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178 results on '"Buckley-Geer, Elizabeth"'

1. TDCOSMO. XVI. Measurement of the Hubble Constant from the Lensed Quasar WGD$\,$2038$-$4008

Author: Wong, Kenneth C., Dux, Frédéric, Shajib, Anowar J., Suyu, Sherry H., Millon, Martin, Mozumdar, Pritom, Wells, Patrick R., Agnello, Adriano, Birrer, Simon, Buckley-Geer, Elizabeth J., Courbin, Frédéric, Fassnacht, Christopher D., Frieman, Joshua, Galan, Aymeric, Lin, Huan, Marshall, Philip J., Poh, Jason, Schuldt, Stefan, Sluse, Dominique, and Treu, Tommaso
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Time-delay cosmography is a powerful technique to constrain cosmological parameters, particularly the Hubble constant ($H_{0}$). The TDCOSMO collaboration is performing an ongoing analysis of lensed quasars to constrain cosmology using this method. In this work, we obtain constraints from the lensed quasar WGD 2038-4008 using new time-delay measurements and previous mass models by TDCOSMO. This is the first TDCOSMO lens to incorporate multiple lens modeling codes and the full time-delay covariance matrix into the cosmological inference. The models are fixed before the time delay is measured, and the analysis is performed blinded with respect to the cosmological parameters to prevent unconscious experimenter bias. We obtain $D_{\Delta t} = 1.68^{+0.40}_{-0.38}$ Gpc using two families of mass models, a power-law describing the total mass distribution, and a composite model of baryons and dark matter, although the composite model is disfavored due to kinematics constraints. In a flat $\Lambda$CDM cosmology, we constrain the Hubble constant to be $H_{0} = 65^{+23}_{-14}\, \rm km\ s^{-1}\,Mpc^{-1}$. The dominant source of uncertainty comes from the time delays, due to the low variability of the quasar. Future long-term monitoring, especially in the era of the Vera C. Rubin Observatory's Legacy Survey of Space and Time, could catch stronger quasar variability and further reduce the uncertainties. This system will be incorporated into an upcoming hierarchical analysis of the entire TDCOSMO sample, and improved time delays and spatially-resolved stellar kinematics could strengthen the constraints from this system in the future., Comment: 8 pages, 5 figures, 3 tables; accepted for publication in Astronomy & Astrophysics
Published: 2024
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2. Project Dinos I: A joint lensing-dynamics constraint on the deviation from the power law in the mass profile of massive ellipticals

Author: Tan, Chin Yi, Shajib, Anowar J., Birrer, Simon, Sonnenfeld, Alessandro, Treu, Tommaso, Wells, Patrick, Williams, Devon, Buckley-Geer, Elizabeth J., Drlica-Wagner, Alex, and Frieman, Joshua
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The mass distribution in massive elliptical galaxies encodes their evolutionary history, thus providing an avenue to constrain the baryonic astrophysics in their evolution. The power-law assumption for the radial mass profile in ellipticals has been sufficient to describe several observables to the noise level, including strong lensing and stellar dynamics. In this paper, we quantitatively constrained any deviation, or the lack thereof, from the power-law mass profile in massive ellipticals through joint lensing-dynamics analysis of a large statistical sample with 77 galaxy-galaxy lens systems. We performed an improved and uniform lens modelling of these systems from archival Hubble Space Telescope imaging using the automated lens modelling pipeline dolphin. We combined the lens model posteriors with the stellar dynamics to constrain the deviation from the power law after accounting for the line-of-sight lensing effects, a first for analyses on galaxy-galaxy lenses. We find that the Sloan Lens ACS Survey (SLACS) lens galaxies with a mean redshift of 0.2 are consistent with the power-law profile within 1.1$\sigma$ (2.8$\sigma$) and the Strong Lensing Legacy Survey (SL2S) lens galaxies with a mean redshift of 0.6 are consistent within 0.8$\sigma$ (2.1$\sigma$), for a spatially constant (Osipkov-Merritt) stellar anisotropy profile. We adopted the spatially constant anisotropy profile as our baseline choice based on previous dynamical observables of local ellipticals. However, spatially resolved stellar kinematics of lens galaxies are necessary to differentiate between the two anisotropy models. Future studies will use our lens models to constrain the mass distribution individually in the dark matter and baryonic components., Comment: 31 pages, 20 figures, 9 tables. This version: accepted to MNRAS
Published: 2023
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3. The impact of human expert visual inspection on the discovery of strong gravitational lenses

Author: Rojas, Karina, Collett, Thomas E., Ballard, Daniel, Magee, Mark R., Birrer, Simon, Buckley-Geer., Elizabeth, Chan, James H. H., Clément, Benjamin, Diego, José M., Gentile, Fabrizio, González, Jimena, Joseph, Rémy, Mastache, Jorge, Schuldt, Stefan, Tortora, Crescenzo, Verdugo, Tomás, Verma, Aprajita, Daylan, Tansu, Millon, Martin, Jackson, Neal, Dye, Simon, Melo, Alejandra, Mahler, Guillaume, Ogando, Ricardo L. C., Courbin, Frédéric, Fritz, Alexander, Herle, Aniruddh, Barroso, Javier A. Acevedo, Cañameras, Raoul, Cornen, Claude, Dhanasingham, Birendra, Glazebrook, Karl, Martinez, Michael N., Ryczanowski, Dan, Savary, Elodie, Góis-Silva, Filipe, Ureña-López, L. Arturo, Wiesner, Matthew P., Wilde, Joshua, Calçada, Gabriel Valim, Cabanac, Rémi, Pan, Yue, Sierra, Isaac, Despali, Giulia, Cavalcante-Gomes, Micaele V., Macmillan, Christine, Maresca, Jacob, Grudskaia, Aleksandra, O'Donnell, Jackson H., Paic, Eric, Niemiec, Anna, de la Bella, Lucia F., Bromley, Jane, Williams, Devon M., More, Anupreeta, and Levine, Benjamin C.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate the ability of human 'expert' classifiers to identify strong gravitational lens candidates in Dark Energy Survey like imaging. We recruited a total of 55 people that completed more than 25$\%$ of the project. During the classification task, we present to the participants 1489 images. The sample contains a variety of data including lens simulations, real lenses, non-lens examples, and unlabeled data. We find that experts are extremely good at finding bright, well-resolved Einstein rings, whilst arcs with $g$-band signal-to-noise less than $\sim$25 or Einstein radii less than $\sim$1.2 times the seeing are rarely recovered. Very few non-lenses are scored highly. There is substantial variation in the performance of individual classifiers, but they do not appear to depend on the classifier's experience, confidence or academic position. These variations can be mitigated with a team of 6 or more independent classifiers. Our results give confidence that humans are a reliable pruning step for lens candidates, providing pure and quantifiably complete samples for follow-up studies., Comment: 16 pages, 20 Figures
Published: 2023
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4. The MegaMapper: A Stage-5 Spectroscopic Instrument Concept for the Study of Inflation and Dark Energy

Author: Schlegel, David J., Kollmeier, Juna A., Aldering, Greg, Bailey, Stephen, Baltay, Charles, Bebek, Christopher, BenZvi, Segev, Besuner, Robert, Blanc, Guillermo, Bolton, Adam S., Bonaca, Ana, Bouri, Mohamed, Brooks, David, Buckley-Geer, Elizabeth, Cai, Zheng, Crane, Jeffrey, Demina, Regina, DeRose, Joseph, Dey, Arjun, Doel, Peter, Fan, Xiaohui, Ferraro, Simone, Finkbeiner, Douglas, Font-Ribera, Andreu, Gontcho, Satya Gontcho A, Green, Daniel, Gutierrez, Gaston, Guy, Julien, Heetderks, Henry, Huterer, Dragan, Infante, Leopoldo, Jelinsky, Patrick, Karagiannis, Dionysios, Kent, Stephen M., Kim, Alex G., Kneib, Jean-Paul, Kremin, Anthony, Kronig, Luzius, Konidaris, Nick, Lahav, Ofer, Lampton, Michael L., Landriau, Martin, Lang, Dustin, Leauthaud, Alexie, Levi, Michael E., Liguori, Michele, Linder, Eric V., Magneville, Christophe, Martini, Paul, Mateo, Mario, McDonald, Patrick, Miller, Christopher J., Moustakas, John, Myers, Adam D., Mulchaey, John, Newman, Jeffrey A., Nugent, Peter E., Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Piro, Antonella Palmese Anthony L., Poppett, Claire, Prochaska, Jason X., Pullen, Anthony R., Rabinowitz, David, Raichoor, Anand, Ramirez, Solange, Rix, Hans-Walter, Ross, Ashley J., Samushia, Lado, Schaan, Emmanuel, Schubnell, Michael, Seljak, Uros, Seo, Hee-Jong, Shectman, Stephen A., Schlafly, Edward F., Silber, Joseph, Simon, Joshua D., Slepian, Zachary, Slosar, Anže, Soares-Santos, Marcelle, Tarlé, Greg, Thompson, Ian, Valluri, Monica, Wechsler, Risa H., White, Martin, Wilson, Michael J., Yèche, Christophe, Zaritsky, Dennis, and Zhou, Rongpu
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment
Abstract: In this white paper, we present the MegaMapper concept. The MegaMapper is a proposed ground-based experiment to measure Inflation parameters and Dark Energy from galaxy redshifts at $2
Published: 2022

5. A Spectroscopic Road Map for Cosmic Frontier: DESI, DESI-II, Stage-5

Author: Schlegel, David J., Ferraro, Simone, Aldering, Greg, Baltay, Charles, BenZvi, Segev, Besuner, Robert, Blanc, Guillermo A., Bolton, Adam S., Bonaca, Ana, Brooks, David, Buckley-Geer, Elizabeth, Cai, Zheng, DeRose, Joseph, Dey, Arjun, Doel, Peter, Drlica-Wagner, Alex, Fan, Xiaohui, Gutierrez, Gaston, Green, Daniel, Guy, Julien, Huterer, Dragan, Infante, Leopoldo, Jelinsky, Patrick, Karagiannis, Dionysios, Kent, Stephen M., Kim, Alex G., Kneib, Jean-Paul, Kollmeier, Juna A., Kremin, Anthony, Lahav, Ofer, Landriau, Martin, Lang, Dustin, Leauthaud, Alexie, Levi, Michael E., Linder, Eric V., Magneville, Christophe, Martini, Paul, McDonald, Patrick, Miller, Christopher J., Myers, Adam D., Newman, Jeffrey A., Nugent, Peter E., Palanque-Delabrouille, Nathalie, Padmanabhan, Nikhil, Palmese, Antonella, Poppett, Claire, Prochaska, Jason X., Raichoor, Anand, Ramirez, Solange, Sailer, Noah, Schaan, Emmanuel, Schubnell, Michael, Seljak, Uros, Seo, Hee-Jong, Silber, Joseph, Simon, Joshua D., Slepian, Zachary, Soares-Santos, Marcelle, Tarle, Greg, Valluri, Monica, Weaverdyck, Noah J., Wechsler, Risa H., White, Martin, Yeche, Christophe, and Zhou, Rongpu
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Experiment
Abstract: In this white paper, we present an experimental road map for spectroscopic experiments beyond DESI. DESI will be a transformative cosmological survey in the 2020s, mapping 40 million galaxies and quasars and capturing a significant fraction of the available linear modes up to z=1.2. DESI-II will pilot observations of galaxies both at much higher densities and extending to higher redshifts. A Stage-5 experiment would build out those high-density and high-redshift observations, mapping hundreds of millions of stars and galaxies in three dimensions, to address the problems of inflation, dark energy, light relativistic species, and dark matter. These spectroscopic data will also complement the next generation of weak lensing, line intensity mapping and CMB experiments and allow them to reach their full potential., Comment: Contribution to Snowmass 2021
Published: 2022

6. The Robotic Multi-Object Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)

Author: Silber, Joseph Harry, Fagrelius, Parker, Fanning, Kevin, Schubnell, Michael, Aguilar, Jessica Nicole, Ahlen, Steven, Ameel, Jon, Ballester, Otger, Baltay, Charles, Bebek, Chris, Beard, Dominic Benton, Besuner, Robert, Cardiel-Sas, Laia, Casas, Ricard, Castander, Francisco Javier, Claybaugh, Todd, Dobson, Carl, Duan, Yutong, Dunlop, Patrick, Edelstein, Jerry, Emmet, William T., Elliott, Ann, Evatt, Matthew, Gershkovich, Irena, Guy, Julien, Harris, Stu, Heetderks, Henry, Heetderks, Ian, Honscheid, Klaus, Illa, Jose Maria, Jelinsky, Patrick, Jelinsky, Sharon R., Jimenez, Jorge, Karcher, Armin, Kent, Stephen, Kirkby, David, Kneib, Jean-Paul, Lambert, Andrew, Lampton, Mike, Leitner, Daniela, Levi, Michael, McCauley, Jeremy, Meisner, Aaron, Miller, Timothy N., Miquel, Ramon, Mundet, Juliá, Poppett, Claire, Rabinowitz, David, Reil, Kevin, Roman, David, Schlegel, David, Serrano, Santiago, Van Shourt, William, Sprayberry, David, Tarlé, Gregory, Tie, Suk Sien, Weaverdyck, Curtis, Zhang, Kai, Azzaro, Marco, Bailey, Stephen, Becerril, Santiago, Blackwell, Tami, Bouri, Mohamed, Brooks, David, Buckley-Geer, Elizabeth, Castro, Jose Peñate, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Doel, Peter, Eisenstein, Daniel J., Fahim, Nasib, Garcia-Bellido, Juan, Gaztañaga, Enrique, Gontcho, Satya Gontcho A, Gutierrez, Gaston, Hörler, Philipp, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Kronig, Luzius, Landriau, Martin, Guillou, Laurent Le, Martini, Paul, Moustakas, John, Palanque-Delabrouille, Nathalie, Peng, Xiyan, Percival, Will, Prada, Francisco, Prieto, Carlos Allende, de Rivera, Guillermo Gonzalez, Sanchez, Eusebio, Sanchez, Justo, Sharples, Ray, Soares-Santos, Marcelle, Schlafly, Edward, Weaver, Benjamin Alan, Zhou, Zhimin, Zhu, Yaling, and Zou, Hu
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A system of 5,020 robotic fiber positioners was installed in 2019 on the Mayall Telescope, at Kitt Peak National Observatory. The robots automatically re-target their optical fibers every 10 - 20 minutes, each to a precision of several microns, with a reconfiguration time less than 2 minutes. Over the next five years, they will enable the newly-constructed Dark Energy Spectroscopic Instrument (DESI) to measure the spectra of 35 million galaxies and quasars. DESI will produce the largest 3D map of the universe to date and measure the expansion history of the cosmos. In addition to the 5,020 robotic positioners and optical fibers, DESI's Focal Plane System includes 6 guide cameras, 4 wavefront cameras, 123 fiducial point sources, and a metrology camera mounted at the primary mirror. The system also includes associated structural, thermal, and electrical systems. In all, it contains over 675,000 individual parts. We discuss the design, construction, quality control, and integration of all these components. We include a summary of the key requirements, the review and acceptance process, on-sky validations of requirements, and lessons learned for future multi-object, fiber-fed spectrographs., Comment: 51 pages, 41 figures
Published: 2022
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7. Cosmology Intertwined: A Review of the Particle Physics, Astrophysics, and Cosmology Associated with the Cosmological Tensions and Anomalies

