A Python Toolkit for Cosmology, Large-Scale Structure, and Dark Matter Halos
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Anti-Helium from Dark Matter Annihilations Arxiv:1401.4017V3 [Hep-Ph] 24 Aug 2016
SACLAY{T14/003 Anti-helium from Dark Matter annihilations Marco Cirelli a, Nicolao Fornengo b;c, Marco Taoso a, Andrea Vittino a;b;c a Institut de Physique Th´eorique, CNRS, URA 2306 & CEA/Saclay, F-91191 Gif-sur-Yvette, France b Department of Physics, University of Torino, via P. Giuria 1, I-10125 Torino, Italy c INFN - Istituto Nazionale di Fisica Nucleare, Sezione di Torino, via P. Giuria 1, I-10125 Torino, Italy Abstract Galactic Dark Matter (DM) annihilations can produce cosmic-ray anti-nuclei via the nuclear coalescence of the anti-protons and anti-neutrons originated directly from the annihilation process. Since anti-deuterons have been shown to offer a distinctive DM signal, with potentially good prospects for detection in large portions of the DM-particle parameter space, we explore here the production of heavier anti-nuclei, specifically anti-helium. Even more than for anti-deuterons, the DM-produced anti-He flux can be mostly prominent over the astrophysical anti-He background at low kinetic energies, typically below 3-5 GeV/n. However, the larger number of anti-nucleons involved in the formation process makes the anti-He flux extremely small. We therefore explore, for a few DM benchmark cases, whether the yield is sufficient to allow for anti-He detection in current-generation experiments, such as Ams-02. We account for the uncertainties due to the propagation in the Galaxy and to the uncertain details of the coalescence process, and we consider the constraints already imposed by anti-proton searches. We find that only for very optimistic configurations might it be possible to achieve detection with current generation detectors. -
Letter of Interest Cosmic Probes of Ultra-Light Axion Dark Matter
Snowmass2021 - Letter of Interest Cosmic probes of ultra-light axion dark matter Thematic Areas: (check all that apply /) (CF1) Dark Matter: Particle Like (CF2) Dark Matter: Wavelike (CF3) Dark Matter: Cosmic Probes (CF4) Dark Energy and Cosmic Acceleration: The Modern Universe (CF5) Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before (CF6) Dark Energy and Cosmic Acceleration: Complementarity of Probes and New Facilities (CF7) Cosmic Probes of Fundamental Physics (TF09) Astro-particle physics and cosmology Contact Information: Name (Institution) [email]: Keir K. Rogers (Oskar Klein Centre for Cosmoparticle Physics, Stockholm University; Dunlap Institute, University of Toronto) [ [email protected]] Authors: Simeon Bird (UC Riverside), Simon Birrer (Stanford University), Djuna Croon (TRIUMF), Alex Drlica-Wagner (Fermilab, University of Chicago), Jeff A. Dror (UC Berkeley, Lawrence Berkeley National Laboratory), Daniel Grin (Haverford College), David J. E. Marsh (Georg-August University Goettingen), Philip Mocz (Princeton), Ethan Nadler (Stanford), Chanda Prescod-Weinstein (University of New Hamp- shire), Keir K. Rogers (Oskar Klein Centre for Cosmoparticle Physics, Stockholm University; Dunlap Insti- tute, University of Toronto), Katelin Schutz (MIT), Neelima Sehgal (Stony Brook University), Yu-Dai Tsai (Fermilab), Tien-Tien Yu (University of Oregon), Yimin Zhong (University of Chicago). Abstract: Ultra-light axions are a compelling dark matter candidate, motivated by the string axiverse, the strong CP problem in QCD, and possible tensions in the CDM model. They are hard to probe experimentally, and so cosmological/astrophysical observations are very sensitive to the distinctive gravitational phenomena of ULA dark matter. There is the prospect of probing fifteen orders of magnitude in mass, often down to sub-percent contributions to the DM in the next ten to twenty years. -
Arxiv:1306.3244V2 [Astro-Ph.CO] 4 Feb 2014
