DOCSLIB.ORG

Dark Matter in Galaxy Clusters

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Dark Matter in Galaxy Clusters ESHEP School, Bansko (Bulgaria) - Sept 2015 Cosmology Lecture 2 Andrea De Simone Outline • LECTURE 1: The Universe around us. Dynamics. Energy Budget. The Standard Model of Cosmology: the 3 pillars (Expansion, Nucleosynthesis, CMB). • LECTURE 2: Dark Energy. Dark Matter as a thermal relic. Searches for WIMPs. • LECTURE 3: Shortcomings of Big Bang cosmology. Inflation. Baryogenesis A. De Simone 2 Outline • LECTURE 1: The Universe around us. Dynamics. Energy Budget. The Standard Model of Cosmology: the 3 pillars (Expansion, Nucleosynthesis, CMB) • LECTURE 2: Dark Energy. Dark Matter as a thermal relic. Searches for WIMPs. • LECTURE 3: Shortcomings of Big Bang cosmology. Inflation. Baryogenesis A. De Simone 3 Dark Energy 2 main sets of evidences for Dark Energy: 1. energy budget: fit to CMB anisotropy map provides many cosmological parameters: Ωtot ~ 1.0, Ωmatter ~ 0.3, Ωradiation ~ 0.0 ΩΛ ~ 0.7 2. distant SuperNovae (SN) (1998-Pelmutter, Schmidt, Riess - Nobel prize 2011) A. De Simone 4 20 20 Dark Energy luminosity distance dL =(1+z)r(z) depens on Ωmatter, ΩΛ ,Ωradiation , Ωk absolute (M) and apparent (m) magnitude are d related to distance: m M = 5 log L + K − 10pc ✓ ◆ FigureSN 5. ΛareCDM model: ʻstandard68.3%, 95.4%,and99 .7%candlesconfidence regions ofʼ the(known(Ωm, ΩΛ) plane from absolute SNe Ia combined with themagnitude). constraints from BAO and CMB. The left panel shows the SN Ia confidence region only including statistical errors while the right panel shows the SN Iaconfidenceregionwithboth statistical and systematic errors. Measure m measure dL measure Ωmatter, ΩΛ Figure 5. ΛCDM model: 68.3%, 95.4%,and99.7% confidence regions of the (Ωm, ΩΛ) plane from SNe Ia combined with the constraints from BAO and CMB. The left panel[arXiv:1105.3470] shows the SN Ia confidence region only including statistical errors while the right panel shows the SN Iaconfidenceregionwithboth statistical and systematic errors. new form of energy with negative pressure (w<0) results consistent with cosmological constant (vacuum energy with w=-1) Figure 6. wCDM model: 68.3%, 95.4%,and99.7% confidence regions in the (Ωm,w) plane from SNe Ia BAO and CMB. The left panel shows the SN Ia confidence region for statistical uncertainties only, whiletherightpanelshowstheconfidenceregionincludingbothstatistical and systematic uncertainties. We A.note thatDe CMB and Simone SN Ia constraints are orthogonal, making this combination of cosmological probes very powerful for investigating the nature of dark energy. 5 Figure 6. wCDM model: 68.3%, 95.4%,and99.7% confidence regions in the (Ωm,w) plane from SNe Ia BAO and CMB. The left panel shows the SN Ia confidence region for statistical uncertainties only, whiletherightpanelshowstheconfidenceregionincludingbothstatistical and systematic uncertainties. We note that CMB and SN Ia constraints are orthogonal, making this combination of cosmological probes very powerful for investigating the nature of dark energy. Dark Energy so WHAT IS DARK ENERGY? 