The morning discussion section will take place in Smith Laboratory 1005, which is next door to the Physics Research Building.

Lunch break on your own. There are a number of nice restaurants near the Ohio State campus.

The afternoon discussion section will take place in Smith Laboratory 1005, which is next door to the Physics Research Building.

The morning discussion section will take place in Physics Research Building 4138.

Lunch break on your own. There are a number of nice restaurants near the Ohio State campus.

The afternoon discussion section will take place in Physics Research Building 4138.

The morning discussion section will take place in Smith Laboratory 1005, which is next door to the Physics Research Building.

Lunch break on your own. There are a number of nice restaurants near the Ohio State campus.

The afternoon discussion section will take place in Smith Laboratory 1076, which is next door to the Physics Research Building.

The morning discussion section will take place in the Smith Seminar Room in the Physics Research Building.

Lunch break on your own. There are a number of nice restaurants near the Ohio State campus.

The afternoon discussion section will take place in the Smith Seminar Room in the Physics Research Building.

The morning discussion section will take place in the Physics Research Building M2015.

Lunch break on your own. There are a number of nice restaurants near the Ohio State campus.

The afternoon discussion section will take place in the Physics Research Building M2015.

The morning discussion section will take place in the Price Place in the Physics Research Building.

Lunch break on your own. There are a number of nice restaurants near the Ohio State campus.

The afternoon discussion section will take place in the Price Place in the Physics Research Building.

Strong gravitational lensing provides a means of measuring the halo mass function into regimes below which baryons are reliable tracers of structure. In this low mass regime (M_vir<10^9 M_sun), the microscopic characteristics of dark matter affect the predicted abundance of dark matter halos. Strong gravitational lensing has been limited by the small number of systems which can be used to detect dark matter substructure. I will discuss the narrow-line lensing technique, which enables a significant increase in the number of systems which can be used to measure the subhalo mass function, and the projected constraint on Cold vs. Warm Dark Matter with just the current sample of known strong gravitational lenses.

Astrometry in the Gaia era will give an unprecedented amount of information about the full 6D phase space distribution of the local galactic halo. In this talk, I will use an analysis of vertical motions to show how the Gaia data will be sensitive to the presence of structures including dark disks (either from novel dark matter microphysics or from baryonic dragging.)

We present our first results from a deep LBT survey of dwarf satellites of nearby star-forming galaxies outside the local group. We present our candidates and report the number and distribution of satellites for our first system. We are sensitive to deep within the ultra faint dwarf and ultra diffuse galaxy regime outside. We discuss the implications of these new observations on the dark matter halo distribution function and dark matter models.

Deep optical imaging surveys have revealed a population of extremely low luminosity and dark matter dominated galaxies orbiting the Milky Way. The total number of Milky Way satellite galaxies and the demographics of this population are still largely unknown, in part, because of complex selection effects that limit our ability to detect the lowest surface brightness galaxies. The Dark Energy Survey (DES) has now finished a complete reprocessing of data from the first three observing seasons, yielding a dataset with substantially improved depth, homogeneity, and photometric precision. We will describe progress towards a more robust statistical search for Milky Way satellite galaxies in DES data with the ultimate goal of constraining the luminosity function of the faintest galaxies as a test of galaxy formation and dark matter physics.

We identify new astrophysical signatures of NS-imploding DM, which could decisively test these hypotheses in the next few years. First, NS-imploding DM forms ≪10−10 solar mass black holes inside NSs, thereby converting NSs into ∼1.5 solar mass BHs. This decreases the number of NS mergers seen by LIGO/VIRGO (LV) and associated merger kilonovae seen by telescopes like DES, BlackGEM, and ZTF, instead producing a population of "black mergers" containing ∼1.5 solar mass black holes. Second, DM-induced NS implosions create a new kind of kilonovae that lacks a detectable, accompanying gravitational signal. Using DES data and the Milky Way's r-process abundance, we set bounds on these DM-initiated "quiet-kilonovae." Third, the spatial distribution of merger kilonovae, quiet kilonovae, and fast radio bursts in galaxies can be used to detect dark matter. NS-imploding DM destroys most NSs at the centers of mature disc galaxies, so that NS merger kilonovae would appear mostly in a donut at large radii. We find that as few as ten NS merger kilonova events, located to ∼1 kpc precision could validate or exclude DM-induced NS implosions at 2σ confidence, exploring DM-nucleon cross-sections over an order of magnitude below current limits. Similarly, NS-imploding dark matter as the source of fast radio bursts can be tested at 2σ confidence once 20 bursts are located in host galaxies by radio arrays like CHIME and HIRAX. URL: https://arxiv.org/abs/1706.00001 I am also submitting an abstract to the track Particle Physics.

A largely model-independent probe of dark matter-nucleon interactions is proposed. Accelerated by gravity to relativistic speeds, local dark matter scattering against old neutron stars deposits kinetic energy that heats them to infrared blackbody temperatures. The resulting radiation could be detected by next generation telescopes such as James Webb, the Thirty Meter Telescope and the European Extremely Large Telescope. While underground direct detection searches are not (or poorly) sensitive to dark matter with sub-GeV masses, higher-than-weak-scale masses, scattering below neutrino floors, spin-dependent scattering well below nuclear cross-sections, pseudoscalar-mediated scattering, and inelastic scattering for inter-state transitions exceeding O(100 keV), dark kinetic heating of neutron stars advances these frontiers by orders of magnitude, and should vastly complement these searches. Popular dark matter candidates previously suspected challenging to probe, such as thermal Higgsinos, may be discovered.

Coffee Break in the Oak Room

New results from the Large Underground Xenon (LUX) detector, a 100-kg-scale, 2-phase xenon direct dark matter search experiment, will be shared. Dark matter, the missing ~25% of the mass-energy content of the universe, is sought in new ways, using effective field theory operators to extend the search to higher-mass Weakly Interacting Massive Particles (WIMPs), spin-dependent interaction operators, and electron instead of nuclear recoil, to seek axions. In addition, 2-neutrino double electron capture of 124Xe will be explored. Lastly, both old and new calibrations and position and energy reconstruction techniques will be reviewed, in the context of the new background and signal models being developed by LUX which will be expanded to higher energies and with inclusion of pulse-shape discrimination.

Xenon-based dark matter experiments have been leading the field of direct detection for a decade now, as realized most recently by the PandaX, LUX, and now XENON1T results, setting increasingly stringent limits on WIMP scattering. The near-future commencement of construction of LUX and ZEPLIN’s 10-ton-scale scale-up, next-generation successor, LZ, will be discussed here. We plan on achieving our baseline sensitivity of 2.3 x 10^-48 cm^2 for a WIMP of 40 GeV/c^2 rest mass, with a 5.6-ton fiducial mass in a two-phase xenon time-projection chamber. LZ has recently passed its final CD-2/3 approvals from the DOE, and unveiled its design details, background estimates, and projected sensitivities for different types of dark matter in its technical design Report. These will all be presented.

Understanding the properties of dark matter particle is a fundamental problem in particle physics and cosmology. The search of dark matter particle scattering off nuclei target using ultra-low background detector is one of the most promising technology to decipher the nature of dark matter. The XENON1T experiment, which is a dual phase detector with ~2.0 tons of xenon running at the Gran Sasso Laboratory in Italy, is designed to lead the field of dark matter direct detection. Since November 2016, the XENON1T detector is continuously taking data, with a background rate of more than one order of magnitude lower than any current generation dark matter search experiment. In this talk, I will present the first dark matter search results from XENON1T. Details about the XENON1T detector as well as the data analysis techniques will also be covered.

The PandaX project consists of a series of xenon-based experiments, located at China JinPing underground Laboratory. The current experiment, PandaX-II, is a direct dark matter search experiment with a 500 kg-scale liquid xenon dual-phase time projection chamber. PandaX-II started physics data taking in 2016. In this talk we report latest results and the current status of the PandaX-II experiment.

The CRESST (Cryogenic Rare Event Search with Superconducting Thermometers) experiment aims at the direct detection of dark matter particles via their elastic scattering off nuclei. The target material consists of scintillating CaWO$_4$ single crystals operated as cryogenic detectors at a temperature of ~10mK. For several years, these crystals have successfully been produced within the collaboration at the Technical University of Munich (TUM) and a significant improvement in radiopurity could be achieved. In CRESST-II Phase 2, an extended physics run between 2013 and 2015, the experiment demonstrated its leading sensitivity in the field of direct searches for dark matter masses below ~1.7GeV/c$^2$. A further detector optimization for the search of low-mass dark matter particles was performed for CRESST-III, whose Phase 1 started taking data in summer 2016. In this contribution the performance of the CRESST-III detectors as well as preliminary results will be presented. Requirements and perspectives for the upcoming CRESST-III Phase 2, in particular with respect to radiopurity, will be discussed.

The PICO collaboration uses superheated fluid detectors to attempt to directly detect interactions between dark matter particles and ordinary matter. These detectors can be operated in conditions under which they are insensitive to gamma and beta radiation, typically the dominant backgrounds for direct dark matter searches. The PICO-60 bubble chamber is located 2km underground at SNOLAB in Sudbury, Ontario, where neutron backgrounds from cosmic rays are strongly suppressed. These backgrounds are further suppressed by a water tank surrounding the chamber, and by the selection and clean handling of very radiopure components. Piezoacoustic transducers detect the sound of bubble nucleation, which can be used to distinguish between nuclear recoils and U/Th chain alpha decays, the predominant background in superheated fluid dark matter searches. During its first physics run the PICO-60 C$_3$F$_8$ bubble chamber was operated at a thermodynamic energy threshold of 3.3 keV, acquiring a background-free WIMP-search exposure of 1167 kg-days. A similar exposure was then acquired at 2.4 keV and is currently under analysis. Its successor, PICO-40L, will begin commissioning in the latter part of 2017. This detector has an inverted vertical orientation, intended to eliminate potential backgrounds caused by water droplets, particulates, and surface tension effects in previous chambers. It is intended to act as a prototype and proof-of-principle for the proposed ton-scale bubble chamber PICO-500.

Many extensions of the Standard Model of particle physics predict a parallel sector of at least one new U(1) symmetry, giving rise to hidden photons. If produced non-thermally in the early universe, these hidden photons can be candidate particles for cold Dark Matter. Hidden photons are expected to kinetically mix with regular photons. If hidden photons pass through a conducting surface a tiny electromagnetic signal is produced. Due to the kinematics of the process, these photons are emitted almost perpendicularly to the surface. The corresponding photon frequency is given by the mass of the hidden photons. In this contribution we present results of a search for dark photons in the mass range from 2 to 8 eV using a spherical metallic mirror of 14 m^2 area. We will also discuss future Dark Matter searches in the eV and sub-eV range by application of different detectors for electromagnetic radiation.

Recent HAWC observations have found extended TeV emission coincident with the Geminga and Monogem pulsars. In this talk, I will show that these detections have significant implications for our understanding of pulsar emission. The isotropic nature of this emission provides a new avenue for detecting nearby pulsars with radio beams that are not oriented towards Earth. Additionally, I will show that the total emission from all unresolved pulsars produces the majority of the TeV gamma-ray flux observed from the Milky Way.

Several starburst galaxies have been observed in the GeV and TeV bands; in this regime, gamma-rays are mainly produced by cosmic-ray interactions with the interstellar medium ($p_{\rm cr}p_{\rm ism} \to \pi^{0} \to \gamma\gamma$). Furthermore, the dense environments of starbursts may act as proton "calorimeters" where collisions dominate losses, so that a substantial fraction of cosmic-ray energy input is emitted in gamma rays. Here we build a one-zone, "thick-target" model implementing calorimetry and placing a firm upper bound on gamma-ray emission from cosmic-ray interactions. The model assumes that cosmic rays are accelerated by supernovae, and all suffer nuclear interactions rather than escape. Our model has only two free parameters: the cosmic-ray proton acceleration energy per supernova $\epsilon_{\rm cr}$, and the proton injection spectral index $s$. We calculate the pionic gamma-ray emission from 10 MeV to 10 TeV, and derive thick-target parameters for six galaxies with *Fermi*, *H.E.S.S.*, and/or *VERITAS* data. Our model provides good fits for the M82 and NGC 253, and yields $\epsilon_{\rm cr}$ and $s$ values suggesting that supernova cosmic-ray acceleration is similar in starbursts and in our Galaxy. We find that these starbursts are indeed nearly if not fully proton calorimeters. For NGC 4945 and NGC 1068, the models are consistent with calorimetry but are less well-constrained due to the lack of TeV data. However, the Circinus galaxy and the ultraluminous infrared galaxy Arp 220 exceed our pionic upper-limit; possible explanations will be discussed.

When analyzed together, radio and gamma-ray observations make for a very powerful tool for studying and diagnosing extragalactic cosmic ray populations. The recent gamma-ray detection of the ultra-luminous galaxy Arp 220 is well above past predictions, indicating evidence of a very large cosmic ray population. Whether the star formation or an active galactic nucleus is the source of the additional cosmic, there is a clear excess of gamma-ray emission in comparison to the observed radio flux. Here, we analyze the amount of energy necessary to power the observed gamma-ray flux and compare with traditional tracers of the star-formation rate. We also explore possible mechanisms for lowering the corresponding radio flux and check for consistency with observed properties of the interstellar medium.

It has been suggested that high-energy gamma-ray emission ($>$100MeV ) of nearby star-forming galaxies may be produced predominantly by cosmic rays colliding with the interstellar medium through neutral pion decay. The pion-decay mechanism predicts a unique spectral signature in the gamma-ray spectrum, characterized by a fast rising spectrum and a spectral break below a few hundreds of MeV. We here report the evidence of a spectral break around 500 MeV in the disk emission of Large Magellanic Cloud (LMC), which is found in the analysis of the gamma-ray data extending down to 60 MeV observed by {\it Fermi}-Large Area Telescope. The break is well consistent with the pion-decay model for the gamma-ray emission, although leptonic models, such as the electron bremsstrahlung emission, cannot be ruled out completely.

The repeating fast radio burst (FRB) 121102 was recently localized to a star-forming region in a dwarf host galaxy remarkably similar to those of superluminous supernovae (SLSNe) and long gamma-ray bursts (GRB), both of which were previously proposed to be powered by the birth of a millisecond magnetar. We demonstrate how a single magnetar engine can power both a SLSN and GRB, depending on the engine lifetime and the misalignment angle between the magnetar's rotation and magnetic axes. We also show that the production of a successful relativistic jet may be ubiquitous in engine-powered SLSNe, and describe several observational tests of this connection, including orphan radio afterglows and early optical signatures in the SLSN light curve. Finally, we describe recent results on the time-dependent ionization structure of the expanding supernova ejecta on timescales of decades following the explosion, due to photo-ionization by the nascent ‘magnetar wind nebula’. We precisely quantify when a fast radio burst can escape through the ejecta; create probability distributions of the local dispersion measure; and make predictions for the synchrotron radio emission from the magnetar wind nebula (analogous to the quiescent radio counterpart to FRB 121102).

Optical Synchrotron emission from blazars is significantly polarized and the polarization probes the magnetic field structure in the jet. Rotations of the polarization angle in blazars reveal important information about the evolution of disturbances responsible for blazar flares. Early results indicated that such rotations might be coincident with unusual gamma-ray activity of such sources. The RoboPol program for the polarimetric monitoring of statistically complete samples of blazars was developed in 2013 to systematically study this class of events and their possible connection with gamma-ray flares. RoboPol uses an innovative polarimeter installed at the 1.3m telescope of the University of Crete, and it is a collaboration between the University of Crete, Caltech, the Max-Planck Institute for Radio Astronomy, the Inter-University Centre for Astronomy and Astrophysics in India, and the Nicolaus Copernicus University in Poland. I will review the results of the 4-year aggressive, high-cadence gamma-ray—loud blazar monitoring with RoboPol, including the classification of the optopolarimetric properties of gama-ray—loud blazars, the statistical properties of polarization rotations, and their, now confirmed, relation to gamma-ray activity in blazar jets.

Coffee Break in the Oak Room

Blazars are thought to possess a relativistic jet that is pointing toward the direction of the Earth and the effect of relativistic beaming enhances its apparent brightness. Although numerous measurements have been performed, the mechanisms behind jet variability, creation, and composition are still debated. We performed simultaneous gamma-ray and optical photopolarimetry observations of 45 blazars with Fermi/LAT and Kanata telescope between 2008 July and 2014 December to investigate the mechanisms of variability and search for a basic relation between the several subclasses of blazars. Consequently, we found that a correlation between the gamma-ray and optical flux might be related to gamma-ray luminosity and the maximum polarization degree might be related to gamma-ray luminosity or the ratio of gamma-ray to optical flux. These results imply that low gamma-ray luminosity blazars emit from multiple regions.

By using deep radio source catalogs currently available, we present a new blazar candidate catalog, BROS, which includes 56314 sources located at declination $\delta > -40^{\circ}$ and outside the Galactic Plane ($|b| > 10^{\circ}$). We picked up flat-spectrum radio sources of $\alpha > -0.5$ ($\alpha$ is defined as $F_{\nu} \propto \nu^{\alpha}$) from 0.15 GHz TGSS and 1.4 GHz NVSS catalogs. Then, we identified their optical counterparts by cross-matching with the Pan-STARRS1 data. Color-color and color-magnitude plots for the selected flat-spectrum radio sources clearly showed two populations, “quasar-like” and “elliptical-galaxy-like” sequences. We emphasize that the latter population emerged for the first time and is missed by previous CRATES catalog because of the higher radio flux threshold. We found that the color-magnitude relation of nearby bright elliptical galaxies up to z=0.3 follows the “elliptical-galaxy-like" sequence. The index of the logN-logS distribution for this sample is $1.44\pm0.06$, supporting the interpretation of "nearby" because the measurement is consistent with a value for a static Euclidean universe. This BROS catalog is useful to search for electromagnetic counterparts of ultra-high-energy cosmic rays as well as PeV neutrions recently detected by IceCube, thus a powerful catalog in the era of multi-messenger astronomy. We also emphasize that this BROS catalog includes nearby ($z \leq 0.3$) BL Lac objects, a fraction of which would be TeV emitters and detectable by future Cherenkov Telescope Array. We will soon make this catalog available once published.

Recent high-energy missions have allowed keeping watch over quasars in flaring states, which provide deep insights into the engine powered by supermassive black holes. However, having a quasar caught in a very bright flaring state is not easy requiring long surveys. Therefore, the observation of such flaring events represents a goldmine for theoretical studies. Such a flaring event was captured by the INTEGRAL mission in June 2015 while performing its today’s deepest extragalactic survey when it caught the prominent quasar 3C 279 in its brightest flare ever recorded at gamma-ray energies. The flare was simultaneously recorded by the Fermi-LAT mission, by the Swift mission, and by observations ranging from UV, through optical to the near-IR bands. The derived snapshot of this broad spectral energy distribution of the flare has been modeled in the context of a one-zone radiation transfer leptonic and lepto-hadronic models constraining the single emission components. I will discuss results and challenges faced by trying to reconcile these observations and theory. Also implications for the detection of VHE gamma rays by Atmospheric Cherenkov Telescopes for such a flare will be discussed.

With the installation of a fifth 28-m diameter telescope in the center of the array, the H.E.S.S. telescope array is now in its phase II, characterized by a low energy threshold below 100 GeV. The low-energy window is particularly appealing for extragalactic gamma-ray astronomy, because it allows the study of more distant sources, as well as sources characterized by softer spectra. In particular, flat-spectrum radio-quasars (FSRQs), which dominate the Fermi-LAT extragalactic sky but are rarer in the very-high-energy (VHE) gamma-ray band due to their low-frequency SED peak, are among the most interesting targets for H.E.S.S. II observations. In this contribution I will review some recent results from H.E.S.S. II observations on FSRQs, including the discovery of VHE emission from PKS 0736+017, the detection of 3C 279 during the 2015 outburst, and the detection of PKS 1510-089 during the 2016 outburst.

Radio Galaxies are the most likely class of sources for the diffuse flux of high-energy neutrinos reported by the IceCube Collaboration as suggested by multi-messenger data. Here, the gamma-ray spectrum from four nearby radio galaxies (Centaurus A, PKS 0625-35, NGC 1275, and IC 310) is analyzed in order to constrain the spectral shape and intensity of their respective injected emission. Our analysis handles gamma ray propagation though galactic and extragalactic environments accounting for the effects of electromagnetic cascades. Assuming interactions of cosmic ray protons with gas are the origin of this gamma-ray emission, we calculate the resulting neutrino flux for the selected sources. While the predicted neutrino fluxes are consistent with constraints published by the IceCube and ANTARES Collaborations, they consistently fall within an order of magnitude below the current point source sensitivity. The prospects appear very encouraging for the future detection of neutrino emission from the nearest radio galaxies.predicted from each of these sources. Although this scenario is consistent with the constraints published by the IceCube and ANTARES Collaborations, the predicted fluxes consistently fall within an order of magnitude of the current point source sensitivity. The prospects appear very encouraging for the future detection of neutrino emission from the nearest radio galaxies.

The Compton Spectrometer and Imager is a 0.2-5 MeV Compton telescope capable of imaging, spectroscopy and polarimetry of astrophysical sources. Such capabilities are made possible by COSI's twelve germanium cross-strip detectors, which provide for high efficiency, high resolution spectroscopy, and precise 3D positioning of photon interactions. In May 2016, COSI took flight from Wanaka, New Zealand on a NASA super-pressure balloon. For 46 days, COSI floated at a nominal altitude of 33.5 km, continually telemetering science data in real-time. The payload made a safe landing in Peru, and the hard drives containing the full raw data set were recovered. Analysis efforts have resulted in detections of various sources such as the Crab Nebula, Cyg X-1, Cen A, Galactic Center e+e- annihilation, and the long duration gamma-ray burst GRB 160530A. In this presentation, I will provide an overview of our main results, which include measuring the polarization of GRB 160530A, and our image of the Galactic Center at 511 keV. Additionally, I will summarize results pertaining to our detections of the Crab Nebula, Cyg X-1, and Cen A.

