Search

Your search keyword '"Biswas, Rahul"' showing total 13 results
Start Over Author "Biswas, Rahul" Topic fos: physical sciences
13 results on '"Biswas, Rahul"'

1. DESC DC2 Data Release Note

Author

LSST Dark Energy Science Collaboration, Abolfathi, Bela, Armstrong, Robert, Awan, Humna, Babuji, Yadu N., Bauer, Franz Erik, Beckett, George, Biswas, Rahul, Bogart, Joanne R., Boutigny, Dominique, Chard, Kyle, Chiang, James, Cohen-Tanugi, Johann, Connolly, Andrew J., Daniel, Scott F., Digel, Seth W., Drlica-Wagner, Alex, Dubois, Richard, Gawiser, Eric, Glanzman, Thomas, Habib, Salman, Hearin, Andrew P., Heitmann, Katrin, Hernandez, Fabio, Hložek, Renée, Hollowed, Joseph, Jarvis, Mike, Jha, Saurabh W., Kalmbach, J. Bryce, Kelly, Heather M., Kovacs, Eve, Korytov, Danila, Krughoff, K. Simon, Lage, Craig S., Lanusse, François, Larsen, Patricia, Li, Nan, Longley, Emily Phillips, Lupton, Robert H., Mandelbaum, Rachel, Mao, Yao-Yuan, Marshall, Phil, Meyers, Joshua E., Park, Ji Won, Peloton, Julien, Perrefort, Daniel, Perry, James, Plaszczynski, Stéphane, Pope, Adrian, Rykoff, Eli S., Sánchez, F. Javier, Schmidt, Samuel J., Uram, Thomas D., Villarreal, Antonia, Walter, Christopher W., Wiesner, Matthew P., Wood-Vasey, W. Michael, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), LSST Dark Energy Science, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and HEP, INSPIRE

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], FOS: Physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In preparation for cosmological analyses of the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST), the LSST Dark Energy Science Collaboration (LSST DESC) has created a 300 deg$^2$ simulated survey as part of an effort called Data Challenge 2 (DC2). The DC2 simulated sky survey, in six optical bands with observations following a reference LSST observing cadence, was processed with the LSST Science Pipelines (19.0.0). In this Note, we describe the public data release of the resulting object catalogs for the coadded images of five years of simulated observations along with associated truth catalogs. We include a brief description of the major features of the available data sets. To enable convenient access to the data products, we have developed a web portal connected to Globus data services. We describe how to access the data and provide example Jupyter Notebooks in Python to aid first interactions with the data. We welcome feedback and questions about the data release via a GitHub repository., Comment: 25 pages, 3 figures; 9 tables. A detailed changelog can be found in Appendix A. To obtain data, visit the DESC Data Portal at https://data.lsstdesc.org/