Author: Abdalla, Elcio, Abellán, Guillermo Franco, Aboubrahim, Amin, Agnello, Adriano, Akarsu, Ozgur, Akrami, Yashar, Alestas, George, Aloni, Daniel, Amendola, Luca, Anchordoqui, Luis A., Anderson, Richard I., Arendse, Nikki, Asgari, Marika, Ballardini, Mario, Barger, Vernon, Basilakos, Spyros, Batista, Ronaldo C., Battistelli, Elia S., Battye, Richard, Benetti, Micol, Benisty, David, Berlin, Asher, de Bernardis, Paolo, Berti, Emanuele, Bidenko, Bohdan, Birrer, Simon, Blakeslee, John P., Boddy, Kimberly K., Bom, Clecio R., Bonilla, Alexander, Borghi, Nicola, Bouchet, François R., Braglia, Matteo, Buchert, Thomas, Buckley-Geer, Elizabeth, Calabrese, Erminia, Caldwell, Robert R., Camarena, David, Capozziello, Salvatore, Casertano, Stefano, Chen, Angela, Chen, Geoff C. F., Chen, Hsin-Yu, Chluba, Jens, Chudaykin, Anton, Cicoli, Michele, Copi, Craig J., Courbin, Fred, Cyr-Racine, Francis-Yan, Czerny, Bozena, Dainotti, Maria, D'Amico, Guido, Davis, Anne-Christine, Pérez, Javier de Cruz, de Haro, Jaume, Delabrouille, Jacques, Denton, Peter B., Dhawan, Suhail, Dienes, Keith R., Di Valentino, Eleonora, Du, Pu, Eckert, Dominique, Escamilla-Rivera, Celia, Ferté, Agnès, Finelli, Fabio, Fosalba, Pablo, Freedman, Wendy L., Frusciante, Noemi, Gaztañaga, Enrique, Giarè, William, Giusarma, Elena, Gómez-Valent, Adrià, Handley, Will, Harrison, Ian, Hart, Luke, Hazra, Dhiraj Kumar, Heavens, Alan, Heinesen, Asta, Hildebrandt, Hendrik, Hill, J. Colin, Hogg, Natalie B., Holz, Daniel E., Hooper, Deanna C., Hosseininejad, Nikoo, Huterer, Dragan, Ishak, Mustapha, Ivanov, Mikhail M., Jaffe, Andrew H., Jang, In Sung, Jedamzik, Karsten, Jimenez, Raul, Joseph, Melissa, Joudaki, Shahab, Kamionkowski, Mark, Karwal, Tanvi, Kazantzidis, Lavrentios, Keeley, Ryan E., Klasen, Michael, Komatsu, Eiichiro, Koopmans, Léon V. E., Kumar, Suresh, Lamagna, Luca, Lazkoz, Ruth, Lee, Chung-Chi, Lesgourgues, Julien, Said, Jackson Levi, Lewis, Tiffany R., L'Huillier, Benjamin, Lucca, Matteo, Maartens, Roy, Macri, Lucas M., Marfatia, Danny, Marra, Valerio, Martins, Carlos J. A. P., Masi, Silvia, Matarrese, Sabino, Mazumdar, Arindam, Melchiorri, Alessandro, Mena, Olga, Mersini-Houghton, Laura, Mertens, James, Milakovic, Dinko, Minami, Yuto, Miranda, Vivian, Moreno-Pulido, Cristian, Moresco, Michele, Mota, David F., Mottola, Emil, Mozzon, Simone, Muir, Jessica, Mukherjee, Ankan, Mukherjee, Suvodip, Naselsky, Pavel, Nath, Pran, Nesseris, Savvas, Niedermann, Florian, Notari, Alessio, Nunes, Rafael C., Colgáin, Eoin Ó, Owens, Kayla A., Ozulker, Emre, Pace, Francesco, Paliathanasis, Andronikos, Palmese, Antonella, Pan, Supriya, Paoletti, Daniela, Bergliaffa, Santiago E. Perez, Perivolaropoulos, Leadros, Pesce, Dominic W., Pettorino, Valeria, Philcox, Oliver H. E., Pogosian, Levon, Poulin, Vivian, Poulot, Gaspard, Raveri, Marco, Reid, Mark J., Renzi, Fabrizio, Riess, Adam G., Sabla, Vivian I., Salucci, Paolo, Salzano, Vincenzo, Saridakis, Emmanuel N., Sathyaprakash, Bangalore S., Schmaltz, Martin, Schöneberg, Nils, Scolnic, Dan, Sen, Anjan A., Sehgal, Neelima, Shafieloo, Arman, Sheikh-Jabbari, M. M., Silk, Joseph, Silvestri, Alessandra, Skara, Foteini, Sloth, Martin S., Soares-Santos, Marcelle, Peracaula, Joan Solà, Songsheng, Yu-Yang, Soriano, Jorge F., Staicova, Denitsa, Starkman, Glenn D., Szapudi, István, Teixeira, Elsa M., Thomas, Brooks, Treu, Tommaso, Trott, Emery, van de Bruck, Carsten, Vazquez, J. Alberto, Verde, Licia, Visinelli, Luca, Wang, Deng, Wang, Jian-Min, Wang, Shao-Jiang, Watkins, Richard, Watson, Scott, Webb, John K., Weiner, Neal, Weltman, Amanda, Witte, Samuel J., Wojtak, Radosław, Yadav, Anil Kumar, Yang, Weiqiang, Zhao, Gong-Bo, and Zumalacárregui, Miguel
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology
Abstract: In this paper we will list a few important goals that need to be addressed in the next decade, also taking into account the current discordances between the different cosmological probes, such as the disagreement in the value of the Hubble constant $H_0$, the $\sigma_8$--$S_8$ tension, and other less statistically significant anomalies. While these discordances can still be in part the result of systematic errors, their persistence after several years of accurate analysis strongly hints at cracks in the standard cosmological scenario and the necessity for new physics or generalisations beyond the standard model. In this paper, we focus on the $5.0\,\sigma$ tension between the {\it Planck} CMB estimate of the Hubble constant $H_0$ and the SH0ES collaboration measurements. After showing the $H_0$ evaluations made from different teams using different methods and geometric calibrations, we list a few interesting new physics models that could alleviate this tension and discuss how the next decade's experiments will be crucial. Moreover, we focus on the tension of the {\it Planck} CMB data with weak lensing measurements and redshift surveys, about the value of the matter energy density $\Omega_m$, and the amplitude or rate of the growth of structure ($\sigma_8,f\sigma_8$). We list a few interesting models proposed for alleviating this tension, and we discuss the importance of trying to fit a full array of data with a single model and not just one parameter at a time. Additionally, we present a wide range of other less discussed anomalies at a statistical significance level lower than the $H_0$--$S_8$ tensions which may also constitute hints towards new physics, and we discuss possible generic theoretical approaches that can collectively explain the non-standard nature of these signals.[Abridged], Comment: Contribution to Snowmass 2021. 224 pages, 27 figures. Accepted for publication in JHEAp
Published: 2022
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8. LensingETC: a tool to optimize multi-filter imaging campaigns of galaxy-scale strong lensing systems

Author: Shajib, Anowar J., Glazebrook, Karl, Barone, Tania, Lewis, Geraint F., Jones, Tucker, Tran, Kim-Vy H., Buckley-Geer, Elizabeth, Collett, Thomas E., Frieman, Joshua, and Jacobs, Colin
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Imaging data is the principal observable required to use galaxy-scale strong lensing in a multitude of applications in extragalactic astrophysics and cosmology. In this paper, we develop Lensing Exposure Time Calculator (LensingETC) to optimize the efficiency of telescope time usage when planning multi-filter imaging campaigns for galaxy-scale strong lenses. This tool simulates realistic data tailored to specified instrument characteristics and then automatically models them to assess the power of the data in constraining lens model parameters. We demonstrate a use case of this tool by optimizing a two-filter observing strategy (in IR and UVIS) within the limited exposure time per system allowed by a Hubble Space Telescope (HST) Snapshot program. We find that higher resolution is more advantageous to gain constraining power on the lensing observables, when there is a trade-off between signal-to-noise ratio and resolution; e.g., between the UVIS and IR filters of the HST. We also find that, whereas a point spread function (PSF) with sub-Nyquist sampling allows the sample mean for a model parameter to be robustly recovered for both galaxy-galaxy and point-source lensing systems, a sub-Nyquist sampled PSF introduces a larger scatter than a Nyquist sampled one in the deviation from the ground truth for point-source lens systems., Comment: 10 pages, 7 figures, 3 tables
Published: 2022

9. Discovery of a Candidate Binary Supermassive Black Hole in a Periodic Quasar from Circumbinary Accretion Variability

Author: Liao, Wei-Ting, Chen, Yu-Ching, Liu, Xin, Holgado, A. Miguel, Guo, Hengxiao, Gruendl, Robert, Morganson, Eric, Shen, Yue, Davis, Tamara, Kessler, Richard, Martini, Paul, McMahon, Richard G., Allam, Sahar, Annis, James, Avila, Santiago, Banerji, Manda, Bechtol, Keith, Bertin, Emmanuel, Brooks, David, Buckley-Geer, Elizabeth, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Cunha, Carlos, D'Andrea, Chris, da Costa, Luiz, Davis, Christopher, De Vicente, Juan, Desai, Shantanu, Diehl, H. Thomas, Doel, Peter, Eifler, Tim, Evrard, August, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Glazebrook, Karl, Gruen, Daniel, Gschwend, Julia, Gutierrez, Gaston, Hartley, Will, Hollowood, Devon L., Honscheid, Klaus, Hoyle, Ben, James, David, Krause, Elisabeth, Kuehn, Kyler, Lima, Marcos, Maia, Marcio, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Malagón, Andrés Plazas, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Smith, Mathew, Smith, R. Chris, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly, Tarle, Gregory, Vikram, Vinu, Walker, Alistair, and Collaboration, the DES
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Binary supermassive black holes (BSBHs) are expected to be a generic byproduct from hierarchical galaxy formation. The final coalescence of BSBHs is thought to be the loudest gravitational wave (GW) siren, yet no confirmed BSBH is known in the GW-dominated regime. While periodic quasars have been proposed as BSBH candidates, the physical origin of the periodicity has been largely uncertain. Here we report discovery of a periodicity (P=1607$\pm$7 days) at 99.95% significance (with a global p-value of ~$10^{-3}$ accounting for the look elsewhere effect) in the optical light curves of a redshift 1.53 quasar, SDSS J025214.67-002813.7. Combining archival Sloan Digital Sky Survey data with new, sensitive imaging from the Dark Energy Survey, the total ~20-yr time baseline spans ~4.6 cycles of the observed 4.4-yr (restframe 1.7-yr) periodicity. The light curves are best fit by a bursty model predicted by hydrodynamic simulations of circumbinary accretion disks. The periodicity is likely caused by accretion rate modulation by a milli-parsec BSBH emitting GWs, dynamically coupled to the circumbinary accretion disk. A bursty hydrodynamic variability model is statistically preferred over a smooth, sinusoidal model expected from relativistic Doppler boost, a kinematic effect proposed for PG1302-102. Furthermore, the frequency dependence of the variability amplitudes disfavors Doppler boost, lending independent support to the circumbinary accretion variability hypothesis. Given our detection rate of one BSBH candidate from circumbinary accretion variability out of 625 quasars, it suggests that future large, sensitive synoptic surveys such as the Vera C. Rubin Observatory Legacy Survey of Space and Time may be able to detect hundreds to thousands of candidate BSBHs from circumbinary accretion with direct implications for Laser Interferometer Space Antenna., Comment: Accepted to MNRAS, 17 pages, 9 figures
Published: 2020
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10. Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances and Weak Lensing

Author: DES Collaboration, Abbott, Tim, Aguena, Michel, Alarcon, Alex, Allam, Sahar, Allen, Steve, Annis, James, Avila, Santiago, Bacon, David, Bermeo, Alberto, Bernstein, Gary, Bertin, Emmanuel, Bhargava, Sunayana, Bocquet, Sebastian, Brooks, David, Brout, Dillon, Buckley-Geer, Elizabeth, Burke, David, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Cawthon, Ross, Chang, Chihway, Chen, Xinyi, Choi, Ami, Costanzi, Matteo, Crocce, Martin, da Costa, Luiz, Davis, Tamara, De Vicente, Juan, DeRose, Joseph, Desai, Shantanu, Diehl, H. Thomas, Dietrich, Jörg, Dodelson, Scott, Doel, Peter, Drlica-Wagner, Alex, Eckert, Kathleen, Eifler, Tim, Elvin-Poole, Jack, Estrada, Juan, Everett, Spencer, Evrard, August, Farahi, Arya, Ferrero, Ismael, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gatti, Marco, Gaztanaga, Enrique, Gerdes, David, Giannantonio, Tommaso, Giles, Paul, Grandis, Sebastian, Gruen, Daniel, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hartley, Will, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klaus, Hoyle, Ben, Huterer, Dragan, James, David, Jarvis, Mike, Jeltema, Tesla, Johnson, Margaret, Kent, Stephen, Krause, Elisabeth, Kron, Richard, Kuehn, Kyler, Kuropatkin, Nikolay, Lahav, Ofer, Li, Ting, Lidman, Christopher, Lima, Marcos, Lin, Huan, MacCrann, Niall, Maia, Marcio, Mantz, Adam, Marshall, Jennifer, Martini, Paul, Mayers, Julian, Melchior, Peter, Mena, Juan, Menanteau, Felipe, Miquel, Ramon, Mohr, Joe, Nichol, Robert, Nord, Brian, Ogando, Ricardo, Palmese, Antonella, Paz-Chinchon, Francisco, Malagón, Andrés Plazas, Prat, Judit, Rau, Markus Michael, Romer, Kathy, Roodman, Aaron, Rooney, Philip, Rozo, Eduardo, Rykoff, Eli, Sako, Masao, Samuroff, Simon, Sanchez, Carles, Saro, Alexandro, Scarpine, Vic, Schubnell, Michael, Scolnic, Daniel, Serrano, Santiago, Sevilla, Ignacio, Sheldon, Erin, Smith, J. Allyn, Suchyta, Eric, Swanson, Molly, Tarle, Gregory, Thomas, Daniel, To, Chun-Hao, Troxel, Michael A., Tucker, Douglas, Varga, Tamas Norbert, von der Linden, Anja, Walker, Alistair, Wechsler, Risa, Weller, Jochen, Wilkinson, Reese, Wu, Hao-Yi, Yanny, Brian, Zhang, Zhuowen, and Zuntz, Joe
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a joint analysis of the counts and weak lensing signal of redMaPPer clusters selected from the Dark Energy Survey (DES) Year 1 dataset. Our analysis uses the same shear and source photometric redshifts estimates as were used in the DES combined probes analysis. Our analysis results in surprisingly low values for $S_8 =\sigma_8(\Omega_{\rm m}/0.3)^{0.5}= 0.65\pm 0.04$, driven by a low matter density parameter, $\Omega_{\rm m}=0.179^{+0.031}_{-0.038}$, with $\sigma_8-\Omega_{\rm m}$ posteriors in $2.4\sigma$ tension with the DES Y1 3x2pt results, and in $5.6\sigma$ with the Planck CMB analysis. These results include the impact of post-unblinding changes to the analysis, which did not improve the level of consistency with other data sets compared to the results obtained at the unblinding. The fact that multiple cosmological probes (supernovae, baryon acoustic oscillations, cosmic shear, galaxy clustering and CMB anisotropies), and other galaxy cluster analyses all favor significantly higher matter densities suggests the presence of systematic errors in the data or an incomplete modeling of the relevant physics. Cross checks with X-ray and microwave data, as well as independent constraints on the observable--mass relation from SZ selected clusters, suggest that the discrepancy resides in our modeling of the weak lensing signal rather than the cluster abundance. Repeating our analysis using a higher richness threshold ($\lambda \ge 30$) significantly reduces the tension with other probes, and points to one or more richness-dependent effects not captured by our model., Comment: 35 pages, 20 figures, submitted to Physical Review D
Published: 2020
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11. Astro2020 APC White Paper: The MegaMapper: a z > 2 spectroscopic instrument for the study of Inflation and Dark Energy

Author: Schlegel, David J., Kollmeier, Juna A., Aldering, Greg, Bailey, Stephen, Baltay, Charles, Bebek, Christopher, BenZvi, Segev, Besuner, Robert, Blanc, Guillermo, Bolton, Adam S., Bouri, Mohamed, Brooks, David, Buckley-Geer, Elizabeth, Cai, Zheng, Crane, Jeffrey, Dey, Arjun, Doel, Peter, Fan, Xiaohui, Ferraro, Simone, Font-Ribera, Andreu, Gutierrez, Gaston, Guy, Julien, Heetderks, Henry, Huterer, Dragan, Infante, Leopoldo, Jelinsky, Patrick, Johns, Matthew, Karagiannis, Dionysios, Kent, Stephen M., Kim, Alex G., Kneib, Jean-Paul, Kronig, Luzius, Konidaris, Nick, Lahav, Ofer, Lampton, Michael L., Lang, Dustin, Leauthaud, Alexie, Liguori, Michele, Linder, Eric V., Magneville, Christophe, Martini, Paul, Mateo, Mario, McDonald, Patrick, Miller, Christopher J., Moustakas, John, Myers, Adam D., Mulchaey, John, Newman, Jeffrey A., Nugent, Peter E., Palanque-Delabrouille, Nathalie, Padmanabhan, Nikhil, Piro, Anthony L., Poppett, Claire, Prochaska, Jason X., Pullen, Anthony R., Rabinowitz, David, Ramirez, Solange, Rix, Hans-Walter, Ross, Ashley J., Samushia, Lado, Schaan, Emmanuel, Schubnell, Michael, Seljak, Uros, Seo, Hee-Jong, Shectman, Stephen A., Silber, Joseph, Simon, Joshua D., Slepian, Zachary, Soares-Santos, Marcelle, Tarle, Greg, Thompson, Ian, Valluri, Monica, Wechsler, Risa H., White, Martin, Wilson, Michael J., Yeche, Christophe, and Zaritsky, Dennis
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment
Abstract: MegaMapper is a proposed ground-based experiment to measure Inflation parameters and Dark Energy from galaxy redshifts at 2
Published: 2019

12. Spectral Variability of a Sample of Extreme Variability Quasars and Implications for the MgII Broad-line Region

Author: Yang, Qian, Shen, Yue, Chen, Yu-Ching, Liu, Xin, Annis, James, Avila, Santiago, Bertin, Emmanuel, Brooks, David, Buckley-Geer, Elizabeth, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, da Costa, Luiz, Desai, Shantanu, Diehl, H. Thomas, Doel, Peter, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David, Gruen, Daniel, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hollowood, Devon L., Honscheid, Klaus, Hoyle, Ben, James, David, Krause, Elisabeth, Kuehn, Kyler, Lidman, Christopher, Lima, Marcos, Maia, Marcio, Marshall, Jennifer, Martini, Paul, Menanteau, Felipe, Miquel, Ramon, Malagon, Andres Plazas, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Schubnell, Michael, Serrano, Santiago, Sevilla, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly, Tarle, Gregory, Vikram, Vinu, and Walker, Alistair
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present new Gemini/GMOS optical spectroscopy of 16 extreme variability quasars (EVQs) that dimmed by more than 1.5 mag in the $g$ band between the Sloan Digital Sky Survey (SDSS) and the Dark Energy Survey (DES) epochs (separated by a few years in the quasar rest frame). The quasar sample covers a redshift range of $0.5 < z < 2.1$. Nearly half of these EVQs brightened significantly (by more than 0.5 mag in the $g$ band) in a few years after reaching their previous faintest state, and some EVQs showed rapid (non-blazar) variations of greater than 1-2 mag on timescales of only months. Leveraging on the large dynamic range in continuum variability between the earlier SDSS and the new GMOS spectra, we explore the associated variations in the broad Mg II,$\lambda2798$ line, whose variability properties have not been well studied before. The broad Mg II flux varies in the same direction as the continuum flux, albeit with a smaller amplitude, which indicates at least some portion of Mg II is reverberating to continuum changes. However, the width (FWHM) of Mg II does not vary accordingly as continuum changes for most objects in the sample, in contrast to the case of the broad Balmer lines. Using the width of broad Mg II to estimate the black hole mass therefore introduces a luminosity-dependent bias., Comment: Submitted to MNRAS
Published: 2019
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13. Inflation and Dark Energy from spectroscopy at $z > 2$

