Author: "Nicholas L. Rodd" / Topic: 010308 nuclear & particles physics - Searchworks@Jio Institute Digital Library Search Results

23 results on '"Nicholas L. Rodd"'

1. Dark matter spectra from the electroweak to the Planck scale

Author: Bryan R. Webber, Christian W. Bauer, Nicholas L. Rodd, Rodd, Nicholas L. [0000-0003-3472-7606], Apollo - University of Cambridge Repository, and Rodd, NL [0000-0003-3472-7606]
Subjects: Nuclear and High Energy Physics, Particle physics, Photon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, QC770-798, 01 natural sciences, Atomic, Standard Model, High Energy Physics - Phenomenology (hep-ph), Particle and Plasma Physics, Nuclear and particle physics. Atomic energy. Radioactivity, 0103 physical sciences, Perturbative QCD, Nuclear, Symmetry breaking, 010306 general physics, Mathematical Physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Quantum Physics, 010308 nuclear & particles physics, Electroweak interaction, High Energy Physics::Phenomenology, Molecular, hep-ph, Nuclear & Particles Physics, High Energy Physics - Phenomenology, Antiproton, astro-ph.CO, High Energy Physics::Experiment, Resummation, Neutrino, Regular Article - Theoretical Physics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We compute the decay spectrum for dark matter (DM) with masses above the scale of electroweak symmetry breaking, all the way to the Planck scale. For an arbitrary hard process involving a decay to the unbroken standard model, we determine the prompt distribution of stable states including photons, neutrinos, positrons, and antiprotons. These spectra are a crucial ingredient in the search for DM via indirect detection at the highest energies as being probed in current and upcoming experiments including IceCube, HAWC, CTA, and LHAASO. Our approach improves considerably on existing methods. For example, we include all relevant electroweak interactions. The importance of these effects grow with DM mass, and by an EeV our spectra can differ by orders of magnitude from existing results., 8+24 pages, 3+12 figures, updated to published version. Spectra available at https://github.com/nickrodd/HDMSpectra
Published: 2021

2. Deep Search for Decaying Dark Matter with XMM-Newton Blank-Sky Observations

Author: Yujin Park, Benjamin R. Safdi, Marius Kongsore, Kyle Cranmer, Nicholas L. Rodd, Joshua W. Foster, and Christopher Dessert
Subjects: Sterile neutrino, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Continuum (design consultancy), Dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics, 01 natural sciences, Standard Model, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Galactic Center, High Energy Physics - Phenomenology, 13. Climate action, Sky, High Energy Physics::Experiment, Halo, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Sterile neutrinos with masses in the keV range are well-motivated extensions to the Standard Model that could explain the observed neutrino masses while also making up the dark matter (DM) of the Universe. If sterile neutrinos are DM then they may slowly decay into active neutrinos and photons, giving rise to the possibility of their detection through narrow spectral features in astrophysical X-ray data sets. In this work, we perform the most sensitive search to date for this and other decaying DM scenarios across the mass range from 5 to 16 keV using archival XMM-Newton data. We reduce 547 Ms of data from both the MOS and PN instruments using observations taken across the full sky and then use this data to search for evidence of DM decay in the ambient halo of the Milky Way. We determine the instrumental and astrophysical baselines with data taken far away from the Galactic Center, and use Gaussian Process modeling to capture additional continuum background contributions. No evidence is found for unassociated X-ray lines, leading us to produce the strongest constraints to date on decaying DM in this mass range., 8+29 pages, 3+31 figures, Supplementary Data at https://github.com/bsafdi/XMM_BSO_DATA ; v2 additional cross-checks, expanded discussion
Published: 2021

3. Prospects for detecting heavy WIMP dark matter with the Cherenkov Telescope Array: The Wino and Higgsino

Author: Oscar Macias, Tracy R. Slatyer, Lucia Rinchiuso, Nicholas L. Rodd, Emmanuel Moulin, Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and Département de Physique des Particules (ex SPP) (DPhP)
Subjects: Cherenkov Telescope Array, scale: TeV, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Wino, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Cherenkov counter: atmosphere, WIMP: dark matter, 01 natural sciences, thermal, Standard Model, mass: scale, WIMP, 0103 physical sciences, Higgsino, 010306 general physics, Cherenkov radiation, Physics, background, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, sensitivity, cosmic radiation, Weakly interacting massive particles, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics
Abstract: TeV-scale particles that couple to the standard model through the weak force represent a compelling class of dark matter candidates. The search for such Weakly Interacting Massive Particles (WIMPs) has already spanned multiple decades, and whilst it has yet to provide any definitive evidence for their existence, viable parameter space remains. In this paper, we show that the upcoming Cherenkov Telescope Array (CTA) has significant sensitivity to uncharted parameter space at the TeV mass scale. To do so, we focus on two prototypical dark matter candidates, the Wino and Higgsino. Sensitivity forecasts for both models are performed including the irreducible background from misidentified cosmic rays, as well as a range of estimates for the Galactic emissions at TeV energies. For each candidate, we find substantial expected improvements over existing bounds from current imaging atmospheric Cherenkov telescopes. In detail, for the Wino we find a sensitivity improvement of roughly an order of magnitude in $\langle \sigma v \rangle$, whereas for the Higgsino we demonstrate that CTA has the potential to become the first experiment that has sensitivity to the thermal candidate. Taken together, these enhanced sensitivities demonstrates the discovery potential for dark matter at CTA in the 1-100 TeV mass range.
Published: 2021

4. Foreground mismodeling and the point source explanation of the Fermi Galactic Center excess

Author: Laura J. Chang, Oscar Macias, Mariangela Lisanti, Malte Buschmann, Siddharth Mishra-Sharma, Nicholas L. Rodd, Benjamin R. Safdi, and GRAPPA (ITFA, IoP, FNWI)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Point source, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Population, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), Millisecond pulsar, 0103 physical sciences, 010306 general physics, education, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Annihilation, 010308 nuclear & particles physics, Galactic Center, High Energy Physics - Phenomenology, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: The Fermi Large Area Telescope has observed an excess of ~GeV energy gamma rays from the center of the Milky Way, which may arise from near-thermal dark matter annihilation. Firmly establishing the dark matter origin for this excess is however complicated by challenges in modeling diffuse cosmic-ray foregrounds as well as unresolved astrophysical sources, such as millisecond pulsars. Non-Poissonian Template Fitting (NPTF) is one statistical technique that has previously been used to show that at least some fraction of the GeV excess is likely due to a population of dim point sources. These results were recently called into question by Leane and Slatyer (2019), who showed that a synthetic dark matter annihilation signal injected on top of the real Fermi data is not recovered by the NPTF procedure. In this work, we perform a dedicated study of the Fermi data and explicitly show that the central result of Leane and Slatyer (2019) is likely driven by the fact that their choice of model for the Galactic foreground emission does not provide a sufficiently good description of the data. We repeat the NPTF analyses using a state-of-the-art model for diffuse gamma-ray emission in the Milky Way and introduce a novel statistical procedure, based on spherical-harmonic marginalization, to provide an improved description of the Galactic diffuse emission in a data-driven fashion. With these improvements, we find that the NPTF results continue to robustly favor the interpretation that the Galactic Center excess is due, in part, to unresolved astrophysical point sources across the analysis variations that we have explored., Comment: 27 pages, 18 figures, comments welcome
Published: 2020

5. Characterizing the nature of the unresolved point sources in the Galactic Center: An assessment of systematic uncertainties

Author: Malte Buschmann, Nicholas L. Rodd, Benjamin R. Safdi, Mariangela Lisanti, Laura J. Chang, and Siddharth Mishra-Sharma
Subjects: Physics, Annihilation, 010308 nuclear & particles physics, Point source, Astrophysics::High Energy Astrophysical Phenomena, Galactic Center, Dark matter, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Millisecond pulsar, 0103 physical sciences, 010306 general physics, Luminosity function, Fermi Gamma-ray Space Telescope
Abstract: The Galactic Center Excess (GCE) of GeV gamma rays can be explained as a signal of annihilating dark matter or of emission from unresolved astrophysical sources, such as millisecond pulsars. Evidence for the latter is provided by a statistical procedure---referred to as Non-Poissonian Template Fitting (NPTF)---that distinguishes the smooth distribution of photons expected for dark matter annihilation from a "clumpy" photon distribution expected for point sources. In this paper, we perform an extensive study of the NPTF on simulated data, exploring its ability to recover the flux and luminosity function of unresolved sources at the Galactic Center. When astrophysical background emission is perfectly modeled, we find that the NPTF successfully distinguishes between the dark matter and point source hypotheses when either component makes up the entirety of the GCE. When the GCE is a mixture of dark matter and point sources, the NPTF may fail to reconstruct the correct contribution of each component. We further study the impact of mismodeling the Galactic diffuse backgrounds, finding that while a dark matter signal could be attributed to point sources in some outlying cases for the scenarios we consider, the significance of a true point source signal remains robust. Our work enables us to comment on a recent study by Leane and Slatyer (2019) that questions prior NPTF conclusions because the method does not recover an artificial dark matter signal injected on actual Fermi data. We demonstrate that the failure of the NPTF to extract an artificial dark matter signal can be natural when point sources are present in the data---with the effect further exacerbated by the presence of diffuse mismodeling---and does not on its own invalidate the conclusions of the NPTF analysis in the Inner Galaxy.
Published: 2020

6. Indirect searches for dark matter bound state formation and level transitions

Author: Nicholas L. Rodd, Francesca Calore, Iason Baldes, Kalliopi Petraki, Vincent Poireau, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Hautes Energies (LPTHE), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)
Subjects: Particle physics, Photon, Dark matter, General Physics and Astronomy, Flux, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Dark photon, GLAST, High Energy Physics - Phenomenology (hep-ph), photon: mass, 0103 physical sciences, Bound state, mediation, 010306 general physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Annihilation, 010308 nuclear & particles physics, energy: dissipation, Généralités, dark matter: annihilation, Dissipation, stability, bound state: formation, lcsh:QC1-999, flux, High Energy Physics - Phenomenology, Yield (chemistry), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], lcsh:Physics
Abstract: Indirect searches for dark matter (DM) have conventionally been applied to the products of DM annihilation or decay. If DM couples to light force carriers, however, it can be captured into bound states via dissipation of energy that may yield detectable signals. We extend the indirect searches to DM bound state formation and transitions between bound levels, and constrain the emission of unstable dark photons. Our results significantly refine the predicted signal flux that could be observed in experiments. As a concrete example, we use Fermi-LAT dwarf spheroidal observations to obtain constraints in terms of the dark photon mass and energy which we use to search for the formation of stable or unstable bound states., SCOPUS: ar.j, info:eu-repo/semantics/published
Published: 2020
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7. Response to a comment on Dessert et al. 'The dark matter interpretation of the 3.5 keV line is inconsistent with blank-sky observations'

Author: Christopher Dessert, Nicholas L. Rodd, and Benjamin R. Safdi
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, FOS: Physical sciences, Astrophysics, 01 natural sciences, Blank, Atomic, Interpretation (model theory), Particle and Plasma Physics, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Nuclear, 010303 astronomy & astrophysics, media_common, Line (formation), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Molecular, Astronomy and Astrophysics, High Energy Physics - Phenomenology, Space and Planetary Science, Sky, Astrophysics - High Energy Astrophysical Phenomena, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The dark matter explanation of the 3.5 keV line is strongly disfavored by our work in Dessert et al. 2020. Boyarsky et al. 2020 questions that conclusion: modeling additional background lines is claimed to weaken the limit sufficiently to re-allow a dark matter interpretation. We respond as follows. 1) A more conservative limit is obtained by modeling additional lines; this point appeared in its entirety in our work in Dessert et al., though we also showed that the inclusion of such lines is not necessary. 2) Despite suggestions in Boyarsky et al., even the more conservative limits strongly disfavor a decaying dark matter origin of the 3.5 keV line., Comment: 7 pages, 1 figure, response to technical comment solicited by Science. Version published in PDU. Full analysis available at https://github.com/bsafdi/BlankSkyfor3p5
Published: 2020
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8. Comment on 'Characterizing the population of pulsars in the Galactic bulge with the Fermi large area telescope' [arXiv:1705.00009v1]

