Astrophysics and Cosmology Prof Ian DellAntonio Prof. Ian Dell - - PowerPoint PPT Presentation

Astrophysics and Cosmology

Prof Ian Dell’Antonio Prof Rick Gaitskell Prof Greg Tucker Prof Savvas Koushiappas

• Prof. Ian Dell Antonio
• Prof. Rick Gaitskell
• Prof. Greg Tucker
• Prof. Savvas Koushiappas

Observational Cosmology Gravitational Lensing Astro‐particle Physics Dark Matter searches Theoretical Cosmology/Astrophysics Observational Cosmology From Cosmic Microwave Background to Star Formation

Observational Cosmology and Gravitational Lensing Group

• Prof. Ian Dell’Antonio

Currently: Dell’Antonio, 4 graduate students, 4 undergraduate students undergraduate students Close collaboration with groups at Yale, Harvard and UC Davis Former members: Gillian Wilson (associate Professor, UCRiverside) Jeff Kubo (postdoc Fermilab)

Paul Huwe Richard Cook Van Dao Ryan Michney

Jeff Kubo (postdoc, Fermilab) Hossein Khiabanian (postdoc, Columbia) Wessyl Kelly (postdoc/technician, Pitt)

y y

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 How we achieve this goal: Using optical, X‐ray and Infrared observations of galaxies and clusters

• f galaxies. We aim to measure the growth of clustering and the evolution of galaxies within that

clustering.

Example Graduate Student Project: The evolution of the cluster mass function using

• rthogonal transfer arrays

New technology—the One Degree Imager at the WIYN telescope in 2012.

• rthogonal 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. p g The increase in sensitivity will allow more clusters to be detected: best constraint on Dark Energy

xies per sq. arcmin Seeing

A parallel effort will use DECam

Exposure time

Number of gala

A parallel effort will use DECam (installed early 2012) to measure a larger area but in less detail.

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 LSST camera 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
• f WIMPs orbit

h f h the center of the galaxy

• 50 billion

h h through 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) Spokesperson) 2011‐2013 LZS 2011 2013 LZS 3 tonne LXe 2013‐2020 LZD 20 tonne LXe Dark Matter, Double Beta Decay and Solar Neutrinos

8

and Solar Neutrinos

The LUX Experiment

Thermosyphon Titanium Vessels PMT Holder Copper Plates Dodecagonal field cage g g + PTFE reflector panels

• 350 kg LXe detector
• 8m x 6m water shield

2’’ Hamamatsu R8778

• 8m x 6m water shield
• 1 mile underground
• 122 PMTs (2’’ round)
• Low-background Ti cryostat

2 Hamamatsu R8778 Photomultiplier Tubes (PMTs)

• bac g ou d

c yostat

• PTFE reflector cage
• Thermosyphon used for cooling (>1 kW)

Richard Gaitskell PI, Professor Simon Fiorucci Research Associate M i P ili P td

Brown

XENON10, CDMS

Collaboration meeting, Homestake, March 2010 Collaboration meeting, Homestake, March 2010

The LUX Collaboration

Monica Pangilinan Postdoc 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 Tom Coffey Postdoc Karen Gibson Postdoc Adam Bradley Graduate Student , , ,

SD School of Mines Texas A&M

ZEPLIN II

Formed in 2007, fully funded DOE/NSF in 2008

Adam Bradley Graduate Student Patrick Phelps Graduate Student Chang Lee Graduate Student Xinhua Bai Professor Mark Hanardt Undergraduate Student Frank Wolfs Professor Ud Sh d P f James White Professor Robert Webb Professor Rachel Mannino Graduate Student Tyana Stiegler Graduate Student Clement Sofka Graduate Student

SD School of Mines UC Davis

Double Chooz CMS ZEPLIN II

University of Rochester

ZEPLIN II IceCube Isabel Lopes Professor José Pinto da Cunha Assistant Professor Vladimir Solovov Senior Researcher

LIP Coimbra

ZEPLIN III Bob Jacobsen Professor Jim Siegrist Professor

Lawrence Berkeley + UC Berkeley

SNO, KamLAND Udo Shroeder Professor Wojtek Skutski Senior Scientist Jan Toke Senior Scientist Eryk Druszkiewicz Graduate Student Mani Tripathi Professor Robert Svoboda Professor Richard Lander Professor Britt Hollbrook Senior Engineer John Thomson Engineer Matthew Szydagis Postdoc Jeremy Mock Graduate Student M li d S G d t St d t Double Chooz, CMS DongMing Mei Professor