Published
2021

2. Dark Matter Science in the Era of LSST

Author

Bechtol, Keith, Drlica-Wagner, Alex, Abazajian, Kevork N., Abidi, Muntazir, Adhikari, Susmita, Ali-Haïmoud, Yacine, Annis, James, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Baccigalupi, Carlo, Banerjee, Arka, Banik, Nilanjan, Bennett, Charles, Beutler, Florian, Bird, Simeon, Birrer, Simon, Biswas, Rahul, Biviano, Andrea, Blazek, Jonathan, Boddy, Kimberly K., Bonaca, Ana, Borrill, Julian, Bose, Sownak, Bovy, Jo, Frye, Brenda, Brooks, Alyson M., Buckley, Matthew R., Buckley-Geer, Elizabeth, Bulbul, Esra, Burchat, Patricia R., Burgess, Cliff, Calore, Francesca, Caputo, Regina, Castorina, Emanuele, Chang, Chihway, Chapline, George, Charles, Eric, Chen, Xingang, Clowe, Douglas, Cohen-Tanugi, Johann, Comparat, Johan, Croft, Rupert Ac, Cuoco, Alessandro, Cyr-Racine, Francis-Yan, D Amico, Guido, Davis, Tamara M., Dawson, William A., Macorra, Axel La, Valentino, Eleonora Di, Rivero, Ana Díaz, Digel, Seth, Dodelson, Scott, Doré, Olivier, Dvorkin, Cora, Eckner, Christopher, Ellison, John, Erkal, Denis, Farahi, Arya, Fassnacht, Christopher D., Ferreira, Pedro G., Flaugher, Brenna, Foreman, Simon, Friedrich, Oliver, Frieman, Joshua, García-Bellido, Juan, Gawiser, Eric, Gerbino, Martina, Maurizio Giannotti, Gill, Mandeep Ss, Gluscevic, Vera, Golovich, Nathan, Gontcho, Satya Gontcho A., González-Morales, Alma X., Grin, Daniel, Gruen, Daniel, Hearin, Andrew P., Hendel, David, Hezaveh, Yashar D., Hirata, Christopher M., Hložek, Renee, Horiuchi, Shunsaku, Jain, Bhuvnesh, Jee, M. James, Jeltema, Tesla E., Kamionkowski, Marc, Kaplinghat, Manoj, Keeley, Ryan E., Keeton, Charles R., Khatri, Rishi, Koposov, Sergey E., Koushiappas, Savvas M., Kovetz, Ely D., Lahav, Ofer, Lam, Casey, Lee, Chien-Hsiu, Li, Ting S., Liguori, Michele, Lin, Tongyan, Lisanti, Mariangela, Loverde, Marilena, Lu, Jessica R., Mandelbaum, Rachel, Mao, Yao-Yuan, Mcdermott, Samuel D., Mcnanna, Mitch, Medford, Michael, Meerburg, P. Daniel, Meyer, Manuel, Mirbabayi, Mehrdad, Mishra-Sharma, Siddharth, Marc, Moniez, More, Surhud, Moustakas, John, Muñoz, Julian B., Murgia, Simona, Myers, Adam D., Nadler, Ethan O., Necib, Lina, Newburgh, Laura, Newman, Jeffrey A., Nord, Brian, Nourbakhsh, Erfan, Nuss, Eric, O Connor, Paul, Pace, Andrew B., Padmanabhan, Hamsa, Palmese, Antonella, Peiris, Hiranya V., Peter, Annika Hg, Piacentni, Francesco, Piacentini, Francesco, Plazas, Andrés, Polin, Daniel A., Prakash, Abhishek, Prescod-Weinstein, Chanda, Read, Justin I., Ritz, Steven, Robertson, Brant E., Rose, Benjamin, Rosenfeld, Rogerio, Rossi, Graziano, Samushia, Lado, Sánchez, Javier, Sánchez-Conde, Miguel A., Schaan, Emmanuel, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Shipp, Nora, Simon, Joshua D., Simon, Sara, Slatyer, Tracy R., Slosar, Anže, Sridhar, Srivatsan, Stebbins, Albert, Straniero, Oscar, Strigari, Louis E., Tait, Tim Mp, Tollerud, Erik, Troxel, Ma, Tyson, J. Anthony, Uhlemann, Cora, Urenña-López, L. Arturo, Verma, Aprajita, Vilalta, Ricardo, Walter, Christopher W., Wang, Mei-Yu, Watson, Scott, Wechsler, Risa H., Wittman, David, Xu, Weishuang, Yanny, Brian, Young, Sam, Yu, Hai-Bo, Zaharijas, Gabrijela, Zentner, Andrew R., Zuntz, Joe, 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), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and HEP, INSPIRE

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex], Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Compact star, 01 natural sciences, Standard Model, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Particle mass, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, hep-ex, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, 13. Climate action, Fundamental physics, astro-ph.CO, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Particle Physics - Experiment, dark matter: parameter space, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Astrophysical observations currently provide the only robust, empirical measurements of dark matter. In the coming decade, astrophysical observations will guide other experimental efforts, while simultaneously probing unique regions of dark matter parameter space. This white paper summarizes astrophysical observations that can constrain the fundamental physics of dark matter in the era of LSST. We describe how astrophysical observations will inform our understanding of the fundamental properties of dark matter, such as particle mass, self-interaction strength, non-gravitational interactions with the Standard Model, and compact object abundances. Additionally, we highlight theoretical work and experimental/observational facilities that will complement LSST to strengthen our understanding of the fundamental characteristics of dark matter., 11 pages, 2 figures, Science Whitepaper for Astro 2020, more information at https://lsstdarkmatter.github.io

Published
2019

3. Effects of Massive Neutrinos and Dynamical Dark Energy on the Cluster Mass Function

Author

Biswas, Rahul, Heitmann, Katrin, Habib, Salman, Upadhye, Amol, Pope, Adrian, and Frontiere, Nicholas

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

The presence of massive neutrinos affects the growth of large-scale structure in the universe, leaving a potentially observable imprint on the abundance and properties of massive dark matter-dominated halos. Cosmological surveys detect large numbers of these halos in the form of rich groups and clusters, using the information as an input to constraining the properties of dark energy. We use a suite of N-body simulations that include the effects of massive neutrinos as well as of dynamical dark energy to study the properties of the mass function. As in our previous work, we follow an approach valid at low neutrino mass, where the neutrino overdensities are assumed to be too small to act as a significant nonlinear source term for gravity. We study how well a universal form for the halo mass function describes our numerical results, finding that the use of an appropriate linear power spectrum within the formalism yields a good match to the simulation results, correctly accounting for the (neutrino mass-dependent) suppression of the mass function., 11 pages, 5 figures, to be submitted to PRD