The blazar Mrk 501 is a well-known BL-Lac type object emitting very high energy photons interacting with the EBL despite the modest redshift and is highly variable across wavelengths down to timescales of a few minutes at TeV energies. This makes it an excellent laboratory for studying particle acceleration and radiative emission processes in jets through the spectral and temporal properties of the observed emission. It also allows us to constrain the Extragalactic Background Light (EBL) and Lorentz Invariance Violation (LIV). H.E.S.S. has observed Mrk 501 during some of its active states at the highest energies in 2014, triggered by FACT which continuously monitors it, profiling its long-term TeV behaviour as Fermi-LAT does at GeV energies. Here, we present the temporal and spectral behaviour of Mrk 501 at gamma ray energies. We compute the gamma ray power spectral density as well as the energy spectrum for the highest TeV flux state observed by H.E.S.S. and FACT in June 2014 that shows rapid variability and contrast it with the long term average behaviour. We also derive strong constraints on the LIV scale via the non-detection of EBL opacity modifications and from time-of-flight studies from the H.E.S.S. flare data.

Neutrinos from charmed hadrons produced by cosmic ray interactions with air nuclei are the main background to high energy astrophysical neutrino flux measurements. Recent evaluations of the prompt neutrino flux from charm will be reviewed, including approaches using next-to-leading order QCD, the dipole model and kT factorization. Nuclear corrections and the impact of multi-component models of the incident cosmic ray flux will be discussed.

The DeepCore infill array of the IceCube Neutrino Observatory enables observations of atmospheric neutrinos with energies as low as 5 GeV. Using a set of 40,000 neutrino events with energies ranging from 5.6 - 56 GeV recorded during three years of DeepCore operation, we measure the atmospheric oscillation parameters $\theta_{23}$ and $\Delta m^2_{32}$ with precision competitive with long-baseline neutrino experiments, by observing distortions in the neutrino energy-zenith angle distribution. Our measurements are consistent with those made at lower energies, and prefer a value of $\theta_{23}$ close to maximal.

As is well known, dark matter direct detection experiments will ultimately be limited by a "neutrino floor," due to the scattering of nuclei by MeV neutrinos from, e.g., nuclear fusion in the Sun. Here we point out the existence of a new "neutrino floor" that will similarly limit indirect detection with the Sun, due to high-energy neutrinos from cosmic-ray interactions with the solar atmosphere. We have two key findings. First, solar atmospheric neutrinos ≲1 TeV cause a sensitivity floor for standard WIMP scenarios, for which higher-energy neutrinos are absorbed in the Sun. This floor will be reached once the present sensitivity is improved by just one order of magnitude. Second, for neutrinos ≳1 TeV, which can be isolated by muon energy loss rate, solar atmospheric neutrinos should soon be detectable in IceCube. Discovery will help probe the complicated effects of solar magnetic fields on cosmic rays. These events will also be backgrounds to WIMP scenarios with long-lived mediators, for which higher-energy neutrinos can escape from the Sun.

High-energy neutrinos are expected to be produced in cosmic-ray interactions with the solar atmosphere. The resulting neutrino flux is expected to offer insights into cosmic ray transport in the inner solar system and on solar magnetic fields. Besides the high theoretical interest in solar atmospheric neutrinos, an observed signal could be the first high-energy neutrino point source and valuable for calibration. Preliminary selection criteria and optimization studies will be discussed. We present sensitivities and the prospects to observe the solar atmospheric neutrino signal with IceCube data. The interplay with on-going dark matter searches from the Sun will be discussed.

In this talk I will discuss the production of high-energy neutrinos from interactions of cosmic rays with the solar atmosphere. Production of solar atmospheric neutrinos has been previously considered in the literature both as a potential source of high-energy neutrinos and as an irreducible background for dark matter searches. In our new calculation we estimate the uncertainties that arise from the solar atmosphere and hadronic interaction models. We further improve on previous calculations by considering neutrino oscillations in the propagation of neutrinos through the Sun. We predict that current event selections should observe ~ 1 event per year in detectors such as IceCube or the proposed mediterranean neutrino observatory, Km3Net. Finally, we put this rate in the context of indirect dark matter searches from the Sun by calculating the high-energy solar neutrino floor, which is analogous to the low-energy solar neutrino floor in dark matter direct detection experiments.

Coffee Break in the Oak Room

IceCube is a cubic kilometer scale detector in the deep antarctic ice. The 5160 deployed digital optical modules lead to the unambiguous detection of astrophysical neutrinos using events starting inside the detector with deposited energies above 60 TeV. Lowering the energy threshold down to 1 TeV, while maintaining a >90% neutrino-pure sample, greatly increases statistics. We will present the latest results of this data sample, containing more than 7000 all-sky neutrino-induced cascades and tracks. The data set allows a more precise measurement of the astrophysical spectrum, down to the atmospherically dominated region. Astrophysical models involving a second power-law component will be tested. Furthermore, we will present improved limits on the contribution of neutrinos from charmed mesons to the atmospheric flux. Having a significant contribution of both tracks and cascades in the same data sample allows to constrain the neutrino flavor space.

We report a new measurement of the diffuse flux of high energy extraterrestrial neutrinos from the whole sky with energies of O(1 TeV) and above, that is predominantly sensitive to electron and tau flavors. We analyzed 4 years of IceCube data recorded from 2012-2015 focusing on neutrino-induced cascades. Cascades provide good energy resolution and have a lower atmospheric neutrino background contribution than muon neutrinos. A new event selection has been developed combining straight cuts with gradient boosted multi-class decision trees to isolate cascades with increased efficiency over previous methods, resulting in the largest cascade sample obtained by IceCube to date. Our methods achieve a neutrino purity of better than 90%. At energies above 20 TeV the contribution of muon neutrinos to the total number of expected astrophysical neutrinos in this cascade sample is estimated to be 10%. At these energies the extra-terrestrial component dominates the observed spectrum and is well described by a single, unbroken power-law. We will discuss preliminary fit results and study the possibility of a spectral hardening at the upper end of the spectrum by allowing a second power-law component to enter our flux model.

The IceCube neutrino observatory has observed a flux of high-energy astrophysical neutrinos using both track events from muon neutrino interactions and cascade events from interactions of all neutrino flavors. Searches for astrophysical neutrino sources have focused on track events due to the significantly better angular resolution of track reconstructions. To date, no such sources have been confirmed. In this talk we turn our attention to complementary and statistically-independent source searches using cascade events with deposited energies as small as 1 TeV. Compared to the classic approach using tracks, the cascade channel offers improved sensitivity to sources in the southern sky, especially if the emission is spatially extended or follows a soft energy spectrum. We will show results from a first search using 263 cascades collected from May 2010 to May 2012, as well as projected sensitivity estimates for an upcoming analysis of six years of data.

PeV neutrinos detected by the IceCube observatory are the highest-energy extraterrestrial elementary particles ever seen on Earth. More knowledge on PeV neutrinos such as seeing a spectral cut-off would help understand the possible connection to the sources of ultra-high energy cosmic rays. A new selection has been developed for PeV neutrinos which are not selected by the existing high-energy searches. The new channel has been optimised for partially-contained cascades generated via Glashow resonance. It has then been combined with samples of high-energy starting events and extremely-high-energy tracks to determine the characteristics of the high-energy end of the diffuse spectrum. In this talk, results on the cut-off energy will be shown and constraints on scenarios which predict cosmogenic PeV neutrinos will be discussed.

Neutrino interactions occurring in IceCube require accurate reconstruction techniques to quantify the neutrino's energy and arrival direction. At the highest energies, the angular resolution of IceCube is limited primarily by ice property uncertainties. Previous studies have shown that a perfect knowledge of the ice may improve cascade angular resolutions by a factor of two or more. We present a new method for evaluating the effect of ice model uncertainties and explore several channels by which the reconstructed angular resolution may be improved.

IceCube analyses which look for an astrophysical neutrino signal in the southern sky face a large background of atmospheric neutrinos and muons created in cosmic ray air showers. Earlier, it was found that rejecting events that deposit energy in the outer region of the detector reduces not only the muon background, but also the atmospheric neutrino background in the southern sky due to the atmospheric self-veto effect. However, using outer layer fiducial cuts reduces the size of the detector and leads to a selection optimized for cascades. In this event sample, we select for muon tracks which have a starting vertex contained inside the detector. By using the improved directional reconstruction from muons, the selection determines a veto region behind the starting vertex for each event and calculates the likelihood for not observing a hit on the IceCube optical modules (DOMs) in the veto region. These cuts give a selection which has a high astrophysical neutrino purity above 10 TeV in the southern sky. We will present our most recent results from our neutrino point source and diffuse flux searches and provide a first look at the realtime events stream derived from the selection.

We present prospects for IceCube to detect neutrino emission from Galactic TeV gamma-ray sources outlined in the HAWC Observatory's recently published 2HWC catalog. We do this by evaluating the sensitivity of two analyses using IceCube data. The first is a stacked analysis of promising point sources from the catalog which are chosen based on their high TeV photon fluxes and lack of association with known pulsar wind nebula. Here we assume the highest energy photons originate from the decay of charged pions produced by hadronic interactions at each source. The second is a template analysis using the full Galactic plane morphology measured by HAWC. This morphology should trace neutrino emission if pion decay predominantly occurs in the environment surrounding identified HAWC sources.

Supernova remnants (SNRs) are the long lived structures that result from the explosive end of a massive star. The expanding shock-front produced by the supernova explosion heats stellar ejecta and swept-up ISM to X-ray emitting temperatures, and are sites in which populations of relativistic particles can be efficiently accelerated to the knee of the Cosmic-ray spectrum. For SNRs that are born in regions of high density, the interaction between the SNR with this dense molecular material has a profound effect on the morphology and emission properties of these objects. Until recently, most studies have focused on individual sources, however, in this talk I will focus on the importance of systematically studying the properties of these objects. In particular, I will highlight current investigations into the high energy emission of these remnants using X-ray and gamma-ray satellites, and discuss the insights these studies have provided us with in regards to the properties of their progenitor, and their surrounding environment, as well as their ability to accelerate particles.

The Vela supernova remnant is a canonical example of a middle-aged composite system in which the SNR reverse shock has disrupted the central pulsar wind nebula, Vela X. Due to a non-uniform ambient medium, the shock has propagated asymmetrically, crushing the northern part of the PWN. The result is a complex structure characterized by nonthermal X-rays from the pulsar wind, thermal X-rays from ejecta mixed into the nebula, and gamma-ray emission in both the GeV and TeV bands, for which the morphology shows striking differences. Here we report on an XMM Large Project to study Vela X. We study variations in the spectral index of the nonthermal X-ray emission, along with the distribution and thermal properties of the shocked ejecta, and correlate these with the gamma-ray properties of the PWN. We evaluate these properties using hydrodynamical simulations in the context of the evolution of PWNe in composite SNRs, with a view to the ultimate fate of the relativistic particles produced in these systems.

The survey of the Galactic plane in TeV gamma-rays by H.E.S.S. allows a systematic study of the population of pulsar wind nebulae (PWNe) in this energy domain. We find a mild trend of decreasing TeV luminosity with age, or decreasing spin-down power, as well as a trend of increasing size with age. Older TeV PWNe are generally displaced from the pulsar position, with offsets larger than can plausibly be explained by pulsar proper motion, which could be due to PWN interaction with the reverse shock in an asymmetric environment. The observed gamma-ray spectra can be ascribed to inverse Compton scattering of ambient photons, in which the Galactic far-infrared background often predominates; this may explain why luminous TeV PWNe are more readily detected in the inner spiral arms than in the outer Galaxy. We also present a more detailed morphological study of the TeV emission from the PWN in the composite supernova remnant MSH 15-52. We compare its gamma-ray morphology with that in synchrotron emission, obtained from archival X-ray observations, and discuss the implications for the magnetic field in the nebula. We also discuss potential extended gamma-ray emission beyond the X-ray PWN. Such an extended morphological component could come from electrons and positrons which have escaped the PWN, which would have implications for scenarios of PWNe as sources of leptonic cosmic rays.

Coffee Break in the Oak Room

I present the results of large kinetic simulations of particle acceleration at non-relativistic collisionless shocks, which allow an ab-initio investigation of diffusive shock acceleration (DSA) at the blast waves of supernova remnants, the most prominent sources of Galactic cosmic rays (GCRs).  Ion acceleration efficiency and magnetic field amplification are obtained as a function of the shock properties and compared with theoretical predictions and multi-wavelength observations of individual remnants. In particular, I will focus on two new results: 1) the origin of the chemical enhancement of heavy elements observed in GCRs as naturally due to DSA, and 2) the re-acceleration of energetic particle “seeds” and its phenomenological implications.

I will discuss cosmic ray production at relativistic shocks. I will emphasize the differences expected for relativistic shocks compared to non-relativistic ones and examine possible applications such as relativistic supernovae and gamma ray bursts.

The X-ray emission from pulsar wind nebulae arises from particles accelerated at the shock that terminates the relativistic, strongly magnetized pulsar wind. However, conventional theories of particle acceleration break down at this shock, because the combination of low particle density and strong magnetic field places it outside the domain of validity of MHD. We first discuss how particles are, nevertheless, injected into a first-order-Fermi-like process and accelerated. We then study their acceleration in the equatorial region of the termination shock. To do so, we integrate the individual trajectories of electrons and positrons, in the test-particle limit, in the background electromagnetic fields present in that region. We find that the spectrum of accelerated electrons (or positrons, depending on the polarity) is significantly harder than $E^{-2.2}$. We calculate the resulting synchrotron spectrum, and compare our results with Chandra observations of the X-ray spectrum of the Crab nebula. I am also submitting an abstract to the track "cosmic rays".

MAGIC is a stereoscopic system of two imaging atmospheric Cherenkov telescopes, located at the Roque de los Muchachos Observatory, in La Palma (Spain) sensitive to gamma rays from few tens of GeV to tens of TeV. Pulsar physics is one of important topics in the MAGIC scientific program. In 2008, MAGIC for the first time detected VHE gamma-rays demission above 25 GeV from the Crab pulsar. Ever since, crab observations with MAGIC have beenIn this talk, we will present the recent scientific results derived from observations of the Crab pulsar, we will describe the technical innovations of MAGIC for the study of pulsars at a few tens of GeV, and will give an outlook to future pulsar observations at very-high-energy gamma rays and their relevance to understanding these extreme celestial objects. providing important results for the understanding of pulsar physics.

The Sun must shine brightly in GeV—TeV gamma rays and neutrinos.  These particles are produced by the interactions of cosmic rays with solar matter and radiation.  Additional fluxes may be caused by the annihilation of dark matter in the solar core, perhaps with the eventual particles produced outside of the Sun through the decay of metastable mediators.  Importantly, a new generation of experiments is reaching the sensitivity required to detect the Sun at high energies.  In gamma rays, the Sun has been detected in the GeV range by Fermi and will soon be studied in the TeV range by ARGO-YBJ, HAWC, and LHAASO.  In neutrinos, IceCube is nearing the sensitivity required to detect TeV neutrinos.  I will detail the physics prospects for what these observations will teach us about cosmic rays in the inner solar system, solar magnetic fields, and dark matter.  This talk will highlight work from our group, including arXiv:1508.06276, arXiv:1612.02420, arXiv:1703.04629, arXiv:1703.10280, as well as the rapid growth in interest from other groups.

Only a handful of High Mass X-ray Binaries (HMXB) in our galaxy are known emitters of TeV gamma rays. The variable VHE emission from these sources are generally attributed to modulation by their orbital periods but the particle acceleration and gamma-ray production processes in these HMXBs are not well understood. In its 10 years of operation, VERITAS has observed 2 of these TeV emitting HMXBs, LS I +61 303 and HESS J0632+057 for more than 450 hours, conducting many multi-wavelength campaigns. The results from recent observations, long-term monitoring and multi-wavelength study with X-ray (Swift-XRT) and GeV (Fermi-LAT) for LS I +61 303 and HESS J0632+057 are discussed. Besides these two TeV binaries, an outline of the binary discovery program by VERITAS is presented with particular emphasis on PSR J2032+4127, the long period (45-50 years) binary in a highly eccentric orbit with the Be star MT91 213. This system could be the origin of very high energy emission from the unidentified source TeV J2032+4130. We present the status of observations of PSR J2032+4127, preliminary results and the plan for continued monitoring through periastron in 2017.

Supernovae (SNe) and their remnants are important cosmic ray sources. However, the origin of one major type of SNe, the Type Ia, is still not well understood. Two most popular hypotheses are the single-degenerate scenario, where one white dwarf (WD) accretes matter from its giant companion until the Chandrasekhar limit is reached, and the double-degenerate scenario, where two WDs merge and explode. We focus on the second scenario. It has long been realized that binary WD systems normally take extremely long time to merge via gravitational waves and it is still unclear whether WD mergers can fully account for the observed SN Ia rate. Recent effort has been devoted to the effects of introducing a distant tertiary to the binary system. The standard “Kozai-Lidov” mechanism can lead to high eccentricities of the binary WDs, which could lead to direct collisions or much efficient energy dissipation. Alternatively, we investigate the long-term evolution of the hierarchical quadruple systems, i.e. WD binary with a binary companion, which are basically unexplored, yet they should be numerous. We explore their interesting dynamics and find that the fraction of reaching high eccentricities is largely enhanced, which hints on a higher WD merger rate than predicted from triple systems with the same set of secular and non-secular effects considered. Considering the population of quadruple stellar systems, the quadruple scenario might contribute significantly to the overall rate of Ia SNe.

Cosmological observations represent a powerful tool to constrain neutrino physics, complementary to laboratory experiments. In particular, observations of the cosmic microwave background (CMB) have the potential to constrain the properties of relic neutrinos, as well as of additional light relic particles in the Universe. I will present current constraints on neutrino properties, focusing on their mass and effective number, from the most recent Planck data, possibly in combination with other cosmological probes, especially galaxy surveys. I will also discuss prospects from future experiments, both from the ground and from space.

We study and constrain the impact of non-standard neutrino interactions on the CMB angular power spectrum. Starting from the collisional Boltzmann equation, we derive the Boltzmann hierarchy for neutrinos including interactions with a massive scalar particle. In contrast to the Boltzmann hierarchy for photons, our interacting neutrino Boltzmann hierarchy is momentum dependent, which reflects non-negligible energy transfer in the considered neutrino interactions. We implement this Boltzmann hierarchy into the Boltzmann solver CLASS and compare our results with known approximations in the literature. We thereby find a very good agreement between our exact approach and the relaxation time approximation (RTA). The popular $\left( c_{\text{eff}}^2,c_{\text{vis}}^2 \right)$-parametrization however does not reproduce the correct signal in the CMB angular power spectrum. Using the RTA, we furthermore derive constraints on the effective coupling constant $G_{\text{eff}}$ from currently available cosmological data. Our results reveal a bimodal posterior distribution, where one mode represents the standard $\Lambda$CDM limit, and the other a scenario of neutrinos self-interacting with $G_{\rm eff} \simeq 3 \times 10^9 \, G_{\rm F}$ (where $G_{\text{F}}$ is the Fermi coupling).

Light sterile neutrinos with eV mass have been suggested by different anomalies observed in short-baseline neutrino experiments. These particles would have been produced in the Early Universe changing the amount of relativistic energy density by increasing the effective number of relativistic species ($N_{\rm{eff}}$). This results in a conflict with existing cosmological bounds on primordial radiation density and neutrino mass. In order to alleviate these discrepancies, basically avoiding the thermalization of eV sterile neutrinos in the early Universe, secret interactions in the sterile sector mediated by a massive vector boson ($M_X < M_W$ ) have been proposed. Secret interactions reduce the effective mixing angle generating a large matter potential in the sterile neutrino sector and suppressing the active-sterile oscillations. In particular if the interactions are mediated by a gauge boson having $M_X < 10$ MeV, the sterile neutrino productions is suppressed for $T > 0.1$ eV; this behaviour seems to ameliorate the conflict between the cosmological constraints and laboratory experiments. Observations of the cosmic microwave background (CMB) radiation represent a powerful and unique tool to test this model in more detail. During my presentation I will show results of a dedicated study presenting constraints on the strength of the secret interaction and the corresponding mass bounds using the latest CMB Planck 2015 data. Finally I will discuss the status of the sterile neutrino secret interaction scenario after this work. Page 23

A number of ground-based CMB surveys are currently in the planning stages that will provide significant new information on properties of physics beyond the standard model. Measurements of the lensing of the CMB are expected to provide evidence for neutrino mass in the case of a minimal mass as expected from neutrino oscillation experiments. Meanwhile measurements of the phase of the acoustic plasma will provide constraints on particles that are in equilibrium with the standard model prior to decoupling. After reviewing the prospects for these measurements I will discuss some of the technical challenges involved.

The standard $\Lambda$CDM cosmological model has successfully explained large scale cosmological observations. However, there are some discrepancies between the $\Lambda$CDM predictions and measurements at small scales. Even though these discrepancies could be due to unaccounted effects on weak lensing analyses and/or numerical simulations, in this talk, I will explore the possibility of extending the standard cosmological model with an additional, subdominant, non-cold dark matter component. In particular, I will show the impact of such a scenario on various cosmological probes, including the CMB (Planck), weak lensing surveys measurements (KIDS) and the number of satellite galaxies in the Milky Way.

