Constraining Galactic Structures of Mirror Dark Matter
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Current Perspectives on Dark Matter
Cosmological Signatures of a Mirror Twin Higgs Zackaria Chacko University of Maryland, College Park Curtin, Geller & Tsai Introduction The Twin Higgs framework is a promising approach to the naturalness problem of the Standard Model (SM). In Mirror Twin Higgs models, the SM is extended to include a complete mirror (“twin”) copy of the SM, with its own particle content and gauge groups. The SM and its twin counterpart are related by a discrete Z2 “twin” symmetry. Z2 SMA SMB The mirror particles are completely neutral under the SM strong, weak and electromagnetic forces. Only feel gravity. In Mirror Twin Higgs models, the one loop quadratic divergences that contribute to the Higgs mass are cancelled by twin sector states that carry no charge under the SM gauge groups. Discovery of these states at LHC is therefore difficult. May explain null results. The SM and twin SM primarily interact through the Higgs portal. This interaction is needed for cancellation of quadratic divergences. After electroweak symmetry breaking, SM Higgs and twin Higgs mix. • Higgs couplings to SM states are suppressed by the mixing. • Higgs now has (mixing suppressed) couplings to twin states. A soft breaking of the Z2 symmetry ensures that 퐯B, the VEV of the twin Higgs, is greater than 퐯A, the VEV of the SM Higgs. The mixing angle ~ 퐯A/퐯B. Higgs measurements constrain 퐯A/퐯B ≤ ퟏ/ퟑ. Twin fermions are heavier than SM fermions by a factor of 퐯B/퐯A . Naturalness requires 퐯A/퐯B ≥ ퟏ/ퟓ. (Twin top should not be too heavy.) The Higgs portal interaction has implications for cosmology. -
Searches for Dark Matter Self-Annihilation Signals from Dwarf Spheroidal Galaxies and the Fornax Galaxy Cluster with Imaging Air Cherenkov Telescopes
Searches for dark matter self-annihilation signals from dwarf spheroidal galaxies and the Fornax galaxy cluster with imaging air Cherenkov telescopes Dissertation zur Erlangung des Doktorgrades des Fachbereichs Physik der Universität Hamburg vorgelegt von Björn Helmut Bastian Opitz aus Warburg Hamburg 2014 Gutachter der Dissertation: Prof. Dr. Dieter Horns JProf. Dr. Christian Sander Gutachter der Disputation: Prof. Dr. Dieter Horns Prof. Dr. Jan Conrad Datum der Disputation: 17. Juni 2014 Vorsitzender des Prüfungsausschusses: Dr. Georg Steinbrück Vorsitzende des Promotionsausschusses: Prof. Dr. Daniela Pfannkuche Leiter des Fachbereichs Physik: Prof. Dr. Peter Hauschildt Dekan der MIN-Fakultät: Prof. Dr. Heinrich Graener Abstract Many astronomical observations indicate that dark matter pervades the universe and dominates the formation and dynamics of cosmic structures. Weakly inter- acting massive particles (WIMPs) with masses in the GeV to TeV range form a popular class of dark matter candidates. WIMP self-annihilation may lead to the production of γ-rays in the very high energy regime above 100 GeV, which is observable with imaging air Cherenkov telescopes (IACTs). For this thesis, observations of dwarf spheroidal galaxies (dSph) and the For- nax galaxy cluster with the Cherenkov telescope systems H.E.S.S., MAGIC and VERITAS were used to search for γ-ray signals of dark matter annihilations. The work consists of two parts: First, a likelihood-based statistical technique was intro- duced to combine published results of dSph observations with the different IACTs. The technique also accounts for uncertainties on the “J factors”, which quantify the dark matter content of the dwarf galaxies. Secondly, H.E.S.S. -
Signs of Dark Matter May Point to Mirror Matter Candidate 27 April 2010, by Lisa Zyga
