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Start Over Author "Annis, James" Publisher escholarship, university of california
11 results on '"Annis, James"'

1. Probing galaxy evolution in massive clusters using ACT and DES: splashback as a cosmic clock

Author

Adhikari, Susmita, Shin, Tae-hyeon, Jain, Bhuvnesh, Hilton, Matt, Baxter, Eric, Chang, Chihway, Wechsler, Risa H, Battaglia, Nick, Bond, J Richard, Bocquet, Sebastian, DeRose, Joseph, Choi, Steve K, Devlin, Mark, Dunkley, Jo, Evrard, August E, Ferraro, Simone, Hill, J Colin, Hughes, John P, Gallardo, Patricio A, Lokken, Martine, MacInnis, Amanda, McMahon, Jeffrey, Madhavacheril, Mathew S, Nati, Frederico, Newburgh, Laura B, Niemack, Michael D, Page, Lyman A, Palmese, Antonella, Partridge, Bruce, Rozo, Eduardo, Rykoff, Eli, Salatino, Maria, Schillaci, Alessandro, Sehgal, Neelima, Sifón, Cristóbal, To, Chun-Hao, Wollack, Ed, Wu, Hao-Yi, Xu, Zhilei, Aguena, Michel, Allam, Sahar, Amon, Alexandra, Annis, James, Avila, Santiago, Bacon, David, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Burke, David L, Rosell, Aurelio C, Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Choi, Ami, Costanzi, Matteo, Costa, Luiz N da, Vicente, Juan De, Desai, Shantanu, Diehl, Thomas H, Doel, Peter, Everett, Spencer, Ferrero, Ismael, Ferté, Agnès, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, García-Bellido, Juan, Gaztanaga, Enrique, Gruen, Daniel, Gruendl, Robert A, Gschwend, Julia, Gutierrez, Gaston, Hartley, Will G, Hinton, Samuel R, Hollowood, Devon L, Honscheid, Klaus, James, David J, Jeltema, Tesla, Kuehn, Kyler, Kuropatkin, Nikolay, Lahav, Ofer, Lima, Marcos, Maia, Marcio AG, Marshall, Jennifer L, Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Ogando, Ricardo LC, Paz-Chinchón, Francisco, Malagón, Andrés Plazas, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, and Suchyta, Eric

Subjects
astro-ph.GA
Abstract

We measure the projected number density profiles of galaxies and thesplashback feature in clusters selected by the Sunyaev--Zeldovich (SZ) effectfrom the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxiesobserved by the Dark Energy Survey (DES). The splashback radius for thecomplete galaxy sample is consistent with theoretical measurements fromCDM-only simulations, and is located at $2.4^{+0.3}_{-0.4}$ Mpc $h^{-1}$. Wesplit the sample based on galaxy color and find significant differences in theprofile shapes. Red galaxies and those in the green valley show asplashback-like minimum in their slope profile consistent with theoreticalpredictions, while the bluest galaxies show a weak feature that appears at asmaller radius. We develop a mapping of galaxies to subhalos in $N$-bodysimulations by splitting subhalos based on infall time onto the cluster halos.We find that the location of the steepest slope and differences in the shapesof the profiles can be mapped to differences in the average time of infall ofgalaxies of different colors. The minima of the slope in the galaxy profilestrace a discontinuity in the phase space of dark matter halos. By relatingspatial profiles to infall time for galaxies of different colours, we can usesplashback as a clock to understand galaxy quenching. We find that red galaxieshave on average been in their clusters for over $3.2 ~\rm Gyrs$, green galaxiesabout $2.2 ~\rm Gyrs$, while blue galaxies have been accreted most recently andhave not reached apocenter. Using the information from the complete radialprofiles, we fit a simple quenching model and find that the onset of galaxyquenching in clusters occurs after a delay of about a gigayear, and thatgalaxies quench rapidly thereafter with an exponential timescale of $0.6$ Gyr.