Published
2019

4. Optimizing the LSST Observing Strategy for Dark Energy Science: DESC Recommendations for the Wide-Fast-Deep Survey

Author

Lochner, Michelle, Scolnic, Daniel M., Awan, Humna, Regnault, Nicolas, Gris, Philippe, Mandelbaum, Rachel, Gawiser, Eric, Almoubayyed, Husni, Setzer, Christian N., Huber, Simon, Graham, Melissa L., Hložek, Renée, Biswas, Rahul, Eifler, Tim, Rothchild, Daniel, Allam, Tarek, Blazek, Jonathan, Chang, Chihway, Collett, Thomas, Goobar, Ariel, Hook, Isobel M., Jarvis, Mike, Jha, Saurabh W., Kim, Alex G., Marshall, Phil, Mcewen, Jason D., Moniez, Marc, Newman, Jeffrey A., Hiranya Peiris, Petrushevska, Tanja, Rhodes, Jason, Sevilla-Noarbe, Ignacio, Slosar, Anže, Suyu, Sherry H., Tyson, J. Anthony, Yoachim, Peter, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), LSST Dark Energy Science, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), astro-ph.IM
Abstract

Cosmology is one of the four science pillars of LSST, which promises to be transformative for our understanding of dark energy and dark matter. The LSST Dark Energy Science Collaboration (DESC) has been tasked with deriving constraints on cosmological parameters from LSST data. Each of the cosmological probes for LSST is heavily impacted by the choice of observing strategy. This white paper is written by the LSST DESC Observing Strategy Task Force (OSTF), which represents the entire collaboration, and aims to make recommendations on observing strategy that will benefit all cosmological analyses with LSST. It is accompanied by the DESC DDF (Deep Drilling Fields) white paper (Scolnic et al.). We use a variety of metrics to understand the effects of the observing strategy on measurements of weak lensing, large-scale structure, clusters, photometric redshifts, supernovae, strong lensing and kilonovae. In order to reduce systematic uncertainties, we conclude that the current baseline observing strategy needs to be significantly modified to result in the best possible cosmological constraints. We provide some key recommendations: moving the WFD (Wide-Fast-Deep) footprint to avoid regions of high extinction, taking visit pairs in different filters, changing the 2x15s snaps to a single exposure to improve efficiency, focusing on strategies that reduce long gaps (>15 days) between observations, and prioritizing spatial uniformity at several intervals during the 10-year survey., The LSST DESC response (WFD) to the Call for White Papers on LSST Cadence Optimization. Comments welcome

Published
2018

5. Optimizing the LSST Observing Strategy for Dark Energy Science: DESC Recommendations for the Deep Drilling Fields and other Special Programs

Author

Scolnic, Daniel M., Lochner, Michelle, Gris, Phillipe, Regnault, Nicolas, Hlo��ek, Ren��e, Aldering, Greg, Allam, Tarek, Awan, Humna, Biswas, Rahul, Blazek, Jonathan, Chang, Chihway, Gawiser, Eric, Goobar, Ariel, Hook, Isobel M., Jha, Saurabh W., McEwen, Jason D., Mandelbaum, Rachel, Marshall, Phil, Neilsen, Eric, Rhodes, Jason, Rothchild, Daniel, Noarbe, Ignacio Sevilla, Slosar, An��e, Yoachim, Peter, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), LSST Dark Energy Science, Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS)

Subjects
FOS: Physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We review the measurements of dark energy enabled by observations of the Deep Drilling Fields and the optimization of survey design for cosmological measurements. This white paper is the result of efforts by the LSST DESC Observing Strategy Task Force (OSTF), which represents the entire collaboration, and aims to make recommendations on observing strategy for the DDFs that will benefit all cosmological analyses with LSST. It is accompanied by the DESC-WFD white paper (Lochner et al.). We argue for altering the nominal deep drilling plan to have $>6$ month seasons, interweaving $gri$ and $zy$ observations every 3 days with 2, 4, 8, 25, 4 visits in $grizy$, respectively. These recommendations are guided by metrics optimizing constraints on dark energy and mitigation of systematic uncertainties, including specific requirements on total number of visits after Y1 and Y10 for photometric redshifts (photo-$z$) and weak lensing systematics. We specify the precise locations for the previously-chosen LSST deep fields (ELAIS-S1, XMM-LSS, CDF-S, and COSMOS) and recommend Akari Deep Field South as the planned fifth deep field in order to synergize with Euclid and WFIRST. Our recommended DDF strategy uses $6.2\%$ of the LSST survey time. We briefly discuss synergy with white papers from other collaborations, as well as additional mini-surveys and Target-of-Opportunity programs that lead to better measurements of dark energy., The LSST DESC response (DDF) to the Call for White Papers on LSST Cadence Optimization. Comments welcome

Published
2018

6. The Photometric LSST Astronomical Time-series Classification Challenge (PLAsTiCC): Data set

Author

The PLAsTiCC Team, Allam, Tarek, Bahmanyar, Anita, Biswas, Rahul, Dai, Mi, Galbany, Llu��s, Hlo��ek, Ren��e, Ishida, Emille E. O., Jha, Saurabh W., Jones, David O., Kessler, Richard, Lochner, Michelle, Mahabal, Ashish A., Malz, Alex I., Mandel, Kaisey S., Mart��nez-Galarza, Juan Rafael, McEwen, Jason D., Muthukrishna, Daniel, Narayan, Gautham, Peiris, Hiranya, Peters, Christina M., Ponder, Kara, Setzer, Christian N., Collaboration, The LSST Dark Energy Science, Transients, The LSST, and Collaboration, Variable Stars Science