Signs of dark matter may point to mirror matter candidate 27 April 2010, by Lisa Zyga (PhysOrg.com) -- Dark matter, which contains the At first, mirror matter may sound a bit like antimatter "missing mass" that's needed to explain why (which is ordinary matter with an opposite charge). galaxies stay together, could take any number of In both theories, the number of known particles forms. The main possible candidates include would double. However, while antimatter interacts MACHOS and WIMPS, but there is no shortage of very strongly with ordinary matter, annihilating itself proposals. Rather, the biggest challenge is finding into photons, mirror matter would interact very some evidence that would support one or more of weakly with ordinary matter. For this reason, some these candidates. Currently, more than 30 physicists have speculated that mirror particles experiments are underway trying to detect a sign of could be candidates for dark matter. Even though dark matter. So far, only two experiments claim to mirror matter would produce light, we would not see have found signals, with the most recent it, and it would be very difficult to detect. observations coming just a month ago. Now, physicist Robert Foot from the University of However, mirror matter would not be impossible to Melbourne has shown that the results of these two detect, and Foot thinks that the DAMA experiment experiments can be simultaneously explained by and the CoGeNT experiment may have detected an intriguing dark matter candidate called mirror mirror matter. In DAMA, scientists observed a piece matter. of sodium iodide, which should generate a photon when struck by a dark matter particle. -
Highlights and Discoveries from the Chandra X-Ray Observatory1
Highlights and Discoveries from the Chandra X-ray Observatory1 H Tananbaum1, M C Weisskopf2, W Tucker1, B Wilkes1 and P Edmonds1 1Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138. 2 NASA/Marshall Space Flight Center, ZP12, 320 Sparkman Drive, Huntsville, AL 35805. Abstract. Within 40 years of the detection of the first extrasolar X-ray source in 1962, NASA’s Chandra X-ray Observatory has achieved an increase in sensitivity of 10 orders of magnitude, comparable to the gain in going from naked-eye observations to the most powerful optical telescopes over the past 400 years. Chandra is unique in its capabilities for producing sub-arcsecond X-ray images with 100-200 eV energy resolution for energies in the range 0.08<E<10 keV, locating X-ray sources to high precision, detecting extremely faint sources, and obtaining high resolution spectra of selected cosmic phenomena. The extended Chandra mission provides a long observing baseline with stable and well-calibrated instruments, enabling temporal studies over time-scales from milliseconds to years. In this report we present a selection of highlights that illustrate how observations using Chandra, sometimes alone, but often in conjunction with other telescopes, have deepened, and in some instances revolutionized, our understanding of topics as diverse as protoplanetary nebulae; massive stars; supernova explosions; pulsar wind nebulae; the superfluid interior of neutron stars; accretion flows around black holes; the growth of supermassive black holes and their role in the regulation of star formation and growth of galaxies; impacts of collisions, mergers, and feedback on growth and evolution of groups and clusters of galaxies; and properties of dark matter and dark energy. -
Stats2010 E Final.Pdf
Imprint Publisher: Max-Planck-Institut für extraterrestrische Physik Editors and Layout: W. Collmar und J. Zanker-Smith Personnel 1 PERSONNEL 2010 Directors Min. Dir. J. Meyer, Section Head, Federal Ministry of Prof. Dr. R. Bender, Optical and Interpretative Astronomy, Economics and Technology also Professorship for Astronomy/Astrophysics at the Prof. Dr. E. Rohkamm, Thyssen Krupp AG, Düsseldorf Ludwig-Maximilians-University Munich Prof. Dr. R. Genzel, Infrared- and Submillimeter- Scientifi c Advisory Board Astronomy, also Prof. of Physics, University of California, Prof. Dr. R. Davies, Oxford University (UK) Berkeley (USA) (Managing Director) Prof. Dr. R. Ellis, CALTECH (USA) Prof. Dr. Kirpal Nandra, High-Energy Astrophysics Dr. N. Gehrels, NASA/GSFC (USA) Prof. Dr. G. Morfi ll, Theory, Non-linear Dynamics, Complex Prof. Dr. F. Harrison, CALTECH (USA) Plasmas Prof. Dr. O. Havnes, University of Tromsø (Norway) Prof. Dr. G. Haerendel (emeritus) Prof. Dr. P. Léna, Université Paris VII (France) Prof. Dr. R. Lüst (emeritus) Prof. Dr. R. McCray, University of Colorado (USA), Prof. Dr. K. Pinkau (emeritus) Chair of Board Prof. Dr. J. Trümper (emeritus) Prof. Dr. M. Salvati, Osservatorio Astrofi sico di Arcetri (Italy) Junior Research Groups and Minerva Fellows Dr. N.M. Förster Schreiber Humboldt Awardee Dr. S. Khochfar Prof. Dr. P. Henry, University of Hawaii (USA) Prof. Dr. H. Netzer, Tel Aviv University (Israel) MPG Fellow Prof. Dr. V. Tsytovich, Russian Academy of Sciences, Prof. Dr. A. Burkert (LMU) Moscow (Russia) Manager’s Assistant Prof. S. Veilleux, University of Maryland (USA) Dr. H. Scheingraber A. v. Humboldt Fellows Scientifi c Secretary Prof. Dr. D. Jaffe, University of Texas (USA) Dr. -