Published
2020

2. 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

3. Dark Matter Science in the Era of LSST

Author

Bechtol, Keith, Drlica-Wagner, Alex, Abazajian, Kevork N, Abidi, Muntazir, Adhikari, Susmita, Ali-Haïmoud, Yacine, Annis, James, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Baccigalupi, Carlo, Banerjee, Arka, Banik, Nilanjan, Bennett, Charles, Beutler, Florian, Bird, Simeon, Birrer, Simon, Biswas, Rahul, Biviano, Andrea, Blazek, Jonathan, Boddy, Kimberly K, Bonaca, Ana, Borrill, Julian, Bose, Sownak, Bovy, Jo, Frye, Brenda, Brooks, Alyson M, Buckley, Matthew R, Buckley-Geer, Elizabeth, Bulbul, Esra, Burchat, Patricia R, Burgess, Cliff, Calore, Francesca, Caputo, Regina, Castorina, Emanuele, Chang, Chihway, Chapline, George, Charles, Eric, Chen, Xingang, Clowe, Douglas, Cohen-Tanugi, Johann, Comparat, Johan, Croft, Rupert AC, Cuoco, Alessandro, Cyr-Racine, Francis-Yan, D'Amico, Guido, Davis, Tamara M, Dawson, William A, Macorra, Axel de la, Valentino, Eleonora Di, Rivero, Ana Díaz, Digel, Seth, Dodelson, Scott, Doré, Olivier, Dvorkin, Cora, Eckner, Christopher, Ellison, John, Erkal, Denis, Farahi, Arya, Fassnacht, Christopher D, Ferreira, Pedro G, Flaugher, Brenna, Foreman, Simon, Friedrich, Oliver, Frieman, Joshua, García-Bellido, Juan, Gawiser, Eric, Gerbino, Martina, Giannotti, Maurizio, Gill, Mandeep SS, Gluscevic, Vera, Golovich, Nathan, Gontcho, Satya Gontcho A, González-Morales, Alma X, Grin, Daniel, Gruen, Daniel, Hearin, Andrew P, Hendel, David, Hezaveh, Yashar D, Hirata, Christopher M, Hložek, Renee, Horiuchi, Shunsaku, Jain, Bhuvnesh, Jee, M James, Jeltema, Tesla E, Kamionkowski, Marc, Kaplinghat, Manoj, Keeley, Ryan E, Keeton, Charles R, Khatri, Rishi, Koposov, Sergey E, Koushiappas, Savvas M, Kovetz, Ely D, Lahav, Ofer, Lam, Casey, Lee, Chien-Hsiu, Li, Ting S, Liguori, Michele, Lin, Tongyan, and Lisanti, Mariangela

Subjects
astro-ph.CO, astro-ph.HE, hep-ex
Abstract

Astrophysical observations currently provide the only robust, empiricalmeasurements of dark matter. In the coming decade, astrophysical observationswill guide other experimental efforts, while simultaneously probing uniqueregions of dark matter parameter space. This white paper summarizesastrophysical observations that can constrain the fundamental physics of darkmatter in the era of LSST. We describe how astrophysical observations willinform our understanding of the fundamental properties of dark matter, such asparticle mass, self-interaction strength, non-gravitational interactions withthe Standard Model, and compact object abundances. Additionally, we highlighttheoretical work and experimental/observational facilities that will complementLSST to strengthen our understanding of the fundamental characteristics of darkmatter.

Published
2019

4. 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 HG, 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 MP, Verma, Aprajita, Vilalta, Ricardo, Walter, Christopher W, Yanny, Brian, and Zentner, Andrew R

Subjects
astro-ph.CO, astro-ph.GA, astro-ph.HE, hep-ex, hep-ph
Abstract

Astrophysical and cosmological observations currently provide the onlyrobust, empirical measurements of dark matter. Future observations with LargeSynoptic Survey Telescope (LSST) will provide necessary guidance for theexperimental dark matter program. This white paper represents a communityeffort to summarize the science case for studying the fundamental physics ofdark matter with LSST. We discuss how LSST will inform our understanding of thefundamental properties of dark matter, such as particle mass, self-interactionstrength, non-gravitational couplings to the Standard Model, and compact objectabundances. Additionally, we discuss the ways that LSST will complement otherexperiments to strengthen our understanding of the fundamental characteristicsof dark matter. More information on the LSST dark matter effort can be found athttps://lsstdarkmatter.github.io/ .