• U. South Dakota

Majorana, CLEAN-DEAP Vladimir Solovov Senior Researcher Luiz de Viveiros Postdoc Alexandre Lindote Postdoc Francisco Neves Postdoc Jim Siegrist Professor Joseph Rasson Engineer Mia ihm Grad Student Adam Bernstein PI, Leader of Adv. Detectors Group Dennis Carr Senior Engineer

Lawrence Livermore

XENON10 Melinda Sweany Graduate Student Nick Walsh Graduate Student Michael Woods Graduate Student Daniel McKinsey Professor Wengchang Xiang Postdoc Chao Zhang Postdoc Jason Spaans Graduate Student Xiaoyi Yang Graduate Student

Yale

XENON10, CLEAN-DEAP Harry Nelson Professor Dean White Engineer

UC Santa Barbara

CDMS Masahiro Morii Professor Michal Wlasenko Postdoc

Harvard

BABAR, ATLAS Kareem Kazkaz Staff Physicist Peter Sorensen Postdoc

University of Maryland

EXO Carter Hall Professor Douglas Leonard Postdoc Daniel McKinsey Professor James Nikkel Research Scientist Sidney Cahn Research Scientist Alexey Lyashenko Postdoc Ethan Bernard Postdoc Louis Kastens Graduate Student Nicole Larsen Graduate Student Dean White Engineer Susanne Kyre Engineer

Observational Cosmology

• Prof. Greg Tucker
• Dr. Andrei Korotkov

Kyle Helson Ata Karakci Former students: Matt Truch (postdoc, UPenn) 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 g (CMB) Far Infrared Background (from the first dust enshrouded galaxies) Inflation

Measuring Polarization of the Cosmic Microwave Background (CMB)

CMB l i ti b th i 10 35 ft th Bi B (th CMB polarization probes the universe 10‐35 s after the Big Bang (the epoch of inflation).

QUBIC – QU Bolometric Interferometer for The Millimeter‐wave Bolometric Cosmology will be installed at Dome C (~2013) Interferometer (MBI) MBI is a prototype to demonstrate the BI technique. Projects involve designing and building QUBIC, simulating performance and analyzing data

The E and B Experiment (EBEX) Another way to search for CMB polarization 1000 ft 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 E b i thi i Every bump in this map is a galaxy

GOODS‐S Chandra 2 Ms

Reradiated Starlight Direct Starlight

Chandra/VLA/FIDEL/LABOCA BGS‐Deep ECDF‐S Spitzer SWIRE

How do stars form? The collapse time from a gas cloud What BLAST is doing now (from the Antarctic in December 2010) p g 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 BLAST map Optical map This ~10 K cloud is the future birthplace of stars http://blastexperiment.info p

Theoretical Astrophysics/Cosmology

• Prof. Savvas Koushiappas
• Dr. Jacqueline Chen

Alex Geringer-Sameth Andrew Favaloro http://www.physics.brown.edu/BTAC/Home.html

Theoretical Astrophysics/Cosmology

What we do: Develop methods that help us understand the distribution of dark matter in the Universe - structure formation http://www.physics.brown.edu/BTAC/Home.html

Theoretical Astrophysics/Cosmology

What we do: Develop methods that help us understand the distribution of dark matter in the Why we do it: Dark matter detection (direct, indirect) is ultimately linked to the understanding of hierarchical structure formation - the growth of primordial perturbations Universe - structure formation g p p http://www.physics.brown.edu/BTAC/Home.html

Theoretical Astrophysics/Cosmology

What we do: Develop methods that help us understand the distribution of dark matter in the Why we do it: Dark matter detection (direct, indirect) is ultimately linked to the understanding of hierarchical structure formation - the growth of primordial perturbations Universe - structure formation g p p How we do it: We use analytical, numerical and semi-analytical techniques http://www.physics.brown.edu/BTAC/Home.html

Theoretical Astrophysics/Cosmology

Example: Develop new statistical tools for the extraction of a time-dependent spatial signal in an

• therwise diffuse unresolved background

FGST http://www.physics.brown.edu/BTAC/Home.html

Alex Geringer-Sameth & Koushiappas arXiv:1012.1873

Theoretical Astrophysics/Cosmology

Future Directions: Develop a framework where cosmological predictions can be used to interpret data from dark matter experiments

Physics approach to the problem: Physics approach to the problem: 1) Data from different experimental techniques 2) Sophisticated theory and modelling 3) High-performance computing simulations 4) New and existing statistical and analysis tools

http://www.physics.brown.edu/BTAC/Home.html