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1. Observational Evidence for Primordial Black Holes: A Positivist Perspective

Author

Carr, Bernard, Clesse, Sebastien, Garcia-Bellido, Juan, Hawkins, Michael, and Kuhnel, Florian

Subjects
High Energy Physics - Phenomenology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We review numerous arguments for primordial black holes (PBHs) based on observational evidence from a variety of lensing, dynamical, accretion and gravitational-wave effects. This represents a shift from the usual emphasis on PBH constraints and provides what we term a positivist perspective. Microlensing observations of stars and quasars suggest that PBHs of around $1\,M_{\odot}$ could provide much of the dark matter in galactic halos, this being allowed by the Large Magellanic Cloud observations if the PBHs have an extended mass function. More generally, providing the mass and dark matter fraction of the PBHs is large enough, the associated Poisson fluctuations could generate the first bound objects at a much earlier epoch than in the standard cosmological scenario. This simultaneously explains the recent detection of high-redshift dwarf galaxies, puzzling correlations of the source-subtracted infrared and X-ray cosmic backgrounds, the size and the mass-to-light ratios of ultra-faint-dwarf galaxies, the dynamical heating of the Galactic disk, and the binary coalescences observed by LIGO/Virgo/KAGRA in a mass range not usually associated with stellar remnants. Even if PBHs provide only a small fraction of the dark matter, they could explain various other observational conundra, and sufficiently large ones could seed the supermassive black holes in galactic nuclei or even early galaxies themselves. We argue that PBHs would naturally have formed around the electroweak, quantum chromodynamics and electron-positron annihilation epochs, when the sound-speed inevitably dips. This leads to an extended PBH mass function with a number of distinct bumps, the most prominent one being at around $1\,M_{\odot}$, and this would allow PBHs to explain much of the evidence in a unified way., Comment: 107 pages, 39 figures, 2 tables, 380 references; invited review for Physics Reports

Published
2023
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2. Cosmic GREA from SMBH growth

Author

Garcia-Bellido, Juan

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

General Relativistic Entropic Acceleration (GREA) gives a general framework in which to study multiple out-of-equilibrium phenomena in the context of general relativity, like the late accelerated expansion of the universe or the formation of galaxies and the large scale structure of the universe. Here we study the consequences of mass accretion onto massive Black Holes. We find that a population of Super Massive Black Holes (SMBH) whose mass grows significantly due to accretion can act as a source of entropic acceleration and constitute a significant part of the present acceleration of the Universe., Comment: 4 pages

Published
2023
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3. Snowmass2021 Cosmic Frontier White Paper: Probing dark matter with small-scale astrophysical observations

Author

Richard Brito, Chakrabarti, Sukanya, Clesse, Sebastien, Dvorkin, Cora, Garcia-Bellido, Juan, Meyers, Joel, Ng, Ken K. Y., Miller, Andrew L., Shandera, Sarah, and Sun, Ling

Subjects
High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The current understanding of dark matter comes largely from measurements of the total matter content in the universe, from the distribution of gravitating matter on very large scales, and from rotation curves and velocity dispersions on sub-galactic scales. However, small-scale structure may well hold the key to unlocking the particle physics of the still-mysterious 85% of matter in the universe. Novel small-scale astrophysical probes of new particles and dark matter will become possible with a large data volume of high-precision measurements enabled by next-generation gravitational-wave detectors and advanced astrometry instruments. Cosmic microwave background and large-scale structure surveys will provide complementary constraints on dark matter models with unique small-scale signatures. We lay out the studies of small-scale structures and compact objects as dark matter probes, and summarize the requirements to achieve the goals., Comment: 43 pages, 7 figures

Published
2022
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4. Constraints on dark matter to dark radiation conversion in the late universe with DES-Y1 and external data

Author

Chen, Angela, Huterer, Dragan, Lee, Sujeong, Ferté, Agnès, Weaverdyck, Noah, Alves, Otavio Alonso, Leonard, C. Danielle, MacCrann, Niall, Raveri, Marco, Porredon, Anna, Di Valentino, Eleonora, Muir, Jessica, Lemos, Pablo, Liddle, Andrew, Blazek, Jonathan, Campos, Andresa, Cawthon, Ross, Choi, Ami, Dodelson, Scott, Elvin-Poole, Jack, Gruen, Daniel, Ross, Ashley, Secco, Lucas F., Sevilla, Ignacio, Sheldon, Erin, Troxel, Michael A., Zuntz, Joe, Abbott, Tim, Aguena, Michel, Allam, Sahar, Annis, James, Avila, Santiago, Bertin, Emmanuel, Bhargava, Sunayana, Bridle, Sarah, Brooks, David, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Costanzi, Matteo, Crocce, Martin, da Costa, Luiz, Pereira, Maria Elidaiana da Silva, Davis, Tamara, Doel, Peter, Eifler, Tim, Ferrero, Ismael, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klaus, Hoyle, Ben, James, David, Jarvis, Mike, Kuehn, Kyler, Lahav, Ofer, Maia, Marcio, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Palmese, Antonella, Paz-Chinchon, Francisco, Malagón, Andrés Plazas, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Smith, Mathew, Suchyta, Eric, Tarle, Gregory, Thomas, Daniel, To, Chun-Hao, Varga, Tamas Norbert, Weller, Jochen, Wilkinson, Reese, UAM. Departamento de Física Teórica, National Science Foundation (US), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, University of Michigan, Duke University, California Institute of Technology, Universidade Estadual Paulista (UNESP), Newcastle Unviersity, Ohio State University, University of Chicago, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), University of Manchester, Stanford University, University College London, Universidade de Lisboa, University of Edinburgh, Perimeter Institute for Theoretical Physics, Observatoire de Sauverny, Carnegie Mellon University, University of Wisconsin-Madison, 382 Via Pueblo Mall, Menlo Park, University of Pennsylvania, Medioambientales y Tecnológicas (CIEMAT), Brookhaven National Laboratory, NSF's National Optical-Infrared Astronomy Research Laboratory, Universidade de São Paulo (USP), LIneA, Fermi National Accelerator Laboratory, Universidad Autonoma de Madrid, Institut d'Astrophysique de Paris, University of Sussex, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Barcelona Institute of Science and Technology, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Queensland, University of Arizona, University of Oslo, Santa Cruz Institute for Particle Physics, Ludwig-Maximilians-Universität, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Texas AandM University, Institució Catalana de Recerca i Estudis Avançats, University of Cambridge, Peyton Hall, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, Chen, Angela, Huterer, Dragan, Lee, Sujeong, Ferté, Agnè, Weaverdyck, Noah, Alonso Alves, Otavio, Leonard, C. Danielle, Maccrann, Niall, Raveri, Marco, Porredon, Anna, Di Valentino, Eleonora, Muir, Jessica, Lemos, Pablo, Liddle, Andrew, Blazek, Jonathan, Campos, Andresa, Cawthon, Ro, Choi, Ami, Dodelson, Scott, Elvin-Poole, Jack, Gruen, Daniel, Ross, Ashley, Secco, Lucas F., Sevilla, Ignacio, Sheldon, Erin, Troxel, Michael A., Zuntz, Joe, Abbott, Tim, Aguena, Michel, Allam, Sahar, Annis, Jame, Avila, Santiago, Bertin, Emmanuel, Bhargava, Sunayana, Bridle, Sarah, Brooks, David, Carnero Rosell, Aurelio, Carrasco Kind, Matia, Carretero, Jorge, Costanzi, Matteo, Crocce, Martin, da Costa, Luiz, Elidaiana da Silva Pereira, Maria, Davis, Tamara, Doel, Peter, Eifler, Tim, Ferrero, Ismael, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klau, Hoyle, Ben, James, David, Jarvis, Mike, Kuehn, Kyler, Lahav, Ofer, Maia, Marcio, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Palmese, Antonella, Paz-Chinchon, Francisco, Plazas Malagón, André, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Smith, Mathew, Suchyta, Eric, Tarle, Gregory, Thomas, Daniel, Chun-Hao, To, Varga, Tamas Norbert, Weller, Jochen, and Wilkinson, Reese