4 ⌦⇤ 0.7= ⇢⇤ (meV) New physics at the meV scale? ' ) ' Some form of energy density which stays 3(1+w) ⇢ a− const. constant as the Universe expands: ⇤ / ⇠ at what scales do we expect new physics? Mweak~TeV, MPlanck~1022 GeV 123 4 60 4 ⇢ 10− M ⇢ 10− M ⇤ ⇠ Planck ⇤ ⇠ weak the “WRONGEST” estimate of particle physics (and biggest hierarchy problem...) SO WHAT? - maybe anthropic principle (we could only live in universes with small Λ) - maybe quantum gravity... A. De Simone 6 Evidences for Dark Matter Dark Matter Energy budget of the Universe Ordinary Matter Dark Energy 2 ⇢DM 3H 5 2 3 ⌦DM ⇢c 1.05 10− h GeV cm− ⌘ ⇢c ⌘ 8⇡GN ' ⇥ H0 2 ⇢DM h 1 1 0.67 ⌦DMh = =0.1196 0.0031 ⌘ 100 km s− Mpc− ' 2 ⇢c/h ±(Planck Coll.) Observational Evidences for Dark Matter: • Galaxy clusters • Galaxies • Cosmology (CMB and Large Scale Structure formation) Firmly established, but only gravitational interactions are probed A. De Simone 7 Dark Matter in Galaxy Clusters F. Zwicky (1933) measured proper motion of galaxies in Coma cluster (~1000 galaxies within radius ~ 1 Mpc) Virial Theorem: V +2 K =0 h i h i N 2 m2 average potential en. due to N2/2 V = G h i h i − 2 N R pairs of galaxies mv2 K = N h i average kinetic en. due to N galaxies h i 2 2R v2 M M 1933AcHPh...6..110Z Total mass M = N m h i = 300h h i⇠ GN ) L ⇠ L “should this be true, this surprising result 1933AcHPh...6..110Z would show that dark matter is of much greater density than luminous matter” Most of the matter is NOT LUMINOUS A. De Simone 8 Dark Matter in Galaxy Clusters - X-ray observations most ordinary mass in clusters is hot gas, emitting X-rays Pressure is due to electrons: P (r)=ne(r)Te(r) Law of hydrostatic equilibrium: accel dV G M(R) G M(R) dP = dm = ⇢ (R) N = ⇢ (R) N dR − Area − b Area R2 − b R2 R where M(R)=4⇡ ⇢(r)r2dr ⇢b(r)=µne(r)mb Z0 dP G M(R) = µn (R)m N dR − e b R2 EXTRACT THE MASS from X-ray luminosity from temperature maps and spatial distributions More matter than just baryons! A. De Simone 9 Dark Matter in Galaxy Clusters - Gravitational Lensing General Relativity at work! Abell NGC 2218 - “Bullet” Cluster Two colliding clusters of galaxies A. De Simone 10 1991MNRAS.249..523B Dark Matter in Galaxies Rotation curves G M(R) R v(R)= N ,M(R)=4⇡ ⇢(r)r2dr R r Z0 1/2 Expectation: v(r) R− at large R / Observations: v(r) const. at large R ' More matter than visible! and distributed differently (in the halo) halo disk 2 MDM R requires ⇢DM 1/r / / gas A. De Simone 11 Dark Matter in Cosmology CMB Recall that CMB temperature maps give accurate information about cosmological parameters (H0, Ωtot, ΩB etc...) (see 1st lecture) Formation of Large-Scale Structures different DM types give different scenarios: Hot DM ``top-down'': large structures fragment into smaller pieces. Cold DM ``bottom-up'': smaller objects merge into bigger structures hierarchically. cosmological observations (CMB and galaxy observations) + numerical simulations exclude HDM. A. De Simone 12 Problems of Cold DM (?) “cusp-core problem” 1 1.5 Numerical simulations predict “cuspy” density profiles ⇢ r − ÷ − (small r) ⇠ Observations favor more constant densities “missing satellite problem” Numerical simulations predict large number (100-1000) of sub-haloes Only ~ 10 observed NOT CLEAR SITUATION Some propose Wark Dark Matter It may simply be that Numerical Simulations are not accurate enough (baryons not included) and small sub-haloes are invisible. A. De Simone 13 Alternatives to Dark Matter (?) explanation of flat rotation curves with modification of gravity (rather than DM)? MOND (MOdified Newtonian Dynamics) GN M(R)m ma (a>a ) 11 2 = 2 ⇤ (critical acceleration a 10 − m/s ) R2 ma /a (a<a ) ⇤ ⇠ ⇢ ⇤ ⇤ 1/2 [GN M(R)/R] (Newton) v(R)= 1/4 [GN M(R)a ] (MOND) ⇢ ⇤ (flat) MOND IS FALSE! 1. evidence for DM is much more than rotation curves 2. bullet cluster contradicts MOND 3. some galaxies do not have a flat rotation curve A. De Simone 14 Key Properties of Particle DM • stable (or with lifetime at least longer than the age of the Universe) • no electric charge, no color charge • non-collisional • not hot • DM is in a fluid limit (not a collection of discrete compact objects) MAssive Compact Halo Objects (MACHOs) are astrophysical objects with macroscopic mass (large planets or small dead stars). MACHOs searches exclude 7 10− M . M . 10M (using gravitational lensing) A small window for primordial black holes still open 13 7 10− M . M . 10− M A. De Simone 15 Key Properties of Particle DM • DM is classical (non-relativistic) today confined on galactic scales ~ 1 kpc, with densities ~ 1 GeV cm-3 and velocities ~ 100 km/s. For bosons: De Broglie wavelength λ = h/p must be less than 1 kpc h 2⇡ 1 14 22 m (2 10− cm GeV) 10− eV & 1 3 21 1kpc v ' 10− c 3 10 cm · · ' · 3 · (v=100 km/s) For fermions: DM quantum occupation number must be <1 (Pauli) 3 1/4 ⇢(r ) 3 m h ⇢(r ) λ . 1= ⇢(r ) . = m & 1keV m ) λ3 ) v3 ' (Gunn-Tremaine bound) 3 4 ( ⇢ ( r )=0 . 4 GeV cm − (0 . 04 eV) ) ' A. De Simone 16 Candidates for Dark Matter (an incomplete list) WIMP non-WIMP neutralino axion minimal DM gravitino heavy neutrino sterile neutrino inert Higgs doublet techni-baryon, LKP topological defects LTP primordial black holes ... ... WIMP = Weakly Interacting Massive Particle (or... the “Holy Grail” of DM physics) A. De Simone 17 Candidates for Dark Matter (an incomplete list) WIMP non-WIMP neutralino axion minimal DM gravitino heavy neutrino sterile neutrino inert Higgs doublet techni-baryon, LKP topological defects LTP primordial black holes ... ... WIMP = Weakly Interacting Massive Particle (or... the “Holy Grail” of DM physics) A. De Simone 18 Thermal Production28 Chapter 4. What is Dark Matter? Assume: 102 • X is stable 108 • X is in thermal eq. at T >> mX 104 eq QUALITATIVE ANALYSIS Y Y 6 Y - initially, in thermal equilibrium 10 109 χχ SM SM abundance 8 $ 10 equilibrium DM - Universe cools, less and less X Y smaller ⇤ of Out / 10 10 ⇥ χχ SM SM Y bigger ⇤ ! Yeq - Universe expands, reaction slows down 1012 1010 1 2 ⇥ 3 2 3 and X abundance “freezes out” of the 10 1 10 10 10 1 10 10 10 expansion z ⇥ M T z ⇥ M T / χχ / SM SM ⇤ ! Figure 4.4: Sample of DM freeze-out. Left:sampleoftheevolutionoftheDMabundanceY = n/s as function of z = T/M. Right:sampleoftheevolutionofthenon-equilibriumabundance Y Yeq,comparedtotheanalyticapproximationofeq.(4.48)(dashed,validforz zf )andof − ⇧ A.
