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11 results on '"Nick Mostek"'

1. Investigating emission-line galaxy surveys with the Sloan Digital Sky Survey infrastructure

Author

Claudia Maraston, F. Lamareille, Johan Comparat, Jian Ge, Daniel Thomas, David J. Schlegel, Alexie Leauthaud, Stephanie Escoffier, Anne Ealet, Will J. Percival, Adam S. Bolton, Stephen Bailey, Joel R. Brownstein, Jean-Paul Kneib, Jeremy L. Tinker, Donald P. Schneider, Kyle S. Dawson, Julien Zoubian, Nick Mostek, Nicholas P. Ross, Éric Aubourg, Oliver Steele, C. Schimd, Benjamin A. Weaver, and Olivier Ilbert

Subjects
Physics, 010308 nuclear & particles physics, Standard ruler, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift survey, 01 natural sciences, Galaxy, Cosmology, Redshift, Metric expansion of space, Space and Planetary Science, Observational cosmology, 0103 physical sciences, Baryon acoustic oscillations, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The Baryon Acoustic Oscillation (BAO) feature in the power spectrum of galaxies can be used as a standard ruler to probe the accelerated expansion of the Universe. The current surveys covering a comoving volume sufficient to unveil the BAO scale are limited to redshift $z \lesssim 0.7$. In this paper, we study several galaxy selection schemes aiming at building an emission-line-galaxy (ELG) sample in the redshift range $0.6

Published
2012
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2. Reducing zero-point systematics in dark energy supernova experiments

Author

Chris Stoughton, Albert Stebbins, William Carithers, Ramon Miquel, Susana E. Deustua, David Tucker, Natalia Connolly, D. W. Gerdes, Eric V. Linder, Alain Bonissent, Gary Bernstein, Shawn McKee, Matthew Brown, G. Kushner, Hemant Shukla, Nick Mostek, Lorenzo Faccioli, L. Gladney, Jodi L. Christiansen, Alex G. Kim, 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), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), RENOIR, and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Cosmic distance ladder, Astrophysics::Instrumentation and Methods for Astrophysics, Scalar field dark matter, FOS: Physical sciences, Zero-point energy, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Supernova, 0103 physical sciences, Calibration, Dark energy, Satellite, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the effect of filter zero-point uncertainties on future supernova dark energy missions. Fitting for calibration parameters using simultaneous analysis of all Type Ia supernova standard candles achieves a significant improvement over more traditional fit methods. This conclusion is robust under diverse experimental configurations (number of observed supernovae, maximum survey redshift, inclusion of additional systematics). This approach to supernova fitting considerably eases otherwise stringent mission calibration requirements. As an example we simulate a space-based mission based on the proposed JDEM satellite; however the method and conclusions are general and valid for any future supernova dark energy mission, ground or space-based., 30 pages,8 figures, 5 table, one reference added, submitted to Astroparticle Physics

Published
2011
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3. Stochastic bias of colour-selected BAO tracers by joint clustering-weak lensing analysis

Author

Jean-Paul Kneib, Eric Jullo, Jeffrey A. Newman, Carlos Brandt, David J. Schlegel, Bruno Moraes, Huanyuan Shan, Anne Ealet, Donald P. Schneider, Nick Mostek, Joel R. Brownstein, Stephanie Escoffier, Maria E. S. Pereira, Johan Comparat, Thomas Erben, Francisco Prada, C. Schimd, Olivier Ilbert, Laboratoire d'Astrophysique de Marseille (LAM), 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), 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), BOSS, and 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)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, 01 natural sciences, dark matter, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Galaxy group, 0103 physical sciences, Brightest cluster galaxy, Interacting galaxy, 010303 astronomy & astrophysics, Lenticular galaxy, Weak gravitational lensing, galaxies: statistics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Galaxy, galaxies: haloes, Space and Planetary Science, cosmology: observations, Baryon acoustic oscillations, large-scale structure of Universe, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The baryon acoustic oscillation (BAO) feature in the two-point correlation function of galaxies supplies a standard ruler to probe the expansion history of the Universe. We study here several galaxy selection schemes, aiming at building an emission-line galaxy (ELG) sample in the redshift range $0.61.5$), but we are limited by current data sets depth to derive precise values of the galaxy bias. A survey using such tracers of the mass field will guarantee a high significance detection of the BAO., Comment: 17 pages, 15 figures, submitted to MNRAS

