Author: "Olsen, Knut" / Database: OpenAIRE - Searchworks@Jio Institute Digital Library Search Results

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1. RomAndromeda: The Roman Survey of the Andromeda Halo

Author: Dey, Arjun, Najita, Joan, Filion, Carrie, Han, Jiwon Jesse, Pearson, Sarah, Wyse, Rosemary, Thob, Adrien C. R., Anguiano, Borja, Apfel, Miranda, Arnaboldi, Magda, Bell, Eric F., Silva, Leandro Beraldo e, Besla, Gurtina, Bhattacharya, Aparajito, Bhattacharya, Souradeep, Chandra, Vedant, Choi, Yumi, Collins, Michelle L. M., Cunningham, Emily C., Dalcanton, Julianne J., Escala, Ivanna, Foote, Hayden R., Ferguson, Annette M. N., Gibson, Benjamin J., Gnedin, Oleg Y., Guhathakurta, Puragra, Hawkins, Keith, Horta, Danny, Ibata, Rodrigo, Kallivayalil, Nitya, Koch, Eric W., Koposov, Sergey, Lewis, Geraint F., Macri, Lucas, McKinnon, Kevin A., Nidever, David L., Olsen, Knut A. G., Patel, Ekta, Petersen, Michael S., Petric, Andreea, Price-Whelan, Adrian M., Rich, R. Michael, Riley, Alexander H., Saha, Abhijit, Sanderson, Robyn E., Sharma, Sanjib, Sohn, Sangmo Tony, Soraisam, Monika D., Steinmetz, Matthias, Valluri, Monica, Vivas, A. Katherina, Williams, Benjamin F., and Wojno, J. Leigh
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: As our nearest large neighbor, the Andromeda Galaxy provides a unique laboratory for investigating galaxy formation and the distribution and substructure properties of dark matter in a Milky Way-like galaxy. Here, we propose an initial 2-epoch ($\Delta t\approx 5$yr), 2-band Roman survey of the entire halo of Andromeda, covering 500 square degrees, which will detect nearly every red giant star in the halo (10$\sigma$ detection in F146, F062 of 26.5, 26.1AB mag respectively) and yield proper motions to $\sim$25 microarcsec/year (i.e., $\sim$90 km/s) for all stars brighter than F146 $\approx 23.6$ AB mag (i.e., reaching the red clump stars in the Andromeda halo). This survey will yield (through averaging) high-fidelity proper motions for all satellites and compact substructures in the Andromeda halo and will enable statistical searches for clusters in chemo-dynamical space. Adding a third epoch during the extended mission will improve these proper motions by $\sim t^{-1.5}$, to $\approx 11$ km/s, but this requires obtaining the first epoch in Year 1 of Roman operations. In combination with ongoing and imminent spectroscopic campaigns with ground-based telescopes, this Roman survey has the potential to yield full 3-d space motions of $>$100,000 stars in the Andromeda halo, including (by combining individual measurements) robust space motions of its entire globular cluster and most of its dwarf galaxy satellite populations. It will also identify high-velocity stars in Andromeda, providing unique information on the processes that create this population. These data offer a unique opportunity to study the immigration history, halo formation, and underlying dark matter scaffolding of a galaxy other than our own., Comment: Submitted in response to the call for Roman Space Telescope Core Community Survey white papers
Published: 2023

2. Revealing the Chemical Structure of the Magellanic Clouds with APOGEE. I. Calculating Individual Stellar Ages of RGB Stars in the Large Magellanic Cloud

Author: Povick, Joshua T., Nidever, David L., Massana, Pol, Tayar, Jamie, Olsen, Knut A. G., Hasselquist, Sten, Cioni, Maria-Rosa L., Nitschelm, Christian, Carrera, Ricardo, Choi, Yumi, Roman-Lopes, Alexandre, Majewski, Steven R., Almeida, Andrés, Cunha, Katia, and Smith, Verne V.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: Stellar ages are critical for understanding the temporal evolution of a galaxy. We calculate the ages of over 6000 red giant branch stars in the Large Magellanic Cloud (LMC) observed with SDSS-IV / APOGEE-S. Ages are derived using multi-band photometry, spectroscopic parameters (T$_\text{eff}$, $\log{g}$, [Fe/H], and [$\alpha$/Fe]) and stellar isochrones and the assumption that the stars lie in a thin inclined plane to get accurate distances. The isochrone age and extinction are varied until a best match is found for the observed photometry. We perform validation using the APOKASC sample, which has asteroseismic masses and accurate ages, and find that our uncertainties are $\sim$20% and range from $\sim$1$-$3 Gyr for the calculated age values. Here we present the LMC age map as well as the age-radius relation and an accurate age-metallicity relation (AMR). The age map and age-radius relation reveal that recent star formation in the galaxy was more centrally located and that there is a slight dichotomy between the north and south with the northern fields being slightly younger. The northern fields that cover a known spiral arm have median ages of $\gtrsim$ 2 Gyr, which is the time when an interaction with the SMC is suggested to have happened. The AMR is mostly flat especially for older ages although recently (about 2.0-2.5 Gyr ago) there is an increase in the median [Fe/H]. Based on the time frame, this might also be attributed to the close interaction between the LMC and SMC., Comment: 21 pages, 22 figures, submitted to MNRAS
Published: 2023

