CCAPP Seminars

Neutrinos from GRBs, and the multi-messenger connection

Philipp Baerwald
(Penn State)

The detection of the first ultra-high energy neutrino events inside the IceCube telescope has finally opened neutrinos as a new "window" into the sky. With the neutrino as a new messenger, it is now possible to test astrophysical source models with several different types of messengers. However, to obtain meaningful results from the different messengers, detailed (particle physics) models of the sources are needed. At the example of GRBs, we will first discuss how the neutrino flux predictions are calculated based on gamma-ray observations and how they are used for current neutrino analyses. Then, we will use the particle physics involved to also obtain a prediction of the cosmic ray spectra self-consistently together with the neutrinos. Finally, we will discuss how the combination of neutrino, cosmic ray, and photon data can be used to derive strong constraints on the internal shock fireball model for GRBs and even rule out some of its forms.

The Fermi Bubbles: Possible Nearby Laboratory for AGN Jet Activity

Karen Hsiang-Yi Yang
(U. of Michigan)

One of the most important discoveries of the Fermi Gamma-ray Space Telescope is the detection of two giant bubbles extending 50 degrees above and below the Galactic center (GC). The symmetry about the GC of the Fermi bubbles suggests some episode of energy injection from the GC, possibly related to past jet activity of the central active galactic nuclei (AGN). Thanks to the proximity to the GC, the Fermi Bubbles are excellent laboratories for studying cosmic rays (CRs), Galactic magnetic field, and AGN feedback in general. Using three-dimensional magnetohydrodynamic simulations that include relevant CR physics, I will show how leptonic AGN jets can explain the key characteristics of the Fermi bubbles and the spatially correlated features observed in the X-ray, microwave, and radio wavelengths. I will also discuss how we use our simulations in combination with the multi-wavelength data to obtain constraints on the composition of the Fermi bubbles.

First measurement of pp neutrinos in real time in the Borexino detector

Pablo Mosteiro

The Sun is fueled by a series of nuclear reactions that produce the energy that makes it shine. Neutrinos (ν) produced by these nuclear reactions exit the Sun and reach Earth within minutes, providing us with key information about what goes on at the core of our star. For decades since the first detection of solar neutrinos in the late 1960's, an apparent deficit in their detection rate was known as the Solar Neutrino Problem. Today, the Mikheyev-Smirnov-Wolfenstein (MSW) effect is the accepted mechanism by which neutrinos oscillate inside the Sun, arriving at Earth as a mixture of νe, νμ and ντ, the latter two of which were invisible to early detectors. Several experiments have now confirmed the observation of neutrino oscillations. These experiments, when their results are combined together, have demonstrated that neutrino oscillations are well described by the Large Mixing Angle (LMA) parameters of the MSW effect.
This talk presents progress towards the first measurement of pp neutrinos in the Borexino detector, which would be the first direct real-time measurement of pp neutrinos independent of other experiments. This would be, furthermore, another validation of the LMA-MSW model of neutrino oscillations. In addition, it would complete the spectroscopy of pp chain neutrinos in Borexino, thus validating the experiment itself and its previous results. We also report on a measurement of neutrons in a dedicated system within the Borexino detector, which resulted in an improved understanding of neutron rates in liquid scintillator detectors at Gran Sasso depths. This result is crucial to the development of novel direct dark matter detection experiments.

Seeing Gravitational Waves: Transients in the Local Universe

Mansi Kasliwal
(Observatories of the Carnegie Institution for Science)

The advent of wide-field synoptic imaging has re-invigorated the venerable field of time domain astronomy. Our framework of optical transients no longer has a wide six-magnitude luminosity "gap" between the brightest novae and faintest supernovae. Multiple new and distinct classes of very rare explosions have been uncovered just in the past few years. I review the surge of excitement (and debate) on the physics of these transients with unprecedented explosion signatures. "Gap transients" represent missing pieces in two fundamental pictures: the fate of massive stars and the evolution of compact binaries. Calcium-rich gap transients may even be the key to solving a long standing abundance problem in the intra-cluster medium. Two classes of gap transients are extremely red, hinting that the infrared dynamic sky is ripe for exploration. I conclude with the next frontier in gap transients --- discovering elusive binary neutron star mergers, a goal which may soon be within reach with coordination between the next generation of synoptic surveys and advanced gravitational wave interferometers. This search may literally be the 21st century gold rush!

Fast, Accurate Predictions of the Galaxy Power Spectrum

Juliana Kwan
(Argonna National Lab)

Two point galaxy clustering statistics are a key observable for large scale structure surveys. Unfortunately, they are very difficult to model accurately within the halo model and perturbation theory. In this talk, I will be presenting a new framework for calculating the galaxy power spectrum, called emulation, which can make predictions accurate to ~3%. Our technique uses a set of fully non-linear galaxy power spectra derived from applying the halo occupation model on a dark matter halo catalogue identified in a LCDM N-body simulation. A Gaussian process model then interpolates over the set of input power spectra. Unlike fitting functions, the cosmic emulation framework can be easily generalised to other problems and I will also describe a number of other projects currently in progress, such as emulating the redshift space power spectrum.

Discovery of Fermi Bubbles and Evidence for Past Activities in the Galactic Center

Meng Su
(KIASR (MIT), ITC (Harvard-Smithsonian Center for Astrophysics))

Analysis of data from the Fermi Gamma-ray Space Telescope revealed a pair of gigantic gamma-ray bubble structures, named the Fermi bubbles, each extending ~10 kpc above and below the Galactic center. I will present new results using five years Fermi-LAT data and multi-wavelength observations of the Fermi bubbles in X-ray, microwave, and radio, including updates from dedicated observations. New observations help us to distinguish hadronic from leptonic origin of the cosmic-ray electrons emitting gamma-ray/microwave emission, and constrain the magnetic field within the Fermi bubbles. I will also show our numerical simulations which demonstrate that the bubble structure could be evidence for past accretion events and outflow from the central supermassive black hole. Furthermore, we recently found evidence for large-scale collimated structure penetrating through the bubbles from the Galactic center from Fermi-LAT data. We have proposed to change the survey strategy of Fermi to increase the exposure at the inner Galaxy by more than a factor of 2. New survey strategy has been initiated since December 2013 and will last for at least one year. I will end up with a discussion of future gamma-ray space missions.

Beyond Dark Energy

Bhuvnesh Jain
(U. Penn)

The discovery that our universe is accelerating poses fascinating challenges for physics and astronomy. Vacuum energy, more generally called dark energy, is a possible explanation for the observed cosmic acceleration. Modifications to Einstein's general relativity are being explored as alternatives to dark energy. I will describe the theoretical motivations and experimental tests of gravity theories and other effects involving dark sector couplings. On large scales, they require a different take on cosmological observations such as gravitational lensing and large-scale structure in the universe. On much smaller scales the new tests of gravity use pulsating stars, rotating disk galaxies and other astronomical phenomena. I will describe how these diverse observations are being used to look "beyond dark energy".

Very High Energy Blazars: A Broadband Perspective

Amy Furniss

Blazars, a type of active galaxy with a jet pointed toward the observer, are perplexing objects harboring relativistic particle populations with intrinsic characteristics which, despite more than 20 years of investigation, remain an enigma. These sources emit non-thermal radiation and display bright, variable emission at all energies. Blazars are the most commonly detected type of very high energy (VHE; E > 100 GeV) source and can be observed at these energies by imaging atmospheric Cherenkov telescopes such as VERITAS. A foundational understanding of the underlying acceleration mechanisms, particle environment, non-thermal emission and definitive extragalactic distance enable the use of these extraordinary objects to constrain the star formation history of the Universe through the indirect measurement of the extragalactic background light, the accumulated and reprocessed radiation of all starlight produced over the life of the Universe. I will summarize the results from a variety of innovative and complementary multiwavelength observations which can be used to address long-standing questions regarding the underlying acceleration mechanism, the emission environment and constituent particles within VHE blazar jets.

Constraints on the parameter space of axion dark matter

Kfir Blum
(Princeton / IAS)

I will discuss phenomenological constraints on the parameter space of axion dark matter. First, I will review how standard chiral perturbation theory relates the axion mass to the induced neutron electric dipole moment (nEDM). I will argue that this well known relation can only be avoided at the price of fine-tuning, and show that it has significant implications for proposed experimental searches for the oscillating nEDM induced by the background field of axion dark matter. I will then show that, if one is willing to accept this kind of fine-tuning, another constraint comes up by requiring that axion-driven operators in the chiral Lagrangian, that redshift up in the early Universe, do not ruin the success of Big-Bang Nucleosynthesis at z~10^10.

Order out of chaos:
Towards understanding galaxy formation in the cosmological context

Andrey Kravtsov

Galaxy formation is a complex, hierarchical, highly non-linear process, which involves gravitational collapse of dark matter and baryons, supersonic, highly compressible and turbulent flows of gas, star formation, stellar feedback, as well as heating, cooling, and chemical processes that affect the gas and, indirectly, the stellar and dark matter distributions. Nevertheless, despite the apparent complexity of processes accompanying galaxy formation, galaxies exhibit a number of striking regularities, such as tight correlations between galaxy sizes, masses, luminosities, and internal velocities and surprisingly tight correlations between properties of stars and gas in galaxies and the mass and extent of their parent halos dominated by dark matter. Existence of such correlations indicates that powerful processes operate to bring order out of chaos. Understanding what these processes are and how they operate is not only fascinating scientifically, but is critical for interpreting the avalanche of current and future observations of galaxies across cosmic time. I will describe recent progress in our understanding of how such regularities can arise in a seemingly chaotic and nonlinear process of galaxy formation.