Published
2013
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4. Mapping the universe with BigBOSS

Author

K. Barbary, Patrick McDonald, Michael Levi, Michael Sholl, Michael Lampton, Patrick N. Jelinsky, Claire Poppett, Alex G. Kim, David J. Schlegel, Jerry Edelstein, Nick Mostek, Natalie A. Roe, Arjun Dey, and Chris Bebek

Subjects
Physics, Galactic astronomy, Standard ruler, Dark energy, Astronomy, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Baryon acoustic oscillations, Astrophysics, Redshift survey, Astrophysics::Galaxy Astrophysics, Galaxy, Redshift
Abstract

[The BigBOSS experiment is a redshift survey designed to map the large scale structure of the universe and probe the nature of dark energy. Using massively-multiplexed _ber spectroscopy over 14,000 deg2 of sky, the survey will deliver more than 20 million galaxy and quasar redshifts. The resulting three dimensional sky map will contain signatures from primordial baryon acoustic oscillations (BAO) that set a "standard ruler" distance scale. Using the BAO signature, BigBOSS will measure the cosmological distance scale to < 1% accuracy from 0.5

Published
2012
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5. The BigBOSS Experiment

Author

Timothy M. Heckman, D. H. Weinberg, Saul Perlmutter, Jeffrey A. Newman, S. LeBohec, Peter Nugent, Brice Ménard, D. Eppelle, Jason X. Prochaska, S. R. Majewski, X. Yang., Michael Schubnell, C. Schimd, David Kieda, H. Heetderks, Javier Sánchez, Ch Yèche, M. Azzaro, M. E. Levi, P. Jelinsky, Chong H. Ahn, Nick Mostek, P. Doel, U. Seljak, Alex G. Kim, Antonio D. Montero-Dorta, M. L. Lampton, C. Tao, Natalie A. Roe, Celine Peroux, H. T. Diehl, Sheila G. Bailey, Benjamin C. Bromley, C. Magneville, G. Rudnick, Dragan Huterer, C. Frenk, R. Mccloskey, O. Lahav, Anne Ealet, C. Allende Prieto, N. Palanque-Delabrouille, David J. Schlegel, R. N. Cahn, Anze Slosar, Marla Geha, J. Annis, H. Lim, Thomas Matheson, D. W. Gerdes, S. Becerril, Will J. Percival, I. Morales, Jordi Miralda-Escudé, J. Tinker, M. Liang, Kevin Reil, Alexander S. Szalay, F. B. Abdalla, M. Wood-Vasey, Marina Cortês, M. R. Blanton, C. Li, P. H. Carton, Nadia L. Zakamska, J. Yang, F. Valdes, W. Springer, Éric Aubourg, W. Lin, A. de la Macorra, N. Ross, Arthur Kosowsky, Steve Kent, Inese I. Ivans, C. Baltay, August E. Evrard, I. Park, Pengjie Zhang, Maryam Modjaz, Nikhil Padmanabhan, Mark Dickinson, Dick Joyce, Bruce Grossan, Michael Sholl, Francisco Prada, V. Le Brun, Chris Bebek, O. Ilbert, D. Sawyer, Kyle Dawson, D. S. Smith, John A. Peacock, Martin White, C. Marinoni, Emmanuel Rollinde, Andrew R. Zentner, R. Scoccimaro, L. Faccioli, Vicent J. Martínez, Jeff McMahon, K. Honscheid, K. A. G. Olsen, P. Petitjean, George F. Smoot, Patrick McDonald, Wolfgang Lorenzon, Roger F. Malina, Y. Jing, G. Tarle, Y. Chu, B. A. Weaver, Stephanie Escoffier, Eric Prieto, Hee-Jong Seo, Arjun Dey, Jerry Edelstein, Erin Sheldon, Antonio González-Arroyo, Adam S. Bolton, C. M. Rockosi, A. Roodman, Carlton M. Baugh, Tinggui Wang, J. P. Kneib, R. Nichol, C. Zhai, K. Krishnan, V. Ruhlmann-Kleider, Eric V. Linder, A. Stril, P. Gondolo, Timothy A. McKay, Jorge L. Cervantes-Cota, R. Shulte-Ladbeck, J. Wang, Tony Abraham, A. Tilquin, C. Kim, Shirley Ho, Xu Kong, R. D. Kennedy, E. N. Taylor, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-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)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Laboratoire d'Astrophysique de Marseille (LAM), 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), Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Cristofol, Danielle, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-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)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU)