Author: Ferraro, Simone, Wilson, Michael J., Abidi, Muntazir, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Baccigalupi, Carlo, Bandura, Kevin, Battaglia, Nicholas, Bavdhankar, Chetan, Bernal, José Luis, Beutler, Florian, Biagetti, Matteo, Blanc, Guillermo A., Blazek, Jonathan, Bolton, Adam S., Borrill, Julian, Frye, Brenda, Buckley-Geer, Elizabeth, Bull, Philip, Burgess, Cliff, Byrnes, Christian T., Cai, Zheng, Castander, Francisco J, Castorina, Emanuele, Chang, Tzu-Ching, Chaves-Montero, Jonás, Chen, Shi-Fan, Chen, Xingang, Balland, Christophe, Yèche, Christophe, Cohn, J. D., Coulton, William, Courtois, Helene, Croft, Rupert A. C., Cyr-Racine, Francis-Yan, D'Amico, Guido, Dawson, Kyle, Delabrouille, Jacques, Dey, Arjun, Doré, Olivier, Douglass, Kelly A., Yutong, Duan, Dvorkin, Cora, Eggemeier, Alexander, Eisenstein, Daniel, Fan, Xiaohui, Ferreira, Pedro G., Font-Ribera, Andreu, Foreman, Simon, García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A, Green, Daniel, Guy, Julien, Hahn, ChangHoon, Hanany, Shaul, Handley, Will, Hathi, Nimish, Hawken, Adam J., Hernández-Aguayo, César, Hložek, Renée, Huterer, Dragan, Ishak, Mustapha, Kamionkowski, Marc, Karagiannis, Dionysios, Keeley, Ryan E., Kehoe, Robert, Khatri, Rishi, Kim, Alex, Kneib, Jean-Paul, Kollmeier, Juna A., Kovetz, Ely D., Krause, Elisabeth, Krolewski, Alex, L'Huillier, Benjamin, Landriau, Martin, Levi, Michael, Liguori, Michele, Linder, Eric, Lukić, Zarija, de la Macorra, Axel, Plazas, Andrés A., Marshall, Jennifer L., Martini, Paul, Masui, Kiyoshi, McDonald, Patrick, Meerburg, P. Daniel, Meyers, Joel, Mirbabayi, Mehrdad, Moustakas, John, Myers, Adam D., Palanque-Delabrouille, Nathalie, Newburgh, Laura, Newman, Jeffrey A., Niz, Gustavo, Padmanabhan, Hamsa, Palunas, Povilas, Percival, Will J., Piacentini, Francesco, Pieri, Matthew M., Piro, Anthony L., Prakash, Abhishek, Rhodes, Jason, Ross, Ashley J., Rossi, Graziano, Rudie, Gwen C., Samushia, Lado, Sasaki, Misao, Schaan, Emmanuel, Schlegel, David J., Schmittfull, Marcel, Schubnell, Michael, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Simon, Joshua D., Simon, Sara, Slepian, Zachary, Slosar, Anže, Sridhar, Srivatsan, Stebbins, Albert, Escoffier, Stephanie, Switzer, Eric R., Tarlé, Gregory, Trodden, Mark, Uhlemann, Cora, Urenña-López, L. Arturo, Di Valentino, Eleonora, Vargas-Magaña, M., Wang, Yi, Watson, Scott, White, Martin, Xu, Weishuang, Yu, Byeonghee, Zhao, Gong-Bo, Zheng, Yi, and Zhu, Hong-Ming
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: The expansion of the Universe is understood to have accelerated during two epochs: in its very first moments during a period of Inflation and much more recently, at $z < 1$, when Dark Energy is hypothesized to drive cosmic acceleration. The undiscovered mechanisms behind these two epochs represent some of the most important open problems in fundamental physics. The large cosmological volume at $2 < z < 5$, together with the ability to efficiently target high-$z$ galaxies with known techniques, enables large gains in the study of Inflation and Dark Energy. A future spectroscopic survey can test the Gaussianity of the initial conditions up to a factor of ~50 better than our current bounds, crossing the crucial theoretical threshold of $\sigma(f_{NL}^{\rm local})$ of order unity that separates single field and multi-field models. Simultaneously, it can measure the fraction of Dark Energy at the percent level up to $z = 5$, thus serving as an unprecedented test of the standard model and opening up a tremendous discovery space., Comment: Science white paper submitted to the Astro2020 Decadal Survey
Published: 2019

14. Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics

Author: Green, Daniel, Amin, Mustafa A., Meyers, Joel, Wallisch, Benjamin, Abazajian, Kevork N., Abidi, Muntazir, Adshead, Peter, Ahmed, Zeeshan, Ansarinejad, Behzad, Armstrong, Robert, Baccigalupi, Carlo, Bandura, Kevin, Barron, Darcy, Battaglia, Nicholas, Baumann, Daniel, Bechtol, Keith, Bennett, Charles, Benson, Bradford, Beutler, Florian, Bischoff, Colin, Bleem, Lindsey, Bond, J. Richard, Borrill, Julian, Buckley-Geer, Elizabeth, Burgess, Cliff, Carlstrom, John E., Castorina, Emanuele, Challinor, Anthony, Chen, Xingang, Cooray, Asantha, Coulton, William, Craig, Nathaniel, Crawford, Thomas, Cyr-Racine, Francis-Yan, D'Amico, Guido, Demarteau, Marcel, Doré, Olivier, Yutong, Duan, Dunkley, Joanna, Dvorkin, Cora, Ellison, John, van Engelen, Alexander, Escoffier, Stephanie, Essinger-Hileman, Tom, Fabbian, Giulio, Filippini, Jeffrey, Flauger, Raphael, Foreman, Simon, Fuller, George, Garcia, Marcos A. G., García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A, Górski, Krzysztof M., Grin, Daniel, Grohs, Evan, Gudmundsson, Jon E., Hanany, Shaul, Handley, Will, Hill, J. Colin, Hirata, Christopher M., Hložek, Renée, Holder, Gilbert, Horiuchi, Shunsaku, Huterer, Dragan, Kadota, Kenji, Kamionkowski, Marc, Keeley, Ryan E., Khatri, Rishi, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., L'Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Lin, Tongyan, Loverde, Marilena, Madhavacheril, Mathew, Masui, Kiyoshi, McMahon, Jeff, McQuinn, Matthew, Meerburg, P. Daniel, Mirbabayi, Mehrdad, Motloch, Pavel, Mukherjee, Suvodip, Munõz, Julian B., Nagy, Johanna, Newburgh, Laura, Niemack, Michael D., Nomerotski, Andrei, Page, Lyman, Piacentni, Francesco, Pierpaoli, Elena, Pogosian, Levon, Pryke, Clement, Puglisi, Giuseppe, Stompor, Radek, Raveri, Marco, Reichardt, Christian L., Rose, Benjamin, Rossi, Graziano, Ruhl, John, Schaan, Emmanuel, Schubnell, Michael, Schutz, Katelin, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Sherwin, Blake D., Simon, Sara, Slosar, Anže, Staggs, Suzanne, Stebbins, Albert, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tristram, Matthieu, Trodden, Mark, Tsai, Yu-Dai, Umiltà, Caterina, Di Valentino, Eleonora, Vargas-Magaña, M., Vieregg, Abigail, Watson, Scott, Weiler, Thomas, Whitehorn, Nathan, Wu, W. L. K., Xu, Weishuang, Xu, Zhilei, Yasini, Siavash, Zaldarriaga, Matias, Zhao, Gong-Bo, Zhu, Ningfeng, and Zuntz, Joe
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology
Abstract: The hot dense environment of the early universe is known to have produced large numbers of baryons, photons, and neutrinos. These extreme conditions may have also produced other long-lived species, including new light particles (such as axions or sterile neutrinos) or gravitational waves. The gravitational effects of any such light relics can be observed through their unique imprint in the cosmic microwave background (CMB), the large-scale structure, and the primordial light element abundances, and are important in determining the initial conditions of the universe. We argue that future cosmological observations, in particular improved maps of the CMB on small angular scales, can be orders of magnitude more sensitive for probing the thermal history of the early universe than current experiments. These observations offer a unique and broad discovery space for new physics in the dark sector and beyond, even when its effects would not be visible in terrestrial experiments or in astrophysical environments. A detection of an excess light relic abundance would be a clear indication of new physics and would provide the first direct information about the universe between the times of reheating and neutrino decoupling one second later., Comment: 5 pages + references; 1 figure; science white paper submitted to the Astro2020 decadal survey
Published: 2019

15. 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 A. C., Cuoco, Alessandro, Cyr-Racine, Francis-Yan, D'Amico, Guido, Davis, Tamara M, Dawson, William A., de la Macorra, Axel, Di Valentino, Eleonora, 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, Giannotti, Maurizio, Gill, Mandeep S. S., 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 H. G., 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 M. P., Tollerud, Erik, Troxel, M. A., 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., and Zuntz, Joe
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
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., Comment: 11 pages, 2 figures, Science Whitepaper for Astro 2020, more information at https://lsstdarkmatter.github.io
Published: 2019

16. 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, Jee, M. James, 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, Tyson, J. Anthony, Wang, Mei-Yu, Wechsler, Risa H., Wittman, David, Yu, Hai-Bo, Zaharijas, Gabrijela, Ali-Haïmoud, 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, Mishra-Sharma, Siddharth, 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: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, High Energy Physics - Phenomenology
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
Published: 2019

17. The Buzzard Flock: Dark Energy Survey Synthetic Sky Catalogs

Author: DeRose, Joseph, Wechsler, Risa H., Becker, Matthew R., Busha, Michael T., Rykoff, Eli S., MacCrann, Niall, Erickson, Brandon, Evrard, August E., Kravtsov, Andrey, Gruen, Daniel, Allam, Sahar, Avila, Santiago, Bridle, Sarah, Brooks, David, Buckley-Geer, Elizabeth, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco J., Cawthon, Ross, Crocce, Martin, da Costa, Luiz N., Davis, Christopher, De Vicente, Juan, Dietrich, Jörg P., Doel, Peter, Drlica-Wagner, Alex, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gutierrez, Gaston, Hartley, Will G., Hollowood, Devon L., Hoyle, Ben, James, David J., Krause, Elisabeth, Kuehn, Kyler, Kuropatkin, Nikolay, Lima, Marcos, Maia, Marcio A. G., Menanteau, Felipe, Miller, Christopher J., Miquel, Ramon, Ogando, Ricardo L. C., Malagón, Andrés Plazas, Romer, A. Kathy, Sanchez, Eusebio, Schindler, Rafe, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, and Vikram, Vinu
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a suite of 18 synthetic sky catalogs designed to support science analysis of galaxies in the Dark Energy Survey Year 1 (DES Y1) data. For each catalog, we use a computationally efficient empirical approach, ADDGALS, to embed galaxies within light-cone outputs of three dark matter simulations that resolve halos with masses above ~5x10^12 h^-1 m_sun at z <= 0.32 and 10^13 h^-1 m_sun at z~2. The embedding method is tuned to match the observed evolution of galaxy counts at different luminosities as well as the spatial clustering of the galaxy population. Galaxies are lensed by matter along the line of sight --- including magnification, shear, and multiple images --- using CALCLENS, an algorithm that calculates shear with 0.42 arcmin resolution at galaxy positions in the full catalog. The catalogs presented here, each with the same LCDM cosmology (denoted Buzzard), contain on average 820 million galaxies over an area of 1120 square degrees with positions, magnitudes, shapes, photometric errors, and photometric redshift estimates. We show that the weak-lensing shear catalog, redMaGiC galaxy catalogs and redMaPPer cluster catalogs provide plausible realizations of the same catalogs in the DES Y1 data by comparing their magnitude, color and redshift distributions, angular clustering, and mass-observable relations, making them useful for testing analyses that use these samples. We make public the galaxy samples appropriate for the DES Y1 data, as well as the data vectors used for cosmology analyses on these simulations., Comment: 33 pages, 13 figures, catalogs will be made public upon publication; interested users may contact us beforehand
Published: 2019

18. Astrometry and Occultation predictions to Trans-Neptunian and Centaur Objects observed within the Dark Energy Survey

Author: Banda-Huarca, Martin, Camargo, Julio, Desmars, Josselin, Ogando, Ricardo, Vieira-Martins, Roberto, Assafin, Marcelo, da Costa, Luiz, Bernstein, Gary, Kind, Matias Carrasco, Wagner, Alex Drlica, Gomes, Rodney, Gysi, Matheus, Ribas, Felipe Braga, Maia, Marcio, Gerdes, David, Hamilton, Stephanie, Wester, William, Abbot, Tim, Abdalla, Filipe, Allam, Sahar, Avila, Santiago, Bertin, Emmanuel, Brooks, David, Buckley-Geer, Elizabeth, Burke, David, Rossell, Aurelio Carnero, Carretero, Jorge, Cunha, Carlos, Davis, Christopher, de Vicente, Juan, Diehl, Thomas, Doel, Peter, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gruen, Daniel, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hartley, Will, Hollowood, Devon, Honscheid, Klaus, James, David, Kuehn, Kyler, Kuropatkin, Nikolay, Menanteau, Felipe, Miller, Christopher, Miquel, Ramon, Plazas, Andres, Romer, Kathy, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Sevilla, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly, and Tarle, Gregory
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Transneptunian objects (TNOs) are a source of invaluable information to access the history and evolution of the outer solar system. However, observing these faint objects is a difficult task. As a consequence, important properties such as size and albedo are known for only a small fraction of them. Now, with the results from deep sky surveys and the Gaia space mission, a new exciting era is within reach as accurate predictions of stellar occultations by numerous distant small solar system bodies become available. From them, diameters with kilometer accuracies can be determined. Albedos, in turn, can be obtained from diameters and absolute magnitudes. We use observations from the Dark Energy Survey (DES) from November 2012 until February 2016, amounting to 4292847 CCD frames. We searched them for all known small solar system bodies and recovered a total of 202 TNOs and Centaurs, 63 of which have been discovered by the DES collaboration until the date of this writing. Their positions were determined using the Gaia Data Release 2 as reference and their orbits were refined. Stellar occultations were then predicted using these refined orbits plus stellar positions from Gaia. These predictions are maintained, and updated, in a dedicated web service. The techniques developed here are also part of an ambitious preparation to use the data from the Large Synoptic Survey Telescope (LSST), that expects to obtain accurate positions and multifilter photometry for tens of thousands of TNOs., Comment: 25 pages, submitted to Astronomical Journal
Published: 2018
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19. The DESI Instrument Control System: Status and Early Testing

Author: Honscheid, Klaus, Elliott, Ann, Buckley-Geer, Elizabeth, Abreshi, Bezhad, Castender, Francisco, daCosta, Luiz, Kent, Stephen, Kirkby, David, Marshall, Robert, Neilsen, Eric, Ogando, Riccardo, Rabinowitz, David, roodman, Aaron, Serrano, Santiago, Brooks, David, Levi, Michael, and Tarle, Greg
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) is a new instrument currently under construction for the Mayall 4-m telescope at Kitt Peak National Observatory. It will consist of a wide-field optical corrector with a 3.2 degree diameter field of view, a focal plane with 5,000 robotically controlled fiber positioners and 10 fiber-fed broad-band spectrographs. The DESI Instrument Control System (ICS) coordinates fiber positioner operations, interfaces to the Mayall telescope control system, monitors operating conditions, reads out the 30 spectrograph CCDs and provides observer support and data quality monitoring. In this article, we summarize the ICS design, review the current status of the project and present results from a multi-stage test plan that was developed to ensure the system is fully operational by the time the instrument arrives at the observatory in 2019., Comment: SPIE Astronomical Telescopes + Instrumentation, Austin, TX (2018)
Published: 2018

20. Astro2020 APC White Paper: The MegaMapper: a z > 2 spectroscopic instrument for the study of Inflation and Dark Energy

Author: Schlegel, David J, Kollmeier, Juna A, Aldering, Greg, Bailey, Stephen, Baltay, Charles, Bebek, Christopher, BenZvi, Segev, Besuner, Robert, Blanc, Guillermo, Bolton, Adam S, Bouri, Mohamed, Brooks, David, Buckley-Geer, Elizabeth, Cai, Zheng, Crane, Jeffrey, Dey, Arjun, Doel, Peter, Fan, Xiaohui, Ferraro, Simone, Font-Ribera, Andreu, Gutierrez, Gaston, Guy, Julien, Heetderks, Henry, Huterer, Dragan, Infante, Leopoldo, Jelinsky, Patrick, Johns, Matthew, Karagiannis, Dionysios, Kent, Stephen M, Kim, Alex G, Kneib, Jean-Paul, Kronig, Luzius, Konidaris, Nick, Lahav, Ofer, Lampton, Michael L, Lang, Dustin, Leauthaud, Alexie, Liguori, Michele, Linder, Eric V, Magneville, Christophe, Martini, Paul, Mateo, Mario, McDonald, Patrick, Miller, Christopher J, Moustakas, John, Myers, Adam D, Mulchaey, John, Newman, Jeffrey A, Nugent, Peter E, Palanque-Delabrouille, Nathalie, Padmanabhan, Nikhil, Piro, Anthony L, Poppett, Claire, Prochaska, Jason X, Pullen, Anthony R, Rabinowitz, David, Ramirez, Solange, Rix, Hans-Walter, Ross, Ashley J, Samushia, Lado, Schaan, Emmanuel, Schubnell, Michael, Seljak, Uros, Seo, Hee-Jong, Shectman, Stephen A, Silber, Joseph, Simon, Joshua D, Slepian, Zachary, Soares-Santos, Marcelle, Tarle, Greg, Thompson, Ian, Valluri, Monica, Wechsler, Risa H, White, Martin, Wilson, Michael J, Yeche, Christophe, and Zaritsky, Dennis
Subjects: astro-ph.IM, hep-ex
Abstract: MegaMapper is a proposed ground-based experiment to measure Inflationparameters and Dark Energy from galaxy redshifts at 2
Published: 2019

