October 5, 2011 | 3:30 PM | BSLC 001 Where will Einstein fail? Insights into Gravity and Dark Energy Niayesh Afshordi, Perimeter Institute/ University of Waterloo
Despite being the most successfully tested theory in physics, there are strong theoretical and observational arguments for why General Relativity should fail. It is not a question of if, but rather a question of where and when! I start by summarizing the pathologies in Einstein's theory of gravity, and then attempt to forecast where we should first observe its failure. My best bets so far are: 1) Cosmological matter-radiation transition, 2) Neutron stars, 3) Astrophysical black holes, and their potential connection to dark energy. What all these scenarios have in common is the violation of Lorentz symmetry, or a revival of "gravitational aether".
October 19, 2011 | 3:30 PM | BSLC 001 Direct dark matter Detection with Liquefied Noble Gases Daniel McKinsey, Yale University
Astrophysical evidence on a variety of distance scales clearly shows that we cannot account for a large fraction of the mass of the universe. This matter is “dark”, not emitting or absorbing any electromagnetic radiation. A compelling explanation for this missing mass is the existence of Weakly Interacting Massive Particles (WIMPs). Detectors that are low in radioactivity and sensitive to small energy depositions can search for the rare nuclear recoil events predicted by WIMP models. In recent years, several new efforts on direct dark matter detection have begun in which the detection material is a liquefied noble gas. Advantages include: large nuclear recoil signals in both scintillation and ionization channels, good scalability to large target masses, effective discrimination against gamma ray backgrounds, easy purification, and reasonable cost. I will review the results from recent experiments, describe some recent R&D, and present the status of two of the new detectors currently under construction, LUX and MiniCLEAN. I will also discuss the possibility of using superfluid helium as a target for relatively light WIMPs.
October 26, 2011 | 3:30 PM | BSLC 001 Equivalence principle and cosmic acceleration Lam Hui, Columbia University
Theories that attempt to explain the observed acceleration of the universe by modifying gravity typically introduces a new long range force, which must be screened on small scales to satisfy solar system tests. I will discuss when and how such screening mechanisms lead to O(1) violations of the equivalence principle. Astronomical tests involving large scale structure, rotation curves and red giants will be discussed.
November 2, 2011 | 3:30 PM | BSLC 001 Measuring Cosmic Acceleration David H. Weinberg, Ohio State University
The discovery of accelerating cosmic expansion has inspired ambitious programs to measure the expansion history and growth of structure with perecent-level precision over a wide range of redshift. These programs include some of the largest cosmological surveys currently underway and some of the highest priority projects recommended by the Astro2010 decadal survey. I will summarize highlights from a nearly completed, book-length review article on "Observational Probes of Cosmic Acceleration" (Weinberg, Mortonson, Eisenstein, Hirata, Riess, Rozo, in prep.). I will pay particular attention to the complementarity of baryon acoustic oscillations (BAO) and supernovae as distance indicators, to the potential of galaxy clusters calibrated by stacked weak lensing as a probe of structure growth, and to the power of a balanced, multi-pronged observational program that combines supernovae, BAO, weak lensing, and additional methods enabled by the same data sets. The dark energy community is now searching for subtle quantitative anomalies that would have profound physical implications, distinguishing among fundamentally different theories of the energy content of the universe, the nature of gravity, and the origin of cosmic acceleration. The road from 5-percent measurements to 1-percent or sub-percent measurements is a challenging one, but we are well equipped for the journey.