Coffee Break in the Oak Room

I will discuss new signatures in direct detection experiments if part or all of the dark matter particles in nature are in the form of bound states. It will allow the sub-GeV dark matter candidates to be much more visible at dark matter and neutrino detectors.

The spectrum of Weakly-Interacting-Massive-Particle (WIMP) dark matter generically possesses bound states when the WIMP mass becomes sufficiently large relative to the mass of the electroweak gauge bosons. The presence of these bound states enhances the annihilation rate via resonances in the Sommerfeld enhancement, but they can also be produced directly with the emission of a low-energy photon. I will present a calculation of the rate for SU(2)-triplet dark matter (the wino) to bind into WIMPonium -- which is possible via single-photon emission for wino masses above 5 TeV for relative velocity v < O(10^{-2}) -- and the subsequent decays of these bound states. I will also present results with applications beyond the wino case, e.g. for dark matter inhabiting a general nonabelian dark sector.

The LHC Dark Matter Working Group (LHC DM WG) brings together theorists and experimentalists to provide the benchmark models, interpretation, and characterisation needed for a robust and broad set of searches for dark matter at the LHC. I will discuss the work of the LHC DM WG, and its predecessor the ATLAS/CMS Dark Matter Forum---the interaction between theory and experiment, the types of signals being considered for LHC Run-2 searches, the evolving interpretation of the LHC results alongside direct and indirect detection, and the future.

New particles with long lifetimes are introduced by many extensions to the standard model and would produce striking and non-conventional signatures in collider experiments such as long-lived charged particles, highly displaced jets, and particles that come to a rest within the detector and later decay. We present the results of several recent searches for long-lived particles with the CMS experiment in Run II of the LHC.

We present several complementary searches for low mass dijet resonances using a 35.9 inverse femtobarn data set of proton-proton collisions at 13 TeV collected with the CMS experiment at the LHC in 2016. One search uses the CMS scouting data stream concept to record larger data rates than otherwise possible. Another search uses an initial state radiation jet to overcome trigger thresholds and search for boosted dijet resonances, whose decay products are merged into a single jet. Novel jet substructure techniques are used to avoid sculpting the distribution of the jet mass distribution and the dominant background is estimated from data. Both searches are interpreted in the context of leptophobic vector resonances and simplified models of dark matter with a leptophobic mediator. This approach has also been extended to the search for boosted Higgs bosons decaying to bottom quark-antiquark pairs.

We present the latest results in the search for rare, exotic, and invisible Higgs boson decays in proton-proton collision events collected with the CMS detector at the LHC. The rich experimental program we describe, which includes searches for lepton flavor violation and decays to dark matter and light scalars, provides a wide ranging probe for physics beyond the standard model.

The wide range of probes of physics beyond the standard model (BSM) lead to the need for tools that consistently combine experimental results to make the most robust possible statements about the validity of new physics theories and the preferred regions of their parameter space. In this talk, I will introduce a new publicly released code for such studies: GAMBIT, the Global and Modular BSM Inference Tool. GAMBIT is a flexible and extensible framework for global fits of essentially any BSM theory. The code currently incorporates constraints from the dark matter relic density, direct and indirect dark matter searches, limits on production of new particles from the LHC and LEP, complete flavor constraints from LHCb, LHC Higgs production and decay measurements, and various electroweak precision observables. I will discuss the code’s capabilities and results of scans of the parameter space of the Minimal Supersymmetric Standard Model.

Recent Fermi-LAT observations of dwarf spheroidal galaxies in the Milky Way have placed strong limits on the gamma-ray flux from dark matter annihilation. In order to produce the strongest limit on the dark matter annihilation cross-section, the observations of each dwarf galaxy have typically been “stacked” in a joint-likelihood analysis, utilizing optical observations to constrain the dark matter density profile in each dwarf. These limits have typically been computed only for singular annihilation final states, such as bb or τ+τ−. In this paper, we generalize this approach by producing an independent joint-likelihood analysis to set constraints on models where the dark matter particle annihilates to multiple final state fermions. We interpret these results in the context of the most popular simplified models, including those with s- and t-channel dark matter annihilation through scalar and vector mediators. We present our results as constraints on the minimum dark matter mass and the mediator sector parameters. Additionally, we compare our simplified model results to those of Effective Field Theory contact interactions in the high-mass limit.

Extragalactic galaxies and galaxy clusters are expected to be some of the brightest sources of dark matter annihilation on the sky. Further, catalogs such as the 2MASS survey, tell us where thousands of these objects are. The challenge, however, is that catalogs only detail a subset of the baryonic properties of these galaxies. In this talk I will outline how to map from a catalog of galaxies to map of the extragalactic dark matter distribution on the sky. I will show how the biases and systematics of the method can be understood in the context of an N-body simulation, and demonstrate that the projected sensitivity of this method at Fermi-LAT could produce limits comparable with those coming from the Milky Way Dwarfs.

We perform a search for dark matter (DM) annihilation in nearby galaxies using 413 weeks of publicly-available Fermi Pass 8 gamma-ray data, utilizing a novel method that takes advantage of recently-developed galaxy group catalogs based on the 2MASS Redshift Survey. Having validated our method using N-body simulations, we construct nearly all-sky maps of an expected DM annihilation signal in the local (z < 0.03) universe and look for this structure in the Fermi data, probing theoretically well-motivated regions of parameter space for conservative assumptions about substructure enhancement. I will present the results of our analysis, discussing the effect of modeling uncertainty and implications for the DM interpretation of the Galactic Center excess.

Milky Way dwarf spheroidal satellite galaxies are the most dark-matter-dominated galaxies known. Due to their proximity, high dark matter content, and lack of astrophysical backgrounds, dwarf spheroidal galaxies are one of the most promising targets for the indirect detection of dark matter annihilation via gamma rays. Indeed, Fermi-LAT observations of previously known dwarf galaxies have robustly constrained the dark matter annihilation cross section to be less than the generic thermal relic cross section for dark matter particles with mass < 100 GeV. Recently, large optical surveys, such as the Dark Energy Survey and Pan-STARRS, have nearly doubled the known population of confirmed and candidate dwarf galaxies. We will present an updated gamma-ray analysis combining previously known and recently discovered dwarf galaxies, and discuss how current and future optical surveys will improve the sensitivity of gamma-ray searches for dark matter annihilation in dwarf galaxies.

For models in which dark matter annihilation is Sommerfeld-enhanced, the annihilation cross section increases at low relative velocities. Dwarf spheroidal galaxies (dSphs) have low characteristic dark matter particle velocities and are thus ideal candidates to study such models. We model the dark matter phase space of dSphs as isotropic and spherically-symmetric and determine the $J$-factors for several of the most important targets for indirect dark matter searches. For Navarro-Frenk-White density profiles, we quantify the scatter in the $J$-factor arising from the astrophysical uncertainty in the dark matter potential. We show that, in Sommerfeld-enhanced models, the ordering of the most promising dSphs may be different relative to the standard case of velocity-independent cross sections. This result can have important implications for derived upper limits on the annihilation cross section, or on possible signals, from dSphs.

The Milky Way's Galactic Center may harbor the signal of annihilating dark matter in a gamma-ray excess, though dwarf galaxies remain dark in their expected commensurate emission. We incorporate Milky Way dark matter halo profile uncertainties, as well as an accounting of diffuse gamma ray emission uncertainties in dark matter annihilation models for the Galactic Center Extended gamma-ray excess (GCE) detected by the Fermi Gamma Ray Space Telescope. The range of particle annihilation rate and masses expand when including these unknowns. However, two of the most precise empirical determinations of the Milky Way halo's local density and density profile leave the signal region to be in considerable tension with dark matter annihilation searches from combined dwarf galaxy analyses for single-channel dark matter annihilation models. Accordingly, we quantify this tension in a joint likelihood analysis. We also show that astrophysical models and a representative self-interacting dark matter model avoid the tensions between the GCE signal and lack of a signal from the dwarfs. Since these arguments disfavor the intepretation of the GCE as prompt annihilation of dark matter, we set limits on the cross section for that process.

We propose a novel method to search for signatures of dark matter annihilation in Galactic substructure using gamma-ray data from the $\it Fermi$ Large Area Telescope. The method takes advantage of the fundamentally different photon-count statistics that describe dark matter annihilation from a population of subhalos versus from the smooth Milky Way halo. In addition, it exploits differences in the spatial distribution of subhalos and other astrophysical populations to improve the sensitivity to the substructure signature. We apply this analysis method to simulated $\it Fermi$ data and derive the projected sensitivity to dark matter annihilation in substructure. We can probe theoretically well-motivated regions of parameter space, providing a complementary method to existing dark matter searches.

Coffee Break in the Oak Room

In this talk, we discuss a scenario called late-decaying two-component dark matter (LD2DM), where the entire DM consists of two semi-degenerate species. Within this framework, the heavier species is produced as a thermal relic in the early universe and decays to the lighter species over cosmological timescales. Consequently, the lighter species becomes the DM which populates the universe today. We show that annihilation of the lighter DM species with an enhanced cross-section, produced via such a non-thermal mechanism, can explain the observed excess in AMS-02 positron flux while avoiding CMB constraints from the recombination epoch. We demonstrate that the scenario is robust, subject to constraints from structure formation and CMB constraints on late-time energy depositions during the cosmic dark ages. We explore possible cosmological and particle physics signatures in a toy model that realizes this scenario.

The most dramatic "Sommerfeld enhancements'' of neutral-wino-pair annihilation occur when the wino mass is near a critical value where there is a zero-energy S-wave resonance at the neutral-wino-pair threshold. Near a critical mass, low-energy winos can be described by a zero-range effective field theory in which the winos interact nonperturbatively through a contact interaction. The effective field theory is controlled by a renormalization-group fixed point at which the neutral and charged winos are degenerate in mass and their scattering length is infinite. The parameters of the zero-range effective field theory can be determined by matching wino-wino scattering amplitudes calculated by solving the Schrödinger equation for winos interacting through a potential due to the exchange of weak gauge bosons. If the wino mass is larger than the critical value, the resonance is a wino-pair bound state. The power of the zero-range effective field theory is illustrated by calculating the rate for formation of the bound state in the collision of two neutral winos through the emission of two soft photons.

In this talk, I will discuss a class of models in which thermal dark matter is lighter than an MeV. If dark matter thermalizes with the Standard Model below the temperature of neutrino-photon decoupling, constraints from measurements of the effective number of neutrino species are alleviated. This framework motivates new experiments in the direct search for sub-MeV thermal dark matter and light force carriers.

We investigate the feasibility of the indirect detection of dark matter in a simple model using the neutrino portal. The model is very economical, with right-handed neutrinos generating neutrino masses through the Type-I seesaw mechanism and simultaneously mediating interactions with dark matter. Given the small neutrino Yukawa couplings expected in a Type-I seesaw, direct detection and accelerator probes of dark matter in this scenario are challenging. However, dark matter can efficiently annihilate to right-handed neutrinos, which then decay via active-sterile mixing through the weak interactions, leading to a variety of indirect astronomical signatures. We derive the existing constraints on this scenario from Planck cosmic microwave background measurements, Fermi dwarf spheroidal galaxies and Galactic Center gamma-rays observations, and AMS-02 antiprotons observations, and also discuss the future prospects of Fermi and the Cherenkov Telescope Array. Thermal annihilation rates are already being probed for dark matter lighter than about 50 GeV, and this can be extended to dark matter masses of 100 GeV and beyond in the future. This scenario can also provide a dark matter interpretation of the Fermi Galactic Center gamma ray excess, and we confront this interpretation with other indirect constraints. Finally we discuss some of the exciting implications of extensions of the minimal model with large neutrino Yukawa couplings and Higgs portal couplings.

Recent results on the Extragalactic Background Light (EBL) intensity obtained from a combined likelihood analysis of blazar spectra detected by the MAGIC telescopes are reported. The EBL is the optical-infrared diffuse background light accumulated during galaxy evolution, directly and/or reprocessed by dust, which provides unique information about the history of galaxy formation. The low energy photons from the EBL may interact with very high energy (VHE, E > 100 GeV) photons from blazars, which are a subclass of Active Galactic Nuclei whose relativistic jets point towards Earth. This interaction between the EBL and the gamma-ray photons leaves an energy-dependent imprint of the EBL on the VHE gamma-ray spectra of the blazars. Therefore, the study of their spectra can be used to constrain the EBL density at different wavelengths and its evolution in time. The MAGIC telescopes are a stereoscopic system of two Imaging Atmospheric Cherenkov Telescopes of 17 m diameter each, situated in La Palma, Spain, and sensitive to gamma-ray photons with energies larger than about 50 GeV. In the last few years the MAGIC telescopes obtained accurate measurements of the spectra of 12 blazars in the redshift range from z=0.03 to z=0.944 for over 300 hours of observation. This allows us to improve upon previous constraints on EBL by MAGIC, compatible with the state-of-the-art EBL models.

We have calculated the extragalactic IR-UV photon density as a function of redshift, and the resulting IR-UV spectrum of the extragalactic background light. Our empirically-based approach is based on local-to-deep galaxy survey data obtained in different wavelength bands using many space-based telescopes. This approach allowed us, for the first time, to obtain a completely model independent determination of extragalactic photon densities, and also to quantify their uncertainties. Using our photon density results, we were able to place 68% confidence upper and lower limits on the opacity of the universe to gamma-rays as a function of energy and redshift. We compared our results with Fermi analyses of the spectra of extragalactic gamma-ray sources.

Gamma-rays with energy exceeding 100 GeV emitted by extragalactic sources initiate cascades in the intergalactic medium. The angular and temporal distribution of the cascade photons that arrive at the Earth depend on the strength and configuration of extragalactic magnetic fields in the line of sight. For weak enough fields, extended emission around the source (halo) is expected to be detectable, and the characteristics (angular size, energy dependence, and shape) of this emission are a sensitive probe of EGMF strength and correlation length. We model the expected specta and angular profiles of blazars, and misaligned active galactic nuclei (radio-galaxies) in a wide range of parameter space of the extra-galactic magnetic field strength and correlation length, which is unconstrained by existing measurements. Our calculations focus on the time dependence of such halo emission, which is being discussed for the first time in this work. We present the competitive bounds on/measurement of the extragalactic magnetic field strength and correlation length that are implied by the absence/detection of such, extended emission, in stacked searches of GeV halo emission by blazars, and radio-galaxies.

We report on the Fermi High-Latitude Extended Source Catalog (FHES), a systematic search for spatial extension of gamma-ray point sources detected with the Fermi Large Area Telescope (LAT) at Galactic latitudes |b| > 5 degrees. Point sources listed in the 3FGL and 3FHL catalogs are used for this search. While the majority of high-latitude LAT sources are extragalactic blazars that appear point-like within the LAT angular resolution, there are several physics scenarios that predict the existence of populations of spatially extended sources. If dark matter consists of weakly interacting massive particles, the annihilation or decay of these particles in subhalos of the Milky Way would appear as a population of unassociated gamma-ray sources with finite angular extent. Gamma-ray emission from blazars could also be extended (so-called pair halos) due to the deflection of electron-positron pairs in the intergalactic magnetic field (IGMF). The pairs are produced in the absorption of gamma rays in the intergalactic medium and subsequently up-scatter photons of background radiation fields to gamma-ray energies. The measurement of pair halos would constrain the strength and coherence length scale of the IGMF. We report on new extended source candidates and their associations found in the FHES as well as limits on the IGMF based on the non-observation of the cascade.

The very high energy ($E > 100 $ GeV) gamma-ray flux from extragalactic sources is attenuated due to $e^+e^-$ pair production on the extragalactic background light (EBL). This attenuation process can lead to the development of electromagnetic cascades from the inverse-Compton scattering of background photons by the produced $e^+e^-$ pairs. The cascade secondary gamma-ray emission is reprocessed at lower energies and its spectral and temporal behavior depends on the properties of the extragalactic magnetic field (EGMF) along the line of sight due to the deflections of the charged component of the cascade. The temporal and spectral energy distribution structure of the gamma-ray emission from blazars can then be used to probe the EGMF. In this contribution the gamma-ray blazar PG 1553+113 is identified as a promising target to search for secondary emission, based on H.E.S.S. and Fermi-LAT energy spectra. Monte-Carlo simulations of cascades using the public code ELMAG are performed to derive EGMF constraints under different assumptions on the intrinsic spectrum and the time span of the gamma-ray activity of the source. Prospects to take advantage of the quasi-periodic modulation seen in the activity of PG 1553+113 to look for secondary gamma-ray emission are also presented.

Poisson regression of the Fermi-LAT data in the inner Milky Way reveals an extended gamma-ray excess. An important question is whether the signal is coming from a collection of unresolved point sources, possibly old recycled pulsars, or constitutes a truly diffuse emission component. Previous analyses have relied on non-Poissonian template fits or wavelet decomposition of the Fermi-LAT data, which find evidence for a population of faint point sources just below the 3FGL flux limit. In order to test this hypothesis, we use a Bayesian, transdimensional, and hierarchical inference framework, PCAT (Probabilistic Cataloger), by sampling from the posterior catalog space of faint point sources consistent with the observed gamma-ray emission in the inner Milky Way. By marginalizing over faint point sources, we constrain their spatial and spectral distributions. We then compare the performance of probabilistic cataloging with that of fluctuation analysis when inferring unresolved point sources in the low signal-to-noise limit.

Coffee Break in the Oak Room

All models for Galactic diffuse gamma-ray emission share one property:  They give formally a remarkably bad fit to the data.  A large number of statistically significant residuals remain, making it very challenging to discriminate genuine features in the data from analysis artefacts. We present SkyFACT (Sky Factorization with Adaptive Constrained Templates) [1], a new approach for studying, modeling and decomposing diffuse gamma-ray emission. In contrast to previous approaches, we can account for fine-grained variations related to uncertainties in gas tracers and small scale variations in the cosmic-ray density, that are missed in predictions from cosmic-ray propagation codes, by introducing (and handling) ~100,000 nuisance parameters. We combine methods of image reconstruction and adaptive spatio-spectral template regression in one coherent hybrid approach. We apply the method to the gamma-ray emission from the inner Galaxy, as observed by the Fermi Large Area Telescope. We define a simple reference model that removes most of the residual emission from the inner Galaxy and characterize extended emission components: the Fermi bubbles, the Fermi Galactic center excess, and extended sources along the Galactic disk. [1] E.Storm, C. Weniger and F. Calore, arXiv:1705.04065 [astro-ph.HE], Submitted to JCAP.

The High-Altitude Water-Cherenkov (HAWC) experiment is a TeV gamma-ray observatory located at 4100 m above sea level on the Sierra Negra mountain in Puebla, Mexico. Each of the detector's 300 water-filled tanks is instrumented with four photomultiplier tubes that detect the Cherenkov radiation produced by charged particles created in extensive air showers. With an instantaneous field of view of 2 sr and a duty cycle exceeding 95%, HAWC is a powerful survey instrument sensitive to pulsar wind nebulae, supernova remnants, active galactic nuclei, and other gamma-ray sources. The mechanisms of particle acceleration at these sites can be probed by measuring their emitted photon energy spectra. To this end, we have developed an event-by-event method for reconstructing the energies of HAWC gamma-ray events using an artificial neural network. We will show that this new technique greatly improves HAWC's energy resolution and enables it to precisely resolve energies as high as 100 TeV in Monte Carlo. We will also present the progress towards measuring high-energy spectra with the new energy-estimation method.

We present a self-consistent model of the Fermi Bubbles, described as a decelerating outflow of gas and non-thermal particles produced within the Galactic center region, on a $\sim 100$ Myr timescale. Motivated by observations, we use an outflow with velocity O(100 km/s), which is slower than the velocities used in models describing the Bubbles as a more recent outburst. We take into account cosmic-ray (CR) energy losses due to proton-proton interactions, and calculate the resulting gamma-ray emission. Our model can reproduce both the spatial morphology and the spectra of the Bubbles, on a range of different scales. We find that CRs diffusing and advecting within a breeze outflow result in an approximately flat surface brightness profile of the gamma-ray emission, as observed by Fermi satellite. Finally, we apply similar outflow profiles to larger Galactocentric radii, and investigate their effects on the CR spectrum and boron-to-carbon ratio. Hardenings can appear in the spectrum, even in cases with equal CR diffusion coefficients in the disk and halo. It is postulated that this hardening effect may relate to the observed hardening feature in the CR spectrum at a rigidity of $\sim 200$ GV.

Cosmic rays can be probed by their non thermal emission in the radio and in gamma-ray bands. One-zone models of cosmic rays have been used to match the integrated emission of starburst galaxies. We construct multi-dimensional models of the local starburst M82 using cosmic ray propagation code GALPROP. Using the integrated gamma-ray and radio spectra, along with the vertical distribution of radio emission along the minor axis, we constrain the gas density, magnetic field strength, and cosmic ray population. We show that the wind velocity and diffusion coefficient can be constrained by the morphology of the radio halo. We discuss the interplay between gas density, magnetic field, and outflow velocity and how they effect the emission. We comment on the energetics of cosmic ray species in the system. We provide direct constraints on the dynamical importance of cosmic rays in driving the outflow of the galaxy.

Advanced LIGO's ongoing observation runs provided humanity with the first direct detection of gravitational waves, just in time for the 100th anniversary of Einstein's prediction. Beyond the discovery, there is a growing focus on incorporating gravitational waves as a new window on questions from violent transients to cosmology. I will discuss some aspects of (i) the instrumental breakthroughs that enabled the unprecedented sensitivity reached by Advanced LIGO and (ii) the key scientific directions in which gravitational wave searches can be utilized, directly as well as in the context of multimessenger astronomy.