21. Overview of the DESI Legacy Imaging Surveys

Author: Dey, Arjun, Schlegel, David J, Lang, Dustin, Blum, Robert, Burleigh, Kaylan, Fan, Xiaohui, Findlay, Joseph R, Finkbeiner, Doug, Herrera, David, Juneau, Stéphanie, Landriau, Martin, Levi, Michael, McGreer, Ian, Meisner, Aaron, Myers, Adam D, Moustakas, John, Nugent, Peter, Patej, Anna, Schlafly, Edward F, Walker, Alistair R, Valdes, Francisco, Weaver, Benjamin A, Yèche, Christophe, Zou, Hu, Zhou, Xu, Abareshi, Behzad, Abbott, TMC, Abolfathi, Bela, Aguilera, C, Alam, Shadab, Allen, Lori, Alvarez, A, Annis, James, Ansarinejad, Behzad, Aubert, Marie, Beechert, Jacqueline, Bell, Eric F, BenZvi, Segev Y, Beutler, Florian, Bielby, Richard M, Bolton, Adam S, Briceño, César, Buckley-Geer, Elizabeth J, Butler, Karen, Calamida, Annalisa, Carlberg, Raymond G, Carter, Paul, Casas, Ricard, Castander, Francisco J, Choi, Yumi, Comparat, Johan, Cukanovaite, Elena, Delubac, Timothée, DeVries, Kaitlin, Dey, Sharmila, Dhungana, Govinda, Dickinson, Mark, Ding, Zhejie, Donaldson, John B, Duan, Yutong, Duckworth, Christopher J, Eftekharzadeh, Sarah, Eisenstein, Daniel J, Etourneau, Thomas, Fagrelius, Parker A, Farihi, Jay, Fitzpatrick, Mike, Font-Ribera, Andreu, Fulmer, Leah, Gänsicke, Boris T, Gaztanaga, Enrique, George, Koshy, Gerdes, David W, Gontcho, Satya Gontcho A, Gorgoni, Claudio, Green, Gregory, Guy, Julien, Harmer, Diane, Hernandez, M, Honscheid, Klaus, Huang, Lijuan, James, David J, Jannuzi, Buell T, Jiang, Linhua, Joyce, Richard, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Jean-Paul, Kneib, Kueter-Young, Andrea, Lan, Ting-Wen, Lauer, Tod R, Le Guillou, Laurent, Le Van Suu, Auguste, Lee, Jae Hyeon, Lesser, Michael, Levasseur, Laurence Perreault, Li, Ting S, Mann, Justin L, and Marshall, Robert
Subjects: Space Sciences, Physical Sciences, catalogs, surveys, astro-ph.IM, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics
Abstract: The DESI Legacy Imaging Surveys (http://legacysurvey.org/) are a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image ≈14,000 deg2 of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerro Tololo Inter-American Observatory. The combined survey footprint is split into two contiguous areas by the Galactic plane. The optical imaging is conducted using a unique strategy of dynamically adjusting the exposure times and pointing selection during observing that results in a survey of nearly uniform depth. In addition to calibrated images, the project is delivering a catalog, constructed by using a probabilistic inference-based approach to estimate source shapes and brightnesses. The catalog includes photometry from the grz optical bands and from four mid-infrared bands (at 3.4, 4.6, 12, and 22 μm) observed by the Wide-field Infrared Survey Explorer satellite during its full operational lifetime. The project plans two public data releases each year. All the software used to generate the catalogs is also released with the data. This paper provides an overview of the Legacy Surveys project.
Published: 2019

22. ProtoDESI: First On-Sky Technology Demonstration for the Dark Energy Spectroscopic Instrument

Author: Fagrelius, Parker, Abareshi, Behzad, Allen, Lori, Ballester, Otger, Baltay, Charles, Besuner, Robert, Buckley-Geer, Elizabeth, Butler, Karen, Cardiel, Laia, Dey, Arjun, Elliott, Ann, Emmet, William, Gershkovich, Irena, Honscheid, Klaus, Illa, Jose M., Jimenez, Jorge, Levi, Michael, Manser, Christopher, Marshall, Robert, Martini, Paul, Paat, Anthony, Probst, Ronald, Rabinowitz, David, Reil, Kevin, Robertson, Amy, Rockosi, Connie, Schlegel, David, Schubnell, Michael, Serrano, Santiago, Silber, Joseph, Soto, Christian, Sprayberry, David, Summers, David, Tarle, Greg, Weaver, Benjamin A., and Duan, Y. T.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the universe using the baryon acoustic oscillations technique. The spectra of 35 million galaxies and quasars over 14,000 square degrees will be measured during a 5-year survey. A new prime focus corrector for the Mayall telescope at Kitt Peak National Observatory will deliver light to 5,000 individually targeted fiber-fed robotic positioners. The fibers in turn feed ten broadband multi-object spectrographs. We describe the ProtoDESI experiment, that was installed and commissioned on the 4-m Mayall telescope from August 14 to September 30, 2016. ProtoDESI was an on-sky technology demonstration with the goal to reduce technical risks associated with aligning optical fibers with targets using robotic fiber positioners and maintaining the stability required to operate DESI. The ProtoDESI prime focus instrument, consisting of three fiber positioners, illuminated fiducials, and a guide camera, was installed behind the existing Mosaic corrector on the Mayall telescope. A Fiber View Camera was mounted in the Cassegrain cage of the telescope and provided feedback metrology for positioning the fibers. ProtoDESI also provided a platform for early integration of hardware with the DESI Instrument Control System that controls the subsystems, provides communication with the Telescope Control System, and collects instrument telemetry data. Lacking a spectrograph, ProtoDESI monitored the output of the fibers using a Fiber Photometry Camera mounted on the prime focus instrument. ProtoDESI was successful in acquiring targets with the robotically positioned fibers and demonstrated that the DESI guiding requirements can be met., Comment: Accepted version
Published: 2017
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23. DES Science Portal: Creating Science-Ready Catalogs

Author: Neto, Angelo Fausti, da Costa, Luiz, Rosell, Aurelio Carnero, Gschwend, Julia, Ogando, Ricardo, Sobreira, Flavia, Maia, Marcio, Santiago, Basilio, Rosenfeld, Rogerio, Singulani, Cristiano, Nunes, Lucas, Adean, Carlos, Campisano, Riccardo, Brito, Rafael, Soares, Guilherme, Vila-Verde, Glauber C., Abbott, Tim, Abdalla, Filipe, Allam, Sahar, Benoit-Lévy, Aurélien, Brooks, David, Buckley-Geer, Elizabeth, Capozzi, Diego, Kind, Matias Carrasco, Carretero, Jorge, D'Andrea, Chris, Desai, Shantanu, Doel, Peter, Drlica-Wagner, Alex, Evrard, August, Fosalba, Pablo, Garcia-Bellido, Juan, Gerdes, David, Gruendl, Robert, Gutierrez, Gaston, Honscheid, Klaus, James, David, Jeltema, Tesla, Kuehn, Kyler, Kuhlmann, Steve, Kuropatkin, Nikolay, Lahav, Ofer, Lima, Marcos, Marshall, Jennifer, Melchior, Peter, Menanteau, Felipe, Malagón, Andrés Plazas, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Schubnell, Michael, Sevilla, Ignacio, Smith, Mathew, Smith, R. Chris, Suchyta, Eric, Swanson, Molly, Tarle, Gregory, and Walker, Alistair
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present a novel approach for creating science-ready catalogs through a software infrastructure developed for the Dark Energy Survey (DES). We integrate the data products released by the DES Data Management and additional products created by the DES collaboration in an environment known as DES Science Portal. Each step involved in the creation of a science-ready catalog is recorded in a relational database and can be recovered at any time. We describe how the DES Science Portal automates the creation and characterization of lightweight catalogs for DES Year 1 Annual Release, and show its flexibility in creating multiple catalogs with different inputs and configurations. Finally, we discuss the advantages of this infrastructure for large surveys such as DES and the Large Synoptic Survey Telescope. The capability of creating science-ready catalogs efficiently and with full control of the inputs and configurations used is an important asset for supporting science analysis using data from large astronomical surveys., Comment: The second paper of the series about the DES Science Portal, submitted to the Astronomy & Computing journal. It shows the infrastructure to create science-ready catalogs from DES photometric data and ancillary maps. This is the version accepted by the journal
Published: 2017
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24. Extreme variability quasars from the Sloan Digital Sky Survey and the Dark Energy Survey

Author: Rumbaugh, Nick, Shen, Yue, Morganson, Eric, Liu, Xin, Banerji, Manda, McMahon, Richard G., Abdalla, Filipe, Benoit-Levy, Aurelien, Bertin, Emmanuel, Brooks, David, Buckley-Geer, Elizabeth, Capozzi, Diego, Rosell, Aurelio Carnero, Kind, M. Carrasco, Carretero, Jorge, Cunha, Carlos, D'Andrea, Chris, da Costa, Luiz, DePoy, Darren, Desai, Shantanu, Doel, Peter, Frieman, Joshua, Garcia-Bellido, Juan, Gruen, Daniel, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Honscheid, Klaus, James, David, Kuehn, Kyler, Kuhlmann, Steve, Kuropatkin, Nikolay, Lima, Marcos, Maia, Marcio, Marshall, Jennifer, Martini, Paul, Menanteau, Felipe, Malagon, Andres Plazas, Reil, Kevin, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Schubnell, Michael, Sheldon, Erin, Smith, Mathew, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly, Walker, Alistair, and Wester, William
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a systematic search for long-term extreme variability quasars (EVQs) in the overlapping Sloan Digital Sky Survey (SDSS) and 3-Year Dark Energy Survey (DES) imaging, which provide light curves spanning more than 15 years. We identified ~1000 EVQs with a maximum g band magnitude change of more than 1 mag over this period, about 10% of all quasars searched. The EVQs have L_bol~10^45-10^47 erg/s and L/L_Edd~0.01-1. Accounting for selection effects, we estimate an intrinsic EVQ fraction of ~30-50% among all g<~22 quasars over a baseline of ~15 years. These EVQs are good candidates for so-called "changing-look quasars", where a spectral transition between the two types of quasars (broad-line and narrow-line) is observed between the dim and bright states. We performed detailed multi-wavelength, spectral and variability analyses for the EVQs and compared to their parent quasar sample. We found that EVQs are distinct from a control sample of quasars matched in redshift and optical luminosity: (1) their UV broad emission lines have larger equivalent widths; (2) their Eddington ratios are systematically lower; and (3) they are more variable on all timescales. The intrinsic difference in quasar properties for EVQs suggest that internal processes associated with accretion are the main driver for the observed extreme long-term variability. However, despite their different properties, EVQs seem to be in the tail of a continuous distribution of quasar properties, rather than standing out as a distinct population. We speculate that EVQs are normal quasars accreting at relatively low accretion rates, where the accretion flow is more likely to experience instabilities that drive the factor of few changes in flux on multi-year timescales., Comment: submitted to ApJ; comments welcome
Published: 2017
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25. Core or cusps: The central dark matter profile of a redshift one strong lensing cluster with a bright central image

Author: Collett, Thomas E., Buckley-Geer, Elizabeth, Lin, Huan, Bacon, David, Nichol, Robert C., Nord, Brian, Morice-Atkinson, Xan, Amara, Adam, Birrer, Simon, Kuropatkin, Nikolay, More, Anupreeta, Papovich, Casey, Romer, Kathy K., Tessore, Nicolas, Abbott, Tim M. C., Allam, Sahar, Annis, James, Benoit-Lévy, Aurélien, Brooks, David, Burke, David L., Kind, Matias Carrasco, Castander, Francisco Javier J., D'Andrea, Chris B., da Costa, Luiz N., Desai, Shantanu, Diehl, H. Thomas, Doel, Peter, Eifler, Tim F., Flaugher, Brenna, Frieman, Josh, Gerdes, David W., Goldstein, Daniel A., Gruen, Daniel, Gschwend, Julia, Gutierrez, Gaston, James, David J., Kuehn, Kyler, Kuhlmann, Steve, Lahav, Ofer, Li, Ting S., Lima, Marcos, Maia, Marcio A. G., March, Marisa, Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Miquel, Ramon, Plazas, Andrés A., Rykoff, Eli S., Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Schubnell, Michael, Sevilla-Noarbe, Ignacio, Smith, Mathew, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Tucker, Douglas L., and Walker, Alistair R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We report on SPT-CLJ2011-5228, a giant system of arcs created by a cluster at $z=1.06$. The arc system is notable for the presence of a bright central image. The source is a Lyman Break galaxy at $z_s=2.39$ and the mass enclosed within the 14 arc second radius Einstein ring is $10^{14.2}$ solar masses. We perform a full light profile reconstruction of the lensed images to precisely infer the parameters of the mass distribution. The brightness of the central image demands that the central total density profile of the lens be shallow. By fitting the dark matter as a generalized Navarro-Frenk-White profile---with a free parameter for the inner density slope---we find that the break radius is $270^{+48}_{-76}$ kpc, and that the inner density falls with radius to the power $-0.38\pm0.04$ at 68 percent confidence. Such a shallow profile is in strong tension with our understanding of relaxed cold dark matter halos; dark matter only simulations predict the inner density should fall as $r^{-1}$. The tension can be alleviated if this cluster is in fact a merger; a two halo model can also reconstruct the data, with both clumps (density going as $r^{-0.8}$ and $r^{-1.0}$) much more consistent with predictions from dark matter only simulations. At the resolution of our Dark Energy Survey imaging, we are unable to choose between these two models, but we make predictions for forthcoming Hubble Space Telescope imaging that will decisively distinguish between them., Comment: 13 Pages. Accepted for publication in ApJ
Published: 2017
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26. ProtoDESI: First On-Sky Technology Demonstration for the Dark Energy Spectroscopic Instrument

Author: Fagrelius, Parker, Abareshi, Behzad, Allen, Lori, Ballester, Otger, Baltay, Charles, Besuner, Robert, Buckley-Geer, Elizabeth, Butler, Karen, Cardiel, Laia, Dey, Arjun, Duan, Yutong, Elliott, Ann, Emmet, William, Gershkovich, Irena, Honscheid, Klaus, Illa, Jose M, Jimenez, Jorge, Joyce, Richard, Karcher, Armin, Kent, Stephen, Lambert, Andrew, Lampton, Michael, Levi, Michael, Manser, Christopher, Marshall, Robert, Martini, Paul, Paat, Anthony, Probst, Ronald, Rabinowitz, David, Reil, Kevin, Robertson, Amy, Rockosi, Connie, Schlegel, David, Schubnell, Michael, Serrano, Santiago, Silber, Joseph, Soto, Christian, Sprayberry, David, Summers, David, Tarlé, Greg, and Weaver, Benjamin A
Subjects: Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, instrumentation: miscellaneous, methods: observational, telescopes, (cosmology:) dark energy, astro-ph.IM, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the universe using the baryon acoustic oscillations technique. The spectra of 35 million galaxies and quasars over 14,000 square degrees will be measured during a 5-year survey. A new prime focus corrector for the Mayall telescope at Kitt Peak National Observatory will deliver light to 5,000 individually targeted fiber-fed robotic positioners. The fibers in turn feed ten broadband multi-object spectrographs. We describe the ProtoDESI experiment, that was installed and commissioned on the 4-m Mayall telescope from 2016 August 14 to September 30. ProtoDESI was an on-sky technology demonstration with the goal to reduce technical risks associated with aligning optical fibers with targets using robotic fiber positioners and maintaining the stability required to operate DESI. The ProtoDESI prime focus instrument, consisting of three fiber positioners, illuminated fiducials, and a guide camera, was installed behind the existing Mosaic corrector on the Mayall telescope. A fiber view camera was mounted in the Cassegrain cage of the telescope and provided feedback metrology for positioning the fibers. ProtoDESI also provided a platform for early integration of hardware with the DESI Instrument Control System that controls the subsystems, provides communication with the Telescope Control System, and collects instrument telemetry data. Lacking a spectrograph, ProtoDESI monitored the output of the fibers using a fiber photometry camera mounted on the prime focus instrument. ProtoDESI was successful in acquiring targets with the robotically positioned fibers and demonstrated that the DESI guiding requirements can be met.
Published: 2018

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

Author: DESI Collaboration, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E., Prieto, Carlos Allende, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C., Bell, Eric F., Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S., Briceno, Cesar, Brooks, David, Brownstein, Joel R., Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G., Cahn, Robert N., Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G., Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J., Cervantes-Cota, Jorge L., Claybaugh, Todd M., Close, Madeline, Coker, Carl T., Cole, Shaun, Comparat, Johan, Cooper, Andrew P., Cousinou, M. -C., Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P., Davis, Tamara M., Dawson, Kyle S., de la Macorra, Axel, De Vicente, Juan, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T., Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R., Finkbeiner, Douglas P., Fitzpatrick, Michael J., Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E., Fosalba, Pablo, Frenk, Carlos S., Fumagalli, Michele, Gaensicke, Boris T., Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Fusillo, Nicola Pietro Gentile, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-de-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, Guy, Julien, Habib, Salman, Heetderks, Henry, Heetderks, Ian, Heitmann, Katrin, Hellwing, Wojciech A., Herrera, David A., Ho, Shirley, Holland, Stephen, Honscheid, Klaus, Huff, Eric, Hutchinson, Timothy A., Huterer, Dragan, Hwang, Ho Seong, Laguna, Joseph Maria Illa, Ishikawa, Yuzo, Jacobs, Dianna, Jeffrey, Niall, Jelinsky, Patrick, Jennings, Elise, Jiang, Linhua, Jimenez, Jorge, Johnson, Jennifer, Joyce, Richard, Jullo, Eric, Juneau, Stéphanie, Kama, Sami, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kennamer, Noble, Kent, Stephen, Kilbinger, Martin, Kim, Alex G., Kirkby, David, Kisner, Theodore, Kitanidis, Ellie, Kneib, Jean-Paul, Koposov, Sergey, Kovacs, Eve, Koyama, Kazuya, Kremin, Anthony, Kron, Richard, Kronig, Luzius, Kueter-Young, Andrea, Lacey, Cedric G., Lafever, Robin, Lahav, Ofer, Lambert, Andrew, Lampton, Michael, Landriau, Martin, Lang, Dustin, Lauer, Tod R., Goff, Jean-Marc Le, Guillou, Laurent Le, Van Suu, Auguste Le, Lee, Jae Hyeon, Lee, Su-Jeong, Leitner, Daniela, Lesser, Michael, Levi, Michael E., L'Huillier, Benjamin, Li, Baojiu, Liang, Ming, Lin, Huan, Linder, Eric, Loebman, Sarah R., Lukić, Zarija, Ma, Jun, MacCrann, Niall, Magneville, Christophe, Makarem, Laleh, Manera, Marc, Manser, Christopher J., Marshall, Robert, Martini, Paul, Massey, Richard, Matheson, Thomas, McCauley, Jeremy, McDonald, Patrick, McGreer, Ian D., Meisner, Aaron, Metcalfe, Nigel, Miller, Timothy N., Miquel, Ramon, Moustakas, John, Myers, Adam, Naik, Milind, Newman, Jeffrey A., Nichol, Robert C., Nicola, Andrina, da Costa, Luiz Nicolati, Nie, Jundan, Niz, Gustavo, Norberg, Peder, Nord, Brian, Norman, Dara, Nugent, Peter, O'Brien, Thomas, Oh, Minji, Olsen, Knut A. G., Padilla, Cristobal, Padmanabhan, Hamsa, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Palmese, Antonella, Pappalardo, Daniel, Pâris, Isabelle, Park, Changbom, Patej, Anna, Peacock, John A., Peiris, Hiranya V., Peng, Xiyan, Percival, Will J., Perruchot, Sandrine, Pieri, Matthew M., Pogge, Richard, Pollack, Jennifer E., Poppett, Claire, Prada, Francisco, Prakash, Abhishek, Probst, Ronald G., Rabinowitz, David, Raichoor, Anand, Ree, Chang Hee, Refregier, Alexandre, Regal, Xavier, Reid, Beth, Reil, Kevin, Rezaie, Mehdi, Rockosi, Constance M., Roe, Natalie, Ronayette, Samuel, Roodman, Aaron, Ross, Ashley J., Ross, Nicholas P., Rossi, Graziano, Rozo, Eduardo, Ruhlmann-Kleider, Vanina, Rykoff, Eli S., Sabiu, Cristiano, Samushia, Lado, Sanchez, Eusebio, Sanchez, Javier, Schlegel, David J., Schneider, Michael, Schubnell, Michael, Secroun, Aurélia, Seljak, Uros, Seo, Hee-Jong, Serrano, Santiago, Shafieloo, Arman, Shan, Huanyuan, Sharples, Ray, Sholl, Michael J., Shourt, William V., Silber, Joseph H., Silva, David R., Sirk, Martin M., Slosar, Anze, Smith, Alex, Smoot, George F., Som, Debopam, Song, Yong-Seon, Sprayberry, David, Staten, Ryan, Stefanik, Andy, Tarle, Gregory, Tie, Suk Sien, Tinker, Jeremy L., Tojeiro, Rita, Valdes, Francisco, Valenzuela, Octavio, Valluri, Monica, Vargas-Magana, Mariana, Verde, Licia, Walker, Alistair R., Wang, Jiali, Wang, Yuting, Weaver, Benjamin A., Weaverdyck, Curtis, Wechsler, Risa H., Weinberg, David H., White, Martin, Yang, Qian, Yeche, Christophe, Zhang, Tianmeng, Zhao, Gong-Bo, Zheng, Yi, Zhou, Xu, Zhou, Zhimin, Zhu, Yaling, Zou, Hu, and Zu, Ying
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tracers of the underlying dark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the Ly-$\alpha$ forest absorption features in their spectra, which will be used to trace the distribution of neutral hydrogen. When moonlight prevents efficient observations of the faint targets of the baseline survey, DESI will conduct a magnitude-limited Bright Galaxy Survey comprising approximately 10 million galaxies with a median $z\approx 0.2$. In total, more than 30 million galaxy and quasar redshifts will be obtained to measure the BAO feature and determine the matter power spectrum, including redshift space distortions.
Published: 2016

