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Arxiv:1803.02804V1 [Hep-Ph] 7 Mar 2018 It Must Have Some Rather Specific Characteristics
FERMILAB-PUB-18-066-A Severely Constraining Dark Matter Interpretations of the 21-cm Anomaly Asher Berlina,∗ Dan Hooperb;c;d,y Gordan Krnjaicb,z and Samuel D. McDermottbx aSLAC National Accelerator Laboratory, Menlo Park CA, 94025, USA bFermi National Accelerator Laboratory, Theoretical Astrophysics Group, Batavia, IL, USA cUniversity of Chicago, Kavli Institute for Cosmological Physics, Chicago IL, USA and dUniversity of Chicago, Department of Astronomy and Astrophysics, Chicago IL, USA (Dated: March 8, 2018) The EDGES Collaboration has recently reported the detection of a stronger-than-expected ab- sorption feature in the global 21-cm spectrum, centered at a frequency corresponding to a redshift of z ∼ 17. This observation has been interpreted as evidence that the gas was cooled during this era as a result of scattering with dark matter. In this study, we explore this possibility, applying constraints from the cosmic microwave background, light element abundances, Supernova 1987A, and a variety of laboratory experiments. After taking these constraints into account, we find that the vast majority of the parameter space capable of generating the observed 21-cm signal is ruled out. The only range of models that remains viable is that in which a small fraction, ∼ 0:3 − 2%, of the dark matter consists of particles with a mass of ∼ 10 − 80 MeV and which couple to the photon through a small electric charge, ∼ 10−6 −10−4. Furthermore, in order to avoid being overproduced in the early universe, such models must be supplemented with an additional depletion mechanism, such as annihilations through a Lµ − Lτ gauge boson or annihilations to a pair of rapidly decaying hidden sector scalars. -
Correction: Corrigendum: the Superluminous Transient ASASSN
LETTERS PUBLISHED: 12 DECEMBER 2016 | VOLUME: 1 | ARTICLE NUMBER: 0002 The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole G. Leloudas1,2*, M. Fraser3, N. C. Stone4, S. van Velzen5, P. G. Jonker6,7, I. Arcavi8,9, C. Fremling10, J. R. Maund11, S. J. Smartt12, T. Krühler13, J. C. A. Miller-Jones14, P. M. Vreeswijk1, A. Gal-Yam1, P. A. Mazzali15,16, A. De Cia17, D. A. Howell8,18, C. Inserra12, F. Patat17, A. de Ugarte Postigo2,19, O. Yaron1, C. Ashall15, I. Bar1, H. Campbell3,20, T.-W. Chen13, M. Childress21, N. Elias-Rosa22, J. Harmanen23, G. Hosseinzadeh8,18, J. Johansson1, T. Kangas23, E. Kankare12, S. Kim24, H. Kuncarayakti25,26, J. Lyman27, M. R. Magee12, K. Maguire12, D. Malesani2, S. Mattila3,23,28, C. V. McCully8,18, M. Nicholl29, S. Prentice15, C. Romero-Cañizales24,25, S. Schulze24,25, K. W. Smith12, J. Sollerman10, M. Sullivan21, B. E. Tucker30,31, S. Valenti32, J. C. Wheeler33 and D. R. Young12 8 12,13 When a star passes within the tidal radius of a supermassive has a mass >10 M⊙ , a star with the same mass as the Sun black hole, it will be torn apart1. For a star with the mass of the could be disrupted outside the event horizon if the black hole 8 14 Sun (M⊙) and a non-spinning black hole with a mass <10 M⊙, were spinning rapidly . The rapid spin and high black hole the tidal radius lies outside the black hole event horizon2 and mass can explain the high luminosity of this event. -
Perrett RTA.Pdf
The Astronomical Journal, 140:518–532, 2010 August doi:10.1088/0004-6256/140/2/518 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. REAL-TIME ANALYSIS AND SELECTION BIASES IN THE SUPERNOVA LEGACY SURVEY∗ K. Perrett1,2, D. Balam3, M. Sullivan4, C. Pritchet5, A. Conley1,6, R. Carlberg1,P.Astier7, C. Balland7,S.Basa8, D. Fouchez9,J.Guy7, D. Hardin7,I.M.Hook3,10, D. A. Howell11,12,R.Pain7, and N. Regnault7 1 Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON, M5S 3H4, Canada; [email protected] 2 Network Information Operations, DRDC Ottawa, 3701 Carling Avenue, Ottawa, ON K1A 0Z4, Canada 3 Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada 4 Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH, UK; [email protected] 5 Department of Physics & Astronomy, University of