KICP Colloquia: 2006
DateTalk TitleSpeaker
Jan 4, 2006Astrophysics and Cosmology with HESSFelix Aharonian, MPI Heidelberg
Jan 11, 2006The tension in Standard Big Bang Nucleosynthesis:the baryon density, D, He and Li.David Tytler, UCSD
Jan 18, 2006Well-posedness of the Cauchy problem of General RelativityVasileios Paschalidis, University of Chicago
Jan 25, 2006Carbon Enhancement in the Galaxy -- A New Probe of the First StarsTimothy Beers, Michigan State University
Feb 1, 2006Searching for EnlightenmentJeff Peterson, CMU
Feb 8, 2006Reflections of AGN Outbursts In the Hot Gas in Galaxies and ClustersChristine Jones, Harvard-Smithsonian Center for Astrophysics
Feb 15, 2006Probing fundamental physics with the Atacama Cosmology TelescopeJoseph Fowler, Princeton University
Feb 22, 2006High-Energy Astrophysics with Gamma-Ray TelescopesRoland Diehl, Max-Planck-Institute for Extraterrestrial Physics
Mar 1, 2006Probing high-redshift luminous galaxies into the ALMA epochAndrew Blain, CalTech
Mar 8, 2006How Did Cassiopeia A Explode? A Chandra Very Large ProjectJohn Martin Laming, Naval Research Laboratory
Mar 29, 2006The Formation of the Solar SystemRe'em Sari, Caltech
Apr 5, 2006Gravitational Lensing with Large Imaging SurveysBhuvnesh Jain, University of Pennsylvania
Apr 12, 2006Extrasolar Planets: From Hot Jupiters to Hot Earths and BeyondSara Seager, Carnegie Institute of Washington
Apr 26, 2006Peeking into a Neutron Star: Neutrons, Condensates, or Quarks?Feryal Ozel, University of Arizona
May 3, 2006Forming the Milky Way Halo: smooth vs chunkyHeather Morrison, Case Western Reserve University
May 10, 2006Report from the Dark Energy Task ForceAndy Albrecht, University of California, Davis
May 17, 2006Gravitational Waves from StringsCraig Hogan, University of Washington
May 24, 2006The Giant Magellan TelescopeWendy Freedman, Carnegie Institute
Sep 27, 2006Type Ia Supernovae from the CFHT Legacy SurveyEric Aubourg, APC Paris / Princeton University
Oct 11, 2006Massive Black Holes from Early Times to the PresentMarta Volonteri, Northwestern University
Oct 25, 2006The Origin of Spheroidal GalaxiesSandy Faber, University of California, Santa Cruz
Nov 8, 2006Neutrino Telescopes and Their MissionTeresa Montaruli, University of Wisconsin, Madison
Nov 29, 2006Mergers of Massive Galaxies, Central Black Holes, and Dark Matter HalosChung-Pei Ma, University of California, Berkeley
Dec 13, 2006Mapping Dark Matter and Dark Energy Using Gravitational LensingPriya Natarajan, Yale University

Astrophysics and Cosmology with HESS
Jan 4, 2006 | RI 480 | 3:30 PM
Felix Aharonian, MPI Heidelberg

The High Energy Stereoscopic System (HESS) of imaging atmospheric Cherenkov telescopes is a powerful multi-functional tool for spectrometric, morphological and temporal studies of nonthermal phenomena and objects representing different Galactic and Extragalactic source populations. I will overview the recent discoveries by HESS with an emphasis on the detection of TeV emission from relatively distant blazars, and discuss some cosmological implications of these results for the Extragalactic Background Light (EBL) at optical and near-infrared wavelengths.

The tension in Standard Big Bang Nucleosynthesis:the baryon density, D, He and Li.
Jan 11, 2006 | RI 480 | 3:30 PM
David Tytler, UCSD

Three methods of measuring the cosmological baryons density now agree within about 10%: the CMB, the D/H ratio using Standard Big Bang Nucleosynthesis, and the Lyman-alpha absorption from the IGM at z=2 to 3. We recently measured the mean amount of absorption in the IGM with an error of 1%, and we use these measurements, and a large set of hydrodynamic simulations to determine the cosmological and astrophysical parameters of the IGM, including the temperature and the baryon density. Using this baryon density, SBBN predicts a factor 3 more 7Li than is seen in halo stars, and systematically more 4He that most measurements. We review the systematic errors and new measurements, and we discuss modifications to BBN that might explain the tension between D, He and Li.