28. The DESI Experiment Part II: Instrument Design

Author: DESI Collaboration, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E., Prieto, Carlos Allende, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C., Bell, Eric F., Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S., Briceno, Cesar, Brooks, David, Brownstein, Joel R., Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G., Cahn, Robert N., Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G., Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J., Cervantes-Cota, Jorge L., Claybaugh, Todd M., Close, Madeline, Coker, Carl T., Cole, Shaun, Comparat, Johan, Cooper, Andrew P., Cousinou, M. -C., Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P., Davis, Tamara M., Dawson, Kyle S., de la Macorra, Axel, De Vicente, Juan, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T., Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R., Finkbeiner, Douglas P., Fitzpatrick, Michael J., Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E., Fosalba, Pablo, Frenk, Carlos S., Fumagalli, Michele, Gaensicke, Boris T., Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Fusillo, Nicola Pietro Gentile, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-de-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, Guy, Julien, Habib, Salman, Heetderks, Henry, Heetderks, Ian, Heitmann, Katrin, Hellwing, Wojciech A., Herrera, David A., Ho, Shirley, Holland, Stephen, Honscheid, Klaus, Huff, Eric, Hutchinson, Timothy A., Huterer, Dragan, Hwang, Ho Seong, Laguna, Joseph Maria Illa, Ishikawa, Yuzo, Jacobs, Dianna, Jeffrey, Niall, Jelinsky, Patrick, Jennings, Elise, Jiang, Linhua, Jimenez, Jorge, Johnson, Jennifer, Joyce, Richard, Jullo, Eric, Juneau, Stéphanie, Kama, Sami, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kennamer, Noble, Kent, Stephen, Kilbinger, Martin, Kim, Alex G., Kirkby, David, Kisner, Theodore, Kitanidis, Ellie, Kneib, Jean-Paul, Koposov, Sergey, Kovacs, Eve, Koyama, Kazuya, Kremin, Anthony, Kron, Richard, Kronig, Luzius, Kueter-Young, Andrea, Lacey, Cedric G., Lafever, Robin, Lahav, Ofer, Lambert, Andrew, Lampton, Michael, Landriau, Martin, Lang, Dustin, Lauer, Tod R., Goff, Jean-Marc Le, Guillou, Laurent Le, Van Suu, Auguste Le, Lee, Jae Hyeon, Lee, Su-Jeong, Leitner, Daniela, Lesser, Michael, Levi, Michael E., L'Huillier, Benjamin, Li, Baojiu, Liang, Ming, Lin, Huan, Linder, Eric, Loebman, Sarah R., Lukić, Zarija, Ma, Jun, MacCrann, Niall, Magneville, Christophe, Makarem, Laleh, Manera, Marc, Manser, Christopher J., Marshall, Robert, Martini, Paul, Massey, Richard, Matheson, Thomas, McCauley, Jeremy, McDonald, Patrick, McGreer, Ian D., Meisner, Aaron, Metcalfe, Nigel, Miller, Timothy N., Miquel, Ramon, Moustakas, John, Myers, Adam, Naik, Milind, Newman, Jeffrey A., Nichol, Robert C., Nicola, Andrina, da Costa, Luiz Nicolati, Nie, Jundan, Niz, Gustavo, Norberg, Peder, Nord, Brian, Norman, Dara, Nugent, Peter, O'Brien, Thomas, Oh, Minji, Olsen, Knut A. G., Padilla, Cristobal, Padmanabhan, Hamsa, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Palmese, Antonella, Pappalardo, Daniel, Pâris, Isabelle, Park, Changbom, Patej, Anna, Peacock, John A., Peiris, Hiranya V., Peng, Xiyan, Percival, Will J., Perruchot, Sandrine, Pieri, Matthew M., Pogge, Richard, Pollack, Jennifer E., Poppett, Claire, Prada, Francisco, Prakash, Abhishek, Probst, Ronald G., Rabinowitz, David, Raichoor, Anand, Ree, Chang Hee, Refregier, Alexandre, Regal, Xavier, Reid, Beth, Reil, Kevin, Rezaie, Mehdi, Rockosi, Constance M., Roe, Natalie, Ronayette, Samuel, Roodman, Aaron, Ross, Ashley J., Ross, Nicholas P., Rossi, Graziano, Rozo, Eduardo, Ruhlmann-Kleider, Vanina, Rykoff, Eli S., Sabiu, Cristiano, Samushia, Lado, Sanchez, Eusebio, Sanchez, Javier, Schlegel, David J., Schneider, Michael, Schubnell, Michael, Secroun, Aurélia, Seljak, Uros, Seo, Hee-Jong, Serrano, Santiago, Shafieloo, Arman, Shan, Huanyuan, Sharples, Ray, Sholl, Michael J., Shourt, William V., Silber, Joseph H., Silva, David R., Sirk, Martin M., Slosar, Anze, Smith, Alex, Smoot, George F., Som, Debopam, Song, Yong-Seon, Sprayberry, David, Staten, Ryan, Stefanik, Andy, Tarle, Gregory, Tie, Suk Sien, Tinker, Jeremy L., Tojeiro, Rita, Valdes, Francisco, Valenzuela, Octavio, Valluri, Monica, Vargas-Magana, Mariana, Verde, Licia, Walker, Alistair R., Wang, Jiali, Wang, Yuting, Weaver, Benjamin A., Weaverdyck, Curtis, Wechsler, Risa H., Weinberg, David H., White, Martin, Yang, Qian, Yeche, Christophe, Zhang, Tianmeng, Zhao, Gong-Bo, Zheng, Yi, Zhou, Xu, Zhou, Zhimin, Zhu, Yaling, Zou, Hu, and Zu, Ying
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DESI (Dark Energy Spectropic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. The DESI instrument is a robotically-actuated, fiber-fed spectrograph capable of taking up to 5,000 simultaneous spectra over a wavelength range from 360 nm to 980 nm. The fibers feed ten three-arm spectrographs with resolution $R= \lambda/\Delta\lambda$ between 2000 and 5500, depending on wavelength. The DESI instrument will be used to conduct a five-year survey designed to cover 14,000 deg$^2$. This powerful instrument will be installed at prime focus on the 4-m Mayall telescope in Kitt Peak, Arizona, along with a new optical corrector, which will provide a three-degree diameter field of view. The DESI collaboration will also deliver a spectroscopic pipeline and data management system to reduce and archive all data for eventual public use.
Published: 2016

29. VDES J2325-5229 a z=2.7 gravitationally lensed quasar discovered using morphology independent supervised machine learning

Author: Ostrovski, Fernanda, McMahon, Richard G., Connolly, Andrew J., Lemon, Cameron A., Auger, Matthew W., Banerji, Manda, Hung, Johnathan M., Koposov, Sergey E., Lidman, Christopher E., Reed, Sophie L., Allam, Sahar, Benoit-Lévy, Aurélien, Bertin, Emmanuel, Brooks, David, Buckley-Geer, Elizabeth, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Cunha, Carlos E., da Costa, Luiz N., Desai, Shantanu, Diehl, H. Thomas, Dietrich, Jörg P., Evrard, August E., Finley, David A., Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Gerdes, David W., Goldstein, Daniel A., Gruen, Daniel, Gruendl, Robert A., Gutierrez, Gaston, Honscheid, Klaus, James, David J., Kuehn, Kyler, Kuropatkin, Nikolay, Lima, Marcos, Lin, Huan, Maia, Marcio A. G., Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Miquel, Ramon, Ogando, Ricardo, Malagón, Andrés Plazas, Reil, Kevin, Romer, Kathy, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Sevilla-Noarbe, Ignacio, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Tarle, Gregory, Thomas, Daniel, Tucker, Douglas L., and Walker, Alistair R.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present the discovery and preliminary characterization of a gravitationally lensed quasar with a source redshift $z_{s}=2.74$ and image separation of $2.9"$ lensed by a foreground $z_{l}=0.40$ elliptical galaxy. Since the images of gravitationally lensed quasars are the superposition of multiple point sources and a foreground lensing galaxy, we have developed a morphology independent multi-wavelength approach to the photometric selection of lensed quasar candidates based on Gaussian Mixture Models (GMM) supervised machine learning. Using this technique and $gi$ multicolour photometric observations from the Dark Energy Survey (DES), near IR $JK$ photometry from the VISTA Hemisphere Survey (VHS) and WISE mid IR photometry, we have identified a candidate system with two catalogue components with $i_{AB}=18.61$ and $i_{AB}=20.44$ comprised of an elliptical galaxy and two blue point sources. Spectroscopic follow-up with NTT and the use of an archival AAT spectrum show that the point sources can be identified as a lensed quasar with an emission line redshift of $z=2.739\pm0.003$ and a foreground early type galaxy with $z=0.400\pm0.002$. We model the system as a single isothermal ellipsoid and find the Einstein radius $\theta_E \sim 1.47"$, enclosed mass $M_{enc} \sim 4 \times 10^{11}$M$_{\odot}$ and a time delay of $\sim$52 days. The relatively wide separation, month scale time delay duration and high redshift make this an ideal system for constraining the expansion rate beyond a redshift of 1., Comment: 11 pages, 7 figures, 7 tables, MNRAS accepted
Published: 2016
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30. Core or Cusps: The Central Dark Matter Profile of a Strong Lensing Cluster with a Bright Central Image at Redshift 1

Author: Collett, Thomas E, Buckley-Geer, Elizabeth, Lin, Huan, Bacon, David, Nichol, Robert C, Nord, Brian, Morice-Atkinson, Xan, Amara, Adam, Birrer, Simon, Kuropatkin, Nikolay, More, Anupreeta, Papovich, Casey, Romer, Kathy K, Tessore, Nicolas, Abbott, Tim MC, Allam, Sahar, Annis, James, Benoit-Lévy, Aurlien, Brooks, David, Burke, David L, Kind, Matias Carrasco, Castander, Francisco Javier J, D’Andrea, Chris B, da Costa, Luiz N, Desai, Shantanu, Diehl, H Thomas, Doel, Peter, Eifler, Tim F, Flaugher, Brenna, Frieman, Josh, Gerdes, David W, Goldstein, Daniel A, Gruen, Daniel, Gschwend, Julia, Gutierrez, Gaston, James, David J, Kuehn, Kyler, Kuhlmann, Steve, Lahav, Ofer, Li, Ting S, Lima, Marcos, Maia, Marcio AG, March, Marisa, Marshall, Jennifer L, Martini, Paul, Melchior, Peter, Miquel, Ramon, Plazas, Andrs A, Rykoff, Eli S, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Schubnell, Michael, Sevilla-Noarbe, Ignacio, Smith, Mathew, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly EC, Tarle, Gregory, Tucker, Douglas L, and Walker, Alistair R
Subjects: Nuclear and Plasma Physics, Physical Sciences, dark matter, galaxies: clusters: individual, galaxies: halos, gravitational lensing: strong, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We report on SPT-CLJ2011-5228, a giant system of arcs created by a cluster at z = 1.06. The arc system is notable for the presence of a bright central image. The source is a Lyman break galaxy at z s = 2.39 and the mass enclosed within the Einstein ring of radius 14 arcsec is . We perform a full reconstruction of the light profile of the lensed images to precisely infer the parameters of the mass distribution. The brightness of the central image demands that the central total density profile of the lens be shallow. By fitting the dark matter as a generalized Navarro-Frenk-White profile - with a free parameter for the inner density slope - we find that the break radius is kpc, and that the inner density falls with radius to the power -0.38 ±0.04 at 68% confidence. Such a shallow profile is in strong tension with our understanding of relaxed cold dark matter halos; dark matter-only simulations predict that the inner density should fall as . The tension can be alleviated if this cluster is in fact a merger; a two-halo model can also reconstruct the data, with both clumps (density varying as and ) much more consistent with predictions from dark matter-only simulations. At the resolution of our Dark Energy Survey imaging, we are unable to choose between these two models, but we make predictions for forthcoming Hubble Space Telescope imaging that will decisively distinguish between them.
Published: 2017

31. Discovery of two gravitationally lensed quasars in the Dark Energy Survey

Author: Agnello, Adriano, Treu, Tommaso, Ostrovski, Fernanda, Schechter, Paul L., Buckley-Geer, Elizabeth J., Lin, Huan, Auger, Matthew W., Courbin, Frederic, Fassnacht, Christopher D., Frieman, Josh, Kuropatkin, Nikolay, Marshall, Philip J., McMahon, Richard G., Meylan, Georges, More, Anupreeta, Suyu, Sherry H., Rusu, Cristian E., Finley, David, Abbott, Tim, Abdalla, Filipe B., Allam, Sahar, Annis, James, Banerji, Manda, Benoit-Lévy, Aurélien, Bertin, Emmanuel, Brooks, David, Burke, David L., Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Cunha, Carlos E., D'Andrea, Chris B., da Costa, Luiz N., Desai, Shantanu, Diehl, H. Thomas, Dietrich, Jörg P., Doel, Peter, Eifler, Tim F., Estrada, Juan, Neto, Angelo Fausti, Flaugher, Brenna, Fosalba, Pablo, Gerdes, David W., Gruen, Daniel, Gutierrez, Gaston, Honscheid, Klaus, James, David J., Kuehn, Kyler, Lahav, Ofer, Lima, Marco, Maia, Marcio A. G., March, Marina, Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Miller, Christopher J., Miquel, Ramon, Nichol, Robert C., Ogando, Ricardo, Plazas, Andres A., Reil, Kevin, Romer, A. Kathy, Roodman, Aaron, Sako, Masao, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Schubnell, Michael, Sevilla-Noarbe, Ignacio, Smith, R. Chris, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Thaler, Jon, Tucker, Douglas, Walker, Alistair R., Wechsler, Risa H., and Zhang, Yuanyuan
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present spectroscopic confirmation of two new lensed quasars via data obtained at the 6.5m Magellan/Baade Telescope. The lens candidates have been selected from the Dark Energy Survey (DES) and WISE based on their multi-band photometry and extended morphology in DES images. Images of DES J0115-5244 show two blue point sources at either side of a red galaxy. Our long-slit data confirm that both point sources are images of the same quasar at $z_{s}=1.64.$ The Einstein Radius estimated from the DES images is $0.51$". DES J2200+0110 is in the area of overlap between DES and the Sloan Digital Sky Survey (SDSS). Two blue components are visible in the DES and SDSS images. The SDSS fiber spectrum shows a quasar component at $z_{s}=2.38$ and absorption compatible with Mg II and Fe II at $z_{l}=0.799$, which we tentatively associate with the foreground lens galaxy. The long-slit Magellan spectra show that the blue components are resolved images of the same quasar. The Einstein Radius is $0.68$" corresponding to an enclosed mass of $1.6\times10^{11}\,M_{\odot}.$ Three other candidates were observed and rejected, two being low-redshift pairs of starburst galaxies, and one being a quasar behind a blue star. These first confirmation results provide an important empirical validation of the data-mining and model-based selection that is being applied to the entire DES dataset., Comment: 7 pages, 1 figure, 2 tables, MNRAS subm. This paper includes data gathered with the 6.5m Baade Telescopes located at Las Campanas Observatory, Chile. This paper has gone through internal review by the DES collaboration, FERMILAB-PUB-15-341-AE
Published: 2015
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32. Project Dinos I: A joint lensing–dynamics constraint on the deviation from the power law in the mass profile of massive ellipticals.

