Astroparticle Physics
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Astronomy 241: Foundations of Astrophysics I. the Solar System
Astronomy 241: Foundations of Astrophysics I. The Solar System Astronomy 241 is the first part of a year-long Prerequisites: Physics 170, Physics 272 introduction to astrophysics. It uses basic (or concurrent), and Math 242 or 252A. classical mechanics and thermodynamics to Contact: Professor Joshua Barnes analyze the structure and evolution of the ([email protected]; 956-8138) Solar System. www.ifa.hawaii.edu/~barnes/ast241 Tuesday, August 21, 2012 Astrophysics BS Degree Proposal in ASTR PHYS MATH CHEM preparation FALL 241 251A 161, 171 or 181 year 1 161L, 171L, or 181L SPRING 170 242 252A 162 year 1 170L 162L Foundations of Astrophysics I: FALL 241 272 243 253A The Solar System year 2 272L Foundations of Astrophysics II: SPRING 242 274 244 Galaxies & Stars year 2 274L Observational Astronomy & FALL 300 310 311 (or 307?) Laboratory year 3 300L 350 SPRING 301 311 Observational Project year 3 450 FALL 423 480 Stellar Astrophysics year 4 495 SPRING 496 481 Senior Project I, II year4 485 1 of: ASTR 320, 426, or 430 Tuesday, August 21, 2012 Units Text uses MKS units (meter, kilo-gram, second); e.g. G ≃ 6.674 × 10-11 m3 kg-1 s-2 (gravitational constant). Astronomers also use non-standard units: AU ≃ 1.496 × 1011 m (“average” Earth-Sun distance) 30 M⊙ ≃ 1.989 × 10 kg (Sun’s mass) yr ≃ 3.156 × 107 s (Earth’s orbital period) Tuesday, August 21, 2012 Order of Magnitude & Dimensional Analysis: An Example Given that Jupiter’s average density is slightly greater than water, estimate the orbital period of a satellite circling just above the planet. -
Dark Matter Sensitivity of Multi-Ton Liquid Xenon Detectors
Prepared for submission to JCAP Dark matter sensitivity of multi-ton liquid xenon detectors Marc Schumann,a;1 Laura Baudis,b Lukas Bütikofer,a Alexander Kish,b Marco Selvic aAlbert Einstein Center for Fundamental Physics, Universität Bern, Switzerland bPhysik-Institut, Universität Zürich, Switzerland cINFN Bologna, Italy E-mail: [email protected], [email protected], [email protected], [email protected], [email protected] Abstract. We study the sensitivity of multi ton-scale time projection chambers using a liquid xenon target, e.g., the proposed DARWIN instrument, to spin-independent and spin- dependent WIMP-nucleon scattering interactions. Taking into account realistic backgrounds from the detector itself as well as from neutrinos, we examine the impact of exposure, energy threshold, background rejection efficiency and energy resolution on the dark matter sensitivity. With an exposure of 200 t × y and assuming detector parameters which have been already demonstrated experimentally, spin-independent cross sections as low as 2:5×10−49 cm2 can be probed for WIMP masses around 40 GeV/c2. Additional improvements in terms of background rejection and exposure will further increase the sensitivity, while the ultimate WIMP science reach will be limited by neutrinos scattering coherently off the xenon nuclei. arXiv:1506.08309v2 [physics.ins-det] 3 Sep 2015 1Corresponding author. Contents 1 Introduction1 2 Light and Charge Signal Generation2 3 Energy Scale and Energy Resolution3 4 Evaluation of the spin-independent WIMP-nucleon Sensitivity4 5 Backgrounds6 6 Electronic Recoil Rejection 10 7 WIMP Sensitivity 12 8 Summary and Discussion 15 1 Introduction The nature of dark matter, contributing about 27% to the matter and energy content of our Universe [1], is one of the outstanding open questions in physics. -
European Astroparticle Physics Strategy 2017-2026 Astroparticle Physics European Consortium
