Astrophysics and Cosmology

Prof. Ian Dell ’ Antonio Prof. Rick Gaitskell Prof. Greg Tucker Prof. Savvas Koushiappas Observational Cosmology Astro‐particle Physics Observational Cosmology Theoretical Cosmology/Astrophysics Gravitational Lensing Dark Matter searches From Cosmic Microwave Background to Star Formation Prof. Ian Dell’Antonio Observational Cosmology and Gravitational Lensing Group

Currently: Dell’Antonio, 4 graduate students, 4 undergraduate students

Close collaboration with groups at Yale, Harvard and UC Davis

Former members: Gillian Wilson (associate Professor, UCRiverside) Jeff Kubo (postdoc, Fermilab) Hossein Khiabanian (postdoc, Columbia) Wessyl Kelly (postdoc/technician, Pitt) Van Dao Paul Huwe Richard Cook Ryan Michney Goal: We want to understand the evolution of matter and energy in the Universe.

How we achieve this goal: Using optical, X‐ray and Infrared observations of galaxies and clusters of galaxies. We aim to measure the growth of clustering and the evolution of galaxies within that clustering. New technology—the One Degree Imager at the Example Graduate Student Project: WIYN telescope in 2012. The evolution of the cluster mass function using orthogonal transfer arrays

The camera/telescope combination will have the best image quality of any ground‐based optical imager. We are leading a program that will use 150 nights of time in 2013‐2015 to map out dark matter clustering.

Seeing The increase in sensitivity will allow more clusters arcmin

sq. to be detected: best constraint on Dark Energy per

A parallel effort will use DECam xies gala

(installed early 2012) to measure a larger area but in Exposure time less detail. Number LSST camera Gravitational lensing as a tool for the study of DARK ENERGY

Beyond ODI and DECam. The 2010 decadal survey highlighted that understanding Dark Energy and its equation of state is one of the critical problems in physics, let alone cosmology. Gravitational lensing is a tool to measure dark energy, and our group is positioned to contribute strongly to this effort.

We are participating in the design and planning for the next generation of missions to be launched in the coming decade, such as WFIRST. We are leading the effort on gravitational lensing by clusters of galaxies for LSST.

Direct Detection Dark Matter (Gaitskell)

• Direct Detection of WIMPs orbit the center of the galaxy • 50 billion thhhrough a person each second • Occasionally collides with an atom in normal matter 1/kg/month ‐> 1/tonne/decade

7 LUX Experiment/LZ/Sanford Lab 2009‐2011 LUX 350 kg LXe (Gaitskell is DOE Spokesperson)

2011‐2013 LZS 3 tonne LXe

2013‐2020 LZD 20 tonne LXe

Dark Matter, Double Beta Decay and Solar Neutrinos

8 The LUX Experiment

Thermosyphon

Titanium Vessels

PMT Holder Copper Plates

Dodecagggonal field cage + PTFE reflector panels

• 350 kg LXe detector • 8m x 6m water shield • 1 mile underground • 122 PMTs (2’’ round) •Low-backg rou nd Ti c ryostat 2’’ Hamamatsu R8778 • PTFE reflector cage Photomultiplier Tubes (PMTs) • Thermosyphon used for cooling (>1 kW) The LUX Collaboration Brown XENON10, CDMS Richard Gaitskell PI, Professor Collaboration meeting, Homestake, March 2010 Simon Fiorucci Research Associate Mon ica Pang ilinan PtdPostdoc Jeremy Chapman Graduate Student Carlos Hernandez Faham Graduate Student David Malling Graduate Student James Verbus Graduate Student