Author: Tan, Chin Yi, Shajib, Anowar J, Birrer, Simon, Sonnenfeld, Alessandro, Treu, Tommaso, Wells, Patrick, Williams, Devon, Buckley-Geer, Elizabeth J, Drlica-Wagner, Alex, and Frieman, Joshua
Subjects: ELLIPTICAL galaxies, DARK matter, ASTROPHYSICS, GALACTIC redshift, SPACE telescopes, STELLAR dynamics
Abstract: The mass distribution in massive elliptical galaxies encodes their evolutionary history, thus providing an avenue to constrain the baryonic astrophysics in their evolution. The power-law assumption for the radial mass profile in ellipticals has been sufficient to describe several observables to the noise level, including strong lensing and stellar dynamics. In this paper, we quantitatively constrained any deviation, or the lack thereof, from the power-law mass profile in massive ellipticals through joint lensing–dynamics analysis of a large statistical sample with 77 galaxy–galaxy lens systems. We performed an improved and uniform lens modelling of these systems from archival Hubble Space Telescope imaging using the automated lens modelling pipeline dolphin. We combined the lens model posteriors with the stellar dynamics to constrain the deviation from the power law after accounting for the line-of-sight lensing effects, a first for analyses on galaxy–galaxy lenses. We find that the Sloan Lens ACS Survey lens galaxies with a mean redshift of 0.2 are consistent with the power-law profile within 1.1σ (2.8σ) and the Strong Lensing Legacy Survey lens galaxies with a mean redshift of 0.6 are consistent within 0.8σ (2.1σ), for a spatially constant (Osipkov–Merritt) stellar anisotropy profile. We adopted the spatially constant anisotropy profile as our baseline choice based on previous dynamical observables of local ellipticals. However, spatially resolved stellar kinematics of lens galaxies are necessary to differentiate between the two anisotropy models. Future studies will use our lens models to constrain the mass distribution individually in the dark matter and baryonic components. [ABSTRACT FROM AUTHOR]
Published: 2024
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33. The DESI Experiment Part I: Science,Targeting, and Survey Design

Author: Collaboration, DESI, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E, Prieto, Carlos Allende, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C, Bell, Eric F, Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S, Briceno, Cesar, Brooks, David, Brownstein, Joel R, Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G, Cahn, Robert N, Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G, Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J, Cervantes-Cota, Jorge L, Claybaugh, Todd M, Close, Madeline, Coker, Carl T, Cole, Shaun, Comparat, Johan, Cooper, Andrew P, Cousinou, M-C, Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P, Davis, Tamara M, Dawson, Kyle S, Macorra, Axel de la, Vicente, Juan De, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T, Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J, Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R, Finkbeiner, Douglas P, Fitzpatrick, Michael J, Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E, Fosalba, Pablo, Frenk, Carlos S, Fumagalli, Michele, Gaensicke, Boris T, Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Fusillo, Nicola Pietro Gentile, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-de-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, and Guy, Julien
Subjects: astro-ph.IM, astro-ph.CO
Abstract: DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based darkenergy experiment that will study baryon acoustic oscillations (BAO) and thegrowth of structure through redshift-space distortions with a wide-area galaxyand quasar redshift survey. To trace the underlying dark matter distribution,spectroscopic targets will be selected in four classes from imaging data. Wewill measure luminous red galaxies up to $z=1.0$. To probe the Universe out toeven higher redshift, DESI will target bright [O II] emission line galaxies upto $z=1.7$. Quasars will be targeted both as direct tracers of the underlyingdark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for theLy-$\alpha$ forest absorption features in their spectra, which will be used totrace the distribution of neutral hydrogen. When moonlight prevents efficientobservations of the faint targets of the baseline survey, DESI will conduct amagnitude-limited Bright Galaxy Survey comprising approximately 10 milliongalaxies with a median $z\approx 0.2$. In total, more than 30 million galaxyand quasar redshifts will be obtained to measure the BAO feature and determinethe matter power spectrum, including redshift space distortions.
Published: 2016

34. The DESI Experiment Part II: Instrument Design

Author: Collaboration, DESI, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E, Prieto, Carlos Allende, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C, Bell, Eric F, Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S, Briceno, Cesar, Brooks, David, Brownstein, Joel R, Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G, Cahn, Robert N, Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G, Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J, Cervantes-Cota, Jorge L, Claybaugh, Todd M, Close, Madeline, Coker, Carl T, Cole, Shaun, Comparat, Johan, Cooper, Andrew P, Cousinou, M-C, Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P, Davis, Tamara M, Dawson, Kyle S, Macorra, Axel de la, Vicente, Juan De, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T, Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J, Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R, Finkbeiner, Douglas P, Fitzpatrick, Michael J, Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E, Fosalba, Pablo, Frenk, Carlos S, Fumagalli, Michele, Gaensicke, Boris T, Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Fusillo, Nicola Pietro Gentile, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-de-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, and Guy, Julien
Subjects: astro-ph.IM, astro-ph.CO
Abstract: DESI (Dark Energy Spectropic Instrument) is a Stage IV ground-based darkenergy experiment that will study baryon acoustic oscillations and the growthof structure through redshift-space distortions with a wide-area galaxy andquasar redshift survey. The DESI instrument is a robotically-actuated,fiber-fed spectrograph capable of taking up to 5,000 simultaneous spectra overa wavelength range from 360 nm to 980 nm. The fibers feed ten three-armspectrographs with resolution $R= \lambda/\Delta\lambda$ between 2000 and 5500,depending on wavelength. The DESI instrument will be used to conduct afive-year survey designed to cover 14,000 deg$^2$. This powerful instrumentwill be installed at prime focus on the 4-m Mayall telescope in Kitt Peak,Arizona, along with a new optical corrector, which will provide a three-degreediameter field of view. The DESI collaboration will also deliver aspectroscopic pipeline and data management system to reduce and archive alldata for eventual public use.
Published: 2016

35. Strong Gravitational Lensing

Author: Amara, Adam, primary, Buckley-Geer, Elizabeth, additional, Makler, Martin, additional, and Nord, Brian, additional
Published: 2020
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36. The impact of human expert visual inspection on the discovery of strong gravitational lenses

Author: Rojas, Karina, primary, Collett, Thomas E, additional, Ballard, Daniel, additional, Magee, Mark R, additional, Birrer, Simon, additional, Buckley-Geer, Elizabeth, additional, Chan, James H H, additional, Clément, Benjamin, additional, Diego, José M, additional, Gentile, Fabrizio, additional, González, Jimena, additional, Joseph, Rémy, additional, Mastache, Jorge, additional, Schuldt, Stefan, additional, Tortora, Crescenzo, additional, Verdugo, Tomás, additional, Verma, Aprajita, additional, Daylan, Tansu, additional, Millon, Martin, additional, Jackson, Neal, additional, Dye, Simon, additional, Melo, Alejandra, additional, Mahler, Guillaume, additional, Ogando, Ricardo L C, additional, Courbin, Frédéric, additional, Fritz, Alexander, additional, Herle, Aniruddh, additional, Acevedo Barroso, Javier A, additional, Cañameras, Raoul, additional, Cornen, Claude, additional, Dhanasingham, Birendra, additional, Glazebrook, Karl, additional, Martinez, Michael N, additional, Ryczanowski, Dan, additional, Savary, Elodie, additional, Góis-Silva, Filipe, additional, Arturo Ureña-López, L, additional, Wiesner, Matthew P, additional, Wilde, Joshua, additional, Valim Calçada, Gabriel, additional, Cabanac, Rémi, additional, Pan, Yue, additional, Sierra, Isaac, additional, Despali, Giulia, additional, Cavalcante-Gomes, Micaele V, additional, Macmillan, Christine, additional, Maresca, Jacob, additional, Grudskaia, Aleksandra, additional, O’Donnell, Jackson H, additional, Paic, Eric, additional, Niemiec, Anna, additional, de la Bella, Lucia F, additional, Bromley, Jane, additional, Williams, Devon M, additional, More, Anupreeta, additional, and Levine., Benjamin C, additional
Published: 2023
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37. The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)

Author: Silber, Joseph Harry, primary, Fagrelius, Parker, additional, Fanning, Kevin, additional, Schubnell, Michael, additional, Aguilar, Jessica Nicole, additional, Ahlen, Steven, additional, Ameel, Jon, additional, Ballester, Otger, additional, Baltay, Charles, additional, Bebek, Chris, additional, Beard, Dominic Benton, additional, Besuner, Robert, additional, Cardiel-Sas, Laia, additional, Casas, Ricard, additional, Castander, Francisco Javier, additional, Claybaugh, Todd, additional, Dobson, Carl, additional, Duan, Yutong, additional, Dunlop, Patrick, additional, Edelstein, Jerry, additional, Emmet, William T., additional, Elliott, Ann, additional, Evatt, Matthew, additional, Gershkovich, Irena, additional, Guy, Julien, additional, Harris, Stu, additional, Heetderks, Henry, additional, Heetderks, Ian, additional, Honscheid, Klaus, additional, Illa, Jose Maria, additional, Jelinsky, Patrick, additional, Jelinsky, Sharon R., additional, Jimenez, Jorge, additional, Karcher, Armin, additional, Kent, Stephen, additional, Kirkby, David, additional, Kneib, Jean-Paul, additional, Lambert, Andrew, additional, Lampton, Mike, additional, Leitner, Daniela, additional, Levi, Michael, additional, McCauley, Jeremy, additional, Meisner, Aaron, additional, Miller, Timothy N., additional, Miquel, Ramon, additional, Mundet, Juliá, additional, Poppett, Claire, additional, Rabinowitz, David, additional, Reil, Kevin, additional, Roman, David, additional, Schlegel, David, additional, Serrano, Santiago, additional, Van Shourt, William, additional, Sprayberry, David, additional, Tarlé, Gregory, additional, Tie, Suk Sien, additional, Weaverdyck, Curtis, additional, Zhang, Kai, additional, Azzaro, Marco, additional, Bailey, Stephen, additional, Becerril, Santiago, additional, Blackwell, Tami, additional, Bouri, Mohamed, additional, Brooks, David, additional, Buckley-Geer, Elizabeth, additional, Castro, Jose Peñate, additional, Derwent, Mark, additional, Dey, Arjun, additional, Dhungana, Govinda, additional, Doel, Peter, additional, Eisenstein, Daniel J., additional, Fahim, Nasib, additional, Garcia-Bellido, Juan, additional, Gaztañaga, Enrique, additional, A Gontcho, Satya Gontcho, additional, Gutierrez, Gaston, additional, Hörler, Philipp, additional, Kehoe, Robert, additional, Kisner, Theodore, additional, Kremin, Anthony, additional, Kronig, Luzius, additional, Landriau, Martin, additional, Le Guillou, Laurent, additional, Martini, Paul, additional, Moustakas, John, additional, Palanque-Delabrouille, Nathalie, additional, Peng, Xiyan, additional, Percival, Will, additional, Prada, Francisco, additional, Prieto, Carlos Allende, additional, de Rivera, Guillermo Gonzalez, additional, Sanchez, Eusebio, additional, Sanchez, Justo, additional, Sharples, Ray, additional, Soares-Santos, Marcelle, additional, Schlafly, Edward, additional, Weaver, Benjamin Alan, additional, Zhou, Zhimin, additional, Zhu, Yaling, additional, and Zou, Hu, additional
Published: 2022
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38. LensingETC: A Tool to Optimize Multifilter Imaging Campaigns of Galaxy-scale Strong Lensing Systems

Author: Shajib, Anowar J., primary, Glazebrook, Karl, additional, Barone, Tania, additional, Lewis, Geraint F., additional, Jones, Tucker, additional, Tran, Kim-Vy H., additional, Buckley-Geer, Elizabeth, additional, Collett, Thomas E., additional, Frieman, Joshua, additional, and Jacobs, Colin, additional
Published: 2022
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39. Astro2020 APC White Paper: The MegaMapper: a z > 2 Spectroscopic Instrument for the Study of Inflation and Dark Energy

Author: Schlegel, David, primary, Kollmeier, Juna, additional, Aldering, Greg, additional, Bailey, Stephen, additional, Baltay, Charles, additional, Bebek, Christopher, additional, BenZvi, Segev, additional, Besuner, Robert, additional, Blanc, Guillermo, additional, Bolton, Adam, additional, Bouri, Mohamed, additional, Brooks, David, additional, Buckley-Geer, Elizabeth, additional, Cai, Zheng, additional, Crane, Jeffrey, additional, Dey, Arjun, additional, Doel, Peter, additional, Fan, Xiaohui, additional, Ferraro, Simone, additional, Font-Ribera, Andreu, additional, Gutierrez, Gaston, additional, Guy, Julien, additional, Heetderks, Henry, additional, Huterer, Dragan, additional, Infante, Leopoldo, additional, Jelinsky, Patrick, additional, Johns, Matthew, additional, Karagiannis, Dionysios, additional, Kent, Stephen, additional, Kim, Alex, additional, Kneib, Jean-Paul, additional, Kronig, Luzius, additional, Konidaris, Nick, additional, Lahav, Ofer, additional, Lampton, Michael, additional, Lang, Dustin, additional, Leauthaud, Alexie, additional, Liguori, Michele, additional, Linder, Eric, additional, Magneville, Christophe, additional, Martini, Paul, additional, Mateo, Mario, additional, McDonald, Patrick, additional, Miller, Christopher, additional, Moustakas, John, additional, Myers, Adam, additional, Mulchaey, John, additional, Newman, Jeffrey, additional, Nugent, Peter, additional, Palanque-Delabrouille, Nathalie, additional, Padmanabhan, Nikhil, additional, Piro, Anthony, additional, Poppett, Claire, additional, Prochaska, Jason, additional, Pullen, Anthony, additional, Rabinowitz, David, additional, Ramirez, Solange, additional, Rix, Hans-Walter, additional, Ross, Ashley, additional, Samushia, Lado, additional, Schaan, Emmanuel, additional, Schubnell, Michael, additional, Seljak, Uros, additional, Seo, Hee-Jong, additional, Shectman, Stephen, additional, Silber, Joseph, additional, Simon, Joshua, additional, Slepian, Zachary, additional, Soares-Santos, Marcelle, additional, Tarle, Greg, additional, Thompson, Ian, additional, Valluri, Monica, additional, Wechsler, Risa, additional, White, Martin, additional, Wilson, Michael, additional, Yeche, Christophe, additional, and Zaritsky, Dennis, additional
Published: 2019
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40. Cosmology intertwined: A review of the particle physics, astrophysics, and cosmology associated with the cosmological tensions and anomalies

Author: Abdalla, Elcio, primary, Abellán, Guillermo Franco, additional, Aboubrahim, Amin, additional, Agnello, Adriano, additional, Akarsu, Özgür, additional, Akrami, Yashar, additional, Alestas, George, additional, Aloni, Daniel, additional, Amendola, Luca, additional, Anchordoqui, Luis A., additional, Anderson, Richard I., additional, Arendse, Nikki, additional, Asgari, Marika, additional, Ballardini, Mario, additional, Barger, Vernon, additional, Basilakos, Spyros, additional, Batista, Ronaldo C., additional, Battistelli, Elia S., additional, Battye, Richard, additional, Benetti, Micol, additional, Benisty, David, additional, Berlin, Asher, additional, de Bernardis, Paolo, additional, Berti, Emanuele, additional, Bidenko, Bohdan, additional, Birrer, Simon, additional, Blakeslee, John P., additional, Boddy, Kimberly K., additional, Bom, Clecio R., additional, Bonilla, Alexander, additional, Borghi, Nicola, additional, Bouchet, François R., additional, Braglia, Matteo, additional, Buchert, Thomas, additional, Buckley-Geer, Elizabeth, additional, Calabrese, Erminia, additional, Caldwell, Robert R., additional, Camarena, David, additional, Capozziello, Salvatore, additional, Casertano, Stefano, additional, Chen, Geoff C.-F., additional, Chluba, Jens, additional, Chen, Angela, additional, Chen, Hsin-Yu, additional, Chudaykin, Anton, additional, Cicoli, Michele, additional, Copi, Craig J., additional, Courbin, Fred, additional, Cyr-Racine, Francis-Yan, additional, Czerny, Bożena, additional, Dainotti, Maria, additional, D'Amico, Guido, additional, Davis, Anne-Christine, additional, de Cruz Pérez, Javier, additional, de Haro, Jaume, additional, Delabrouille, Jacques, additional, Denton, Peter B., additional, Dhawan, Suhail, additional, Dienes, Keith R., additional, Di Valentino, Eleonora, additional, Du, Pu, additional, Eckert, Dominique, additional, Escamilla-Rivera, Celia, additional, Ferté, Agnès, additional, Finelli, Fabio, additional, Fosalba, Pablo, additional, Freedman, Wendy L., additional, Frusciante, Noemi, additional, Gaztañaga, Enrique, additional, Giarè, William, additional, Giusarma, Elena, additional, Gómez-Valent, Adrià, additional, Handley, Will, additional, Harrison, Ian, additional, Hart, Luke, additional, Hazra, Dhiraj Kumar, additional, Heavens, Alan, additional, Heinesen, Asta, additional, Hildebrandt, Hendrik, additional, Hill, J. Colin, additional, Hogg, Natalie B., additional, Holz, Daniel E., additional, Hooper, Deanna C., additional, Hosseininejad, Nikoo, additional, Huterer, Dragan, additional, Ishak, Mustapha, additional, Ivanov, Mikhail M., additional, Jaffe, Andrew H., additional, Jang, In Sung, additional, Jedamzik, Karsten, additional, Jimenez, Raul, additional, Joseph, Melissa, additional, Joudaki, Shahab, additional, Kamionkowski, Marc, additional, Karwal, Tanvi, additional, Kazantzidis, Lavrentios, additional, Keeley, Ryan E., additional, Klasen, Michael, additional, Komatsu, Eiichiro, additional, Koopmans, Léon V.E., additional, Kumar, Suresh, additional, Lamagna, Luca, additional, Lazkoz, Ruth, additional, Lee, Chung-Chi, additional, Lesgourgues, Julien, additional, Levi Said, Jackson, additional, Lewis, Tiffany R., additional, L'Huillier, Benjamin, additional, Lucca, Matteo, additional, Maartens, Roy, additional, Macri, Lucas M., additional, Marfatia, Danny, additional, Marra, Valerio, additional, Martins, Carlos J.A.P., additional, Masi, Silvia, additional, Matarrese, Sabino, additional, Mazumdar, Arindam, additional, Melchiorri, Alessandro, additional, Mena, Olga, additional, Mersini-Houghton, Laura, additional, Mertens, James, additional, Milaković, Dinko, additional, Minami, Yuto, additional, Miranda, Vivian, additional, Moreno-Pulido, Cristian, additional, Moresco, Michele, additional, Mota, David F., additional, Mottola, Emil, additional, Mozzon, Simone, additional, Muir, Jessica, additional, Mukherjee, Ankan, additional, Mukherjee, Suvodip, additional, Naselsky, Pavel, additional, Nath, Pran, additional, Nesseris, Savvas, additional, Niedermann, Florian, additional, Notari, Alessio, additional, Nunes, Rafael C., additional, Ó Colgáin, Eoin, additional, Owens, Kayla A., additional, Özülker, Emre, additional, Pace, Francesco, additional, Paliathanasis, Andronikos, additional, Palmese, Antonella, additional, Pan, Supriya, additional, Paoletti, Daniela, additional, Perez Bergliaffa, Santiago E., additional, Perivolaropoulos, Leandros, additional, Pesce, Dominic W., additional, Pettorino, Valeria, additional, Philcox, Oliver H.E., additional, Pogosian, Levon, additional, Poulin, Vivian, additional, Poulot, Gaspard, additional, Raveri, Marco, additional, Reid, Mark J., additional, Renzi, Fabrizio, additional, Riess, Adam G., additional, Sabla, Vivian I., additional, Salucci, Paolo, additional, Salzano, Vincenzo, additional, Saridakis, Emmanuel N., additional, Sathyaprakash, Bangalore S., additional, Schmaltz, Martin, additional, Schöneberg, Nils, additional, Scolnic, Dan, additional, Sen, Anjan A., additional, Sehgal, Neelima, additional, Shafieloo, Arman, additional, Sheikh-Jabbari, M.M., additional, Silk, Joseph, additional, Silvestri, Alessandra, additional, Skara, Foteini, additional, Sloth, Martin S., additional, Soares-Santos, Marcelle, additional, Solà Peracaula, Joan, additional, Songsheng, Yu-Yang, additional, Soriano, Jorge F., additional, Staicova, Denitsa, additional, Starkman, Glenn D., additional, Szapudi, István, additional, Teixeira, Elsa M., additional, Thomas, Brooks, additional, Treu, Tommaso, additional, Trott, Emery, additional, van de Bruck, Carsten, additional, Vazquez, J. Alberto, additional, Verde, Licia, additional, Visinelli, Luca, additional, Wang, Deng, additional, Wang, Jian-Min, additional, Wang, Shao-Jiang, additional, Watkins, Richard, additional, Watson, Scott, additional, Webb, John K., additional, Weiner, Neal, additional, Weltman, Amanda, additional, Witte, Samuel J., additional, Wojtak, Radosław, additional, Yadav, Anil Kumar, additional, Yang, Weiqiang, additional, Zhao, Gong-Bo, additional, and Zumalacárregui, Miguel, additional
Published: 2022
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41. Spectroscopic Confirmation of Dark Energy Survey Strong Lensing Systems and Spectra for Photometric Redshift Calibration