European Astroparticle Physics Strategy 2017-2026 Astroparticle Physics European Consortium August 2017 European Astroparticle Physics Strategy 2017-2026 www.appec.org Executive Summary Astroparticle physics is the fascinating field of research long-standing mysteries such as the true nature of Dark at the intersection of astronomy, particle physics and Matter and Dark Energy, the intricacies of neutrinos cosmology. It simultaneously addresses challenging and the occurrence (or non-occurrence) of proton questions relating to the micro-cosmos (the world decay. of elementary particles and their fundamental interactions) and the macro-cosmos (the world of The field of astroparticle physics has quickly celestial objects and their evolution) and, as a result, established itself as an extremely successful endeavour. is well-placed to advance our understanding of the Since 2001 four Nobel Prizes (2002, 2006, 2011 and Universe beyond the Standard Model of particle physics 2015) have been awarded to astroparticle physics and and the Big Bang Model of cosmology. the recent – revolutionary – first direct detections of gravitational waves is literally opening an entirely new One of its paths is targeted at a better understanding and exhilarating window onto our Universe. We look of cataclysmic events such as: supernovas – the titanic forward to an equally exciting and productive future. explosions marking the final evolutionary stage of massive stars; mergers of multi-solar-mass black-hole Many of the next generation of astroparticle physics or neutron-star binaries; and, most compelling of all, research infrastructures require substantial capital the violent birth and subsequent evolution of our infant investment and, for Europe to remain competitive Universe. -
The Gran Sasso Underground Laboratory Program
The Gran Sasso Underground Laboratory Program Eugenio Coccia INFN Gran Sasso and University of Rome “Tor Vergata” [email protected] XXXIII International Meeting on Fundamental Physics Benasque - March 7, 2005 Underground Laboratories Boulby UK Modane France Canfranc Spain INFN Gran Sasso National Laboratory LNGSLNGS ROME QuickTime™ and a Photo - JPEG decompressor are needed to see this picture. L’AQUILA Tunnel of 10.4 km TERAMO In 1979 A. Zichichi proposed to the Parliament the project of a large underground laboratory close to the Gran Sasso highway tunnel, then under construction In 1982 the Parliament approved the construction, finished in 1987 In 1989 the first experiment, MACRO, started taking data LABORATORI NAZIONALI DEL GRAN SASSO - INFN Largest underground laboratory for astroparticle physics 1400 m rock coverage cosmic µ reduction= 10–6 (1 /m2 h) underground area: 18 000 m2 external facilities Research lines easy access • Neutrino physics 756 scientists from 25 countries Permanent staff = 66 positions (mass, oscillations, stellar physics) • Dark matter • Nuclear reactions of astrophysics interest • Gravitational waves • Geophysics • Biology LNGS Users Foreigners: 356 from 24 countries Italians: 364 Permanent Staff: 64 people Administration Public relationships support Secretariats (visa, work permissions) Outreach Environmental issues Prevention, safety, security External facilities General, safety, electrical plants Civil works Chemistry Cryogenics Mechanical shop Electronics Computing and networks Offices Assembly halls Lab -
Radiochemical Solar Neutrino Experiments, "Successful and Otherwise"
BNL-81686-2008-CP Radiochemical Solar Neutrino Experiments, "Successful and Otherwise" R. L. Hahn Presented at the Proceedings of the Neutrino-2008 Conference Christchurch, New Zealand May 25 - 31, 2008 September 2008 Chemistry Department Brookhaven National Laboratory P.O. Box 5000 Upton, NY 11973-5000 www.bnl.gov Notice: This manuscript has been authored by employees of Brookhaven Science Associates, LLC under Contract No. DE-AC02-98CH10886 with the U.S. Department of Energy. The publisher by accepting the manuscript for publication acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. This preprint is intended for publication in a journal or proceedings. Since changes may be made before publication, it may not be cited or reproduced without the author’s permission. DISCLAIMER This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor any agency thereof, nor any of their employees, nor any of their contractors, subcontractors, or their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or any third party’s use or the results of such use of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof or its contractors or subcontractors. -
In the Light of LSND, Miniboone and Other Data