September 30, 2011 | 12:00 PM | LASR Conference Room The Search for CMB B-Mode Polarization James Bock, Jet Propulsion Laboratory
Precise CMB temperature and polarization measurements strongly support the theory of inflation, a period of exponential super-luminal expansion in the instant following the big bang. However the physical basis of inflation remains elusive, arising at energy scales beyond the reach of terrestrial particle accelerators. Inflation also generates a background of gravitational waves that imprint a distinct 'B-mode' polarization pattern on the CMB, with an amplitude that depends on inflationary physics. An active competition between a dozen current experiments is well underway to detect or constrain inflationary polarization. We describe a CMB polarization program at the South Pole, progressing from BICEP, with the current best upper limits on inflationary polarization, to the Keck Polarimeter Array, partially deployed in the field, to POLAR, now in development with a large and sensitive bolometric focal plane array. POLAR is also designed to map the yet-undetected polarization signal from gravitational lensing of the background CMB by intervening matter, a new cosmological tool for probing the formation of large-scale structure. Advances in superconducting bolometer arrays with planar antennas are propelling this rapid improvement in capability. We describe recent results, efforts to control systematic errors, and new innovations. This program ultimately has the capability to search to an amplitude of r ~ 0.01, below which it becomes necessary to remove Galactic and CMB lensing polarization foregrounds. These developments inform the scientific and technical case for the Inflation Probe, a future space-borne CMB successor to the ESA Planck satellite.
October 7, 2011 | 12:00 PM | LASR Conference Room Constraining Asymmetric Dark Matter Matthew R Buckley, Fermilab
Asymmetric dark matter takes the coincidence between the baryon and dark matter densities as the basic principle around which to build models. In this talk, I will provide an overview of the asymmetric models currently on the market. I will then discuss experimental constraints which apply to broad classes of these models, and their implications for a successful asymmetric scenario.
October 14, 2011 | 12:00 PM | LASR Conference Room Cosmological Constraints from a Combined Analysis of Clustering and Galaxy-Galaxy Lensing in the SDSS Frank C. van den Bosch, Yale University
In recent years much progress has been made in constraining halo occupation statistics, the statistical description of how galaxies of different properties are distributed over dark matter halos of different mass. This progress is due to (i) a dramatic increase in data in the form of galaxy redshift surveys, and (ii) the development of the Halo Model, which allows for an analytical description of the non-linear dark matter mass distribution in terms of its halo building blocks. After an introduction to the Halo Model, I present the Conditional Luminosity Function, which is a statistical tool to describe the galaxy-dark matter connection, and show how it can be constrained using either galaxy clustering or galaxy-galaxy lensing. Next, I show that a combination of these two data sets allows one to put tight constraints on cosmological parameters, in a manner that is both complementary to and comparative with other probes, such as Baryon Acoustic Oscillations, Cosmic Shear and SuperNovae Ia. Finally I give some brief examples of how halo occupation statistics can be used to further our understanding of galaxy formation and evolution.
October 21, 2011 | 12:00 PM | LASR Conference Room Dark matter microhalos: messengers from the early universe Adrienne L Erickcek, CITA/Perimeter Institute
The abundance of dark matter microhalos depends on the primordial power spectrum and the thermal history of the Universe. First, I will show how an effectively matter-dominated era between the end of inflation and the onset of radiation domination leaves an imprint on the small-scale matter power spectrum. This imprint depends on the origin of dark matter and can trigger the formation of numerous dark matter microhalos during the cosmic dark ages. Second, I will describe how large primordial perturbations on small scales can similarly lead to early-forming microhalos. These microhalos may be detected through their astrometric microlensing signatures, and I will show how a high-precision astrometry survey like Gaia can be used to probe the primordial power spectrum on very small scales.
October 28, 2011 | 12:00 PM | LASR Conference Room A new view of the CMB from the ATACAMA cosmology telescope Sudeep Das, UC Berkeley
Over the coming decade, tiny fluctuations in temperature and polarization of the Cosmic Microwave Background (CMB) will be mapped with unprecedented resolution. The Planck Surveyor, the Atacama Cosmology Telescope (ACT), and the South Pole Telescope (SPT) are already making great advances. In a few years, high resolution polarization experiments, such as PolarBear, ACTPol, and SPTPol will be in full swing. While these new arc-minute resolution observations will continue to help constrain the physics of the early universe and possible deviations from the Standard Model, they will also be unique in a new way - they will allow us to measure the gravitational lensing of the CMB. This lensing is the deflection of CMB photons by intervening large scale structure. CMB lensing will probe the growth of structure over cosmic time, helping constrain the total mass of neutrinos and the behavior of dark energy. In the first part of the talk, I will review the recent progress made with ACT. In the second part, I will discuss the scientific potential of the CMB lensing signal, its first detection, a new way to constrain dark energy, and its prospects for cross-correlation with other datasets. Finally, I will discuss the upcoming polarized counterpart of ACT --- the ACTPol project, which will have greater sensitivity than ACT, and will be a premier CMB lensing experiment. I will describe our plans to extract different flavors of science from the ACTPol data, including the cross-correlations with optical lensing and galaxy surveys, such as SDSS, BOSS, DES and LSST.