Elizabeth Fernandez

A Multiwavelength Understanding of the Epoch of Reionization

Elizabeth Fernandez

Up until very recently, the Epoch of Reionization has been largely observationally unexplored . However, with advancements of modern telescopes, we are now able to observe this period of the Universe in multiple ways. While observations are still very challenging due to a host of foreground contaminants, combining observations at multiple wavelengths can lead to a greater understanding of the populations of stars and galaxies at these redshifts. I will describe two of these observables: the Cosmic Infrared Background, which is partially the integrated light from all stars and galaxies at high redshifts, and the 21cm Background, which results from emission from neutral gas. These observables, when paired with theory and simulations, can tell us about some of the first stars and galaxies that formed within our Universe.


"Light WIMPs" in direct dark matter detection

Graciela Gelmini

Four direct dark matter detection experiments, DAMA, CoGeNT, CRESST and CDMS-II-Si, find potential signals of "Light WIMPs" (Weakly Interacting Massive Particles with mass 10 GeV or lighter) while several other experiments, CDMS-II-Ge, CDMSlite, SuperCDMS, XEONON10, XENON100, LUX..., do not find any. Are all or some the positive and negative signals compatible with each other? I will review the experimental situation and compare the data for different particle candidates in a dark halo model dependent and in a dark halo model independent manner.

Using Millions of SDSS Halo Stars to Robustly Measure the Shape of the Milky Way's Dark Matter Halo

Sarah Loebman

I will present detailed evidence from the Sloan Digital Sky Survey (SDSS) for the presence of a dark matter halo within Milky Way (MW). Using the number density distribution and kinematics of SDSS halo stars, my collaborators and I probe the dark matter distribution to heliocentric distances exceeding ~10 kpc and galactocentric distances exceeding ~20 kpc. Our analysis utilizes Jeans equations to generate two-dimensional acceleration maps throughout the volume; this approach is thoroughly tested on a cosmologically derived N-body+SPH simulation of a MW-like galaxy. We show that the known accelerations (gradients of the gravitational potential) can be successfully recovered in such a realistic system. The SDSS observations reveal that, in Newtonian framework, the implied gravitational potential cannot be explained by visible matter alone: the gravitational force experienced by stars at galactocentric distances of ~20 kpc is as much as three times stronger than what can be attributed to purely visible matter. Leveraging the baryonic gravitational potential derived by Bovy & Rix (2013), we show that the SDSS halo stars also provide a strong constraint on the shape of the dark matter halo potential. Within galactocentric distances of ~20 kpc, the dark matter halo potential is well described as an oblate halo with axis ratio q_DM=0.7+/-0.1. Thanks to precise two-dimensional measurements of acceleration for halo stars, we can reject MOND model as an explanation of the observed behavior, irrespective of the details in assumed in the interpolating function and the value of characteristic acceleration. In the era of Gaia and LSST, these techniques can be used to map the MW dark matter halo with a much better fidelity, and to a much larger galactocentric radius.

Review of the proton radius puzzle

Maxim Pospelov
(Victoria, Perimeter)

Recent measurements of the Lamb shift in the muonic hydrogen and deuterium revealed a puzzling discrepancy with similar measurements in e-p systems. This is often presented as a difference in the value for the proton charge radius. The origin of the discrepancy is not known, and in my talk I will cover possible scenarios for its resolution: an experimental error, "unusual" QCD effects, or new MeV-scale forces. For the latter, I describe a new idea for searches of MeV-scale force carriers using underground accelerators.

The Physics of Gas Sloshing in the Cores of Galaxy Clusters

John ZuHone

Many X-ray observations of relaxed galaxy clusters reveal the presence of sharp, spiral-shaped discontinuities in the surface brightness of the X-ray emitting gas. Spectral analysis of these features shows that the colder gas is on the brighter side, hence they have been dubbed "cold fronts." These features arise naturally in simulations from the cool-core gas "sloshing" in the gravitational potential. Their sharpness and stability has important implications for the microphysics of the ICM. The sloshing motions may have other effects, such as contributing to the heating of the cluster core and the acceleration of relativistic particles. I will present simulations of gas sloshing in clusters, explain their formation and evolution, and discuss the implications for the physics of the ICM, including fresh results on heat conduction, viscosity, and radio mini-halos. I will also briefly discuss yt, an emerging software toolkit for analyzing astrophysical data from simulations and other datasets.

Statistically probing the merger history of the Milky Way

Facundo Gomez
(Michigan State)

Despite a wealth of observational information that is currently available, the details of the formation of our own Galaxy remain a puzzle. Thanks to the latest generation of stellar surveys it is now possible to study in detail how the Milky Way has evolved to become the galaxy we currently observe During the first part of this talk I will discuss how semi-analytic models of Galaxy formation, coupled to cosmological N-body simulations, could allow us to constrain the Milky Way merger history. Statistical model emulators are used to efficiently explore the multi-dimensional input parameter space of our model. We search for the sets of input parameters that can best reproduce the cumulative Luminosity Function (cLF) of satellite galaxies. Our results indicate that the determination of "best-fit" parameters is highly susceptible to the particular merger history of the Milky Way-like host. When comparing the resulting best-fitting models against independent sets of observational data, we find that only one of these models was able to simultaneously reproduce the stellar halo mass within 40 kpc of the Galactic center and the cLF. On the basis of this analysis it is possible to disregard certain models, and their corresponding merger histories, as good representations of the underlying merger history of the Milky Way. During the second part of this talk I will discuss about the perturbations that a minor merger event may induce in the phase-space distribution of Solar Neighborhood stars. In particular, I will show how the interaction between the Milky Way disc and the Sagittarius dwarf galaxy could qualitatively explain some of the radial and vertical perturbations identified in current observational data sets.

Cosmology with the Baryon Oscillation Spectroscopic Survey (BOSS)

Florian Beutler

I will present the results of the BOSS-DR11 analysis which we published 4 months ago. I will also present measurements of the growth of structure through redshift-space distortions using the power spectrum multipoles. Such a measurement can be used to test General Relativity. Our measurements are in some tension with the expectation of LCDM and I will suggest ways in which this tension can be alleviated.

Constraints on Dark Matter from Merging Galaxy Clusters

Doug Clowe
(Ohio University)

Over the past decade, merging galaxy clusters have become one of the primary sources of data for constraining properties of dark matter particles as well as the force law of gravity on Mpc scales. Using the Bullet Cluster, I will demonstrate how merging clusters prove that dark matter makes up the majority of the mass of their systems independent of assumptions regarding the nature of the force law of gravity and place constraints on the self-interaction cross-section of dark matter. I will review the dozen merging clusters that have been studied since the Bullet Cluster, and discuss whether any of them show serious departures from a light-traces-mass paradigm that would cause significant problems for a LCDM universe.

Interpretation of standard problems associated with Milky Way dwarf spheroidals

Louis Strigari
(Indiana U.)

Improvements in theory and observations have put a new spin on the classical problems involving Milky Way dwarf spheroidals, and dwarf galaxies in general. In this talk, I will discuss what information can robustly be extracted from these observations, and how this information can be connected to the large scale cosmological model. I will close by discussing how this field will progress in the era of 30m class telescopes and with forthcoming galaxy surveys.

High redshift starburst galaxies revealed by SPT, ALMA, and gravitational lensing

Joaquin Vieira
(Illinois, Urbana-Champaign)

The South Pole Telescope (SPT) has systematically identified a large number of high-redshift strongly gravitationally lensed starburst galaxies in a 2500 square degree cosmological survey of the millimeter (mm) sky. With ALMA, we have performed an unbiased spectroscopic redshift survey with these sources and determined that roughly 40% lie at z>4. Two sources are at z=5.7, placing them among the highest redshift starbursts known, and demonstrating that large reservoirs of molecular gas and dust can be present in massive galaxies near the end of the epoch of cosmic reionization. These sources were additionally targeted with high resolution imaging with ALMA, unambiguously demonstrating them to be strongly gravitationally lensed by foreground structure. We are undertaking a comprehensive and systematic followup campaign to use these ``cosmic magnifying glasses'' to study the infrared background in unprecedented detail, inform the condition of the interstellar medium in starburst galaxies at high redshift, and place limits on dark matter substructure. I will discuss the scientific context and potential for these strongly lensed starburst galaxies, give an overview of our team's extensive followup efforts, and describe our latest science results.

Microlensing techniques: revealing the "black box"

Ana Mosquera

You know that microlensing techniques are powerful. You know that our group and collaborators have used them to set by the first time limits on quasar's X-ray emitting regions. And you know that currently you can only rely upon us to study the inner structure of AGNs. But, how does the microlesing machinery actually works? Under which assumptions do we fit and analyze the data? And why is our technique so robust? In my talk I'll answer to these questions following Mosquera et al. 2013.

Magnetic Deflections of Ultra-High Energy Cosmic Rays

Michael Sutherland

The nature of cosmic rays are mysterious even more than a century after their discovery. At the highest energies ($E > 10^{18}$ eV), their composition and sources are unknown. Deflection in cosmic magnetic fields, even at these ultra-high energies, complicates source identification due to a direct dependence on the composition as well as uncertainties in the magnetic fields. For a nearby source, for example Centaurus A (Cen A), deflection from the extragalactic magnetic field is minimized. This allows for deflection studies of the Galactic magnetic field (GMF), which itself is capable of significantly altering UHECR trajectories. I will highlight a study of simulated UHECR trajectories from Cen A to Earth for a range of rigidities, allowing for primaries as heavy as Fe nuclei with energies exceeding 50 EeV. The Galactic magnetic field is modeled using the recent work of Jansson and Farrar which fitted its parameters from extragalactic Faraday rotation measures and WMAP7 synchrotron emission maps. This model also includes parameters for a detailed turbulent component. Aspects of the arrival direction distributions are examined for dependencies on rigidity and properties of turbulent field realizations.

Galaxy intrinsic alignments: systematic nuisance or powerful probe?