I present my recent paper arXiv:1704.05073 on making projections for measuring the black hole birth rate from the diffuse supernova neutrino background (DSNB) by future neutrino experiments, and the information which can be gained by combining this with the merger rate from LIGO. The DSNB originates from neutrinos emitted by all the supernovae in the Universe, and is expected to be made up of two components: neutrinos from neutron-star-forming supernovae, and a sub-dominant component at higher energies from black-hole-forming "unnovae". We perform a Markov Chain Monte Carlo analysis of simulated data of the DSNB in an experiment similar to Hyper Kamiokande, focusing on this second component. Since the only evidence for unnovae comes from simulations of collapsing stars, we choose two sets of priors: one where the unnovae are well-understood and one where their neutrino emission is poorly known. By combining the black hole birth rate from the DSNB with projected measurements of the black hole merger rate from LIGO, we show that the fraction of black holes which lead to binary mergers observed today ϵ could be constrained to be within the range 8⋅10^−4≤ϵ≤5⋅10^−3, after ten years of running an experiment like Hyper Kamiokande.

We study gravitational wave (GW) production from bubble dynamics during a cosmic first-order phase transition by using the method of relating the GW spectrum to the two-point correlation function of the energy-momentum tensor < T(x) T(y) >. We adopt the thin-wall approximation but not the envelope approximation, and take the (long-lasting) non-envelope parts into account by assuming free propagation after collision. We first write down the analytic expressions for the spectrum, and then evaluate them with numerical methods. As a result, the growth and saturation of the spectrum are observed as a function of the duration time of the non-envelope parts. It is found that the IR region of the spectrum shows a significant enhancement compared to the one with the envelope approximation, growing from $f^3$ to $f^1$ in the long-lasting limit. In addition, we find saturation in the spectrum in the same limit, indicating a decrease in the correlation of the energy-momentum tensor at late times. Our results are relevant to GW production from bubble collisions and sound waves.

With the discovery of binary black hole mergers by LIGO, the era of gravitational wave (GW) astronomy and multi-messenger astronomy including GWs has begun. As the advanced LIGO and Virgo detectors approach design sensitivity in the next few years, exciting discoveries are expected to be made, including neutron star mergers, which are among the most promising GW events for multi-messenger astronomy. In this talk, I will present recent results from general-relativistic magnetohydrodynamic simulations of the merger and long-term post-merger evolution, and discuss how multi-messenger observations of NS mergers may represent the key to understand and solve several long-standing problems in astrophysics; these include the origin and generation of GWs and accompanied electromagnetic transients across the electromagnetic spectrum including short gamma-ray bursts and kilonovae, the properties of nuclear matter at high densities, and the origin of the heavy elements in the universe.

Coffee Break in the Oak Room

The Astrophysical Multimessenger Observatory Network (AMON), will connect observatories from around the world, enabling real-time coincidence searches of all four messengers (neutrinos, cosmic rays, gamma rays, and gravitational waves) and rapid follow-up observations of these alerts. AMON’s first real-time alerts were commissioned in 2016 with “pass-through” notices of IceCube likely-cosmic (HESE and EHE type) neutrino events, leading to multiple follow-up campaigns which have been reported through the GCN circulars. Looking ahead, AMON's first bona-fide multimessenger real-time alerts are planned to be high-energy neutrino + gamma-ray (“nu + gamma”) alerts resulting from coincidence of IceCube neutrinos and Swift, Fermi, or High-Altitude Water Cherenkov (HAWC) gamma-ray transients or subthreshold signals. The talk will summarize key properties of current alert streams and preview the expected properties of upcoming nu+gamma AMON Alerts.

Fast radio bursts (FRBs) are non-periodic millisecond radio outbursts that are thought to be of astrophysical origin. Since the first FRB was discovered by the Parkes Radio Telescope in 2007, a total of 23 FRBs with unique locations (FRB 121102 has repeated dozens of times) have been observed to date, with multiple radio telescopes. Although the nature of the FRBs is still largely unknown, the high dispersion measures of the FRBs indicate that they are most likely originating from extragalactic sources. A large multitude of models have been proposed to explain the FRB phenomena, most of which involve strong magnetic fields and are of leptonic nature. Currently, there are no concrete models predicting high-energy neutrinos from FRBs, while in principle a strongly magnetized environment such as that from a magnetar could produce short radio bursts due to the volatility of the magnetic fields, and having hadronic processes present at the same time. We will present the results from a recent search for high-energy neutrinos coincident spatially and temporally with FRBs in 6 years of IceCube data.

Recently a repeating fast radio burst (FRB) 121102 has been confirmed to be an extragalactic event and a persistent radio counterpart has been identified. One of the leading models is the young neutron star model, in which a pulsar (or magnetar) of $\leq$ 100 yrs-old surrounded by a wind nebula and supernova remnant are considered and connections between FRBs and luminous pulsar-driven supernovae are predicted. I will discuss multi-messenger/multi-wavelength approaches to testing the scenario.

IceCube has reported discovery of the first high-energy astrophysical neutrino candidates, however the nature of the sources responsible for these neutrinos - potentially also the sources of the highest-energy cosmic rays - is still unknown and no high-confidence electromagnetic counterparts to any of the neutrino events have yet been detected. If the sources producing these highest-energy cosmic neutrinos are transient, they may be identifiable in rapid-response observations at Swift. The possibility of discovering multimessenger transient sources in this fashion is one of the main motivations for the Astrophysical Multimessenger Observatory Network (AMON). I will present the results of the first Swift satellite follow-up campaigns seeking to identify transient or variable X-ray or UV/optical sources that might be associated with the high-energy neutrinos detected by the IceCube Neutrino Observatory. Real-time public alerts providing coordinates and arrival times of high-energy neutrino events have been provided by IceCube and distributed via AMON and Gamma-Ray Coordinates Network (GCN) since April 2016.

Knowledge of the energy dependence of the 3He-to-4He flux ratio (3He/4He) is important in understanding the propagation of cosmic rays. As 3He is assumed to be produced by interactions of heavier nuclei with the interstellar matter, the 3He/4He ratio is a powerful tool for determining the amount of interstellar material traversed by cosmic rays. AMS results are based on 9 million 3He events and 56 million 4He events collected in the first five years of operation onboard the ISS. The precise measurement of the 3He/4He ratio from 0.7 GeV/n to 10GeV/n is presented for the first time. The AMS results are unique and distinct from all the previous data.

Supernova remnants are known to be the main sources of galactic cosmic-rays. They could also be a possible explanation for rise of the positron fraction, if secondary positrons are produced and then accelerated around the supernova shock front. Yet, if secondary positrons are stochastically accelerated in such shocks, other secondary cosmic ray species will also be accelerated. Using recent measurements of the cosmic-ray antiproton and proton fluxes in the energy range of 1 – 1000 GeV, we study the contribution to the antiproton to proton ratio from stochastically accelerated secondary antiprotons in SNRs. We consider several well-motivated models for cosmic-ray propagation in the interstellar medium and marginalize our results over the uncertainties related to the antiproton production cross section and the time-, charge-, and energy-dependent effects of solar modulation. We find that the increase in the antiproton to proton ratio at energies above 100 GeV cannot be accounted for within the context of conventional cosmic-ray propagation models and that there is statistical evidence for an additional component that could be provided by the stochastically accelerated secondary antiprotons. Under the same conditions in SNRs, we show that accelerated secondary positrons, can account for a significant fraction of the observed positron flux excess.

The role of cosmic rays generated by supernovae and young stars has very recently begun to receive significant attention in studies of galaxy formation and evolution due to the realization that cosmic rays can efficiently accelerate galactic winds. Microscopic cosmic ray transport processes are fundamental for determining the efficiency of cosmic ray wind driving. Previous studies focused on modeling of cosmic ray transport either via a constant diffusion coefficient or via streaming proportional to the Alfven speed. However, in predominantly neutral gas, cosmic rays can propagate faster than in the ionized medium and the effective transport can be substantially larger; i.e., cosmic rays can decouple from the gas. We perform three-dimensional magnetohydrodynamical simulations of patches of galactic disks including the effects of cosmic rays. Our simulations include the decoupling of cosmic rays from the neutral interstellar medium. We find that, compared to the ordinary diffusive cosmic ray transport case, accounting for the decoupling leads to significantly different wind properties such as the gas density and temperature, significantly broader spatial distribution of cosmic rays, and larger wind speed. These results have implications for X-ray, gamma-ray and radio emission, and for the magnetization and pollution of the circumgalactic medium by cosmic rays.

We evaluated flux of cosmic ray anti-deuteron and anti-Helium3 from secondary astrophysical production. The production cross section at proton-proton collision is one of the most important input parameter to determine the secondary cosmic ray flux. However, composite (anti-)nuclei production cross section is very small and the cross section data at collider experiments is quite limited. That is why proton-heavy ion and heavy ion-heavy ion collision data are often used to determine anti-nuclei production cross sections in the literature. In heavy ion collision, physical volume of hadron emission region is larger than that of proton-proton collision. Also, in nuclear physics, it is known that composite nuclei production rate obeys a scaling law with the volume of emission region. However, this point has been neglected in the calculation of cosmic ray flux. We applied this scaling law to calculate anti-deuteron and anti-Helium3 flux. Our result is larger than the previous works by 1-2 orders of magnitudes. In particular, secondary anti-Helium3 flux could be within the reach of a five-year exposure of AMS-02.

Measurements of the Geminga and B0656+14 pulsars by HAWC and Milagro indicate that these objects generate significant fluxes of very high-energy electrons. From the very high-energy gamma-ray intensity and spectrum of these pulsars, one can calculate their expected contributions to the local cosmic-ray positron spectrum. From these considerations, we find that pulsars produce a flux of high-energy positrons that is similar in spectrum and magnitude to the positron fraction measured by PAMELA and AMS-02. In light of this result, we conclude that it is very likely that pulsars provide the dominant contribution to the long perplexing cosmic-ray positron excess. I will also discuss the implications of these results for pulsars in the Galactic Center region.

The CALorimetric Electron Telescope (CALET) space experiment, which has been developed by Japan in collaboration with Italy and the United States, is a high-energy astroparticle physics mission to be installed on the International Space Station (ISS). The primary goals of the CALET mission include investigating possible nearby sources of high energy electrons, studying the details of galactic particle propagation and searching for dark matter signatures. During a two-year mission, extendable to five years, the CALET experiment will be measureing the flux of cosmic-ray electrons (including positrons) to 20 TeV, gamma-rays to 10 TeV and nuclei with Z=1 to 40 up to 1,000 TeV. The instrument consists of two layers of segmented plastic scintillators for the cosmic-ray charge identification (CHD), a 3 radiation length thick tungsten-scintillating fiber imaging calorimeter (IMC) and a 27 radiation length thick lead-tungstate calorimeter (TASC). CALET has sufficient depth, imaging capabilities and excellent energy resolution to allow for a clear separation between hadrons and electrons and between charged particles and gamma rays. The instrument was launched on August 19,2015 to the ISS. Since the start of operation, a continuos observation has successfully being kept. We will have a summary of the CALET observation: 1) Electron energy spectrum, 2) Proton and Nuclei spectrum, 3) Gamma-ray observation, with results of the performance study on orbit. We also present the results of observations of the electromagnetic counterparts to LIGO-VIRGO gravitational wave events.

Coffee Break in the Oak Room

The objectives of the Pierre Auger Observatory are to probe the origin and characteristics of cosmic rays above $10^{17}$ eV and to study the interactions of these, the most energetic particles observed in nature. The Observatory design features an array of water Cherenkov stations deployed over a surface of $3000$ km$^2$ overlooked by fluorescence telescopes. This design and a sophisticated data analysis pipeline provide us with a large set of high quality data, which has led to major breakthroughs in the last decade. The Observatory has recorded data from an exposure exceeding $60,000$ km$^2$ sr yr since its beginning in 2004. The latest results together with systematic uncertainties are discussed in this talk. A major upgrade, known as AugerPrime, with an emphasis on improved mass composition determination using the surface detector is also presented.

The Telescope Array (TA) measures the properties of ultra high energy cosmic ray (UHECR) induced extensive air showers. TA employs a hybrid detector comprised of a large surface array of scintillator detectors overlooked by three fluorescence telescopes stations. The TA Low Energy extension (TALE) detector has operated as a monocular Cherenkov/fluorescence detector for nearly three years, and has just been complemented by a closely spaced surface array to commence data taking in hybrid mode. The TAx4 upgrade is underway and aims to, as the name suggests, quadruple the size of the surface array to improve statistics at the highest energies (post-GZK events). In this talk we will describe the experiment and it's various upgrades, and we will summarize the latest results on the energy spectrum, composition, and anisotropy of UHECR, obtained with nine years of observation. The energy spectrum measured by the TALE FD, extending from a low energy of 4 PeV to a high of few EeV, will be presented in some detail.

The flux of cosmic rays is observed at the Pierre Auger Observatory spanning almost three decades in energy. This energy range is possible by combining the measurements from the nested 1500 m and 750 m surface detector arrays. The energy scale relies on the almost calorimetric energy measurements performed with Auger's fluorescence detectors. With a total exposure of about 52000 [km^2 sr yr] the observatory has accumulated large statistics which allows for a precise measurement of the flux spectrum above 300 PeV. A spectral shape, motivated by potential cosmic ray source models, is used to identify the spectral features including the ankle and the suppression at the highest energies. The shape of the spectrum is discussed along with its implications.

The Fluorescence detector Array of Single-pixel Telescopes (FAST) is a design concept for the next generation of Ultra-High-Energy Cosmic Ray (UHECR) observatories, addressing the requirements for a large-area, low-cost detector suitable for measuring the properties of the highest energy cosmic rays. In the FAST design, a large field of view is covered by a few pixels at the focal plane of an optical apparatus. Motivated by the successful detection of UHECRs using a prototype comprised of a single 200 mm PMT and a 1 square meter Fresnel lens system, we have developed a new full-scale prototype consisting offour 200 mm PMTs at the focus of a 1.6m segmented mirror. In October 2016 we installed the full-scale prototype at the Telescope Array site in central Utah, USA, and began steady data acquisition. We report on first results of the full-scale FAST prototype, including measurements of artificial light sources, distant ultraviolet lasers, and UHECRs.

Present measurements are not able to firmly single out nature’s choice for the neutrino mass hierarchy. Consequently, in the absence of a robust measurement of the neutrino mass ordering, a desirable bound on the neutrino mass would be one which relies on the less informative possible assumption about the hierarchical distribution of the total mass among the three eigenstates. We will discuss a novel method to quantify the sensitivity of cosmological data to the neutrino mass hierarchy in the context of Bayesian analysis.

In recent years, advances in numerical methods have allowed us to calculate precision observables with fewer assumptions. Here I will discuss two of these observables, Hubble Diagrams and the Weak Lensing Convergence Power Spectrum. I will comment on the role that inhomogeneities, entering at high order, effects cosmological measurements.

I will describe how statistical anisotropies, such as dipole modulations of the cosmic microwave background temperature and polarization fluctuations, are more likely if the primordial fluctuations are non-Gaussian. I will then discuss the implications of this effect for observations in the cosmic microwave background temperature and polarization anisotropies, and how such observations can be used to constrain the level of non-Gaussianities in the primordial fluctuations. In particular, I will focus on how the addition of statistical anisotropy information from E-mode polarization can help tighten current primordial non-Gaussianity constraints.

In this talk we will present the latest development of the CLUMPY code. The first version aimed at the calculation of the astrophysical J-factors from dark matter annihilation/decay in any galaxy or galaxy cluster dark matter halo including substructures. While refining on several aspects of the first version (halo-to-halo concentration scatter, multi-level boost factors, and triaxiality), the second release additionally provides i) a full refactoring of the I/O, ii) skymaps for γ-ray and ν fluxes from generic annihilation/decay spectra and the associated angular power spectrum, and iii) a Jeans analysis module to obtain dark matter density profiles and J-factors from kinematic data in relaxed spherical systems (e.g., dwarf spheroidal galaxies). After presenting some examples of these functionalities, we will also discuss the ongoing development of a third release that will include the overall extragalactic γ-ray flux from cosmic dark matter structure.

Particles present in the early Universe can leave observable imprints if they affect dark matter properties after dark matter has gone out of equilibrium with the thermal bath. We will investigate such possibilities and their associated observable signatures in several well-motivated dark matter frameworks.

Milky Way satellite dwarf galaxies are among the oldest, smallest, and most dark matter dominated galaxies in the known Universe. The study of these tiny galaxies can help shed light on the nature of dark matter and the mysteries of galaxy formation. Over the last two years, efforts using the Dark Energy Camera (DECam) have nearly doubled the known population of Milky Way satellite galaxies. However, to date, only a fraction of the southern sky has been uniformly imaged by DECam. We will present results from two new surveys, the Magellanic Satellites Survey (MagLiteS) and the Blanco Imaging of the Southern Sky (BLISS) survey, which are using DECam to image the southern sky to unprecedented depths.

Coffee Break in the Oak Room

Hyper Suprime-Cam (HSC) is an imaging camera mounted at the Prime Focus of the Subaru 8.2-m telescope operated by the National Astronomical Observatory of Japan on the summit of Maunakea in Hawaii. A consortium of astronomers from Japan, Taiwan and Princeton University is carrying out a three-layer, 300-night, multiband survey from 2014-2019 with this instrument. In this talk, I will focus on the HSC survey Wide Layer, which will cover 1400 square degrees in five broad bands (grizy), to a 5 sigma point-source depth of r~26. We have covered 240 square degrees of the Wide Layer in all five bands, and the median seeing in the i band is 0.60 arcseconds. This powerful combination of depth and image quality makes the HSC survey unique compared to other ongoing imaging surveys. In this talk I will describe the HSC survey dataset and the completed and ongoing science analyses with the survey Wide layer, including galaxy studies, strong and weak gravitational lensing, but with an emphasis on weak lensing. I will demonstrate the level of systematics control, the potential for competitive cosmology constraints, some early results, and describe some lessons learned that will be of use for other ongoing and future lensing surveys.

I will present a suite of new algorithms for measuring higher-point statistics from large-scale structure surveys. I will begin with a transformatively-fast algorithm that enables computation of the isotropic 3-point correlation function scaling as the number of galaxies squared. This algorithm was applied to BOSS data to make the first high-significance detection of the Baryon Acoustic Oscillations as well as to constrain novel forms of biasing. I will then present a generalization of the algorithm allowing computation of the anisotropic 3PCF. I'll close by showing how the fundamental kernel of these algorithms enables measurement of N-point functions for any desired N scaling as the square of the number of galaxies.

We analyze the Extended Quasi-Dilaton Massive Gravity model around a Friedmann-Lemaitre-Robertson-Walker cosmological background. We present a careful stability analysis of asymptotic fixed points. We find that the traditional fixed point cannot be approached dynamically, except from a perfectly fine-tuned initial condition involving both the quasi-dilaton and the Hubble parameter. A less-well examined fixed-point solution, where the time derivative of the 0-th Stuckelberg field vanishes $\dot\phi^0=0$, encounters no such difficulty, and the fixed point is an attractor in some finite region of initial conditions. We examine the question of the presence of a Boulware-Deser ghost in the theory. We show that the additional constraint which generically allows for the elimination of the Boulware-Deser mode is $\textit{only}$ present under special initial conditions. We find that the only possibility corresponds to the traditional fixed point, and the initial conditions are the same fine-tuned conditions that allow the fixed point to be approached dynamically. Statement of Acknowledgement: This presentation was made possible, in part, through financial support from the School of Graduate Studies at Case Western Reserve University.

In this talk, I will show that metal poor halo stars have similar kinematics as dark matter in the solar neighborhood, using the hydrodynamic zoom-in simulation Eris of the Milky Way. Within this expectation, I extract the first empirically-determined dark matter velocity distribution using the velocity dispersions of the halo stars as measured by the Sloan Digital Sky Survey, and show that using this newly-found velocity distribution, the direct detection limits on dark matter scattering off nuclei are loosened by almost an order of magnitude at low dark matter masses.

Predictions for direct dark matter searches rely on the knowledge of the local speed distribution of dark matter particles. This distribution can be derived within a dynamically constrained Milky Way mass model using the Eddington formalism or some extended versions of it. This method, however, can lead to unconsistent or unphysical solutions, depending on the details of the mass model. I will discuss the limitations of the method and its applicability to predictions in direct detection. I will also discuss how it may, or may not, capture the actual dynamics of dark matter by comparing with cosmological simulation results.

The interpretation of dark matter direct detection results is complicated due to the unknown distribution of dark matter in our local neighborhood. Astrophysical uncertainties in the dark matter distribution are a major barrier preventing a precise determination of the properties of the dark matter particle. High resolution cosmological simulations of galaxy formation including baryons have recently become possible, and provide important information on the properties of the dark matter halo. I will discuss the local dark matter density and velocity distribution of Milky Way-like galaxies obtained from recent hydrodynamical simulations. In particular I will discuss the effect of baryons on the dark matter velocity distribution, the prevalence of dark disks, and implications for dark matter direct detection.

Many dark matter studies have considered indirect detection (χχ → ff), direct detection (χf →χf ), and collider searches (ff → χχ). We propose a new strategy in searching for dark matter elastic cross section by considering cosmic-ray propagation in the galactic dark matter halo. We find that cosmic rays can lose significant fraction of their energy through scattering with dark matter (fχ → fχ). Using existing cosmic-ray data and a simple cosmic-ray propagation model, we study the qualitative effects of dark matter scattering on cosmic-ray propagation and obtain new constraints of dark matter elastic cross sections on light dark matter (keV–GeV), a regime that is difficult for traditional direct detection experiments to probe.