The Scientific Reach of Multi-Ton Scale Dark Matter Direct Detection Experiments Jayden L. Newsteada, Thomas D. Jacquesa, Lawrence M. Kraussa;b, James B. Dentc, and Francesc Ferrerd a Department of Physics and School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA, b Research School of Astronomy and Astrophysics, Mt. Stromlo Observatory, Australian National University, Canberra 2614, Australia, c Department of Physics, University of Louisiana at Lafayette, Lafayette, LA 70504, USA, and d Physics Department and McDonnell Center for the Space Sciences, Washington University, St Louis, MO 63130, USA (Dated: November 6, 2018) Abstract The next generation of large scale WIMP direct detection experiments have the potential to go beyond the discovery phase and reveal detailed information about both the particle physics and astrophysics of dark matter. We report here on early results arising from the development of a detailed numerical code modeling the proposed DARWIN detector, involving both liquid argon and xenon targets. We incorporate realistic detector physics, particle physics and astrophysical uncertainties and demonstrate to what extent two targets with similar sensitivities can remove various degeneracies and allow a determination of dark matter cross sections and masses while also probing rough aspects of the dark matter phase space distribution. We find that, even assuming arXiv:1306.3244v2 [astro-ph.CO] 4 Feb 2014 dominance of spin-independent scattering, multi-ton scale experiments still have degeneracies that depend sensitively on the dark matter mass, and on the possibility of isospin violation and inelas- ticity in interactions. We find that these experiments are best able to discriminate dark matter properties for dark matter masses less than around 200 GeV. -
Arxiv:2107.12380V1 [Astro-Ph.CO] 26 Jul 2021
UTTG-04-2021 Observational constraints on dark matter scattering with electrons David Nguyen,1 Dimple Sarnaaik,1 Kimberly K. Boddy,2 Ethan O. Nadler,3, 4, 1 and Vera Gluscevic1 1Department of Physics & Astronomy, University of Southern California, Los Angeles, CA, 90007, USA 2Department of Physics, University of Texas at Austin, Austin, TX, 78712, USA 3Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, Stanford, CA 94305, USA 4Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA We present new observational constraints on the elastic scattering of dark matter with electrons for dark matter masses between 10 keV and 1 TeV. We consider scenarios in which the momentum- transfer cross section has a power-law dependence on the relative particle velocity, with a power-law index n 2 {−4; −2; 0; 2; 4; 6g. We search for evidence of dark matter scattering through its sup- pression of structure formation. Measurements of the cosmic microwave background temperature, polarization, and lensing anisotropy from Planck 2018 data and of the Milky Way satellite abundance measurements from the Dark Energy Survey and Pan-STARRS1 show no evidence of interactions. We use these data sets to obtain upper limits on the scattering cross section, comparing them with exclusion bounds from electronic recoil data in direct detection experiments. Our results provide the strongest bounds available for dark matter{electron scattering derived from the distribution of matter in the Universe, extending down to sub-MeV dark matter masses, where current direct detection experiments lose sensitivity. I. INTRODUCTION effective field theory operators [24{26]; in a cosmologi- cal context, these operators produce momentum-transfer Cosmological observations are a powerful tool for cross sections with a power-law dependence on the rela- studying the fundamental particle properties of dark tive velocity between scattering DM particles and nucle- matter (DM). -
The Boundary of Galaxy Clusters and Its Implications on SFR Quenching
The splashback boundary of galaxy clusters in mass and light and its implications for galaxy evolution T.-H. Shin, Ph.D. candidate at UPenn Collaborators: S. Adhikari, E. J. Baxter, C. Chang, B. Jain, N. Battaglia et al. (DES collaboration) (SPT collaboration) (ACT collaboration) https://arxiv.org/abs/1811.06081 (accepted to MNRAS); 2019 paper in preparation Based on ~400 public cluster sample from ACT+SPT Ongoing analysis of 1000+ SZ-selected clusters from DES+ACT+SPT Background Mass and boundary of dark matter halos However, MΔ and RΔ are subject to pseudo-evolution due to the decrease in the ρ ρ reference density ( c or m) Haloes continuously accrete matter; there is no radius within which the matter is fully virialized ⇒ where is the physical boundary of the halos? Credit: Andrey Kravtsov Cosmology with galaxy clusters Galaxy clusters live in the high-mass tail of the halo mass function ⇒ very sensitive to the growth of the structure Ω σ ( m and 8) Thus, it is important to accurately define/measure Tinker et al. (2008) the mass of the cluster Preliminary work by Diemer et al. illuminates that the mass function becomes more universal against redshift when we use so-called “splashback radius” as the physical boundary of the dark matter halos Background ● Galaxies fall into the cluster potential, escaping from the Hubble flow ● They form a sharp “physical” boundary around their first apocenters after the infall, which we call “splashback radius” Background ● A simple spherical collapse model can predict the existence of the splashback feature (Gunn & Gott 1972, Fillmore & Goldreich 1984, Bertschinger 1985, Adhikari et al. -