Author: Siddharth Mishra-Sharma, Tracy R. Slatyer, Tim Linden, Benjamin R. Safdi, Richard Bartels, Dan Hooper, and Nicholas L. Rodd
Subjects: Physics, education.field_of_study, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Galactic Center, Population, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Pulsar, Space and Planetary Science, Bulge, Millisecond pulsar, 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function, Fermi Gamma-ray Space Telescope
Abstract: The Fermi-LAT Collaboration recently presented a new catalog of gamma-ray sources located within the 40 ° × 40 ° region around the Galactic Center Ajello et al. (2017) — the Second Fermi Inner Galaxy (2FIG) catalog. Utilizing this catalog, they analyzed models for the spatial distribution and luminosity function of sources with a pulsar-like gamma-ray spectrum. Ajello et al. (2017) v1 also claimed to detect, in addition to a disk-like population of pulsar-like sources, an approximately 7 σ preference for an additional centrally concentrated population of pulsar-like sources, which they referred to as a “Galactic Bulge” population. Such a population would be of great interest, as it would support a pulsar interpretation of the gamma-ray excess that has long been observed in this region. In an effort to further explore the implications of this new source catalog, we attempted to reproduce the results presented by the Fermi-LAT Collaboration, but failed to do so. Mimicking as closely as possible the analysis techniques undertaken in Ajello et al. (2017), we instead find that our likelihood analysis favors a very different spatial distribution and luminosity function for these sources. Most notably, our results do not exhibit a strong preference for a “Galactic Bulge” population of pulsars. Furthermore, we find that masking the regions immediately surrounding each of the 2FIG pulsar candidates does not significantly impact the spectrum or intensity of the Galactic Center gamma-ray excess. Although these results refute the claim of strong evidence for a centrally concentrated pulsar population presented in Ajello et al. (2017), they neither rule out nor provide support for the possibility that the Galactic Center excess is generated by a population of low-luminosity and currently largely unobserved pulsars. In a spirit of maximal openness and transparency, we have made our analysis code available at https://github.com/bsafdi/GCE-2FIG .
Published: 2018

9. Precision Photon Spectra for Wino Annihilation

Author: Ian Moult, Varun Vaidya, Nicholas L. Rodd, Timothy Cohen, Matthew Baumgart, Emmanuel Moulin, Iain W. Stewart, Lucia Rinchiuso, Tracy R. Slatyer, Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and Département de Physique des Particules (ex SPP) (DPhP)
Subjects: Nuclear and High Energy Physics, Particle physics, Photon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), electroweak interaction: symmetry breaking, leading logarithm approximation: higher-order, FOS: Physical sciences, photon: spectrum, Photon energy, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), effective field theory, factorization, 0103 physical sciences, Jets, Effective field theory, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, Symmetry breaking, Resummation, 010306 general physics, Phenomenological Models, Physics, Coupling constant, High Energy Astrophysical Phenomena (astro-ph.HE), Annihilation, electroweak interaction: coupling constant, 010308 nuclear & particles physics, Electroweak interaction, higher-order: 1, dark matter: annihilation, photon: energy, High Energy Physics - Phenomenology, annihilation, SU(2), resummation, Wino: annihilation, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], lcsh:QC770-798, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We provide precise predictions for the hard photon spectrum resulting from neutral SU$(2)_W$ triplet (wino) dark matter annihilation. Our calculation is performed utilizing an effective field theory expansion around the endpoint region where the photon energy is near the wino mass. This has direct relevance to line searches at indirect detection experiments. We compute the spectrum at next-to-leading logarithmic (NLL) accuracy within the framework established by a factorization formula derived previously by our collaboration. This allows simultaneous resummation of large Sudakov logarithms (arising from a restricted final state) and Sommerfeld effects. Resummation at NLL accuracy shows good convergence of the perturbative series due to the smallness of the electroweak coupling constant - scale variation yields uncertainties on our NLL prediction at the level of $5\%$. We highlight a number of interesting field theory effects that appear at NLL associated with the presence of electroweak symmetry breaking, which should have more general applicability. We also study the importance of using the full spectrum as compared with a single endpoint bin approximation when computing experimental limits. Our calculation provides a state of the art prediction for the hard photon spectrum that can be easily generalized to other DM candidates, allowing for the robust interpretation of data collected by current and future indirect detection experiments., Comment: 56 pages, 12 figures; v2, updated to JHEP version
Published: 2019

10. Hunting for Heavy Winos in the Galactic Center

Author: Iain W. Stewart, Timothy Cohen, Ian Moult, Matthew Baumgart, Emmanuel Moulin, Varun Vaidya, Nicholas L. Rodd, Lucia Rinchiuso, Tracy R. Slatyer, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Département de Physique des Particules (ex SPP) (DPP), and Département de Physique des Particules (ex SPP) (DPhP)
Subjects: dark matter: interaction, Astrophysics, showers: hadronic, 7. Clean energy, 01 natural sciences, thermal, High Energy Physics - Phenomenology (hep-ph), effective field theory, WIMP, energy resolution: effect, HESS, Effective field theory, gamma ray: flux, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Annihilation, Wino: heavy, Galactic Center, imaging, tension, photon: energy spectrum, High Energy Physics - Phenomenology, electron: background, soft collinear effective theory, numerical calculations: Monte Carlo, Astrophysics - High Energy Astrophysical Phenomena, cosmic radiation: flux, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, FOS: Physical sciences, dark matter: density, Photon energy, Cherenkov counter: atmosphere, 0103 physical sciences, finite energy, 010306 general physics, Line search, electroweak interaction, 010308 nuclear & particles physics, pi: decay, dark matter: annihilation, sensitivity, Galaxy, gamma ray: VHE, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], spectral, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, Astrophysics and astroparticle physics
Abstract: Observing gamma rays using ground-based atmospheric Cherenkov telescopes provides one of the only probes of heavy weakly interacting dark matter. A canonical target is the thermal wino, for which the strongest limits come from searches for photon lines from annihilations in the Galactic Center. Irreducible finite energy resolution effects motivate refining the prediction for a wino signal beyond the photon line approximation; recently, modern effective field theory techniques have been utilized to obtain a precise calculation of the full photon energy spectrum from wino annihilation. In this paper, we investigate the implications for a realistic mock H.E.S.S.-like line search. We emphasize the impact of including the non-trivial spectral shape, and we carefully treat the region of interest, presenting results for choices between $1^{\circ}$ and $4^{\circ}$ from the Galactic Center. Projected limits for wino masses from $1$-$70$ TeV are interpreted as a constraint on the wino annihilation rate, or alternatively as the minimum core size required such that the wino is not excluded. If there is a thermal wino, H.E.S.S. will be able to probe cores of several kpc, which would begin to cause tension between this dark matter candidate and astrophysical observations/simulations., 18 pages, 14 figures
Published: 2018

11. Revealing the dark matter halo with axion direct detection

Author: Nicholas L. Rodd, Joshua W. Foster, and Benjamin R. Safdi
Subjects: Physics, Quantum chromodynamics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cold dark matter, 010308 nuclear & particles physics, Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Gravitation, Dark matter halo, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Gravitational field, 0103 physical sciences, Substructure, 010306 general physics, Axion, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The next generation of axion direct detection experiments may rule out or confirm axions as the dominant source of dark matter. We develop a general likelihood-based framework for studying the time-series data at such experiments, with a focus on the role of dark-matter astrophysics, to search for signatures of the QCD axion or axion like particles. We illustrate how in the event of a detection the likelihood framework may be used to extract measures of the local dark matter phase-space distribution, accounting for effects such as annual modulation and gravitational focusing, which is the perturbation to the dark matter phase-space distribution by the gravitational field of the Sun. Moreover, we show how potential dark matter substructure, such as cold dark matter streams or a thick dark disk, could impact the signal. For example, we find that when the bulk dark matter halo is detected at 5$\sigma$ global significance, the unique time-dependent features imprinted by the dark matter component of the Sagittarius stream, even if only a few percent of the local dark matter density, may be detectable at $\sim$2$\sigma$ significance. A co-rotating dark disk, with lag speed $\sim$50 km$/$s, that is $\sim$20$\%$ of the local DM density could dominate the signal, while colder but as-of-yet unknown substructure may be even more important. Our likelihood formalism, and the results derived with it, are generally applicable to any time-series based approach to axion direct detection., Comment: 34 pages, 12 figures, code available at: https://github.com/bsafdi/AxiScan v2, updated to PRD version v3, minor improvements
Published: 2018

12. What the Milky Way’s dwarfs tell us about the Galactic Center extended gamma-ray excess

Author: Kevork N. Abazajian, Ryan E. Keeley, Anna Kwa, Benjamin R. Safdi, and Nicholas L. Rodd
Subjects: Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Milky Way, Galactic Center, Dark matter, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Dark matter halo, Spitzer Space Telescope, 0103 physical sciences, Halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Fermi Gamma-ray Space Telescope
Abstract: Author(s): Keeley, Ryan E; Abazajian, Kevork N; Kwa, Anna; Rodd, Nicholas L; Safdi, Benjamin R | Abstract: The Milky Way's Galactic Center harbors a gamma-ray excess that is a candidate signal of annihilating dark matter. Dwarf galaxies remain predominantly dark in their expected commensurate emission. In this work we quantify the degree of consistency between these two observations through a joint likelihood analysis. In doing so 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 preferred range of annihilation rates and masses expands when including these unknowns. Even so, using two recent determinations of the Milky Way halo's local density leave the GCE preferred region of single-channel dark matter annihilation models to be in strong tension with annihilation searches in combined dwarf galaxy analyses. A third, higher Milky Way density determination, alleviates this tension. Our joint likelihood analysis allows us to quantify this inconsistency. We provide a set of tools for testing dark matter annihilation models' consistency within this combined dataset. As an example, we test a representative inverse Compton sourced self-interacting dark matter model, which is consistent with both the GCE and dwarfs.
Published: 2018

