expansion phases: rarefaction and bulk expansion. Almost all the burning to 56Ni occurs only in the rarefaction phase, and its expansion timescale is influenced by pre-existing flow structure in the star, in particular by the pre-detonation stellar velocity profile. We find that the mass fractions of the alpha-particle nuclei, including 56Ni, are tight functions of the empirical physical parameter den_up/v_down, where den_up is the mass density immediately upstream of the detonation wave front and v_down is the velocity of the flow immediately downstream of the detonation wave front. We conclude that the properties of the pre-existing flow, in particular the internal stellar velocity profile, influence the final isotopic composition of burned matter produced by the detonation.

DESSN workshop
July 15 - 19, 2013 | Chicago, IL
The KICP at the University of Chicago will host a week-long workshop dedicated to the Supernova program within the Dark Energy Survey (DES). Since the first DES season starts in September 2013, this workshop will be the final gathering of collaboration-wide expertise to prepare the SN-search software pipelines that run at both NCSA and at Fermilab. While the first three days of the workshop (Mon-Wed) are focussed on the search pipelines, the latter three days (Wed-Fri) will be dedicated to ramping up the analysis, with a focus on cross-cutting tasks that are needed in many analyses. Cross-cutting tasks include final photometry, simulations, measuring the search efficiency, SN-host matching and photometric classification of light curves.