Victoria, P.O. Box 3055, Stn CSC, Victoria, BC V8W 3P6, Canada 6 Center for Astrophysics and Space Astronomy, University of Colorado, 593 UCB, Boulder, CO 80309-0593, USA 7 LPNHE, CNRS-IN2P3 and University of Paris VI & VII, 75005 Paris, France 8 Laboratoire d’Astrophysique de Marseille, Poledel’ˆ Etoile´ Site de Chateau-Gombert,ˆ 38, rue Fred´ eric´ Joliot-Curie, 13388 Marseille cedex 13, France 9 CPPM, CNRS-IN2P3 and University Aix Marseille II, Case 907, 13288 Marseille cedex 9, France 10 INAF, Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy 11 Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA 12 Department of Physics, University of California, Santa Barbara, Broida Hall, Mail Code 9530, Santa Barbara, CA 93106-9530, USA Received 2010 February 17; accepted 2010 June 4; published 2010 July 1 ABSTRACT The Supernova Legacy Survey (SNLS) has produced a high-quality, homogeneous sample of Type Ia supernovae (SNe Ia) out to redshifts greater than z = 1. -
Publications RENOIR – 24 Sep 2021 Article
Publications RENOIR { 24 Sep 2021 article 2021 1. The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: one thousand multi-tracer mock catalogues with redshift evolution and systematics for galaxies and quasars of the final data release, C. Zhao et al., Mon. Not. Roy. Astron. Soc 503 (2021) 1149-1173 2. Euclid preparation: XI. Mean redshift determination from galaxy redshift probabilities for cosmic shear tomography, O. Ilbert et al., Euclid Collaboration, Astron. Astrophys. 647 (2021) A117 2020 1. Improving baryon acoustic oscillation measurement with the combination of cosmic voids and galaxies, C. Zhao et al., SDSS Collaboration, Mon. Not. Roy. Astron. Soc 491 (2020) 4554-4572 2. Strong Dependence of Type Ia Supernova Standardization on the Local Specific Star Formation Rate, M. Rigault et al., Nearby Supernova Factory Collaboration, Astron. Astrophys. 644 (2020) A176 3. High-precision Monte-Carlo modelling of galaxy distribution, P. Baratta et al., Astron. Astrophys. 633 (2020) A26 4. Constraints on the growth of structure around cosmic voids in eBOSS DR14, A. J. Hawken et al., J. Cosmol. Astropart. P 2006 (2020) 012 5. SUGAR: An improved empirical model of Type Ia Supernovae based on spectral features, P.-F. L´eget et al., Nearby Supernova Factory Collaboration, Astron. Astrophys. 636 (2020) A46 6. Euclid: Reconstruction of Weak Lensing mass maps for non- Gaussianity studies, S. Pires et al., Euclid Collaboration, Astron. Astrophys. 638 (2020) A141 7. Euclid preparation: VII. Forecast validation for Euclid cosmological probes, A. Blanchard et al., Euclid Collaboration, Astron. Astrophys. 642 (2020) A191 8. Euclid preparation: VI. Verifying the Performance of Cosmic Shear Experiments, P. -
Arxiv:1707.01004V1 [Astro-Ph.CO] 4 Jul 2017
July 5, 2017 0:15 WSPC/INSTRUCTION FILE coc2ijmpe International Journal of Modern Physics E c World Scientific Publishing Company Primordial Nucleosynthesis Alain Coc Centre de Sciences Nucl´eaires et de Sciences de la Mati`ere (CSNSM), CNRS/IN2P3, Univ. Paris-Sud, Universit´eParis–Saclay, Bˆatiment 104, F–91405 Orsay Campus, France [email protected] Elisabeth Vangioni Institut d’Astrophysique de Paris, UMR-7095 du CNRS, Universit´ePierre et Marie Curie, 98 bis bd Arago, 75014 Paris (France), Sorbonne Universit´es, Institut Lagrange de Paris, 98 bis bd Arago, 75014 Paris (France) [email protected] Received July 5, 2017 Revised Day Month Year Primordial nucleosynthesis, or big bang nucleosynthesis (BBN), is one of the three evi- dences for the big bang model, together with the expansion of the universe and the Cos- mic Microwave Background. There is a good global agreement over a range of nine orders of magnitude between abundances of 4He, D, 3He and 7Li deduced from observations, and calculated in primordial nucleosynthesis. However, there remains a yet–unexplained discrepancy of a factor ≈3, between the calculated and observed lithium primordial abundances, that has not been reduced, neither by recent nuclear physics experiments, nor by new observations. The precision in deuterium observations in cosmological clouds has recently improved dramatically, so that nuclear cross sections involved in deuterium BBN need to be known with similar precision. We will shortly discuss nuclear aspects re- lated to BBN of Li and D, BBN with non-standard neutron sources, and finally, improved sensitivity studies using Monte Carlo that can be used in other sites of nucleosynthesis. -