Load more

Recommended publications
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • 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 →
    [Show full text]
  • Analytical Properties of Einasto Dark Matter Haloes
    A&A 540, A70 (2012) Astronomy DOI: 10.1051/0004-6361/201118543 & c ESO 2012 Astrophysics Analytical properties of Einasto dark matter haloes E. Retana-Montenegro1 , E. Van Hese2, G. Gentile2,M.Baes2, and F. Frutos-Alfaro1 1 Escuela de Física, Universidad de Costa Rica, 11501 San Pedro, Costa Rica e-mail: [email protected] 2 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281-S9, 9000 Gent, Belgium e-mail: [email protected] Received 29 November 2011 / Accepted 19 January 2012 ABSTRACT Recent high-resolution N-body CDM simulations indicate that nonsingular three-parameter models such as the Einasto profile perform better than the singular two-parameter models, e.g. the Navarro, Frenk and White, in fitting a wide range of dark matter haloes. While many of the basic properties of the Einasto profile have been discussed in previous studies, a number of analytical properties are still not investigated. In particular, a general analytical formula for the surface density, an important quantity that defines the lensing properties of a dark matter halo, is still lacking to date. To this aim, we used a Mellin integral transform formalism to derive a closed expression for the Einasto surface density and related properties in terms of the Fox H and Meijer G functions, which can be written as series expansions. This enables arbitrary-precision calculations of the surface density and the lensing properties of realistic dark matter halo models. Furthermore, we compared the Sérsic and Einasto surface mass densities and found differences between them, which implies that the lensing properties for both profiles differ.
    [Show full text]
  • Cosmology Meets Condensed Matter
    Cosmology Meets Condensed Matter Mark N. Brook Thesis submitted to the University of Nottingham for the degree of Doctor of Philosophy. July 2010 The Feynman Problem-Solving Algorithm: 1. Write down the problem 2. Think very hard 3. Write down the answer – R. P. Feynman att. to M. Gell-Mann Supervisor: Prof. Peter Coles Examiners: Prof. Ed Copeland Prof. Ray Rivers Abstract This thesis is concerned with the interface of cosmology and condensed matter. Although at either end of the scale spectrum, the two disciplines have more in common than one might think. Condensed matter theorists and high-energy field theorists study, usually independently, phenomena embedded in the structure of a quantum field theory. It would appear at first glance that these phenomena are disjoint, and this has often led to the two fields developing their own procedures and strategies, and adopting their own nomenclature. We will look at some concepts that have helped bridge the gap between the two sub- jects, enabling progress in both, before incorporating condensed matter techniques to our own cosmological model. By considering ideas from cosmological high-energy field theory, we then critically examine other models of astrophysical condensed mat- ter phenomena. In Chapter 1, we introduce the current cosmological paradigm, and present a somewhat historical overview of the interplay between cosmology and condensed matter. Many concepts are introduced here that later chapters will follow up on, and we give some examples in which condensed matter physics has had a very real effect on informing cosmology. We also reflect on the most recent incarnations of the condensed matter / cosmology interplay, and the future of these developments.
    [Show full text]
  • Arxiv:1705.02358V2 [Hep-Ph] 24 Nov 2017
    Dark Matter Self-interactions and Small Scale Structure Sean Tulin1, ∗ and Hai-Bo Yu2, y 1Department of Physics and Astronomy, York University, Toronto, Ontario M3J 1P3, Canada 2Department of Physics and Astronomy, University of California, Riverside, California 92521, USA (Dated: November 28, 2017) Abstract We review theories of dark matter (DM) beyond the collisionless paradigm, known as self-interacting dark matter (SIDM), and their observable implications for astrophysical structure in the Universe. Self- interactions are motivated, in part, due to the potential to explain long-standing (and more recent) small scale structure observations that are in tension with collisionless cold DM (CDM) predictions. Simple particle physics models for SIDM can provide a universal explanation for these observations across a wide range of mass scales spanning dwarf galaxies, low and high surface brightness spiral galaxies, and clusters of galaxies. At the same time, SIDM leaves intact the success of ΛCDM cosmology on large scales. This report covers the following topics: (1) small scale structure issues, including the core-cusp problem, the diversity problem for rotation curves, the missing satellites problem, and the too-big-to-fail problem, as well as recent progress in hydrodynamical simulations of galaxy formation; (2) N-body simulations for SIDM, including implications for density profiles, halo shapes, substructure, and the interplay between baryons and self- interactions; (3) semi-analytic Jeans-based methods that provide a complementary approach for connecting particle models with observations; (4) merging systems, such as cluster mergers (e.g., the Bullet Cluster) and minor infalls, along with recent simulation results for mergers; (5) particle physics models, including light mediator models and composite DM models; and (6) complementary probes for SIDM, including indirect and direct detection experiments, particle collider searches, and cosmological observations.