Particle - Mirror Particle Oscillations: CP-Violation and Baryon Asymmetry
Particle - Mirror Particle Oscillations: CP-violation and Baryon Asymmetry Zurab Berezhiani Università di L’Aquila and LNGS, Italy 0 CPT at ICTP, Triest, 2-5 July 2008 n − n oscillations etc ... - p. 1/42 Alice & Mirror World Lewis Carroll, "Through the Looking-Glass" ‘Now, if you’ll only attend, Kitty, and not talk so much, I’ll tell you all my ideas about Looking-glass House. There’s the room you can see through the glass – that’s just the same ● Carrol’s Alice... ● Mirror World as our drawing-room, only the things go the other way... the books are something like our ● Mirror Particles ● Interactions books, only the words go the wrong way: I know that, because I’ve held up one of our books to ● B & L violation ● BBN demands the glass, and then they hold up one in the other room. I can see all of it – all but the bit just ● Present Cosmology ● Visible vs. Dark matter behind the fireplace. I do so wish I could see that bit! I want so to know whether they’ve a fire ● B vs. D – Fine Tuning demonstration ● Unification in the winter: you never can tell, you know, unless our fire smokes, and then smoke comes up ● Neutrino Mixing ● See-Saw in that room too – but that may be only pretence, just to make it look as if they had a fire... ● Leptogenesis: diagrams ● Leptogenesis: formulas ‘How would you like to leave in the Looking-glass House, Kitty? I wander if they’d give you milk ● Epochs ● Neutron mixing in there? But perhaps Looking-glass milk isn’t good to drink? Now we come to the passage: ● Neutron mixing ● Oscillation it’s very like our passage as far as you can see, only you know it may be quite on beyond. -
Glossary of Terms Absorption Line a Dark Line at a Particular Wavelength Superimposed Upon a Bright, Continuous Spectrum
Glossary of terms absorption line A dark line at a particular wavelength superimposed upon a bright, continuous spectrum. Such a spectral line can be formed when electromag- netic radiation, while travelling on its way to an observer, meets a substance; if that substance can absorb energy at that particular wavelength then the observer sees an absorption line. Compare with emission line. accretion disk A disk of gas or dust orbiting a massive object such as a star, a stellar-mass black hole or an active galactic nucleus. An accretion disk plays an important role in the formation of a planetary system around a young star. An accretion disk around a supermassive black hole is thought to be the key mecha- nism powering an active galactic nucleus. active galactic nucleus (agn) A compact region at the center of a galaxy that emits vast amounts of electromagnetic radiation and fast-moving jets of particles; an agn can outshine the rest of the galaxy despite being hardly larger in volume than the Solar System. Various classes of agn exist, including quasars and Seyfert galaxies, but in each case the energy is believed to be generated as matter accretes onto a supermassive black hole. adaptive optics A technique used by large ground-based optical telescopes to remove the blurring affects caused by Earth’s atmosphere. Light from a guide star is used as a calibration source; a complicated system of software and hardware then deforms a small mirror to correct for atmospheric distortions. The mirror shape changes more quickly than the atmosphere itself fluctuates. -
Meeting Program