Subjects
matter: power spectrum, Cosmic microwave background, cosmic background radiation: polarization, Astrophysics, power spectrum, 01 natural sciences, Cosmology, hubble constant, High Energy Physics - Phenomenology (hep-ph), Scale Structure, cosmological model: parameter space, Power Spectrum, Dark energy, Astrophysics - Cosmology and Nongalactic Astrophysic, Large-scale structure of the Universe, 010303 astronomy & astrophysics, media_common, Physics, Energy, massive neutrinos, Hubble Constant, tension, Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology, halo-model, statistics, dark energy: density, Dark radiation, symbols, Halo-Model, energy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, galaxy formation, Evolution of the Universe, symbols.namesake, scale structure, 0103 physical sciences, supernova, Galaxy formation and evolution, Self-Interactions, Massive Neutrinos, STFC, Sdss, 010308 nuclear & particles physics, RCUK, resolution, Física, self-interactions, inconsistent, Universe, cosmic background radiation: temperature, 13. Climate action, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Galaxy Formation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, Hubble's law
Abstract

Chen, A., et al. DES Collaboration, We study a phenomenological class of models where dark matter converts to dark radiation in the low redshift epoch. This class of models, dubbed DMDR, characterizes the evolution of comoving dark-matter density with two extra parameters, and may be able to help alleviate the observed discrepancies between early and late-time probes of the Universe. We investigate how the conversion affects key cosmological observables such as the cosmic microwave background (CMB) temperature and matter power spectra. Combining 3x2pt data from Year 1 of the Dark Energy Survey, Planck-2018 CMB temperature and polarization data, supernovae (SN) Type Ia data from Pantheon, and baryon acoustic oscillation (BAO) data from BOSS DR12, MGS and 6dFGS, we place new constraints on the amount of dark matter that has converted to dark radiation and the rate of this conversion. The fraction of the dark matter that has converted since the beginning of the Universe in units of the current amount of dark matter, ζ, is constrained at 68% confidence level to be, he DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (Grant No. FP7/2007-2013) including ERC Grants Agreement No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2).

Published
2021
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5. Unveiling the Gravitational Universe at ��-Hz Frequencies

Author

Sesana, Alberto, Korsakova, Natalia, Sedda, Manuel Arca, Baibhav, Vishal, Barausse, Enrico, Barke, Simon, Berti, Emanuele, Bonetti, Matteo, Capelo, Pedro R., Caprini, Chiara, Garcia-Bellido, Juan, Haiman, Zoltan, Jani, Karan, Jennrich, Oliver, Johansson, Peter, Khan, Fazeel Mahmood, Korol, Valeriya, Lamberts, Astrid, Lupi, Alessandro, Mangiagli, Alberto, Mayer, Lucio, Nardini, Germano, Pacucci, Fabio, Petiteau, Antoine, Raccanelli, Alvise, Rajendran, Surjeet, Regan, John, Shao, Lijing, Spallicci, Alessandro, Tamanini, Nicola, Volonteri, Marta, Warburton, Niels, Wong, Kaze, and Zumalacarregui, Miguel

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We propose a space-based interferometer surveying the gravitational wave (GW) sky in the milli-Hz to $��$-Hz frequency range. By the 2040s', the $��$-Hz frequency band, bracketed in between the Laser Interferometer Space Antenna (LISA) and pulsar timing arrays, will constitute the largest gap in the coverage of the astrophysically relevant GW spectrum. Yet many outstanding questions related to astrophysics and cosmology are best answered by GW observations in this band. We show that a $��$-Hz GW detector will be a truly overarching observatory for the scientific community at large, greatly extending the potential of LISA. Conceived to detect massive black hole binaries from their early inspiral with high signal-to-noise ratio, and low-frequency stellar binaries in the Galaxy, this instrument will be a cornerstone for multimessenger astronomy from the solar neighbourhood to the high-redshift Universe., 28 pages, 8 figures; White Paper submitted to ESA's Voyage 2050 call for papers on behalf of the LISA Consortium 2050 Task Force

Published
2019
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6. LIGO Lo(g)Normal MACHO: Primordial Black Holes survive SN lensing constraints

Author

Garcia-Bellido, Juan, Clesse, Sebastien, and Fleury, Pierre

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), General Relativity and Cosmology, gr-qc, astro-ph.GA, FOS: Physical sciences, hep-ph, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics - Astrophysics of Galaxies, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Astrophysics::Galaxy Astrophysics, Particle Physics - Phenomenology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

It has been claimed in Ref.[arXiv:1712.02240] that massive primordial black holes (PBH) cannot constitute all of the dark matter (DM), because their gravitational-lensing imprint on the Hubble diagram of type Ia supernovae (SN) would be incompatible with present observations. In this paper, we critically review those constraints and find several caveats on the analysis. First of all, the constraints on the fraction $\alpha$ of PBH in matter seem to be driven by a very restrictive choice of priors on the cosmological parameters. In particular, the degeneracy between $\Omega_{\rm M}$ and $\alpha$ is ignored and thus, by fixing $\Omega_{\rm M}$, transferred the constraining power of SN magnitudes to $\alpha$. Furthermore, by considering more realistic physical sizes for the type-Ia supernovae, we find an effect on the SN lensing magnification distribution that leads to significantly looser constraints. Moreover, considering a wide mass spectrum of PBH, such as a lognormal distribution, further softens the constraints from SN lensing. Finally, we find that the fraction of PBH that could constitute DM today is bounded by $f_{\rm PBH} < 1.09\ (1.38)$, for JLA (Union 2.1) catalogs, and thus it is perfectly compatible with an all-PBH dark matter scenario in the LIGO band., Comment: 7 pages, 7 figures