Jonathan Blazek

The shapes and orientations of galaxies arise from complex processes on comparatively small scales. In the context of weak gravitational lensing measurements, large-scale correlations between these shapes, known as "intrinsic alignments" (IA), constitute the most significant astrophysical source of uncertainty and have the potential to degrade cosmological constraints. If sufficiently understood, however, IA can probe the physics of the formation and evolution of galaxies and their surrounding dark matter halos. IA may also provide a valuable tracer of large-scale structure. In this talk, I will outline why understanding IA is critical for current and future weak lensing surveys, including DES and LSST. I will describe recent and ongoing work in which we use both analytic modeling and observational data to make significant progress towards this goal.

Quasars and their absorption lines: a legacy survey of the high redshift universe with X-shooter

Kelly Denney

Utilizing the X-shooter spectrograph on the VLT, we have obtained spectra of 100 z>3.5 QSOs with high S/N (95% of the reduced spectra have S/N>20 and ~50% have S/N>30). X-shooter is a unique, 3-arm echelle spectrograph that covers wavelengths from the UV cutoff ~3000A through K-band (2.48 microns) at R~6,000. This Large Programme represents the first major spectroscopic QSO survey in the rest-frame UV and optical at z>3.5. I will present our data and science goals, though given the time allotted, I will only be able to discuss in more detail some of our plans for this exquisite data set, which encompass (1) measurement of the matter power spectrum with the Ly-alpha forest at high redshift, including an independent measurement of cosmological parameters with a joint analysis of these and the Planck publicly released data; (2) determination of the incidence of MgII absorbers at z > 2.5 with unprecedented sensitivity to test predictions from the cosmic star formation rate; (3) investigation of the physical environments of the quasars, including, e.g., accurate measurements of black-hole masses, luminosities and metal abundances in a homogeneous sample; and (4) measurement of the universe's opacity at the Lyman limit and constraint of the UV background via the proximity effect.

AGN-STORM - Space Telescope and Optical Reverberation Mapping of NGC 5548

Gisela DeRosa

Active Galactic Nuclei are the spectacular manifestation of accreting black holes and can tell us many things about their central powering engines. Reverberation mapping is a powerful technique to study the region near the supermassive black holes, allowing a full geometric and kinematic modeling of the broad line region gas through the study of variations of the emission line profiles. After a brief review of reverberation mapping methods, I will focus on AGN-STORM, a program centered on 180 daily HST observations designed to study in unprecedented details the broad line region in one AGN: NGC 5548. I will describe the observing strategy, the challenges and the aims of this ambitious project and present preliminary results.

Detecting absorption signatures of warm / hot gas circum-galactic gas in COS archival data

Stephan Frank

A large fraction of the baryons at the low redshift universe (z=1, and below) has thus far escaped our heroic detection efforts. Simulations predict that part of these "missing" baryons may be located in areas of the temperature-density parameter space that would produce weak UV absorption features when seen against bright background sources like QSOs. Here, I am going to report on our ongoing project to detect such a weak signature of this gas, focusing on a specific transition (NeVIII). Instead of presenting polished results, however, I will focus on the method itself we have specifically developed for this prupose ('agnostic stacking'), but also highlighting its broader applicability for similar searches.

Model Independent Measurements of Angular Power Spectra

Sheldon Campbell

Spatial fluctuations of astrophysical signals are a powerful probe of source distributions, radiation production mechanisms, and propagation effects. The precision of measuring angular power spectra is currently estimated as a combination of shot noise, instrument systematics, and cosmic variance. We show that an important contribution, dependent on the finite statistics of the experiment, has been neglected. These new results allow for improved estimates of sensitivities to angular power by statistics-limited observations, such as for high-energy gamma rays.

First exoplanet similar to Uranus

Radek Poleski

We know exoplanets similar to both inner rocky planets of Solar System as well as Jupiter and Saturn. However, the long orbital periods of Uranus and Neptune make their analogs inaccessible to methods that depend on periodic phenomenon i.e. radial velocities and transits. Also direct imaging is not sensitive enough. I present the first discovery of extrasolar planet that has orbit and mass similar to Uranus using gravitational microlensing method. Moreover, the host star has a relatively nearby stellar or brown dwarf companion. All the basic properties of the lens triple system can be understood without detail modeling.

Dynamical Modeling of the Broad Line Region in AGNs with Reverberation
Mapping Data

Kate Grier

Both theoretical and observational evidence suggests that galaxies and their central supermassive black holes are connected. In order to understand these connections, we must have accurate measurements of supermassive black hole masses in objects across the observable universe. All black hole mass measurements in distant galaxies are made using emission lines in active galactic nuclei (AGN) -- however, the unknown conditions within the broad line-emitting region could be a source of serious systematic errors in black hole mass measurements in these objects. Reverberation mapping methods have the capability of both yielding black hole mass easurements as well as information about the broad line region itself. I will discuss the use of dynamical modeling techniques with reverberation mapping data to probe the geometry and kinematics of the broad line region in active galactic nuclei to help better constrain black hole mass estimates in these galaxies and understand the physics of the BLR, highlighting preliminary results using data from a 2010 reverberation campaign carried out here at OSU.

Understanding the Detector Background for Astrophysical MeV
Neutrino Detection

Shirley Li

Background rejections are crucial for MeV neutrino detection. When muons travel through matter, their energy losses lead to nuclear breakup (“spallation”) processes. Subsequent beta decays can lead to detector backgrounds that mimic neutrino signals, and isotopes with long lifetimes are especially difficult to cut. In a recent paper from Super-Kamiokande collaboration, a correlation between the spallation event position and a peak in the prior muon Cherenkov light profile was found. We calculate the rates of isotopes produced by muons and their secondaries in Super-Kamiokande and study the properties of electromagnetic showers induced by muons. A better theoretical understanding of these processes will help in developing new techniques to reduce detector backgrounds.

Answers from the void

Paul Sutter

Voids are the large, underdense regions in the cosmic web, and they are potentially powerful cosmological probes due to their intimate connection to the growth of structure, their domination by dark energy, and their relative lack of systematics. I will present our latest work to identify voids in galaxy redshift surveys, our efforts to understand their fundamental nature and their connection to dark matter underdensities, and an overview of many diverse cosmological applications, including gravitational lensing, the ISW effect, and the Alcock-Paczynski effect.

Clustering, Proximity, and Balrog

Eric Suchyta

I will present work in progress about what happens to galaxy clustering when the influence of proximity effects in the data are included. I will touch on a new software package we have developed which is directly related to problem at hand. I will demonstrate in simple terms what is difficult about the problem and what the answer must look like.

Fishing for the FIR Line Deficit in the Local Swimming Hole: Heating and Cooling in the ISM

Kevin Croxall

The physical state of interstellar gas and dust is dependent on the processes which heat and cool this medium. The principal mechanisms responsible for the heating and cooling of this gas are thought to be the injection of photoelectrons from dust and far-infrared line emission, respectively. In standard practice, we express the efficiency of the photoelectric effect as the ratio of the strong [CII] cooling line emission to thermal dust emission, [CII]/TIR. As the average temperature of dust grains increases a deficit appears in the ratio of [CII]/TIR, according to studies of the global properties of galaxies. While several solutions to this occurrence have been suggested, its cause has not been clear. However, galaxies host a complex ISM, that is most certainly inhomogeneous. Deeper understanding of this deficit requires observations with better spatial resolution to disentangle environments with different radiation fields. Using data from the Herschel space observat ory we investigate the [CII] deficit in nearby galaxies.

Testing the wedge effect on future 21cm BAO surveys

Hee-Jong Seo

Baryon acoustic oscillations (BAO) provide a robust standard ruler with which to measure the acceleration of the Universe. The BAO feature has so far been detected in optical galaxy/qso surveys. Intensity mapping of neutral hydrogen emission with a ground-based radio telescope provides another promising window for measuring BAO at redshifts of order unity for relatively low cost. Although very promising in terms of performance per cost, the major challenge for this method is the severe foreground contamination. I will discuss the effect of the foregrounds on 21cm surveys when they are not removed properly.

Unorthodox weak-lensing applications in DES

Peter Melchior

The Dark Energy Survey (DES) will soon start the second season of observations. I'll review the current state of the survey and summarize the efforts to control and improve the quality of observations and data processing. I will then discuss ideas how to exploit the existing data for weak-lensing purposes in several ways other than cosmic shear.

An Ultra-high Energy Neutrino Search with the ARA Testbed

Carl Pfendner

The Askaryan Radio Array (ARA) is an ultra-high energy (UHE) cosmic neutrino detector located at the South Pole. The cosmic ray flux cut off above primary energies of 10^19.5 eV leads us to expect a UHE neutrino flux due to the GZK effect. The detection of these UHE cosmic neutrinos will add to the understanding of the sources and physics of UHE cosmic rays. ARA uses the radio Cherenkov technique to search for UHE neutrinos by deploying radio frequency (RF) antennas at 200m depth in the Antarctic ice and searching for impulsive RF signals. A prototype ARA Testbed station was deployed in the 2010-2011 season and the first design-level ARA stations were deployed in the 2011-2012 and 2012-2013 seasons. I will present the results of one of the first neutrino searches with 2011-2012 ARA Testbed data.