Author: Buckley-Geer, Elizabeth, primary
Published: 2021
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42. Discovery of a Candidate Binary Supermassive Black Hole in a Periodic Quasar from Circumbinary Accretion Variability

Author: Liao, Wei-Ting, primary, Chen, Yu-Ching, additional, Liu, Xin, additional, Holgado, A Miguel, additional, Guo, Hengxiao, additional, Gruendl, Robert, additional, Morganson, Eric, additional, Shen, Yue, additional, Davis, Tamara, additional, Kessler, Richard, additional, Martini, Paul, additional, McMahon, Richard G, additional, Allam, Sahar, additional, Annis, James, additional, Avila, Santiago, additional, Banerji, Manda, additional, Bechtol, Keith, additional, Bertin, Emmanuel, additional, Brooks, David, additional, Buckley-Geer, Elizabeth, additional, Rosell, Aurelio Carnero, additional, Kind, Matias Carrasco, additional, Carretero, Jorge, additional, Castander, Francisco Javier, additional, Cunha, Carlos, additional, D’Andrea, Chris, additional, da Costa, Luiz, additional, Davis, Christopher, additional, De Vicente, Juan, additional, Desai, Shantanu, additional, Diehl, H Thomas, additional, Doel, Peter, additional, Eifler, Tim, additional, Evrard, August, additional, Flaugher, Brenna, additional, Fosalba, Pablo, additional, Frieman, Josh, additional, Garcia-Bellido, Juan, additional, Gaztanaga, Enrique, additional, Glazebrook, Karl, additional, Gruen, Daniel, additional, Gschwend, Julia, additional, Gutierrez, Gaston, additional, Hartley, Will, additional, Hollowood, Devon L, additional, Honscheid, Klaus, additional, Hoyle, Ben, additional, James, David, additional, Krause, Elisabeth, additional, Kuehn, Kyler, additional, Lima, Marcos, additional, Maia, Marcio, additional, Marshall, Jennifer, additional, Menanteau, Felipe, additional, Miquel, Ramon, additional, Malagń, Andrés Plazas, additional, Roodman, Aaron, additional, Sanchez, Eusebio, additional, Scarpine, Vic, additional, Schubnell, Michael, additional, Serrano, Santiago, additional, Smith, Mathew, additional, Smith, R Chris, additional, Soares-Santos, Marcelle, additional, Sobreira, Flavia, additional, Suchyta, Eric, additional, Swanson, Molly, additional, Tarle, Gregory, additional, Vikram, Vinu, additional, and Walker, Alistair, additional
Published: 2020
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43. Spectral variability of a sample of extreme variability quasars and implications for the Mg iibroad-line region

Author: Yang, Qian, primary, Shen, Yue, additional, Chen, Yu-Ching, additional, Liu, Xin, additional, Annis, James, additional, Avila, Santiago, additional, Bertin, Emmanuel, additional, Brooks, David, additional, Buckley-Geer, Elizabeth, additional, Carnero Rosell, Aurelio, additional, Carrasco Kind, Matias, additional, Carretero, Jorge, additional, da Costa, Luiz, additional, Desai, Shantanu, additional, Thomas Diehl, H, additional, Doel, Peter, additional, Frieman, Josh, additional, Garcia-Bellido, Juan, additional, Gaztanaga, Enrique, additional, Gerdes, David, additional, Gruen, Daniel, additional, Gruendl, Robert, additional, Gschwend, Julia, additional, Gutierrez, Gaston, additional, Hollowood, Devon L, additional, Honscheid, Klaus, additional, Hoyle, Ben, additional, James, David, additional, Krause, Elisabeth, additional, Kuehn, Kyler, additional, Lidman, Christopher, additional, Lima, Marcos, additional, Maia, Marcio, additional, Marshall, Jennifer, additional, Martini, Paul, additional, Menanteau, Felipe, additional, Miquel, Ramon, additional, Plazas Malagón, Andrés, additional, Sanchez, Eusebio, additional, Scarpine, Vic, additional, Schindler, Rafe, additional, Schubnell, Michael, additional, Serrano, Santiago, additional, Sevilla, Ignacio, additional, Smith, Mathew, additional, Soares-Santos, Marcelle, additional, Sobreira, Flavia, additional, Suchyta, Eric, additional, Swanson, Molly, additional, Tarle, Gregory, additional, Vikram, Vinu, additional, and Walker, Alistair, additional
Published: 2020
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44. Dark Energy and Modified Gravity

Author: Slosar, Anže, Abazajian, Kevork N., Ahmed, Zeeshan, Alonso, David, Amin, Mustafa A., Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Avila, Santiago, Baccigalupi, Carlo, Ballardini, Mario, Bandura, Kevin, Battaglia, Nicholas, Bender, Amy N., Bennett, Charles, Benson, Bradford, Beutler, Florian, Bianchini, F., Bilicki, Maciej, Bischoff, Colin, Biviano, Andrea, Blazek, Jonathan, Bleem, Lindsey, Bolton, Adam S., Bond, J. Richard, Borrill, Julian, Bose, Sownak, Boucaud, Alexandre, Bouchet, Francois R., Buckley-Geer, Elizabeth, Bull, Philip, Cai, Zheng, Carlstrom, John E., Castander, Francisco J., Castorina, Emanuele, Challinor, Anthony, Chang, Tzu-Ching, Chaves-Montero, Jonas, Chisari, Nora Elisa, Clowe, Douglas, Comparat, Johan, Cooray, Asantha, Croft, Rupert A. C., Cyr-Racine, Francis-Yan, D Amico, Guido, Davis, Tamara M., Dawson, Kyle, Demarteau, Marcel, Dey, Arjun, Dore, Olivier, Yutong, Duan, Dunkley, Joanna, Dvorkin, Cora, Eggemeier, Alexander, Eisenstein, Daniel, Ellison, John, Engelen, Alexander, Escoffier, Stephanie, Fabbian, Giulio, Ferraro, Simone, Ferreira, Pedro G., Font-Ribera, Andreu, Foreman, Simon, Fosalba, Pablo, Friedrich, Oliver, Garcıa-Bellido, Juan, Gerbino, Martina, Gill, Mandeep S. S., Gluscevic, Vera, Gontcho A Gontcho, Satya, Gorski, Krzysztof M., Gruen, Daniel, Gudmundsson, Jon E., Gupta, Nikhel, Guy, Julien, Hanany, Shaul, Handley, Will, Hernández-Aguayo, César, Hill, J. Colin, Hirata, Christopher M., Hlozek, Renée, Holder, Gilbert, Huterer, Dragan, Ishak, Mustapha, Jeltema, Tesla, Jha, Saurabh W., Cohen-Tanugi, Johann, Johnson, Bradley, Kamionkowski, Marc, Karkare, Kirit S., E Keeley, Ryan, Khatri, Rishi, Kirkby, David, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., Koyama, Kazuya, Krause, Elisabeth, Benjamin L'Huillier, Lahav, Ofer, Lattanzi, Massimiliano, Leonard, Danielle, Levi, Michael, Liguori, Michele, Linden, Anja, Loverde, Marilena, Lukic, Zarija, La Macorra, Axel, Madhavacheril, Mathew, Plazas, Andres, Spurio Mancini, Alessio, Manera, Marc, Mantz, Adam, Martini, Paul, Masui, Kiyoshi, Mcmahon, Jeff, Meerburg, P. Daniel, Mertens, James, Meyers, Joel, More, Surhud, Motloch, Pavel, Mukherjee, Suvodip, Muñoz, Julian B., Myers, Adam D., Nagy, Johanna, Palanque-Delabrouille, Nathalie, Newburgh, Laura, Newman, Jeffrey A., Niemack, Michael D., Niz, Gustavo, Nomerotski, Andrei, O Connor, Paul, Page, Lyman, Palmese, Antonella, Penna-Lima, Mariana, Percival, Will J., Piacentni, Francesco, Pieri, Matthew M., Pierpaoli, Elena, Pogosian, Levon, Prakash, Abhishek, Pryke, Clement, Puglisi, Giuseppe, Stompor, Radek, Raveri, Marco, Reichardt, Christian L., Rhodes, Jason, Rodney, Steven, Rose, Benjamin, Ross, Ashley J., Rossi, Graziano, Ruhl, John, Saliwanchik, Benjamin, Samushia, Lado, Sanchez, Javier, Sasaki, Misao, Schaan, Emmanuel, Schlegel, David J., Schmittfull, Marcel, Schubnell, Michael, Scott, Douglas, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Sherwin, Blake D., Shi, Feng, Simon, Sara, Slosar, Anze, Staggs, Suzanne, Starkman, Glenn, Stebbins, Albert, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tolley, Andrew J., Tristram, Matthieu, Trodden, Mark, Troxel, M. A., Uhlemann, Cora, Umilta, Caterina, Urenna-Lopez, L. Arturo, Di Valentino, Eleonora, Vargas-Magana, M., Vieregg, Abigail, Walter, Christopher W., Wang, Yi, Watson, Scott, White, Martin, Whitehorn, Nathan, Wu, W. L. K., Xu, Weishuang, Yasini, Siavash, Zaldarriaga, Matias, Zhao, Gong-Bo, Zheng, Yi, Zhu, Hong-Ming, Zhu, Ningfeng, Zuntz, Joe, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de l'Accélérateur Linéaire (LAL), 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), HEP, INSPIRE, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), 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), 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)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), 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), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: cosmological model, Hubble constant, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitation: model, FOS: Physical sciences, cosmic background radiation, baryon: oscillation: acoustic, gravitation: lens, statistical analysis, supernova, Sunyaev-Zel'dovich effect, astro-ph.CO, galaxy: cluster, expansion: acceleration, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Despite two decades of tremendous experimental and theoretical progress, the riddle of the accelerated expansion of the Universe remains to be solved. On the experimental side, our understanding of the possibilities and limitations of the major dark energy probes has evolved; here we summarize the major probes and their crucial challenges. On the theoretical side, the taxonomy of explanations for the accelerated expansion rate is better understood, providing clear guidance to the relevant observables. We argue that: i) improving statistical precision and systematic control by taking more data, supporting research efforts to address crucial challenges for each probe, using complementary methods, and relying on cross-correlations is well motivated; ii) blinding of analyses is difficult but ever more important; iii) studies of dark energy and modified gravity are related; and iv) it is crucial that R&D for a vibrant dark energy program in the 2030s be started now by supporting studies and technical R&D that will allow embryonic proposals to mature. Understanding dark energy, arguably the biggest unsolved mystery in both fundamental particle physics and cosmology, will remain one of the focal points of cosmology in the forthcoming decade., 5 pages + references; science white paper submitted to the Astro2020 decadal survey
Published: 2019

45. Inflation and Dark Energy from spectroscopy at z > 2

Author: Ferraro, Simone, Wilson, Michael J., Abidi, Muntazir, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Baccigalupi, Carlo, Bandura, Kevin, Battaglia, Nicholas, Bavdhankar, Chetan, Bernal, Jos�� Luis, Beutler, Florian, Biagetti, Matteo, Blanc, Guillermo A., Blazek, Jonathan, Bolton, Adam S., Borrill, Julian, Frye, Brenda, Buckley-Geer, Elizabeth, Bull, Philip, Burgess, Cliff, Byrnes, Christian T., Cai, Zheng, Castander, Francisco J, Castorina, Emanuele, Chang, Tzu-Ching, Chaves-Montero, Jon��s, Chen, Shi-Fan, Chen, Xingang, Balland, Christophe, Y��che, Christophe, Cohn, J. D., Coulton, William, Courtois, Helene, Croft, Rupert A. C., Cyr-Racine, Francis-Yan, D'Amico, Guido, Dawson, Kyle, Delabrouille, Jacques, Dey, Arjun, Dor��, Olivier, Douglass, Kelly A., Yutong, Duan, Dvorkin, Cora, Eggemeier, Alexander, Eisenstein, Daniel, Fan, Xiaohui, Ferreira, Pedro G., Font-Ribera, Andreu, Foreman, Simon, Garc��a-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A, Green, Daniel, Guy, Julien, Hahn, ChangHoon, Hanany, Shaul, Handley, Will, Hathi, Nimish, Hawken, Adam J., Hern��ndez-Aguayo, C��sar, Hlo��ek, Ren��e, Huterer, Dragan, Ishak, Mustapha, Kamionkowski, Marc, Karagiannis, Dionysios, Keeley, Ryan E., Kehoe, Robert, Khatri, Rishi, Kim, Alex, Kneib, Jean-Paul, Kollmeier, Juna A., Kovetz, Ely D., Krause, Elisabeth, Krolewski, Alex, L'Huillier, Benjamin, Landriau, Martin, Levi, Michael, Liguori, Michele, Linder, Eric, Luki��, Zarija, de la Macorra, Axel, Plazas, Andr��s A., Marshall, Jennifer L., Martini, Paul, Masui, Kiyoshi, McDonald, Patrick, Meerburg, P. Daniel, Meyers, Joel, Mirbabayi, Mehrdad, Moustakas, John, Myers, Adam D., Palanque-Delabrouille, Nathalie, Newburgh, Laura, Newman, Jeffrey A., Niz, Gustavo, Padmanabhan, Hamsa, Palunas, Povilas, Percival, Will J., Piacentini, Francesco, Pieri, Matthew M., Piro, Anthony L., Prakash, Abhishek, Rhodes, Jason, Ross, Ashley J., Rossi, Graziano, Rudie, Gwen C., Samushia, Lado, Sasaki, Misao, Schaan, Emmanuel, Schlegel, David J., Schmittfull, Marcel, Schubnell, Michael, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Simon, Joshua D., Simon, Sara, Slepian, Zachary, Slosar, An��e, Sridhar, Srivatsan, Stebbins, Albert, Escoffier, Stephanie, Switzer, Eric R., Tarl��, Gregory, Trodden, Mark, Uhlemann, Cora, Uren��a-L��pez, L. Arturo, Di Valentino, Eleonora, Vargas-Maga��a, M., Wang, Yi, Watson, Scott, White, Martin, Xu, Weishuang, Yu, Byeonghee, Zhao, Gong-Bo, Zheng, Yi, and Zhu, Hong-Ming
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), astro-ph.GA, astro-ph.CO, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract: The expansion of the Universe is understood to have accelerated during two epochs: in its very first moments during a period of Inflation and much more recently, at $z < 1$, when Dark Energy is hypothesized to drive cosmic acceleration. The undiscovered mechanisms behind these two epochs represent some of the most important open problems in fundamental physics. The large cosmological volume at $2 < z < 5$, together with the ability to efficiently target high-$z$ galaxies with known techniques, enables large gains in the study of Inflation and Dark Energy. A future spectroscopic survey can test the Gaussianity of the initial conditions up to a factor of ~50 better than our current bounds, crossing the crucial theoretical threshold of $��(f_{NL}^{\rm local})$ of order unity that separates single field and multi-field models. Simultaneously, it can measure the fraction of Dark Energy at the percent level up to $z = 5$, thus serving as an unprecedented test of the standard model and opening up a tremendous discovery space., Science white paper submitted to the Astro2020 Decadal Survey
Published: 2019

46. Core or cusps:the central dark matter profile of a redshift one strong lensing cluster with a bright central image at Redshift 1

Author: Collett, Thomas E., Buckley-Geer, Elizabeth J., Lin, Huan, Bacon, David, Nichol, Robert C., Nord, Brian, Morice-Atkinson, Xan, Amara, Adam, Birrer, Simon, Kuropatkin, Nikolay, More, Anupreeta, Papovich, Casey, Romer, A. Kathy, Tessore, Nicolas, Abbott, Tim M. C., Allam, Sahar S., Annis, James, Benoit-Lévy, Aurélien, Brooks, David, Burke, David L., Kind, Matias Carrasco, Castander, Francisco Javier, D'Andrea, Chris B., Costa, Luiz A. N. da, Desai, Shantanu, Diehl, H. Thomas, Doel, Peter, Eifler, Tim F., Flaugher, Brenna, Frieman, Josh, Gerdes, David W., Goldstein, Daniel A., Gruen, Daniel, Gschwend, Julia, Gutierrez, Gaston R., James, David J., Kuehn, Kyler, Kuhlmann, Steve, Lahav, Ofer, Li, Ting S., Lima, Marcos, Maia, Marcio Antonio Geimba, March, Marisa C., Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Miquel, Ramon, Plazas, Andrés A., Rykoff, Eli S., Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Schubnell, Michael, Sevilla-Noarbe, Ignacio, Smith, Mathew, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Tucker, Douglas L., and Walker, Alistair R.
Subjects: Cosmology and Gravitation, astro-ph.GA, astro-ph.CO, RCUK, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, STFC
Abstract: We report on SPT-CLJ2011-5228, a giant system of arcs created by a cluster at z = 1.06. The arc system is notable for the presence of a bright central image. The source is a Lyman break galaxy at z s = 2.39 and the mass enclosed within the Einstein ring of radius 14 arcsec is ∼ 1014.2 MΘ. We perform a full reconstruction of the light profile of the lensed images to precisely infer the parameters of the mass distribution. The brightness of the central image demands that the central total density profile of the lens be shallow. By fitting the dark matter as a generalized Navarro–Frenk–White profile—with a free parameter for the inner density slope—we find that the break radius is 270∨{-76}^{+48} kpc, and that the inner density falls with radius to the power −0.38 ± 0.04 at 68% confidence. Such a shallow profile is in strong tension with our understanding of relaxed cold dark matter halos; dark matter-only simulations predict that the inner density should fall as r-1. The tension can be alleviated if this cluster is in fact a merger; a two-halo model can also reconstruct the data, with both clumps (density varying as r-0.8 and r-1.0) much more consistent with predictions from dark matter-only simulations. At the resolution of our Dark Energy Survey imaging, we are unable to choose between these two models, but we make predictions for forthcoming Hubble Space Telescope imaging that will decisively distinguish between them.
Published: 2017