3. Chemo-Dynamical Tagging in the Outskirts: The Origins of Stellar Substructures in the Magellanic Clouds

Author: Muñoz, César, Monachesi, Antonela, Nidever, David L., Majewski, Steven R., Cheng, Xinlun, Olsen, Knut, Choi, Yumi, Zivick, Paul, Geisler, Douglas, Almeida, Andres, Muñoz, Ricardo R., Nitschelm, Christian, Roman-Lopes, Alexandre, Lane, Richard R., and Fernández-Trincado, José G.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present the first detailed chemical analysis from APOGEE-2S observations of stars in six regions of recently discovered substructures in the outskirts of the Magellanic Clouds (MCs) extending to 20 degrees from the Large MC (LMC) center. We also present, for the first time, the metallicity and alpha-abundance radial gradients of the LMC and SMC out to 11 degrees and 6 degrees, respectively. Our chemical tagging includes 13 species including light, alpha, and Fe-peak elements. We find that the abundances of all of these chemical elements in stars populating two regions in the northern periphery - along the northern "stream"-like feature - show good agreement with the chemical patterns of the LMC, and thus likely have an LMC origin. For substructures located in the southern periphery of the LMC, we find more complex chemical and kinematical signatures, indicative of a mix of LMC-like and SMC-like populations. However, the southern region closest to the LMC shows better agreement with the LMC, whereas that closest to the SMC shows a much better agreement with the SMC chemical pattern. When combining this information with 3-D kinematical information for these stars, we conclude that the southern region closest to the LMC has likely an LMC origin, whereas that closest to the SMC has an SMC origin, and the other two southern regions have a mix of LMC and SMC origins. Our results add to the evidence that the southern substructures of the LMC periphery are the product of close interactions between the LMC and SMC, and thus likely hold important clues that can constrain models of their detailed dynamical histories., 20 pages, 15 figures, 9 table; submitted to A&A
Published: 2023

4. Astro Data Lab Spectral Viewer Requirements for Wide-Area Spectroscopic Surveys

Author: Fulmer, Leah M., Juneau, Stephanie, Merrill, Catherine, Bolton, Adam S., Nidever, David L., Nikutta, Robert, Ridgway, Stephen T., Olsen, Knut A. G., and Weaver, Benjamin A.
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The Astro Data Lab is preparing to host large spectroscopic datasets such as a copy of the Dark Energy Spectroscopic Instrument (DESI) survey, which is projected to include approximately 40 million spectra of galaxies and quasars as well as over 10 million spectra of stars by 2026. Currently, we serve DR16 spectra from the Sloan Digital Sky Survey (SDSS), including Baryon Oscillation Spectroscopic Survey (BOSS), and Extended BOSS (eBOSS) spectra. A spectral viewer tool allows users to visually and interactively inspect spectra. Given the large size of these spectroscopic datasets, a typical use case might consist of a selection or query for a subset of objects of interest (e.g., a subsample of stars or galaxies or quasars), followed by visual inspection of the selected spectra. It is anticipated that in some cases, users will want to go through a long list of spectra (e.g., thousands) quickly while looking for specific features. This document contains a description of the requirements for such a spectral viewer tool to be incorporated within the Astro Data Lab environment at NSF's NOIRLab. For each object, the spectral viewer will display the observed spectrum and, if available, the noise spectrum, sky spectrum, and best-fit template spectrum. Users will be able to control the display interactively after they launch the tool as part of their Data Lab workflow. The primary objective will be to support the visualization of spectroscopic datasets hosted at the Astro Data Lab but this requirements document could be a useful reference or inspiration for other applications and/or other datasets in the astronomy community., Spectral Viewer requirements document for astrophysical software, 27 pages
Published: 2023