Hot galactic winds constrained by the X-ray luminosities of galaxies and ram pressure acceleration of cold clouds

Dong Zhang


Galactic superwinds may be driven by very hot outflows generated by overlapping supernovae within the host galaxy. We use the Chevalier & Clegg (CC85) wind model and the observed correlation between X-ray luminosities of galaxies and their SFRs to constrain the mass loss rates across a wide range of star formation rates (SFRs), from dwarf starbursts to ultra-luminous infrared galaxies. We show that for fixed thermalization efficiency and mass loading rate, the X-ray luminosity of the hot wind scales as Lx ~ SFR2, significantly steeper than is observed for star-forming galaxies: Lx ~ SFR. Using this difference we constrain the mass-loading and thermalization efficiency of hot galactic winds. For reasonable values of the thermalization efficiency (<~ 1) and for SFR >~ 10 M_sun/yr we find that \dot{M}hot/SFR <~ 1, significantly lower than required by integrated constraints on the efficiency of stellar feedback in galaxies, and potentially too low to explain observations of winds from rapidly star-forming galaxies. Moreover, we highlight that the CC85-like hot wind is unlikely the mechanism in accelerating neutral cold outflows in most starbursts observed by Na D absorption surveys, expect for some local dwarf starbursts.

Recent progress on Magnification in the Dark Energy Survey

Eric Huff


Magnification is shear's neglected cousin, and by ignoring this lensing measurements ignore half of their potential signal. There are good reasons for this, but recent progress on magnification with Dark Energy Survey data holds out the prospect of magnification's achieving parity with shear. In this talk, I will describe the hybrid image simulations that make this feasible, and show preliminary magnification results using DES data.

Gyrochronology in the Kepler Era: What Can Stellar Rotation Do for You?

Jennifer van Saders


Cool, single main sequence stars have rotation periods that increase as they age. The technique of gyrochronology uses the observed relationship between rotation period, stellar color, and age to date old field stars based on two key assumptions: 1) that all targets can be treated as single main sequence stars that spin down as a function of time, and 2) that the relations can be calibrated on systems of solar age and younger and extrapolated to old stars, where data has traditionally been sparse. With the recent availability of space-based photometry that provides both rotation periods (from stellar spot modulation) and independent ages (from asteroseismology), we are in a unique position to test and better calibrate rotation as a tool. I focus, in particular, on how an understanding of observational selection effects and behavior of rotation across all stellar types is critical for the calibration and interpretation of gyrochronological ages.

Cross-correlating Planck, SPT, DES, Fermi and low-redshift galaxy surveys

Aurelien Benoit-Levy


By deflecting the trajectories of the CMB photon from the last scattering surface, gravitational lensing imprints statistical signatures of the matter distribution in the observed temperature and polarization anisotropies of the CMB. Extracting this signature permits the reconstruction of the lensing potential, a powerful probe of the matter distribution. Matter distribution can also be probed by galaxy surveys thus providing additional information that can be correlated with the CMB lensing potential. In this talk I will present some aspects of these cross-correlations focusing on the complementary of DES and Planck/SPT. I will also present some recent work that focuses on the correlation of the gamma ray sky observed by the Fermi satellite and catalogues of nearby galaxies.

Understanding the Magnetic Variability of M and L dwarfs

Sarah Schmidt


M and early-L dwarfs are often active, revealing the presence of magnetic fields through both quasi-static emission from their chromospheres and coronae in addition to dramatic flares. Even the quasi-static emission exhibited by these low mass stars is intrinsically variable on timescales ranging from minutes to possibly even decades. I will briefly discuss current and future work to understand the magnetic variability of M and L dwarfs through photometric surveys for flares and spectroscopic monitoring for variations in the Halpha emission lines.

Improved limits on sterile neutrino dark matter by Fermi-GBM

Kenny Ng


Sterile neutrinos with mass in the keV range are a well motivated dark matter candidate. Interestingly, these cannot be completely stable, though the lifetimes are very long. The decays produce an X-ray line that provides a distinctive signature. Stringent limits were set using Chandra, XMM-Newton, and INTEGRAL. However, there is a gap in sensitivity for the mass range 20 to 40 keV (with line energy 10 to 20 keV), because this is outside the sensitivity range of the fore-mentioned missions. For the first time, we show that it is possible to use Fermi Gamma-ray Burst Monitor (GBM) data to search for such lines in this gap. Our preliminary result show that we can improve the limit on sterile neutrino decay rate by about an order of magnitude.

Cosmic Rays and Neutrinos as Complementary Probes of Ultra-High Energy Astrophysics

Nathan Griffith


Ultra-high energy cosmic ray and neutrino spectra provide us with a complementary set of information that can be used to uncover a variety of information about ultra-high energy phenomena. This work uses fits to the Pierre Auger Observatory's 2013 data to generate neutrino spectra. Then, looking through the lens of next generation neutrino detectors (EVA, ARA), the ultra-high energy parameters of source distribution and source spectrum are inspected.

An All-Sky, Multi-wavelength Astronomy Computational Engine

Demitri Muna


Astronomy produces extremely large data sets from ground-based telescopes, space missions, and simulation. The problem is that no one institution can host all of this data, let alone have the resources to properly manage it. The result is that applying analyses against full data sets across the wide range of wavelengths available is either beyond the resources of most astronomers or currently impossible. Simply having an extremely large volume of data available in one place is not sufficient; one must be able to make valid, rigorous, scientific comparisons across very different data sets from very different instrumentation. This talk will describe a framework of distributed data and distributed computation for astronomers.

Elizabeth Fernandez

From Nexus to Hopf: on the structure and dynamics of the Cosmic Web

Rien van de Weijgaert
(Kapteyn Institute, University of Groningen)


The Cosmic Web is the fundamental spatial organization of matter on scales of a few up to a hundred Megaparsec, scales at which the Universe still resides in a state of moderate dynamical evolution. galaxies, intergalactic gas and dark matter exist in a wispy weblike spatial arrangement consisting of dense compact clusters, elongated filaments, and sheetlike walls, amidst large near-empty void regions. This seminar will describe recent work on the structure and dynamics of the Cosmic Web. For the analysis of its complex and multiscale structural pattern, we invoke concepts from computational topology and computational geometry. We apply the explicit multi-scale -- parameter-free and scale-free -- Nexus/MMF Multiscale Morphology formalism to dissect the cosmic mass distribution into clusters, filaments, walls and voids. This results in a systematic study of the evolving size and volume distribution of these structural components. Subsequently, we assess the mass and halo distribution in the filaments and walls, and follow their evolution. To study the dynamical evolution of the cosmic web, we have developed an updated adhesion model of cosmic structure formation based on Voronoi and Delaunay tessellations. With this we can systematically follow the outline of the emerging cosmic web and its morphological components. This provides a systematic assessment of the sensitivity of the cosmic web to different cosmologies and/or as a function of power spectrum. We conclude with a short discussion of the detection of galaxy spin alignments with the filaments in which galaxies are embedded, the most direct manifestation of the influence of filaments on the properties of galaxies.

Tova Yoast-Hull

Cosmic Ray Populations in Three Starbursting Galaxies

Tova Yoast-Hull


M82, NGC 253, and Arp 220 are often associated with each other due to similarities in the intense starburst environments contained within each galaxy. Dense concentrations of young massive stars, strong magnetic fields, and high radiation fields characterize their starburst nuclei. Additionally, both M82 and NGC 253 have been detected in gamma-rays with Fermi. Despite their similarities, the interstellar medium and effects of galactic winds differ in these galaxies. However, these distinctions are vital to understanding the role of cosmic ray interactions and the observed radio and gamma-ray spectra from each galaxy. I will discuss results of my single-zone models of the cosmic ray populationsof the starburst nuclei and their implications for future gamma-ray and neutrino observations.

Photometric quasars and primordial non-Gaussianity

Boris Leistedt


Quasars are highly biased tracers of the large-scale structure and therefore powerful probes of the initial conditions and the evolution of the universe. However, current spectroscopic catalogues are relatively small for studying the clustering of quasars on large-scales and over extended redshift ranges. Hence one must resort to photometric catalogues, which include large numbers of quasars identified using imaging data but suffer from significant stellar contamination and systematic uncertainties. I will present a detailed analysis of the photometric quasars from the Sloan Digital Sky Survey, and the resulting constraints on the quasar bias and primordial non-Gaussianity. The constraints on $f_{\rm NL}$, its spectral index, and $g_{\rm NL}$, are the tightest ever obtained from a single population of quasars or galaxies, and are competitive with the results obtained with WMAP, demonstrating the potential of quasars to complement CMB experiments. These results take advantage of a novel technique, 'extended mode projection', to mitigate the complex spatially-varying systematics present in the survey in a blind and robust fashion. This work is a new step towards the exploitation of data from the Dark Energy Survey, Euclid and LSST, which will require a careful mitigation of systematics in order to robustly constrain new physics.

Tova Yoast-Hull

Lessons in Near-Field Cosmology from Simulating the Local Group

Shea Garrison-Kimmel


Studies of the Milky Way (MW) and Andromeda (M31) galaxies, along with their associated satellites and nearby dwarf galaxies, have proven immensely useful for constraining the cosmology of the Universe, particularly on small scales. I will present a number of simulations, many of which are a part of the ELVIS Suite, cosmological zoom-in simulations of Local Group-like volumes of MW/M31 pairs. Using these, and other simulations, I will highlight existing tensions within the LCDM paradigm, as well as illustrate how simulations can provide links between near-field and deep-field observations.

Tova Yoast-Hull

The evolution of early-type galaxies: a strong lensing perspective

Alessandro Sonnenfeld


Early-type galaxies are believed to grow as a result of mergers, but the details of this process are still largely unknown. Do the mergers involve galaxies of comparable mass (major) or are they dominated by small systems (minor)? Is there dissipation (wet) or not (dry)? Different processes leave different signatures on the mass structure of early-type galaxies. Gravitational lensing provides a unique way to detect these signatures. The SL2S project measured the evolution of the mass profile of massive early-type galaxies during the last 7 billion years, including constraints on the mean density slope, dark matter fraction, inner dark matter slope and stellar IMF. Based on collected data, we find that theoretical models for the evolution of early-type galaxies through dry mergers alone are unable to reproduce the observed trends. Additional physical processes, likely related to baryonic physics, are necessary to match the entire set of observables.