Subjects
Physics, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010308 nuclear & particles physics, Dark matter, Astronomy, Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift survey, 01 natural sciences, 7. Clean energy, Redshift, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Redshift-space distortions, [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 13. Climate action, 0103 physical sciences, Dark energy, Baryon acoustic oscillations, [PHYS.ASTR.IM] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

This report is based on the BigBOSS proposal submission to NOAO in October 2010, and reflects the project status at that time with minor updates; BigBOSS is a Stage IV ground-based dark energy experiment to study baryon acoustic oscillations (BAO) and the growth of structure with a wide-area galaxy and quasar redshift survey over 14,000 square degrees. It has been conditionally accepted by NOAO in response to a call for major new instrumentation and a high-impact science program for the 4-m Mayall telescope at Kitt Peak. The BigBOSS instrument is a robotically-actuated, fiber-fed spectrograph capable of taking 5000 simultaneous spectra over a wavelength range from 340 nm to 1060 nm, with a resolution R = 3000-4800. Using data from imaging surveys that are already underway, spectroscopic targets are selected that trace the underlying dark matter distribution. In particular, targets include luminous red galaxies (LRGs) up to z = 1.0, extending the BOSS LRG survey in both redshift and survey area. To probe the universe out to even higher redshift, BigBOSS will target bright [OII] emission line galaxies (ELGs) up to z = 1.7. In total, 20 million galaxy redshifts are obtained to measure the BAO feature, trace the matter power spectrum at smaller scales, and detect redshift space distortions. BigBOSS will provide additional constraints on early dark energy and on the curvature of the universe by measuring the Ly-alpha forest in the spectra of over 600,000 2.2 < z < 3.5 quasars. BigBOSS galaxy BAO measurements combined with an analysis of the broadband power, including the Ly-alpha forest in BigBOSS quasar spectra, achieves a FOM of 395 with Planck plus Stage III priors. This FOM is based on conservative assumptions for the analysis of broad band power (kmax = 0.15), and could grow to over 600 if current work allows us to push the analysis to higher wave numbers (kmax = 0.3). BigBOSS will also place constraints on theories of modified gravity and inflation, and will measure the sum of neutrino masses to 0.024 eV accuracy.

Published
2011

6. BigBOSS: The Ground-Based Stage IV BAO Experiment

Author

Saul Perlmutter, Martin White, Natalie A. Roe, Michael Sholl, Tony Abraham, Knut Olsen, Samir Salim, Mike Merrill, Michael Levi, Michael Lampton, Nick Mostek, Buell T. Jannuzi, Arjun Dey, Ming Liang, Nikhil Padmanabhan, H. Heetderks, David J. Schlegel, Chris Bebek, Shirley Ho, Dick Joyce, and George F. Smoot

Subjects
Baryon, Redshift-space distortions, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Dark energy, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Baryon acoustic oscillations, Redshift survey, Spectrograph, Galaxy, Redshift
Abstract

The BigBOSS experiment is a proposed DOE-NSF Stage IV ground-based dark energy experiment to study baryon acoustic oscillations (BAO) and the growth of structure with an all-sky galaxy redshift survey. The project is designed to unlock the mystery of dark energy using existing ground-based facilities operated by NOAO. A new 4000-fiber R=5000 spectrograph covering a 3-degree diameter field will measure BAO and redshift space distortions in the distribution of galaxies and hydrogen gas spanning redshifts from 0.2< z< 3.5. The Dark Energy Task Force figure of merit (DETF FoM) for this experiment is expected to be equal to that of a JDEM mission for BAO with the lower risk and cost typical of a ground-based experiment.