5. NANCY: Next-generation All-sky Near-infrared Community surveY

Author: Han, Jiwon Jesse, Dey, Arjun, Price-Whelan, Adrian M., Najita, Joan, Schlafly, Edward F., Saydjari, Andrew, Wechsler, Risa H., Bonaca, Ana, Schlegel, David J, Conroy, Charlie, Raichoor, Anand, Drlica-Wagner, Alex, Kollmeier, Juna A., Koposov, Sergey E., Besla, Gurtina, Rix, Hans-Walter, Goodman, Alyssa, Finkbeiner, Douglas, Anand, Abhijeet, Ashby, Matthew, Bahr-Kalus, Benedict, Beaton, Rachel, Behera, Jayashree, Bell, Eric F., Bellm, Eric C, BenZvi, Segev, Silva, Leandro Beraldo e, Birrer, Simon, Blanton, Michael R., Bock, Jamie, Broekgaarden, Floor, Brout, Dillon, Brown, Warren, Brown, Anthony G. A., Bulbul, Esra, Calderon, Rodrigo, Carlin, Jeffrey L, Carrillo, Andreia, Castander, Francisco Javier, Chakraborty, Priyanka, Chandra, Vedant, Chiang, Yi-Kuan, Choi, Yumi, Clark, Susan E., Clarkson, William I., Cooper, Andrew, Crill, Brendan, Cunha, Katia, Cunningham, Emily, Dalcanton, Julianne, Danieli, Shany, Daylan, Tansu, de Jong, Roelof S., DeRose, Joseph, Dey, Biprateep, Dickinson, Mark, Dominguez, Mariano, Dong, Dillon, Eifler, Tim, El-Badry, Kareem, Erkal, Denis, Escala, Ivanna, Fazio, Giovanni, Ferguson, Annette M. N., Ferraro, Simone, Filion, Carrie, Forero-Romero, Jaime E., Fu, Shenming, Galbany, Lluís, Garavito-Camargo, Nicolas, Gawiser, Eric, Geha, Marla, Gnedin, Oleg Y., Gomez, Sebastian, Greene, Jenny, Guy, Julien, Hadzhiyska, Boryana, Hawkins, Keith, Heinrich, Chen, Hernquist, Lars, Hirata, Christopher, Hora, Joseph, Horowitz, Benjamin, Horta, Danny, Huang, Caroline, Huang, Xiaosheng, Huanyuan, Shan, Hunt, Jason A. S., Ibata, Rodrigo, Jannuzi, Buell, Johnston, Kathryn V., Jones, Michael G., Juneau, Stephanie, Kado-Fong, Erin, Kalari, Venu, Kallivayalil, Nitya, Karim, Tanveer, Keeley, Ryan, Khoperskov, Sergey, Kim, Bokyoung, Kovács, András, Krause, Elisabeth, Kremer, Kyle, Kremin, Anthony, Krolewski, Alex, Kulkarni, S. R., Kuna, Marine, L'Huillier, Benjamin, Lacy, Mark, Lan, Ting-Wen, Lang, Dustin, Leahy, Denis, Li, Jiaxuan, Lim, Seunghwan, López-Morales, Mercedes, Macri, Lucas, Marc, Manera, Mau, Sidney, McCarthy, Patrick J, McDonald, Eithne, McQuinn, Kristen, Meisner, Aaron, Melnick, Gary, Merloni, Andrea, Millard, Cléa, Millon, Martin, Minchev, Ivan, Montero-Camacho, Paulo, Morales-Gutierrez, Catalina, Morrell, Nidia, Moustakas, John, Moustakas, Leonidas, Murray, Zachary, Mutlu-Pakdil, Burcin, Myeong, GyuChul, Myers, Adam D., Nadler, Ethan, Navarete, Felipe, Ness, Melissa, Nidever, David L., Nikutta, Robert, Nushkia, Chamba, Olsen, Knut, Pace, Andrew B., Pacucci, Fabio, Padmanabhan, Nikhil, Parkinson, David, Pearson, Sarah, Peng, Eric W., Petric, Andreea O., Petric, Andreea, Ratcliffe, Bridget, Razieh, Emami, Reiprich, Thomas, Rezaie, Mehdi, Ricci, Marina, Rich, R. Michael, Richstein, Hannah, Riley, Alexander H., Rockosi, Constance, Rossi, Graziano, Salvato, Mara, Samushia, Lado, Sanchez, Javier, Sand, David J, Sanderson, Robyn E, Šarčević, Nikolina, Sarkar, Arnab, Savino, Alessandro, Schweizer, Francois, Shafieloo, Arman, Shengqi, Yang, Shields, Joseph, Shipp, Nora, Simon, Josh, Siudek, Malgorzata, Siwei, Zou, Slepian, Zachary, Smith, Verne, Sobeck, Jennifer, Sohn, Sangmo Tony, Som, Debopam, Speagle, Joshua S., Spergel, David, Szabo, Robert, Tan, Ting, Theissen, Christopher, Tollerud, Erik, Tolls, Volker, Tran, Kim-Vy, Tsiane, Kabelo, Vacca, William D., Valluri, Monica, Verberi, TonyLouis, Warfield, Jack, Weaverdyck, Noah, Weiner, Benjamin, Weisz, Daniel, Wetzel, Andrew, White, Martin, Williams, Christina C., Wolk, Scott, Wu, John F., Wyse, Rosemary, Yang, Justina R., Zaritsky, Dennis, Zelko, Ioana A., Zhimin, Zhou, and Zucker, Catherine
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The Nancy Grace Roman Space Telescope is capable of delivering an unprecedented all-sky, high-spatial resolution, multi-epoch infrared map to the astronomical community. This opportunity arises in the midst of numerous ground- and space-based surveys that will provide extensive spectroscopy and imaging together covering the entire sky (such as Rubin/LSST, Euclid, UNIONS, SPHEREx, DESI, SDSS-V, GALAH, 4MOST, WEAVE, MOONS, PFS, UVEX, NEO Surveyor, etc.). Roman can uniquely provide uniform high-spatial-resolution (~0.1 arcsec) imaging over the entire sky, vastly expanding the science reach and precision of all of these near-term and future surveys. This imaging will not only enhance other surveys, but also facilitate completely new science. By imaging the full sky over two epochs, Roman can measure the proper motions for stars across the entire Milky Way, probing 100 times fainter than Gaia out to the very edge of the Galaxy. Here, we propose NANCY: a completely public, all-sky survey that will create a high-value legacy dataset benefiting innumerable ongoing and forthcoming studies of the universe. NANCY is a pure expression of Roman's potential: it images the entire sky, at high spatial resolution, in a broad infrared bandpass that collects as many photons as possible. The majority of all ongoing astronomical surveys would benefit from incorporating observations of NANCY into their analyses, whether these surveys focus on nearby stars, the Milky Way, near-field cosmology, or the broader universe., Comment: Submitted to the call for white papers for the Roman Core Community Survey (June 16th, 2023), and to the Bulletin of the AAS
Published: 2023
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6. From Data to Software to Science with the Rubin Observatory LSST