Tova Yoast-Hull

The DECam Legacy Survey & Image reduction using the Tractor

Dustin Lang


I will introduce the DECam Legacy Survey, a large public imaging program that will observe over 6,000 square degrees in grz, to ~2 mags deeper than SDSS. The survey will be critical for DESI (the Dark Energy Spectroscopic Instrument) and should provide good legacy value to the community. I will show some preliminary data reductions using "the Tractor", a code for generative modeling of multi-band, multi-epoch image collections.

Tova Yoast-Hull

Satellite quenching and the life cycle of dwarf galaxies.

Colin Slater


In the past ten years the known population of Local Group dwarf galaxies has expanded substantially, both to greater distances from the Milky Way and to lower dwarf masses. This growing sample allows us to study the dwarf system as a population, and ask if we can see in aggregate the signs of processes that would otherwise be difficult to trace in dwarfs individually. Following this strategy I will discuss how the quenching of dwarf galaxies can be modeled and understood at the population-level, and how we use that to constrain how possible quenching mechanisms must work if they are to reproduce the Local Group system that we see. I will also discuss work done with Pan-STARRS to study the role of infalling satellites in disrupting the outer disk of the Milky Way and creating the so-called "Monoceros Ring".

Eavesdropping on the Dark Sound of the Universe

Francis-Yan Cyr-Racine

Self-interacting dark matter (DM) has been put forward as a way to address potential problems with the Cold DM paradigm on sub-galactic scales. For a broad class of models the interactions between DM particles are mediated by a light force carrier. At temperatures above its mass, the force carrier effectively behaves as a dark radiation (DR) component that tightly couples to the DM, forming an almost perfect fluid. We expect this combined DM-DR system to give rise to sound waves propagating throughout the cosmos until DM kinematically decouples from the DR. Much like the standard baryon acoustic oscillations, these dark acoustic oscillations (DAO) imprint two characteristic scales, the sound horizon of dark matter and its Silk damping scale, in the matter density field. We find that linear cosmological data and CMB lensing put strong constraints on existence of DAO features in the CMB and the large-scale structure of the Universe. We also study, for the first time, the nonlinear evolution of cosmological structures in this type of theories by performing N-body simulations including both the modified matter power spectrum and the DM self-interactions. We find the resulting phenomenology to be far richer then in the cold or warm DM case. We conclude by discussing how quasar strong gravitational lenses could be used to probe this class of dark matter models.

The Sad Story of the Cosmic EUV Background

Matthew McQuinn

After reionization, a largely uniform ~1 Rydberg background pervaded the Universe, keeping the intergalactic hydrogen extremely ionized. The characteristics of this background depend on the properties of the sources (quasars and galaxies) and the absorbers (Lyman-limit systems). Modeling the sources is difficult, but I will argue that the absorbers seem to be captured in cosmological simulations, at least at high redshifts. Quick evolution (on a time < 0.1 H(z)^-1) in the ionizing background is observed at z=6, which has (controversially) been interpreted as indicating the end of reionization. I will explain why this evolution must owe to the absorbers and discuss how such quick evolution could arise. We can directly measure the ratio of the 1Ry to 4Ry ionizing background by comparing the hydrogen Lyman-alpha forest to the HeII Lyman-alpha forest in the same sightline. Previous attempts to measure this ratio found order-of-magnitude fluctuations on 1-10 Mpc scales, in conflict with theoretical expectations. I will show that these previous analyses were flawed, and that the data is in fact consistent with the expectation of an almost uniform 1 and 4 Rydberg background at z~2.5. Finally, I will discuss whether the EUV background affects galaxy formation, as has been speculated. Unfortunately, all does not end well for the cosmic EUV.

Multi-wavelength analysis of supernova remnant MSH11-61A

Katie Auchettl
(CfA Harvard)

Due to its centrally bright X-ray morphology and limb brightened radio profile, Galactic supernova remnant MSH 11-61A (G290.1-0.8) is classified as mixed morphology. HI and CO observations have determined that the SNR is interacting with a molecular cloud found towards the north and southwest regions of the remnant. As observations of thermal and non-thermal emission of SNRs have provided increasing support in favour of cosmic rays being accelerated at its shock front, SNRs known to be interacting with molecular clouds provide an effective target for detecting and studying the production of gamma-rays from the decay of a neutral pion into two gamma-ray photons. I report on the detection of gamma-ray emission coincident with MSH 11-61A using 70 months of data from the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. To investigate the origin of this emission, we perform broadband modelling of its non-thermal emission considering both leptonic and hadronic cases and concluding that the gamma-ray emission is most likely hadronic in nature. Additionally we also present our analysis of an archival Suzaku observation of this remnant. Our investigation shows that the X-ray emission of MSH 11-61A arises from a two temperature component plasma consisting of a hot, ejecta-rich plasma that is still ionising and a cool, recombining ISM component.

The Extragalactic Gamma-ray Background
Searching for Satellite Galaxies of the Milky Way in the Dark Energy Survey

Keith Bechtol

Part 1: The extragalactic gamma-ray background (EGB) is generated by the superposition of all extragalactic gamma-ray emissions and thus provides a window on both the demographics and evolution of non-thermal phenomena across cosmic time. A significant fraction of the total EGB intensity has now been resolved into individual sources using the Fermi LAT, and there is an emerging understanding of how fainter members of the established extragalactic gamma-ray source classes can account for the residual approximately isotropic component of the gamma-ray sky, called the isotropic gamma-ray background (IGRB). The latest measurement of the IGRB spectrum with the Fermi LAT from 100 MeV to 820 GeV exhibits a high-energy cutoff feature consistent with the attenuation of high-energy gamma rays by pair-production on the IR/optical/UV extragalactic background light. High-energy cosmic neutrinos will be essential to see beyond this gamma-ray horizon to greater distances and higher energies.

Part 2: Searches for indirect dark matter signals in the direction of Milky Way satellite galaxies provide some of the strongest constraints on the annihilation cross section of dark matter derived from gamma-ray observations. Milky Way satellite galaxies have the advantages of low astrophysical backgrounds, the ability to constrain the dark matter abundance and distribution from the kinematics of member stars, and the opportunity to combine observations of multiple satellites in a joint-likelihood framework to increase sensitivity. The discovery of additional Milky Way satellites in wide-field optical imaging surveys may provide substantial advances for indirect dark matter searches. I will discuss a matched-filter maximum-likelihood algorithm to search for and characterize ultra-faint galaxies in the ongoing Dark Energy Survey, which will cover 5000 square degrees in the relatively less explored south Galactic cap.

Studying the Expansion of the Universe with BOSS quasars

Andreu Font-Ribera
(Lawrence Berkeley National Lab)

After six years of observations, the Baryon Oscillation Spectroscopic Survey (BOSS) ended last summer, and will soon make its data public (SDSS Data Release 12). During these years, it has used the SDSS telescope to obtain spectra of 1.5 million galaxies to get very accurate measurements of the Baryon Acoustic Oscillations (BAO) scale at redshift z ~0.5. At the same time, BOSS observed over 184 000 high redshift quasars (z>2.15) with the goal of detecting the BAO feature in the clustering of the intergalactic medium, using a technique known as the Lyman alpha forest (LyaF). In this talk I will overview several results from the LyaF working group in BOSS, including the measurement of BAO at z=2.4 both from the auto-correlation of the LyaF (Delubac et al. 2014), and from its cross-correlation with quasars (Font-Ribera et al. 2014). From the combination of these studies we are able to measure the expansion rate of the Universe 11 billion years ago with a 2% uncertainty.

Relation Between Galaxy Cluster Optical Richness and SZ Effect

Neelima Sehgal

Accurate galaxy cluster masses are important for their use as precision cosmological probes. Measuring the SZ effect and optical richness of clusters are two methods used to estimate cluster masses, and thus it is natural to ask whether these methods yield consistent results. Using data from the Atacama Cosmology Telescope (ACT) to measure the SZ effect, we test the consistency of the two methods. We find that the SZ flux from the Max-BCG optically-selected cluster sample is both lower than expected from the richness-mass relation, and lower than measured by the Planck satellite. Possible implications of these results will be discussed.

Sterile neutrino dark matter: the 3.5keV line and galaxy formation

Mark Lovell
(GRAPPA, Amsterdam)

The non-detection to date of any supersymmetric particles at the LHC, coupled with the large measured value of the Higgs boson, has increased interest in dark matter candidates other than the LSP. One such particle is the keV sterile neutrino, which forms part of a theory that may also explain the masses of known neutrinos and baryogenesis. Further motivation for this hypothesis has come from multiple claimed detections of an X-ray line at 3.5keV in the spectra of clusters of galaxies, M31 and the Galactic centre, which could be produced the decay of sterile neutrino dark matter. In this talk I will discuss the progress of work on the 3.5keV line by use of dark matter halo simulations, and also discuss the consequences of sterile neutrino dark matter for galaxy formation.

Baryons Matter! Challenges and Solutions to LambdaCDM on small scales

Adi Zolotov

The observed properties of dwarf galaxies have raised several notable challenges to the favored Lambda+Cold Dark Matter (CDM) cosmological model. Using some of the highest resolution cosmological galaxy simulations ever produced that include both baryons and dark matter, I will show that baryonic processes can significantly alter the dark matter structure of galaxies, thereby alleviating some of the most worrying tension between observations and the predictions of the CDM model. In particular, I will show that energetic feedback from supernovae and subsequent tidal stripping after infall both significantly reduce the dark matter mass in the central regions of dwarf satellites. I will discuss how the reduced central masses of dwarf satellites resolve three important challenges to the CDM model on small scales by i) reproducing the observed internal dynamics of Milky Way and M31 satellites as a function of luminosity, ii) resolving the cusp/core problem, and iii) resolving the missing satellite problem at the massive end.