A A S MEETING PROGRAM 211TH MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY WITH THE HIGH ENERGY ASTROPHYSICS DIVISION (HEAD) AND THE HISTORICAL ASTRONOMY DIVISION (HAD) 7-11 JANUARY 2008 AUSTIN, TX All scientific session will be held at the: Austin Convention Center COUNCIL .......................... 2 500 East Cesar Chavez St. Austin, TX 78701 EXHIBITS ........................... 4 FURTHER IN GRATITUDE INFORMATION ............... 6 AAS Paper Sorters SCHEDULE ....................... 7 Rachel Akeson, David Bartlett, Elizabeth Barton, SUNDAY ........................17 Joan Centrella, Jun Cui, Susana Deustua, Tapasi Ghosh, Jennifer Grier, Joe Hahn, Hugh Harris, MONDAY .......................21 Chryssa Kouveliotou, John Martin, Kevin Marvel, Kristen Menou, Brian Patten, Robert Quimby, Chris Springob, Joe Tenn, Dirk Terrell, Dave TUESDAY .......................25 Thompson, Liese van Zee, and Amy Winebarger WEDNESDAY ................77 We would like to thank the THURSDAY ................. 143 following sponsors: FRIDAY ......................... 203 Elsevier Northrop Grumman SATURDAY .................. 241 Lockheed Martin The TABASGO Foundation AUTHOR INDEX ........ 242 AAS COUNCIL J. Craig Wheeler Univ. of Texas President (6/2006-6/2008) John P. Huchra Harvard-Smithsonian, President-Elect CfA (6/2007-6/2008) Paul Vanden Bout NRAO Vice-President (6/2005-6/2008) Robert W. O’Connell Univ. of Virginia Vice-President (6/2006-6/2009) Lee W. Hartman Univ. of Michigan Vice-President (6/2007-6/2010) John Graham CIW Secretary (6/2004-6/2010) OFFICERS Hervey (Peter) STScI Treasurer Stockman (6/2005-6/2008) Timothy F. Slater Univ. of Arizona Education Officer (6/2006-6/2009) Mike A’Hearn Univ. of Maryland Pub. Board Chair (6/2005-6/2008) Kevin Marvel AAS Executive Officer (6/2006-Present) Gary J. Ferland Univ. of Kentucky (6/2007-6/2008) Suzanne Hawley Univ. -
Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Andrew Lipnicky [email protected]
Rochester Institute of Technology RIT Scholar Works Theses Thesis/Dissertation Collections 7-2017 Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Andrew Lipnicky [email protected] Follow this and additional works at: http://scholarworks.rit.edu/theses Recommended Citation Lipnicky, Andrew, "Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far" (2017). Thesis. Rochester Institute of Technology. Accessed from This Dissertation is brought to you for free and open access by the Thesis/Dissertation Collections at RIT Scholar Works. It has been accepted for inclusion in Theses by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. R I T · · Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Andrew Lipnicky A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Astrophysical Sciences and Technology in the College of Science, School of Physics and Astronomy Rochester Institute of Technology © A. Lipnicky July, 2017 Rochester Institute of Technology Ph.D. Dissertation Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Author: Advisor: Andrew Lipnicky Dr. Sukanya Chakrabarti A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Astrophysical Sciences and Technology in the College of Science, School of Physics and Astronomy Approved by Dr.AndrewRobinson Date Director, Astrophysical Sciences and Technology Certificate of Approval Astrophysical Sciences and Technology R I T College of Science · · Rochester, NY, USA The Ph.D. Dissertation of Andrew Lipnicky has been approved by the undersigned members of the dissertation committee as satisfactory for the degree of Doctor of Philosophy in Astrophysical Sciences and Technology. -
Publications 2012
Publications - print summary 27 Feb 2013 1 *Abramowski, A.; Acero, F.; Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Balzer, A.; Barnacka, A.; Barres de Almeida, U.; Becherini, Y.; Becker, J.; and 201 coauthors "A multiwavelength view of the flaring state of PKS 2155-304 in 2006". (C) A&A, 539, 149 (2012). 2 *Ackermann, M.; Ajello, J.; Ballet, G.; Barbiellini, D.; Bastieri, A.; Belfiore; Bellazzini, B.; Berenji, R.D. and 57 coauthors "Periodic emission from the Gamma-Ray Binary 1FGL J1018.6–5856". (O) Science, 335, 189-193 (2012). 3 *Agliozzo, C.; Umana, G.; Trigilio, C.; Buemi, C.; Leto, P.; Ingallinera, A.; Franzen, T.; Noriega-Crespo, A. "Radio detection of nebulae around four luminous blue variable stars in the Large Magellanic Cloud". (C) MNRAS, 426, 181-186 (2012). 4 *Ainsworth, R.E.; Scaife, A.M.M.; Ray, T.P.; Buckle, J.V.; Davies, M.; Franzen, T.M.O.; Grainge, K.J.B.; Hobson, M.P.; Shimwell, T.; and 12 coauthors "AMI radio continuum observations of young stellar objects with known outflows". (O) MNRAS, 423, 1089-1108 (2012). 5 *Allison, J.R.; Curran, S.J.; Emonts, B H.C.; Geréb, K.; Mahony, E.K.; Reeves, S.; Sadler, E.M.; Tanna, A.; Whiting, M.T.; Zwaan, M.A. "A search for 21 cm H I absorption in AT20G compact radio galaxies". (C) MNRAS, 423, 2601-2616 (2012). 6 *Allison, J R.; Sadler, E.M.; Whiting, M.T. "Application of a bayesian method to absorption spectral-line finding in simulated ASKAP Data". (A) PASA, 29, 221-228 (2012). 7 *Alves, M.I.R.; Davies, R.D.; Dickinson, C.; Calabretta, M.; Davis, R.; Staveley-Smith, L. -