Well-posedness of the Cauchy problem of General Relativity
Jan 18, 2006 | RI 480 | 3:30 PM
Vasileios Paschalidis, University of Chicago

The most common approach to solving the Cauchy problem of General Relativity (GR) is by implementing free evolution schemes of the 3+1 decomposition of Einstein's equations. A long-standing problem in numerical relativity is achieving long-term and stable numerical integration of the GR equations. At present, this is possible for rather short times or for special symmetric cases. In this talk, we will present a general theory for the study of well-posedness of constrained evolution of 3+1 formulations of GR. This new approach incorporates the constraint equations directly and therefore is principally different from standard analyses of well-posedness of free evolution schemes. We will demonstrate that well-posedness of constrained evolution of 3+1 formulations of GR depends entirely on the properties of the gauge and comment on consequences of this result.

Carbon Enhancement in the Galaxy -- A New Probe of the First Stars
Jan 25, 2006 | RI 480 | 3:30 PM
Timothy Beers, Michigan State University

Recent large surveys of metal-poor stars in the Galaxy have revealed that a surprising fraction of them are enhanced in their carbon-to-iron ratios by factors of from 10-10,000 relative to the solar ratio. Although most of the stars in the metallicity interval -2.7 < [Fe/H] < -2.0 are likely to have arisen from Asymptotic Giant Branch processing (and subsequent dumping via mass transfer to a surviving companion), there exist many stars with [Fe/H[ < -3.0 (including the two lowest [Fe/H] stars known, with [Fe/H] < -5.0) that cannot be accounted for by this process. Rather, primordial (or nearly primordial) progenitors are implicated. I report on the existing information from present surveys, and describe the results that will come from the recently-funded extension of the SDSS, which includes the program SEGUE = Sloan Extension for Galactic Understanding and Exploration. SEGUE will identify some 20,000 stars with [Fe/H] < -2.0, several thousand of which are expected to be carbon enhanced.

Searching for Enlightenment
Feb 1, 2006 | RI 480 | 3:30 PM
Jeff Peterson, CMU

In a remote valley in western China stand 10,000 television antennas spread across ten square kilometers. Tied together by an array of hundreds of PC computers this system, the Primeval Structure Telescope (PaST), will soon be used to search for evidence of the early ionization of the Universe. Today most hydrogen gas in the cosmos is ionized. But, before the first stars formed, neutral hydrogen was ubiquitous. By imaging 21 cm hydrogen hyperfine emission from this gas at redshifts from 6 to 25 the ionization state of the early universe can be explored. As the first stars began to light up, the 21 cm emission was extinguished, leaving a patchy radio sky. This patchy structure will be imaged with the PaST array, allowing the era of the first stars to be dated and studied.

Reflections of AGN Outbursts In the Hot Gas in Galaxies and Clusters
Feb 8, 2006 | RI 480 | 3:30 PM
Christine Jones, Harvard-Smithsonian Center for Astrophysics

Chandra X-ray images show the presense of shocks, jets, cavities and buoyant bubbles in the hot gas in galaxies, groups and clusters. These features all owe their origin to outbursts from the supermassive black hole (SMBH) at the nucleus of the system. In this talk I will review recent results on AGN outbursts in the rich clusters MS0735.6+7421, Perseus, Hercules A, Hydra A and Virgo as well as the effects of outbursts and the X-ray luminosities of low luminosity AGN in a sample of 160 early-type galaxies.