Dark Matter 18Th May 2021.Pdf
Searches for Dark Matter Seminar presentation 18th May 2021 Iida Kostamo 1/20 Contents • Background and history - How did we end up with the dark matter hypothesis? • Hot and cold dark matter - Candidates for cold dark matter • The halo density profile • Simulations (Millennium and Bolshoi) • Summary Seminar presentation 18th May 2021 Iida Kostamo 2/20 Background • The total mass-energy density of the universe (approximately): 1. 5% ordinary baryonic matter 2. 25% dark matter 3. 70% dark energy • Originally dark matter was referred to as "the missing mass" - 1930's: Fritz Zwicky did research on galaxy clusters • ...The problem is the missing light, not the missing mass, hence "dark matter" Seminar presentation 18th May 2021 Iida Kostamo 3/20 The rotation curves of galaxies • The rotation curve describes how the rotation velocity of an object depends on the distance from the center of the galaxy • Assumption: Kepler's III law, i.e. the rotation velocities decrease with increasing distance • In the 1970's Vera Rubin and her colleagues did research on the rotation curves of various spiral galaxies Seminar presentation 18th May 2021 Iida Kostamo 4/20 The rotation curves of galaxies • H = Hubble constant • The rotation curves become flat when the radius is large enough • The same result for all galaxies: the rotation curves are not descending → There must be non-luminous mass in galaxies Seminar presentation 18th May 2021 Iida Kostamo 5/20 MACHOs (Massive Astrophysical Compact Halo Object) • Objects that emit extremely little or no light → -
Probing the Nature of Dark Matter in the Universe
PROBING THE NATURE OF DARK MATTER IN THE UNIVERSE A Thesis Submitted For The Degree Of Doctor Of Philosophy In The Faculty Of Science by Abir Sarkar Under the supervision of Prof. Shiv K Sethi Raman Research Institute Joint Astronomy Programme (JAP) Department of Physics Indian Institute of Science BANGALORE - 560012 JULY, 2017 c Abir Sarkar JULY 2017 All rights reserved Declaration I, Abir Sarkar, hereby declare that the work presented in this doctoral thesis titled `Probing The Nature of Dark Matter in the Universe', is entirely original. This work has been carried out by me under the supervision of Prof. Shiv K Sethi at the Department of Astronomy and Astrophysics, Raman Research Institute under the Joint Astronomy Programme (JAP) of the Department of Physics, Indian Institute of Science. I further declare that this has not formed the basis for the award of any degree, diploma, membership, associateship or similar title of any university or institution. Department of Physics Abir Sarkar Indian Institute of Science Date : Bangalore, 560012 INDIA TO My family, without whose support this work could not be done Acknowledgements First and foremost I would like to thank my supervisor Prof. Shiv K Sethi in Raman Research Institute(RRI). He has always spent substantial time whenever I have needed for any academic discussions. I am thankful for his inspirations and ideas to make my Ph.D. experience produc- tive and stimulating. I am also grateful to our collaborator Prof. Subinoy Das of Indian Institute of Astrophysics, Bangalore, India. I am thankful to him for his insightful comments not only for our publica- tions but also for the thesis. -
Astrophysical Uncertainties of Direct Dark Matter Searches