Published
2017
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7. The DESI Experiment Part II: Instrument Design

Author

Collaboration, DESI, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E, Prieto, Carlos Allende, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C, Bell, Eric F, Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S, Briceno, Cesar, Brooks, David, Brownstein, Joel R, Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G, Cahn, Robert N, Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G, Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J, Cervantes-Cota, Jorge L, Claybaugh, Todd M, Close, Madeline, Coker, Carl T, Cole, Shaun, Comparat, Johan, Cooper, Andrew P, Cousinou, M-C, Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P, Davis, Tamara M, Dawson, Kyle S, Macorra, Axel de la, Vicente, Juan De, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T, Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J, Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R, Finkbeiner, Douglas P, Fitzpatrick, Michael J, Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E, Fosalba, Pablo, Frenk, Carlos S, Fumagalli, Michele, Gaensicke, Boris T, Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Fusillo, Nicola Pietro Gentile, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-de-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, and Guy, Julien

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, astro-ph.CO, Astrophysics::Cosmology and Extragalactic Astrophysics, astro-ph.IM
Abstract

DESI (Dark Energy Spectropic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. The DESI instrument is a robotically-actuated, fiber-fed spectrograph capable of taking up to 5,000 simultaneous spectra over a wavelength range from 360 nm to 980 nm. The fibers feed ten three-arm spectrographs with resolution $R= \lambda/\Delta\lambda$ between 2000 and 5500, depending on wavelength. The DESI instrument will be used to conduct a five-year survey designed to cover 14,000 deg$^2$. This powerful instrument will be installed at prime focus on the 4-m Mayall telescope in Kitt Peak, Arizona, along with a new optical corrector, which will provide a three-degree diameter field of view. The DESI collaboration will also deliver a spectroscopic pipeline and data management system to reduce and archive all data for eventual public use.

Published
2016

8. The DESI Experiment Part I: Science,Targeting, and Survey Design

Author

Collaboration, DESI, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E, Prieto, Carlos Allende, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C, Bell, Eric F, Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S, Briceno, Cesar, Brooks, David, Brownstein, Joel R, Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G, Cahn, Robert N, Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G, Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J, Cervantes-Cota, Jorge L, Claybaugh, Todd M, Close, Madeline, Coker, Carl T, Cole, Shaun, Comparat, Johan, Cooper, Andrew P, Cousinou, M-C, Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P, Davis, Tamara M, Dawson, Kyle S, Macorra, Axel de la, Vicente, Juan De, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T, Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J, Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R, Finkbeiner, Douglas P, Fitzpatrick, Michael J, Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E, Fosalba, Pablo, Frenk, Carlos S, Fumagalli, Michele, Gaensicke, Boris T, Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Fusillo, Nicola Pietro Gentile, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-de-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, and Guy, Julien

Subjects
astro-ph.CO, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, astro-ph.IM
Abstract

DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tracers of the underlying dark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the Ly-$\alpha$ forest absorption features in their spectra, which will be used to trace the distribution of neutral hydrogen. When moonlight prevents efficient observations of the faint targets of the baseline survey, DESI will conduct a magnitude-limited Bright Galaxy Survey comprising approximately 10 million galaxies with a median $z\approx 0.2$. In total, more than 30 million galaxy and quasar redshifts will be obtained to measure the BAO feature and determine the matter power spectrum, including redshift space distortions.

Published
2016

9. The Decay of the Standard Model Higgs after Inflation

Author

Figueroa, Daniel G., Garcia-Bellido, Juan, and Torrenti, Francisco

Subjects
High Energy Physics - Theory, High Energy Physics - Phenomenology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Theory (hep-th), High Energy Physics::Lattice, High Energy Physics::Phenomenology, FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the nonperturbative dynamics of the Standard Model (SM) after inflation, in the regime where the SM is decoupled from (or weakly coupled to) the inflationary sector. We use classical lattice simulations in an expanding box in (3+1) dimensions, modeling the SM gauge interactions with both global and Abelian-Higgs analogue scenarios. We consider different post-inflationary expansion rates. During inflation, the Higgs forms a condensate, which starts oscillating soon after inflation ends. Via nonperturbative effects, the oscillations lead to a fast decay of the Higgs into the SM species, transferring most of the energy into $Z$ and $W^{\pm}$ bosons. All species are initially excited far away from equilibrium, but their interactions lead them into a stationary stage, with exact equipartition among the different energy components. From there on the system eventually reaches equilibrium. We have characterized in detail, in the different expansion histories considered, the evolution of the Higgs and of its dominant decay products, until equipartition is established. We provide a useful mapping between simulations with different parameters, from where we derive a master formula for the Higgs decay time, as a function of the coupling constants, Higgs initial amplitude and postinflationary expansion rate., Comment: Minor changes to match the PRD published version. Modulation of the Higgs amplitude removed for $q > 200$ in Sec. V, due to improving the time resolution in the Higgs equation of motion. Results unaffected

Published
2015
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10. Looking the void in the eyes - the kSZ effect in LTB models

Author

Garcia-Bellido, Juan and Haugboelle, Troels

Subjects
Astrophysics (astro-ph), Void, FOS: Physical sciences, Sunyaev-Zeldovich (kSZ) effect, Astrophysics::Cosmology and Extragalactic Astrophysics, Dimming of supernovae, Astrophysics, Lemaitre-Tolman-Bondi (LTB) metric, Cosmic Microwave Background (CMB) dipole
Abstract

20 pages, 9 figures.-- PACS numbers: 98.65.Dx, 98.80.Es, 98.80.-k.-- Submitted to Journal of Cosmology and Astroparticle Physics (JCAP)., As an alternative explanation of the dimming of distant supernovae it has recently been advocated that we live in a special place in the Universe near the centre of a large void described by a Lemaitre-Tolman-Bondi (LTB) metric. The Universe is no longer homogeneous and isotropic and the apparent late time acceleration is actually a consequence of spatial gradients in the metric. If we did not live close to the centre of the void, we would have observed a Cosmic Microwave Background (CMB) dipole much larger than that allowed by observations. Hence, until now it has been argued, for the model to be consistent with observations, that by coincidence we happen to live very close to the centre of the void or we are moving towards it. However, even if we are at the centre of the void, we can observe distant galaxy clusters, which are off-centre. In their frame of reference there should be a large CMB dipole, which manifests itself observationally for us as a kinematic Sunyaev-Zeldovich (kSZ) effect. kSZ observations give far stronger constraints on the LTB model compared to other observational probes such as Type Ia Supernovae, the CMB, and baryon acoustic oscillations. We show that current observations of only 9 clusters with large error bars already rule out LTB models with void sizes greater than approximately 1.5 Gpc and a significant underdensity, and that near future kSZ surveys like the Atacama Cosmology Telescope, South Pole Telescope, APEX telescope, or the Planck satellite will be able to strongly rule out or confirm LTB models with giga parsec sized voids. On the other hand, if the LTB model is confirmed by observations, a kSZ survey gives a unique possibility of directly reconstructing the expansion rate and underdensity profile of the void., We acknowledge the use of the computer resources of the Danish Centre of Scientific Computing. We also acknowledge financial support from the Spanish Research Ministry, under contract FPA2006-05807 and the Consolider Ingenio 2010 programme under contract CSD2007-00060 "Physics of the Accelerating Universe" (PAU).