Subjects
Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The Photometric LSST Astronomical Time Series Classification Challenge (PLAsTiCC) is an open data challenge to classify simulated astronomical time-series data in preparation for observations from the Large Synoptic Survey Telescope (LSST), which will achieve first light in 2019 and commence its 10-year main survey in 2022. LSST will revolutionize our understanding of the changing sky, discovering and measuring millions of time-varying objects. In this challenge, we pose the question: how well can we classify objects in the sky that vary in brightness from simulated LSST time-series data, with all its challenges of non-representativity? In this note we explain the need for a data challenge to help classify such astronomical sources and describe the PLAsTiCC data set and Kaggle data challenge, noting that while the references are provided for context, they are not needed to participate in the challenge., Research note to accompany the https://www.kaggle.com/c/PLAsTiCC-2018 challenge

Published
2018

7. The LSST Dark Energy Science Collaboration (DESC) Science Requirements Document

Author

The LSST Dark Energy Science Collaboration, Mandelbaum, Rachel, Eifler, Tim, Hlo��ek, Ren��e, Collett, Thomas, Gawiser, Eric, Scolnic, Daniel, Alonso, David, Awan, Humna, Biswas, Rahul, Blazek, Jonathan, Burchat, Patricia, Chisari, Nora Elisa, Dell'Antonio, Ian, Digel, Seth, Frieman, Josh, Goldstein, Daniel A., Hook, Isobel, Ivezi��, ��eljko, Kahn, Steven M., Kamath, Sowmya, Kirkby, David, Kitching, Thomas, Krause, Elisabeth, Leget, Pierre-Fran��ois, Marshall, Philip J., Meyers, Joshua, Miyatake, Hironao, Newman, Jeffrey A., Nichol, Robert, Rykoff, Eli, Sanchez, F. Javier, Slosar, An��e, Sullivan, Mark, and Troxel, M. A.

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

The Large Synoptic Survey Telescope (LSST) Dark Energy Science Collaboration (DESC) will use five cosmological probes: galaxy clusters, large scale structure, supernovae, strong lensing, and weak lensing. This Science Requirements Document (SRD) quantifies the expected dark energy constraining power of these probes individually and together, with conservative assumptions about analysis methodology and follow-up observational resources based on our current understanding and the expected evolution within the field in the coming years. We then define requirements on analysis pipelines that will enable us to achieve our goal of carrying out a dark energy analysis consistent with the Dark Energy Task Force definition of a Stage IV dark energy experiment. This is achieved through a forecasting process that incorporates the flowdown to detailed requirements on multiple sources of systematic uncertainty. Future versions of this document will include evolution in our software capabilities and analysis plans along with updates to the LSST survey strategy., 32 pages + 60 pages of appendices. This is v1.0.2 of the DESC SRD, an internal collaboration document that is being made public and is not planned for submission to a journal. Data products for reproducing key plots are available on Zenodo, https://doi.org/10.5281/zenodo.1409815 ; see "Executive Summary and User Guide" for how to use and cite those products

Published
2018

8. The LSST Data Management System

Author

Jurić, Mario, Kantor, Jeffrey, Lim, K-T, Lupton, Robert H., Dubois-Felsmann, Gregory, Jenness, Tim, Axelrod, Tim S., Aleksić, Jovan, Allsman, Roberta A., AlSayyad, Yusra, Alt, Jason, Armstrong, Robert, Basney, Jim, Becker, Andrew C., Becla, Jacek, Bickerton, Steven J., Biswas, Rahul, Bosch, James, Boutigny, Dominique, Kind, Matias Carrasco, Ciardi, David R., Connolly, Andrew J., Daniel, Scott F., Daues, Gregory E., Economou, Frossie, Chiang, Hsin-Fang, Fausti, Angelo, Fisher-Levine, Merlin, Freemon, D. Michael, Gee, Perry, Gris, Philippe, Hernandez, Fabio, Hoblitt, Joshua, Ivezić, Željko, Jammes, Fabrice, Jevremović, Darko, Jones, R. Lynne, Kalmbach, J. Bryce, Kasliwal, Vishal P., Krughoff, K. Simon, Lang, Dustin, Lurie, John, Lust, Nate B., Mullally, Fergal, MacArthur, Lauren A., Melchior, Peter, Moeyens, Joachim, Nidever, David L., Owen, Russell, Parejko, John K, Peterson, J. Matt, Petravick, Donald, Pietrowicz, Stephen R., Price, Paul A., Reiss, David J., Shaw, Richard A., Sick, Jonathan, Slater, Colin T., Strauss, Michael A., Sullivan, Ian S., Swinbank, John D., Van Dyk, Schuyler, Vujčić, Veljko, Withers, Alexander, and Yoachim, Peter