In this talk, we discuss the effects of a non-negligible threshold energy on our model-independent methods developed for reconstructing WIMP properties by using measured recoil energies in direct Dark Matter detection experiments directly. Our expressions for reconstructing the mass and the (ratios between the) spin-independent and the spin-dependent WIMP-nucleon couplings have been modified. We will focus on low-mass (m_chi <~ 50 GeV) WIMPs and present some (preliminary) numerical results obtained by Monte-Carlo simulations.

We discuss direct detection of WIMP dark matter in two benchmark cases: a Majorana fermion that primarily interacts via the Z-boson, and a Majorana fermion whose relic density is primarily set via co-annihilations with colored partners. We discuss the Z-mediated case with reference to a simple UV-completion, the singlet doublet model. We discuss the co-annihilation case with reference to stop co-annihilation in the Minimal Supersymmetric Standard Model. We find that Z-mediated Dark Matter is likely to be largely probed by future experiments, but co-annihilating Dark matter may present a formidable challenge.

Coffee Break in the Oak Room

ABRACADABRA is a proposed experiment to search for ultralight (10^-14 - 10^-6 eV) axion dark matter. When ultralight axion dark matter encounters a static magnetic field, it sources an effective electric current that follows the magnetic field lines and oscillates at the axion Compton frequency. In the presence of axion dark matter, a large toroidal magnet will act like an oscillating current ring, whose induced magnetic flux can be measured by an external pickup loop inductively coupled to a SQUID magnetometer. The readout circuit can be broadband or resonant and both are considered. ABRACADABRA is fielding a 10-cm prototype in 2017 with the intention of scaling to a 1m^3 experiment. The long term goal is to probe QCD axions near the GUT-scale. In this talk I will review the design, sources of noise, and sensitivity of the experiment.

The Axion Dark Matter Experiment, ADMX, is taking data with sensitivity to a possible dark matter candidate that would also solve the strong-CP problem of QCD. The experiment, it's status, and preliminary results will be presented along with a path to cover much of the highly motivated parameter space. Page 51

The nature of dark matter (DM) remains one of the fundamental questions in cosmology. Axions are one of the current leading candidates for the hypothetical, non-baryonic DM. Especially in the light of LHC slowly closing in on WIMP searches, axions and axion-like particles (ALPs) provide a viable alternative approach to solving the dark matter problem. The fact that makes them very appealing is that they were initially introduced to solve a long-standing QCD problem in the Standard Model of particle physics. Helioscopes are searching for axions produced in the core of the Sun via the Primakoff effect. The International Axion Observatory (IAXO) is a next generation axion helioscope aiming at a sensitivity to the axion-photon coupling of 1 - 1.5 orders of magnitude beyond the currently most sensitive axion helioscope (CAST). IAXO will be able to challenge the stringent bounds from SN1987A and test the axion interpretation of anomalous white-dwarf cooling. Beyond standard axions, this new experiment will be able to search for a large variety of ALPs and other novel excitations at the low-energy frontier of elementary particle physics. Mini-IAXO is proposed as a small pilot experiment increasing the sensitivity to axion-photon couplings down to a few 10$\times$11 GeV$^{-1}$. This contribution will introduce the IAXO and mini-IAXO experiments and outline the expected science reach. This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344.

The Axion Resonant InterAction Detection Experiment (ARIADNE) will search for evidence of the QCD axion using nuclear magnetic resonance to search for a short-range spin-dependent interaction in the sub-millimeter range, which results from the Axion. ARIADNE features spin polarized 3He interacting with a rotating unpolarized tungsten mass as a probe for this interaction. We will outline the concept of the measurement and describe the status of the R&D progress to date.

While the discovery of the Higgs boson at the LHC experimentally confirms the widely successful Standard Model (SM) of particle physics, the theory still falls short of explaining several fundamental features of our Universe. A major shortcoming is the SM’s silence on the nature of Dark Matter (DM). Currently, axions and WIMPs are the leading DM candidates with axions simultaneously addressing an additional weakness of the SM, i.e. its inability to explain why strong interactions do not violate charge-parity symmetry as expected from theory. Non-QCD axions on the other hand appear naturally in extensions of the SM, e.g. string theory. If axions exist, they will be created in great numbers in the solar core by the Primakoff effect, via the interaction of a photon from the core’s radiation field with a virtual photon in a nucleus. By the inverse mechanism, one can generate an X-ray flux beyond the solar core. Extensive ground-based searches, notably the CAST experiment at CERN and the proposed next generation helioscope IAXO, use laboratory magnets for the reverse conversion. We employ a novel approach using solar observations of NASA’s hard x-ray astrophysics mission NuSTAR (Nuclear Spectroscopic Telescope Array) to search for the same process via magnetic fields in the solar corona, which, although weaker than those of laboratory magnets, are much more extensive in scale. We will report on the latest results of our research. This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344.

The number of nonrelativistic axions can be changed by inelastic reactions that produce relativistic axions or photons. Any even number of nonrelativistic axions can scatter inelastically into two relativistic axions. Any odd number of axions can annihilate into two photons. This reaction produces a monochromatic radio-frequency signal at an odd-integer harmonic of the fundamental frequency set by the axion mass. The loss rates of axions from axion stars through these inelastic relations are calculated using the framework of a nonrelativistic effective field theory. Odd-integer harmonics of a fundamental radio-frequency signal provide a unique signature for collapsing axion stars or any dense configuration of axions.

ABRACADABRA10cm is a new experiment which seeks to detect axion dark matter through its interactions with the electromagnetic field. The experiment, which is planned to start collecting data this year, will probe unstudied regions of axion parameter space and lay the groundwork for future, larger-scale efforts. I will discuss the results of numerical and analytical work towards understanding the signatures of axion dark matter substructure in the experiment. In particular, I will focus on the effects of dark matter streams, especially as informed by cosmological N-body simulation data.

The Cherenkov Telescope Array (CTA) will be a new observatory to study very-high-energy gamma-ray sources. It is designed to achieve an order of magnitude improvement in sensitivity in the 20 GeV to 300 TeV energy band compared to currently operating instruments: VERITAS, MAGIC, and H.E.S.S. CTA will probe known sources with unprecedented sensitivity, angular resolution, and spectral coverage, while also detecting hundreds of new sources. This presentation describes the science drivers for CTA and the status of the project with an emphasis on the planned US contribution.

The ALPACA (Andes Large area PArticle detector for Cosmic ray physics and Astronomy) experiment is aimed at observing cosmic gamma rays above 10 TeV in the southern sky with wide field of view and high sensitivity. We will construct an 83,000 m^2 surface air-shower array and a 5,400 m^2 underground muon detector array, on a highland (Chacaltaya Hill) at the altitude of 4,740 m halfway up Mt. Chacaltaya on the outskirts of La Paz, Bolivia. Prior to the construction of the full ALPACA array, we are planning to build a 1/10-scale prototype air-shower array. In this talk, the overview and current status of the ALPACA experiment will be reported.

The MeV domain is one of the most underexplored windows on the Universe. From astrophysical jets and extreme physics of compact objects to a large population of unidentified objects, fundamental astrophysics questions can be addressed by a mission that opens a window into the MeV range. AMEGO is a wide-field gamma-ray telescope with sensitivity from ~200 keV to >10 GeV. AMEGO provides three new capabilities in MeV astrophysics: sensitive continuum spectral studies, polarization measurements, and nuclear line spectroscopy. AMEGO will consist of four hardware subsystems: a double-sided silicon strip tracker with analog readout, a segmented CZT calorimeter, a segmented CsI calorimeter and a plastic scintillator anticoincidence detector, and will operate primarily in an all-sky survey mode. In this presentation we will describe the AMEGO mission concept and scientific performance.

The Lunar Occultation Explorer (LOX) is a paradigm shift - a next-generation mission concept that will provide new capabilities in time-domain nuclear astrophysics and establish the Moon as a platform for nuclear astrophysics. Currently under review by NASA’s Explorer Program, LOX's performance requirements are driven by focused science goals designed to resolve the enigma of Type-Ia supernova (SNeIa) and their role in galactic evolution and cosmology. LOX will survey and continuously monitor the Cosmos in the MeV regime (0.1-10 MeV), a unique capability that supports both the primary science goals as well as multi-messenger detection and monitoring campaigns, by leveraging the Lunar Occultation Technique (LOT). Key benefits of the LOX/LOT approach include maximizing the ratio of sensitive-to-total deployed mass, low implementation risk, and demonstrated operational simplicity that leverages extensive experience with planetary orbital geochemistry investigations. LOX will also deliver a time-domain survey of the nuclear cosmos. Proof-of-principle efforts have validated all aspects of the mission using previously deployed lunar science assets, including the first high-energy gamma-ray source detected at the Moon. LOX mission design, performance, and science will be presented.

We present some of the main results from the Third Catalog of Hard Fermi-LAT Sources (3FHL). This catalog, based on the first 7 years of LAT data using the Pass 8 event-level analysis, contains 1556 sources characterized in the 10 GeV--2 TeV energy range. The sensitivity and angular resolution are improved by factors of 3 and 2 relative to the previous LAT catalog in this energy range (1FHL). Most 3FHL sources (79%) are extragalactic, while 9% are Galactic and 12% are unassociated (or associated with a source of unknown nature). The catalog includes 214 new gamma-ray sources. The 3FHL catalog provides an excellent opportunity to relate observations from space to those accessible from the ground (e.g. HESS, MAGIC, VERITAS, HAWC), including in the near future with the Cherenkov Telescope Array.

Coffee Break in the Oak Room

The High-Altitude Water Cherenkov (HAWC) TeV Gamma-Ray Observatory in Mexico is a wide-field-of-view telescope with a nearly 100 % duty cycle. It has been taking data with a complete detector configuration since spring 2015 and is particularly well suited to measure very energetic transient and extended gamma-ray emission in our Galaxy. In my presentation, I will give an overview of the most recent HAWC results relating to Galactic sources. This will include highlights from the 2HWC catalog, measurements of PWNe in the general Geminga region, and observations of binary systems and extended structures such as the Northern Fermi Bubble, molecular clouds, or diffuse emission at TeV energies.

The HAWC (High Altitude Water Cherenkov) observatory recently published their second source catalog with 39 very high energy gamma-ray sources based on 507 days of exposure time. We studied thirteen HAWC sources without known counterparts with VERITAS and Fermi-LAT data. VERITAS, an array of four imaging atmospheric Cherenkov telescopes observing gamma rays with energies higher than 85 GeV, can provide a more detailed image of the source with much shorter exposure time and with better angular resolution. With Fermi-LAT data, we searched for the counterparts at lower energies (E>10 GeV). VERITAS found weak gamma-ray emission in the region of PWN DA495 coinciding with 2HWC J1953+294 in this follow-up study. We will present results focusing on the PWN DA495 region and the SNR G54.1+0.3 region where Fermi-LAT detected a GeV counterpart of SNR G54.1+0.3, a known TeV source detected by both VERITAS and HAWC.

The 2HWC gamma-ray catalog was recently released using 17 months of data from the HAWC observatory, a TeV surveying instrument located in Mexico. A total of 39 sources were detected, of which ~40% are not near known TeV sources and over half do not have clear association with known astrophysical sources. Many are extended and encompass multiple known X-ray and gamma-ray sources. In an effort to identify counterparts that could explain the complex morphology seen by HAWC and understand the emission mechanisms, follow-up observations by VERITAS in TeV have confirmed some detections. We obtained additional follow-up time for two Galactic HAWC sources in hard X-rays by NuSTAR. These are the initial observations of the HAWC-VERITAS-NuSTAR Galactic Survey Legacy program.

Gamma ray astronomy provides a powerful way to study particle acceleration and diffusion within high-energy astrophysical phenomena such as supernova remnants and pulsar wind nebulae. Constructing a coherent physical picture of these sources requires the ability to detect extended regions of gamma-ray emission, the ability to analyze small-scale spatial variation within these regions, and the ability to synthesize data from multiple observatories across multiple wavebands. Air Cherenkov telescopes provide fine angular resolution (<1 degree), but their limited fields of view typically make detection of extended sources challenging. Maximum likelihood methods are well-suited to simultaneous analysis of multiple fields with overlapping sources, and to combining data from multiple gamma-ray observatories. These methods allow for estimation of the cosmic ray background for air Cherenkov observations for sources as large as the entire telescope field of view. We report here on the development of a maximum likelihood approach for the air Cherenkov observatory VERITAS and discuss potential applications of this method.

The Cygnus region consists of multiple gamma-ray source types such as pulsar wind nebulae (PWN), supernova remnants, binary systems, and star clusters. Several gamma-ray instruments have observed gamma-ray sources in this region. For instance, Fermi-LAT found gamma-ray emission at GeV energies due to a Cocoon of freshly accelerated cosmic rays, which is co-located with a known PWN seen by several TeV gamma-ray observatories. TeV J2032+4130 is likely powered by the pulsar PSR J2032+4127 based on the multi-wavelength observation and asymmetric morphology reported by VERITAS. The High Altitude Water Cherenkov (HAWC) observatory has reported five sources within the Cygnus region, three of which lie in the vicinity of the cocoon region reported by Fermi-LAT. This presentation will discuss the analysis of data collected with the HAWC instrument to provide a deeper understanding of the Cygnus cocoon. The study of HAWC data will provide more information regarding the morphology, emission origin, and the correlation with the GeV emission.

Giant Molecular Clouds (GMC) are large reservoirs of gas and dust in the galaxy, which makes them ideal for the production of gamma-ray emission due to the interaction of cosmic rays with the ambient gas. This gamma-ray emission is part of the galactic diffuse gamma-ray emission, which is useful for tracing the propagation and distribution of cosmic rays throughout our Galaxy. The search of gamma-ray emission from GMCs may allow us to probe the flux of cosmic rays in distant galactic regions and compare it with the local cosmic ray flux measured at Earth. The High Altitude Water Cherenkov (HAWC) Observatory is located at 4100 m above sea level in Mexico. It is designed to measure high-energy gamma rays between 300 GeV to 100 TeV. HAWC possesses a large field of view of 2 sr and good sensitivity to spatially extended sources, which currently makes it the best suited ground-based observatory to detect extended regions. HAWC data is used to search for gamma-ray emission from Aquila Rift, Hercules and Taurus GMCs. Preliminary results will be presented.

The High Altitude Water Cherenkov (HAWC) gamma-ray observatory is a continuously operated, wide field-of-view (FOV) observatory sensitive to 100 GeV - 100 TeV gamma rays and cosmic rays. HAWC has been making observations since summer 2012 and officially commenced data-taking operations with the full detector in March 2015. With an FOV of 2 steradians, HAWC observes 2/3 of the sky in 24 hours. HAWC is sensitive to transients and also to galactic steady sources, including both point and more diffuse emission. HAWC can be used to search for astrophysical signatures of dark matter (DM) and primordial black holes (PBHs). I will present HAWC's latest results on searches for evaporating PHBs, which would appear in transients in our archived data, but with energy and time signatures distinct from GRBs. HAWC’s measurement of the spatial distribution of TeV gamma ray emission from the region surrounding nearby pulsars is also relevant to interpretation of the excess of positrons observed at Earth. I will also present our measurements on TeV gamma ray emission near Geminga and the Monogem pulsar.

Neutrino interactions, though feeble, are tremendously important in particle physics and astrophysics. Still, at neutrino energies above ~350 GeV there has been, up to now, no direct experimental information on neutrino interactions; calculations rely on extrapolations from lower energies. Now, for the first time, we can measure the neutrino-nucleon cross section at the TeV scale and above, thanks to the recent discovery, by IceCube, of high-energy astrophysical neutrinos. We will show new cross section measurements extracted from the 4-year sample of IceCube High Energy Starting Event showers between 20 TeV and 2 PeV. The measurements agree with standard cross-section calculations and constrain new physics beyond the Standard Model at these energies.

IceCube observation of high-energy astrophysical neutrinos has opened the astrophysical neutrino window. As we accumulate statistics IceCube not only starts characterizing the astrophysical neutrino component, but also makes improved measurements of the highest energy atmospheric neutrinos. In this talk I will discuss how we can use both high-energy atmospheric neutrinos as well as astrophysical neutrinos as a probe of new physics.

The origin of the observed extraterrestrial neutrinos is still unknown, and their arrival directions are compatible with an isotropic distribution. This observation, together with dedicated studies of Galactic plane correlations, suggest a predominantly extragalactic origin. Dark matter-neutrino interactions, which have been extensively studied in cosmology, would thus lead to a slight suppression of flux at energies below a PeV and deficit of events in the direction of Galactic center, which would be seen by IceCube. I will present results of a recent analysis using the four-year high-energy starting event dataset to constrain the strength of dark matter-neutrino interactions and show that in spite of low statistics IceCube can probe regions of the parameter space inaccessible to current cosmological methods.

Some Planck-scale physics and quantum gravity models predict a slight violation of Lorentz invariance (LIV) at high energies. High-energy cosmic neutrino observations can be used to test for such LIV. Operators in an effective field theory (EFT) can be used to describe the effects of LIV. They can be used to describe kinematically allowed energy losses of possible superluminal neutrinos. These losses can be caused by both vacuum pair emission (VPE) and neutrino splitting. Assuming a reasonable distribution of extragalactic neutrino sources, we determined the resulting after-loss neutrino spectra using Monte Carlo propagation calculations. We then compared them with the neutrino spectrum observed by IceCube to determine the implications of our results regarding Planck-scale physics. If the drop off in the observed IceCube neutrino flux above 2 PeV is caused by LIV, a potentially significant pileup effect would be produced just below the drop-off energy in the case of CPT-even operator dominance. However, such a clear drop off effect would not be observed if a CPT-odd, CPT-violating term dominates.

We study Lorentz violation effects to flavor transitions of high energy astrophysical neutrinos. It is shown that the appearance of Lorentz violating Hamiltonian can drastically change the flavor transition probabilities of astrophysical neutrinos. Predictions of Lorentz violation effects to flavor compositions of astrophysical neutrinos arriving on Earth are compared with IceCube flavor composition measurement which analyzes astrophysical neutrino events in the energy range between $25~{\rm TeV}$ and $2.8~{\rm PeV}$. Such a comparison indicates that the future IceCube-Gen2 will be able to place stringent constraints on Lorentz violating Hamiltonian in the neutrino sector. We work out these expected constraints for different flavor structures of Lorentz violating Hamiltonian. In some cases these expected constraints can improve upon the current constraints obtained from other types of experiments by more than two orders of magnitudes.

If dark energy is some kind of scalar field rather than a cosmological constant and can interact with the neutrino sector, it might cause CPT/Lorentz violating effects and also modifies the neutrino oscillation phenomenology. The effects will be insignificantly small compared to the ordinary oscillation effect at low energies, but might become visible in very high energies, since the terms in the transition probability induced by interactions with dark energy do not depend on the energy, while the ordinary component decreases with 1/E. If such dark energy effects were found, it would be a strong indication that the nature of dark energy is different from a cosmological constant. We investigate the effect of such a dark energy interaction in the three-neutrino scheme and use IceCube data to put constraints on the new oscillation parameters that emerge from this interaction.

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Neutrino spectral indices Galactic vs. Extra-galactic sources, and potential use of Glashow events are analyzed.

The IceCube neutrino discovery was punctuated by three showers with $E_\nu$ ~ 1-2 PeV. Interest is intense in possible fluxes at higher energies, though a marked lack of $E_\nu$ ~ 6 PeV Glashow resonance events implies a spectrum that is soft and/or cutoff below ~few PeV. However, IceCube recently reported a through-going track event depositing 2.6 $\pm$ 0.3 PeV. A muon depositing so much energy can imply $E_{\nu_\mu} \gtrsim$ 10 PeV. We show that extending the soft $E_\nu^{-2.6}$ spectral fit from TeV-PeV data is unlikely to yield such an event. Alternatively, a tau can deposit this much energy, though requiring $E_{\nu_\tau}$ ~10x higher. We find that either scenario hints at a new flux, with the hierarchy of $\nu_\mu$ and $\nu_\tau$ energies suggesting a window into astrophysical neutrinos at $E_\nu$ ~ 100 PeV if a tau. We address implications, including for ultrahigh-energy cosmic-ray and neutrino origins.

After the discovery of extraterrestrial high-energy neutrinos, the next major goal of neutrino telescopes will be identifying astrophysical objects that produce them. The flux of the brightest source Fmax, however, cannot be probed by studying the diffuse neutrino intensity. We aim at constraining Fmax by adopting a broken power-law flux distribution, a hypothesis supported by observed properties of any generic astrophysical sources. The first estimate of Fmax comes from the fact that we can only observe one universe, and hence, the expected number of sources above Fmax cannot be too small compared with one. For abundant source classes such as starburst galaxies, this one-source constraint yields a value of Fmax that is an order of magnitude lower than the current upper limits from point-source searches. Then we derive upper limits on Fmax assuming that the angular power spectrum is consistent with neutrino shot noise yet. We find that the limits obtained with upgoing muon neutrinos in IceCube can already be quite competitive, especially for rare but bright source populations such as blazars. The limits will improve nearly quadratically with exposure, and therefore be even more powerful for the next generation of neutrino telescopes.