Published
2019

5. 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

6. 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

7. The DESI Experiment Part II: Instrument Design

Author

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

Subjects
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

8. A Distributed Network for Intensive Longitudinal Monitoring in Metastatic Triple-Negative Breast Cancer.

Author

Blau, C Anthony, Ramirez, Arturo B, Blau, Sibel, Pritchard, Colin C, Dorschner, Michael O, Schmechel, Stephen C, Martins, Timothy J, Mahen, Elisabeth M, Burton, Kimberly A, Komashko, Vitalina M, Radenbaugh, Amie J, Dougherty, Katy, Thomas, Anju, Miller, Christopher P, Annis, James, Fromm, Jonathan R, Song, Chaozhong, Chang, Elizabeth, Howard, Kellie, Austin, Sharon, Schmidt, Rodney A, Linenberger, Michael L, Becker, Pamela S, Senecal, Francis M, Mecham, Brigham H, Lee, Su-In, Madan, Anup, Ronen, Roy, Dutkowski, Janusz, Heimfeld, Shelly, Wood, Brent L, Stilwell, Jackie L, Kaldjian, Eric P, Haussler, David, and Zhu, Jingchun

Subjects
Biomedical and Clinical Sciences, Oncology and Carcinogenesis, Biotechnology, Cancer, Clinical Research, Clinical Trials and Supportive Activities, Breast Cancer, Good Health and Well Being, Antineoplastic Combined Chemotherapy Protocols, Bone Neoplasms, Community Networks, Drug Resistance, Neoplasm, Drug Screening Assays, Antitumor, Expert Testimony, Female, Follow-Up Studies, Humans, Leukapheresis, Longitudinal Studies, Middle Aged, Neoplasm Metastasis, Neoplastic Cells, Circulating, Research Personnel, Triple Negative Breast Neoplasms, Oncology & Carcinogenesis, Oncology and carcinogenesis, Health services and systems
Abstract

Accelerating cancer research is expected to require new types of clinical trials. This report describes the Intensive Trial of OMics in Cancer (ITOMIC) and a participant with triple-negative breast cancer metastatic to bone, who had markedly elevated circulating tumor cells (CTCs) that were monitored 48 times over 9 months. A total of 32 researchers from 14 institutions were engaged in the patient's evaluation; 20 researchers had no prior involvement in patient care and 18 were recruited specifically for this patient. Whole-exome sequencing of 3 bone marrow samples demonstrated a novel ROS1 variant that was estimated to be present in most or all tumor cells. After an initial response to cisplatin, a hypothesis of crizotinib sensitivity was disproven. Leukapheresis followed by partial CTC enrichment allowed for the development of a differential high-throughput drug screen and demonstrated sensitivity to investigational BH3-mimetic inhibitors of BCL-2 that could not be tested in the patient because requests to the pharmaceutical sponsors were denied. The number and size of CTC clusters correlated with clinical status and eventually death. Focusing the expertise of a distributed network of investigators on an intensively monitored patient with cancer can generate high-resolution views of the natural history of cancer and suggest new opportunities for therapy. Optimization requires access to investigational drugs.

Published
2016

9. THE MULTI-OBJECT, FIBER-FED SPECTROGRAPHS FOR THE SLOAN DIGITAL SKY SURVEY AND THE BARYON OSCILLATION SPECTROSCOPIC SURVEY

Author

Smee, Stephen A, Gunn, James E, Uomoto, Alan, Roe, Natalie, Schlegel, David, Rockosi, Constance M, Carr, Michael A, Leger, French, Dawson, Kyle S, Olmstead, Matthew D, Brinkmann, Jon, Owen, Russell, Barkhouser, Robert H, Honscheid, Klaus, Harding, Paul, Long, Dan, Lupton, Robert H, Loomis, Craig, Anderson, Lauren, Annis, James, Bernardi, Mariangela, Bhardwaj, Vaishali, Bizyaev, Dmitry, Bolton, Adam S, Brewington, Howard, Briggs, John W, Burles, Scott, Burns, James G, Castander, Francisco Javier, Connolly, Andrew, Davenport, James R. A, Ebelke, Garrett, Epps, Harland, Feldman, Paul D, Friedman, Scott D, Frieman, Joshua, Heckman, Timothy, Hull, Charles L, Knapp, Gillian R, Lawrence, David M, Loveday, Jon, Mannery, Edward J, Malanushenko, Elena, Malanushenko, Viktor, Merrelli, Aronne James, Muna, Demitri, Newman, Peter R, Nichol, Robert C, Oravetz, Daniel, Pan, Kaike, Pope, Adrian C, Ricketts, Paul G, Shelden, Alaina, Sandford, Dale, Siegmund, Walter, Simmons, Audrey, Smith, D. Shane, Snedden, Stephanie, Schneider, Donald P, SubbaRao, Mark, Tremonti, Christy, Waddell, Patrick, and York, Donald G