The Reionization of Cosmic Hydrogen by the First Galaxies Abstract 1
David Goodstein’s Cosmology Book The Reionization of Cosmic Hydrogen by the First Galaxies Abraham Loeb Department of Astronomy, Harvard University, 60 Garden St., Cambridge MA, 02138 Abstract Cosmology is by now a mature experimental science. We are privileged to live at a time when the story of genesis (how the Universe started and developed) can be critically explored by direct observations. Looking deep into the Universe through powerful telescopes, we can see images of the Universe when it was younger because of the finite time it takes light to travel to us from distant sources. Existing data sets include an image of the Universe when it was 0.4 million years old (in the form of the cosmic microwave background), as well as images of individual galaxies when the Universe was older than a billion years. But there is a serious challenge: in between these two epochs was a period when the Universe was dark, stars had not yet formed, and the cosmic microwave background no longer traced the distribution of matter. And this is precisely the most interesting period, when the primordial soup evolved into the rich zoo of objects we now see. The observers are moving ahead along several fronts. The first involves the construction of large infrared telescopes on the ground and in space, that will provide us with new photos of the first galaxies. Current plans include ground-based telescopes which are 24-42 meter in diameter, and NASA’s successor to the Hubble Space Telescope, called the James Webb Space Telescope. In addition, several observational groups around the globe are constructing radio arrays that will be capable of mapping the three-dimensional distribution of cosmic hydrogen in the infant Universe. -
DARK AGES of the Universe the DARK AGES of the Universe Astronomers Are Trying to fill in the Blank Pages in Our Photo Album of the Infant Universe by Abraham Loeb
THE DARK AGES of the Universe THE DARK AGES of the Universe Astronomers are trying to fill in the blank pages in our photo album of the infant universe By Abraham Loeb W hen I look up into the sky at night, I often wonder whether we humans are too preoccupied with ourselves. There is much more to the universe than meets the eye on earth. As an astrophysicist I have the privilege of being paid to think about it, and it puts things in perspective for me. There are things that I would otherwise be bothered by—my own death, for example. Everyone will die sometime, but when I see the universe as a whole, it gives me a sense of longevity. I do not care so much about myself as I would otherwise, because of the big picture. Cosmologists are addressing some of the fundamental questions that people attempted to resolve over the centuries through philosophical thinking, but we are doing so based on systematic observation and a quantitative methodology. Perhaps the greatest triumph of the past century has been a model of the uni- verse that is supported by a large body of data. The value of such a model to our society is sometimes underappreciated. When I open the daily newspaper as part of my morning routine, I often see lengthy de- scriptions of conflicts between people about borders, possessions or liberties. Today’s news is often forgotten a few days later. But when one opens ancient texts that have appealed to a broad audience over a longer period of time, such as the Bible, what does one often find in the opening chap- ter? A discussion of how the constituents of the universe—light, stars, life—were created. -
Euclid: Superluminous Supernovae in the Deep Survey? C