Probing fundamental physics with the Atacama Cosmology Telescope
Feb 15, 2006 | RI 480 | 3:30 PM
Joseph Fowler, Princeton University

The Atacama Cosmology Telescope (ACT) is a millimeter-wave telescope designed to map the CMB temperature at arcminute angular scales. ACT will image a few hundred square degrees of the CMB in the southern sky from a site in the Atacama desert. In addition to measuring the primary CMB power spectrum, ACT will survey for massive galaxy clusters through their Sunyaev-Zel'dovich (SZ) signal. Three frequency bands around the SZ null--145, 215, and 265 GHz--will help to separate cluster signals from primordial anisotropy and from point sources. The maps will offer data on a wide variety of questions in fundamental physics and cosmology, including the growth of structure, and the spectrum of primordial perturbations.

High-Energy Astrophysics with Gamma-Ray Telescopes
Feb 22, 2006 | RI 480 | 3:30 PM
Roland Diehl, Max-Planck-Institute for Extraterrestrial Physics

Gamma-rays are messengers of high-energy processes throughout the Universe: Nuclear reactions create radioactive isotopes, and particles which have been accelerated into the relativistic regime create non-thermal radiation. The penetrating nature of these gamma-rays implies that even sources which are invisible or optically thick in other wavelengths can be studied through their gamma-ray emission. The Compton Observatory had surveyed the gamma-ray sky, and had found a few surprises, beyond the images that have been obtained from cosmic-ray interactions with interstellar gas and from diffuse radioactivities originating from cosmic nucleosynthesis. ESA's INTEGRAL observatory recently made possible to probe the low-energy gamma-ray regime at better sensitivity, and, most importantly, add spectroscopy power to resolve characteristics gamma-ray lines. We will discuss the interpretations and findings from recent observations at high energies and the corresponding source models, specifically addressing sources of nucleosynthesis and of particle acceleration in our Galaxy.

Probing high-redshift luminous galaxies into the ALMA epoch
Mar 1, 2006 | RI 480 | 3:30 PM
Andrew Blain, CalTech

I will discuss the observational progress made in understanding the nature and evolution of luminous far-IR galaxies, and highlight the most promising future investigations that lead towards exquisite imaging quality of their optically thick emission from ALMA in about 2012.

How Did Cassiopeia A Explode? A Chandra Very Large Project
Mar 8, 2006 | RI 480 | 3:30 PM
John Martin Laming, Naval Research Laboratory

In April/May 2004 the Chandra X-ray Observatory observed the Cassiopeia A supernova remnant for 1 million seconds as one of the first of the newly instituted 'Very Large Projects'. This is the deepest ever x-ray observation of a supernova remnant, and allows observers to exploit the angular resolution of the Chandra mirrors to the fullest extent, in that spectra of adequate signal/noise can be extracted from very small spatial regions in most locations within the remnant. I will describe progress to date, and future plans, for the analysis of this unique dataset, paying specific attention to quantifying the nature and degree of asymmetry in the explosion, and the abundances and locations of chemical elements synthesized therein.

The Formation of the Solar System
Mar 29, 2006 | RI 480 | 3:30 PM
Re'em Sari, Caltech

How do planets form and how long does it take? Why are their orbits circular and coplanar? What set the number of planets in our solar system? We address these fundamental questions providing a coherent story on the formation of our solar system.

Gravitational Lensing with Large Imaging Surveys
Apr 5, 2006 | RI 480 | 3:00 PM
Bhuvnesh Jain, University of Pennsylvania

I will describe the ideas and challenges in using gravitational lensing for cosmology. Recent results in weak lensing and the observational challenges ahead will be discussed. With planned multi-color imaging surveys, weak lensing can probe dark energy and constrain alternate theories of gravity. I will compare the strengths and weaknesses of lensing with other observational methods.

Extrasolar Planets: From Hot Jupiters to Hot Earths and Beyond
Apr 12, 2006 | RI 480 | 3:30 PM
Sara Seager, Carnegie Institute of Washington

We have entered a new era in planetary astrophysics with over 170 extrasolar giant planets now known. Physical properties of a subset of these planets---the hot transiting giant planets---have been measured, including mass, radius and thermal emission. Even more intriguing than the hot Jupiters are the seven known hot super-massive Earths (mass range 7 to 20 Earth masses), which are expected to consist of a large rocky component. There is a chance to observationally study this class of planets in the near future. Beyond the hot Earths, our own Earth has been studied as an exoplanet, both in its present state and in its paleoclimates. I will summarize which exoplanet physical characteristics can be inferred from spectra, the interpretation of the hot Jupiter spectral data, the possibilities for observation and interpretation of hot supermassive Earths, and the scientific highlights and prospects for the future detection and study of and planets like Earth.