Published
2008

11. Flat direction MSSM (A-term) Inflation

Author

Garcia-Bellido, Juan

Subjects
High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), High Energy Physics::Phenomenology, FOS: Physical sciences
Abstract

The Minimal Supersymmetry Standard Model contains several hundreds of D- and F-flat directions that are lifted by soft susy breaking terms as well as by non-renormalizable terms. In a recent paper we find that only two of these directions, {\bf LLe} and {\bf udd} can accommodate inflation. The model predicts more than $10^3$ e-foldings with an inflationary scale of $H_{\rm inf}\sim 1$ GeV, provides a tilted spectrum compatible with WMAP3, and a negligible tensor perturbation. The reheating temperature could be as low as $T_{rh}\sim 1$ TeV. The model is stable under radiative as well as supergravity corrections, although a significant finetunning has to be imposed on the ratio of two parameters of the model. The RGE equations allow us to relate the model parameters with slepton and gaugino masses explorable in the LHC, while the neutralino in this model could well be within reach of present dark matter searches in the laboratory., Comment: Talk presented at the "Dark Side of the Universe 2006" Conference, June 20-24 2006, Madrid

Published
2006
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12. The Paradigm of Inflation

Author

Garcia-Bellido, Juan

Subjects
High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract

The standard model of cosmology is based on the hot Big Bang theory and the inflationary paradigm. Recent precise observations of the temperature and polarization anisotropies in the cosmic microwave background and the matter distribution in large scale structures like galaxies and clusters confirm the general paradigm and put severe constrains on variations of this simple idea. In this essay I will discuss the epistemological foundations of such a paradigm and speculate on its possible realisation within a more fundamental theory., Comment: 21 pages, 1 figure, uses ws-rv9x6.cls

Published
2004
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13. Bounds on CDM and neutrino isocurvature perturbations from CMB and LSS data

Author

Beltran, Maria, Garcia-Bellido, Juan, Lesgourgues, Julien, Riazuelo, Alain, Departamento de Fisica Teorica, Universidad Autónoma de Madrid (UAM), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidad Autonoma de Madrid (UAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and arXiv, Import

Subjects
[PHYS.GRQC] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, General Relativity and Quantum Cosmology, [PHYS.HPHE] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc]
Abstract

Generic models for the origin of structure predict a spectrum of initial fluctuations with a mixture of adiabatic and isocurvature perturbations. Using the observed anisotropies of the cosmic microwave backgound, the matter power spectra from large scale structure surveys and the luminosity distance vs redshift relation from supernovae of type Ia, we obtain strong bounds on the possible cold dark matter/baryon as well as neutrino isocurvature contributions to the primordial fluctations in the Universe. Neglecting the possible effects of spatial curvature and tensor perturbations, we perform a Bayesian likelihood analysis with thirteen free parameters, including independent spectral indexes for each of the modes and for their cross-correlation angle. We find that around a pivot wavenumber of k=0.05 h/Mpc the amplitude of the correlated isocurvature component cannot be larger than about 60% for the cold dark matter mode, 40% for the neutrino density mode, and 30% for the neutrino velocity mode, at 2 sigma. In the first case, our bound is larger than the WMAP first-year result, presumably because we prefer not to include any data from Lyman-alpha forests, but then obtain large blue spectral indexes for the non-adiabatic contributions. We also translate our bounds in terms of constraints on double inflation models with two uncoupled massive fields., Comment: 12 pages, 5 figures

Published
2004
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17. Single-bubble Open Inflation: An Overview

Author

Garcia-Bellido, Juan

Subjects
High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Particle Physics - Phenomenology
Abstract

The idea that the universe might be open is an old one, and the possibility of having an open universe arise form inflation is not new either. However, a concrete realization of a consistent single-bubble open inflation model is known only recently. There has been great progress in the last two years in the development of models of inflation consistent with observations in such an open universe. In this overview I will describe the basic features and the phenomenological consequences of such models, making emphasis in the predictions of the CMB temperature anisotropies that differ from ordinary inflation., Comment: 20 pages, LaTeX, crckapb.sty macro included, 6 figures included in the text with epsf. Review talk, to appear in the Proceedings of the ``Birth of the Universe II'' Conference in Roma, May 1997

Published
1998
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18. The Open Universe Grishchuk-Zel'dovich Effect

Author

Garcia-Bellido, Juan, Liddle, Andrew R, Lyth, David H, and Wands, David

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, General Relativity and Quantum Cosmology
Abstract

The Grishchuk--Zel'dovich effect is the contribution to the microwave background anisotropy from an extremely large scale adiabatic density perturbation, on the standard hypothesis that this perturbation is a typical realization of a homogeneous Gaussian random field. We analyze this effect in open universes, corresponding to density parameter $\Omega_0, Comment: 10 pages LaTeX file (using RevTeX), plus 4 postscript figures to be printed separately. Final version, to appear in Physical Review D: main change is a new appendix on the dipole anisotropy

Published
1995
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19. Quantum Diffusion of Planck Mass and the Evolution of the Universe

Author

Garcia-Bellido, Juan

Subjects
High Energy Physics - Theory, General Relativity and Quantum Cosmology, High Energy Physics - Theory (hep-th), Astrophysics (astro-ph), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics
Abstract

A theory of evolution for the Universe requires both a mutation mechanism and a selection mechanism. We propose that both can be encountered in the stochastic approach to quantum cosmology. In Brans--Dicke chaotic inflation, the quantum fluctuations of Planck mass behave as mutations, such that new inflationary domains may contain values of Planck mass that differ slightly from their parent's. The selection mechanism establishes that the value of Planck mass should be such as to increase the proper volume of the inflationary domain, which will then generate more offsprings. For generic chaotic potentials we find runaway probability distributions that move towards large values of both inflaton and dilaton fields. Therefore, this mechanism predicts that the effective Planck scale should be much larger than any given scale in the problem., Comment: plain LaTeX, 7 pages, Stanford University preprint SU-ITP-94-23

Published
1994
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20. COrE (Cosmic Origins Explorer) A White Paper