DAPNIA-SPhT Joint Seminar, 21 May 2007 Exotic Neutrino Physics in the light of LSND, MiniBooNE and other data Marco Cirelli + Stéphane Lavignac SPhT - CEA/Saclay Introduction CDHSW Neutrino Physics (pre-MiniBooNE): CHORUS NOMAD NOMAD NOMAD 0 KARMEN2 CHORUS Everything fits in terms of: 10 LSND 3 neutrino oscillations (mass-driven) Bugey BNL E776 K2K SuperK CHOOZ erde 10–3 PaloV Super-K+SNO Cl +KamLAND ] 2 KamLAND [eV 2 –6 SNO m 10 Super-K ∆ Ga –9 10 νe↔νX νµ↔ντ νe↔ντ νe↔νµ 10–12 10–4 10–2 100 102 tan2θ http://hitoshi.berkeley.edu/neutrino Particle Data Group 2006 Introduction CDHSW Neutrino Physics (pre-MiniBooNE): CHORUS NOMAD NOMAD NOMAD 0 KARMEN2 CHORUS Everything fits in terms of: 10 LSND 3 neutrino oscillations (mass-driven) Bugey BNL E776 K2K SuperK Simple ingredients: CHOOZ erde 10–3 PaloV νe, νµ, ντ m1, m2, m3 Super-K+SNO Cl +KamLAND ] θ12, θ23, θ13 δCP 2 KamLAND [eV 2 –6 SNO m 10 Super-K ∆ Ga –9 10 νe↔νX νµ↔ντ νe↔ντ νe↔νµ 10–12 10–4 10–2 100 102 tan2θ http://hitoshi.berkeley.edu/neutrino Particle Data Group 2006 Introduction CDHSW Neutrino Physics (pre-MiniBooNE): CHORUS NOMAD NOMAD NOMAD 0 KARMEN2 CHORUS Everything fits in terms of: 10 LSND 3 neutrino oscillations (mass-driven) Bugey BNL E776 K2K SuperK Simple ingredients: CHOOZ erde 10–3 PaloV νe, νµ, ντ m1, m2, m3 Super-K+SNO Cl +KamLAND ] θ12, θ23, θ13 δCP 2 KamLAND Simple theory: [eV 2 –6 SNO m 10 |ν! = cos θ|ν1! + sin θ|ν2! Super-K ∆ −E1t −E2t |ν(t)! = e cos θ|ν1! + e sin θ|ν2! Ga 2 Ei = p + mi /2p 2 –9 ν ↔ν m L 10 e X 2 2 ∆ ν ↔ν P ν → ν θ µ τ ( α β) = sin 2 αβ sin ν ↔ν E e -
Small Scale Problems of the CDM Model
galaxies Article Small Scale Problems of the LCDM Model: A Short Review Antonino Del Popolo 1,2,3,* and Morgan Le Delliou 4,5,6 1 Dipartimento di Fisica e Astronomia, University of Catania , Viale Andrea Doria 6, 95125 Catania, Italy 2 INFN Sezione di Catania, Via S. Sofia 64, I-95123 Catania, Italy 3 International Institute of Physics, Universidade Federal do Rio Grande do Norte, 59012-970 Natal, Brazil 4 Instituto de Física Teorica, Universidade Estadual de São Paulo (IFT-UNESP), Rua Dr. Bento Teobaldo Ferraz 271, Bloco 2 - Barra Funda, 01140-070 São Paulo, SP Brazil; [email protected] 5 Institute of Theoretical Physics Physics Department, Lanzhou University No. 222, South Tianshui Road, Lanzhou 730000, Gansu, China 6 Instituto de Astrofísica e Ciências do Espaço, Universidade de Lisboa, Faculdade de Ciências, Ed. C8, Campo Grande, 1769-016 Lisboa, Portugal † [email protected] Academic Editors: Jose Gaite and Antonaldo Diaferio Received: 30 May 2016; Accepted: 9 December 2016; Published: 16 February 2017 Abstract: The LCDM model, or concordance cosmology, as it is often called, is a paradigm at its maturity. It is clearly able to describe the universe at large scale, even if some issues remain open, such as the cosmological constant problem, the small-scale problems in galaxy formation, or the unexplained anomalies in the CMB. LCDM clearly shows difficulty at small scales, which could be related to our scant understanding, from the nature of dark matter to that of gravity; or to the role of baryon physics, which is not well understood and implemented in simulation codes or in semi-analytic models. -
The Great Debate Page 6 in This Issue: CLAS Welcomes New Faculty
November 2004 Volume 18 notes CLASThe University of Florida College of Liberal Arts and Sciences The Great Debate page 6 In this Issue: CLAS Welcomes New Faculty ........... 3 The Great Debate ............................. 6 Around the College ......................... 8 Grants .............................................. 10 Bookbeat ........................................ 11 The Dean’s Junk Mail Be Gone! ....................... 12 Musings The Fundamentals As important as our cross-disciplinary interactions are, E-mail [email protected] with your news and especially in the applied sciences and social sciences, events information for publication in CLAS- we need to remind ourselves of the critical importance notes. The deadline for submissions is the 15th of the month prior to the month you would of the fundamental academic disciplines—the essential like your information published. Don’t wait! units of mathematics, English, philosophy, history, the Send us your news and events today! languages, natural sciences, behavioral sciences and social studies. It is these core units that engage in