Making Robust and Precise Physical Measurements Using Galaxy Surveys

Ashley Ross

What is the nature of Dark Energy? Is General Relativity a correct description of gravity on the largest scales? What is the mass of neutrinos? What is the physical mechanism that seeded the formation of structure in the Universe? These fundamental questions can be addressed by analyzing the clustering of galaxies and I will explain how using examples of measurements made using the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS). I will describe the BOSS galaxy data, the methods used to measure the clustering of BOSS galaxies, and how the most recent clustering measurements have allowed a measurement of the distance to BOSS galaxies to within 1% precision. I will further describe systematic concerns related to the analysis of galaxy clustering data, and the methods and measurements that have been developed to ameliorate these concerns and ensure the robustness of BOSS results. If time allows, I will conclude with a discussion of just-beginning and future surveys, such as DES, eBOSS, and DESI.

On verifying photometric redshift distributions using cross correlations with spectroscopic galaxy surveys

Ami Choi

Cosmological parameter estimation often relies on highly accurate knowledge of the 3-D spatial distribution of the galaxies used in the analysis. Techniques that calibrate redshift distributions by exploiting the physical clustering of galaxies have recently become quite popular as a means of achieving the precision required by LSST and Euclid but have not been tested extensively on existing data sets. I will present measurements of the angular cross-clustering between several combinations of overlapping spectroscopic and photometric surveys (e.g. BOSS/CFHTLenS, WiggleZ/RCS2) as well as comparisons with a model that incorporates both intrinsic clustering and lensing magnification. While a valuable signal in its own right, magnification may also play the role of contaminant in future analyses seeking to recover underlying redshift distributions via cross-correlation clustering and cannot be ignored. Time permitting, I will also report on recent progress and scientific endeavors with the Kilo-Degree Survey (KiDS), an ongoing 1500 sq. deg. survey on the European Southern Observatory's VLT Survey Telescope.

Rethinking Galactic Architecture: Clues from Satellites and Destroyed Dwarfs

Alis Deason

The cannibalistic nature of the Milky Way galaxy leads to the continuous capture and destruction of lower-mass, dwarf galaxies. The remains of destroyed dwarfs are splayed out in a diffuse stellar halo, while the "survivors" comprise the satellite population that orbits the Milky Way. These halo populations provide a unique opportunity to decipher the accretion history of the Milky Way with a level of detail that cannot be achieved in any other galaxy. I will discuss current and future projects aiming to decipher the nature of the halo's building blocks. At present, we have very little understanding of what these building blocks actually are; is the halo built up from many smaller mass dwarfs, or from one massive dwarf? I will discuss recent work comparing the results from halo star counts in SDSS with numerical simulations. This work suggests that the halo may be dominated by one massive accretion event and/or experienced a very short accretion epoch. An ongoing project utilizing multi-epoch HST photometry and Keck spectroscopy will help provide a quantitative analysis of the mass spectrum of dwarfs that built up the halo, and potentially disentangle these two scenarios. I will also discuss the "satellites of satellites" population in the Milky Way. I will present recent results suggesting that the PAndAS stream, the Segue 2 satellite (the "least luminous" galaxy) and the large TriAnd overdensity are all associated, and may be a fossil record of group-infall onto the Milky Way halo. We generally ignore the possibility that the lowest luminosity dwarfs in the Milky Way may be satellites of other satellites, and thus, we may be grossly misinterpreting their properties. Finally, I will outline the future prospects to identify associations of substructures in the Milky Way halo.

Tiny bubbles in the Mine: New Results From Bubble Chamber Dark Matter Searches at SNOLAB

Eric Dahl
(Northwestern U)

The nature of dark matter is one of the greatest mysteries in physics today, spanning astrophysics, cosmology, and particle physics. While astrophysicists search for signs of dark matter annihilation in our galactic neighborhood, and collider physicists look for indications of dark matter production in the LHC, direct detection experiments are making great strides looking for dark matter interactions in detectors deep underground. This progress comes in part from ever-larger detectors, but with the increased exposure comes an increasingly stringent limit on allowed backgrounds from natural radioactivity. The bubble chambers operated by the PICO (formerly COUPP) collaboration are an incredibly powerful tool to wipe out the beta-decay and gamma-interaction backgrounds that plague other direct detection experiments, and have repeatedly set world-leading limits on the spin-dependent WIMP-proton cross section. I will present results from the latest PICO physics run at SNOLAB, and will describe a new aspect of this technology that may produce world-leading discrimination against all radioactivity-induced backgrounds, leading to increased sensitivity and, with luck, a dark matter discovery.

Advancing High-Energy Neutrino Physics with Antarctic Detectors

Jordan Hanson
(U of Kansas)

The Antarctic Ross Ice Shelf Antenna Neutrino Array (ARIANNA) prototype detector, known as the Hexagonal Radio Array, is now complete. ARIANNA is designed to detect cosmogenic neutrinos from the GZK process, and other high-energy astrophysical models, via the Askaryan effect in Antarctic ice sheets. A significant sample of these neutrinos would provide a wealth of information about the high-energy universe, from distances exceeding the range of other astronomical messenger particles. These interactions would also advance our understanding of deep inelastic scattering, parton distribution functions, and probe new physics such as Lorentz invariance violation (LIV). The design and development, data analysis, and sensitivity of ARIANNA will be described, taking into account theoretical modeling of the Askaryan effect and ice properties. Finally, theoretical questions answerable by future ARIANNA data sets will be discussed.

Cosmic Flows: cosmology and astrophysics from galaxy velocities

Simone Ferraro

Velocity fields are a powerful probe of structure formation and the energy content of our Universe. Additionally, the motion of ionized gas on intermediate scales can be used to measure the clustering of baryons and shed light on galaxy formation and feedback mechanisms. I will discuss techniques that can be used to both constrain cosmology and measure baryon properties. I will also present some preliminary results.

Precision Cosmology with Cosmic Voids

Alice Pisani (IAP)

Modern surveys allow us to access to high quality measurements, by sampling the galaxy distribution in detail also in the emptier regions, voids. Cosmic voids present themselves as a new tool to constrain cosmology. While the treatment of systematics is simpler in these empty regions, with the aim of achieving the level of precision cosmology a careful modeling of such effects is necessary. In particular, peculiar velocities affect the way we observe cosmic voids, and thus their effect needs to be understood. Using mock catalogues, I analyse the effect of peculiar velocities on void properties. In this talk I thus present the results of the analysis of the systematic effects affecting voids and discuss it in the framework of current and future surveys. Additionally, I present a preliminary forecast for void abundances with the future Euclid and Wfirst missions and obtain, using the Fisher matrix formalism, a prediction for the constraints that void abundances will set on cosmological parameters.


The Characterization of the Gamma-Ray Signal from the Central Milky Way:
A Compelling Case for Annihilating Dark Matter

Tim Linden

In scenarios where dark matter particles can annihilate to produce standard model particles, the galactic center of the Milky Way is expected to provide the highest flux from dark matter in the sky. This has allowed galactic center observations to set extremely stringent limits on the parameters of the dark matter particle. Recently, we have worked on gamma-ray observations from the Fermi-LAT telescope, and have detected a significant extended excess, which is spherically symmetric around the position of the galactic center, and does not trace any known astrophysical emission profile. In this talk, I will summarize the current status of these observations and discuss dark matter and astrophysical interpretations of the data. I will show forthcoming results which strongly constrain the properties and the possible interpretations of the observed excess. Finally, I will posit upcoming tests which will strongly suggest, or rule out, a dark matter interpretation.


Voids and Scaling in the Halo Model

Jim Fry

The popular halo model has implications that go beyond its usual applications to the galaxy autocorrelation function or power spectrum. I will examine how the model holds up in its predictions for higher order statistics of both mass and galaxy number, and I will revisit the hierarchical scaling behavior of void probabilities.

fermi bubbles

The Fermi Bubbles and Future Gamma-ray Telescopes

Meng Su

The Fermi Bubbles are a pair of giant lobes at the heart of the Milky Way, extending roughly 50 degrees north and south of the Galactic Center, and emitting photons with energies up to 100 GeV. This previously unknown structure could be evidence for past activity of the central supermassive black hole. I will outline the current state of the multiwavelength observations of this structure, and discuss theoretical proposals and numerical simulations for their nature and origin. The Fermi Bubbles was discovered using data from the successful Fermi Gamma-ray Space Telescope, which has proved the great potential of studying astrophysics, cosmology, and fundamental physics in high energy gamma rays. I will talk about three future gamma-ray missions: DAMPE, HERD, and PANGU, and comment on what science could be learned from these future missions.

h258 galaxy

Scrutinizing the Relationship Between Galaxies and Supermassive Black Holes

Jillian Bellovary

Supermassive black holes (SMBHs) have a ubiquitous presence in massive galaxies, but their formation and evolutionary history remain mysteries. One of the strongest observed trends between SMBHs and their host galaxies is the tight relation between black hole mass and the velocity dispersion of the stellar spheroid (aka the M-Sigma relation). While this relation hints at a fundamental link between galaxy and SMBH growth, there are also some challenges regarding scatter and outliers. I will present evidence that the M-Sigma relation is not the clear-cut trend it seems to be; for example, the orientation of galaxies on the sky affects the value of velocity dispersion by up to 30%. Additionally, the existence of SMBHs in dwarf galaxies and galaxies without spheroids challenges the standard paradigm of SMBH-galaxy coevolution. I will offer some alternative methods of forming and growing SMBHs which can provide explanations for these puzzling outliers.