Author

Bouchet, F. R., Bernardis, P., Maffei, B., Natoli, P., Piant, M., Ponthieu, N., Stompor, R., Bersanelli, M., Bielewicz, P., Camus, P., Petris, M., Mauskopf, P., Masi, S., Nati, F., Peacocke, T., Piacentini, F., Piccirillo, L., Piat, M., Pisano, G., Salatino, M. F., Withington, S., Bucher, M., Avilles, M., Barbosa, D., Bartolo, N., Battye, R., Bernard, J. -P, Boulanger, F., Challinor, A., Chongchitnan, S., Colafrancesco, S., Ensslin, T., Fergusson, J., Ferreira, P., Ferriere, K., Finelli, F., Garcia-Bellido, Juan, Galli, S., Gauthier, C., Haverkorn, M., Hindmarsh, M., Jaffe, A., Kung, M., Lesgourgues, J., Liddle, A., Liguori, M., Marchegiani, P., Sabino Matarrese, Melchiorri, A., Mukherjee, P., Pagano, L., Paoletti, D., Peiris, H., Perroto, L., Rath, C., Rubino Martin, J., Shellard, P., Urrestilla, J., Tent, B., Verde, L., Wandelt, B., Burigana, C., Delabrouille, J., Armitage-Caplan, C., Banday, A., Basak, S., Bonaldi, A., Clements, D., Zotti, G., Dickinson, C., Dunkley, J., Lopez-Caniego, M., Martinez-Gonzalez, E., Negrello, M., Ricciardi, S., and Toffolatti, L.

21. Cosmology and Fundamental Physics with the Euclid Satellite

Author

Amendola, Luca, Appleby, Stephen, Bacon, David, Baker, Tessa, Baldi, Marco, Bartolo, Nicola, Blanchard, Alain, Bonvin, Camille, Borgani, Stefano, Branchini, Enzo, Burrage, Clare, Camera, Stefano, Carbone, Carmelita, Casarini, Luciano, Cropper, Mark, Rham, Claudia, Di Porto, Cinzia, Ealet, Anne, Ferreira, Pedro G., Finelli, Fabio, Garcia-Bellido, Juan, Giannantonio, Tommaso, Guzzo, Luigi, Heavens, Alan, Heisenberg, Lavinia, Heymans, Catherine, Hoekstra, Henk, Hollenstein, Lukas, Holmes, Rory, Horst, Ole, Jahnke, Knud, Kitching, Thomas D., Koivisto, Tomi, Kunz, Martin, La Vacca, Giuseppe, March, Marisa, Majerotto, Elisabetta, Markovic, Katarina, Marsh, David, Marulli, Federico, Massey, Richard, Mellier, Yannick, Mota, David F., Nunes, Nelson J., Percival, Will, Pettorino, Valeria, Porciani, Cristiano, Quercellini, Claudia, Read, Justin, Rinaldi, Massimiliano, Sapone, Domenico, Scaramella, Roberto, Constantinos Skordis, Simpson, Fergus, Taylor, Andy, Thomas, Shaun, Trotta, Roberto, Verde, Licia, Vernizzi, Filippo, Vollmer, Adrian, Wang, Yun, Weller, Jochen, Zlosnik, Tom, and Euclid Theory Working Grp

22. PRISM (Polarized Radiation Imaging and Spectroscopy Mission): A White Paper on the Ultimate Polarimetric Spectro-Imaging of the Microwave and Far-Infrared Sky

Author

Prism, Collaboration, Andre, Philippe, Baccigalupi, Carlo, Barbosa, Domingos, Bartlett, James, Bartolo, Nicola, Battistelli, Elia, Battye, Richard, Bendo, George, Bernard, Jean-Philippe, Bersanelli, Marco, Bethermin, Matthieu, Bielewicz, Pawel, Bonaldi, Anna, Bouchet, Francois, Boulanger, Francois, Brand, Jan, Bucher, Martin, Burigana, Carlo, Cai, Zhen-Yi, Casasola, Viviana, Castex, Guillaume, Challinor, Anthony, Jens Chluba, Colafrancesco, Sergio, Cuttaia, Francesco, D Alessandro, Giuseppe, Davis, Richard, Avillez, Miguel, Bernardis, Paolo, Petris, Marco, Rosa, Adriano, Zotti, Gianfranco, Delabrouille, Jacques, Dickinson, Clive, Diego, Jose Maria, Falgarone, Edith, Ferreira, Pedro, Ferriere, Katia, Finelli, Fabio, Fletcher, Andrew, Fuller, Gary, Galli, Silvia, Ganga, Ken, Garcia-Bellido, Juan, Ghribi, Adnan, Gonzalez-Nuevo, Joaquin, Grainge, Keith, Gruppuso, Alessandro, Hall, Alex, Hernandez-Monteagudo, Carlos, Jackson, Mark, Jaffe, Andrew, Khatri, Rishi, Lamagna, Luca, Lattanzi, Massimiliano, Leahy, Paddy, Liguori, Michele, Liuzzo, Elisabetta, Lopez-Caniego, Marcos, Macias-Perez, Juan, Maffei, Bruno, Maino, Davide, Masi, Silvia, Mangilli, Anna, Massardi, Marcella, Matarrese, Sabino, Melchiorri, Alessandro, Melin, Jean-Baptiste, Mennella, Aniello, Mignano, Arturo, Miville-Deschenes, Marc-Antoine, Nati, Federico, Natoli, Paolo, Negrello, Mattia, Noviello, Fabio, Paci, Francesco, Paladino, Rosita, Paoletti, Daniela, Perrotta, Francesca, Piacentini, Francesco, Piat, Michel, Piccirillo, Lucio, Pisano, Giampaolo, Polenta, Gianluca, Ricciardi, Sara, Roman, Matthieu, Rubino-Martin, Jose-Alberto, Salatino, Maria, Schillaci, Alessandro, Shellard, Paul, Silk, Joseph, Stompor, Radek, Sunyaev, Rashid, Tartari, Andrea, Terenzi, Luca, Toffolatti, Luigi, Tomasi, Maurizio, Trombetti, Tiziana, Tucci, Marco, Tent, Bartjan, Verde, Licia, Wandelt, Ben, and Withington, Stafford

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in response to the Call for White Papers for the definition of the L2 and L3 Missions in the ESA Science Programme. PRISM would have two instruments: (1) an imager with a 3.5m mirror (cooled to 4K for high performance in the far-infrared---that is, in the Wien part of the CMB blackbody spectrum), and (2) an Fourier Transform Spectrometer (FTS) somewhat like the COBE FIRAS instrument but over three orders of magnitude more sensitive. Highlights of the new science (beyond the obvious target of B-modes from gravity waves generated during inflation) made possible by these two instruments working in tandem include: (1) the ultimate galaxy cluster survey gathering 10e6 clusters extending to large redshift and measuring their peculiar velocities and temperatures (through the kSZ effect and relativistic corrections to the classic y-distortion spectrum, respectively) (2) a detailed investigation into the nature of the cosmic infrared background (CIB) consisting of at present unresolved dusty high-z galaxies, where most of the star formation in the universe took place, (3) searching for distortions from the perfect CMB blackbody spectrum, which will probe a large number of otherwise inaccessible effects (e.g., energy release through decaying dark matter, the primordial power spectrum on very small scales where measurements today are impossible due to erasure from Silk damping and contamination from non-linear cascading of power from larger length scales). These are but a few of the highlights of the new science that will be made possible with PRISM., Comment: 20 pages Latex