Technische Universit¨atM¨unchen Astrophysical uncertainties of direct dark matter searches Dissertation by Andreas G¨unter Rappelt Physik Department, T30d & Collaborative Research Center SFB 1258 “Neutrinos and Dark Matter in Astro- and Particlephysics” Technische Universit¨atM¨unchen Physik Department T30d Astrophysical uncertainties of direct dark matter searches Andreas G¨unter Rappelt Vollst¨andigerAbdruck der von der Fakult¨atf¨urPhysik der Technischen Universit¨at M¨unchen zur Erlangung des akademischen Grades eines Doktors der Naturwissenschaften genehmigten Dissertation. Vorsitzender: Prof. Dr. Lothar Oberauer Pr¨uferder Dissertation: 1. Prof. Dr. Alejandro Ibarra 2. Prof. Dr. Bj¨ornGarbrecht Die Dissertation wurde am 12.11.2019 bei der Technischen Universit¨at M¨unchen eingereicht und durch die Fakult¨atf¨urPhysik am 24.01.2020 angenommen. Abstract Although the first hints towards dark matter were discovered almost 100 years ago, little is known today about its properties. Also, dark matter has so far only been inferred through astronomical and cosmological observations. In this work, we therefore investi- gate the influence of astrophysical assumptions on the interpretation of direct searches for dark matter. For this, we assume that dark matter is a weakly interacting massive particle. First, we discuss the development of a new analysis method for direct dark matter searches. Starting from the decomposition of the dark matter velocity distribu- tion into streams, we present a method that is completely independent of astrophysical assumptions. We extend this by using an effective theory for the interaction of dark matter with nucleons. This allows to analyze experiments with minimal assumptions on the particle physics of dark matter. Finally, we improve our method so that arbitrarily strong deviations from a reference velocity distribution can be considered. -
Clustering and Halo Abundances in Early Dark Energy Cosmological Models
Swarthmore College Works Physics & Astronomy Faculty Works Physics & Astronomy 6-1-2021 Clustering And Halo Abundances In Early Dark Energy Cosmological Models A. Klypin V. Poulin F. Prada J. Primack M. Kamionkowski See next page for additional authors Follow this and additional works at: https://works.swarthmore.edu/fac-physics Part of the Physics Commons Let us know how access to these works benefits ouy Recommended Citation A. Klypin, V. Poulin, F. Prada, J. Primack, M. Kamionkowski, V. Avila-Reese, A. Rodriguez-Puebla, P. Behroozi, D. Hellinger, and Tristan L. Smith. (2021). "Clustering And Halo Abundances In Early Dark Energy Cosmological Models". Monthly Notices Of The Royal Astronomical Society. Volume 504, Issue 1. 769-781. DOI: 10.1093/mnras/stab769 https://works.swarthmore.edu/fac-physics/430 This work is brought to you for free by Swarthmore College Libraries' Works. It has been accepted for inclusion in Physics & Astronomy Faculty Works by an authorized administrator of Works. For more information, please contact [email protected]. Authors A. Klypin, V. Poulin, F. Prada, J. Primack, M. Kamionkowski, V. Avila-Reese, A. Rodriguez-Puebla, P. Behroozi, D. Hellinger, and Tristan L. Smith This article is available at Works: https://works.swarthmore.edu/fac-physics/430 MNRAS 504, 769–781 (2021) doi:10.1093/mnras/stab769 Advance Access publication 2021 March 31 Clustering and halo abundances in early dark energy cosmological models Anatoly Klypin,1,2‹ Vivian Poulin,3 Francisco Prada,4 Joel Primack,5 Marc Kamionkowski,6 Vladimir Avila-Reese,7 Aldo Rodriguez-Puebla ,7 Peter Behroozi ,8 Doug Hellinger5 and Tristan L. -
Arxiv:1208.6426V2 [Hep-Ph]
FTUAM-12-101 IFT-UAM/CSIC-12-86 Nuclear uncertainties in the spin-dependent structure functions for direct dark matter detection D. G. Cerde˜no 1,2, M. Fornasa 3, J.-H. Huh 1,2,a, and M. Peir´o 1,2,b 1 Instituto de F´ısica Te´orica, UAM/CSIC, Universidad Aut´onoma de Madrid, Cantoblanco, E-28049, Madrid, Spain 2 Departamento de F´ısica Te´orica, Universidad Aut´onoma de Madrid, Cantoblanco, E-28049, Madrid, Spain and 3 School of Physics and Astronomy, University of Nottingham, University Park, NG7 2RD, United Kingdom We study the effect that uncertainties in the nuclear spin-dependent structure functions have in the determination of the dark matter (DM) parameters in a direct detection experiment. We show that different nuclear models that describe the spin-dependent structure function of specific target nuclei can lead to variations in the reconstructed values of the DM mass and scattering cross- section. We propose a parametrization of the spin structure functions that allows us to treat these uncertainties as variations of three parameters, with a central value and deviation that depend on the specific nucleus. The