Peeking into a Neutron Star: Neutrons, Condensates, or Quarks?
Apr 26, 2006 | RI 480 | 3:30 PM
Feryal Ozel, University of Arizona

Neutron stars are the densest objects in the universe and may contain hyperon-dominated matter, condensed mesons, or even deconfined or strange quark matter. Because of their low temperatures and high chemical potentials, the physical conditions in their interiors differ greatly from the dense conditions of the early universe or those achieved at hadron colliders. This region of the QCD phase diagram can only be probed through astrophysical observations that measure the mass and radius of neutron stars. For decades, this effort has been hampered by a number of model uncertainties as well as by the lack of accurate measurements of different spectroscopic phenomena from a single source that would break the degeneracies between the neutron star parameters of interest. I discuss how we can now overcome these problems by combining recent developments in our understanding of neutron star atmospheres with observations of distinct phenomena from the same neutron star source. In particular, I report the first unique measurement of the mass and radius of the neutron star source EXO 0748-676. The high inferred mass and large radius of this neutron star rule out all the soft equations of state of neutron star matter. This result shows that condensates and unconfined quarks do not appear under the conditions found in the centers of the neutron stars.

Forming the Milky Way Halo: smooth vs chunky
May 3, 2006 | RI 480 | 3:30 PM
Heather Morrison, Case Western Reserve University

I will summarize our current understanding of the formation of the Galaxy's halo, using a number of different samples of halo stars from surveys including SDSS-II's SEGUE. Evidence is mounting for a "chunky" origin for much of the halo, via infall of satellite galaxies and subsequent formation of star streams. I will also discuss constraints on the smooth halo from a new, high-quality sample of metal-poor stars in the solar neighborhood.

Report from the Dark Energy Task Force
May 10, 2006 | RI 480 | 3:30 PM
Andy Albrecht, University of California, Davis

Understanding the observed cosmic acceleration is widely ranked among the very most compelling of all outstanding problems in physical science. Many believe that nothing short of a revolution will be required in order to integrate the cosmic acceleration (often attributed to “dark energy”) with our understanding of fundamental physics. The DETF was formed at the request of DOE, NASA and NSF as a joint subcommittee of the Astronomy and Astrophysics Advisory Committee (AAAC) and the High Energy Physics Advisory Panel (HEPAP) to give advice on optimizing our program of dark energy studies. To this end we have assessed a wide variety of possible techniques and strategies, and developed a series of factual findings and recommendations. I will present our main conclusions and discuss their implications.

Gravitational Waves from Strings
May 17, 2006 | RI 480 | 3:30 PM
Craig Hogan, University of Washington

Long discredited as the main source of cosmological perturbations, cosmic strings have re-emerged as natural structures in string theory and natural products of stringy inflation. Techniques will be discussed for detecting them, or setting limits on parameters such as the mass per unit length, using gravitational wave backgrounds. The most sensitive current probe is millisecond pulsar timing; in the future, it will be LISA.

The Giant Magellan Telescope
May 24, 2006 | RI 480 | 3:30 PM
Wendy Freedman, Carnegie Institute

The Giant Magellan Telescope (GMT) is a 21-5-meter collecting-area optical/near-infrared telescope with a resolution of a 24.5-meter. The baseline site for the GMT is Las Campanas, Chile. The GMT primary mirror is comprised of seven borosilicate 8.4-meter segments, and the secondary contains seven fast-steering segments aligned to each of the primary mirrors. The first of the primary mirrors has been cast at the Steward Observatory Mirror Laboratory, and preparations are underway for its polishing and testing. Several instrument concepts have been developed covering the wavelength range from the UV/optical to the thermal infrared. The project has just undergone a Conceptual Design Review, with a recommendation to proceed to the Design Development Phase. The Science Working Group has identified several areas where the GMT will have an impact. These include: 1) the nature of dark matter and dark energy 2) the first stars and galaxies 3) star and planet formation 4) the evolution of galaxies and 5) the growth of black holes. Unique capabilities of the GMT include wide-field (~10-arcminute FOV) spectroscopy and the direct detection of exoplanets. The GMT is a consortium of research institutions consisting of the Australian National University, the Carnegie Institution of Washington, Harvard University, Massachusetts Institute of Technology, Texas A&M University, Smithsonian Astrophysical Observatory, University of Arizona, University of Michigan, and the University of Texas at Austin.