23. The DESI Experiment Part I: Science,Targeting, and Survey Design

Author

Desi, Collaboration, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E., Allende Prieto, Carlos, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C., Bell, Eric F., Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S., Briceno, Cesar, Brooks, David, Brownstein, Joel R., Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G., Cahn, Robert N., Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G., Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J., Cervantes-Cota, Jorge L., Claybaugh, Todd M., Close, Madeline, Coker, Carl T., Cole, Shaun, Comparat, Johan, Cooper, Andrew P., Cousinou, M. -C, Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P., Davis, Tamara M., Dawson, Kyle S., La Macorra, Axel, Vicente, Juan, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T., Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R., Finkbeiner, Douglas P., Fitzpatrick, Michael J., Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E., Fosalba, Pablo, Frenk, Carlos S., Fumagalli, Michele, Gaensicke, Boris T., Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Pietro Gentile Fusillo, Nicola, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-De-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, Guy, Julien, Habib, Salman, Heetderks, Henry, Heetderks, Ian, Heitmann, Katrin, Hellwing, Wojciech A., Herrera, David A., Ho, Shirley, Holland, Stephen, Honscheid, Klaus, Huff, Eric, Hutchinson, Timothy A., Huterer, Dragan, Hwang, Ho Seong, Illa Laguna, Joseph Maria, Ishikawa, Yuzo, Jacobs, Dianna, Jeffrey, Niall, Jelinsky, Patrick, Jennings, Elise, Jiang, Linhua, Jimenez, Jorge, Johnson, Jennifer, Joyce, Richard, Jullo, Eric, Juneau, Stéphanie, Kama, Sami, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kennamer, Noble, Kent, Stephen, Kilbinger, Martin, Kim, Alex G., Kirkby, David, Kisner, Theodore, Kitanidis, Ellie, Kneib, Jean-Paul, Koposov, Sergey, Kovacs, Eve, Koyama, Kazuya, Kremin, Anthony, Kron, Richard, Kronig, Luzius, Kueter-Young, Andrea, Lacey, Cedric G., Lafever, Robin, Lahav, Ofer, Lambert, Andrew, Lampton, Michael, Landriau, Martin, Lang, Dustin, Lauer, Tod R., Le Goff, Jean-Marc, Le Guillou, Laurent, Le Suu, Auguste, Lee, Jae Hyeon, Lee, Su-Jeong, Leitner, Daniela, Lesser, Michael, Levi, Michael E., L Huillier, Benjamin, Li, Baojiu, Liang, Ming, Lin, Huan, Linder, Eric, Loebman, Sarah R., Lukić, Zarija, Ma, Jun, Maccrann, Niall, Magneville, Christophe, Makarem, Laleh, Manera, Marc, Manser, Christopher J., Marshall, Robert, Martini, Paul, Massey, Richard, Matheson, Thomas, Mccauley, Jeremy, Mcdonald, Patrick, Mcgreer, Ian D., Meisner, Aaron, Metcalfe, Nigel, Miller, Timothy N., Miquel, Ramon, Moustakas, John, Myers, Adam, Naik, Milind, Newman, Jeffrey A., Nichol, Robert C., Nicola, Andrina, Nicolati Da Costa, Luiz, Nie, Jundan, Niz, Gustavo, Norberg, Peder, Nord, Brian, Norman, Dara, Nugent, Peter, O Brien, Thomas, Oh, Minji, Olsen, Knut A. G., Padilla, Cristobal, Padmanabhan, Hamsa, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Palmese, Antonella, Pappalardo, Daniel, Pâris, Isabelle, Park, Changbom, Patej, Anna, Peacock, John A., Peiris, Hiranya V., Peng, Xiyan, Percival, Will J., Perruchot, Sandrine, Pieri, Matthew M., Pogge, Richard, Pollack, Jennifer E., Poppett, Claire, Prada, Francisco, Prakash, Abhishek, Probst, Ronald G., Rabinowitz, David, Raichoor, Anand, Ree, Chang Hee, Refregier, Alexandre, Regal, Xavier, Reid, Beth, Reil, Kevin, Rezaie, Mehdi, Rockosi, Constance M., Roe, Natalie, Ronayette, Samuel, Roodman, Aaron, Ross, Ashley J., Ross, Nicholas P., Rossi, Graziano, Rozo, Eduardo, Ruhlmann-Kleider, Vanina, Rykoff, Eli S., Sabiu, Cristiano, Samushia, Lado, Sanchez, Eusebio, Sanchez, Javier, Schlegel, David J., Schneider, Michael, Schubnell, Michael, Secroun, Aurélia, Seljak, Uros, Seo, Hee-Jong, Serrano, Santiago, Shafieloo, Arman, Shan, Huanyuan, Sharples, Ray, Sholl, Michael J., Shourt, William V., Silber, Joseph H., Silva, David R., Sirk, Martin M., Slosar, Anze, Smith, Alex, Smoot, George F., Som, Debopam, Song, Yong-Seon, Sprayberry, David, Staten, Ryan, Stefanik, Andy, Tarle, Gregory, Sien Tie, Suk, Tinker, Jeremy L., Tojeiro, Rita, Valdes, Francisco, Valenzuela, Octavio, Valluri, Monica, Vargas-Magana, Mariana, Verde, Licia, Walker, Alistair R., Wang, Jiali, Wang, Yuting, Weaver, Benjamin A., Weaverdyck, Curtis, Wechsler, Risa H., Weinberg, David H., White, Martin, Yang, Qian, Yeche, Christophe, Zhang, Tianmeng, Zhao, Gong-Bo, Zheng, Yi, Zhou, Xu, Zhou, Zhimin, Zhu, Yaling, Zou, Hu, and Ying Zu

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.CO, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract

DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tracers of the underlying dark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the Ly-$��$ forest absorption features in their spectra, which will be used to trace the distribution of neutral hydrogen. When moonlight prevents efficient observations of the faint targets of the baseline survey, DESI will conduct a magnitude-limited Bright Galaxy Survey comprising approximately 10 million galaxies with a median $z\approx 0.2$. In total, more than 30 million galaxy and quasar redshifts will be obtained to measure the BAO feature and determine the matter power spectrum, including redshift space distortions.