method is illustrated for germanium and xenon detectors with an exposure of 300 kg yr, assuming a hypothetical detection of DM and studying a series of benchmark points for the DM properties. We find that the effect of these uncertainties can be similar in amplitude to that of astrophysical uncertainties, especially in those cases where the spin-dependent contribution to the elastic scattering cross-section is sizable. I. INTRODUCTION [9], XENON100 [10, 11], EDELWEISS [12], SIMPLE [13], KIMS [14], and a combination of CDMS and EDEL- Direct searches of dark matter (DM) aim to observe WEISS data [15] are in strong tension with the regions this abundant but elusive component of the Universe by of the parameter space compatible with WIMP signals detecting its recoils off target nuclei of a detector (for in DAMA/LIBRA or CoGeNT. -
Modified Baryonic Dynamics: Two-Component Cosmological
Preprint typeset in JHEP style - HYPER VERSION Modified Baryonic Dynamics: two-component cosmological simulations with light sterile neutrinos G. W. Angus1,∗ A. Diaferio2,3, B. Famaey4, and K. J. van der Heyden5 1Department of Physics and Astrophysics, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium 2Dipartimento di Fisica, Universita` di Torino, Via P. Giuria 1, I-10125, Torino, Italy 3Istituto Nazionale di Fisica Nucleare, Via P. Giuria 1, I-10125, Torino, Italy 4Observatoire Astronomique de Strasbourg, CNRS UMR 7550, France 5Astrophysics, Cosmology & Gravity Centre, Dept. of Astronomy, University of Cape Town, Private Bag X3, Rondebosch, 7701, South Africa ABSTRACT: In this article we continue to test cosmological models centred on Modified Newtonian Dynamics (MOND) with light sterile neutrinos, which could in principle be a way to solve the fine-tuning problems of the standard model on galaxy scales while preserving successful predictions on larger scales. Due to previous failures of the simple MOND cosmological model, here we test a speculative model where the modified grav- itational field is produced only by the baryons and the sterile neutrinos produce a purely Newtonian field (hence Modified Baryonic Dynamics). We use two component cosmolog- ical simulations to separate the baryonic N-body particles from the sterile neutrino ones. arXiv:1407.1207v1 [astro-ph.CO] 4 Jul 2014 The premise is to attenuate the over-production of massive galaxy cluster halos which were prevalent in the original MOND plus light sterile neutrinos scenario. Theoretical issues with such a formulation notwithstanding, the Modified Baryonic Dynamics model fails to produce the correct amplitude for the galaxy cluster mass function for any reason- able value of the primordial power spectrum normalisation. -
Probing Cosmology at Different Scales
PROBING COSMOLOGY AT DIFFERENT SCALES by Daniel Pfeffer A dissertation submitted to The Johns Hopkins University in conformity with the requirements for the degree of Doctor of Philosophy. Baltimore, Maryland October, 2019 ⃝c 2019 Daniel Pfeffer All rights reserved Abstract Although we are in an era of precision cosmology, there is still much about our Universe that we do not know. Moreover, the concordance ΛCDM model of cosmology faces many challenges at all scales relevant to cosmology. Either discrepancies have been discovered with ΛCDM predictions or the model has simply broken down and is not a useful predictor. The current rate of expansion is incorrectly predicted by ΛCDM, as are the size and distribution of dwarf halo galaxies for Milky Way like galaxies. Obtaining the observed cores in galaxies with the standard description of dark matter is troublesome and requires more than the base ΛCDM model, as does understanding star formation and how it impacted galaxy evolution requires much more than base ΛCDM knowledge and many more. My work focuses on probing different scales in cosmology with different techniques to extract information about our Universe and its history. I use ultra-high-energy cosmic-rays (UHECRs) as a probe of the local universe and tested tidal disruption events (TDES) as a possible source of the UHECRs. By analyzing energy require- ii ABSTRACT ments, source densities and observed fluxes, I find that TDEs can explain the observed UHECR flux. The assumption of TDEs as the source of UHECRs can leadtoa measurement of the density of super massive black holes which reside in the center of galaxies.