Published
2013

10. A catalog of compact groups of galaxies in the RSDSS commissioning data

Author

Lee, Brian C., Allam, Sahar S., Tucker, Douglas L., Annis, James, Blanton, Michael R., Johnston, David E., Scranton, Ryan, Acebo, Yamina, Bahcall, Neta A., Bartelmann, Matthias, Bohringer, Hans, Ellman, Nancy, Grebel, Eva K., Infante, Leopoldo, Loveday, Jon, McKay, Timothy A., Prada, Francisco, Schneider, Donald P., Stoughton, Chris, Szalay, Alexander S., Vogeley, Michael S., Voges, Wolfgang, and Yanny, Brian

Subjects
Physics of elementary particles and fields, Astrophysics Galaxies
Abstract

Compact groups (CGs) of galaxies -- relatively poor groups of galaxies in which the typical separations between members is of the order of a galaxy diameter -- offer an exceptional laboratory for the study of dense galaxian environments with short (

Published
2003

11. Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

Author

Adhikari, Susmita, Shin, Tae-hyeon, Jain, Bhuvnesh, Hilton, Matt, Baxter, Eric, Chang, Chihway, Wechsler, Risa H, Battaglia, Nick, Bond, J Richard, Bocquet, Sebastian, DeRose, Joseph, Choi, Steve K, Devlin, Mark, Dunkley, Jo, Evrard, August E, Ferraro, Simone, Hill, J Colin, Hughes, John P, Gallardo, Patricio A, Lokken, Martine, MacInnis, Amanda, McMahon, Jeffrey, Madhavacheril, Mathew S, Nati, Frederico, Newburgh, Laura B, Niemack, Michael D, Page, Lyman A, Palmese, Antonella, Partridge, Bruce, Rozo, Eduardo, Rykoff, Eli, Salatino, Maria, Schillaci, Alessandro, Sehgal, Neelima, Sifón, Cristóbal, To, Chun-Hao, Wollack, Ed, Wu, Hao-Yi, Xu, Zhilei, Aguena, Michel, Allam, Sahar, Amon, Alexandra, Annis, James, Avila, Santiago, Bacon, David, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Burke, David L, Rosell, Aurelio C, Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Choi, Ami, Costanzi, Matteo, Costa, Luiz N da, Vicente, Juan De, Desai, Shantanu, Diehl, Thomas H, Doel, Peter, Everett, Spencer, Ferrero, Ismael, Ferté, Agnès, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, García-Bellido, Juan, Gaztanaga, Enrique, Gruen, Daniel, Gruendl, Robert A, Gschwend, Julia, Gutierrez, Gaston, Hartley, Will G, Hinton, Samuel R, Hollowood, Devon L, Honscheid, Klaus, James, David J, Jeltema, Tesla, Kuehn, Kyler, Kuropatkin, Nikolay, Lahav, Ofer, Lima, Marcos, Maia, Marcio AG, Marshall, Jennifer L, Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Ogando, Ricardo LC, Paz-Chinchón, Francisco, Malagón, Andrés Plazas, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, and Suchyta, Eric

Subjects
Particle and Plasma Physics, astro-ph.GA, Molecular, Nuclear, Astronomy & Astrophysics, Atomic, Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev--Zeldovich (SZ) effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius for the complete galaxy sample is consistent with theoretical measurements from CDM-only simulations, and is located at $2.4^{+0.3}_{-0.4}$ Mpc $h^{-1}$. We split the sample based on galaxy color and find significant differences in the profile shapes. Red galaxies and those in the green valley show a splashback-like minimum in their slope profile consistent with theoretical predictions, while the bluest galaxies show a weak feature that appears at a smaller radius. We develop a mapping of galaxies to subhalos in $N$-body simulations by splitting subhalos based on infall time onto the cluster halos. We find that the location of the steepest slope and differences in the shapes of the profiles can be mapped to differences in the average time of infall of galaxies of different colors. The minima of the slope in the galaxy profiles trace a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time for galaxies of different colours, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in their clusters for over $3.2 ~\rm Gyrs$, green galaxies about $2.2 ~\rm Gyrs$, while blue galaxies have been accreted most recently and have not reached apocenter. Using the information from the complete radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching in clusters occurs after a delay of about a gigayear, and that galaxies quench rapidly thereafter with an exponential timescale of $0.6$ Gyr.

Published
2021

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