Author: Breivik, Katelyn, Connolly, Andrew J., Ford, K. E. Saavik, Jurić, Mario, Mandelbaum, Rachel, Miller, Adam A., Norman, Dara, Olsen, Knut, O'Mullane, William, Price-Whelan, Adrian, Sacco, Timothy, Sokoloski, J. L., Villar, Ashley, Acquaviva, Viviana, Ahumada, Tomas, AlSayyad, Yusra, Alves, Catarina S., Andreoni, Igor, Anguita, Timo, Best, Henry J., Bianco, Federica B., Bonito, Rosaria, Bradshaw, Andrew, Burke, Colin J., de Campos, Andresa Rodrigues, Cantiello, Matteo, Caplar, Neven, Chandler, Colin Orion, Chan, James, da Costa, Luiz Nicolaci, Danieli, Shany, Davenport, James R. A., Fabbian, Giulio, Fagin, Joshua, Gagliano, Alexander, Gall, Christa, Camargo, Nicolás Garavito, Gawiser, Eric, Gezari, Suvi, Gomboc, Andreja, Gonzalez-Morales, Alma X., Graham, Matthew J., Gschwend, Julia, Guy, Leanne P., Holman, Matthew J., Hsieh, Henry H., Hundertmark, Markus, Ilić, Dragana, Ishida, Emille E. O., Jurkić, Tomislav, Kannawadi, Arun, Kosakowski, Alekzander, Kovačević, Andjelka B., Kubica, Jeremy, Lanusse, François, Lazar, Ilin, Levine, W. Garrett, Li, Xiaolong, Lu, Jing, Luna, Gerardo Juan Manuel, Mahabal, Ashish A., Malz, Alex I., Mao, Yao-Yuan, Medan, Ilija, Moeyens, Joachim, Nikolić, Mladen, Nikutta, Robert, O'Dowd, Matt, Olsen, Charlotte, Pearson, Sarah, Pedraza, Ilhuiyolitzin Villicana, Popinchalk, Mark, Popović, Luka C., Pritchard, Tyler A., Quint, Bruno C., Radović, Viktor, Ragosta, Fabio, Riccio, Gabriele, Riley, Alexander H., Rożek, Agata, Sánchez-Sáez, Paula, Sarro, Luis M., Saunders, Clare, Savić, Đorđe V., Schmidt, Samuel, Scott, Adam, Shirley, Raphael, Smotherman, Hayden R., Stetzler, Steven, Storey-Fisher, Kate, Street, Rachel A., Trilling, David E., Tsapras, Yiannis, Ustamujic, Sabina, van Velzen, Sjoert, Vázquez-Mata, José Antonio, Venuti, Laura, Wyatt, Samuel, Yu, Weixiang, and Zabludoff, Ann
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) dataset will dramatically alter our understanding of the Universe, from the origins of the Solar System to the nature of dark matter and dark energy. Much of this research will depend on the existence of robust, tested, and scalable algorithms, software, and services. Identifying and developing such tools ahead of time has the potential to significantly accelerate the delivery of early science from LSST. Developing these collaboratively, and making them broadly available, can enable more inclusive and equitable collaboration on LSST science. To facilitate such opportunities, a community workshop entitled "From Data to Software to Science with the Rubin Observatory LSST" was organized by the LSST Interdisciplinary Network for Collaboration and Computing (LINCC) and partners, and held at the Flatiron Institute in New York, March 28-30th 2022. The workshop included over 50 in-person attendees invited from over 300 applications. It identified seven key software areas of need: (i) scalable cross-matching and distributed joining of catalogs, (ii) robust photometric redshift determination, (iii) software for determination of selection functions, (iv) frameworks for scalable time-series analyses, (v) services for image access and reprocessing at scale, (vi) object image access (cutouts) and analysis at scale, and (vii) scalable job execution systems. This white paper summarizes the discussions of this workshop. It considers the motivating science use cases, identified cross-cutting algorithms, software, and services, their high-level technical specifications, and the principles of inclusive collaborations needed to develop them. We provide it as a useful roadmap of needs, as well as to spur action and collaboration between groups and individuals looking to develop reusable software for early LSST science., White paper from "From Data to Software to Science with the Rubin Observatory LSST" workshop
Published: 2022