Published
2009
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7. Supernova / Acceleration Probe: a Satellite Experiment to Study the Nature of the Dark Energy

Author

William W. Craig, Eric Prieto, A. L. Spadafora, A. S. Fruchter, T. Diehl, Gregory Tarle, M. E. Levi, N. Palaio, Susana E. Deustua, Josh Frieman, G. Samdja, Alain Mazure, M. L. Lampton, L. Gladney, Armin Karcher, H. Heetderks, N. Kuznetsova, Eric V. Linder, Edvard Mörtsell, D. W. Gerdes, Douglas L. Tucker, Christopher Stoughton, O. Le Fevre, Saul Perlmutter, Michael L. Brown, Steven E. Kahn, J. I. Lamoureux, Guofeng Wang, Scott Dodelson, Roger F. Malina, D. Rusin, Natalie A. Roe, C. Baltay, Nick Mostek, Dragan Huterer, G. Goldhaber, S. C. Loken, J. P. Marriner, R. Lafever, Hakeem M. Oluseyi, Ralph C. Bohlin, S. T. Holland, A. D. Tomasch, H. von der Lippe, Bhuvnesh Jain, Patrick N. Jelinsky, G. Kushner, E. Basa, John Peoples, Peter Nugent, Jason Rhodes, J. Annis, Greg Aldering, R. Pain, B. Krieger, Alain Bonissent, Keith Taylor, C. R. Bower, F. DeJongh, S. L. Mufson, V. Scarpine, E. Barrelet, D. E. Groom, J.-P. Walder, W. Emmet, Michael Sholl, L. Hui, Lars Bergström, Gary Bernstein, J. A. Musser, W. C. Wester, D. Rabinowitz, M. Hoff, Shawn McKee, J. Snyder, Andrew Szymkowiak, Eugene D. Commins, David H. Pankow, Philip J. Marshall, Timothy A. McKay, N. Morgan, Manfred Bester, Wolfgang Lorenzon, C. T. Day, Andre Tilquin, M.E. Huffer, Roger Smith, Dominique Fouchez, D. Vincent, M. Campbell, A. Goobar, Steve Kent, A. Stebbine, Richard Ellis, Ramon Miquel, William Carithers, Richard Massey, Roger Blandford, Alex G. Kim, P. Limon, H. Lin, A. Refregier, Chris Bebek, Anne Ealet, Pierre Astier, W. Althouse, William F. Kolbe, Michael Schubnell, Rahman Amanullah, George F. Smoot, and C. Bigelow

Subjects
Physics, 010308 nuclear & particles physics, Astronomy, Shape of the universe, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmological constant, Astrophysics, 7. Clean energy, 01 natural sciences, Galaxy, Redshift, Gravitational lens, Vacuum energy, 13. Climate action, 0103 physical sciences, Dark energy, 010303 astronomy & astrophysics, Weak gravitational lensing
Abstract