13. A Search for Dark Matter in the Galactic Halo with HAWC

Author: E. Moreno, D. W. Fiorino, Andrea Albert, J. Pretz, Benjamin R. Safdi, Dirk Lennarz, Luis Villaseñor, R. Arceo, Chad Brisbois, Michael DuVernois, R. Luna-Garcia, A. Carraminana, Giacomo Vianello, J. A. Goodman, A. Zepeda, J. P. Harding, J. T. Linnemann, Maria Magdalena González, R. J. Lauer, A. Becerril, Fernando Garfias, Thomas Weisgarber, Juan Carlos Diaz-Velez, Karen S. Caballero-Mora, Ruben Alfaro, E. Ruiz-Velasco, Jesús Martínez-Castro, A. Hernandez-Almada, Tomás Capistrán, Nicholas L. Rodd, H. A. Ayala Solares, O. Enríquez-Rivera, I. Martinez-Castellanos, Ernesto Belmont-Moreno, Daniel Rosa-Gonzalez, Z. Ren, Filiberto Hueyotl-Zahuantitla, Miguel Mostafa, Pedro Miranda-Romagnoli, F. Salesa Greus, H. León Vargas, John Matthews, Anushka Udara Abeysekara, Umberto Cotti, C. De León, I. Taboada, Sabrina Casanova, V. Joshi, Segev BenZvi, Michael Newbold, P. W. Younk, E. De la Fuente, D. Avila Rojas, Ibrahim Torres, Jorge Cotzomi, Abel Bernal, J. C. Arteaga-Velázquez, O. Tibolla, Henrike Fleischhack, G. B. Yodh, Kelly Malone, J. D. Álvarez, Kristi Engel, A. Sandoval, Armelle Jardin-Blicq, M. Castillo, R. Noriega-Papaqui, S. Hernandez, M. J. F. Rosenberg, Michael Schneider, I. G. Wisher, A. González Muñoz, William H. Lee, Brenda Dingus, Sarah Kaufmann, James W. Wood, Arturo Iriarte, Gilgamesh Luis-Raya, Kirsten Tollefson, T. Yapici, Rodrigo Pelayo, O. Martinez, S. Westerhoff, Hao Zhou, Petra Hüntemeyer, T. N. Ukwatta, Pooja Surajbali, Gus Sinnis, Jose Andres Garcia-Gonzalez, Nissim Illich Fraija, S. S. Marinelli, R. W. Springer, E. G. Pérez-Pérez, A. J. Smith, C. Alvarez, L. Nellen, Z. Hampel-Arias, R. Diaz Hernandez, Ruben Lopez-Coto, Anna Lia Longinotti, Humberto Ibarguen Salazar, Mehr Nisa, Chang Dong Rho, and HAWC Collaboartion
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Cosmic background radiation, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galactic halo, High Energy Physics - Phenomenology (hep-ph), Observatory, 0103 physical sciences, 010303 astronomy & astrophysics, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, Physics, HAWC - Abteilung Hinton, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, High Energy Physics - Phenomenology, Navarro–Frenk–White profile, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The High Altitude Water Cherenkov (HAWC) gamma-ray observatory is a wide field-of-view observatory sensitive to 500 GeV - 100 TeV gamma rays and cosmic rays. With its observations over 2/3 of the sky every day, the HAWC observatory is sensitive to a wide variety of astrophysical sources, including possible gamma rays from dark matter. Dark matter annihilation and decay in the Milky Way Galaxy should produce gamma-ray signals across many degrees on the sky. The HAWC instantaneous field-of-view of 2 sr enables observations of extended regions on the sky, such as those from dark matter in the Galactic halo. Here we show limits on the dark matter annihilation cross-section and decay lifetime from HAWC observations of the Galactic halo with 15 months of data. These are some of the most robust limits on TeV and PeV dark matter, largely insensitive to the dark matter morphology. These limits begin to constrain models in which PeV IceCube neutrinos are explained by dark matter which primarily decays into hadrons., 24 pages, 11 figures
Published: 2017

14. Disentangling heavy flavor at colliders

Author: Jesse Thaler, Nicholas L. Rodd, Mike Williams, and Philip Ilten
Subjects: Quantum chromodynamics, Physics, Quark, Particle physics, 010308 nuclear & particles physics, High Energy Physics::Lattice, High Energy Physics::Phenomenology, Hadron, FOS: Physical sciences, Quarkonium, 01 natural sciences, High Energy Physics - Experiment, Gluon, Nuclear physics, High Energy Physics - Phenomenology, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, High Energy Physics::Experiment, Nuclear Experiment, 010306 general physics
Abstract: We propose two new analysis strategies for studying charm and beauty quarks at colliders. The first strategy is aimed at testing the kinematics of heavy-flavor quarks within an identified jet. Here, we use the SoftDrop jet-declustering algorithm to identify two subjets within a large-radius jet, using subjet flavor tagging to test the heavy-quark splitting functions of QCD. For subjets containing a $J / \psi$ or $\Upsilon$, this declustering technique can also help probe the mechanism for quarkonium production. The second strategy is aimed at isolating heavy-flavor production from gluon splitting. Here, we introduce a new FlavorCone algorithm, which smoothly interpolates from well-separated heavy-quark jets to the gluon-splitting regime where jets overlap. Because of its excellent ability to identify charm and beauty hadrons, the LHCb detector is ideally suited to pursue these strategies, though similar measurements should also be possible at ATLAS and CMS. Together, these SoftDrop and FlavorCone studies should clarify a number of aspects of heavy-flavor physics at colliders, and provide crucial information needed to improve heavy-flavor modeling in parton-shower generators., Comment: 22 pages, 14 figures; v2: updated figures with new z_tag condition, references and discussion added
Published: 2017

15. Mapping Extragalactic Dark Matter Annihilation with Galaxy Surveys: A Systematic Study of Stacked Group Searches

Author: Risa H. Wechsler, Mariangela Lisanti, Benjamin R. Safdi, Nicholas L. Rodd, and Siddharth Mishra-Sharma
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Dwarf galaxy problem, Dark matter, Scalar field dark matter, FOS: Physical sciences, Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Dark matter halo, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Galaxy formation and evolution, Dark galaxy, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Galaxy rotation curve, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Dark matter in the halos surrounding galaxy groups and clusters can annihilate to high-energy photons. Recent advancements in the construction of galaxy group catalogs provide many thousands of potential extragalactic targets for dark matter. In this paper, we outline a procedure to infer the dark matter signal associated with a given galaxy group. Applying this procedure to a catalog of sources, one can create a full-sky map of the brightest extragalactic dark matter targets in the nearby Universe ($z\lesssim 0.03$), supplementing sources of dark matter annihilation from within the Local Group. As with searches for dark matter in dwarf galaxies, these extragalactic targets can be stacked together to enhance the signals associated with dark matter. We validate this procedure on mock $\textit{Fermi}$ gamma-ray data sets using a galaxy catalog constructed from the $\texttt{DarkSky}$ $N$-body cosmological simulation and demonstrate that the limits are robust, at $\mathcal{O}(1)$ levels, to systematic uncertainties on halo mass and concentration. We also quantify other sources of systematic uncertainty arising from the analysis and modeling assumptions. Our results suggest that a stacking analysis using galaxy group catalogs provides a powerful opportunity to discover extragalactic dark matter and complements existing studies of Milky Way dwarf galaxies., 17+7 pages, 9+4 figures; v2, updated to PRD version with several updates, results and conclusions unchanged
Published: 2017

16. A Search for Dark Matter Annihilation in Galaxy Groups

Author: Siddharth Mishra-Sharma, Nicholas L. Rodd, Benjamin R. Safdi, and Mariangela Lisanti
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Hot dark matter, Scalar field dark matter, General Physics and Astronomy, Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Dark matter halo, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Mixed dark matter, Galaxy formation and evolution, Warm dark matter, Dark galaxy, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Light dark matter, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use 413 weeks of publicly-available $\textit{Fermi}$ Pass 8 gamma-ray data, combined with recently-developed galaxy group catalogs, to search for evidence of dark matter annihilation in extragalactic halos. In our study, we use luminosity-based mass estimates and mass-to-concentration relations to infer the $J$-factors and associated uncertainties for hundreds of galaxy groups within a redshift range $z \lesssim 0.03$. We employ a conservative substructure boost-factor model, which only enhances the sensitivity by an $\mathcal{O}(1)$ factor. No significant evidence for dark matter annihilation is found and we exclude thermal relic cross sections for dark matter masses below $\sim$30 GeV to 95% confidence in the $b\bar{b}$ annihilation channel. These bounds are comparable to those from Milky Way dwarf spheroidal satellite galaxies. The results of our analysis increase the tension, but do not rule out, the dark matter interpretation of the Galactic Center excess. We provide a catalog of the galaxy groups used in this study and their inferred properties, which can be broadly applied to searches for extragalactic dark matter., 5+18 pages, 1+14 figures, catalog available at: https://github.com/bsafdi/DMCat; v2 updated to journal version with several updates, results and conclusions unchanged
Published: 2017

17. γ-ray Constraints on Decaying Dark Matter and Implications for IceCube

Author: Benjamin R. Safdi, Nicholas L. Rodd, Yotam Soreq, Kohta Murase, and Timothy Cohen
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Cosmic background radiation, General Physics and Astronomy, Flux, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Galaxy, Hidden sector, High Energy Physics - Phenomenology, 13. Climate action, High Energy Physics::Experiment, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: Utilizing the Fermi measurement of the gamma-ray spectrum toward the Galactic Center, we derive some of the strongest constraints to date on the dark matter (DM) lifetime in the mass range from hundreds of MeV to above an EeV. Our profile-likelihood based analysis relies on 413 weeks of Fermi Pass 8 data from 200 MeV to 2 TeV, along with up-to-date models for diffuse gamma-ray emission within the Milky Way. We model Galactic and extragalactic DM decay and include contributions to the DM-induced gamma-ray flux resulting from both primary emission and inverse-Compton scattering of primary electrons and positrons. For the extragalactic flux, we also calculate the spectrum associated with cascades of high-energy gamma-rays scattering off of the cosmic background radiation. We argue that a decaying DM interpretation for the 10 TeV-1 PeV neutrino flux observed by IceCube is disfavored by our constraints. Our results also challenge a decaying DM explanation of the AMS-02 positron flux. We interpret the results in terms of individual final states and in the context of simplified scenarios such as a hidden-sector glueball model., Comment: Updated to correct an issue in Fig. S12, 9+19 pages, 2+14 figures, Supplementary Data available at https://dspace.mit.edu/handle/1721.1/105550
Published: 2017

18. The One-Loop Correction to Heavy Dark Matter Annihilation

Author: Nicholas L. Rodd, Tracy R. Slatyer, Iain W. Stewart, and Grigory Ovanesyan
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Annihilation, 010308 nuclear & particles physics, Dark matter, Scalar field dark matter, FOS: Physical sciences, Scale (descriptive set theory), Fermion, 01 natural sciences, Nuclear physics, Loop (topology), MAJORANA, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Astrophysics - High Energy Astrophysical Phenomena, Boson, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We calculate the one-loop corrections to TeV scale dark matter annihilation in a model where the dark matter is described by an SU(2)$_L$ triplet of Majorana fermions, such as the wino. We use this framework to determine the high and low-scale MS-bar matching coefficients at both the dark matter and weak boson mass scales at one loop. Part of this calculation has previously been performed in the literature numerically; we find our analytic result differs from the earlier work and discuss potential origins of this disagreement. Our result is used to extend the dark matter annihilation rate to NLL' (NLL+O($\alpha_2$) corrections) which enables a precise determination of indirect detection signatures in present and upcoming experiments., Comment: 27 pages, 5 figures. Corrected counter-term contributions, fixing an issue first noted in 1805.07367. Impact on final results in plots is imperceptible, leaving the conclusions and numerical analysis unchanged
Published: 2016