November 4, 2011 | 12:00 PM | LASR Conference Room Constraining the Complete Star Formation History of Observable Galaxies from z=0 to z=8 Peter Behroozi, Stanford University
We present a comprehensive approach for deriving the star formation history of the universe self-consistently with a wide array of observations (stellar mass functions, stellar mass clustering, specific star formation rates, and the cosmic star formation rate) and with merger rates from N-body simulations in the context of LCDM cosmology. Our approach explores a wide parameter space of systematic uncertainties, allowing a broader range of possible star formation scenarios at high redshifts; these uncertainties include aspects (e.g., a steeper faint-end slope for the stellar mass function) which help resolve tensions between the cosmic star formation rate and stellar mass functions for LBGs at z>1. We present derived constraints on the star formation rates and histories for galaxies as a function of stellar and halo mass from z=0 to z=8. We show that constraints from observations favor a clear change in the star formation rates of massive galaxies around z=2, consistent with a transition from cold-mode to hot-mode accretion at that redshift and very old stellar populations at the present day. We find, on the other hand, that low-mass galaxies do not have a similar break and that many have star formation histories which have been increasing ever since the galaxies first formed. We also discuss the largest uncertainties on current constraints and the direction that future surveys should take to best increase our understanding. In summary, we provide for the first time a complete, consistent picture of the evolutionary path of galaxies over 96% of the history of the universe, with profound implications for galaxy simulations, semi-analytic models, and our understanding of star formation in the cosmos.
November 11, 2011 | 12:00 PM | LASR Conference Room NuSTAR: Unveiling the Hard X-ray Universe Varun B Bhalerao, Caltech
The Nuclear Spectroscopic Telescope Array (NuSTAR) mission will carry the first focussing Hard X-ray (6-80 keV) telescope into orbit in Feb 2012. Using grazing incidence optics and pixelated CdZnTe detectors, it will offer two orders of magnitude increase in sensitivity and an order of magnitude improvement in angular resolution over any previous instrument working in this energy range. The two-year primary science mission focuses on four key programs: studying the cosmic evolution of black holes, understanding the populations of compact objects and the nature of the central black hole in the Milky Way, constraining the explosion dynamics and nucleosynthesis in supernovae, and probing the nature of particle acceleration in active galactic nuclei. A number of additional observations will be included in the primary mission, and a guest observer program will be proposed for an extended mission to expand the range of scientific targets. I will talk about the instrument capabilities of NuSTAR and discuss the science programs.
November 18, 2011 | 12:00 PM | LASR Conference Room Gravity Waves from Cosmological Phase Transitions John T Giblin, Kenyon College/Case Western
Cosmological phase transitions occurred. I will talk about recent advances in modeling possible phase transitions when these transitions are mediated by scalar fields. I will discuss first- and second-order transitions, at various scales, and show how we can compute the background of stochastic gravitational waves produced during (and after) these transitions.
December 2, 2011 | 12:00 PM | LASR Conference Room WFIRST and Euclid Jason D Rhodes, NASA JPL
The past decade has seen tremendous progress in astronomy that has brought us to the brink of being able to answer two very fundamental questions: What is the Universe made of? Are we alone? The first question can only be answered by trying to understand the mysterious 'dark energy' causing the accelerated expansion of the Universe. This dark energy, the dominant constituent of the Universe, has a number of possible theoretical explanations, ranging from a cosmological constant, to possible modifications to Einstein's General Theory of Relativity. The second question is motivated by the increasing frequency of detections of exoplanets and can be explored by seeking out the frequency of Earth-like planets in the habitable zone of stars similar to the sun. Both of these science goals can be best explored with a space-based wide-field telescope capable of imaging and spectroscopy. Such a platform, operating in optical to near infrared wavelengths would also make great strides in a myriad of ancillary astrophysical areas, including the evolution of galaxies and structures over two thirds of the age of the Universe. The European Space Agency is in the final stages of examining the Euclid mission, which is optimized to study dark matter and dark energy. NASA has begun planning for the Wide Field Infrared Survey Telescope designed to explore dark energy and perform an exoplanet survey. I'll discuss the scientific motivations of both missions and give an overview of the hardware, observing strategy and status of each mission.