A&A 609, A83 (2018) Astronomy DOI: 10.1051/0004-6361/201731758 & c ESO 2018 Astrophysics Euclid: Superluminous supernovae in the Deep Survey? C. Inserra1; 2, R. C. Nichol3, D. Scovacricchi3, J. Amiaux4, M. Brescia5, C. Burigana6; 7; 8, E. Cappellaro9, C. S. Carvalho30, S. Cavuoti5; 11; 12, V. Conforti13, J.-C. Cuillandre4; 14; 15, A. da Silva10; 16, A. De Rosa13, M. Della Valle5; 17, J. Dinis10; 16, E. Franceschi13, I. Hook18, P. Hudelot19, K. Jahnke20, T. Kitching21, H. Kurki-Suonio22, I. Lloro23, G. Longo11; 12, E. Maiorano13, M. Maris24, J. D. Rhodes25, R. Scaramella26, S. J. Smartt2, M. Sullivan1, C. Tao27; 28, R. Toledo-Moreo29, I. Tereno16; 30, M. Trifoglio13, and L. Valenziano13 (Affiliations can be found after the references) Received 11 August 2017 / Accepted 3 October 2017 ABSTRACT Context. In the last decade, astronomers have found a new type of supernova called superluminous supernovae (SLSNe) due to their high peak luminosity and long light-curves. These hydrogen-free explosions (SLSNe-I) can be seen to z ∼ 4 and therefore, offer the possibility of probing the distant Universe. Aims. We aim to investigate the possibility of detecting SLSNe-I using ESA’s Euclid satellite, scheduled for launch in 2020. In particular, we study the Euclid Deep Survey (EDS) which will provide a unique combination of area, depth and cadence over the mission. Methods. We estimated the redshift distribution of Euclid SLSNe-I using the latest information on their rates and spectral energy distribution, as well as known Euclid instrument and survey parameters, including the cadence and depth of the EDS. -
Dermining the Photon Budget of Galaxies During Reionization with Numerical Simulations, and Studying the Impact of Dust Joseph Lewis
Who reionized the Universe ? : dermining the photon budget of galaxies during reionization with numerical simulations, and studying the impact of dust Joseph Lewis To cite this version: Joseph Lewis. Who reionized the Universe ? : dermining the photon budget of galaxies during reioniza- tion with numerical simulations, and studying the impact of dust. Astrophysics [astro-ph]. Université de Strasbourg, 2020. English. NNT : 2020STRAE041. tel-03199136 HAL Id: tel-03199136 https://tel.archives-ouvertes.fr/tel-03199136 Submitted on 15 Apr 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. UNIVERSITÉ DE STRASBOURG ÉCOLE DOCTORALE 182 UMR 7550, Observatoire astronomique de Strasbourg THÈSE présentée par : Joseph Lewis soutenue le : 25 septembre 2020 pour obtenir le grade de : Docteur de l’université de Strasbourg Discipline/ Spécialité : Astrophysique Qui a réionisé l’Univers ? Détermination par la simulation numérique du budget de photons des galaxies pendant l’époque de la Réionisation, et étude de l’impact des poussières THÈSE dirigée par : M. AUBERT Dominique Professeur des universités, Université de Strasbourg RAPPORTEURS : M. GONZALES Mathias Maître de conférences, Université de Paris M. LANGER Mathieu Professeur des universités, Université Paris-Saclay AUTRES MEMBRES DU JURY : M. -
Determining the Redshift of Reionization from the Spectra Of
CORE Metadata, citation and similar papers at core.ac.uk Provided by CERN Document Server Determining the Redshift of Reionization From the Sp ectra of High{Redshift Sources 1;2 1 Zoltan Haiman and Abraham Lo eb ABSTRACT The redshift at which the universe was reionized is currently unknown. We examine the optimal strategy for extracting this redshift, z , from the sp ectra of reion early sources. For a source lo cated at a redshift z beyond but close to reionization, s 32 (1 + z ) < (1 + z ) < (1 + z ), the Gunn{Peterson trough splits into disjoint reion s reion 27 Lyman , , and p ossibly higher Lyman series troughs, with some transmitted ux in b etween these troughs. We show that although the transmitted ux is suppressed considerably by the dense Ly forest after reionization, it is still detectable for suciently bright sources and can b e used to infer the reionization redshift. The Next Generation Space Telescop e will reach the sp ectroscopic sensitivity required for the detection of such sources. Subject headings: cosmology: theory { quasars: absorption lines { galaxies: formation {intergalactic medium { radiative transfer Submitted to The Astrophysical Journal, July 1998 1. Intro duction The standard Big Bang mo del predicts that the primeval plasma recombined and b ecame predominantly neutral as the universe co oled b elow a temp erature of several thousand degrees at 3 a redshift z 10 (Peebles 1968). Indeed, the recent detection of Cosmic Microwave Background (CMB) anisotropies rules out a fully ionized intergalactic medium (IGM) beyond z 300 (Scott, Silk & White 1995). However, the lack of a Gunn{Peterson trough (GP, Gunn & Peterson 1965) in the sp ectra of high{redshift quasars (Schneider, Schmidt & Gunn 1991) and galaxies (Franx et < al. -