19. Model-independent indirect detection constraints on hidden sector dark matter

Author: Tracy R. Slatyer, Nicholas L. Rodd, Wei Xue, Gilly Elor, Massachusetts Institute of Technology. Center for Theoretical Physics, Massachusetts Institute of Technology. Department of Physics, Elor, Gilly, Rodd, Nicholas Llewellyn, Slatyer, Tracy Robyn, and Xue, Wei
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Particle physics, Annihilation, 010308 nuclear & particles physics, Dark matter, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Hidden sector, High Energy Physics - Phenomenology, symbols.namesake, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, symbols, Neutrino, Planck, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, Fermi Gamma-ray Space Telescope
Abstract: If dark matter inhabits an expanded ``hidden sector'', annihilations may proceed through sequential decays or multi-body final states. We map out the potential signals and current constraints on such a framework in indirect searches, using a model-independent setup based on multi-step hierarchical cascade decays. While remaining agnostic to the details of the hidden sector model, our framework captures the generic broadening of the spectrum of secondary particles (photons, neutrinos, e+e− and p̄ p) relative to the case of direct annihilation to Standard Model particles. We explore how indirect constraints on dark matter annihilation limit the parameter space for such cascade/multi-particle decays. We investigate limits from the cosmic microwave background by Planck, the Fermi measurement of photons from the dwarf galaxies, and positron data from AMS-02. The presence of a hidden sector can change the constraints on the dark matter by up to an order of magnitude in either direction (although the effect can be much smaller). We find that generally the bound from the Fermi dwarfs is most constraining for annihilations to photon-rich final states, while AMS-02 is most constraining for electron and muon final states; however in certain instances the CMB bounds overtake both, due to their approximate independence on the details of the hidden sector cascade. We provide the full set of cascade spectra considered here as publicly available code with examples at http://web.mit.edu/lns/research/CascadeSpectra.html., United States. Department of Energy (grant contract number DE-SC00012567), United States. Department of Energy (grant contract number DE−SC0013999)
Published: 2016

20. The High-Energy Tail of the Galactic Center Gamma-Ray Excess

Author: Tracy R. Slatyer, Benjamin R. Safdi, Tim Linden, and Nicholas L. Rodd
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Galactic Center, Center (category theory), Gamma ray, FOS: Physical sciences, Astrophysics, Galactic plane, 01 natural sciences, Galaxy, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Energy (signal processing), Fermi Gamma-ray Space Telescope
Abstract: Observations by the Fermi-LAT have uncovered a bright, spherically symmetric excess surrounding the center of the Milky Way galaxy. The spectrum of the gamma-ray excess peaks sharply at an energy ~2 GeV, exhibiting a hard spectrum at lower energies, and falls off quickly above an energy ~5 GeV. The spectrum of the excess above ~10 GeV is potentially an important discriminator between different physical models for its origin. We focus our study on observations of the gamma-ray excess at energies exceeding 10 GeV, finding: (1) a statistically significant excess remains in the energy range 9.5-47.5 GeV, which is not degenerate with known diffuse emission templates such as the Fermi Bubbles, (2) the radial profile of the excess at high energies remains relatively consistent with data near the spectral peak, (3) the data above ~5 GeV prefer a slightly greater ellipticity with a major axis oriented perpendicular to the Galactic plane. Using the recently developed non-Poissonian template fit, we find mild evidence for a point-source origin for the high-energy excess, although given the statistical and systematic uncertainties we show that a smooth origin of the high-energy emission cannot be ruled out. We discuss the implication of these findings for pulsar and dark matter models of the gamma-ray excess. Finally we provide a number of updated measurements of the gamma-ray excess, utilizing novel diffuse templates and the Pass 8 dataset., 40 pages, 36 figures
Published: 2016

21. NPTFit: A Code Package for Non-Poissonian Template Fitting

Author: Nicholas L. Rodd, Benjamin R. Safdi, and Siddharth Mishra-Sharma
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Milky Way, Population, FOS: Physical sciences, 01 natural sciences, Methods statistical, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Code (cryptography), education, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, computer.programming_language, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Python (programming language), High Energy Physics - Phenomenology, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Algorithm, computer, Astrophysics - Cosmology and Nongalactic Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: We present NPTFit, an open-source code package, written in python and cython, for performing non-Poissonian template fits (NPTFs). The NPTF is a recently-developed statistical procedure for characterizing the contribution of unresolved point sources (PSs) to astrophysical data sets. The NPTF was first applied to Fermi gamma-ray data to give evidence that the excess of ~GeV gamma-rays observed in the inner regions of the Milky Way likely arises from a population of sub-threshold point sources, and the NPTF has since found additional applications studying sub-threshold extragalactic sources at high Galactic latitudes. The NPTF generalizes traditional astrophysical template fits to allow for the ability to search for populations of unresolved PSs that may follow a given spatial distribution. NPTFit builds upon the framework of the fluctuation analyses developed in X-ray astronomy, and thus likely has applications beyond those demonstrated with gamma-ray data. The NPTFit package utilizes novel computational methods to perform the NPTF efficiently. The code is available at https://github.com/bsafdi/NPTFit and up-to-date and extensive documentation may be found at http://nptfit.readthedocs.io, Comment: 18 pages, 4 figure; v2, AJ version; with accompanying code at https://github.com/bsafdi/NPTFit
Published: 2017

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

Author: Douglas P. Finkbeiner, Tim Linden, Dan Hooper, Nicholas L. Rodd, Tansu Daylan, Stephen K. N. Portillo, Tracy R. Slatyer, Massachusetts Institute of Technology. Center for Theoretical Physics, Rodd, Nicholas Llewellyn, and Slatyer, Tracy Robyn
Subjects: High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), Pulsar, 0103 physical sciences, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Annihilation, 010308 nuclear & particles physics, Galactic Center, Astronomy and Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Galaxy, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Past studies have identified a spatially extended excess of ~1-3 GeV gamma rays from the region surrounding the Galactic Center, consistent with the emission expected from annihilating dark matter. We revisit and scrutinize this signal with the intention of further constraining its characteristics and origin. By applying cuts to the Fermi event parameter CTBCORE, we suppress the tails of the point spread function and generate high resolution gamma-ray maps, enabling us to more easily separate the various gamma-ray components. Within these maps, we find the GeV excess to be robust and highly statistically significant, with a spectrum, angular distribution, and overall normalization that is in good agreement with that predicted by simple annihilating dark matter models. For example, the signal is very well fit by a 36-51 GeV dark matter particle annihilating to bb with an annihilation cross section of σv=(1-3)×10-26cm3/s (normalized to a local dark matter density of 0.4 GeV/cm 3 ). Furthermore, we confirm that the angular distribution of the excess is approximately spherically symmetric and centered around the dynamical center of the Milky Way (within ~0.05 ° of Sgr A * ), showing no sign of elongation along the Galactic Plane. The signal is observed to extend to at least ≃10° from the Galactic Center, which together with its other morphological traits disfavors the possibility that this emission originates from previously known or modeled pulsar populations. Keywords: Dark matter; Indirect detection; Gamma-rays, United States. Department of Energy (Contract DE-FG02-05ER41360)
Published: 2014
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23. Search for anomalous production of prompt like-sign lepton pairs at sqrt(s) = 7 TeV with the ATLAS detector