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The Large Synoptic Survey Telescope (LSST) is a large-aperture, wide-field, ground-based survey system that will image the sky in six optical bands from 320 to 1050 nm, uniformly covering approximately $18,000$deg$^2$ of the sky over 800 times. The LSST is currently under construction on Cerro Pach\'on in Chile, and expected to enter operations in 2022. Once operational, the LSST will explore a wide range of astrophysical questions, from discovering "killer" asteroids to examining the nature of Dark Energy. The LSST will generate on average 15 TB of data per night, and will require a comprehensive Data Management system to reduce the raw data to scientifically useful catalogs and images with minimum human intervention. These reductions will result in a real-time alert stream, and eleven data releases over the 10-year duration of LSST operations. To enable this processing, the LSST project is developing a new, general-purpose, high-performance, scalable, well documented, open source data processing software stack for O/IR surveys. Prototypes of this stack are already capable of processing data from existing cameras (e.g., SDSS, DECam, MegaCam), and form the basis of the Hyper-Suprime Cam (HSC) Survey data reduction pipeline., Comment: 10 pages, 3 figures, to appear in the Proceedings of ADASS XXV

Published
2015
Full Text
View/download PDF

9. The reliability of the AIC method in Cosmological Model Selection

Author

Tan, Ming Yang Jeremy and Biswas, Rahul

Subjects
Statistics::Machine Learning, Statistics::Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Statistics::Applications, Physics - Data Analysis, Statistics and Probability, Statistics::Methodology, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Data Analysis, Statistics and Probability (physics.data-an), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Akaike information criterion (AIC) has been used as a statistical criterion to compare the appropriateness of different dark energy candidate models underlying a particular data set. Under suitable conditions, the AIC is an indirect estimate of the Kullback-Leibler divergence D(T//A) of a candidate model A with respect to the truth T. Thus, a dark energy model with a smaller AIC is ranked as a better model, since it has a smaller Kullback-Leibler discrepancy with T. In this paper, we explore the impact of statistical errors in estimating the AIC during model comparison. Using a parametric bootstrap technique, we study the distribution of AIC differences between a set of candidate models due to different realizations of noise in the data and show that the shape and spread of this distribution can be quite varied. We also study the rate of success of the AIC procedure for different values of a threshold parameter popularly used in the literature. For plausible choices of true dark energy models, our studies suggest that investigating such distributions of AIC differences in addition to the threshold is useful in correctly interpreting comparisons of dark energy models using the AIC technique., Comment: Figures and further discussions of the results were added, and the version matches the version published in MNRAS

Published
2011
Full Text
View/download PDF

10. Parameters and pitfalls in dark energy models with time varying equation of state

Author

Biswas, Rahul and Wandelt, Benjamin D.

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

Are geometrical summaries of the CMB and LSS sufficient for estimating cosmological parameters? And how does our choice of a dark energy model impact the current constraints on standard cosmological parameters? We address these questions in the context of the widely used CPL parametrization of a time varying equation of state w in a cosmology allowing spatial curvature. We study examples of different behavior allowed in a CPL parametrization in a phase diagram, and relate these to effects on the observables. We examine parameter constraints in such a cosmology by combining WMAP5, SDSS, SNe, HST data sets by comparing the power spectra. We carefully quantify the differences of these constraints to those obtained by using geometrical summaries for the same data sets. We find that (a) using summary parameters instead of the full data sets give parameter constraints that are similar, but with discernible differences, (b) due to degeneracies, the constraints on the standard parameters broaden significantly for the same data sets. In particular, we find that in the context of CPL dark energy, (i) a Harrison-Zeldovich spectrum cannot be ruled out at $2\sigma$ levels with our current data sets. and (ii) the SNe IA, HST, and WMAP 5 data are not sufficient to constrain spatial curvature; we additionally require the SDSS DR4 data to achieve this., Comment: 20 pages, 11 figures, Submitted to Astrophysical Journal