Dark Energy and CMB
Dark Energy and CMB Conveners: S. Dodelson and K. Honscheid Topical Conveners: K. Abazajian, J. Carlstrom, D. Huterer, B. Jain, A. Kim, D. Kirkby, A. Lee, N. Padmanabhan, J. Rhodes, D. Weinberg Abstract The American Physical Society's Division of Particles and Fields initiated a long-term planning exercise over 2012-13, with the goal of developing the community's long term aspirations. The sub-group \Dark Energy and CMB" prepared a series of papers explaining and highlighting the physics that will be studied with large galaxy surveys and cosmic microwave background experiments. This paper summarizes the findings of the other papers, all of which have been submitted jointly to the arXiv. arXiv:1309.5386v2 [astro-ph.CO] 24 Sep 2013 2 1 Cosmology and New Physics Maps of the Universe when it was 400,000 years old from observations of the cosmic microwave background and over the last ten billion years from galaxy surveys point to a compelling cosmological model. This model requires a very early epoch of accelerated expansion, inflation, during which the seeds of structure were planted via quantum mechanical fluctuations. These seeds began to grow via gravitational instability during the epoch in which dark matter dominated the energy density of the universe, transforming small perturbations laid down during inflation into nonlinear structures such as million light-year sized clusters, galaxies, stars, planets, and people. Over the past few billion years, we have entered a new phase, during which the expansion of the Universe is accelerating presumably driven by yet another substance, dark energy. Cosmologists have historically turned to fundamental physics to understand the early Universe, successfully explaining phenomena as diverse as the formation of the light elements, the process of electron-positron annihilation, and the production of cosmic neutrinos. -
High Redshift Quasar Hunting with the Dark Energy Survey
High Redshift Quasar Hunting with the Dark Energy Survey Quasars in the Epoch of Reionisation Sophie Reed Supervisors: Richard McMahon, Manda Banerji 1 Why? ★ Theories of black hole formation and evolution z = 6 - 15 z = 2 WORDS Epoch of peak of galaxy Reionization and quasar ★ Metal abundances in the early universe activity ★ Gas distribution and reionisationv z = 20 - 30 z = 6 - 8 Start of z = 1100 first stars Reionization matter-radiation “Population III” decoupling (CMB) 2 Quasar Spectrum at z ~ 6 Spectrum of a z = 5.86 quasar from Venemans et al 2007 Continuum break across rest frame Lyman-alpha (λrest = 121.6nm) gives distinctive colours 3 Quasar Spectrum at z ~ 6 480 nm 640 nm 780 nm 920 nm 990 nm 1252 nm 2147 nm 4 The Dark Energy Survey (DES) First Light September 2012 Very large area when completed: ~5000 deg2, currently have ~2000 deg2 Deep imaging: 10 σ limits for i and z are AB = 23.4 and AB = 23.2 Sophisticated camera, DECam Credit: DES Collaboration 5 DECam Mosaic of 62 2k by 4k CCDs (0.27” pixels) Multi waveband imaging: Visible (400 nm) to Near IR (1050 nm), g, r, i, z and Y bands covered Much more sensitive to red light than SDSS Credit: DES Collaboration 6 DES - SDSS Comparison SDSS was most sensitive to bluer light in the r band DES is most sensitive to redder light in the z band u g r i z Y 7 The VISTA Hemisphere Survey (VHS) Will cover 10,000 deg2 in the infrared when completed VHS-DES (J, H and K) overlaps DES and is deeper VHS-ATLAS (Y, J, H and K) is a shallower survey 8 Currently Known Objects Lots of quasars known