December 9, 2011 | 11:00 AM | KPTC 206 Lumps and bumps in the early (and late) universe Mustafa A Amin, Massachusetts Institute of Technology
In this talk I will address the following two (related) questions (1) What does the universe could look like at the end of inflation in the early universe ? (2) What if dark energy undergoes a phase transition in the late universe (similar to the one undergone by the inflaton at the end of inflation)? Both involve understanding some novel nonlinear scalar field dynamics which could also have implications for axionic dark matter. (1) How did inflation end? I will discuss the different scenarios of of the end of inflation, concentrating on a particular (new) scenario: the fragmentation of the inflaton into localized, long-lived excitations of the inflaton field (oscillons), which can end up dominating the energy density of the universe. I will provide conditions for the existence, stability, emergence and domination of oscillons after inflation as well as their theoretical and possible observational consequences. (2) In the second half, I will discuss the observational consequences of the quintessence field rolling to and oscillating near a minimum in its potential, "if" it happens close to the present epoch. The oscillations can lead to a rapid growth of the field fluctuations and the gravitational potential (times scales<< H^(-1)) on subhorizon scales. The gravitational potential power spectrum changes in a scale-dependent manner, however, the dark matter/galaxy power spectrum and the expansion history need not be significantly affected. Such a transition in the quintessence field can be constrained best by Integrated Sachs-Wolfe (ISW) and lensing. Two quoted "signatures" of modified gravity are a scale-dependent growth of the gravitational potential and a difference between the matter power spectrum inferred from measurements of lensing and galaxy clustering. Here, both effects are achieved by a minimally coupled scalar field in general relativity with a canonical kinetic term.
October 20, 2011 | 2:30 PM | LASR Conference Room Bimetric Gravity from Ghost-free Massive Gravity Rachel Rosen, Columbia University
I will review recent developments in massive gravity, including the resolution of the Boulware-Deser ghost problem. I'll then give arguments that the recently proposed ghost-free massive gravity theories can be consistently promoted to bimetric theories of gravity with two dynamical, interacting spin-2 fields. I'll explain why such a promotion is desirable from a theoretical standpoint and how it leads to a greater range of classical solutions.
October 25, 2011 | 2:00 PM | LASR Conference Room Chasing Down Cosmic Acceleration Eric Linder, UC Berkeley / LBNL
Nearly 14 years after discovery of the acceleration of the universe, where does our understanding of the physics stand? I discuss some of the most recent data and what we do - and do not - know about dark energy. For the present, the observed behavior near to Einstein's cosmological constant can result from a wide range of different physics. For the future, I explore an array of promising ideas such as how varieties of gravitational lensing or mapping the three-dimensional galaxy distribution will allow us to test cosmology and gravity.
October 27, 2011 | 10:00 AM | LASR Conference Room Self-Similar Secondary Infall: A Physical Model of Galaxy Halo Formation Philip Zukin, Massachusetts Institute of Technology
N-body simulations have revealed a wealth of information about dark matter halos, but their results are largely empirical. Using analytic means, we attempt to shed light on simulation results by generalizing the self-similar secondary infall model to include tidal torque. Imposing self-similarity allows us to analytically calculate the structure of the the halo in different radial regimes and numerically compute the profiles of the halo without being limited by resolution effects inherent to N-body codes. I will describe this simplified halo formation model and compare our results to mass and velocity profiles from recent N-body simulations. We find that angular momentum plays an important role in determining the structure of the halo at small radii.