The Supernova/Acceleration Probe (SNAP) is a proposed space-based experiment designed to study the dark energy and alternative explanations of the acceleration of the Universe's expansion by performing a series of complementary systematics-controlled astrophysical measurements. We here describe a self-consistent reference mission design that can accomplish this goal with the two leading measurement approaches being the Type Ia supernova Hubble diagram and a wide-area weak gravitational lensing survey. This design has been optimized to first order and is now under study for further modification and optimization. A 2-m three-mirror anastigmat wide-field telescope feeds a focal plane consisting of a 0.7 square-degree imager tiled with equal areas of optical CCDs and near infrared sensors, and a high-efficiency low-resolution integral field spectrograph. The instrumentation suite provides simultaneous discovery and light-curve measurements of supernovae and then can target individual objects for detailed spectral characterization. The SNAP mission will discover thousands of Type Ia supernovae out to z = 3 and will obtain high-signal-to-noise calibrated light-curves and spectra for a subset of > 2000 supernovae at redshifts between z = 0.1 and 1.7 in a northern field and in a southern field. A wide-field survey covering one thousand square degrees in both northern and southern fields resolves {approx} 100 galaxies per square arcminute, or a total of more than 300 million galaxies. With the PSF stability afforded by a space observatory, SNAP will provide precise and accurate measurements of gravitational lensing. The high-quality data available in space, combined with the large sample of supernovae, will enable stringent control of systematic uncertainties. The resulting data set will be used to determine the energy density of dark energy and parameters that describe its dynamical behavior. The data also provide a direct test of theoretical models for the dark energy, including discrimination of vacuum energy due to the cosmological constant and various classes of dynamical scalar fields. If we assume we live in a cosmological-constant-dominated Universe, the matter density, dark energy density, and flatness of space can all be measured with SNAP supernova and weak-lensing measurements to a systematics-limited accuracy of 1%. For a flat universe, the density-to-pressure ratio of dark energy or equation of state w(z) can be similarly measured to 5% for the present value w{sub 0} and {approx} 0.1 for the time variation w' {triple_bond} dw/d ln a|{sub z=1}. For a fiducial SUGRA-inspired universe, w{sub 0} and w' can be measured to an even tighter uncertainty of 0.03 and 0.06 respectively. Note that no external priors are needed. As more accurate theoretical predictions for the small-scale weak-lensing shear develop, the conservative estimates adopted here for space-based systematics should improve, allowing even tighter constraints. While the survey strategy is tailored for supernova and weak gravitational lensing observations, the large survey area, depth, spatial resolution, time-sampling, and nine-band optical to NIR photometry will support additional independent and/or complementary dark-energy measurement approaches as well as a broad range of auxiliary science programs.

Published
2005
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8. Supernova Acceleration Probe: Studying Dark Energy with Type Ia Supernovae

Author

P. Limon, Albert Stebbins, Ralph C. Bohlin, Douglas L. Tucker, Armin Karcher, H. Heetderks, Edvard Mörtsell, H. Lin, G. Smadja, J. Musser, C. T. Day, T. Davies, Andre Tilquin, H. von der Lippe, B. Besuner, Martin White, Justin Albert, M. L. Lampton, N. Kuznetsova, A. Refregier, N. Palaio, Susana E. Deustua, L. Gladney, G. Goldhaber, Alex G. Kim, Roger F. Malina, Nick Mostek, Chris Bebek, V. Scarpine, D. Cole, William Carithers, A. D. Tomasch, Richard Massey, Bhuvnesh Jain, Keith Taylor, Roger Blandford, J. P. Marriner, Greg Aldering, David H. Pankow, Michael Seiffert, Eric Prieto, C. R. Bower, Alain Bonissent, Peter Nugent, D. Figer, R. Lafever, John Peoples, D. Vincent, M. Campbell, Stephen Bailey, Michael Sholl, B. Krieger, Alain Mazure, J. I. Lamoureux, M.E. Huffer, Anne Ealet, N. Morgan, S. C. Loken, Dominique Fouchez, A. S. Fruchter, M. Deharveng, V. Lebrun, O. Le Fevre, F. DeJongh, Guofeng Wang, Andrew Szymkowiak, J. Snyder, L. Marian, D. Rusin, Natalie A. Roe, Wolfgang Lorenzon, M. E. Levi, P. Jelinsky, Ramon Miquel, E. Barrelet, L. Hui, W. Emmet, R. Nakajima, Roger Smith, G. Tarle, C. Baltay, Stéphane Basa, Michael L. Brown, Hakeem M. Oluseyi, Christopher Stoughton, S. Allam, S. L. Mufson, M. Frerking, Steven E. Kahn, C. Juramy, W. C. Wester, D. Rabinowitz, D. Peterson, Scott Dodelson, Lars Bergström, H. Shuka, F. Stabenau, B. Bigelow, A. Goobar, Michael Schubnell, B. Mcginnis, M. Hoff, D. E. Groom, Steve Kent, Rahman Amanullah, J.-P. Walder, Saul Perlmutter, Richard Ellis, G. Kushner, Eugene D. Commins, Manfred Bester, Gary Bernstein, Shawn McKee, M. Aumeunier, Philip J. Marshall, A. L. Spadafora, T. Dobson, T. Diehl, B. Mobqsher, D. W. Gerdes, Pierre Astier, W. Althouse, William F. Kolbe, Josh Frieman, Eric V. Linder, Timothy A. McKay, George F. Smoot, William W. Craig, Dragan Huterer, S. T. Holland, A. Weinstein, Jason Rhodes, J. Annis, R. Pain, 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), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-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), SNAP, Flores, Sylvie, Université Claude Bernard Lyon 1 (UCBL), and 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)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, 7. Clean energy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Acceleration, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, Computer Science::Distributed, Parallel, and Cluster Computing, media_common, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy, Universe, Supernova, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Dark energy
Abstract

