Astrophysics and Cosmology - Brown University · Richard Gaitskell PI, Professor Simon Fiorucci...
Transcript of Astrophysics and Cosmology - Brown University · Richard Gaitskell PI, Professor Simon Fiorucci...
Astrophysics and Cosmology
Prof Ian Dell’Antonio Prof Rick Gaitskell Prof Greg Tucker Prof Savvas KoushiappasProf. Ian Dell Antonio Prof. Rick Gaitskell Prof. Greg Tucker Prof. Savvas KoushiappasObservational Cosmology Gravitational Lensing
Astro‐particle Physics Dark Matter searches
Theoretical Cosmology/AstrophysicsObservational CosmologyFrom Cosmic Microwave Backgroundto Star Formation
Observational Cosmology and Gravitational Lensing Group
Prof. Ian Dell’Antonio
Currently: Dell’Antonio, 4 graduate students, 4 undergraduate studentsundergraduate 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 CookVan Dao Ryan Michney
Jeff Kubo (postdoc, Fermilab)Hossein Khiabanian (postdoc, Columbia)Wessyl Kelly (postdoc/technician, Pitt)
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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 clustersHow 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.
Example Graduate Student Project: The evolution of the cluster mass function using orthogonal transfer arrays
New technology—the One Degree Imager at the WIYN telescope in 2012.
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.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 timeNum
ber o
f galaA 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 of WIMPs orbit h f hthe center of the galaxy
• 50 billion h hthrough a person each second
• Occasionally collides with an atom in normal matter 1/kg/month ‐>1/tonne/decade
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LUX Experiment/LZ/Sanford Lab2009‐2011 LUX350 kg LXe (Gaitskell is DOE Spokesperson)Spokesperson)
2011‐2013 LZS2011 2013 LZS3 tonne LXe
2013‐2020 LZD20 tonne LXe
Dark Matter, Double Beta Decay and Solar Neutrinos
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and Solar Neutrinos
The LUX ExperimentThermosyphon
Titanium Vessels
PMT Holder Copper Plates
Dodecagonal field cageg 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)o bac g ou d c yostat
• PTFE reflector cage• Thermosyphon used for cooling (>1 kW)
Richard Gaitskell PI, ProfessorSimon Fiorucci Research AssociateM i P ili P td
Brown XENON10, CDMSCollaboration meeting, Homestake, March 2010Collaboration meeting, Homestake, March 2010
The LUX CollaborationMonica Pangilinan PostdocJeremy Chapman Graduate StudentCarlos Hernandez Faham Graduate StudentDavid Malling Graduate StudentJames Verbus Graduate Student
Case Western SNO, Borexino, XENON10, CDMSThomas Shutt PI, ProfessorDan Akerib ProfessorMike Dragowsky Research Associate ProfessorCarmen Carmona PostdocKen Clark PostdocTom Coffey PostdocKaren Gibson PostdocAdam Bradley Graduate Student
, , ,
SD School of MinesTexas A&MZEPLIN II
Formed in 2007, fully funded DOE/NSF in 2008
Adam Bradley Graduate StudentPatrick Phelps Graduate StudentChang Lee Graduate Student Xinhua Bai Professor
Mark Hanardt Undergraduate Student
Frank Wolfs ProfessorUd Sh d P f
James White ProfessorRobert Webb ProfessorRachel Mannino Graduate StudentTyana Stiegler Graduate StudentClement Sofka Graduate Student
SD School of Mines
UC Davis Double Chooz CMS
ZEPLIN II
University of RochesterZEPLIN II
IceCube
Isabel Lopes ProfessorJosé Pinto da Cunha Assistant ProfessorVladimir Solovov Senior Researcher
LIP Coimbra ZEPLIN III
Bob Jacobsen ProfessorJim Siegrist Professor
Lawrence Berkeley + UC BerkeleySNO, KamLAND
Udo Shroeder ProfessorWojtek Skutski Senior ScientistJan Toke Senior ScientistEryk Druszkiewicz Graduate Student
Mani Tripathi ProfessorRobert Svoboda ProfessorRichard Lander ProfessorBritt Hollbrook Senior EngineerJohn Thomson EngineerMatthew Szydagis PostdocJeremy Mock Graduate StudentM li d S G d t St d t
Double Chooz, CMS
DongMing Mei Professor
U. South Dakota Majorana, CLEAN-DEAP
Vladimir Solovov Senior ResearcherLuiz de Viveiros PostdocAlexandre Lindote PostdocFrancisco Neves Postdoc
Jim Siegrist ProfessorJoseph Rasson EngineerMia ihm Grad Student
Adam Bernstein PI, Leader of Adv. Detectors GroupDennis Carr Senior Engineer
Lawrence Livermore XENON10
Melinda Sweany Graduate StudentNick Walsh Graduate StudentMichael Woods Graduate Student
Daniel McKinsey Professor
Wengchang Xiang PostdocChao Zhang PostdocJason Spaans Graduate StudentXiaoyi Yang Graduate Student
Yale XENON10, CLEAN-DEAPHarry Nelson ProfessorDean White Engineer
UC Santa BarbaraCDMS
Masahiro Morii ProfessorMichal Wlasenko Postdoc
Harvard BABAR, ATLAS
Kareem Kazkaz Staff PhysicistPeter Sorensen Postdoc
University of Maryland EXOCarter Hall ProfessorDouglas Leonard Postdoc
Daniel McKinsey ProfessorJames Nikkel Research ScientistSidney Cahn Research ScientistAlexey Lyashenko PostdocEthan Bernard PostdocLouis Kastens Graduate StudentNicole Larsen Graduate Student
Dean White EngineerSusanne 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 Backgroundg(CMB)
Far Infrared Background(from the first dust enshrouded galaxies) Inflation
Measuring Polarization of theCosmic Microwave Background (CMB)
CMB l i ti b th i 10 35 ft th Bi B (thCMB 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 MexicoJune 2009 Projects include data pipeline
development and analysis
What BLAST has done: Resolved the far infrared background (re-radiated starlight) into individual galaxies
E b i thi iEvery bump in this map is a galaxy
GOODS‐SChandra 2 Ms
ReradiatedStarlight
DirectStarlight
Chandra/VLA/FIDEL/LABOCABGS‐DeepECDF‐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 gis 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.
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A star forming region in Vela
BLAST mapOptical map
This ~10 K cloud is the future birthplace of stars
http://blastexperiment.info
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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 otherwise 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 predictionscan be used to interpret data from dark matter experiments
Physics approach to the problem:Physics approach to the problem:1) Data from different experimental techniques2) Sophisticated theory and modelling3) High-performance computing simulations 4) New and existing statistical and analysis tools
http://www.physics.brown.edu/BTAC/Home.html