the basic research that historically has led to some of the most far-reaching discoveries and the formation of new interdisciplinary programs. Inventions which have led to revolutionary technologies and analyses that College of Liberal Arts and Sciences News and Publications have changed our understanding of societies and their 2008 Turlington Hall behaviors have often had their as their origin the PO Box 117300 Gainesville FL 32611-7300 research of a challenging academic problem. [email protected] Our college has the responsibility of advancing http://clasnews.clas.ufl.edu these basic areas of inquiry by energizing fundamental CLASnotes is published by the College of Liberal research with support for promising interdisciplinary Arts and Sciences to inform faculty, staff and stu- programs. -
Particle Dark Matter an Introduction Into Evidence, Models, and Direct Searches
Particle Dark Matter An Introduction into Evidence, Models, and Direct Searches Lecture for ESIPAP 2016 European School of Instrumentation in Particle & Astroparticle Physics Archamps Technopole XENON1T January 25th, 2016 Uwe Oberlack Institute of Physics & PRISMA Cluster of Excellence Johannes Gutenberg University Mainz http://xenon.physik.uni-mainz.de Outline ● Evidence for Dark Matter: ▸ The Problem of Missing Mass ▸ In galaxies ▸ In galaxy clusters ▸ In the universe as a whole ● DM Candidates: ▸ The DM particle zoo ▸ WIMPs ● DM Direct Searches: ▸ Detection principle, physics inputs ▸ Example experiments & results ▸ Outlook Uwe Oberlack ESIPAP 2016 2 Types of Evidences for Dark Matter ● Kinematic studies use luminous astrophysical objects to probe the gravitational potential of a massive environment, e.g.: ▸ Stars or gas clouds probing the gravitational potential of galaxies ▸ Galaxies or intergalactic gas probing the gravitational potential of galaxy clusters ● Gravitational lensing is an independent way to measure the total mass (profle) of a foreground object using the light of background sources (galaxies, active galactic nuclei). ● Comparison of mass profles with observed luminosity profles lead to a problem of missing mass, usually interpreted as evidence for Dark Matter. ● Measuring the geometry (curvature) of the universe, indicates a ”fat” universe with close to critical density. Comparison with luminous mass: → a major accounting problem! Including observations of the expansion history lead to the Standard Model of Cosmology: accounting defcit solved by ~68% Dark Energy, ~27% Dark Matter and <5% “regular” (baryonic) matter. ● Other lines of evidence probe properties of matter under the infuence of gravity: ▸ the equation of state of oscillating matter as observed through fuctuations of the Cosmic Microwave Background (acoustic peaks). -
A Survey of the Physics Related to Underground Labs
ANDES: A survey of the physics related to underground labs. Osvaldo Civitarese Dept.of Physics, University of La Plata and IFLP-CONICET ANDES/CLES working group ANDES: A survey of the physics related to underground labs. – p. 1 Plan of the talk The field in perspective The neutrino mass problem The two-neutrino and neutrino-less double beta decay Neutrino-nucleus scattering Constraints on the neutrino mass and WR mass from LHC-CMS and 0νββ Dark matter Supernovae neutrinos, matter formation Sterile neutrinos High energy neutrinos, GRB Decoherence Summary The field in perspective How the matter in the Universe was (is) formed ? What is the composition of Dark matter? Neutrino physics: violation of fundamental symmetries? The atomic nucleus as a laboratory: exploring physics at large scale. Neutrino oscillations Building neutrino flavor states from mass eigenstates νl = Uliνi i X Energy of the state m2c4 E ≈ pc + i i 2E Probability of survival/disappearance 2 ′ −i(Ei−Ep)t/h¯ ∗ P (νl → νl′ )= | δ(l, l )+ Ul′i(e − 1)Uli | 6 Xi=p 2 2 4 (mi −mp )c L provided 2Ehc¯ ≥ 1 Neutrino oscillations The existence of neutrino oscillations was demonstrated by experiments conducted at SNO and Kamioka. The Swedish Academy rewarded the findings with two Nobel Prices : Koshiba, Davis and Giacconi (2002) and Kajita and Mc Donald (2015) Some of the experiments which contributed (and still contribute) to the measurements of neutrino oscillation parameters are K2K, Double CHOOZ, Borexino, MINOS, T2K, Daya Bay. Like other underground labs ANDES will certainly be a good option for these large scale experiments. -