Mirror Matter: Astrophysical Implications
Mirror Matter: Astrophysical implications Zurab Berezhiani Summary Mirror Matter: Astrophysical implications Introduction: Dark Matter from a Parallel World Chapter I: Neutrino - mirror neutrino mixings Zurab Berezhiani Chapter II: neutron { mirror University of L'Aquila and LNGS neutron mixing Chapter IV: n − n0 and Neutron Stars Quarks-2021 , 22-24 June 2021 Contents Mirror Matter: Astrophysical implications Zurab Berezhiani Summary Introduction: Dark Matter from 1 Introduction: Dark Matter from a Parallel World a Parallel World Chapter I: Neutrino - mirror neutrino mixings 2 Chapter I: Neutrino - mirror neutrino mixings Chapter II: neutron { mirror neutron mixing Chapter IV: n − n0 and 3 Chapter II: neutron { mirror neutron mixing Neutron Stars 4 Chapter IV: n n0 and Neutron Stars − Mirror Matter: Astrophysical implications Zurab Berezhiani Summary Introduction: Dark Matter from a Parallel World Introduction Chapter I: Neutrino - mirror neutrino mixings Chapter II: neutron { mirror neutron mixing Chapter IV: n − n0 and Everything can be explained by the Standard Model ! Neutron Stars ... but there should be more than one Standard Models Bright & Dark Sides of our Universe Mirror Matter: Ω 0 05 observable matter: electron, proton, neutron ! Astrophysical B : implications ' ΩD 0:25 dark matter: WIMP? axion? sterile ν? ... Zurab Berezhiani ' ΩΛ 0:70 dark energy: Λ-term? Quintessence? .... Summary ' 3 Introduction: ΩR < 10− relativistic fraction: relic photons and neutrinos Dark Matter from a Parallel World Matter { dark energy coincidence: Ω Ω 0 45, (Ω = Ω + Ω ) Chapter I: M = Λ : M D B Neutrino - mirror 3 ' ρΛ Const., ρM a− ; why ρM /ρΛ 1 { just Today? neutrino mixings ∼ ∼ ∼ Chapter II: Antrophic explanation: if not Today, then Yesterday or Tomorrow. -
Gravitycam: Wide-Filed High-Resolution High-Cadence Imaging Surveys in the Visible Form the Ground
LJMU Research Online Mackay, C, Dominik, M, Steele, IA, Snodgrass, C, Jorgensen, UG, Skottfelt, J, Stefanov, K, Carry, B, Braga-Ribas, F, Doressoundiram, A, Ivanov, VD, Gandhi, P, Evans, DF, Hundertmark, M, Serjeant, S and Ortolani, S GravityCam: Wide-filed high-resolution high-cadence imaging surveys in the visible form the ground http://researchonline.ljmu.ac.uk/id/eprint/10404/ Article Citation (please note it is advisable to refer to the publisher’s version if you intend to cite from this work) Mackay, C, Dominik, M, Steele, IA, Snodgrass, C, Jorgensen, UG, Skottfelt, J, Stefanov, K, Carry, B, Braga-Ribas, F, Doressoundiram, A, Ivanov, VD, Gandhi, P, Evans, DF, Hundertmark, M, Serjeant, S and Ortolani, S (2018) GravityCam: Wide-filed high-resolution high-cadence imaging surveys in LJMU has developed LJMU Research Online for users to access the research output of the University more effectively. Copyright © and Moral Rights for the papers on this site are retained by the individual authors and/or other copyright owners. Users may download and/or print one copy of any article(s) in LJMU Research Online to facilitate their private study or for non-commercial research. You may not engage in further distribution of the material or use it for any profit-making activities or any commercial gain. The version presented here may differ from the published version or from the version of the record. Please see the repository URL above for details on accessing the published version and note that access may require a subscription. For more information please contact [email protected] http://researchonline.ljmu.ac.uk/ http://researchonline.ljmu.ac.uk/ Publications of the Astronomical Society of Australia (PASA) doi: 10.1017/pas.2018.xxx.