The Supernova Acceleration Probe (SNAP) will use Type Ia supernovae (SNe Ia) as distance indicators to measure the effect of dark energy on the expansion history of the Universe. (SNAP's weak-lensing program is described in a companion White Paper.) The experiment exploits supernova distance measurements up to their fundamental systematic limit; strict requirements on the monitoring of each supernova's properties lead to the need for a space-based mission. Results from pre-SNAP experiments, which characterize fundamental SN Ia properties, will be used to optimize the SNAP observing strategy to yield data, which minimize both systematic and statistical uncertainties. SNAP has achieved technological readiness and the collaboration is poised to begin construction., Comment: 12 pages, 4 figures; White paper to the Dark Energy Task Force

Published
2005
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9. Probing Dark Energy via Weak Gravitational Lensing with the SuperNova Acceleration Probe (SNAP)

Author

Greg Aldering, M. Hoff, Ralph C. Bohlin, S. L. Mufson, Andrew Szymkowiak, L. Gladney, O. Le Fevre, D. Cole, Nick Mostek, N. Palaio, Susana E. Deustua, Wolfgang Lorenzon, P. Limon, M. L. Lampton, Dragan Huterer, Scott Dodelson, N. Kuznetsova, Alain Mazure, H. Shuka, S. T. Holland, F. Stabenau, Josh Frieman, Roger Smith, Guofeng Wang, T. Davies, B. Besuner, Martin White, A. Weinstein, Roger F. Malina, Jason Rhodes, J. Annis, R. Lafever, G. Kushner, J. Albert, H. Lin, Saul Perlmutter, Lars Bergström, G. Smadja, R. Pain, Eric V. Linder, B. Krieger, John Peoples, A. D. Tomasch, B. Bigelow, J. Musser, Peter Nugent, A. Refregier, William W. Craig, L. Marian, H. von der Lippe, Michael Seiffert, D. E. Groom, Keith Taylor, Timothy A. McKay, Eric Prieto, Chris Bebek, C. R. Bower, D. Peterson, Albert Stebbins, G. Tarle, Stephen Bailey, J. I. Lamoureux, Christopher Stoughton, J.-P. Walder, F. DeJongh, Alex G. Kim, W. Emmet, Eugene D. Commins, V. Scarpine, M. Frerking, Gary Bernstein, A. Goobar, Douglas L. Tucker, Michael Schubnell, C. T. Day, Andre Tilquin, D. Figer, Shawn McKee, Edvard Mörtsell, Rahman Amanullah, M. Deharveng, Dominique Fouchez, W. C. Wester, D. Rabinowitz, M.E. Huffer, R. Nakajima, J. Snyder, T. Dobson, Armin Karcher, Stéphane Basa, Michael L. Brown, David H. Pankow, Steven E. Kahn, Anne Ealet, C. Juramy, Steve Kent, A. S. Fruchter, S. C. Loken, G. Goldhaber, Bhuvnesh Jain, Alain Bonissent, M. Aumeunier, Philip J. Marshall, J. P. Marriner, M. E. Levi, E. Barrelet, P. Jelinsky, Michael Sholl, A. L. Spadafora, L. Hui, T. Diehl, B. Mcginnis, Richard Ellis, B. Mobqsher, V. Lebrun, S. Allam, William Carithers, George F. Smoot, Richard Massey, Roger Blandford, Pierre Astier, W. Althouse, William F. Kolbe, D. W. Gerdes, D. Rusin, Natalie A. Roe, Ramon Miquel, N. Morgan, H. Heetderks, Manfred Bester, D. Vincent, M. Campbell, C. Baltay, Hakeem M. Oluseyi, Flores, Sylvie, 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), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-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), SNAP, Université Claude Bernard Lyon 1 (UCBL), and 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)