Neutrinos from supernovae (SNe) are crucial probes of explosive phenomena at the deaths of massive stars and neutrino physics. High-energy neutrinos are produced through hadronic processes by cosmic rays, which can be accelerated during interaction between the SN ejecta and circumstellar material (CSM). We investigate high-energy neutrino emission from Galactic SNe. Recent observations of extragalactic SNe have revealed that a dense CSM is commonly expelled by the progenitor star. We show that IceCube/KM3Net can detect about 10-1000 events from Type II-P/II-L SNe at a distance of 10 kpc. A successful detection will give us a multi-energy neutrino view of SN physics and new opportunities to study neutrino properties, as well as clues to the cosmic-ray origin. GeV-TeV neutrinos may also be seen by KM3Net, Hyper-Kamiokande, and PINGU.

Type IIn supernovae (SNe) explode in dense circumstellar media that have been modified by the SNe progenitors at their last evolutionary stages. The interaction of the freely expanding SN ejecta with the circumstellar medium gives rise to a shock wave propagating in the dense SN environment, which may accelerate protons to multi-PeV energies. Inelastic proton-proton collisions between the shock-accelerated protons and those of the circumstellar medium can lead to multi-messenger signatures. I will present our results on the diffuse neutrino emission from SNe IIn in comparison to IceCube observations. In particular, SNe IIn could be the dominant component of the diffuse astrophysical flux, only if 4 per cent of all core collapse SNe were of this type and 30 per cent of the shock energy was channeled to accelerated protons. Even more stringent constraints on the acceleration efficiency can be placed by the identification of a single SN IIn as a neutrino point source with IceCube using up-going muon neutrinos.

Star-forming and starburst galaxies are among candidate sources of high energy neutrino flux detected in the IceCube experiment. Previous studies mainly used simple correlations between gamma-ray and infrared luminosities and assume a common value of gamma-ray spectral index for all starburst galaxies, though it should depend on properties of individual galaxies. In this work, we present a new theoretical prediction of the gamma-ray and neutrino flux from star-forming galaxies by using a semi-analytical model of cosmological galaxy formation, which quantitatively reproduces many observations of local and high-redshift galaxies such as luminosity functions and the cosmic star-formation history. We construct realistic models of gamma-ray and neutrino emission from individual galaxies at various redshifts from their properties, taking into account the cosmic-ray production, propagation and interaction inside them, assuming the energy densities of cosmic-ray and magnetic field are in equilibrium in each galaxy. We calibrate our model by using data of local galaxies detected by Fermi-LAT to make reliable calculations. Our baseline model, which is in remarkable agreement with gamma-ray data of local star-forming galaxies, predicts that less than 10 % of IceCube data can be explained even with the most optimistic parameters. Therefore other sources are required to explain IceCube neutrinos.

High energy neutrinos have been detected by IceCube, but their origin remains a mystery. Determining the sources of this flux is a crucial first step towards multi-messenger studies. In this work we systematically compare two classes of sources with the data: galactic and extragalactic. We build a likelihood function on an event by event basis including energy, event topology, absorption, and direction information. We present the probability that each high energy event with deposited energy $E_{\rm dep}>60$ TeV in the HESE sample is galactic, extragalactic, or background. The galactic fraction of the astrophysical flux has a best fit value of $0.07^{+0.09}_{-0.06}$ and zero galactic flux is allowed at $1.2\sigma$.

Over the last 15 years, we have achieved a detailed understanding of the physics of radio emission from extensive air showers, and have consequently succeeded in developing sophisticated detection schemes and analysis approaches. In particular, we have demonstrated that the important air-shower parameters arrival direction, particle energy and depth of shower maximum can be reconstructed reliably from radio measurements, with both precision and accuracy comparable with those of other detection techniques. In this talk I will review the achievements of the radio detection technique and discuss the potential for future application in existing and new experiments for cosmic-ray detection.

We demonstrate here the ability of TREND, a self-triggered radio array, to autonomously detect and identify air showers induced by cosmic rays. TREND (Tianshan Radio Experiment for Neutrino Detection) is an array of 50 dipolar antennas, deployed over a total area of 1.5km² on the site of the 21CMA radio interferometer in the radio-quiet Tianshan mountains (China), and running between 2009 and 2014. TREND DAQ system was designed to allow for a trigger rate up to 200Hz per antenna, based on a very basic signal-over-threshold trigger condition. The reconstruction and discrimination of air showers from the ultra-dominant background noise is then performed through an offline treatment. We present here, for the first time, the complete analysis of the TREND data. We first detail the background-rejection algorithm which allowed to select about 500 air shower radio candidates from the ~10^9 radio pulses recorded with the TREND array. We then show that the distribution of the directions of arrivals of these 500 candidates is compatible with what is expected for air showers. We finaly compute the TREND air shower detection efficiency, thanks to an end-to-end simulation chain which will be detailed here. Given the fairly basic TREND acquisition chain, these results can be considered extremely encouraging in the perspective of future experiments using radio as a way to detect air showers, such as the Giant Radio Array for Neutrino Detection.

The Interstellar Boundary Explorer (IBEX) is an Earth-orbiting spacecraft equipped with two single-pixel cameras that detect neutral atoms produced by the interaction of the solar wind (SW) with the very local interstellar medium (VLISM), as well as neutral atoms flowing in from the VLISM itself. After its launch in 2009, IBEX discovered the unexpected existence of the “ribbon,” a nearly circular arc of enhanced hydrogen ENA flux at ~keV energies. The enhanced ribbon fluxes are believed to originate from look directions perpendicular to the local interstellar magnetic field draped around the heliosphere. A comparative analysis of ribbon flux simulations with IBEX data derived a “pristine” interstellar field strength of ~3 μG just beyond the influence of the heliosphere, directed towards ~(26°, 50°) in galactic longitude/latitude. IBEX observations complement the only in situ observations of the VLISM made by the Voyager 1 spacecraft. Since crossing the heliopause in August 2012, Voyager 1 has been measuring the VLISM plasma properties, including the galactic cosmic ray flux, (indirectly) the compressed interstellar plasma density, as well as the interstellar magnetic field draped around the heliosphere. This talk will review key IBEX and Voyager observations that inform us of the VLISM environment, in particular the local interstellar magnetic field, which is important for understanding the galactic cosmic ray fluxes observed at Earth.

In 2015, the HAWC Observatory was completed and began operation as the most sensitive TeV cosmic-ray detector in the Northern Hemisphere. Since that time, we have recorded over 1 trillion cosmic-ray air showers, designed a likelihood-based cosmic-ray energy reconstruction, and implemented a new minimally-biased method for reconstructing all-sky anisotropy. These three advances in statistics, energy resolution, and signal recovery allow us to better disentangle the properties of the TeV cosmic-ray anisotropy from detector effects. This has led to a combined anisotropy sky map with IceCube in the Southern Hemisphere. Although the nature of this anisotropy has been explored and modeled, the exact realization of the anisotropy could hold clues important to describing local accelerators of observed cosmic rays and the local magnetic fields through which they propagate. We will share our results for both HAWC and the combined HAWC-IceCube anisotropy sky maps.

Although cosmic rays are nearly isotropic, ground-based arrays sensitive to TeV cosmic rays have measured a small anisotropy in right ascension. Understanding the morphology and energy dependence of this anisotropy can yield insight into cosmic-ray sources and propagation in the local magnetic field. The Fermi Large Area Telescope (LAT) is optimized for gamma-ray measurements, but it records cosmic-ray protons at an even higher rate. We present a Fermi LAT search for cosmic-ray proton anisotropy at energies ~100 GeV and greater. The energy range is complementary to ground-based measurements. Moreover, while ground-based instruments cover only part of the sky and most are only sensitive to the right ascension component of the anisotropy, the LAT is sensitive to the full sky and to all orientations of anisotropy.

Coffee Break in the Oak Room

We have discovered a rare new form of long-term radio variability in the light-curves of active galaxies (AG) (arXiv:1702.06582, arXiv:1702.05519) --- Symmetric Achromatic Variability (SAV) --- a pair of opposed and strongly skewed peaks in the radio flux density observed over a broad frequency range. We propose that SAV arises through gravitational milli-lensing when relativistically moving features in AG jets move through gravitational lensing caustics created by 10^3-10^6 solar mass subhalo condensates or black holes located within intervening galaxies. The lower end of this mass range has been inaccessible with previous gravitational lensing techniques. This new interpretation of some AG variability can easily be tested and if it passes these tests, will enable a new and powerful probe of cosmological matter distribution on these intermediate mass scales, as well as provide, for the first time, micro-arcsecond resolution of the nuclei of AG --- a factor of 30--100 greater resolution than is possible with ground-based millimeter VLBI.

The jets of active galactic nuclei (AGN) are among the most powerful systems in the Universe. Their emission spans over an extremely wide energy range, from radio to gamma-rays or even TeV energies, and often shows pronounced variability with timescales anywhere between a few years and several minutes. Therefore, high-cadence, multi-band monitoring programs are essential in the investigation of their physical conditions and variability processes. The F-GAMMA (Fermi-GST AGN Multi-frequency Monitoring Alliance) was a program for the monitoring of the broad-band radio emission of about 90 Fermi-GST AGN, 25 of which have been detected also at TeV energies. The sources were observed from 2007 to 2015 at 12 radio frequencies between 2.6 GHz and 345 GHz with a mean cadence of 1-1.3 months. Both flux-density and (linear and circular) polarization variability was monitored. Here we present a compilation of science highlights from the F-GAMMA program, which include various multi-band correlation and population studies (e.g. gamma-ray loudness versus radio variability, radio versus gamma-ray fluxes, variability of FSRQs and BL Lacs), the localization of the gamma-ray emission site in AGN jets, the calculation of their Doppler factors using their multi-wavelength variability as well as a unification scheme for their broad-band spectral variability patterns which show an extremely diverse behavior.

We present a search for hour-scale very high energy (VHE) flares from 187 blazars monitored by the HAWC observatory. With a wide field of view of ~2 sr and sensitivity to energies above a few hundred GeV, HAWC functions as a survey instrument and facilitates searches for rapid variability in the VHE band. The currently operational HAWC real-time flare monitor takes advantage of this capability by issuing alerts within minutes of the identification of flaring activity. In this presentation, we describe the real-time flare monitor and report on the detection of several rapid flares in over 2 years of data collected between November 2014 and February 2017. We interpret these observations as an unbiased constraint on the rate of extreme blazar flares. We also summarize the prospects for future multiwavelength studies of extreme flares detected by the real-time flare monitor to provide clues into the mechanisms powering the blazar jets and probe the particles and fields in intergalactic space.

Extensive observations by Fermi, AGILE, and TeV telescopes have opened a new window into the high-energy physical processes of AGNs and raised questions about the physics of their jets, their formation and cosmological evolution, and their impact on their environments and the growth of structure in the Universe. Multiwavelength observations in X-rays and at GeV and TeV energies point to a large class of blazars whose peak output is in the poorly explored MeV band. With unprecedented sensitivity between 200 keV and 10 GeV, the All-Sky Medium Energy Gamma-ray Observatory (AMEGO) will fill in the MeV gap in blazar spectral energy distributions, providing crucial clues about their emission mechanisms in this regime. Also, with its wide field of view, AMEGO will survey the entire sky every 3 hours, allowing it to monitor variations in blazar light curves on short and long timescales that arise from changes in their jets. Furthermore, multiwavelength observations of the blazar population indicate that the sub-population of MeV blazars are among the most distant and luminous AGNs; thus, AMEGO observations of MeV blazars will allow it to probe the growth of supermassive black holes at earlier epochs than allowed by other types of AGNs.

Robust connections exist between various energy regions in the spectra of nearby galaxies. The flux ratios from widely separated spectral regions are often remarkably constant while originating via very different processes with varying efficiencies. Although the radio-far infrared (FIR) correlation is best known, consistent flux ratio relationships also are found between gamma-rays and the FIR, as well as between gamma-ray and radio fluxes. These relationships are understood in cases where the underlying linkage involves related power sources, such as massive stars. However, some systems containing substantial AGNs as well as starbursts still fall close to the standard flux ratio correlations. In this talk, I will explore some of the astronomical issues playing into the interpretation of these correlations and also briefly touch on the range of cosmic power sources that may produce these patterns.

Despite intensive research, some fundamental properties of the most luminous particle accelerators and transients like AGNs, GRBs, etc. are unknown. Location and mechanisms of particle acceleration, connection to flaring and quiescent states, leptonic vs hadronic emission are open questions. Complexity of environments and processes make it hard to disentangle different scenarios. This suggests complementing conventional observables like the broadband spectrum with novel statistical observables like power spectral density (PSD) and the flux probability distribution (PDF) extracted from lightcurves, high and low energy polarisation, etc. While the PSD encodes the temporal structure of dynamical processes, particle acceleration and radiation and observing cadence, the PDF encodes the fundamental form of the emission processes (additive vs multiplicative). Polarised emission provides independent constraints on region geometry, magnetic fields, scattering processes, etc. to those from the above observables. These observables and related methods are also relevant for population studies. For e.g., time series methods used to compute the PSD, can also be used to estimate transient detection probability and resultant changes in source flux distribution, $\frac{dN}{dF}$. A detailed theoretical framework capable of predicting these statistical observables from first principles in these sources is currently in nascency. Finally, they are complementary and potentially crucial crosschecks to neutrino and gravitational wave observations in the multi-messenger era. In this presentation, I demonstrate the potential of using such novel observables and related methods to probe physics of individual particle accelerators and the population at large by applying it to prominent blazars like Mrk 421, BL Lac, PKS 2155, etc.

The recent observations of powerful, minute-timescale TeV flares from several blazars pose serious challenges to theoretical models for the blazar emission. In this talk, I will discuss the magnetic reconnection model for the blazar flaring. I argue that radiation emitted from the reconnection layers can account for the observed “envelope” of ~day-long blazar activity as well as the fastest observed flares. Moreover, I will show that the reconnection model predicts that the emission regions are characterized by rough equipartition between radiating particles and magnetic fields; in agreement with observations. Finally, I will show examples of lightcurves and spectra calculated directly with first-principle Particle in cell simulations of the magnetic reconnection layer.

In models of early universe cosmology, primordial magnetic fields with helicity can be created during cosmological inflation, and they may play a role in the generation of the matter / antimatter asymmetry of the universe. Such a primordial magnetic field will persist in the universe today as an intergalactic magnetic field, and the discovery of this cosmological relic will open a new window onto the early universe. In this talk I will discuss a new probe of helical intergalactic magnetic fields through TeV blazar halo morphology. The emission of TeV gamma rays from blazars at cosmological distances will induce an electromagnetic cascade when the TeV gamma rays are incident upon starlight and produce electron-positron pairs. These charged leptons are deflected by the presence of an intergalactic magnetic field, which forms a halo of GeV cascade gamma rays around the blazar. In this talk I will discuss how the halo can acquire a parity-violating shape if the intergalactic magnetic field is helical.

The WFIRST high-latitude survey (HLS) will provide an exciting dataset for constraining dark energy through a variety of measurement methods. In this talk, I will describe the current plans for the WFIRST HLS and the potential for competitive constraints on dark energy with weak lensing. I will also discuss the potential synergies with other surveys during the same time-frame, including the opportunities provided by joint analysis with LSST, Euclid, and CMB-S4. Finally, I will present the results of ongoing efforts to understand the impact of near-infrared detector systematics on weak lensing measurements, and to place requirements on the hardware to ensure that the scientific goals of the survey can be met.

CHIME will use the 21cm emission line of neutral hydrogen to map large-scale structure between redshifts of 0.8 and 2.5. By measuring Baryon Acoustic Oscillations (BAO) we will place constraints on the dark energy equation of state as it begins to dominate the expansion of the Universe, particularly at redshifts poorly probed by current BAO surveys. In this talk I will introduce CHIME, a transit radio interferometer designed specifically for this purpose. I will discuss its goals and describe the powerful new analysis techniques we have developed to confront the many challenges of such observations, in particular removal of astrophysical foregrounds which are six orders of magnitude larger than the 21cm signal. A smaller 40m x 37m pathfinder telescope is currently operating at the DRAO in Penticton, BC, and the full-sized 80m x 100m instrument will be completed this year. I will report on current progress, and the lessons already learned.

Type Ia supernovae (SNe Ia) provided the first direct evidence for the accelerated expansion of the universe, leading to the now-standard Lambda-CDM model featuring dark energy. Beyond direct dark energy measurements, these accurate standard candles can be employed in a variety of ways to test the Lambda-CDM model. I will show how an analysis of the peculiar velocities of SNe Ia constitutes a powerful test of the cosmological model at the lowest redshifts. I will also illustrate that, while SNe Ia fundamentally measure distance, careful treatment can yield unbiased measurements of the relative expansion rate, facilitating fast subsequent cosmological inference and complementarity with similar measurements from other probes of geometry. I will present the highest-redshift SN Ia measurement of expansion from SNe observed via the HST CANDELS & CLASH programs.

The Hubble constant H0 — the expansion rate of the Universe today — has recently been measured to percent-level precision, but two of the key results are in tension. The local measurements using distance ladders have indicated H0 ~ 73 km/s/Mpc, while the global measurements using cosmic microwave background have indicated H0 ~ 67 km/s/Mpc. In this talk, I will first review the methods and results of both local and global measurements. I will then present our efforts of using simulations to quantify the sample variance in the local measurements of H0. Taking into account the inhomogeneous selection of type Ia supernovae, we find that this tension cannot be alleviated by sample variance or local density fluctuations. I will conclude with other possible causes of this tension.

Coffee Break in the Oak Room

I will revisit the production of baryon asymmetries in the minimal type I seesaw model with two heavy Majorana singlets in the GeV range. Beside the tree level top scattering we include scattering processes on gauge bosons as well as $1\rightarrow 2$ processes of Higgs decay and inverse decays, that can contribute significantly to the wash-out effect. I will show that the region of parameter space that can account for the right baryon asymmetry overlaps considerably with the future experiment SHIP and FCC sensitivity regions. Finally I will show the relevant implication for determinating leptonic CP-violation and actual prediction of the baryon asymmetry from a hypothetical positive measurement in SHiP.

In this talk I will discuss a model in which the matter / anti-matter asymmetry of the universe is generated during a first order cosmological phase transition associated with the spontaneous breaking of lepton-number, which gives rise to the Majorana mass for heavy sterile neutrinos. The dynamics leading to lepton-number generation, namely CP-violating scattering at a bubble wall, are reminiscent of electroweak baryogenesis. However, the degrees of freedom (sterile neutrinos) and energy scale are typically associated with thermal leptogenesis. The model predicts a stochastic background of gravitational waves (as in EW baryogenesis), neutrinoless double beta decay (as in thermal leptogenesis), as well as a light pseudo-Goldstone Majoron, which may play the role of dark matter.

I will introduce the MATHUSLA proposal (Massive Timing Hodoscope for Ultra-Stable neutraL pArticles) for a ~200mx200m tracker above ATLAS or CMS at the HL-LHC. Its primary purpose is the search for exotic long-lived particles with lifetimes up to the BBN bound of ~ 0.1 seconds, where it would extend LHC sensitivity by orders of magnitude. In addition, the design and position of MATHUSLA close to the LHC main detectors may enable it to perform unique cosmic ray measurements. I will present some possible aspects of this cosmic ray physics program, while also soliciting input from the broader community.

We propose the first viable radiative seesaw model, in which the neutrino masses are induced radiatively via the two-loop Feynman diagram involving Strongly Interacting Massive Particles (SIMP). The stability of SIMP dark matter (DM) is ensured by a Z5 discrete symmetry, through which the DM annihilation rate is dominated by the 3 to 2 self-annihilating processes. The right amount of thermal relic abundance can be obtained with perturbative couplings in the resonant SIMP scenario, while the astrophysical bounds inferred from the Bullet cluster and spherical halo shapes can be satisfied. We show that SIMP DM is able to maintain kinetic equilibrium with thermal plasma until the freeze-out temperature via the Yukawa interactions associated with neutrino mass generation.

The J-PARC Sterile Neutrino Search at the J-PARC Spallation Neutron Source (JSNS$^2$) will search for neutrino oscillations with $\Delta m^2 \sim$ 1 eV$^2$ at the J-PARC Material and Life Science Experimental Facility (MLF). The experiment will perform a search for $\bar{\nu}_\mu \rightarrow \bar{\nu}_e$ oscillations over a 24 m baseline using muon decay at rest neutrinos originating from 3 GeV proton interactions with a mercury target. Using two tanks of Gd-doped liquid scintillator with a total fiducial mass of 50 tons, JSNS$^2$ will exploit the unique signature of inverse beta decay (prompt positron signal, delayed gammas from neutron capture) to look for $\bar{\nu}_e$ appearance. Additionally, JSNS$^2$ will do novel cross section measurements using 236 MeV muon neutrinos from kaon decay at rest (KDAR).

In this talk we will present novel ways in which neutrino oscillation experiments can probe dark matter. In particular, we focus on interactions between neutrinos and ultra-light (“fuzzy”) dark matter particles with masses of order $10^{-22}$ eV. It has been shown previously that such dark matter candidates are phenomenologically successful and might help ameliorate the tension between predicted and observed small scale structures in the Universe. We will show that coherent forward scattering of neutrinos on fuzzy dark matter particles can significantly alter neutrino oscillation probabilities and lead to the effects which could be observable in current and future experiments. We present new limits on fuzzy dark matter (both scalar and vector) interacting with neutrinos using data from long-baseline accelerator experiments as well as the solar neutrino data.

Neutron tagging is a promising experimental technique for separating between signal and background in a wide variety of astroparticle measurement. The Accelerator Neutrino Neutron Interaction Experiment (ANNIE) located along the Booster Neutrino Beam at Fermilab has a goal of measuring the final state neutron multiplicity from charged current neutrino-nucleus interactions within the gadolinium-loaded water. Currently, ANNIE is running in Phase-I and it will be upgraded to Phase-II in the summer of 2017, by installing Large Area Picosecond Photodetectors (LAPPDs) in the detector. LAPPDs are a novel photodetector technology with single photoelectron time resolutions less than 100 picoseconds, and spatial imaging capabilities to within a single centimeter. They will play a crucial role to separate events of charged-current quasi-elastic (CCQE) interactions and inelastic multi-track charged current interactions. In this talk, we discuss the current status and future plans of the experiment.