Case Western SNO,,, Borexino, XENON10 , CDMS Thomas Shutt PI, Professor Dan Akerib Professor Mike Dragowsky Research Associate Professor Carmen Carmona Postdoc Ken Clark Postdoc Formed in 2007, fully funded DOE/NSF in 2008 Tom Coffey Postdoc Karen Gibson Postdoc Texas A&M Adam Bradley Graduate Student ZEPLIN II SD School of Mines IceCube Patrick Phelps Graduate Student James White Professor Xinhua Bai Professor Chang Lee Graduate Student Robert Webb Professor Mark Hanardt Undergraduate Student Rachel Mannino Graduate Student LIP Coimbra ZEPLIN III Tyana Stiegler Graduate Student Clement Sofka Graduate Student University of Rochester Isabel Lopes Professor ZEPLIN II José Pinto da Cunha Assistant Professor Frank Wolfs Professor Senior Researcher UC Davis Vladimir Solovov Double Chooz, CMS Udo Shroe der PfProfessor Luiz de Viveiros Postdoc Mani Tripathi Professor Wojtek Skutski Senior Scientist Alexandre Lindote Postdoc Robert Svoboda Professor Jan Toke Senior Scientist Postdoc Francisco Neves Richard Lander Professor Eryk Druszkiewicz Graduate Student Britt Hollbrook Senior Engineer Lawrence Berkeley + UC Berkeley John Thomson Engineer SNO, KamLAND Matthew Szydagis Postdoc U. South Dakota Majorana, CLEAN-DEAP Bob Jacobsen Professor Jeremy Mock Graduate Student DongMing Mei Professor Jim Siegrist Professor MlidMelinda Sweany GdGradua te StdtStudent Wengchang Xiang Postdoc Joseph Rasson Engineer Nick Walsh Graduate Student Chao Zhang Postdoc Mia ihm Grad Student Michael Woods Graduate Student Jason Spaans Graduate Student Xiaoyi Yang Graduate Student Lawrence Livermore XENON10 UC Santa Barbara CDMS Adam Bernstein PI, Leader of Adv. Detectors Group Harry Nelson Professor Yale XENON10, CLEAN-DEAP Dennis Carr Senior Engineer Dean White Engineer Professor Kareem Kazkaz Staff Physicist Daniel McKinsey Susanne Kyre Engineer James Nikkel Research Scientist Peter Sorensen Postdoc Sidney Cahn Research Scientist Alexey Lyashenko Postdoc Harvard BABAR, ATLAS Ethan Bernard Postdoc University of Maryland EXO Masahiro Morii Professor Louis Kastens Graduate Student Carter Hall Professor Michal Wlasenko Postdoc Nicole Larsen Graduate Student Douglas Leonard Postdoc Observational Cosmology

Prof. Greg Tucker

Dr. Andrei Korotkov Kyle Helson Ata Karakci

Former students: Matt Truch (postdoc, UPenn) Jaiseung Kim (postdoc, Niels Bohr Institute, Denmark) Jerry Vinokurov (postdoc, Carnegie Mellon University) A Brief History of the Universe

Power Spectrum of the CMB

Cosmic Microwave Background Far Infrared Background (CMB) (from the first dust enshrouded galaxies) Inflation Measuring Polarization of the Cosmic Microwave Background (CMB)

CMB politilarization probes the universe 10‐35 s after the Big Bang (the epoch of inflation).

The Millimeter‐wave Bolometric QUBIC – QU Bolometric Interferometer for Interferometer (MBI) Cosmology will be installed at Dome C (~2013)

MBI is a prototype to demonstrate the BI technique.

Projects involve designing and building QUBIC, simulating performance and analyzing data Another way to search for CMB polarization The E and B Experiment (EBEX)

Next flight will be long duration from the Antarctic in 2011 1000 ft.

New Mexico June 2009 Projects include data pipeline development and analysis The Balloon‐borne Large Aperture Submillimeter Telescope (BLAST)

Antarctica 2006 What BLAST has done: Resolved the far infrared background (re-radiated starlight) into individual galaxies Every bump in this map is a galaxy

GOODS‐S Chandra 2 Ms Chandra/VLA/FIDEL/LABOCA Reradiated Direct BGS‐Deep Starlight Starlight ECDF‐S Spitzer SWIRE What BLAST is doing now (from the Antarctic in December 2010)

How do stars form? The collapse time from a gas cloud is longer than one would naively expect braking mechanism. Is braking due to magnetic fields or turbulence?⇒ BLAST will answer this by measuring the polarization of dust.

A star forming region in Vela

Optical map BLAST map This ~10 K cloud is the future birthplace of stars

http://blastexperiment.info Theoretical Astrophysics/Cosmology

Prof. Savvas Koushiappas Dr. Jacqueline Chen Alex Geringer-Sameth

Andrew Favaloro