Subjects
Point spread function, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, law.invention, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], law, 0103 physical sciences, 010306 general physics, Weak gravitational lensing, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Redshift, Galaxy, Supernova, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Dark energy, Joint Dark Energy Mission
Abstract

SNAP is a candidate for the Joint Dark Energy Mission (JDEM) that seeks to place constraints on the dark energy using two distinct methods. The first, Type Ia SN, is discussed in a companion white paper. The second method is weak gravitational lensing, which relies on the coherent distortions in the shapes of background galaxies by foreground mass structures. The excellent spatial resolution and photometric accuracy afforded by a 2-meter space-based observatory are crucial for achieving the high surface density of resolved galaxies, the tight control of systematic errors in the telescope's Point Spread Function (PSF), and the exquisite redshift accuracy and depth required by this project. These are achieved by the elimination of atmospheric distortion and much of the thermal and gravity loads on the telescope. The SN and WL methods for probing dark energy are highly complementary and the error contours from the two methods are largely orthogonal., 17 pages, 6 figures; White paper to the Dark Energy Task Force

Published
2005

10. SNAP telescope: an update

Author

Ralph C. Bohlin, D. Fouchez, Edvard Mörtsell, Robert Besuner, Alex G. Kim, J. Bercovitz, Nick Mostek, Michael H. Krim, Armin Karcher, Michael Schubnell, Myron Campbell, Keith Taylor, William Carithers, Alain Mazure, S. Mufson, William Emmett, Charles R. Bower, Eric V. Linder, Michael Levi, Rahman Amanullah, N. Morgan, J. A. Musser, Carl W. Akerlof, R. Lafever, Stéphane Basa, Timothy A. McKay, Guobin Wang, George F. Smoot, Henrik von der Lippe, Ariel Goobar, Peter Nugent, D. Vincent, Donald E. Groom, Pierre Astier, Daniel Levin, Jean-Pierre Walder, William E. Johnston, N. Palaio, Susana E. Deustua, William F. Kolbe, J. I. Lamoureux, Gary Berstein, J.F. Genat, Ramon Miquel, Stephen Holland, David H. Pankow, J. Snyder, H. Heetderks, Saul Perlmutter, Andre Tilquin, M. Eriksson, S. C. Loken, E. Barrelet, Greg Aldering, G. Smadja, R. W. Kadel, C. Baltay, Richard S. Ellis, Chris Bebek, Hakeem M. Oluseyi, David Rabinowitz, Dragan Huterer, Jason Rhodes, Andrew Szymkowiak, Manfred Bester, Lars Bergström, C. T. Day, Roger Smith, Eugene D. Commins, Reynald Pain, A. L. Spadafora, G. Goldhaber, Shawn McKee, Roger F. Malina, Andrew S. Fruchter, A. D. Tomasch, Anne Ealet, Gregory Tarle, R. DiGennaro, Alain Bonissent, Alexandre Refregier, Michael Sholl, Eric Prieto, Natalie A. Roe, Oliver LeFevre, Michael Lampton, and MacEwen, Howard A.

Subjects
Physics, Wavefront, business.industry, Stray light, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Anastigmat, Astronomy, Three-mirror anastigmat, Astrophysics::Cosmology and Extragalactic Astrophysics, Orbital mechanics, Redshift, law.invention, Telescope, Optics, law, Astrophysics::Solar and Stellar Astrophysics, Adaptive optics, business, Astrophysics::Galaxy Astrophysics
Abstract

We present the baseline telescope design for the telescope for the SuperNova/Acceleration Probe (SNAP) space mission. SNAP’s purpose is to determine expansion history of the Universe by measuring the redshifts, magnitudes, and spectral classifications of thousands of supernovae with unprecedented accuracy. Discovering and measuring these supernovae demand both a wide optical field and a high sensitivity throughout the visible and near IR wavebands. We have adopted the annular-field three-mirror anastigmat (TMA) telescope configuration, whose classical aberrations (including chromatic) are zero. We show a preliminary optmechanical design that includes important features for stray light control and on-orbit adjustment and alignment of the optics. We briefly discuss stray light and tolerance issues, and present a preliminary wavefront error budget for the SNAP Telescope. We conclude by describing some of the design tasks being carried out during the current SNAP research and development phase.