Radio and X-ray Studies of Type II-P Supernovae:
What They Reveal About the Parents

Alak Ray
(Tata Institute)

I will describe our ongoing work on studying X-ray and radio emission from a class of supernovae that forms almost half of all core collapse supernovae, namely type II Plateau SNe. We have carried out these with Chandra, EVLA and GMRT telescopes. Because these bands probe the interaction of the SN with the medium it exploded in, they provide valuable information about the star that exploded and the nature of the medium. Our Chandra observations of SN 2004dj for the first time measured the separate contributions of thermal emission from the SN shocks and the power-law nonthermal part arising out of accelerated particles. For this and a few other SNe the combination of radio and X-ray measurements indicate the extent of equipartition between magnetic fields amplified by the shock and the relativistic particles accelerated by it.

detectors in line

Chasing our Cosmic Dawn: Opening the 21cm cosmological window on the universe

Danny Jacobs
(Arizona State)

The Epoch of Reionization (EoR) marks when the first stars ionized the primordial hydrogen half a billion years after the big bang. Direct observation of cosmological hydrogen is possible via the 21cm line and is now being hotly pursued as a new cosmological probe. Danny Jacobs is helping to lead observations with both the Precision Array for Probing the Epoch of Reionization (PAPER) and the Murchison Widefield Array (MWA). PAPER currently holds the deepest limits on the epoch of reionization power spectrum, while the MWA is leading the charge towards understanding foregrounds at a level necessary for imaging large scale structure. The two intertwined themes in these new instruments are the degree to which experimentation is an essential component of the science process and the ascendance of the software pipeline. Experiments currently under-way to refine array sensitivity include high-bandwidth forward-modeling of instrumental response, developing high level heuristics for data flagging, accelerating imaging pipelines, pushing more analysis steps into real-time systems, and in-situ calibration with external drone-mounted transmitters. Lessons learned and systems developed for PAPER and the MWA are being incorporated into the next generation Hydrogen Epoch of Reionization Array (HERA) that will yield 20 times the sensitivity of first generation arrays and also into the upcoming Square Kilometer Array.

telescope to galaxy view

Shedding Light on Distant Galaxies with ~400,000 SDSS Quasars

Britt Lundgren
(UW Madison)

Distant quasars backlight the Universe over most of cosmic time, revealing the evolving gas distribution of the cosmic web. Intervening metal absorption lines in quasar spectra can provide sensitive tracers of the gaseous processes regulating star formation in foreground galaxies to high redshift, but observational difficulties have traditionally limited comparisons to the stellar properties of the absorbing galaxies. The extraction and statistical analysis of absorption line systems from 377,809 unique quasar spectra in the Sloan Digital Sky Survey (SDSS I-III) has recently catalyzed our understanding of the physical environments of the most prolific metal absorption species (e.g., Mg II, C IV) observed in optical quasar spectra. I will present recent stacking and clustering measurements made possible by the vast quasar absorption line samples from the SDSS, and present new, direct observations of Mg II absorber host galaxies at high redshift using the Hubble Space Telescope. Together these studies reveal compelling links between strong Mg II absorbers and large-scale star formation-driven outflows, providing insights into the role of feedback in the evolution of galaxies from z~2.

The Role of Dwarf-Dwarf Interactions in the Evolution of Low Mass Galaxies

Sabrina Stierwalt

I will present the initial results from TiNy Titans, the first systematic study a sample of interacting dwarf galaxies and the mechanisms governing their star formation. Mergers of massive galaxies provide a significant mode of galaxy evolution and are observed to inspire intense starbursts and significant rearranging of the galaxies' gas and dust. However, despite the fact that mergers among low mass galaxies outnumber those between massive ones, whether these effects occur in the shallower gravitational potential wells of dwarf galaxies remains completely unconstrained. A few intriguing examples of dwarf-dwarf interactions exist in the literature, but the efficiency of gas removal and the enhancement of star formation in dwarfs via pre-processing (i.e. dwarf-dwarf interactions occurring before the accretion by a massive host) has never been studied for a uniformly selected sample of dwarfs. Our multiwavelength approach gathers high resolution optical, UV, and radio imaging to probe the effects of interactions on the star formation and ISM in a complete sample of dwarf pairs selected from the Sloan Digital Sky Survey. We find star formation is enhanced in paired dwarfs over isolated dwarfs to an even greater extent than is observed in massive galaxies, but the dwarfs involved in interactions still have large gas reservoirs (and thus capacity for future star formation). Our interacting dwarfs tend to be low metallicity and thus offer a unique window into modes of star formation that were important at earlier epochs.

It's Always Darkest Before the Cosmic Dawn

Josh Dillon

Realizing the promise of 21 cm cosmology to provide an exquisite probe of astrophysics and cosmology during the cosmic dark ages and the epoch of reionization has proven extremely challenging. We're looking for a small signal buried under foregrounds orders of magnitude stronger. We know that we're going to need very sensitive, and thus very large, low frequency interferometers, which present their own set of difficulties. And, as I will explain, we're going to need a rigorous statistical analysis of the maps we make to extract interesting cosmological information. I will discuss the steps we've taken to overcome these obstacles with early data from the Murchison Widefield Array by isolating foregrounds to a region of Fourier space outside a clean "epoch of reionization window." Additionally, I will present some of most recent and exciting predictions for what 21 cm cosmology can tell us as we move to larger telescopes like the Hydrogen Epoch of Reionization Array and higher redshifts.

On Neutrino Decay and Other Non-Unitary Effects on Neutrino Propagation

Andre de Gouvea
(Northwestern U)

After providing a brief overview of the neutrino physics landscape - what we know and what we know we don't know - I discuss in some detail the possibility that neutrino propagation is not unitary, e.g., the neutrinos could, generically, decay, and review what is currently known about the lifetime of the different neutrino mass-eigenstates.

Primordial non-Gaussianity in the CMB and Large-Scale Structure

Kendrick Smith
(Perimeter Inst)

I'll give a pedagogical review of inflation and explain how its physics can be constrained by searching for "primordial non-Gaussianity", i.e. differences between the statistics of the initial curvature field in our universe and the statistics of an ideal Gaussian field. Then I'll talk about observational CMB constraints, including some new results from Planck. Finally I'll discuss future prospects for improving Planck constraints with large-scale surveys such as Euclid and LSST.

The Zen of Core Collapse: How to See A Supernova That Doesn't Happen

Elizabeth Lovegrove

It now seems likely that stars over 8 solar masses, rather than all exploding as some form of core-collapse supernova, have a range of explosion probabilities that depend on mass. Different masses of progenitor may explode with regular CCSNe energies, explode with much lower energies, or fail to explode entirely. Narrowing down these possible outcomes and associating them with stellar masses is important to galactic evolution models and a key step in achieving accurate end-to-end core-collapse simulations. But making progress on this question requires a large sample of observed supernova progenitors, and these are hard to come by. True observational limits, too, require being able to see not only supernovae that happen but also supernovae that don't. In this talk I will present and discuss results from the CASTRO simulation code on both transients from completely-failed supernovae as well as shock breakouts from faint supernovae, a promising channel for retrieving progenitor information.

Exploring the Third Dimension:
Spectroscopic Needs for Imaging Dark Energy Experiments?

Jefferey Newman

This talk will explore a number of applications of wide-area spectroscopic surveys, such as those which the Dark Energy Spectroscopic Instrument (DESI) will enable, to solving key problems for imaging dark energy experiments. First, I will discuss the problem of photometric redshifts (a.k.a. photo-z's): i.e., estimates of the redshifts of objects based only on flux information obtained through broad filters. Higher-quality, lower-scatter photo-z's will result in smaller random errors on cosmological parameters; while systematic errors in photometric redshift estimates, if not constrained, may dominate all other uncertainties from these experiments. In this talk, I will describe the key challenges for training and calibrating photometric redshift algorithms in the next two decades, and describe how DESI can help us address these challenges. Second, I will discuss the contributions the DESI instrument can make to LSST supernova studies by measuring spectroscopic redshifts for large samples of supernova hosts, which would require comparatively modest time allocations. Finally, I will describe the LSST Dark Energy Science Collaboration, highlighting how all of us can get involved now in preparing for this extraordinarily rich imaging dataset.

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The Cosmic Laboratory: Probing Fundamental Physics with Large-Scale Structure and the CMB

Roland de Putter

In the current era of precision cosmology, the Universe on large scales has become a unique probe of many fundamental physics questions that are hard or even impossible to address with conventional terrestrial experiments. In this seminar, I will discuss examples of what this "Cosmic Laboratory" teaches us about neutrino physics, inflation, dark matter and dark energy. I will discuss the following two topics in particular detail. First, I will discuss how currently, and for the foreseeable future, cosmology places the tightest bounds on the absolute mass scale of neutrinos. I will pay specific attention to the robustness of these bounds with respect to assumptions about the primordial power spectrum and thus inflation. Secondly, I will explain what it would take for a galaxy survey to use primordial non-Gaussianity to distinguish between single-field and multi-field inflation and I will introduce a specific proposal for such a survey, called SPHEREx.

Observational Tests of Cosmic-ray Diffusion in the Magellanic Clouds

Laura Lopez
(OSU Astronomy)

Cosmic rays (CRs) play an important role in the interstellar medium: they ionize dense molecular gas, they are responsible for the light elements in the periodic table, and they account for 20% of the ISM energy budget. However, the means by which CRs are first accelerated and then transported through external galaxies are not well understood. I will present results from a recent study of the Magellanic Clouds to constrain CR transport using Fermi gamma-ray observations. I will show how we have characterized the spatial distribution of gamma rays in the LMC and SMC and used the findings, in conjunction with available multiwavelength data, to constrain CR transport based on how the emission depends on physical parameters, such as gas density, massive star formation, magnetic field structure, and turbulence properties.