Published
2009

11. Probing the Fundamental Nature of Dark Matter with the Large Synoptic Survey Telescope

Author

Drlica-Wagner, Alex, Mao, Yao-Yuan, Adhikari, Susmita, Armstrong, Robert, Banerjee, Arka, Banik, Nilanjan, Bechtol, Keith, Bird, Simeon, Boddy, Kimberly K., Bonaca, Ana, Bovy, Jo, Buckley, Matthew R., Bulbul, Esra, Chang, Chihway, Chapline, George, Cohen-Tanugi, Johann, Cuoco, Alessandro, Cyr-Racine, Francis-Yan, Dawson, William A., Rivero, Ana Díaz, Dvorkin, Cora, Erkal, Denis, Fassnacht, Christopher D., García-Bellido, Juan, Giannotti, Maurizio, Gluscevic, Vera, Golovich, Nathan, Hendel, David, Hezaveh, Yashar D., Horiuchi, Shunsaku, James Jee, M., Kaplinghat, Manoj, Keeton, Charles R., Koposov, Sergey E., Lam, Casey Y., Li, Ting S., Lu, Jessica R., Mandelbaum, Rachel, Mcdermott, Samuel D., Mcnanna, Mitch, Medford, Michael, Meyer, Manuel, Marc, Moniez, Murgia, Simona, Nadler, Ethan O., Necib, Lina, Nuss, Eric, Pace, Andrew B., Peter, Annika H. G., Polin, Daniel A., Prescod-Weinstein, Chanda, Read, Justin I., Rosenfeld, Rogerio, Shipp, Nora, Simon, Joshua D., Slatyer, Tracy R., Straniero, Oscar, Strigari, Louis E., Tollerud, Erik, Anthony Tyson, J., Wang, Mei-Yu, Wechsler, Risa H., Wittman, David, Yu, Hai-Bo, Zaharijas, Gabrijela, Ali-Haimoud, Yacine, Annis, James, Birrer, Simon, Biswas, Rahul, Blazek, Jonathan, Brooks, Alyson M., Buckley-Geer, Elizabeth, Caputo, Regina, Charles, Eric, Digel, Seth, Dodelson, Scott, Flaugher, Brenna, Frieman, Joshua, Gawiser, Eric, Hearin, Andrew P., Hložek, Renee, Jain, Bhuvnesh, Jeltema, Tesla E., Koushiappas, Savvas M., Lisanti, Mariangela, Loverde, Marilena, Siddharth Mishra-Sharma, Newman, Jeffrey A., Nord, Brian, Nourbakhsh, Erfan, Ritz, Steven, Robertson, Brant E., Sánchez-Conde, Miguel A., Slosar, Anže, Tait, Tim M. P., Verma, Aprajita, Vilalta, Ricardo, Walter, Christopher W., Yanny, Brian, and Zentner, Andrew R.

Subjects
astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), hep-ex, astro-ph.GA, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, hep-ph, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Experiment, High Energy Physics - Phenomenology, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Astrophysical and cosmological observations currently provide the only robust, empirical measurements of dark matter. Future observations with Large Synoptic Survey Telescope (LSST) will provide necessary guidance for the experimental dark matter program. This white paper represents a community effort to summarize the science case for studying the fundamental physics of dark matter with LSST. We discuss how LSST will inform our understanding of the fundamental properties of dark matter, such as particle mass, self-interaction strength, non-gravitational couplings to the Standard Model, and compact object abundances. Additionally, we discuss the ways that LSST will complement other experiments to strengthen our understanding of the fundamental characteristics of dark matter. More information on the LSST dark matter effort can be found at https://lsstdarkmatter.github.io/ ., Comment: 96 pages, 22 figures, 1 table

12. Science-Driven Optimization of the LSST Observing Strategy

Author

Lsst, Science Collaboration, Marshall, Phil, Anguita, Timo, Bianco, Federica B., Bellm, Eric C., Brandt, Niel, Clarkson, Will, Connolly, Andy, Gawiser, Eric, Ivezic, Zeljko, Jones, Lynne, Lochner, Michelle, Lund, Michael B., Mahabal, Ashish, Nidever, David, Olsen, Knut, Ridgway, Stephen, Rhodes, Jason, Shemmer, Ohad, Trilling, David, Vivas, Kathy, Walkowicz, Lucianne, Willman, Beth, Yoachim, Peter, Anderson, Scott, Antilogus, Pierre, Angus, Ruth, Arcavi, Iair, Awan, Humna, Biswas, Rahul, Bell, Keaton J., Bennett, David, Britt, Chris, Buzasi, Derek, Casetti-Dinescu, Dana I., Chomiuk, Laura, Claver, Chuck, Cook, Kem, Davenport, James, Debattista, Victor, Digel, Seth, Doctor, Zoheyr, Firth, R. E., Foley, Ryan, Fong, Wen-Fai, Lluís Galbany, Giampapa, Mark, Gizis, John E., Graham, Melissa L., Grillmair, Carl, Gris, Phillipe, Haiman, Zoltan, Hartigan, Patrick, Hawley, Suzanne, Hlozek, Renee, Jha, Saurabh W., Johns-Krull, C., Kanbur, Shashi, Kalogera, Vassiliki, Kashyap, Vinay, Kasliwal, Vishal, Kessler, Richard, Kim, Alex, Kurczynski, Peter, Lahav, Ofer, Liu, Michael C., Malz, Alex, Margutti, Raffaella, Matheson, Tom, Mcewen, Jason D., Mcgehee, Peregrine, Meibom, Soren, Meyers, Josh, Monet, Dave, Neilsen, Eric, Newman, Jeffrey, O Dowd, Matt, Peiris, Hiranya V., Penny, Matthew T., Peters, Christina, Poleski, Radoslaw, Ponder, Kara, Richards, Gordon, Rho, Jeonghee, Rubin, David, Schmidt, Samuel, Schuhmann, Robert L., Shporer, Avi, Slater, Colin, Smith, Nathan, Soares-Santos, Marcelles, Stassun, Keivan, Strader, Jay, Strauss, Michael, Street, Rachel, Stubbs, Christopher, Sullivan, Mark, Szkody, Paula, Trimble, Virginia, Tyson, Tony, Val-Borro, Miguel, Valenti, Stefano, Wagoner, Robert, Wood-Vasey, W. Michael, Zauderer, Bevin Ashley, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), LSST, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), 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), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Large Synoptic Survey Telescope is designed to provide an unprecedented optical imaging dataset that will support investigations of our Solar System, Galaxy and Universe, across half the sky and over ten years of repeated observation. However, exactly how the LSST observations will be taken (the observing strategy or "cadence") is not yet finalized. In this dynamically-evolving community white paper, we explore how the detailed performance of the anticipated science investigations is expected to depend on small changes to the LSST observing strategy. Using realistic simulations of the LSST schedule and observation properties, we design and compute diagnostic metrics and Figures of Merit that provide quantitative evaluations of different observing strategies, analyzing their impact on a wide range of proposed science projects. This is work in progress: we are using this white paper to communicate to each other the relative merits of the observing strategy choices that could be made, in an effort to maximize the scientific value of the survey. The investigation of some science cases leads to suggestions for new strategies that could be simulated and potentially adopted. Notably, we find motivation for exploring departures from a spatially uniform annual tiling of the sky: focusing instead on different parts of the survey area in different years in a "rolling cadence" is likely to have significant benefits for a number of time domain and moving object astronomy projects. The communal assembly of a suite of quantified and homogeneously coded metrics is the vital first step towards an automated, systematic, science-based assessment of any given cadence simulation, that will enable the scheduling of the LSST to be as well-informed as possible., 312 pages, 90 figures. Browse the current version at https://github.com/LSSTScienceCollaborations/ObservingStrategy, new contributions welcome!