    [Show full text]
  • Imprint of Pressure on Characteristic Dark Matter Profiles
    galaxies Article Imprint of Pressure on Characteristic Dark Matter Profiles: The Case of ESO0140040 Kuantay Boshkayev 1,2,3,4,* , Talgar Konysbayev 1,4,5,* , Ergali Kurmanov 5,* , Orlando Luongo 1,2,6 and Marco Muccino 1,2,7 1 National Nanotechnology Laboratory of Open Type (NNLOT), Al-Farabi Kazakh National University, Al-Farabi av. 71, Almaty 050040, Kazakhstan; [email protected] (O.L.); [email protected] (M.M.) 2 Department of Theoretical and Nuclear Physics, Al-Farabi Kazakh National University, Al-Farabi ave. 71, Almaty 050040, Kazakhstan 3 Department of Physics, Nazarbayev University, Kabanbay Batyr 53, Nur-Sultan 010000, Kazakhstan 4 Fesenkov Astrophysical Institute, Observatory 23, Almaty 050020, Kazakhstan 5 Department of Solid State Physics and Nonlinear Physics, Al-Farabi Kazakh National University, Al-Farabi ave. 71, Almaty 050040, Kazakhstan 6 Scuola di Scienze e Tecnologie, Università di Camerino, 62032 Camerino, Italy 7 Istituto Nazionale di Fisica Nucleare (INFN), Laboratori Nazionali di Frascati, 00044 Frascati, Italy * Correspondence: [email protected] (K.B.); [email protected] (T.K.); [email protected] (E.K.) Received: 17 September 2020; Accepted: 18 October 2020; Published: 22 October 2020 Abstract: We investigate the dark matter distribution in the spiral galaxy ESO0140040, employing the most widely used density profiles: the pseudo-isothermal, exponential sphere, Burkert, Navarro-Frenk-White, Moore and Einasto profiles. We infer the model parameters and estimate the total dark matter content from the rotation curve data. For simplicity, we assume that dark matter distribution is spherically symmetric without accounting for the complex structure of the galaxy. Our predictions are compared with previous results and the fitted parameters are statistically confronted for each profile.
    [Show full text]
  • Dark Matter Investigation by DAMA at Gran Sasso
    Dark Matter investigation by DAMA at Gran Sasso R. BERNABEI, P. BELLI, S. d’ANGELO, A. DI MARCO and F. MONTECCHIA∗ Dip. di Fisica, Univ. “Tor Vergata”, I-00133 Rome, Italy and INFN, sez. Roma “Tor Vergata”, I-00133 Rome, Italy F. CAPPELLA, A. d’ANGELO and A. INCICCHITTI Dip. di Fisica, Univ. di Roma “La Sapienza”, I-00185 Rome, Italy and INFN, sez. Roma, I-00185 Rome, Italy V. CARACCIOLO, S. CASTELLANO and R. CERULLI Laboratori Nazionali del Gran Sasso, INFN, Assergi, Italy C.J. DAI, H.L. HE, X.H. MA, X.D. SHENG, R.G. WANG and Z.P. YE† Institute of High Energy Physics, CAS, 19B Yuquanlu Road, Shijingshan District, Beijing 100049, China Experimental observations and theoretical arguments at Galaxy and larger scales have suggested that a large fraction of the Universe is composed by Dark Matter particles. This has motivated the DAMA experimental efforts to investigate the presence of such particles in the galactic halo by exploiting a model independent signature and very highly radiopure set-ups deep underground. Few introductory arguments are summarized before presenting a review of the present model independent positive results obtained by the DAMA/NaI and DAMA/LIBRA set-ups at the Gran Sasso National Laboratory of the INFN. Implications and model dependent comparisons with other different kinds of results will be shortly addressed. Some arguments put forward in literature will be arXiv:1306.1411v2 [astro-ph.GA] 12 Jun 2013 confuted. Keywords: Dark Matter; direct detection; annual modulation. PACS numbers: 95.35.+d; 29.40.Mc 1. The Dark component of the Universe Since the publication (1687) of the “Philosophiae Naturalis Principia Mathematica” by Isaac Newton, a large effort has been made to explain the motion of the astrophysical objects by means of the universal gravitation law.