47. A study of quasar selection in the supernova fields of the Dark Energy Survey

Author: Tie, Suk Sien, Martini, Paul, Mudd, Dale, Ostrovski, F., Reed, Sophie L., Lidman, Chris, Kochanek, C.S., Davis, Tamara M., Sharp, Robert G., Uddin, Syed, King, Anthea L., Wester, William Carl, Tucker, Bradley, Tucker, Douglas L., Buckley-Geer, Elizabeth, Carollo, Daniela, Childress, Michael, Glazebrook, Karl, Hinton, Samuel, Lewis, Geraint F., Macaulay, Edward, O'Neill, C. R., Abbott, Timothy M. C., Abdalla, Filipe B., Annis, James T., Benoit-Lévy, Aurélien, Bertin, Emmanuel, Brooks, D., Carnero Rosell, Aurelio, Carrasco Kind, Matías, Carretero Palacios, Jorge, Cunha, Carlos Eduardo, Costa, Luiz N. da, DePoy, Darren L., Desai, S., Doel, Peter, Eifler, Tim, Evrard, August E., Finley, David A., Flaugher, Brenna, Fosalba Vela, Pablo, Frieman, Joshua A., García-Bellido, Juan, Gaztañaga, Enrique, Gerdes, David W., Goldstein, Daniel Abraham, Gruen, Daniel, Gruendl, Robert A., Gutierrez, Gaston R., Honscheid, K., James, David J., Kuehn, Kyler, Kuropatkin, Nikolay P., Lima, Marcos Vinicius Borges Teixeira, Maia, Marcio Antonio Geimba, Marshall, Jennifer L., Menanteau, Felipe, Miller, Christopher J., Miquel, Ramon, Nichol, Robert C., Nord, Brian Dennis, Ogando, Ricardo L.C., Plazas Malagón, Andrés Alejandro, Romer, Anita K., Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Scarpine, Victor Emanuel, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Thomas, D., Walker, Alistair, and DES Collaboration
Subjects: Mapeamentos astronômicos, Fotometria astronômica, Catalogos astronomicos, general [Quasars], Quasars
Abstract: We present a study of quasar selection using the supernova fields of the Dark Energy Survey (DES). We used a quasar catalog from an overlapping portion of the SDSS Stripe 82 region to quantify the completeness and efficiency of selection methods involving color, probabilistic modeling, variability, and combinations of color/ probabilistic modeling with variability. In all cases, we considered only objects that appear as point sources in the DES images. We examine color selection methods based on the Wide-field Infrared Survey Explorer (WISE) mid- IR W1 - W2 color, a mixture of WISE and DES colors (g − i and i - W1), and a mixture of Vista Hemisphere Survey and DES colors (g − i and i − K ). For probabilistic quasar selection, we used XDQSO, an algorithm that employs an empirical multi-wavelength flux model of quasars to assign quasar probabilities. Our variability selection uses the multi-band χ2-probability that sources are constant in the DES Year 1 griz-band light curves. The completeness and efficiency are calculated relative to an underlying sample of point sources that are detected in the required selection bands and pass our data quality and photometric error cuts. We conduct our analyses at two magnitude limits, i85% for both i-band magnitude limits and efficiencies of >80% to the bright limit and >60% to the faint limit; however, the giW1 and giW1+variability methods give the highest quasar surface densities. The XDQSOz method and combinations of W1W2/giW1/XDQSOz with variability are among the better selection methods when both high completeness and high efficiency are desired. We also present the OzDES Quasar Catalog of 1263 spectroscopically confirmed quasars from three years of OzDES observation in the 30 deg2 of the DES supernova fields. The catalog includes quasars with redshifts up to z4 and brighter than i = 22 mag, although the catalog is not complete up to this magnitude limit.
Published: 2017

48. An r -process enhanced star in the dwarf galaxy Tucana III

Author: Hansen, Terese T., Simon, Josh D., Marshall, Jennifer L., Li, T. S., Carollo, Daniela, DePoy, Darren L., Nagasawa, Daniel Q., Bernstein, Rebecca A., Drlica-Wagner, Alex, Abdalla, Filipe B., Allam, Sahar S., Annis, James T., Bechtol, Keith, Benoit-Lévy, Aurélien, Brooks, D., Buckley-Geer, Elizabeth, Carnero Rosell, Aurelio, Carrasco Kind, Matías, Carretero Palacios, Jorge, Cunha, Carlos Eduardo, Costa, Luiz N. da, Desai, S., Eifler, Tim, Fausti Neto, Angelo, Flaugher, Brenna, Frieman, Joshua A., García-Bellido, Juan, Gaztañaga, Enrique, Gerdes, David W., Gruen, Daniel, Gruendl, Robert A., Gschwend, Julia de Figueiredo, Gutierrez, Gaston R., James, David J., Krause, Elisabeth, Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, Miquel, Ramon, Plazas Malagón, Andrés Alejandro, Romer, Anita K., Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Scarpine, Victor Emanuel, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Walker, Alistair, and DES Collaboration
Subjects: dwarf [Galaxies], Readable tables, Nucleosíntese, Captura radioativa de nêutrons, abundances [Stars], abundances [galaxies], Metalicidade, Composicao estelar, machine [Supporting material], chemically peculiar [Stars]
Abstract: Chemically peculiar stars in dwarf galaxies provide a window for exploring the birth environment of stars with varying chemical enrichment. We present a chemical abundance analysis of the brightest star in the newly discovered ultra-faint dwarf galaxy candidate Tucana III. Because it is particularly bright for a star in an ultra-faint Milky Way (MW) satellite, we are able to measure the abundance of 28 elements, including 13 neutron-capture species. This star, DES J235532.66−593114.9 (DES J235532), shows a mild enhancement in neutron-capture elements associated with the r-process and can be classified as an r-I star. DES J235532 is the first r-I star to be discovered in an ultra-faint satellite, and Tuc III is the second extremely low-luminosity system found to contain rprocess enriched material, after Reticulum II. Comparison of the abundance pattern of DES J235532 with r-I and r-II stars found in other dwarf galaxies and in the MW halo suggests a common astrophysical origin for the neutron-capture elements seen in all r-process enhanced stars. We explore both internal and external scenarios for the r-process enrichment of Tuc III and show that with abundance patterns for additional stars, it should be possible to distinguish between them.
Published: 2017

49. Nearest neighbor : the low-mass Milky Way satellite Tucana III

Author: Simon, Josh D., Li, T. S., Drlica-Wagner, Alex, Bechtol, Keith, Marshall, Jennifer L., James, David J., Wang, M., Strigari, Louis E., Balbinot, Eduardo, Kuehn, Kyler, Walker, Alistair, Abbott, Timothy M. C., Allam, Sahar S., Annis, James T., Benoit-Lévy, Aurélien, Brooks, D., Buckley-Geer, Elizabeth, Burke, David Lyle, Carnero Rosell, Aurelio, Carrasco Kind, Matías, Carretero Palacios, Jorge, Cunha, Carlos Eduardo, D'Andrea, Christopher B., Costa, Luiz N. da, DePoy, Darren L., Desai, S., Doel, Peter, Fernandez, Enrique, Flaugher, Brenna, Frieman, Joshua A., García-Bellido, Juan, Gaztañaga, Enrique, Goldstein, Daniel Abraham, Gruen, Daniel, Gutierrez, Gaston R., Kuropatkin, Nikolay P., Maia, Marcio Antonio Geimba, Martini, Paul, Menanteau, Felipe, Miller, Christopher J., Miquel, Ramon, Neilsen, Eric H., Nord, Brian Dennis, Ogando, Ricardo L.C., Plazas Malagón, Andrés Alejandro, Romer, Anita K., Rykoff, Eli, Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Scarpine, Victor Emanuel, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Sobreira, Flávia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Whiteway, L., Yanny, Brian, and DES Collaboration
Subjects: dwarf [Galaxies], Via láctea, individual (Tucana III) [Galaxies], abundances [Stars], Dark matter, Local group, Matéria escura, stellar content [Galaxies], Composicao estelar, Metalicidade, Galáxias
Abstract: We present Magellan/IMACS spectroscopy of the recently discovered Milky Way satellite TucanaIII (Tuc III). We identify 26 member stars in TucIII from which we measure a mean radial velocity of vhel=−102.3±0.4 (stat.)±2.0(sys.) km s-1, a velocity dispersion of - 0.1+0.1 0.7 km s-1, and a mean metallicity of = - - [Fe/H] 2.42+0.08 0.07. The upper limit on the velocity dispersion is σ
Published: 2017

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

Author: Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E., Prieto, Carlos Allende, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C., Bell, Eric F., Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S., Briceno, Cesar, Brooks, David, Brownstein, Joel R., Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolás G., Cahn, Robert N., Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G., Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J., Cervantes-Cota, Jorge L., Claybaugh, Todd M., Close, Madeline, Coker, Carl T., Cole, Shaun, Comparat, Johan, Cooper, Andrew P., Cousinou, M. -C., Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P., Davis, Tamara M., Dawson, Kyle S., de La Macorra, Axel, de Vicente, Juan, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T., Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Elliott, Ann, Escoffier, Stephanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R., Finkbeiner, Douglas P., Fitzpatrick, Michael J., Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E., Fosalba, Pablo, Frenk, Carlos S., Fumagalli, Michele, Gaensicke, Boris T., Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Fusillo, Nicola Pietro Gentile, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-De-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, Guy, Julien, Habib, Salman, Heetderks, Henry, Heetderks, Ian, Heitmann, Katrin, Hellwing, Wojciech A., Herrera, David A., Ho, Shirley, Holland, Stephen, Honscheid, Klaus, Huff, Eric, Hutchinson, Timothy A., Huterer, Dragan, Hwang, Ho Seong, Laguna, Joseph Maria Illa, Ishikawa, Yuzo, Jacobs, Dianna, Jeffrey, Niall, Jelinsky, Patrick, Jennings, Elise, Jiang, Linhua, Jimenez, Jorge, Johnson, Jennifer, Joyce, Richard, Jullo, Eric, Juneau, Stéphanie, Kama, Sami, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kennamer, Noble, Kent, Stephen, Kilbinger, Martin, Kim, Alex G., Kirkby, David, Kisner, Theodore, Kitanidis, Ellie, Kneib, Jean-Paul, Koposov, Sergey, Kovacs, Eve, Koyama, Kazuya, Kremin, Anthony, Kron, Richard, Kronig, Luzius, Kueter-Young, Andrea, Lacey, Cedric G., Lafever, Robin, Lahav, Ofer, Lambert, Andrew, Lampton, Michael, Landriau, Martin, Lang, Dustin, Lauer, Tod R., Goff, Jean-Marc Le, Guillou, Laurent Le, van Suu, Auguste Le, Lee, Jae Hyeon, Lee, Su-Jeong, Leitner, Daniela, Lesser, Michael, Levi, Michael E., L'Huillier, Benjamin, Li, Baojiu, Liang, Ming, Lin, Huan, Linder, Eric, Loebman, Sarah R., Lukić, Zarija, Ma, Jun, Maccrann, Niall, Magneville, Christophe, Makarem, Laleh, Manera, Marc, Manser, Christopher J., Marshall, Robert, Martini, Paul, Massey, Richard, Matheson, Thomas, Mccauley, Jeremy, Mcdonald, Patrick, Mcgreer, Ian D., Meisner, Aaron, Metcalfe, Nigel, Miller, Timothy N., Miquel, Ramon, Moustakas, John, Myers, Adam, Naik, Milind, Newman, Jeffrey A., Nichol, Robert C., Nicola, Andrina, da Costa, Luiz Nicolati, Nie, Jundan, Niz, Gustavo, Norberg, Peder, Nord, Brian, Norman, Dara, Nugent, Peter, O'Brien, Thomas, Oh, Minji, Olsen, Knut A. G., Padilla, Cristobal, Padmanabhan, Hamsa, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Palmese, Antonella, Pappalardo, Daniel, Paris, Isabelle, Park, Changbom, Patej, Anna, Peacock, John A., Peiris, Hiranya V., Peng, Xiyan, Percival, Will J., Perruchot, Sandrine, Pieri, Matthew M., Pogge, Richard, Pollack, Jennifer E., Poppett, Claire, Prada, Francisco, Prakash, Abhishek, Probst, Ronald G., Rabinowitz, David, Raichoor, Anand, Ree, Chang Hee, Refregier, Alexandre, Régal, Xavier, Reid, Beth, Reil, Kevin, Rezaie, Mehdi, Rockosi, Constance M., Roe, Natalie, Ronayette, Samuel, Roodman, Aaron, Ross, Ashley J., Ross, Nicholas P., Rossi, Graziano, Rozo, Eduardo, Ruhlmann-Kleider, Vanina, Rykoff, Eli S., Sabiu, Cristiano, Samushia, Lado, Sanchez, Eusebio, Sanchez, Javier, Schlegel, David J., Schneider, Michael, Schubnell, Michael, Secroun, Aurélia, Seljak, Uros, Seo, Hee-Jong, Serrano, Santiago, Shafieloo, Arman, Shan, Huanyuan, Sharples, Ray, Sholl, Michael J., Shourt, William V., Silber, Joseph H., Silva, David R., Sirk, Martin M., Slosar, Anze, Smith, Alex, Smoot, George F., Som, Debopam, Song, Yong-Seon, Sprayberry, David, Staten, Ryan, Stefanik, Andy, Tarlè, Gregory, Tie, Suk Sien, Tinker, Jeremy L., Tojeiro, Rita, Valdes, Francisco, Valenzuela, Octavio, Valluri, Monica, Vargas-Magaña, Mariana, Verde, Licia, Walker, Alistair R., Wang, Jiali, Wang, Yuting, Weaver, Benjamin A., Weaverdyck, Curtis, Wechsler, Risa H., Weinberg, David H., White, Martin, Yang, Qian, Yeche, Christophe, Zhang, Tianmeng, Zhao, Gong-Bo, Zheng, Yi, Zhou, Xu, Zhou, Zhimin, Zhu, Yaling, Zou, Hu, Zu, Ying, Korea Astronomy and Space Science Institute (KASI), Okayama University, University of California [Berkeley], University of California, National Optical Astronomy Observatory (NOAO), Instituto de Astrofisica de Canarias (IAC), Fermi National Accelerator Laboratory (Fermilab), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Yale University [New Haven], Ohio State University [Columbus] (OSU), The University of Notre Dame [Sydney], Department of Astronomy, University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Space Sciences Laboratory [Berkeley] (SSL), University of California-University of California, University of Portsmouth, University of British Columbia (UBC), Ecole Polytechnique Fédérale de Lausanne (EPFL), 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), Cerro Tololo Inter-American Observatory, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Department of Astronomy & Astrophysics [University of Toronto], University of Toronto, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Carreterra Mexico-Toluca, Department of Physics [Durham University], Durham University, Department of Astronomy, The Ohio State University, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), Institute for Computational Cosmology (ICC), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional Autónoma de México (UNAM), Department of Applied Physics, Departamento de Fisica Aplicada [Granada], Universidad de Granada (UGR)-Universidad de Granada (UGR), University College of London [London] (UCL), University of Wyoming (UW), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Arizona State University [Tempe] (ASU), Department of Information Engineering, Zhejiang University of Technology, Zhejiang University of Technology, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Departamento de Fisica Teorica, Institute of Cosmology & Gravitation [Portsmouth], Carnegie Mellon University [Pittsburgh] (CMU), NASA Goddard Space Flight Center (GSFC), Korea Institute for Advanced Study (KIAS), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UCI), Department of Physics, University of California, University of California [Los Angeles] (UCLA), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Center for Cosmology & AstroParticle Physics, California Institute of Technology (CALTECH), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), School of Physics and Astronomy [Nottingham], University of Nottingham, UK (UON), Department of Physics [Durham], University of New Hampshire (UNH), University of Waterloo [Waterloo], Universität Zürich [Zürich] = University of Zurich (UZH), Department of Astronomy and Space Science [Sejong University], Sejong University, Department of Physics [Oxford], University of Oxford [Oxford], Institute of Plasma Physics, Chinese Academy of Sciences (ASIPP), Department of Physics [Ann Arbor], University of St Andrews [Scotland], University of Science and Technology of China [Hefei] (USTC), Department of Computer Science and Engineering [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Karlsruhe Institute of Technology (KIT), National University of Defense Technology [China], DESI Collaboration, University of California [Berkeley] (UC Berkeley), University of California (UC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of California (UC)-University of California (UC), 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 Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Universidad Autónoma de Madrid (UAM), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Universidad de Granada = University of Granada (UGR)-Universidad de Granada = University of Granada (UGR), Harvard University-Smithsonian Institution, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), University of California [Irvine] (UC Irvine), University of Oxford, and Escoffier, Stephanie
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.IM] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::Galaxy Astrophysics
Abstract: DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tracers of the underlying dark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the Ly-$\alpha$ forest absorption features in their spectra, which will be used to trace the distribution of neutral hydrogen. When moonlight prevents efficient observations of the faint targets of the baseline survey, DESI will conduct a magnitude-limited Bright Galaxy Survey comprising approximately 10 million galaxies with a median $z\approx 0.2$. In total, more than 30 million galaxy and quasar redshifts will be obtained to measure the BAO feature and determine the matter power spectrum, including redshift space distortions.
Published: 2016

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