24. The Hitchhiker's guide to the galaxy catalog approach for gravitational wave cosmology

Author

Gair, Jonathan R., Ghosh, Archisman, Gray, Rachel, Holz, Daniel E., Mastrogiovanni, Simone, Mukherjee, Suvodip, Palmese, Antonella, Tamanini, Nicola, Baker, Tessa, Beirnaert, Freija, Bilicki, Maciej, Chen, Hsin-Yu, Dálya, Gergely, Ezquiaga, Jose Maria, Farr, Will M., Fishbach, Maya, Garcia-Bellido, Juan, Tathagata Ghosh, Huang, Hsiang-Yu, Karathanasis, Christos, Leyde, Konstantin, Magaña Hernandez, Ignacio, Noller, Johannes, Pierra, Gregoire, Raffai, Peter, Romano, Antonio Enea, Seglar-Arroyo, Monica, Steer, Danièle A., Turski, Cezary, Vaccaro, Maria Paola, Vallejo-Peña, Sergio Andrés, Laboratoire des deux Infinis de Toulouse (L2IT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Cosmologie et Gravitation, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
radiation: electromagnetic, cosmological model, data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Hubble constant, gravitational radiation, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Bayesian, General Relativity and Quantum Cosmology, localization, statistical analysis, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We outline the ``dark siren'' galaxy catalog method for cosmological inference using gravitational wave (GW) standard sirens, clarifying some common misconceptions in the implementation of this method. When a confident transient electromagnetic counterpart to a GW event is unavailable, the identification of a unique host galaxy is in general challenging. Instead, as originally proposed by Schutz (1986), one can consult a galaxy catalog and implement a dark siren statistical approach incorporating all potential host galaxies within the localization volume. Trott & Hunterer 2021 recently claimed that this approach results in a biased estimate of the Hubble constant, $H_0$, when implemented on mock data, even if optimistic assumptions are made. We demonstrate explicitly that, as previously shown by multiple independent groups, the dark siren statistical method leads to an unbiased posterior when the method is applied to the data correctly. We highlight common sources of error possible to make in the generation of mock data and implementation of the statistical framework, including the mismodeling of selection effects and inconsistent implementations of the Bayesian framework, which can lead to a spurious bias., 19 pages, 11 figures. Submitted to ApJ

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25. The DESI Experiment Part II: Instrument Design

Author

Desi, Collaboration, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E., Allende Prieto, Carlos, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C., Bell, Eric F., Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S., Briceno, Cesar, Brooks, David, Brownstein, Joel R., Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G., Cahn, Robert N., Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G., Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J., Cervantes-Cota, Jorge L., Claybaugh, Todd M., Close, Madeline, Coker, Carl T., Cole, Shaun, Comparat, Johan, Cooper, Andrew P., Cousinou, M. -C, Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P., Davis, Tamara M., Dawson, Kyle S., La Macorra, Axel, Vicente, Juan, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T., Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R., Finkbeiner, Douglas P., Fitzpatrick, Michael J., Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E., Fosalba, Pablo, Frenk, Carlos S., Fumagalli, Michele, Gaensicke, Boris T., Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Pietro Gentile Fusillo, Nicola, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-De-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, Guy, Julien, Habib, Salman, Heetderks, Henry, Heetderks, Ian, Heitmann, Katrin, Hellwing, Wojciech A., Herrera, David A., Ho, Shirley, Holland, Stephen, Honscheid, Klaus, Huff, Eric, Hutchinson, Timothy A., Huterer, Dragan, Hwang, Ho Seong, Illa Laguna, Joseph Maria, Ishikawa, Yuzo, Jacobs, Dianna, Jeffrey, Niall, Jelinsky, Patrick, Jennings, Elise, Jiang, Linhua, Jimenez, Jorge, Johnson, Jennifer, Joyce, Richard, Jullo, Eric, Juneau, Stéphanie, Kama, Sami, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kennamer, Noble, Kent, Stephen, Kilbinger, Martin, Kim, Alex G., Kirkby, David, Kisner, Theodore, Kitanidis, Ellie, Kneib, Jean-Paul, Koposov, Sergey, Kovacs, Eve, Koyama, Kazuya, Kremin, Anthony, Kron, Richard, Kronig, Luzius, Kueter-Young, Andrea, Lacey, Cedric G., Lafever, Robin, Lahav, Ofer, Lambert, Andrew, Lampton, Michael, Landriau, Martin, Lang, Dustin, Lauer, Tod R., Le Goff, Jean-Marc, Le Guillou, Laurent, Le Suu, Auguste, Lee, Jae Hyeon, Lee, Su-Jeong, Leitner, Daniela, Lesser, Michael, Levi, Michael E., L Huillier, Benjamin, Li, Baojiu, Liang, Ming, Lin, Huan, Linder, Eric, Loebman, Sarah R., Lukić, Zarija, Ma, Jun, Maccrann, Niall, Magneville, Christophe, Makarem, Laleh, Manera, Marc, Manser, Christopher J., Marshall, Robert, Martini, Paul, Massey, Richard, Matheson, Thomas, Mccauley, Jeremy, Mcdonald, Patrick, Mcgreer, Ian D., Meisner, Aaron, Metcalfe, Nigel, Miller, Timothy N., Miquel, Ramon, Moustakas, John, Myers, Adam, Naik, Milind, Newman, Jeffrey A., Nichol, Robert C., Nicola, Andrina, Nicolati Da Costa, Luiz, Nie, Jundan, Niz, Gustavo, Peder Norberg, Nord, Brian, Norman, Dara, Nugent, Peter, O Brien, Thomas, Oh, Minji, Olsen, Knut A. G., Padilla, Cristobal, Padmanabhan, Hamsa, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Palmese, Antonella, Pappalardo, Daniel, Pâris, Isabelle, Park, Changbom, Patej, Anna, Peacock, John A., Peiris, Hiranya V., Peng, Xiyan, Percival, Will J., Perruchot, Sandrine, Pieri, Matthew M., Pogge, Richard, Pollack, Jennifer E., Poppett, Claire, Prada, Francisco, Prakash, Abhishek, Probst, Ronald G., Rabinowitz, David, Raichoor, Anand, Ree, Chang Hee, Refregier, Alexandre, Regal, Xavier, Reid, Beth, Reil, Kevin, Rezaie, Mehdi, Rockosi, Constance M., Roe, Natalie, Ronayette, Samuel, Roodman, Aaron, Ross, Ashley J., Ross, Nicholas P., Rossi, Graziano, Rozo, Eduardo, Ruhlmann-Kleider, Vanina, Rykoff, Eli S., Sabiu, Cristiano, Samushia, Lado, Sanchez, Eusebio, Sanchez, Javier, Schlegel, David J., Schneider, Michael, Schubnell, Michael, Secroun, Aurélia, Seljak, Uros, Seo, Hee-Jong, Serrano, Santiago, Shafieloo, Arman, Shan, Huanyuan, Sharples, Ray, Sholl, Michael J., Shourt, William V., Silber, Joseph H., Silva, David R., Sirk, Martin M., Slosar, Anze, Smith, Alex, Smoot, George F., Som, Debopam, Song, Yong-Seon, Sprayberry, David, Staten, Ryan, Stefanik, Andy, Tarle, Gregory, Sien Tie, Suk, Tinker, Jeremy L., Tojeiro, Rita, Valdes, Francisco, Valenzuela, Octavio, Valluri, Monica, Vargas-Magana, Mariana, Verde, Licia, Walker, Alistair R., Wang, Jiali, Wang, Yuting, Weaver, Benjamin A., Weaverdyck, Curtis, Wechsler, Risa H., Weinberg, David H., White, Martin, Yang, Qian, Yeche, Christophe, Zhang, Tianmeng, Zhao, Gong-Bo, Zheng, Yi, Zhou, Xu, Zhou, Zhimin, Zhu, Yaling, Zou, Hu, Zu, Ying, Korea Astronomy and Space Science Institute (KASI), University of California [Berkeley] (UC Berkeley), University of California (UC), Boston University [Boston] (BU), Carnegie Mellon University [Pittsburgh] (CMU), University of Edinburgh, National Optical Astronomy Observatory (NOAO), Instituto de Astrofisica de Canarias (IAC), Fermi National Accelerator Laboratory (Fermilab), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Yale University [New Haven], Ohio State University [Columbus] (OSU), The University of Notre Dame [Sydney], Department of Astronomy, University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Space Sciences Laboratory [Berkeley] (SSL), University of California (UC)-University of California (UC), University of Portsmouth, Centre for Astrophysics & Supercomputing, Swinburne University of Technology (Hawthorn campus), Ecole Polytechnique Fédérale de Lausanne (EPFL), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), The University of Utah, Cerro Tololo Inter-American Observatory, University College of London [London] (UCL), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institute for Astronomy [Edinburgh] (IfA), Department of Astronomy & Astrophysics [University of Toronto], University of Toronto, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Carreterra Mexico-Toluca, Department of Physics [Durham University], Durham University, Department of Astronomy, The Ohio State University, Institute for Computational Cosmology (ICC), Instituto de Fisica Teorica C-XVI (IFT-UAM/CSIC), Universidad Autónoma de Madrid (UAM), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Department of Applied Physics, Departamento de Fisica Aplicada [Granada], Universidad de Granada = University of Granada (UGR)-Universidad de Granada = University of Granada (UGR), University of Wyoming (UW), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Arizona State University [Tempe] (ASU), Department of Physics, University of California, University of California [Los Angeles] (UCLA), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Department of Physics [Durham], University of New Hampshire (UNH), Departamento de Fisica Teorica, Korea Institute for Advanced Study (KIAS), Centre d'Immunologie et des Maladies Infectieuses (CIMI), Institut National de la Santé et de la Recherche Médicale (INSERM)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Center for Cosmology & AstroParticle Physics, Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), School of Physics and Astronomy [Nottingham], University of Nottingham, UK (UON), School of Physics, University of Waterloo [Waterloo], Department of Astronomy and Space Science [Sejong University], Sejong University, Brookhaven National Laboratory [Upton, NY] (BNL), UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY)-U.S. Department of Energy [Washington] (DOE), Department of Physics [Ann Arbor], University of St Andrews [Scotland], University of Science and Technology of China [Hefei] (USTC), Department of Computer Science and Engineering [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Karlsruhe Institute of Technology (KIT), Key Laboratory for Liquid-Solid Structural Evolution and Processing of Materials, Shandong University, National University of Defense Technology [China], Avidea Technologies, Inc, DESI Collaboration, Okayama University, University of California [Berkeley], University of California, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), University of California-University of California, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universidad Autonoma de Madrid (UAM), Universidad Nacional Autónoma de México (UNAM), Universidad de Granada (UGR)-Universidad de Granada (UGR), Harvard University [Cambridge]-Smithsonian Institution, Centre d'Immunologie et de Maladies Infectieuses (CIMI), University of California [Irvine] (UCI), U.S. Department of Energy [Washington] (DOE)-UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), and Escoffier, Stephanie