Author: A. Dos Anjos, Emily Nurse, M. Kaci, Elizabeth Gallas, Jianbei Liu, A. B. Fenyuk, Federico Bertolucci, G. Sartisohn, Veysi Erkcan Ozcan, Andreas Petridis, Jelena Krstic, Nimrod Taiblum, Mark Slater, Andrew Nelson, L. Chikovani, U. Soldevila, F. Lepold, Ki Lie, Fumihiko Ukegawa, Andrea Formica, Venetios Polychronakos, S. Fratina, S. Marti-Garcia, A. Loginov, Marumi Kado, Al Goshaw, Kenji Hamano, J. Inigo-Golfin, Mark Scarcella, E. E. Schmidt, John Baines, R. Van Berg, Sergei Chekanov, J. Godfrey, R. Mehdiyev, M. Saleem, Gustaaf Brooijmans, J. N. Jackson, Per Werner, Simon Head, Emily Thompson, E. Torró Pastor, S. S.A. Livermore, L. Bellagamba, G. W. Brandenburg, E. Romero Adam, Aston Komar, Alberto Mengarelli, P. D. Thompson, Wladyslaw Dabrowski, G. A. Rosenbaum, J. P. Ottersbach, T. Fonseca Martin, Yona Oren, Daniel Fournier, M. S. Kayl, S. A. Olivares Pino, M. Kurata, Andrew Pilkington, Bobby Samir Acharya, H. A. Neal, M. Aharrouche, Johannes Elmsheuser, Sergey Peleganchuk, C. Cowden, I. Chalupkova, J. Hoffman, M. T. Pérez García-Estañ, Guillaume Unal, J. T. Linnemann, A. Artamonov, J. A. Gray, Gaetano Barone, E. Jansen, Alexander Khodinov, David Yu, António Amorim, Lulu Liu, A. Blondel, Giuseppe Costa, Rustem Ospanov, Sergey Panitkin, Todd Brian Huffman, K. A. Johns, B. Demirkoz, J. Colas, Marzio Nessi, T. Hayakawa, Jeremy Love, Kendall Reeves, D. Schouten, James Frost, Pier-Olivier Deviveiros, Jonas Strandberg, N. S. Knecht, Tapas Sarangi, Z. Czyczula, David Malon, Stefan Guindon, Stefania Spagnolo, Daniel Muenstermann, Vincent Garonne, Sandro Palestini, F. Mueller, E. Pueschel, Jamal Eddine Derkaoui, M. L. Andrieux, Kristin Lohwasser, Nikolai Rusakovich, T. Mueller, C. J. Curtis, J. Farley, Kevin Varvell, G. Polesello, Jan Valenta, Helio Takai, Benjamin Kaplan, Jun Wakabayashi, V. Juranek, Ph. Schwegler, J. P. Thomas, Dusan Bruncko, Paolo Francavilla, Andreas W. W. Ludwig, Kyle Cranmer, Claudio Ferretti, J. Z. Will, Anna Kaczmarska, I. Dolenc, S. N. White, Frank Fiedler, Giovanni Maccarrone, Vaclav Vrba, Heberth Torres, T. Kuhl, S. Pashapour, Francois Touchard, M. A. Wildt, P. J. Bussey, S. Lablak, Siarhei Harkusha, M. Uslenghi, Attilio Picazio, Thorsten Wengler, Laurent Vacavant, A. Rose, Giancarlo Spigo, R. Beccherle, Kathleen Whalen, S. Owen, Matthias Klein, Evgeny Starchenko, M. Mechtel, C. Padilla Aranda, A. Jantsch, Mathieu Benoit, R. R. Debbe, Yuji Yamazaki, G. Cattani, L. Micu, B. Alvarez Gonzalez, Preema Rennee Pais, Andrej Filipcic, Lydia Roos, Stephen Maxfield, N. Krieger, P. Matricon, Liron Barak, Alexander Undrus, Tatsuya Masubuchi, Oliver Keith Baker, Jiri Kvita, Yanwen Wu, Alexey Talyshev, R. Giordano, Vladimir Cindro, Pierre-Hugues Beauchemin, G. Volpi, Aaron James Armbruster, Davide Costanzo, M. G. Wilson, J-P. Meyer, I. Massa, A. Do Valle Wemans, M. Strang, Olivier Arnaez, Elliot Lipeles, Saleh Sultansoy, Antonio Salvucci, R. Tanaka, Ehud Duchovni, T. Spreitzer, Oleg Brandt, J. Hartert, Michael A. Strauss, A. M. Castaneda Hernandez, Keita Hanawa, Chong-Yu Xu, C. Melachrinos, J. Hrivnac, C. J.S. Young, J. Fleckner, A. Khomich, M. Kaneda, Philip Phillips, Samuel Silverstein, L. Hooft van Huysduynen, Victoria Jane Martin, John Alison, G. L. Glonti, Attila Krasznahorkay, H. O. Danielsson, Andrew D. Hamilton, J. Blocki, Sara Valentinetti, Peter Love, N. D. Topilin, V. Kartvelishvili, N. A. McCubbin, Frank Winklmeier, L. R. Flores Castillo, Luc Poggioli, Christine Kourkoumelis, E. Ros, J. D. Price, H. H. Williams, S. Youssef, Steinar Stapnes, R. Ueno, T. Cuhadar Donszelmann, R. S. Orr, I. P. Duerdoth, J. G. Saraiva, Marco Delmastro, Elena Plotnikova, A. J. Lankford, Shinichi Shimizu, L. Han, G. G.G. Massaro, P. L. Rosendahl, Marcella Bona, Abdenour Lounis, M. I. Gostkin, G. Wooden, G. Rahal, Pamela Ferrari, Sw. Banerjee, Suyog Shrestha, Paul Laycock, J. Boek, T. Ohshima, Vasiliki A Mitsou, R. Kwee, Emmanuel Sauvan, Iacopo Vivarelli, R. S. B. King, Reda Tafirout, Klaus Kurt Desch, Richard Nickerson, Y. Davygora, J. Bouchami, Francisco Alonso, M. Agustoni, Arnaud Lucotte, Y. A. Kurochkin, Liza Mijović, J. G. Rocha de Lima, R. Davidson, Pavel Staroba, S. Koenig, R. P. Thun, Pavol Strizenec, V. Sopko, J. Salt, V. A. Korotkov, Siegfried Wenig, Giuseppe Iacobucci, P. Hansson, Heiko Lacker, D. Pomeroy, Alberto Annovi, E. Perez Codina, K. J. Grahn, R. K. Keeler, J. Machado Miguens, G. Anders, Martin Rybar, Thomas Koffas, Benjamin Trocmé, J. Bronner, A. Seiden, M. Tsiakiris, C. M. Cuciuc, James Catmore, Peter Schacht, M. Turala, Kostantinos Kordas, Michael Begel, G. Sellers, L. S. Gomez Fajardo, S. Stern, R. J. Miller, M. Goebel, R. Caputo, Roberto Spighi, Sylvain Tisserant, Wolfgang Walkowiak, J. Keung, E. Vinek, C. Le Maner, N. M. Bolnet, Minoru Hirose, Steven Farrell, Fridolin Dittus, Diedi Hu, Tommaso Colombo, Sahal Yacoob, Josh Moss, Kerstin Lantzsch, F. Tarrade, D. E. Ferreira de Lima, Carlos Escobar, B. Brelier, Toshi Sumida, Zvi Hirsh Citron, Z. Zajacova, Till Eifert, Abner Soffer, F. Rühr, B. Epp, Takahiko Kondo, Pedro Jorge, Gvantsa Mchedlidze, P. Giovannini, E. Ptacek, Tom McCarthy, D. Axen, Andrea Knue, Miao Liu, Sarah Heim, Mauro Iodice, S. V. Mouraviev, Ruggero Turra, Maia Mosidze, C. Belanger-Champagne, Vipul Jain, Dominique Pallin, B. Chapleau, K. Pretzl, A. R. Davison, Igor Gavrilenko, Massimo Lamanna, E. Torrence, M. Leyton, Ben Smart, Augusto Santiago Cerqueira, M. D. Joergensen, Alexander Kupco, Edoardo Gorini, Evgeniy Khramov, Nathalie Besson, Daniele Zanzi, Predrag Cirkovic, T. Greenshaw, S. Cabrera Urbán, V. V. Zmouchko, Francesco Michelangelo Giorgi, S. Swedish, G. H. A. Viehhauser, Tomas Davidek, A. Borisov, Filippo Ceradini, R. Schwierz, John Penwell, S. Gozpinar, M. Rescigno, S. E. Allwood-Spiers, D.C. Rahm, Deepak Kar, J. A. Ernst, Nikolaos Rompotis, S. De Castro, A. V. Ivashin, Dimitris Varouchas, A. Polini, Nikolina Ilic, D. M. Gingrich, J. Glatzer, William Buttinger, A. Dotti, P. Chang, Viktor Kramarenko, M. Petteni, Manolis Dris, G. Mahout, D. De Pedis, W. Bhimji, V. Rossetti, Sandrine Laplace, A. Bogouch, James M. Buchanan, Iwona Grabowska-Bold, G. Khoriauli, J. B. Blanchard, Ikuo Ueda, D. M. Strom, G. H. Lewis, K. Amako, Enrique Kajomovitz, J. Nadal, Carlos Sandoval, David-leon Pohl, Louis Helary, B. Pinto, Anna Mastroberardino, Bruno Lenzi, T. Göpfert, Marco Schioppa, Ljiljana Morvaj, Nicola Orlando, Susanne Kuehn, Stephen Sekula, Xifeng Ruan, M. A. L. Leite, Evangelos Gazis, Enrico Rossi, K. Bendtz, H. S. Bansil, K. Ellis, B. Martin, I. Jen-La Plante, G. Tzanakos, Andrea Bocci, S. Yu. Sivoklokov, L. Batkova, Sascha Caron, E. Reinherz-Aronis, Nicholas Adam Styles, Federico Meloni, H. Duran Yildiz, C. Guicheney, H. J. Yang, Juergen Kroseberg, A. T. Doyle, F. Lo Sterzo, V. Zutshi, Cigdem Issever, Muhammad Alhroob, Hiroshi Sakamoto, R. Calkins, W. M. Thong, H. S. Chen, Antonio Limosani, K. E. Selbach, Stefania Xella, T. Rador, R. Camacho Toro, Sarah Demers, P. Cavalleri, A. Henrichs, J. J. Goodson, V. Boldea, Vladimir Sulin, T. Lari, Ryo Nagai, Antonio Sbrizzi, Fr Pastore, Michal Vlasak, Lily Asquith, C. Zeitnitz, S. Caughron, Chunhui Chen, Arnulf Quadt, E. Gornicki, A. Basye, Krzysztof Wozniak, I. Gough Eschrich, S. Tanaka, M. Vranjes Milosavljevic, Corrinne Mills, K. E. Johansson, Mark Stockton, Yoichi Ikegami, L. La Rotonda, Mauro Citterio, C. Topfel, Emmerich Kneringer, Martin Johannes Schultens, D. van der Ster, Donatella Cavalli, U. Mallik, M. Cooke, Frederic Brochu, Ryszard Stroynowski, T. Doherty, J. R. Lessard, Paul Nilsson, S. Prasad, M. Virchaux, A. M. Cooper-Sarkar, B. Budick, Lixin Ma, M. R. Jaekel, Y. Jiang, J. Ferencei, T. Vazquez Schroeder, Deywis Moreno, Raymond Brock, Ivan Sykora, L. M. Mir, Meng Xiao, Moritz Backes, Sofia Chouridou, Jason Nielsen, Michael Düren, Tobias Golling, I. Aracena, S. Haas, B. DeWilde, G. Sauvage, G. 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Montejo Berlingen, Timothy Barklow, Daria Zieminska, E. Magradze, C. A. Chavez Barajas, Andrei Snesarev, Ahmimed Ouraou, V. V. Ammosov, Alan Litke, L. K. Gladilin, C. Garc Ia, Evelin Meoni, V. Nguyen Thi Hong, Carolina Gabaldon, Stefan Stonjek, T. Burgess, Frantisek Krejci, Mark Hodgkinson, A. Harvey, V. Bansal, Jiri Chudoba, R. Mackeprang, Eiliv Lund, S. W. Snow, E. Davies, J. de Graat, G. Mirabelli, Matt Dobbs, R. E. Long, B. Clement, Q. Ouyang, V. Martinez Outschoorn, Sascha Mehlhase, S. Horner, Yasushi Nagasaka, Boris Lemmer, R. J. Hawkings, M. A. Chelstowska, Ph Gris, M. J. Losty, I. I. Tsukerman, P. Johansson, William Trischuk, Yury Tikhonov, A. Passeri, S. Fleischmann, Oxana Smirnova, T. Todorov, Konstantinos Bachas, R. D. Schamberger, E. Auge, Malte Backhaus, Pascal Pralavorio, Lamberto Luminari, M. Shamim, Maciej Trzebinski, G. Cortiana, M. Fiascaris, Gabriella Sciolla, Y. Munwes, Victor Solovyev, K. Perez, J. A. Wilson, Tomas Slavicek, P. Lichard, C. P. Marino, F. Marchese, Valery Pozdnyakov, Jean-Francois Laporte, Lidia Dell'Asta, C. Schroeder, Fabrice Hubaut, M. Aurousseau, I. Turk Cakir, Kazunori Hanagaki, G. Nanava, E. Sedykh, A. Khoroshilov, B. M. Waugh, H. Czirr, Marcello Borri, Charles Leggett, M. Rammes, Fabian Huegging, J. Wetter, A. M. Zaitsev, M. Mazzanti, A. A. Carter, M. Miñano Moya, A. Firan, S. Binet, Aldo Saavedra, Atsuhiko Ochi, S. Di Luise, James Howarth, Stephen Haywood, Sotirios Vlachos, Walter Lampl, V. Moeller, F. Parodi, David Miller, Vladimir Vinogradov, Gabriel Stoicea, T. Ženiš, C. Ruwiedel, Jing Wang, Juraj Bracinik, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Centre de Calcul de l'IN2P3 (CC-IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique Corpusculaire - Clermont-Ferrand (LPC), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Corpusculaire, Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Neutrinos, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), ATLAS, Aad, G., Bianco, Michele, Chiodini, G., Gorini, Edoardo, Primavera, Margherita, Spagnolo, Stefania Antonia, Ventura, Andrea, Doğuş Üniversitesi, Fen Edebiyat Fakültesi, Fizik Bölümü, TR3959, Çetin, Serkant Ali, G. Aad, T. Abajyan, B. Abbott, J. Abdallah, S. Abdel Khalek, A. A. Abdelalim, O. Abdinov, R. Aben, B. Abi, M. Abolin, O. S. AbouZeid, H. Abramowicz, H. Abreu, E. Acerbi, B. S. Acharya, L. Adamczyk, D. L. Adam, T. N. Addy, J. Adelman, S. Adomeit, P. Adragna, T. Adye, S. Aefsky, J. A. Aguilar-Saavedra, M. Agustoni, M. Aharrouche, S. P. Ahlen, F. Ahle, A. Ahmad, M. Ahsan, G. Aielli, T. Akdogan, T. P. A. Åkesson, G. Akimoto, A. V. Akimov, M. S. Alam, M. A. Alam, J. Albert, S. Albrand, M. Aleksa, I. N. Aleksandrov, F. Alessandria, C. Alexa, G. Alexander, G. Alexandre, T. Alexopoulo, M. Alhroob, M. Aliev, G. Alimonti, J. Alison, B. M. M. Allbrooke, P. P. Allport, S. E. Allwood-Spier, J. Almond, A. Aloisio, R. Alon, A. Alonso, F. Alonso, B. Alvarez Gonzalez, M. G. Alviggi, K. Amako, C. Amelung, V. V. Ammosov, S. P. Amor Dos Santo, A. Amorim, N. Amram, C. Anastopoulo, L. S. Ancu, N. Andari, T. Andeen, C. F. Ander, G. Ander, K. J. Anderson, A. Andreazza, V. Andrei, M-L. Andrieux, X. S. Anduaga, P. Anger, A. Angerami, F. Anghinolfi, A. Anisenkov, N. Anjo, A. Annovi, A. Antonaki, M. Antonelli, A. Antonov, J. Anto, F. Anulli, M. Aoki, S. Aoun, L. Aperio