Type Ia Supernovae from the CFHT Legacy Survey
Sep 27, 2006 | RI 480 | 3:30 PM
Eric Aubourg, APC Paris / Princeton University

The Supernovae Legacy Survey aims at discovering and spectroscopically identifying 700 type-Ia SN during its five years of operations at CFHT in Hawaii. I will present the survey and the current constraints on matter and energy content of the Universe and on the dark energy equation of state parameter. I will focus on how we plan to increase the expected number of SN to about 1000 using an offline analysis and discuss perspectives of the survey.

Massive Black Holes from Early Times to the Present
Oct 11, 2006 | RI 480 | 3:30 PM
Marta Volonteri, Northwestern University

I'll discuss models for the hierarchical growth of supermassive black holes, feeding pregalactic black hole seeds. Mergers and dynamical interactions, as well as their implications, will be critically addressed. I'll also discuss the constraints on the early evolution of the black holes required by the observations of z=6 quasars.

The Origin of Spheroidal Galaxies
Oct 25, 2006 | RI 480 | 3:30 PM
Sandy Faber, University of California, Santa Cruz

For decades, the standard paradigm for spheroidal galaxy formation was the monolithic collapse theory, in which spheroids collapsed gravitationally in bulk and formed all their stars at very high redshift. This talk will examine evidence that has accumulated over the past year that suggests an extended formation period for spheroidal systems, with many of them forming rather recently via the quenching of blue, star-forming galaxies AFTER z = 1. The mechanism for this quenching is not well understood, but it might be feedback from active black holes. If true, the symbiosis is complete in that the galaxy gives birth to the black hole, but the black hole eventually determines the star-formation history of the galaxy.

Neutrino Telescopes and Their Mission
Nov 8, 2006 | RI 480 | 3:30 PM
Teresa Montaruli, University of Wisconsin, Madison

The current generation of neutrino telescopes, such as AMANDA and Baikal, has proved that the neutrino measurement is feasible using natural gigantic radiators, such as the polar ice and lake deep water. The cubic kilometer scale detectors are becoming a reality with IceCube being built at the South Pole. Sea water is a critical environment but European collaborations are proving that detectors can operate with good angular resolution, but with larger optical background induced by bioluminescence and potassium 40. I will discuss what could be the most interesting signatures for neutrino telescopes, which could be the astrophysical impact of observations and which are the performances of existing and under construction experiments.

Mergers of Massive Galaxies, Central Black Holes, and Dark Matter Halos
Nov 29, 2006 | RI 480 | 3:30 PM
Chung-Pei Ma, University of California, Berkeley

While mergers of gas-rich disk galaxies are thought to lead to the formation of elliptical galaxies, merging of elliptical galaxies is a potentially important process for building up the most massive galaxies and their central black holes in the low-redshift universe. I will discuss results of simulations of these mergers and the dynamical interplay among stars, dark matter, and black holes in forming the global as well as central properties of massive galaxies. New results from recent analyses of SDSS luminous galaxies find similar trends as seen in the simulations. I will also discuss recent work on understanding the mergers of dark matter halos and the halo mass function using the Smoluchowski coagulation equation.

Mapping Dark Matter and Dark Energy Using Gravitational Lensing
Dec 13, 2006 | RI 480 | 3:30 PM
Priya Natarajan, Yale University

Results will be presented on the detailed distribution of dark matter and implications for the nature of dark matter using gravitational lensing of background sources by massive foreground clusters. Strong lensing arcs offer a unique probe of dark energy as well, and I will discuss the utility and feasibility of this technique.