Subjects
[SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.CO, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), astro-ph.IM, Astrophysics - Cosmology and Nongalactic Astrophysics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

DESI (Dark Energy Spectropic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. The DESI instrument is a robotically-actuated, fiber-fed spectrograph capable of taking up to 5,000 simultaneous spectra over a wavelength range from 360 nm to 980 nm. The fibers feed ten three-arm spectrographs with resolution $R= \lambda/\Delta\lambda$ between 2000 and 5500, depending on wavelength. The DESI instrument will be used to conduct a five-year survey designed to cover 14,000 deg$^2$. This powerful instrument will be installed at prime focus on the 4-m Mayall telescope in Kitt Peak, Arizona, along with a new optical corrector, which will provide a three-degree diameter field of view. The DESI collaboration will also deliver a spectroscopic pipeline and data management system to reduce and archive all data for eventual public use.

26. The cold spot in the cosmic microwave background: The shadow of a supervoid

Author

Szapudi, István, Kovács, András, Granett, Benjamin R., Frei, Zsolt, Silk, Joseph, Garcia-Bellido, Juan, Burgett, Will, Shaun Cole, Draper, Peter W., Farrow, Daniel J., Kaiser, Nicholas, Magnier, Eugene A., Metcalfe, Nigel, Morgan, Jeffrey S., Price, Paul, Tonry, John, and Wainscoat, Richard

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Standard inflationary hot big bang cosmology predicts small fluctuations in the Cosmic Microwave Background (CMB) with isotropic Gaussian statistics. All measurements support the standard theory, except for a few anomalies discovered in the Wilkinson Microwave Anisotropy Probe maps and confirmed recently by the Planck satellite. The Cold Spot is one of the most significant of such anomalies, and the leading explanation of it posits a large void that imprints this extremely cold area via the linear Integrated Sachs-Wolfe (ISW) effect due to the decay of gravitational potentials over cosmic time, or via the Rees-Sciama (RS) effect due to late-time non-linear evolution. Despite several observational campaigns targeting the Cold Spot region, to date no suitably large void was found at higher redshifts $z > 0.3$. Here we report the detection of an $R =(192 \pm 15) h^{-1}Mpc$ size supervoid of depth $\delta = -0.13 \pm 0.03$, and centred at redshift $z = 0.22$. This supervoid, possibly the largest ever found, is large enough to significantly affect the CMB via the non-linear RS effect, as shown in our Lemaitre-Tolman-Bondi framework. This discovery presents the first plausible explanation for any of the physical CMB anomalies, and raises the possibility that local large-scale structure could be responsible for other anomalies as well., Comment: 8 pages, 4 figures, to appear in the proceedings of the Moriond Cosmology Conference 2014

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