Bella, R. Apolle, G. Arabidze, I. Aracena, Y. Arai, A. T. H. Arce, S. Arfaoui, J-F. Arguin, E. Arik, M. Arik, A. J. Armbruster, O. Arnaez, V. Arnal, C. Arnault, A. Artamonov, G. Artoni, D. Arutinov, S. Asai, R. Asfandiyarov, S. Ask, B. Åsman, L. Asquith, K. Assamagan, A. Astbury, M. Atkinson, B. Aubert, E. Auge, K. Augsten, M. Aurousseau, G. Avolio, R. Avramidou, D. Axen, G. Azuelo, Y. Azuma, M. A. Baak, G. Baccaglioni, C. Bacci, A. M. Bach, H. Bachacou, K. Bacha, M. Backe, M. Backhau, E. Badescu, P. Bagnaia, S. Bahinipati, Y. Bai, D. C. Bailey, T. Bain, J. T. Baine, O. K. Baker, M. D. Baker, S. Baker, E. Bana, P. Banerjee, Sw. Banerjee, D. Banfi, A. Bangert, V. Bansal, H. S. Bansil, L. Barak, S. P. Baranov, A. Barbaro Galtieri, T. Barber, E. L. Barberio, D. Barberi, M. Barbero, D. Y. Bardin, T. Barillari, M. Barisonzi, T. Barklow, N. Barlow, B. M. Barnett, R. M. Barnett, A. Baroncelli, G. Barone, A. J. Barr, F. Barreiro, J. Barreiro Guimarães Costa, P. Barrillon, R. Bartoldu, A. E. Barton, V. Bartsch, A. Basye, R. L. Bate, L. Batkova, J. R. Batley, A. Battaglia, M. Battistin, F. Bauer, H. S. Bawa, S. Beale, T. Beau, P. H. Beauchemin, R. Beccherle, P. Bechtle, H. P. Beck, A. K. Becker, S. Becker, M. Beckingham, K. H. Beck, A. J. Beddall, A. Beddall, S. Bedikian, V. A. Bednyakov, C. P. Bee, L. J. Beemster, M. Begel, S. Behar Harpaz, P. K. Behera, M. Beimforde, C. Belanger-Champagne, P. J. Bell, W. H. Bell, G. Bella, L. Bellagamba, F. Bellina, M. Bellomo, A. Belloni, O. Beloborodova, K. Belotskiy, O. Beltramello, O. Benary, D. Benchekroun, K. Bendtz, N. Beneko, Y. Benhammou, E. Benhar Noccioli, J. A. Benitez Garcia, D. P. Benjamin, M. Benoit, J. R. Bensinger, K. Benslama, S. Bentvelsen, D. Berge, E. Bergeaas Kuutmann, N. Berger, F. Berghau, E. Berglund, J. Beringer, P. Bernat, R. Bernhard, C. Berniu, T. Berry, C. Bertella, A. Bertin, F. Bertolucci, M. I. Besana, G. J. Besje, N. Besson, S. Bethke, W. Bhimji, R. M. Bianchi, M. Bianco, O. Biebel, S. P. Bieniek, K. Bierwagen, J. Biesiada, M. Biglietti, H. Bilokon, M. Bindi, S. Binet, A. Bingul, C. Bini, C. Biscarat, B. Bittner, K. M. Black, R. E. Blair, J.-B. Blanchard, G. Blanchot, T. Blazek, I. Bloch, C. Blocker, J. Blocki, A. Blondel, W. Blum, U. Blumenschein, G. J. Bobbink, V. B. Bobrovnikov, S. S. Bocchetta, A. Bocci, C. R. Boddy, M. Boehler, J. Boek, N. Boelaert, J. A. Bogaert, A. Bogdanchikov, A. Bogouch, C. Bohm, J. Bohm, V. Boisvert, T. Bold, V. Boldea, N. M. Bolnet, M. Bomben, M. Bona, M. Boonekamp, C. N. Booth, S. Bordoni, C. Borer, A. Borisov, G. Borissov, I. Borjanovic, M. Borri, S. Borroni, V. Bortolotto, K. Bo, D. Boscherini, M. Bosman, H. Boterenbrood, J. Bouchami, J. Boudreau, E. V. Bouhova-Thacker, D. Boumediene, C. Bourdario, N. Bousson, A. Boveia, J. Boyd, I. R. Boyko, I. Bozovic-Jelisavcic, J. Bracinik, P. Branchini, G. W. Brandenburg, A. Brandt, G. Brandt, O. Brandt, U. Bratzler, B. Brau, J. E. Brau, H. M. Braun, S. F. Brazzale, B. Brelier, J. Bremer, K. Brendlinger, R. Brenner, S. Bressler, D. Britton, F. M. Brochu, I. Brock, R. Brock, F. Broggi, C. Bromberg, J. Bronner, G. Brooijman, T. Brook, W. K. Brook, G. Brown, H. Brown, P. A. Bruckman Renstrom, D. Bruncko, R. Bruneliere, S. Brunet, A. Bruni, G. Bruni, M. Bruschi, T. Buane, Q. Buat, F. Bucci, J. Buchanan, P. Buchholz, R. M. Buckingham, A. G. Buckley, S. I. Buda, I. A. Budagov, B. Budick, V. Büscher, L. Bugge, O. Bulekov, A. C. Bundock, M. Bunse, T. Buran, H. Burckhart, S. Burdin, T. Burge, S. Burke, E. Busato, P. Bussey, C. P. Buszello, B. Butler, J. M. Butler, C. M. Buttar, J. M. Butterworth, W. Buttinger, S. Cabrera Urbán, D. Caforio, O. Cakir, P. Calafiura, G. Calderini, P. Calfayan, R. Calkin, L. P. Caloba, R. Caloi, D. Calvet, S. Calvet, R. Camacho Toro, P. Camarri, D. Cameron, L. M. Caminada, R. Caminal Armadan, S. Campana, M. Campanelli, V. Canale, F. Canelli, A. Canepa, J. Cantero, R. Cantrill, L. Capasso, M. D. M. Capeans Garrido, I. Caprini, M. Caprini, D. Capriotti, M. Capua, R. Caputo, R. Cardarelli, T. Carli, G. Carlino, L. Carminati, B. Caron, S. Caron, E. Carquin, G. D. Carrillo-Montoya, A. A. Carter, J. R. Carter, J. Carvalho, D. Casadei, M. P. Casado, M. Cascella, C. Caso, A. M. Castaneda Hernandez, E. Castaneda-Miranda, V. Castillo Gimenez, N. F. Castro, G. Cataldi, P. Catastini, A. Catinaccio, J. R. Catmore, A. Cattai, G. Cattani, S. Caughron, V. Cavaliere, P. Cavalleri, D. Cavalli, M. Cavalli-Sforza, V. Cavasinni, F. Ceradini, A. S. Cerqueira, A. Cerri, L. Cerrito, F. Cerutti, S. A. Cetin, A. Chafaq, D. Chakraborty, I. Chalupkova, K. Chan, P. Chang, B. Chapleau, J. D. Chapman, J. W. Chapman, E. Chareyre, D. G. Charlton, V. Chavda, C. A. Chavez Baraja, S. Cheatham, S. Chekanov, S. V. Chekulaev, G. A. Chelkov, M. A. Chelstowska, C. Chen, H. Chen, S. Chen, X. Chen, Y. Chen, A. Cheplakov, R. Cherkaoui Moursli, V. Chernyatin, E. Cheu, S. L. Cheung, L. Chevalier, G. Chiefari, L. Chikovani, J. T. Childer, A. Chilingarov, G. Chiodini, A. S. Chisholm, R. T. Chislett, A. Chitan, M. V. Chizhov, G. Choudalaki, S. Chouridou, I. A. Christidi, A. Christov, D. Chromek-Burckhart, M. L. Chu, J. Chudoba, G. Ciapetti, A. K. Ciftci, R. Ciftci, D. Cinca, V. Cindro, C. Ciocca, A. Ciocio, M. Cirilli, P. Cirkovic, Z. H. Citron, M. Citterio, M. Ciubancan, A. Clark, P. J. Clark, R. N. Clarke, W. Cleland, J. C. Clemen, B. Clement, C. Clement, Y. Coadou, M. Cobal, A. Coccaro, J. Cochran, J. G. Cogan, J. Coggeshall, E. Cognera, J. Cola, S. Cole, A. P. Colijn, N. J. Collin, C. Collins-Tooth, J. Collot, T. Colombo, G. Colon, P. Conde Muiño, E. Coniaviti, M. C. Conidi, S. M. Consonni, V. Consorti, S. Constantinescu, C. Conta, G. Conti, F. Conventi, M. Cooke, B. D. Cooper, A. M. Cooper-Sarkar, K. Copic, T. Cornelissen, M. Corradi, F. Corriveau, A. Cortes-Gonzalez, G. Cortiana, G. Costa, M. J. Costa, D. Costanzo, D. Côté, L. Courneyea, G. Cowan, C. Cowden, B. E. Cox, K. Cranmer, F. Crescioli, M. Cristinziani, G. Crosetti, S. Crépé-Renaudin, C.-M. Cuciuc, C. Cuenca Almenar, T. Cuhadar Donszelmann, M. Curatolo, C. J. Curti, C. Cuthbert, P. Cwetanski, H. Czirr, P. Czodrowski, Z. Czyczula, S. D’Auria, M. D’Onofrio, A. D’Orazio, M. J. Da Cunha Sargedas De Sousa, C. Via, W. Dabrowski, A. Dafinca, T. Dai, C. Dallapiccola, M. Dam, M. Dameri, D. S. Damiani, H. O. Danielsson, V. Dao, G. Darbo, G. L. Darlea, J. A. Dassoula, W. Davey, T. Davidek, N. Davidson, R. Davidson, E. Davie, M. Davie, O. Davignon, A. R. Davison, Y. Davygora, E. Dawe, I. Dawson, R. K. Daya-Ishmukhametova, K. De, R. Asmundi, S. Castro, S. Cecco, J. Graat, N. Groot, P. Jong, C. Taille, H. Torre, F. Lorenzi, L. Mora, L. Nooij, D. Pedi, A. Salvo, U. Sancti, A. Santo, J. B. De Vivie De Regie, G. Zorzi, W. J. Dearnaley, R. Debbe, C. Debenedetti, B. Dechenaux, D. V. Dedovich, J. Degenhardt, C. Papa, J. Peso, T. Prete, T. Delemontex, M. Deliyergiyev, A. Dell’Acqua, L. Dell’Asta, M. Della Pietra, D. Volpe, M. Delmastro, P. A. Delsart, C. Deluca, S. Demer, M. Demichev, B. Demirkoz, J. Deng, S. P. Denisov, D. Derendarz, J. E. Derkaoui, F. Derue, P. Dervan, K. Desch, E. Devetak, P. O. Deviveiro, A. Dewhurst, B. DeWilde, S. Dhaliwal, R. Dhullipudi, A. Ciaccio, L. Ciaccio, A. Girolamo, B. Girolamo, S. Luise, A. Mattia, B. Micco, R. Nardo, A. Simone, R. Sipio, M. A. Diaz, E. B. Diehl, J. Dietrich, T. A. Dietzsch, S. Diglio, K. Dindar Yagci, J. Dingfelder, F. Dinut, C. Dionisi, P. Dita, S. Dita, F. Dittu, F. Djama, T. Djobava, M. A. B. Vale, A. Do Valle Weman, T. K. O. Doan, M. Dobb, R. Dobinson, D. Dobo, E. Dobson, J. Dodd, C. Doglioni, T. Doherty, Y. Doi, J. Dolejsi, I. Dolenc, Z. Dolezal, B. A. Dolgoshein, T. Dohmae, M. Donadelli, J. Donini, J. Dopke, A. Doria, A. Dos Anjo, A. Dotti, M. T. Dova, A. D. Doxiadi, A. T. Doyle, N. Dressnandt, M. Dri, J. Dubbert, S. Dube, E. Duchovni, G. Duckeck, D. Duda, A. Dudarev, F. Dudziak, M. Dührssen, I. P. Duerdoth, L. Duflot, M-A. Dufour, L. Duguid, M. Dunford, H. Duran Yildiz, R. Duxfield, M. Dwuznik, F. Dydak, M. Düren, W. L. Ebenstein, J. Ebke, S. Eckweiler, K. Edmond, W. Edson, C. A. Edward, N. C. Edward, W. Ehrenfeld, T. Eifert, G. Eigen, K. Einsweiler, E. Eisenhandler, T. Ekelof, M. Kacimi, M. Ellert, S. Elle, F. Ellinghau, K. Elli, N. Elli, J. Elmsheuser, M. Elsing, D. Emeliyanov, R. Engelmann, A. Engl, B. Epp, J. Erdmann, A. Ereditato, D. Eriksson, J. Ernst, M. Ernst, J. Ernwein, D. Errede, S. Errede, E. Ertel, M. Escalier, H. Esch, C. Escobar, X. Espinal Curull, B. Esposito, F. Etienne, A. I. Etienvre, E. Etzion, D. Evangelakou, H. Evan, L. Fabbri, C. Fabre, R. M. Fakhrutdinov, S. Falciano, Y. Fang, M. Fanti, A. Farbin, A. Farilla, J. Farley, T. Farooque, S. Farrell, S. M. Farrington, P. Farthouat, F. Fassi, P. Fassnacht, D. Fassoulioti, B. Fatholahzadeh, A. Favareto, L. Fayard, S. Fazio, R. Febbraro, P. Federic, O. L. Fedin, W. Fedorko, M. Fehling-Kaschek, L. Feligioni, D. Fellmann, C. Feng, E. J. Feng, A. B. Fenyuk, J. Ferencei, W. Fernando, S. Ferrag, J. Ferrando, V. Ferrara, A. Ferrari, P. Ferrari, R. Ferrari, D. E. Ferreira de Lima, A. Ferrer, D. Ferrere, C. Ferretti, A. Ferretto Parodi, M. Fiascari, F. Fiedler, A. Filipčič, F. Filthaut, M. Fincke-Keeler, M. C. N. Fiolhai, L. Fiorini, A. Firan, G. Fischer, M. J. Fisher, M. Flechl, I. Fleck, J. Fleckner, P. Fleischmann, S. Fleischmann, T. Flick, A. Floderu, L. R. Flores Castillo, M. J. Flowerdew, T. Fonseca Martin, A. Formica, A. Forti, D. Fortin, D. Fournier, A. J. Fowler, H. Fox, P. Francavilla, M. Franchini, S. Franchino, D. Franci, T. Frank, S. Franz, M. Fraternali, S. Fratina, S. T. French, C. Friedrich, F. Friedrich, R. Froeschl, D. Froidevaux, J. A. Frost, C. Fukunaga, E. Fullana Torregrosa, B. G. Fulsom, J. Fuster, C. Gabaldon, O. Gabizon, T. Gadfort, S. Gadomski, G. Gagliardi, P. Gagnon, C. Galea, B. Galhardo, E. J. 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Rurikova, N. A. Rusakovich, J. P. Rutherfoord, C. Ruwiedel, P. Ruzicka, Y. F. Ryabov, M. Rybar, G. Rybkin, N. C. Ryder, A. F. Saavedra, I. Sadeh, H. F-W. Sadrozinski, R. Sadykov, F. Safai Tehrani, H. Sakamoto, G. Salamanna, A. Salamon, M. Saleem, D. Salek, D. Salihagic, A. Salnikov, J. Salt, B. M. Salvachua Ferrando, D. Salvatore, F. Salvatore, A. Salvucci, A. Salzburger, D. Sampsonidi, B. H. Samset, A. Sanchez, V. Sanchez Martinez, H. Sandaker, H. G. Sander, M. P. Sander, M. Sandhoff, T. Sandoval, C. Sandoval, R. Sandstroem, D. P. C. Sankey, A. Sansoni, C. Santamarina Rio, C. Santoni, R. Santonico, H. Santo, J. G. Saraiva, T. Sarangi, E. Sarkisyan-Grinbaum, F. Sarri, G. Sartisohn, O. Sasaki, Y. Sasaki, N. Sasao, I. Satsounkevitch, G. Sauvage, E. Sauvan, J. B. Sauvan, P. Savard, V. Savinov, D. O. Savu, L. Sawyer, D. H. Saxon, J. Saxon, C. Sbarra, A. Sbrizzi, D. A. Scannicchio, M. Scarcella, J. Schaarschmidt, P. Schacht, D. Schaefer, U. Schäfer, S. Schaepe, S. Schaetzel, A. C. Schaffer, D. Schaile, R. D. Schamberger, A. G. Schamov, V. Scharf, V. A. Schegelsky, D. Scheirich, M. Schernau, M. I. Scherzer, C. Schiavi, J. Schieck, M. Schioppa, S. Schlenker, E. Schmidt, K. Schmieden, C. Schmitt, S. Schmitt, M. Schmitz, B. Schneider, U. Schnoor, A. Schoening, A. L. S. Schorlemmer, M. Schott, D. Schouten, J. Schovancova, M. Schram, C. Schroeder, N. Schroer, M. J. Schulten, J. Schulte, H.