13. LSST Science Book, Version 2.0

Author

Lsst, Science Collaboration, Abell, Paul A., Allison, Julius, Anderson, Scott F., Andrew, John R., Angel, J. Roger P., Armus, Lee, Arnett, David, Asztalos, S. J., Axelrod, Tim S., Bailey, Stephen, Ballantyne, D. R., Bankert, Justin R., Barkhouse, Wayne A., Barr, Jeffrey D., Barrientos, L. Felipe, Barth, Aaron J., Bartlett, James G., Becker, Andrew C., Becla, Jacek, Beers, Timothy C., Bernstein, Joseph P., Biswas, Rahul, Blanton, Michael R., Bloom, Joshua S., Bochanski, John J., Boeshaar, Pat, Borne, Kirk D., Bradac, Marusa, Brandt, W. N., Bridge, Carrie R., Brown, Michael E., Brunner, Robert J., Bullock, James S., Burgasser, Adam J., Burge, James H., Burke, David L., Cargile, Phillip A., Chandrasekharan, Srinivasan, Chartas, George, Chesley, Steven R., Chu, You-Hua, Cinabro, David, Claire, Mark W., Claver, Charles F., Clowe, Douglas, Connolly, A. J., Cook, Kem H., Cooke, Jeff, Cooray, Asantha, Covey, Kevin R., Culliton, Christopher S., Jong, Roelof, Vries, Willem H., Debattista, Victor P., Delgado, Francisco, Antonio, Ian P., Dhital, Saurav, Di Stefano, Rosanne, Dickinson, Mark, Dilday, Benjamin, Djorgovski, S. G., Dobler, Gregory, Donalek, Ciro, Dubois-Felsmann, Gregory, Durech, Josef, Eliasdottir, Ardis, Eracleous, Michael, Eyer, Laurent, Falco, Emilio E., Fan, Xiaohui, Fassnacht, Christopher D., Ferguson, Harry C., Fernandez, Yanga R., Fields, Brian D., Finkbeiner, Douglas, Figueroa, Eduardo E., Fox, Derek B., Francke, Harold, Frank, James S., Frieman, Josh, Fromenteau, Sebastien, Furqan, Muhammad, Galaz, Gaspar, Gal-Yam, A., Garnavich, Peter, Gawiser, Eric, Geary, John, Gee, Perry, Gibson, Robert R., Gilmore, Kirk, Grace, Emily A., Green, Richard F., Gressler, William J., Grillmair, Carl J., Habib, Salman, Haggerty, J. S., Hamuy, Mario, Harris, Alan W., Hawley, Suzanne L., Heavens, Alan F., Hebb, Leslie, Henry, Todd J., Hileman, Edward, Hilton, Eric J., Hoadley, Keri, Holberg, J. B., Holman, Matt J., Howell, Steve B., Infante, Leopoldo, Ivezic, Zeljko, Jacoby, Suzanne H., Jain, Bhuvnesh, R, Jedicke, Jee, M. James, Garrett Jernigan, J., Jha, Saurabh W., Johnston, Kathryn V., Jones, R. Lynne, Juric, Mario, Kaasalainen, Mikko, Styliani, Kafka, Kahn, Steven M., Kaib, Nathan A., Kalirai, Jason, Kantor, Jeff, Kasliwal, Mansi M., Keeton, Charles R., Kessler, Richard, Knezevic, Zoran, Kowalski, Adam, Krabbendam, Victor L., Krughoff, K. Simon, Kulkarni, Shrinivas, Kuhlman, Stephen, Lacy, Mark, Lepine, Sebastien, Liang, Ming, Lien, Amy, Lira, Paulina, Long, Knox S., Lorenz, Suzanne, Lotz, Jennifer M., Lupton, R. H., Lutz, Julie, Macri, Lucas M., Mahabal, Ashish A., Mandelbaum, Rachel, Marshall, Phil, May, Morgan, Mcgehee, Peregrine M., Meadows, Brian T., Meert, Alan, Milani, Andrea, Miller, Christopher J., Miller, Michelle, Mills, David, Minniti, Dante, Monet, David, Mukadam, Anjum S., Nakar, Ehud, Neill, Douglas R., Newman, Jeffrey A., Nikolaev, Sergei, Nordby, Martin, O Connor, Paul, Oguri, Masamune, Oliver, John, Olivier, Scot S., Olsen, Julia K., Olsen, Knut, Olszewski, Edward W., Oluseyi, Hakeem, Padilla, Nelson D., Parker, Alex, Pepper, Joshua, Peterson, John R., Petry, Catherine, Pinto, Philip A., Pizagno, James L., Popescu, Bogdan, Prsa, Andrej, Radcka, Veljko, Raddick, M. Jordan, Rasmussen, Andrew, Rau, Arne, Rho, Jeonghee, Rhoads, James E., Richards, Gordon