October 27, 2011 | 2:00 PM | LASR Conference Room Spatially Covariant Theories of a Transverse, Traceless Graviton Godfrey Miller, University of Pennsylvania
General relativity is a covariant theory of two transverse, traceless graviton degrees of freedom. According to a theorem of Hojman, Kuchar, and Teitelboim, modifications of general relativity must either introduce new degrees of freedom or violate the principle of general covariance. In my talk, I will discuss modifications of general relativity that retain the same number of gravitational degrees of freedom, and therefore explicitly break general covariance. Motivated by cosmology, the modifications of interest maintain spatial covariance. Demanding consistency of the theory forces the physical Hamiltonian density to obey an analogue of the renormalization group equation, which encodes the invariance of the theory under flow through the space of conformally equivalent spatial metrics.
November 17, 2011 | 11:00 AM | LASR Conference Room A Paradise Island for Deformed Gravity Florian Kuhnel, Ludwig-Maximilians-University Munchen, Germany
I will discuss our recently-proposed model (hep-th/1106.3566) of deformations of general relativity that are consistent and potentially phenomenologically viable, since they respect cosmological backgrounds. These deformations have unique symmetries in accordance with unitarity requirements, and give rise to a curvature induced self-stabilizing mechanism. Furthermore, our findings include the possibility of consistent and potentially phenomenologically viable deformations of general relativity that are solely operative on curved spacetime geometries, reducing to Einstein's theory on the Minkowski background. I will also comment on possible phenomenological implications.
November 29, 2011 | 2:00 PM | LASR Conference Room Odd-Parity Bipolar Spherical Harmonics Laura Book, Caltech
Bipolar spherical harmonics (BiPoSHs) provide a general formalism for quantifying departures in the cosmic microwave background (CMB) from statistical isotropy and from Gaussianity. However, prior work has focused only on BiPoSHs with even parity. In this talk I will introduce BiPoSHs and their applicability to the CMB. I will then go on to discuss BiPoSH parity, and the sources that may induce even- and odd-parity BiPoSH modes.
December 1, 2011 | 3:00 PM | LASR Conference Room Nongaussianity in Axion Inflation Neil Barnaby, University of Minnesota
Primordial nongaussianity is generated by interactions of the inflaton field, either self-interactions or couplings to other sectors. The latter class of interactions are generically present and may be required for reheating. However, the impact of these couplings during inflation is often overlooked. In this talk I will show how such interactions provide a natural source of observable nongaussianity, without invoking any exotic ingredients. I will focus on one of the simplest and most well-motivated models: single field inflation with an underlying shift symmetry. In this case, observable nongaussianity is correlated with a detectable tensor-to-scalar ratio and also gravitational waves detectable with interferometers.
September 28, 2011 | 3:30 PM | BSLC 001 (Knapp Bldg.) Infrared Extragalactic Backgrounds Near and Far James Bock, Caltech
The extragalactic background light (EBL) provides an integral measure of the radiation produced by galaxy formation over cosmic history. Precise measurements of the spatial structure of the EBL promise to reveal the formation of galaxies from dark matter over-densities, and tease out signatures from the epoch of reionization. The ESA Herschel Space Observatory, with unprecedented sensitivity and mapping speed, has opened a new window on the far-infrared extragalactic universe. I will discuss recent results from the Hermes/Herschel guaranteed-time extragalactic survey, a large nested far-infrared photometric survey using the SPIRE and PACS instruments. In the near-infrared, the CIBER experiment is conducting a search for the EBL component produced by starlight from the epoch of reionization. CIBER uses a new Fraunhofer line measurement to improve absolute EBL photometry, and a multi-wavelength fluctuations measurement to probe for the reionization component based on spatial power spectra. Finally this is a field with rich potential for future measurements, and I will discuss plans for combining EBL measurements with CMB and 21 cm surveys.
October 12, 2011 | 3:00 PM | BSLC 001 Feedback and Galaxy Formation Norm Murray, CITA
Feedback from young stars plays a critical role in shaping the galaxy mass function, particularly at the low mass end, while feedback from supermassive black holes appears to shape the high mass end, statements supported by both numerical and semi-analytic models of galaxy formation. However, the exact form of the feedback is not certain. I will describe recent work shedding light on this problem. First I will describe three dimensional radiative magnetohydrodynamics calculations of the effects of young stars and supernovae on giant molecular clouds, showing that star formation is rapid, but that feedback halts star formation when ~5-10% of the cloud is turned into stars; supernovae play only a minor role. Next I will describe high resolution (~1 parsec) SPH simulations of star forming galaxies employing momentum feedback from young stars, as well as heating from supernovae, O star winds, and HII regions, showing that all these forms of feedback have a role to play, with different forms of feedback coming to the fore in different galaxies. These simulations naturally produce galactic scale superwinds, with mass loss rates from 1-10 times the star formation rate. Finally, I will briefly describe recent results on quasar feedback, including observational constraints one the launching mechanism of BAL winds, one of the more promising forms of "quasar mode" feedback.