-C. Schultz-Coulon, H. Schulz, M. Schumacher, B. A. Schumm, Ph. Schune, C. Schwanenberger, A. Schwartzman, Ph. Schwegler, Ph. Schwemling, R. Schwienhorst, R. Schwierz, J. Schwindling, T. Schwindt, M. Schwoerer, G. Sciolla, W. G. Scott, J. Searcy, G. Sedov, E. Sedykh, S. C. Seidel, A. Seiden, F. Seifert, J. M. Seixa, G. Sekhniaidze, S. J. Sekula, K. E. Selbach, D. M. Seliverstov, B. Sellden, G. Seller, M. Seman, N. Semprini-Cesari, C. Serfon, L. Serin, L. Serkin, R. Seuster, H. Severini, A. Sfyrla, E. Shabalina, M. Shamim, L. Y. Shan, J. T. Shank, Q. T. Shao, M. Shapiro, P. B. Shatalov, K. Shaw, D. Sherman, P. Sherwood, A. Shibata, S. Shimizu, M. Shimojima, T. Shin, M. Shiyakova, A. Shmeleva, M. J. Shochet, D. Short, S. Shrestha, E. Shulga, M. A. Shupe, P. Sicho, A. Sidoti, F. Siegert, Dj. Sijacki, O. Silbert, J. Silva, Y. Silver, D. Silverstein, S. B. Silverstein, V. Simak, O. Simard, Lj. Simic, S. Simion, E. Simioni, B. Simmon, R. Simoniello, M. Simonyan, P. Sinervo, N. B. Sinev, V. Sipica, G. Siragusa, A. Sircar, A. N. Sisakyan, S. Yu. Sivoklokov, J. Sjölin, T. B. Sjursen, L. A. Skinnari, H. P. Skottowe, K. Skovpen, P. Skubic, M. Slater, T. Slavicek, K. Sliwa, V. Smakhtin, B. H. Smart, L. Smestad, S. Yu. Smirnov, Y. Smirnov, L. N. Smirnova, O. Smirnova, B. C. Smith, D. Smith, K. M. Smith, M. Smizanska, K. Smolek, A. A. Snesarev, S. W. Snow, J. Snow, S. Snyder, R. Sobie, J. Sodomka, A. Soffer, C. A. Solan, M. Solar, J. Solc, E. Yu. Soldatov, U. Soldevila, E. Solfaroli Camillocci, A. A. Solodkov, O. V. Solovyanov, V. Solovyev, N. Soni, V. Sopko, B. Sopko, M. Sosebee, R. Soualah, A. Soukharev, S. Spagnolo, F. Spanò, R. Spighi, G. Spigo, R. Spiwok, M. Spousta, T. Spreitzer, B. Spurlock, R. D. St. Deni, J. Stahlman, R. Stamen, E. Stanecka, R. W. Stanek, C. Stanescu, M. Stanescu-Bellu, M. M. Stanitzki, S. Stapne, E. A. Starchenko, J. Stark, P. Staroba, P. Starovoitov, R. Staszewski, A. Staude, P. Stavina, G. Steele, P. Steinbach, P. Steinberg, I. Stekl, B. Stelzer, H. J. Stelzer, O. Stelzer-Chilton, H. Stenzel, S. Stern, G. A. Stewart, J. A. Stilling, M. C. Stockton, K. Stoerig, G. Stoicea, S. Stonjek, P. Strachota, A. R. Stradling, A. Straessner, J. Strandberg, S. Strandberg, A. Strandlie, M. Strang, E. Strau, M. Strau, P. Strizenec, R. Ströhmer, D. M. Strom, J. A. Strong, R. Stroynowski, J. Strube, B. Stugu, I. Stumer, J. Stupak, P. Sturm, N. A. Style, D. A. Soh, D. Su, HS. Subramania, A. Succurro, Y. Sugaya, C. Suhr, M. Suk, V. V. Sulin, S. Sultansoy, T. Sumida, X. Sun, J. E. Sundermann, K. Suruliz, G. Susinno, M. R. Sutton, Y. Suzuki, M. Svato, S. Swedish, I. Sykora, T. Sykora, J. Sánchez, D. Ta, K. Tackmann, A. Taffard, R. Tafirout, N. Taiblum, Y. Takahashi, H. Takai, R. Takashima, H. Takeda, T. Takeshita, Y. Takubo, M. Talby, A. Talyshev, M. C. Tamsett, K. G. Tan, J. Tanaka, R. Tanaka, S. Tanaka, A. J. Tanasijczuk, K. Tani, N. Tannoury, S. Tapprogge, D. Tardif, S. Tarem, F. Tarrade, G. F. Tartarelli, P. Ta, M. Tasevsky, E. Tassi, M. Tatarkhanov, Y. Tayalati, C. Taylor, F. E. Taylor, G. N. Taylor, W. Taylor, M. Teinturier, F. A. Teischinger, M. Teixeira Dias Castanheira, P. Teixeira-Dia, K. K. Temming, H. Kate, P. K. Teng, S. Terada, K. Terashi, J. Terron, M. Testa, R. J. Teuscher, J. Therhaag, T. Theveneaux-Pelzer, S. Thoma, J. P. Thoma, E. N. Thompson, P. D. Thompson, A. S. Thompson, L. A. Thomsen, E. Thomson, M. Thomson, W. M. Thong, R. P. Thun, F. Tian, M. J. Tibbett, T. Tic, V. O. Tikhomirov, Y. A. Tikhonov, S. Timoshenko, P. Tipton, S. Tisserant, T. Todorov, S. Todorova-Nova, B. Toggerson, J. Tojo, S. Tokár, K. Tokushuku, K. Tollefson, M. Tomoto, L. Tompkin, K. Tom, A. Tonoyan, C. Topfel, N. D. Topilin, I. Torchiani, E. Torrence, E. Torró Pastor, J. Toth, F. Touchard, D. R. Tovey, T. Trefzger, L. Tremblet, A. Tricoli, I. M. Trigger, S. Trincaz-Duvoid, M. F. Tripiana, N. Triplett, W. Trischuk, B. Trocmé, C. Troncon, M. Trottier-McDonald, M. Trzebinski, A. Trzupek, C. Tsaroucha, J. C-L. Tseng, M. Tsiakiri, P. V. Tsiareshka, D. Tsionou, G. Tsipoliti, S. Tsiskaridze, V. Tsiskaridze, E. G. Tskhadadze, I. I. Tsukerman, V. Tsulaia, J.-W. Tsung, S. Tsuno, D. Tsybychev, A. Tua, A. Tudorache, V. Tudorache, J. M. Tuggle, M. Turala, D. Turecek, I. Turk Cakir, E. Turlay, R. Turra, P. M. Tut, A. Tykhonov, M. Tylmad, M. Tyndel, G. Tzanako, K. Uchida, I. Ueda, R. Ueno, M. Ugland, M. Uhlenbrock, M. Uhrmacher, F. Ukegawa, G. Unal, A. Undru, G. Unel, Y. Unno, D. Urbaniec, G. Usai, M. Uslenghi, L. Vacavant, V. Vacek, B. Vachon, S. Vahsen, J. Valenta, S. Valentinetti, A. Valero, S. Valkar, E. Valladolid Gallego, S. Vallecorsa, J. A. Valls Ferrer, R. Berg, P. C. Deijl, R. Geer, H. Graaf, R. Leeuw, E. Poel, D. Ster, N. Eldik, P. Gemmeren, I. Vulpen, M. Vanadia, W. Vandelli, A. Vaniachine, P. Vankov, F. Vannucci, R. Vari, E. W. Varne, T. Varol, D. Varoucha, A. Vartapetian, K. E. Varvell, V. I. Vassilakopoulo, F. Vazeille, T. Vazquez Schroeder, G. Vegni, J. J. Veillet, F. Veloso, R. Vene, S. Veneziano, A. Ventura, D. Ventura, M. Venturi, N. Venturi, V. Vercesi, M. Verducci, W. Verkerke, J. C. Vermeulen, A. Vest, M. C. Vetterli, I. Vichou, T. Vickey, O. E. Vickey Boeriu, G. H. A. Viehhauser, S. Viel, M. Villa, M. Villaplana Perez, E. Vilucchi, M. G. Vincter, E. Vinek, V. B. Vinogradov, M. Virchaux, J. Virzi, O. Vitell, M. Viti, I. Vivarelli, F. Vives Vaque, S. Vlacho, D. Vladoiu, M. Vlasak, A. Vogel, P. Vokac, G. Volpi, M. Volpi, G. Volpini, H. Schmitt, H. Radziewski, E. Toerne, V. Vorobel, V. Vorwerk, M. Vo, R. Vo, T. T. Vo, J. H. Vossebeld, N. Vranje, M. Vranjes Milosavljevic, V. Vrba, M. Vreeswijk, T. Vu Anh, R. Vuillermet, I. Vukotic, W. Wagner, P. Wagner, H. Wahlen, S. Wahrmund, J. Wakabayashi, S. Walch, J. Walder, R. Walker, W. Walkowiak, R. Wall, P. Waller, B. Walsh, C. Wang, H. Wang, J. Wang, R. Wang, S. M. Wang, T. Wang, A. Warburton, C. P. Ward, M. Warsinsky, A. Washbrook, C. Wasicki, I. Watanabe, P. M. Watkin, A. T. Watson, I. J. Watson, M. F. Watson, G. Watt, S. Watt, A. T. Waugh, B. M. Waugh, M. S. Weber, P. Weber, A. R. Weidberg, P. Weigell, J. Weingarten, C. Weiser, P. S. Well, T. Wenau, D. Wendland, Z. Weng, T. Wengler, S. Wenig, N. Werme, M. Werner, P. Werner, M. Werth, M. Wessel, J. Wetter, C. Weydert, K. Whalen, S. J. Wheeler-Elli, A. White, M. J. White, S. White, S. R. Whitehead, D. Whiteson, D. Whittington, F. Wicek, D. Wicke, F. J. Wicken, W. Wiedenmann, M. Wieler, P. Wienemann, C. Wiglesworth, L. A. M. Wiik-Fuch, P. A. Wijeratne, A. Wildauer, M. A. Wildt, I. Wilhelm, H. G. Wilken, J. Z. Will, E. William, H. H. William, W. Willi, S. Willocq, J. A. Wilson, M. G. Wilson, A. Wilson, I. Wingerter-Seez, S. Winkelmann, F. Winklmeier, M. Wittgen, S. J. Wollstadt, M. W. Wolter, H. Wolter, W. C. Wong, G. Wooden, B. K. Wosiek, J. Wotschack, M. J. Woudstra, K. W. Wozniak, K. Wraight, M. Wright, B. Wrona, S. L. Wu, X. Wu, Y. Wu, E. Wulf, B. M. Wynne, S. Xella, M. Xiao, S. Xie, C. Xu, D. Xu, B. Yabsley, S. Yacoob, M. Yamada, H. Yamaguchi, A. Yamamoto, K. Yamamoto, S. Yamamoto, T. Yamamura, T. Yamanaka, J. Yamaoka, T. Yamazaki, Y. Yamazaki, Z. Yan, H. Yang, U. K. Yang, Y. Yang, Z. Yang, S. Yanush, L. Yao, Y. Yao, Y. Yasu, G. V. Ybeles Smit, J. Ye, S. Ye, M. Yilmaz, R. Yoosoofmiya, K. Yorita, R. Yoshida, C. Young, C. J. Young, S. Youssef, D. Yu, J. Yu, L. Yuan, A. Yurkewicz, M. Byszewski, B. Zabinski, R. Zaidan, A. M. Zaitsev, Z. Zajacova, L. Zanello, D. Zanzi, A. Zaytsev, C. Zeitnitz, M. Zeman, A. Zemla, C. Zendler, O. Zenin, T. Ženiš, Z. Zinono, S. Zenz, D. Zerwa, G. Zevi Porta, Z. Zhan, D. Zhang, H. Zhang, J. Zhang, X. Zhang, Z. Zhang, L. Zhao, T. Zhao, Z. Zhao, A. Zhemchugov, J. Zhong, B. Zhou, N. Zhou, Y. Zhou, C. G. Zhu, H. Zhu, J. Zhu, Y. Zhu, X. Zhuang, V. Zhuravlov, D. Zieminska, N. I. Zimin, R. Zimmermann, S. Zimmermann, M. Ziolkowski, R. Zitoun, L. Živković, V. V. Zmouchko, G. Zobernig, A. Zoccoli, M. Nedden, V. Zutshi, L. Zwalinski, Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Współautorami artykułu są członkowie ATLAS Collaboration w liczbie 2908, Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC)-AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universidade do Minho, and ATLAS Collaboration (ukupan broj autora: 2911)
Subjects: Particle physics, Nuclear and High Energy Physics, Ciências Naturais::Ciências Físicas, Physics beyond the Standard Model, Ciências Físicas [Ciências Naturais], FOS: Physical sciences, 7. Clean energy, 01 natural sciences, Electric charge, Standard Model, Luminosity, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), Atlas (anatomy), 0103 physical sciences, medicine, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Invariant mass, ddc:530, High Energy Physics, 010306 general physics, Physics, LEFT-RIGHT SYMMETRY, Large Hadron Collider, Science & Technology, Hadron-Hadron Scattering, 010308 nuclear & particles physics, Settore FIS/01 - Fisica Sperimentale, High Energy Physics::Phenomenology, ATLAS, medicine.anatomical_structure, HADRON-HADRON COLLISIONS, Experimental High Energy Physics, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, High Energy Physics::Experiment, LHC, CHARGED HIGGS BOSONS, Particle Physics - Experiment, Lepton, NUMBER-VIOLATING PROCESSES
Abstract: An inclusive search for anomalous production of two prompt, isolated leptons with the same electric charge is presented. The search is performed in a data sample corresponding to 4.7 fb(-1) of integrated luminosity collected in 2011 at root s = 7TeV with the ATLAS detector at the LHC. Pairs of leptons (e(+/-)e(+/-), e(+/-)mu(+/-), and mu(+/-)mu(+/-)) with large transverse momentum are selected, and the dilepton invariant mass distribution is examined for any deviation from the Standard Model expectation. No excess is found, and upper limits on the production cross section of like-sign lepton pairs from physics processes beyond the Standard Model are placed as a function of the dilepton invariant mass within a fiducial region close to the experimental selection criteria. The 95% confidence level upper limits on the cross section of anomalous e(+/-)e(+/-), e(+/-)mu(+/-), or mu(+/-)mu(+/-) production range between 1.7 fb and 64 fb depending on the dilepton mass and flavour combination., We acknowledge the support of ANPCyT, Argentina; YerPhI, Armenia; ARC, Australia; BMWF and FWF, Austria; ANAS, Azerbaijan; SSTC, Belarus; CNPq and FAPESP, Brazil; NSERC, NRC and CFI, Canada; CERN; CONICYT, Chile; CAS, MOST and NSFC, China; COLCIENCIAS, Colombia; MSMT CR, MPO CR and VSC CR, Czech Republic; DNRF, DNSRC and Lundbeck Foundation, Denmark; EPLANET and ERC, European Union; IN2P3-CNRS, CEA-DSM/IRFU, France; GNSF, Georgia; BMBF, DFG, HGF, MPG and AvH Foundation, Germany; GSRT, Greece; ISF, MINERVA, GIF, DIP and Benoziyo Center, Israel; INFN, Italy; MEXT and JSPS, Japan; CNRST, Morocco; FOM and NWO, Netherlands; BRF and RCN, Norway; MNiSW, Poland; GRICES and FCT, Portugal; MERYS (MECTS), Romania; MES of Russia and ROSATOM, Russian Federation; JINR; MSTD, Serbia; MSSR, Slovakia; ARRS and MVZT, Slovenia; DST/NRF, South Africa; MICINN, Spain; SRC and Wallenberg Foundation, Sweden; SER, SNSF and Cantons of Bern and Geneva, Switzerland; NSC, Taiwan; TAEK, Turkey; STFC, the Royal Society and Leverhulme Trust, United Kingdom; DOE and NSF, United States of America., info:eu-repo/semantics/publishedVersion
Published: 2012