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Searching for Dark Matter with Gamma Rays

Andrea Albert

There is overwhelming evidence that non-baryonic dark matter constitutes ~27% of the energy density of the Universe. Weakly Interacting Massive Particles (WIMPs) are promising dark matter candidates that may produce gamma rays via annihilation or decay in the Universe. A detection of gamma rays from WIMPs would not only confirm the existence of dark matter through a non-gravitational force, but also indicate the existence of physics beyond the Standard Model. I will present recent Fermi-LAT Collaboration results from WIMP searches including looking for gamma-ray spectral lines and gamma-ray excesses in areas of large dark matter concentration like the Galactic center and dwarf spheroidal galaxies.

Interpretation of IceCube results in the multi-messenger context

Walter Winter
(DESY Zeuthen, Germany)

The discovery of high-energetic cosmic neutrinos is one of the recent major breakthroughs in science. We discuss the concept of the neutrino production, and interpret recent results taking into account the information from other messengers (gamma-rays, cosmic rays). For example, one question is if these neutrinos come from the most powerful accelerators in the universe, i.e., the ones which can accelerate cosmic rays to the highest observed energies. We also discuss future perspectives for neutrino astronomy.

The PAU Survey at the William Herschel Telescope

Ignacio Sevilla

We present PAUCam: a multi-narrow band camera designed to conduct a photometric survey from the 4m William Herschel Telescope, starting this year. The scientific goals (which include intrinsic galaxy alignments, magnification and redshift space distortions), camera design and current status will be described.

The future of weak gravitational lensing in cosmology

Ludo van Waerbeke

Gravitational lensing by large scale structures is poised to play a central role in the future of precision cosmology, to help constraining modified theories of gravity, the neutrino mass, quantifying the dark energy equation of state and a lot more. It is quite possible however that gravitational lensing will first shed light on some of the complex astrophysical processes taking place in galaxy and galaxy cluster formation, before it can reach the high precision needed for dark energy and modified gravity tests. After a short introduction of the basic concepts and ideas, I will discuss some of the recent and most promising developments and what challenges lie ahead for future surveys such as LSST, Euclid or WFIRST.

New Physics at IceCube

Bhupal Dev
(U. of Manchester)

The recent observation of ultra-high energy neutrino events at IceCube has spurred a lot of interest in the scientific community. From a particle physics viewpoint, several exotic phenomena have been proposed to explain the data. For a reliable interpretation, it is however important to first scrutinize the Standard Model (SM) expectations carefully, including all known theoretical and experimental uncertainties. In this talk, we discuss the compatibility of the 3-year IceCube dataset with some well-motivated flavor and spectral compositions of the astrophysical flux within the SM framework, and show that the SM interactions are sufficient to explain the current data within the known uncertainties. Using this result, we can derive constraints on some New Physics scenarios, which are otherwise difficult to probe at the LHC or other existing low-energy experiments.

Cosmological Constraints on Newton's Gravitational Constant for Matter and Dark Matter

Jordi Salvado
(UW Madison)

In this talk I will present a study using cosmological data of the gravitational interaction in ordinary and dark matter sectors. In the first part I will present a new constraint of Newton's gravitational constant by making use of the latest CMB data from the Planck experiment and independent constraints coming from Big Bang Nucleosynthesis and low redshift experiments. In the second part of the talk I will focus on the dark matter sector, giving a constraint to the dark matter equivalence principle and long-range fifth forces.

The Fermi Galactic Center excess

Ilias Cholis

The possible gamma-ray excess in the inner Galaxy and the Galactic center suggested by Fermi-LAT observations has triggered great interest in the astro-particle physics community. Among its various interpretations have been WIMP dark matter annihilations, gamma-ray emission from a population of millisecond pulsars, or emission from cosmic rays injected in a sequence of burst-like events or continuously at the GC. Given that the galactic diffuse emission is the dominant (by an order of magnitude or more) at any direction greater than 2 degrees from the GC understanding the background systematics has been a vital missing piece in the discussion. I will present the first comprehensive study of model systematics coming from the Galactic diffuse emission in the inner part of our Galaxy and their impact on the inferred properties of the excess emission at Galactic latitudes between 2 and 20 degrees and energies 300 MeV to 500 GeV. I will show both theoretical and empirical model systematics, which are deduced from a large range of Galactic diffuse emission models and a principal component analysis of residuals in numerous test regions along the Galactic plane. The hypothesis of an extended spherical excess emission with a uniform energy spectrum is compatible with the Fermi-LAT data in the region of interest at 95% CL. Assuming that this excess is the extended counterpart of the one seen in the inner few degrees of the Galaxy, a lower limit of 10 degrees (95% CL) can be derived on its extension away from the GC. In light of the large correlated uncertainties that affect the subtraction of the Galactic diffuse emission in the relevant regions, the energy spectrum of the excess is equally compatible with both a simple broken power-law of break energy 2.1 $\pm$ 0.2 and with spectra predicted by the self-annihilation of dark matter, implying in the case of $\bar{b}b$ final states a dark matter mass of 49$^{+6.4}_{-5.4}$ GeV. I will also briefly discuss interpretations of this excess, based on annihilating DM, leptonic CR outburst and a population of millisecond pulsars.

Simulating Massive Neutrinos

Simeon Bird

Massive neutrinos make up a fraction of the dark matter, but due to their large thermal velocities, cluster significantly less than cold dark matter (CDM) on small scales. An accurate theoretical modelling of their effect on structure formation is required to fully exploit large-scale structure data. I will discuss different methods to add neutrinos to cosmological simulations, finishing with one which is accurate for current cosmological mass bounds and requires minimal extra computational cost. I will then talk about the impact of neutrino masses on cluster counts and perhaps the Lyman-alpha forest.

Gravitational Signals from Noise in the Hubble Diagram

Edward Macaulay
(Univ of Queensland)

Understanding the nature of the dark universe requires precise measurements of the background expansion history, and also the growth rate of density fluctuations. In this talk, I'll consider both regimes with supernova lensing for the OzDES spectroscopic survey - which is measuring the redshifts of hundreds of supernova and thousands of galaxies identified by the Dark Energy Survey. I'll start by reviewing the more established method of growth rate measurements with Redshift Space Distortions, and discuss possible tension between RSDs and expectations from Planck CMB measurements. I'll then consider how OzDES can place novel constraints on the growth rate and amplitude of density fluctuations by correlating noise in the supernova Hubble diagram with the gravitational effects of lensing and peculiar velocities expected from the observed density field.

Not with a Bang, but a Whimper: Evidence for Low-energy Supernovae

Scott Adams

I will present new HST and Spitzer late-time imaging of SN 2008S and NGC 300-OT, the prototypes of a class of stellar transients whose true nature is debated. Both objects have faded below the luminosity of their progenitors and are now undetected in both the near and mid-IR, providing strong evidence that these events were terminal. This, combined with the mass constraints on the progenitors, indicates that this class of transients likely arise from electron-capture supernovae.

Indirect Detection of Dark Matter Using MeV-Range Gamma-Ray Telescopes

Kimberly Boddy

The astrophysics community is considering plans for a variety of gamma-ray telescopes in the energy range 1--100 MeV, which can fill in the so-called "MeV gap" in current sensitivity. We investigate the utility of such detectors for the study of low-mass dark matter annihilation or decay. For annihilating (decaying) dark matter with a mass below about 140 MeV (280 MeV) and couplings to first generation quarks, the final states will be dominated by photons or neutral pions, producing striking signals in gamma-ray telescopes. We determine the sensitivity of future detectors to the kinematically allowed final states. In particular, we find that planned detectors can improve on current sensitivity to this class of models by up to a few orders of magnitude.

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Weighing the Giants: Anchoring Galaxy Cluster Cosmology

Adam Mantz
(KICP Chicago)

The gas mass fractions and the distribution in mass and redshift of the galaxy cluster population provide powerful probes of cosmology, constraining the cosmic matter density, the amplitude of the matter power spectrum, properties of dark energy, and the mass of neutrinos, among other parameters. Historically, these tests have been limited by the absolute accuracy of cluster mass determinations. Here, mass measurements from weak lensing have an advantage over estimates based on observations of the intracluster medium (ICM), because the former are nearly unbiased and can be straightforwardly tested against simulations. I will describe recent cosmological constraints obtained from an analysis of X-ray selected cluster samples, incorporating extensive gravitational lensing data from the Weighing the Giants project -- the first cluster cosmology study to consistently integrate a lensing mass calibration, including a rigorous quantification of all systematic uncertainties. The results highlight the power and potential of galaxy clusters, which constrain both the expansion of the Universe and the growth of cosmic structure, and their complementarity with other probes such as type Ia supernovae, large-scale galaxy surveys, and the cosmic microwave background.

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Probing the nature of AGN coronae through future X-ray and sub-mm observations

Yoshiyuki Inoue

While the cosmic X-ray background is likely to originate from individual AGNs, the origin of the cosmic MeV gamma-ray background is not fully understood. We proposed that AGNs having non-thermal electrons in coronae may explain the MeV background. Such non-thermal electrons are expected to exist if a corona is heated by magnetic reconnections. However, the sensitivity of current MeV gamma-ray instrument is not sufficiently good to detect the expected power-law tail in the MeV band from individual AGNs. Furthermore, the heating mechanism of coronae in AGNs is still unknown, although magnetic reconnection heating is one possibility. In this talk, I would like to introduce how we can probe the origin of the MeV background and the nature of AGN coronae such as magnetic field and non-thermal content through future observations by ASTRO-H and ALMA.

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High energy neutrinos from extra-galactic astrophysical sources

Irene Tamborra

The IceCube neutrino telescope recently discovered a flux of astrophysical neutrinos with energies up to few PeV. In light of the new born high-energy neutrino astronomy era, I will discuss the expected high-energy neutrino emission from extra-galactic astrophysical sources as well as our chances to unveil the physics of the cosmic accelerators by employing neutrinos and their photon counterparts.

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