SNOLAB Construction Status and Experimental Program
M. Chen Queen’s University SNOLAB Construction Status and Experimental Program SNOLAB located 2 km underground in an active nickel mine near Sudbury, Canada it’s an expansion of the underground facility on the same level as the SNO experiment Surface Facility Excavation Status (Today) -Blasting for Phase I Excavation complete. - Shotcrete walls complete - Concrete floors almost finished. BLADDER ROOM BLADDER ROOM SHOWER ROOM SHOWER ROOM DOUBLE TRACKS DOUBLE TRACKS LADDER LABS LADDER LABS CUBE HALL CUBE HALL Phase I - Cube Hall (18x15x15 m) - Ladder Labs (~7mx~7mx60m) Utility Area - Chiller, generator, Lab Entrance water systems Existing SNO - Personnel Areas Facilities -Material Handling -SNO Cavern (30m x 22m dia) - Utility & Control Rms SNOLAB Workshop V, 21 August 2006 Phase II -Cryopit Phase I (15m x15m dia) - Cube Hall (18x15x15 m) - Ladder Labs (~7mx~7mx60m) Utility Area - Chiller, generator, Lab Entrance water systems Existing SNO - Personnel Areas Facilities -Material Handling -SNO Cavern (30m x 22m dia) - Utility & Control Rms Rectangular Hall Control Rm Utility Drift Staging Area Rectangular Hall 60’L x 50’W 50’ (shoulder) 65’ (back) SNOLAB Workshop IV, 15 Aug 2005 Ladder Labs Wide Drift Electrical, 20’x12’ AHUs (19’ to back) Wide Drift 25’x17’ (25’ to back) Access Drift 15’x10’ (15’ to back) Chemistry Lab SNOLAB Workshop IV, 15 Aug 2005 SNOLAB Experiments z Some 20 projects submitted Letters of Interest in locating at SNOLAB. Of these, 10 have been encouraged by the Experiment Advisory Committee as being both scientifically important and particularly suited to the SNOLAB location. z The experimental physics program includes − Neutrinos: Low energy solar neutrinos, geo-neutrinos, reactor neutrinos, supernova neutrino detection z Tests of neutrino properties, precision measurements of solar neutrinos, radiogenic heat generation in the earth, stellar evolution. -
Dark Matter, Oscillations, Exotics Subgroup
Dark matter from ZeV to aeV: 3rd IBS-MultiDark-IPPP Workshop Durham, November 2016 Juande ZZornozaornoza (IFIC, UV-CSIC) Introduction X-rays and sterile neutrinos Neutrino telescopes Results . Sun . Earth . Milky Way . Extra-galactic Future Summary The evidence for the existence Virial theorem of dark matter is very solid and, which is very important, at many different scales Rotation curves Comma Cluster Cosmic Microwave Background Bullet Cluster Gravitational Lensing + BNN, N-body simulations… We do not know what is dark matter, so it is hard to say which is the winning strategy: multi-front attack! PAMELA, AMS FERMI, MAGIC ANTARES, IceCube… Indirect detection XENON χ q, W+, Z… CDMS In any case: CoGENT -we want more than one DAMA “detection” +astrophysical ANAIS -results (constraints) of each … probes ( self- strategy are input for the others interaction of χ Directdetection q, W-, Z… DM affecting dark matter densities in Accelerators LHC galaxies…) Credit: Sky & Telescope / Gregg Dinderman X-ray astronomy (1-100 keV) differs from gamma ray astronomy in the detection strategy Atmosphere absorbs X-rays and fluxes are high, so observation is based on balloons and satellites X-rays cannot be focused by lenses, so focusing is based on total reflection (Wolter telescope) Projects: Chandra, XMM-Newton, Suzaku XMM-Newton: Large collecting area Simultaneous imaging and high resolution spectroscopy Monochromatic 3.5 keV photon line observed in data of XMM-Newton from 73 galaxy clusters Located within 50-100 eV of several known faint lines Interpreted as decay from sterile Bulbul, arxiv:1402.2301 neutrinos with ms=7.1 keV, which would be dark matter Boyarsky, arxiv:1402.4119 Also observed in Andromeda and Perseus Interpretation as sterile neutrino (sin2 (2θ)∼7x10-11) consistent with present constraints However, significant astrophysical unknowns involved (for instance, potassium XVIII line) Bulbul, arxiv:1402.2301 Boyarsky, arxiv:1402.4119 Astro-H Chandra Astro-H satellite (aka Hitomi), equipped with a X-ray spectrometer, was launched in Feb 2016.