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23 results on '"Nicholas L. Rodd"'

1. Dark matter spectra from the electroweak to the Planck scale

2. Deep Search for Decaying Dark Matter with XMM-Newton Blank-Sky Observations

3. Prospects for detecting heavy WIMP dark matter with the Cherenkov Telescope Array: The Wino and Higgsino

4. Foreground mismodeling and the point source explanation of the Fermi Galactic Center excess

5. Characterizing the nature of the unresolved point sources in the Galactic Center: An assessment of systematic uncertainties

6. Indirect searches for dark matter bound state formation and level transitions

7. Response to a comment on Dessert et al. 'The dark matter interpretation of the 3.5 keV line is inconsistent with blank-sky observations'

8. Comment on 'Characterizing the population of pulsars in the Galactic bulge with the Fermi large area telescope' [arXiv:1705.00009v1]

9. Precision Photon Spectra for Wino Annihilation

10. Hunting for Heavy Winos in the Galactic Center

11. Revealing the dark matter halo with axion direct detection

12. What the Milky Way’s dwarfs tell us about the Galactic Center extended gamma-ray excess

13. A Search for Dark Matter in the Galactic Halo with HAWC

14. Disentangling heavy flavor at colliders

15. Mapping Extragalactic Dark Matter Annihilation with Galaxy Surveys: A Systematic Study of Stacked Group Searches

16. A Search for Dark Matter Annihilation in Galaxy Groups

17. γ-ray Constraints on Decaying Dark Matter and Implications for IceCube

18. The One-Loop Correction to Heavy Dark Matter Annihilation

19. Model-independent indirect detection constraints on hidden sector dark matter

20. The High-Energy Tail of the Galactic Center Gamma-Ray Excess

21. NPTFit: A Code Package for Non-Poissonian Template Fitting

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

23. Search for anomalous production of prompt like-sign lepton pairs at sqrt(s) = 7 TeV with the ATLAS detector

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