MicroBooNE is a liquid argon TPC neutrino experiment based at Fermilab and situated on the Booster Neutrino Beam. MicroBooNE's primary aim is to investigate the excess of electron neutrino-like events seen by the MiniBooNE experiment, which is potential evidence for new non-Standard physics such as sterile neutrinos. This talk will discuss a search for low-energy electron neutrino interactions within the MicroBooNE detector. This analysis features a hybrid approach of traditional reconstruction methods along with a novel application of convolutional neural networks (CNNs), a deep learning algorithm highly adept at pattern recognition. This talk will describe the identification of events and the ways in which the CNNs are used. It will also outline the ways we are addressing issues related to applying CNNs, which are trained on simulated data, to data from the detector

One of the best current constraints for indirect detection of dark matter at the 1-100 GeV mass scale is the Fermi-LAT stacking analysis of satellite dwarf galaxies of the Milky Way. This constraint is based on observations in a very small fraction of the sky, whereas undetectable, dense dark matter structures are predicted to be distributed throughout the Milky Way halo. I will describe strategies that open up searches for dark matter signatures to the whole sky. These methods improve sensitivity to cold thermal relics, as well as other dark matter scenarios.

There is overwhelming evidence that non-baryonic dark matter constitutes ~85% of the mass in the Universe. Many promising dark matter candidates, like Weakly Interacting Massive Particles (WIMPs), are predicted to produce Standard Model particles like gamma rays via annihilation or decay. These gamma-rays would be observed by ground-based arrays like the High Altitude Water Cherenkov (HAWC) Observatory. With its wide field of view and constant monitoring, HAWC is well-suited to search for dark matter in extended targets like M31. We will present results from our search for a signal from dark matter annihilation or decay in M31 using 760 days of data from HAWC. A detection of dark matter through cosmic messengers 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.

The High Altitude Water Cherenkov (HAWC) gamma-ray observatory is a wide field-of-view observatory sensitive to 0.5 TeV - 100 TeV gamma-rays and cosmic-rays in the State of Puebla, Mexico at an altitude of 4100m. The HAWC observatory performed an indirect search for dark matter via GeV-TeV photons resulting from dark matter annihilation and decay considering various sources, including 15 dwarf spheroidal galaxies (dSphs) and 31 dwarf irregular galaxies (dIrr), as well as combined limits for the dSphs and dIrrs. We searched for dark matter annihilation and decay at dark matter masses above 1 TeV. We have not detected statistically significant excess from these sources, thus we will present the calculated annihilation cross-section and decay lifetime limits.

In the current understanding of structure formation in the Universe, the Milky Way is embedded in a clumpy halo of dark matter (DM). Regions of higher DM density are expected to present an enhanced rate of annihilation into gamma-rays with respect to the smooth halo regions. These point-like gamma-ray fluxes can possibly be detected by gamma-ray observatories on Earth, like the forthcoming Cherenkov Telescope Array (CTA). In this talk, I will present the expected gamma-ray fluxes from DM annihilation in Galactic subhalos together with a rigorous assessment of modeling and statistical uncertainties. I will then discuss the sensitivity of the CTA instrument to detect the brightest Galactic DM density clump in the projected extragalactic sky survey. I will also show how a CTA extragalactic survey dataset can be used to search for DM substructures as anisotropies in the angular power spectrum of the data.

Well motivated dark matter particle models predict self-annihilating dark matter to yield Standard Model particles that can potentially be detected by astrophysical observations in systems such as dwarf galaxies, normal galaxies, and galaxy clusters. The potential emission from the charged particle byproducts of dark matter annihilation includes radio emission due to synchrotron radiation as well as X-rays from inverse Compton scattering of CMB and starlight photons. These secondary emissions provide a method of probing the nature of dark matter that is complementary to previous gamma-ray searches and can place competitive constraints on dark matter properties. To facilitate multi-wavelength dark matter searches we have developed RX-DMFIT (Radio and X-ray - DMFIT), a tool for calculating the the expected radio and X-ray signals from dark matter annihilation. In this talk I will present RX-DMFIT and discuss the relevant particle and astrophysical components of the multi-wavelength approach including diffusion effects, radiative energy loss processes, and magnetic field modeling.

The GAPS Experiment is the first experiment optimized specifically for low-energy antideuteron and antiproton cosmic-ray signatures. Low-energy antideuterons have been recognized as an extraordinarily low-background signature of new physics, and low-energy antiprotons are probes of both light dark matter and cosmic-ray propagation models. Together, these signatures offer a potential breakthrough in unexplored dark matter parameter space, providing complementary coverage with direct detection, collider, and other indirect searches. The GAPS program is designed to utilize long-duration balloon flights from Antarctica, and is currently scheduled by NASA for its first Antarctic flight in late 2020. The experiment uses a novel detection technique, based on exotic atom capture and decay, to be sensitive to antinuclei in an unprecedented low energy range (<0.25 GeV/n). The heart of GAPS will be 10 planes of lithium-drifted Si (Si(Li)) detectors, surrounded on all sides by a plastic scintillator time-of-flight. In this contribution, I will present the design, status, and discovery potential of the GAPS scientific program.

Coffee Break in the Oak Room

Energy injection from dark matter (DM) between recombination and reionization could affect the ionization and thermal history of the universe, leaving a distinctive imprint on the cosmic microwave background (CMB). Therefore, precise measurements of the temperature and polarization anisotropies of the CMB provide a powerful tool by which to constrain DM. In this talk, I will characterize the possible CMB signatures via principal component analysis (PCA) and set constraints on the DM lifetime and decaying fraction. I will show that in many cases, a single number can be used to parameterize the effect of DM on the CMB. This result yields a simple prescription for detectability and an easy way to set model-independent bounds, which I have validated using Markov chain Monte Carlo methods applied to the Planck likelihood.

While constraints on primordial black holes as dark matter are strong over a wide mass range, a narrow window in the stellar-mass range remains relatively unconstrained. The recent discoveries of gravitational waves from merging black holes in roughly the 10-30 solar mass range has re-ignited the discussion of whether primordial black holes in this mass range could be a candidate for dark matter. If such sources exist in our Galaxy, they should produce observational signatures in the form of broadband radiation due to the accretion of gas onto the black holes. I will discuss a novel approach to constraining primordial black holes as dark matter using X-ray and radio observations of the Milky Way bulge, where both the density of gas and dark matter is highest, by including a realistic treatment of accretion processes based on observational evidence of inefficient accretion in our Galaxy today. The resulting constraints essentially rule out primordial black holes as a dark matter candidate in this unconstrained stellar-mass regime, and are complementary to searches in the early universe and other constraints from the dynamics of local systems. I will also comment on the potential of future surveys with SKA to further constrain this dark matter candidate.

Supernova 1987A provides strong constraints on hidden-sector particles with masses below ~100 MeV. If such particles are produced in sufficient quantity, they reduce the cooling time of the supernova, in conflict with observations. We consider the resulting constraints on dark photons, milli-charged particles, and sub-GeV dark matter coupled to dark photons. For the first time, we include the effects of finite temperature and density on the kinetic-mixing parameter, ε, in this environment. Furthermore, we estimate the systematic uncertainties on the cooling bounds by deriving constraints assuming one analytic and four different simulated temperature and density profiles of the proto-neutron star. Our constraints exclude novel parameter spaces for sub-GeV dark matter, and for dark photons differs significantly from previous work in the literature.

Dark matter decays or annihilations that produce line-like spectra may be smoking-gun signals. However, even such distinctive signatures can be mimicked by astrophysical or instrumental causes. We show that velocity spectroscopy-the measurement of energy shifts induced by relative motion of source and observer-can separate these three causes with minimal theoretical uncertainties. The principal obstacle has been energy resolution, but upcoming experiments will reach the required 0.1% level. We demonstrate this technique using existing technologies.

The era of precision cosmology has revealed that ~80% of the matter in the universe is dark matter. Two leading candidates, motivated by both particle and astro-physics, are Weakly Interacting Massive Particles (WIMPs) and axionlike particles (ALPs), both of which have distinct gamma-ray signatures. The Fermi Large Area Telescope (Fermi-LAT) Collaboration continues to search for WIMP and ALP signatures spanning the 50 MeV to >300 GeV energy range in dwarf spheroidal galaxies, galaxy clusters, pulsars, the Galactic center, and a variety of other astrophysical targets. Thus far, Fermi-LAT has not conclusively detected a dark matter signature. There is however an intriguing excess of gamma rays associated with Galactic center (GCE). The poorer angular resolution of the LAT at lower energies makes source selection challenging and the true nature of the detected signal remains unknown. Identifying whether the GCE excess is a dark matter signature, a population of astrophysical point sources, or a combination of the two, requires higher resolution observations. ALP searches would also greatly benefit from increased angular and energy resolution at lower energies. To address these, we are developing AMEGO, the All-sky Medium Energy Gamma-ray Observatory. It has a projected energy and angular resolution that will increase sensitivity by a factor of 20-50 over previous instruments. This will allow us to explore new areas of WIMP and ALP parameter space and provide unprecedented access to the particle nature of dark matter. I will present an overview of the AMEGO dark matter search strategy as well as sensitivity projections.

The AMS-02 experiment has recently released a new measurement of the cosmic-ray antiproton spectrum. Assuming that cold dark matter (CDM) is made of self-annihilating particles, the AMS-02 data can be used to constrain the annihilation cross section. It is known however that CDM structures itself on scales much smaller than typical galaxies. This structuring translates into a very large population of subhalos which must impact predictions for indirect searches. I will present a dynamically constrained and consistent semi-analytic model of Galactic subhalos (based on arXiv:1610.02233) and discuss its impact on current constraints (or hot spots) inferred from the AMS-02 antiproton data.

The IceCube neutrino observatory routinely detects astrophysical neutrinos at TeV to PeV energies, but the origin of this signal is still unknown. To facilitate the identification of electromagnetic counterparts via time-domain searches, IceCube has begun issuing realtime public alerts for the highest confidence and best-localized neutrino events (median angular uncertainty < 1.0 deg). During the same period, the Dark Energy Survey (DES) has developed a Target-of-Opportunity program to search for optical transients associated with gravitational wave events using the Dark Energy Camera (DECam) on the Blanco telescope. During the 2017-2018 observing season for DES, we will expand this program to search for explosive optical transients, such as core-collapse supernovae, coincident with several IceCube alerts. The large aperture (4 m), wide field of view (3 deg^2), and southern location (latitude -30 deg) of Blanco/DECam complements the existing follow-up program for IceCube events. By targeting several neutrino events per year, beginning in 2017, we can reasonably expect to identify the first individual TeV-PeV neutrino source, or else place meaningful constraints on the internal physical processes occurring within core-collapse supernovae and other explosive optical transients.

The Fermi Gamma-ray Burst Monitor (GBM) is an all-sky monitoring instrument sensitive to energies from 8 keV to 40 MeV. Over the past 8 years of operation, the GBM has detected over 240 gamma-ray bursts per year and provided timely GCN notices with localization to few-degree accuracy for follow-up observations. In addition to GRBs, Galactic transients, solar flares, and terrestrial gamma-ray flashes have also been observed. In recent years we have also been searching the continuous GBM data for electromagnetic counterparts to astrophysical neutrinos and gravitational wave events, as these are believed to be associated with gamma-ray bursts. With continuous data downlink every few hours and a temporal resolution of 2 microseconds, GBM is well suited for observing transients and supporting EM followup in the era of multi-messenger astronomy. I will discuss the details of our searches and summarize their current status.

We present the results of an archival coincidence analysis between public gamma-ray data from the Fermi LAT satellite and public neutrino data from the IceCube neutrino observatory during its 40-string and 59-string observing runs. The analysis has the potential to detect either a statistical excess of correlated neutrino + gamma-emitting sources or alternatively, one or more rare, high-multiplicity events such as gamma-ray burst + neutrino coincidences. This work is an example of the multimessenger studies currently being performed by the Astrophysical Multimessenger Observatory Network (AMON). We will present the relevant datasets, the statistical approach, and the results of the analysis.

Recently many observational facilities have entered in their operational phase or they will approach the design sensitivity in the nearest future, allowing us to observe the universe with very high energy photons, cosmic rays, neutrinos and gravitational waves. The MAGIC observatory: a system of two Imaging Atmospheric Cherenkov Telescopes located at the Canary Island of La Palma, thanks to its low energy threshold (~ 50 GeV) and fast slewing capability is taking an active role in many multi-messenger activities. Since many years MAGIC is involved in several multi-instrument programs mostly connected to transient phenomena such as: Gamma Ray Bursts, Fast Radio Bursts, follow-up of gravitational wave and neutrino alerts. In this talk I will present the MAGIC telescopes strategies for multi-messenger follow-up and observations of transient sources and their recent results.

The direct detection, for the first time, of gravitational wave (GW) transients by Advanced LIGO has motivated searches for their electromagnetic counterparts at all wavelengths. Neutrino astronomy is an emerging area of study in high-energy astrophysics, and astrophysical neutrinos are natural cousins of very high energy (VHE; E > 100 GeV) gamma rays. The VERITAS gamma-ray observatory has an active program of follow-up observations in the directions of potentially astrophysical high-energy neutrinos detected by IceCube, including prompt alerts, as well as in the direction of GW transients. The next-generation gamma-ray observatory Cherenkov Telescope Array (CTA) has similar plans. Since both neutrinos and gamma rays are produced in hadronic interactions, a joint study of both channels could reinforce the hadronic origin of the gamma rays, revealing high-power cosmic-ray accelerators and probing their properties. The directions of GW transients are uncertain at the level of tens to hundreds of square degrees, but the wide field of view provided by gamma-ray observatories (3.5° for VERITAS and ≥ 4.5° for CTA) can rapidly scan large regions; detections can yield improved localizations as well as insights on the astrophysics of the GW transient events. We present recent results from the VERITAS follow-up program and strategies for CTA.

Coffee Break in the Oak Room

The current generation of Cherenkov telescopes, together with Fermi-LAT, has greatly improved our knowledge of blazar physics, providing a precise measurement of their gamma-ray emission. The modeling of multi-wavelength spectral energy distributions of blazars has been proven to be a unique tool to constrain and refine blazar emission models, and thus the physics of outflows from super-massive black-holes. However, the long-standing question on leptonic vs hadronic models still remains open. A smoking-gun for hadronic processes in blazars is represented by neutrinos. In this contribution I will discuss blazar hadronic models and their associated neutrino emission, comparing it to current and future neutrino observatories.

We test the hypothesis that blazars are sources of Ultra-High Energy Cosmic Rays (UHECR), considering acceleration of isotopes heavier than Hydrogen. We perform numerical simulations of CR interactions using the NeuCosmA code. The injected isotope may efficiently disintegrate at high energies, thus producing a population of lighter secondaries. We study the ejected CR composition and neutrino spectra for different blazar classes: Flat-Spectrum Radio Quasars (FSRQs) and BL Lacs. We conclude that the former contribute significantly to the diffuse neutrino flux, whose maximal energy depends on the injected composition. BL Lacs, on the other hand, are found to dominate the UHECR flux. We show that blazars are able to power the UHECRs, while not violating the most recent IceCube limits on blazar neutrinos.

Neutrino stacking analyses constrain the paradigm that Gamma-Ray Bursts (GRBs) are the sources of the Ultra-High Energy Cosmic Rays (UHECRs). The majority of previous studies focused on a pure proton composition of UHECRs; however, recent measurements by the Pierre Auger Observatory indicate a trend towards a mixed UHECR composition. Here, we present a combined source-propagation model for neutrino and cosmic-ray emission by GRBs with the injection of nuclei, where we take into account that a nuclear cascade from photo-disintegration can fully develop in the source. Our main objective is to test whether recent results from the IceCube and Pierre Auger Observatory can be accommodated with the paradigm that GRBs can be the sources of UHECRs. We demonstrate that the expected prompt neutrino flux weakly depends on the injected composition, which translates into strong constraints on UHECR models even in the case of nuclei. While the UHECR spectrum and composition measured by the Pierre Auger Observatory can be self-consistently reproduced over an energy range even covering the ankle, the IceCube bounds from the GRB stacking are already in tension with this hypothesis. If, however, only the UHECRs beyond the ankle come from GRBs, future neutrino data will be needed to further constrain this hypothesis.

It has been a mystery that with ten orders of magnitude difference in energy, high-energy neutrinos, ultrahigh-energy cosmic rays, and sub-TeV gamma rays all present comparable energy injection rate, hinting an unknown common origin. Here we show that black hole jets embedded in clusters of galaxies may work as sources of all three messengers. By simulating the particle propagation in the magnetized intracluster medium (ICM), we show that the highest-energy particles leave the source rectilinearly and contribute to the observed cosmic rays above 0.1 EeV, the intermediate-energy cosmic rays interact with the ICM gas and produce secondary neutrinos and gamma rays, and the lowest-energy cosmic rays are cooled due to the expansion of the radio lobes inflated by the jets. The energy output required to explain the measurements of all three messengers is consistent with observations and theoretical predictions of black hole jets in clusters.

I will summarize the All-Sky Automated Survey for Supernovae (ASAS-SN), the first astronomical survey to observe the entire visible sky for bright optical transients on a nightly basis.

The ANTARES neutrino telescope has operated in the Mediterranean deep sea for roughly ten years. Its goal is to search for astrophysical neutrinos, both as a diffuse flux and originating from possible point sources. ANTARES is complementary to other neutrino observatories such as IceCube because of its good angular resolution and distinctive sky coverage. The ANTARES science program also includes indirect dark matter searches and participation in the so-called multi-messenger approach for transient sources. KM3NeT is the successor of ANTARES. Currently under construction, this neutrino telescope uses a single detector technology at two separate geographical sites, featuring different detector geometries. The respective science programs are dubbed KM3NeT ARCA and ORCA. KM3NeT ARCA is situated off the Sicilian coast in Italy and aims to detect multi-TeV astrophysical neutrinos. Due to an excellent angular resolution for all neutrino flavors, KM3NeT is able to study the point of origin of astrophysical neutrinos with unprecedented precision. In doing so, KM3NeT can independently confirm the IceCube astrophysical flux within one year of data taking. KM3NeT ORCA on the other hand will study atmospheric neutrino oscillations in the energy range below 100 GeV. Located off the southern French coast, it aims at a determination of the neutrino mass hierarchy with a precision of 3 sigma in three years of data taking. This presentation gives an overview of the latest ANTARES results. In addition, the current status of KM3NeT as well as its physics potential is discussed.

The IceCube Neutrino Observatory has detected the first high-energy neutrinos of astrophysical origin, characterized its diffuse flux, and performed point- source searches throughout the sky. Now, a next-generation, in-ice Cherenkov telescope is being designed with increased sensitivities to high-energy neutrinos. IceCube-Gen2 will encompass about 8 cubic-kilometers of ice at the South Pole. Additional envisioned components such as a large surface array, dense infill array, and complementary radio array would improve sensitivities across a wide energy band. Further, several studies to upgrade and optimize the optical module are ongoing and show promise to cost-effectively increase the photosensitive area. We will summarize these developments and focus on the projected sensitivities for high-energy neutrinos with IceCube-Gen2.

The ANtarctic Impulsive Transient Antenna (ANITA) is a long-duration balloon experiment with an interferometric radio payload. ANITA scans Antarctic ice for Askaryan radio emission from interactions of extremely-high-energy (>1 EeV) cosmogenic neutrinos. ANITA is also sensitive to geomagnetic radio emission from extensive air showers (EAS) initiated by both ultra-high-energy cosmic rays and tau leptons generated by Earth-skimming tau neutrinos. The fourth flight of ANITA recently was successfully completed in December 2016. After an overview of the instrument and analysis methods, this talk will highlight key results and ongoing analyses from the four flights of ANITA. Improvements for future flights will also be briefly discussed.

The Antarctic Impulsive Transient Antenna (ANITA) is a NASA long-duration balloon experiment with the primary goal of detecting ultra-high-energy ($>10^{18}\,\mbox{eV}$) neutrinos via the Askaryan Effect. The fourth ANITA mission, ANITA-IV, recently flew from Dec 2 to Dec 29, 2016. The most significant change in signal processing in ANITA-IV from previous flights was the inclusion of the Tunable Universal Filter Frontend (TUFF) boards. The TUFF boards had a three-fold purpose: 1) second-stage amplification by 45 dB to help boost the $\sim\,\mu\mbox{V-level}$ radio frequency (RF) signals to $\sim$ mV-level for digitization, 2) mitigation of narrow-band, anthropogenic noise with tunable, switchable RLC notch filters and 3) supplying power via bias tees to the first-stage, antenna-mounted amplifiers. In this talk, we outline the design and performance of the TUFF boards during the ANITA-IV flight.

ANITA is a NASA balloon-borne radio (200-1200 MHz) telescope with a primary goal of detecting coherent radio emission from ultra-high-energy (UHE) neutrinos. The instrument is also sensitive to detect radio impulses produced by cosmic ray induced extensive air showers. ANITA-4 flew Dec 2, 2016 and landed Dec 29, 2016 after 28 days. This talk will present the ANITA-IV instrument, flight operation, calibration, and the status of ongoing data analysis.