    [Show full text]
  • Presentación De Powerpoint
    Theoretical aspects of Dark Matter search Carlos Muñoz RICAP-13, Roma, May 22-24 Evidence for DM Evidence for dark matter since 1930’s: COBE, WMAP, Planck Carlos Muñoz Dark Matter 2 UAM & IFT Last results from the Planck satellite, 2 W DM h 0.12 2 W b h 0.022 2 W DE h 0.31 confirm that about 85% of the matter in the Universe is dark Carlos Muñoz Dark Matter 3 UAM & IFT PARTICLE CANDIDATES The only possible candidate for DM within the Standard Model of Particle Physics, the neutrino, is excluded 2 Its mass seems to be too small, m ~ eV to account for W DM h 0.1 This kind of (hot) DM cannot reproduce correctly the observed structure in the Universe; galaxies would be too young This is a clear indication that we need to go beyond the standard model of particle physics Carlos Muñoz Dark Matter 4 UAM & IFT We need a new particle with the following properties: Stable or long-lived Produced after the Big Bang and still present today Neutral Otherwise it would bind to nuclei and would be excluded from unsuccessful searches for exotic heavy isotopes 2 Reproduce the observed amount of dark matter W DM h 0.1 A stable and neutral WIMP is a good candidate for DM, since it is able to reproduce this number WIMP f In the early Universe, at some temperature the annihilation rate of DM WIMPs dropped below the expansion rate WIMP f and their density has been 2 3 x 10-27 cm3 s-1 the same since then, with: W WIMP h 0.1 sannv sann = sweak Carlos Muñoz Dark Matter 5 UAM & IFT DIRECT DETECTION through elastic scattering with nuclei in a detector is possible DAMA/LIBRA photo 3 r0 ~ 0.3 GeV/cm v0 ~ 220 km/s J ~ r0 v0 /mWIMP 4 2 ~ 10 WIMPs /cm s -8 -6 For sWIMP-nucleon 10 -10 pb a material with nuclei composed of about 100 nucleons, i.e.
    [Show full text]
  • Extension of Minimal Fermionic Dark Matter Model: a Study with Two Higgs Doublet Model
    Eur. Phys. J. C (2015) 75:364 DOI 10.1140/epjc/s10052-015-3589-0 Regular Article - Theoretical Physics Extension of minimal fermionic dark matter model: a study with two Higgs doublet model Amit Dutta Banika, Debasish Majumdarb Astroparticle Physics and Cosmology Division, Saha Institute of Nuclear Physics, 1/AF Bidhannagar, Kolkata 700064, India Received: 28 May 2015 / Accepted: 30 July 2015 / Published online: 12 August 2015 © The Author(s) 2015. This article is published with open access at Springerlink.com Abstract We explore a fermionic dark matter model with a experiments provide stringent bounds on DM-nucleon scat- possible extension of Standard Model of particle physics into tering cross-section for different Dark matter masses. Dark two Higgs doublet model. Higgs doublets couple to the sin- matter particles can also be trapped in a highly gravitating glet fermionic dark matter through a non-renormalisable cou- astrophysical objects and can eventually undergo annihila- pling providing a new physics scale. We explore the viability tion to produce γ ’s or fermion anti-fermion pairs. Such events of such dark matter candidate and constrain the model param- should show up as excesses over the expected abundance of eter space by collider serach, relic density of DM, direct these particles in the cosmos (for instance in cosmic rays). detection measurements of DM-nucleon scattering cross- Indirect searches of dark matter by detecting their annihila- section and with the experimentally obtained results from tion products can be realised by looking for these excesses in indirect search of dark matter. the Universe. In fact the satellite borne experiments such as Fermi-Lat [9] (also known as Fermi gamma-ray space tele- scope or FGST), Alpha Magnetic Spectrometer AMS [10]on 1 Introduction board International Space Station (ISS) or the earth bound experiment H.E.S.S.