Published
2004
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11. Weak lensing from space I: instrumentation and survey strategy

Author

S. Harris, H. von der Lippe, Dominique Fouchez, Lars Bergström, C. T. Day, Alex G. Kim, B. Bigelow, Chris Bebek, Myron Campbell, A. L. Spadafora, Saul Perlmutter, Eric Prieto, R. Pratt, M. L. Lampton, S.E. Holland, G. Smadja, A. S. Fruchter, Armin Karcher, B. Krieger, J.-P. Walder, N. Morgan, Gary Bernstein, Peter Nugent, C. Baltay, Eric V. Linder, Shawn McKee, Ariel Goobar, Justin Albert, William E. Johnston, Timothy A. McKay, Hakeem M. Oluseyi, N. Palaio, Susana E. Deustua, Greg Aldering, J. Bercovitz, Nick Mostek, George F. Smoot, David Rabinowitz, Roger F. Malina, Pierre Astier, David Bacon, Keith Taylor, C. R. Bower, William F. Kolbe, R. Lafever, Andrew Szymkowiak, H. Heetderks, David H. Pankow, A. D. Tomasch, G. Kushner, J. A. Musser, Wolfgang Lorenzon, Peter Harvey, D. Rusin, Natalie A. Roe, W. Emmet, Anne Ealet, Roger Smith, S. C. Loken, Ramon Miquel, Edvard Mörtsell, Gerson Goldhaber, E. Barrelet, R. DiGennaro, Alain Bonissent, M. E. Levi, Andre Tilquin, S. L. Mufson, Alexandre Refregier, M. Eriksson, Michael Sholl, Manfred Bester, Richard S. Ellis, Bhuvnesh Jain, D. W. Gerdes, William Carithers, Richard Massey, L. Gladney, D. Vincent, Guofeng Wang, Alain Mazure, Michael Schubnell, Carl W. Akerlof, Rahman Amanullah, Eugene D. Commins, Reynald Pain, Donald E. Groom, J. F. Genat, K. Robinson, Gregory Tarle, Dragan Huterer, Michael E. Brown, J. I. Lamoureux, Ralph C. Bohlin, J. Snyder, N. Kuznetsova, Jason Rhodes, 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), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-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), California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Mathematics [Berkeley], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Engineering [Edinburgh], University of Edinburgh, 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), Department of Physics, Stockholm University, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), 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), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Dispositifs et Instrumentation en Optoélectronique et micro-ondes (DIOM), Université Jean Monnet - Saint-Étienne (UJM), Dept Mat Sci & Engn, Zhejiang University, California Institute of Technology (CALTECH)-NASA, University of California [Berkeley], University of California-University of California, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Harvard University [Cambridge]-Smithsonian Institution, DIOM (DIOM), and Université Jean Monnet [Saint-Étienne] (UJM)

Subjects
Point spread function, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, law.invention, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Spitzer Space Telescope, law, 0103 physical sciences, Dark energy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Instrumentation, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Supernova
Abstract

A wide field space-based imaging telescope is necessary to fully exploit the technique of observing dark matter via weak gravitational lensing. This first paper in a three part series outlines the survey strategies and relevant instrumental parameters for such a mission. As a concrete example of hardware design, we consider the proposed Supernova/Acceleration Probe (SNAP). Using SNAP engineering models, we quantify the major contributions to this telescope's Point Spread Function (PSF). These PSF contributions are relevant to any similar wide field space telescope. We further show that the PSF of SNAP or a similar telescope will be smaller than current ground-based PSFs, and more isotropic and stable over time than the PSF of the Hubble Space Telescope. We outline survey strategies for two different regimes - a ``wide'' 300 square degree survey and a ``deep'' 15 square degree survey that will accomplish various weak lensing goals including statistical studies and dark matter mapping., 25 pages, 8 figures, 1 table, replaced with Published Version

Published
2004
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