November 9, 2011 | 3:30 PM | BSLC 001 Ultra-Faint Galaxies Around the Milky Way Marla Geha, Yale University
In the past several years, fourteen new satellite galaxies have been discovered around the Milky Way, more than doubling the known population. These "ultra-faint" galaxies have emerged as the least luminous and most dark-matter-dominated galaxies in the known Universe. They are dramatically reshaping our understanding of galaxy formation and may hold the keys to deciphering the nature of dark matter. I will review our current understand of the ultra-faint galaxies, focusing on the constraints these objects provide on dark matter.
November 16, 2011 | 3:30 PM | BSLC 001 Gas Outflow and Inflow in redshift 0.2<z<2 galaxies Crystal Martin, University of California, Santa Barbara
We present new results on the kinematics of metal-enriched gas near galaxies over a period in which star formation activity and gas accretion mechanism are thought to evolve strongly. We focus on constraints provided by near-ultraviolet spectroscopy of star-forming galaxies between redshift 2.0 and 0.4 obtained over a several year period with multislit spectroscopy at Keck. In particular, we investigate the properties of galactic outflows via interstellar absorption lines, resonance emission, and fluorescent emission. We compare the properties of the galaxies that host the outflows to those that do not; and we examine how outflow velocity varies with galactic mass and star formation rate. The most interesting aspect of this analysis, however, may be the discovery of infalling, metal-enriched gas in a small, but significant, fraction of the galaxies. Because the properties of these 'inflow galaxies' appear to be otherwise indistinguishable from the outflow galaxies; it is possible that they mark a ubiquitous phenomemon observed at an optimal orientation. From this more quantitative understanding of how metals circulate in and out of galaxies, we discuss both the escape of metals from galaxies and the mixing of gas ejected by winds with the "cold flows" that characterize cosmological models of galaxy formation.
December 7, 2011 | 3:30 PM | BSLC 001 Damped Lyman alpha Absorption Systems: Neutral Gas Reservoirs for Star Formation in Early Galaxies Arthur M. Wolfe, University California, San Diego
Damped Lyman-alpha absorption systems (DLAs) are gas layers that dominate the neutral-gas content of the Universe in the redshift interval z=[0,5] and serves as neutral-gas reservoirs for star formation in early galaxies. I first discuss results of our recent Keck survey for the DLAs out to z=5. I focus on evolution of metal content of the gas. I emphasize the connection between DLAs and the galactic stellar populations, in particular the galactic halo. I next discuss our recent study of the star formation efficiency of DLA neutral gas. I focus on two independent tests indicating that the efficiency of star formation in DLAs is far below that indicated by the standard Kennicutt-Schmidt (K-S) Law. Finally, I discuss DLA thermodynamics. I emphasize the importance of detecting the principal coolant of neutral gas in DLAs, i.e., the [C II] 158 micron emission line.
October 10, 2011 | 3:00 PM | AAC 123 Accretion, jets and winds: High-energy emission from young stellar objects Hans Moritz Guenther, Harvard-Smithsonian Center for Astrophysics
Young stars form by contraction from large molecular clouds, they accrete mass from their environment. In the stage of classical T Tauri stars (CTTS) they are surrounded by an accretion disk, in which planet formation takes place. At this time, there are three possible mechanisms to power X-ray and UV emission: First, a corona similar to main-sequence stars, second, an accretion shock when infalling matter from the disk hits the star and, third, wind and collimated jets. I will present X-ray and UV observations that tell us about the physical conditions in the emission regions and show that all three mechanisms can be observed, albeit to a different degree in different objects.