    [Show full text]
  • Analytical Properties of Einasto Dark Matter Haloes
    A&A 540, A70 (2012) Astronomy DOI: 10.1051/0004-6361/201118543 & c ESO 2012 ! Astrophysics Analytical properties of Einasto dark matter haloes E. Retana-Montenegro1 ,E.VanHese2,G.Gentile2,M.Baes2,andF.Frutos-Alfaro1 1 Escuela de Física, Universidad de Costa Rica, 11501 San Pedro, Costa Rica e-mail: [email protected] 2 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281-S9, 9000 Gent, Belgium e-mail: [email protected] Received 29 November 2011 / Accepted 19 January 2012 ABSTRACT Recent high-resolution N-body CDM simulations indicate that nonsingular three-parameter models such as the Einasto profile perform better than the singular two-parameter models, e.g. the Navarro, Frenk and White, in fitting a wide range of dark matter haloes. While many of the basic properties of the Einasto profile have been discussed in previous studies, a number of analytical properties are still not investigated. In particular, a general analytical formula for the surface density, an important quantity that defines the lensing properties of a dark matter halo, is still lacking to date. To this aim, we used a Mellin integral transform formalism to derive a closed expression for the Einasto surface density and related properties in terms of the Fox H and Meijer G functions, which can be written as series expansions. This enables arbitrary-precision calculations of the surface density and the lensing properties of realistic dark matter halo models. Furthermore, we compared the Sérsic and Einasto surface mass densities and found differences between them, which implies that the lensing properties for both profiles differ.
    [Show full text]
  • Evolution of Galactic Star Formation in Galaxy Clusters and Post-Starburst Galaxies
    Evolution of galactic star formation in galaxy clusters and post-starburst galaxies Marcel Lotz M¨unchen2020 Evolution of galactic star formation in galaxy clusters and post-starburst galaxies Marcel Lotz Dissertation an der Fakult¨atf¨urPhysik der Ludwig{Maximilians{Universit¨at M¨unchen vorgelegt von Marcel Lotz aus Frankfurt am Main M¨unchen, den 16. November 2020 Erstgutachter: Prof. Dr. Andreas Burkert Zweitgutachter: Prof. Dr. Til Birnstiel Tag der m¨undlichen Pr¨ufung:8. Januar 2021 Contents Zusammenfassung viii 1 Introduction 1 1.1 A brief history of astronomy . .1 1.2 Cosmology . .5 1.2.1 The Cosmological Principle and our expanding Universe . .6 1.2.2 Dark matter, dark energy and the ΛCDM cosmological model . .9 1.2.3 Chronology of the Universe . 13 1.3 Galaxy properties . 16 1.3.1 Morphology . 17 1.3.2 Colour . 20 1.4 Galaxy evolution . 22 1.4.1 Galaxy formation . 22 1.4.2 Star formation and feedback . 24 1.4.3 Mergers . 25 1.4.4 Galaxy clusters and environmental quenching . 26 1.4.5 Post-starburst galaxies . 29 2 State-of-the-art simulations 33 2.1 Brief introduction to numerical simulations . 33 2.1.1 Treatment of the gravitational force . 34 2.1.2 Varying hydrodynamic approaches . 35 2.2 Magneticum Pathfinder simulations . 39 2.2.1 Smoothed particle hydrodynamics . 39 2.2.2 Details of the Magneticum Pathfinder simulations . 40 3 Gone after one orbit: How cluster environments quench galaxies 45 3.1 Data sample . 46 3.1.1 Observational comparison with CLASH . 46 3.2 Velocity-anisotropy Profiles .
    [Show full text]