T., Ridgway, Stephen T., Robertson, Brant E., Roskar, Rok, Saha, Abhijit, Sarajedini, Ata, Scannapieco, Evan, Schalk, Terry, Schindler, Rafe, Schmidt, Samuel, Schmidt, Sarah, Schneider, Donald P., Schumacher, German, Scranton, Ryan, Sebag, Jacques, Seppala, Lynn G., Ohad Shemmer, Simon, Joshua D., Sivertz, M., Smith, Howard A., Allyn Smith, J., Smith, Nathan, Spitz, Anna H., Stanford, Adam, Stassun, Keivan G., Strader, Jay, Strauss, Michael A., Stubbs, Christopher W., Sweeney, Donald W., Szalay, Alex, Szkody, Paula, Takada, Masahiro, Thorman, Paul, Trilling, David E., Trimble, Virginia, Tyson, Anthony, Berg, Richard, Vanden Berk, Daniel, Vanderplas, Jake, Verde, Licia, Vrsnak, Bojan, Walkowicz, Lucianne M., Wandelt, Benjamin D., Wang, Sheng, Wang, Yun, Warner, Michael, Wechsler, Risa H., West, Andrew A., Wiecha, Oliver, Williams, Benjamin F., Willman, Beth, Wittman, David, Wolff, Sidney C., Wood-Vasey, W. Michael, Wozniak, Przemek, Young, Patrick, Zentner, Andrew, Zhan, Hu, 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)-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), LSST, Bartlett, James, 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), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Active galactic nucleus, 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], media_common.quotation_subject, Milky Way, FOS: Physical sciences, Large Synoptic Survey Telescope, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Weak gravitational lensing, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Astrophysics - Solar and Stellar Astrophysics, Sky, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics of Galaxies (astro-ph.GA), Dark energy, Instrumentation and Methods for Astrophysics, Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

A survey that can cover the sky in optical bands over wide fields to faint magnitudes with a fast cadence will enable many of the exciting science opportunities of the next decade. The Large Synoptic Survey Telescope (LSST) will have an effective aperture of 6.7 meters and an imaging camera with field of view of 9.6 deg^2, and will be devoted to a ten-year imaging survey over 20,000 deg^2 south of +15 deg. Each pointing will be imaged 2000 times with fifteen second exposures in six broad bands from 0.35 to 1.1 microns, to a total point-source depth of r~27.5. The LSST Science Book describes the basic parameters of the LSST hardware, software, and observing plans. The book discusses educational and outreach opportunities, then goes on to describe a broad range of science that LSST will revolutionize: mapping the inner and outer Solar System, stellar populations in the Milky Way and nearby galaxies, the structure of the Milky Way disk and halo and other objects in the Local Volume, transient and variable objects both at low and high redshift, and the properties of normal and active galaxies at low and high redshift. It then turns to far-field cosmological topics, exploring properties of supernovae to z~1, strong and weak lensing, the large-scale distribution of galaxies and baryon oscillations, and how these different probes may be combined to constrain cosmological models and the physics of dark energy., 596 pages. Also available at full resolution at http://www.lsst.org/lsst/scibook

Catalog

Books, media, physical & digital resources
See catalog results