Coffee Break in the Oak Room

The Askaryan Radio Array (ARA) is a gigaton, ultra-high energy (>10 PeV) radio neutrino detector under construction at South Pole; it searches for the characteristic radio Cherenkov pulses that are produced by neutrino interactions in the dense polar ice. The array has deployed three of the proposed ~37 stations so far, at depths up to 200m. In this talk, we will summarize the current status of the experiment’s neutrino searches and hardware developments. We will also discuss the future of the array, including the planned deployment of an additional two upgraded stations in austral summer 2017, one of which is equipped with phased-array triggering capabilities.

The Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) mission is being designed to establish charged particle astronomy with ultra-high energy cosmic rays (UHECRs) and to observe astrophysical and cosmogenic neutrinos using both fluorescence and Cherenkov emission from extensive air-showers (EAS). The POEMMA design combines the concept developed for the Orbiting Wide-field Light-collectors (OWL) mission, the experience of the Extreme Universe Space Observatory (EUSO) on the Japanese Experiment Module (JEM-EUSO) fluorescence detection camera as recently flown on EUSO-SPB1 by a NASA Super Pressure Balloon (SPB) from Wanaka, New Zealand, with the recently proposed CHerenkov from Astrophysical Neutrinos Telescope (CHANT) concept to form a multi-messenger probe of the most extreme environments in the Universe. The fluorescence and Cherenkov study of EASs from space will yield orders-of-magnitude increase in statistics of observed UHECRs at the highest energies and the observation of astrophysical and cosmogenic flux of neutrinos for a range of UHECR models. These observations should solve the long-standing puzzle of the origin of the highest energy particles ever observed, providing a new window onto the most energetic environments and events in the Universe, and on studies of particle interactions well beyond accelerator energies.

Two ultrahigh-energy ($>10^{17}$ eV) neutrino detectors are being deployed in Antarctica: the Askaryan Radio Array (ARA) and the Antarctic Ross Ice-Shelf Antenna Neutrino Array (ARIANNA). As the experiments differ in both the design and the surrounding ice, we describe the progress of a joint effort to understand the importance of these differences and we demonstrate convergent results in their simulated detector responses.

The ARIANNA experiment is designed to observe cosmogenic neutrinos with energies in excess of 10^16 eV. The design envisions a grid of over 1000 independent radio detector stations, using high-gain log-periodic dipole antennas just below the surface to measure the characteristic Askaryan radio pulses from particle cascades generated in the ice by these neutrinos. Spaced a kilometer apart, this array would effectively survey nearly 1000 cubic kilometers of Antarctic ice. A pilot array has been operating on the Ross Ice-Shelf since December 2014. We will report on most recent results concerning the hardware performance, the search for neutrinos, detection of cosmic ray background, signal propagation in the ice, and the future potential of a large array.

The Giant Radio Array for Neutrino Detection (GRAND) aims at detecting ultra-high-energy extraterrestrial neutrinos via the extensive air showers induced by the decay of tau leptons created in the interaction of neutrinos under the Earth's surface. Consisting of an array of $\sim 10^5$ radio antennas deployed over $\sim 2\cdot 10^5\,\mbox{km}^2$, GRAND plans to reach, for the first time, a sensitivity of $\sim 10^{-10}\,\mbox{GeV cm}^{-2} \mbox{s}^{-1} \mbox{sr}^{-1}$ above $5\cdot10^{17}\,\mbox{eV}$ and a sub-degree angular resolution, beyond the reach of other planned detectors. In this talk, we will show preliminary designs and simulation results, plans for the ongoing, staged approach to construction, and the rich research program made possible by the proposed sensitivity and angular resolution.

The predictions of the flux of cosmogenic neutrinos at $10^{9}$ GeV are pretty solid and solely depend on the composition of the primary flux of cosmic-rays above $10^{10}$ GeV. Pushing the experimental sensitivity into the predicted flux levels is a challenge and the hunt to detect the first cosmogenic neutrino is ongoing. A major obstacle for experiments is to get a large enough acceptance while keeping costs reasonable. We have performed a conceptual design study of a dedicated array of Cherenkov telescopes that uses the Earth skimming technique to detect taus, which are produced when tau neutrinos convert in the Earth's crust and then emerge from the ground. Our study shows that one can build an experiment based on small Cherenkov telescopes, which reaches a sensitivity of $2\cdot10^{-9}$ GeV cm$^{-2}$ s$^{-1}$ sr$^{-1}$ at $10^9$\,GeV for a total cost envelope of $4M. The projected sensitivity is competitive with other proposed neutrino experiments in that energy range and outperforms them in terms of costs. In this talk we present details of our design study and discuss the proposed array of Cherenkov telescopes, which we named Trinity.

Cosmogenic neutrinos produced by cosmic rays during propagation are expected to arrive at Earth in roughly equal ratios of electron, muon, and tau neutrinos. Due the cyclic regeneration of tau neutrinos and tau leptons, radio-based experiments are sensitive to the air showers produced by tau leptons emerging from the interaction of Earth-skimming tau neutrinos. We present a study of the sensitivity and optimization of radio detectors at altitudes to tau-lepton showers and discuss prospects for future mountain-top or balloon-borne instruments.

Very high energy gamma-rays produced by extragalactic sources are absorbed in the intergalactic medium. High energy photons interact with low energy photons from the extragalactic background light (UV to IR) producing pairs of electron positrons. Newly created leptons scatter CMB photons to gamma-ray energies. Spectral properties, halo extension and time delay due to the cascade strongly depend on the source and intergalactic medium properties. In particular, the development of such a cascade is crucial to probe the extragalactic magnetic field (EGMF) which cannot be probed by other means. We have developed a new Monte Carlo code to simulate the cascade physics. After a short presentation of the code, I will review how the search for cascade signatures can be used to derive constrains on the extragalactic medium. To conclude I will discuss the cascade contribution to the extragalactic gamma-rays background derived from recent Fermi data.

A Type Ia supernova (SNIa) could go entirely unnoticed in the Milky Way and nearby starburst galaxies, due to the large optical and near-IR extinction in the dusty environment, low radio and X-ray luminosities, and a weak neutrino signal. But the recent SN2014J confirms that Type Ia supernovae emit γ-ray lines from $^{56}$Ni→$^{56}$Co→$^{56}$Fe radioactive decay, spanning 158 keV to 2.6 MeV. The Galaxy and nearby starbursts are optically thin to γ-rays, so the supernova line flux will suffer negligible extinction. The All-Sky Medium Energy Gamma-ray Observatory (AMEGO) will monitor the entire sky every 3 hours from ~200 keV to >10 GeV. Most of the SNIa gamma-ray lines are squarely within the AMEGO energy range. Thus AMEGO will be an ideal SNIa monitor and early warning system. We will show that the supernova signal is expected to emerge as distinct from the AMEGO background within days after the explosion in the SN2014J shell model. The early stage observations of SNIa will allow us to explore the progenitor types and the nucleosynthesis of SNIa. Moreover, with the excellent line sensitivity, AMEGO will be able to detect the SNIa at a rate of a few events per year and will obtain enough gamma-ray observations over the mission lifetimes (~10 SNIa) to sample the SNIa. The high SNIa detection

It is widely accepted that supernova (SN) shocks can accelerate particles to very high energies, although the maximum energies are still unclear. These accelerated particles can interact with other particles to produce gamma-ray emission. Details of the process are not well characterized, including the dynamics and kinematics of the SN shock wave, the nature and magnitude of the magnetic field, and the details of the particle acceleration process. The properties of the SN shock itself are regulated by the surrounding medium, which in a massive star is formed by mass-loss from the pre-SN progenitor during its lifetime. Thus the spectra of accelerated particles, and the resultant gamma-ray emission, depend on the evolution of the SN progenitor before it explodes. Herein we explore detailed aspects of SN evolution, particle acceleration, and the non-thermal emission, for young SNe right after outburst. We use these calculations to predict and constrain the detectability of young SNe of various types, via their hadronic signatures, namely gamma-ray emission from pp interactions, and synchrotron emission from secondary leptons. Our calculations also allow us to constrain the resulting TeV neutrino flux. After outlining the general considerations, we will provide a quantitative example in the form of the well-studied radio SN 1993J, for which we will calculate the gamma-ray and neutrino flux. We will also comment on the horizon of detectability of 1993J-like SNe with the upcoming Cherenkov Telescope Array (CTA).

Using a simplified model for the hadronic emission from young supernova remnants (SNRs), we derive an expression to calculate the hadronic luminosity with time, depending on the supernova (SN) ejecta density profile and the density structure of the surrounding medium. We then use this to estimate the gamma-ray emission from SN 1987A, the nearest visible supernova to us in over 300 years. The SN is surrounded by a three-ringed wind-blown structure that encloses a dense and complex surrounding medium. We present a hydrodynamic model of the medium surrounding SN 1987A, and the evolution of the SN shock wave within this medium. We demonstrate that our model is able to reproduce the time-evolution of the X-ray emission from SN 1987A, including detailed X-ray spectra. We then use this same hydrodynamic model to compute the gamma-ray emission from SN 1987A, and compare to observational constraints. Finally we reference recent observations of SN 1987A to predict the gamma-ray detectability of 87A in future. (I have also submitted an abstract to the Extragalactic sources (incl. transients) track, with various co-authors).

Even when ultrahigh-energy (E > 10^10 GeV) cosmic rays (UHECRs) are heavy nuclei (with nuclear charge Z) as indicated by existing data, the pointing of cosmic rays to the nearest extragalactic sources (distance D) at highest energies remains expected, because the bending of the cosmic ray goes as BZD/E (B is the extra-galactic magnetic field). In addition, the acceleration capability of the sources grows linearly in Z, while the energy loss per distance traveled decreases with increasing Z and nucleon number A. Each of these facts favors heavy nuclei as the primaries of UHECRs. A single dimensional analysis may miss the relative importance of the phenomena depending on these variables (D,B,E,Z,A, and direction). A multi-dimensional cross-correlation (MDCC) of the individual emission spectra with nearby putative sources is needed. I will use MDCC to study the hypothesis that primaries are heavy nuclei subject to GZK photo-disintegration, and that metal-rich starburst galaxies are the most plausible candidate sources by far: combining the 3.9-sigma probability of starburst-galaxy sources from Auger data with the significance of the hotspot derived from Telescope Array data, we arrive at a 5-sigma probability that starburst galaxies are the origin sites for UHECRs. Also, starburst galaxies possess a large density of supernovae and therefore of pulsars, and so can accelerate heavy nuclei to the hard spectrum that is needed to accommodate Auger observations. At face value, this result provides an important step in resolving the more than 100 year old mystery of the origin of highest-energy cosmic rays.

The arrival directions of multi-TeV cosmic rays show significant anisotropies at large and small angular scales. I will argue that these features can be understood from standard cosmic ray diffusion. It is well-known that a large-scale dipole anisotropy is expected from a cosmic ray density gradient following the distribution of Galactic sources. However, the observed anisotropy depends on cosmic ray propagation in our local magnetic environment. The observed dipole amplitude and phase are a result of anisotropic diffusion along the local ordered magnetic field. The small-scale structures, on the other hand, are expected to arise from cosmic ray scattering in local magnetic turbulence.

Coffee Break in the Oak Room

The shape of the large-scale cosmic-ray (CR) anisotropy depends on (and therefore contains information on) the local interstellar turbulence within ~ 10 pc from Earth. We calculate the TeV-PeV CR anisotropies predicted for a range of Goldreich-Sridhar (GS) and isotropic models of interstellar turbulence, and compare them with IceTop and IceCube data. The narrow deficits in the 400TeV and 2PeV data sets of IceTop can be fitted with a GS model that contains a smooth deficit of parallel-propagating waves and a broad resonance function, although some other models cannot, as yet, be ruled out. In particular, isotropic fast magnetosonic wave turbulence can match the observations at high energy, but cannot accommodate an energy dependence in the shape of the CR anisotropy. We discuss the impact of possible anisotropies in the power-spectrum of fast modes. Our findings suggest that data on the large-scale CR anisotropy could provide a new probe of the properties of the local turbulence. Finally, we compare our constraints with those (on bigger scales) from Planck’s dust-polarization measurements.

Tidal disruption events (TDEs) by supermassive or intermediate mass black holes have been suggested as candidate sources of ultrahigh-energy cosmic rays (UHECRs) and high-energy neutrinos. Motivated by the recent measurements from the Pierre Auger Observatory, which indicates a metal-rich cosmic-ray composition at ultrahigh energies, we investigate the fate of UHECR nuclei loaded in TDE jets. First, we consider the production and survival of UHECR nuclei at internal shocks, external forward and reverse shocks, and nonrelativistic winds. Based on the observations of Swift J1644+57, we show that the UHECRs can survive for external reverse and forward shocks, and disk winds. On the other hand, UHECR nuclei are significantly disintegrated in internal shocks, although they could survive for low-luminosity TDE jets. Assuming that UHECR nuclei can survive, we consider implications of different composition models of TDEs. Tidal disruption of main sequence stars or carbon-oxygen white dwarfs is difficult to reproduce the observed composition or spectrum. The observed mean depth of the shower maximum and its deviation could be explained by oxygen-neon-magnesium white dwarfs, but they may be too rare to be the sources of UHECRs.

There is tentative evidence for an ultra-high-energy cosmic-ray (UHECR) “hot spot” coming from the direction of Centaurus A and also evidence for another hot spot that might be associated with the M81 group. Although the evidence is not firmly established, it is not all unreasonable, given the energetics and the physical conditions in Cen A and in various galaxies in the M81 group, that these signals might be real. In this talk I will discuss how additional evidence to establish or disprove the existence of a hot spot can be obtained with some simple modeling of the energy and angular distribution expected from an UHECR source. I discuss the improvements that can potentially be done with current data and also forecast how well parameters of a hot-spot model may be constrained with future measurements.

The various coherent and turbulent components of the Galactic magnetic field have sufficiently high field strengths to alter the arrival distributions of cosmic rays, including those at ultra-high energies. I will highlight the results of a study considering a realistic GMF model including a persistent turbulent component, and rigidities $R \equiv E / Z \geq 10^{18}$ V reaching sufficiently low values as to describe Fe nuclei at energies above 50 EeV. In addition to the large scale Jansson-Farrar coherent field, our study investigates multiple realizations of the turbulent field; we vary the coherence length to determine its effect on the arrival distributions. For each rigidity and field model, the UHECR arrival direction distribution can be determined for an arbitrary source direction, by inverting the trajectories of more than $5 \times 10^{7}$ isotropically-distributed anti-CRs of the given rigidity, which we backtrack using the public code CRT. Aspects of the arrival direction distributions are examined for dependencies on rigidity and properties of turbulent field realizations. Except at high rigidity, the pattern of multiple images is very complex and depends strongly on the coherence length and source direction.

The sources of the highest-energy particles in the Universe remain a still-unresolved mystery. The reason is that charged-particle astronomy is severely complicated by magnetic deflections, which, for sources in the local Universe, are dominated by the effect of the Galactic magnetic field. I will discuss the PHAESTOS project - a radically new approach to identifying individual sources of UHECR: constructing a 3-dimensional map of the Galactic magnetic field through optopolarimetric magnetic tomography, and backtracking the paths that UHECR traverse through the Galaxy before reaching us, to improve agreement between their (corrected) arrival directions and the location of their sources on the sky. Effectively, this technique aims to improve the charged-particle point-spread-function by a factor of several, boosting the sensitivity to individual sources by a similar factor. This approach is becoming possible for the first time thanks to two experimental breakthroughs: the unparalleled wealth of stellar distances that the Gaia mission is in the process of providing; and recent advances in optopolarimetry of point sources that make possible systematic large-area surveys of stars, such as the upcoming PASIPHAE survey. The combination of Gaia and PASIPHAE data enable the construction, for the first time, of a tomographic map of the Galactic magnetic field, paving the way to ultra-high-energy cosmic-ray astronomy.

Local Radio galaxies (RGs) like Centaurus A are intensively discussed as the source of the observed Cosmic Rays above 3 EeV (UHECRs). In this talk a first systematic study is presented where all observational features of the UHECRs, i.e. the energy spectrum, the chemical composition and the arrival directions, are used to draw severe constraints on the UHECR contribution from the local RGs (up to a distance of about 120 Mpc from the Earth). Here, the radio luminousity of the RGs is linked to the UHECR luminosity to take the different states of the individual sources into account. Further, we also discuss the necessary contribution of the non-local sources. The propagation of the UHECR candidates is performed with the publicly available code CRPropa3 where the extragalactic magnetic field (EGMF) model from cosmological MHD simulations is used.

We propose an astrophysical scenario for ultrahigh-energy cosmic-ray production, in which galactic cosmic rays are reaccelerated by kiloparsec-scale jets in active galactic nuclei. We perform Monte Carlo simulations of transrelativistic shear acceleration dedicated to a jet-cocoon system of active galactic nuclei. A certain fraction of galactic cosmic rays in a halo is entrained, and sufficiently high-energy particles can be injected to the reacceleration process and further accelerated up to a few EeV for protons and around 100 EeV for irons. We show that the shear reacceleration mechanism leads to a hard spectrum of escaping cosmic rays, and the supersolar abundance of ultrahigh-energy nuclei is achieved due to injections at TeV-PeV energies. As a result, the highest-energy spectrum and mass composition can be reasonably explained without contradictions with the anisotropy data.

In this talk, I will present the status and plans of a new dedicated experiment called milliQan that we propose to install at LHC Point 5. It is designed to be sensitive to particles produced in pp collisions that have EM charges ranging from 0.001 e to 0.1 e, as can arise in a variety of beyond-the-standard model scenarios.

One interesting class of models involves dark matter as the lightest state of a strongly interacting hidden sector, similar to the pions of QCD. In this talk, I will examine the possibility that the lightest vector resonances of the hidden sector are nearby in mass and accessible within the current operating energy of fixed-target experiments. These states significantly modify processes in the early universe and give rise to striking signals at low-energy accelerators, involving missing energy and displaced pairs of leptons.

In this talk we discuss the sensitivity of probing light bosons in the Borexino-SOX experiment, and the possibility of detecting heavy leptons in the SHiP and DUNE experiments. Bringing an external radioactive source close to a large underground detector can significantly advance sensitivity not only to sterile neutrinos but also to "dark" gauge bosons and scalars. Here we address in detail the sensitivity reach of the Borexino-SOX configuration, which will see a powerful (a few PBq) 144Ce−144Pr source installed next to the Borexino detector, to light scalar particles coupled to the SM fermions. The mass reach of this configuration is limited by the energy release in the radioactive γγ-cascade, which in this particular case is 2.2 MeV. Within that reach one year of operations will achieve an unprecedented sensitivity to coupling constants of such scalars, reaching down to g∼10^{−7} levels and probing significant parts of parameter space not excluded by either beam dump constraints or astrophysical bounds. Should the current proton charge radius discrepancy be caused by the exchange of a MeV-mass scalar, then the simplest models will be decisively probed in this setup. We also update the beam dump constraints on light scalars and vectors, and in particular rule out dark photons with mass below 1 MeV, and couplings constants ϵ≥10^{−5}. We then move on to briefly discuss the possibility of utilizing SHiP and DUNE experiments to probe long-lived heavy leptons.

Nanosecond precision timing synchronization via the Global Positioning System has become a common technique for a variety of particle physics and astrophysics experiments including, for example, large arrays of detectors for cosmic ray air showers. By using the common time-standard in GPS, time synchronization can be achieved at low cost, even over large areas in remote locations. However, in principle, synchronization accuracy is limited by atmospheric effects, especially over large distances. Here we present a new measurement of the accuracy of GPS timing synchronization, particularly as a function of distance between two receivers.

A direct measurement of the gravitational acceleration of antimatter has never been performed to date. Recently, such an experiment has been proposed, using antihydrogen with an atom interferometer and an Antihydrogen confinament has been realized at CERN. In alternative we propose an experimental test of the gravitational interaction with antimatter by measuring the branching fraction of the CP violating decay of KL in space. We show that at the altitude of the International Space Station, gravitational effects may change the level of CP violation such that a 5 sigma discrimination may be obtained by collecting the KL produced by the cosmic proton flux within a few years.

Coffee Break in the Oak Room

In the minimal left-right symmetric model which could accommodate the tiny neutrino masses via TeV seesaw mechanism, the neutral scalar from the right-handed symmetry breaking sector could be much lighter than the electroweak scale. Limited by the meson oscillation and decay data, such a light particle is necessarily long-lived and decays predominantly into two photons, mediated by the heavy $W_R$ boson. It could be searched for at the LHC and in the intensity frontier experiments via (displaced) photon signals, if its mass is of order GeV scale. This provides a unique test of TeV scale left-right models and the seesaw mechanisms.

Despite the recent discovery of the Higgs boson contributing to the success of the Standard Model, the large excess of dark matter in the Universe remains one of the outstanding questions in science. This excess cannot be explained by Standard Model particles. A compelling hypothesis is that dark matter is comprised of particles can be produced at the LHC, called Weakly Interacting Massive Particles (WIMPs). This talk presents a number of ATLAS searches for WIMP dark matter, outlining the main theoretical benchmarks and issues in terms of complementarity with direct and indirect detection experiments, and presents the prospects for dark matter searches at future LHC runs.

Dark matter can be sought in complementary experiments: direct detection, indirect detection and colliders all contribute to a comprehensive set of searches for weakly interacting massive particles (WIMPs). This talk underlines the searches for Dark Matter by the ATLAS experiment in the context of this complementarity, using models that include a mediator particle between SM and DM.

Will cover searches for neutralinos and electroweakinos.

Several theories beyond the Standard Model predict the existence of high mass neutral or charged Higgs particles or BSM decay modes of the 125 GeV Higgs boson. In this presentation, the latest ATLAS results on searches for these particles will be discussed.