7. Lærerstudenters forventninger til arbeidet som profesjonelle lærere i skolen: Resultater fra en spørreundersøkelse i regi av NFR-prosjektet STEP: Partnerskap for bærekraftig overgang fra lærerutdanning til yrke

Author: Olsen, Knut-Rune, Wedde, Elise, Antonsen, Yngve, Bjerkholt, Eva, Brokke, Tonje Harbek, Gallavara, Gunn, Gilberg, Heidi, Havre, Sissel, Hjardemaal, Finn R, Jakhelln, Rachel, Madsen, Janne, Sandsmark, Jorun, and Stenseth, Anna-Maria
Subjects: lærerutdanning, Samfunnsvitenskap: 200::Pedagogiske fag: 280 [VDP], praksis, lærere
Abstract: Formålet med undersøkelsen var å kartlegge hvilke forventninger det første kullet i den femårige integrerte masterutdanningen for grunnskolelærere har til arbeidet som profesjonelle lærere i skolen. Det empiriske grunnlaget for rapporten består av svar fra studenter som nettopp hadde startet i det siste året i grunnskolelærerutdanningen. Spørreskjemaet omfattet i hovedsak spørsmål med faste svaralternativer, men med anledning for respondentene til å kommentere sine svar. Datainnsamlingen ble gjennomført høsten 2021, i en periode preget av Covid19-pandemien med nedstengning og utstrakt nettbasert undervisning som erstatning for planlagt undervisning på campus. Det er også verdt å merke seg at undersøkelsen ble gjennomført før studentene hadde startet arbeidet med masteroppgaven, og deres vurderinger av utdanningen og betydningen av masteroppgaven må forstås i lys av det. Resultatene viser at studentene generelt sett ser fram til yrkesstarten med forventning og spenning. De føler seg godt forberedt til å undervise i fagene de har fordypning i fra utdanningen. Samtidig viser kommentarene at mange er usikre på om de i tilstrekkelig grad er rustet for bredden og kompleksiteten i utfordringene de forventer å møte i skolen. Denne usikkerheten handler i første rekke om to forhold: For det første er de urolige med tanke på eventuelt å undervise i fag de ikke har fordypning i. Videre indikerer svar og kommentarer at de mener de er lite forberedt til å håndtere en del av de oppgavene som understøtter møtet med elevene i klasserommet. Det gjelder i første rekke samarbeid med foresatte, kontaktlærerrollen, samarbeid med skolens hjelpetjenester og tilrettelegging for elever med særskilte behov. Studentene forventer at overgangen fra utdanning til arbeidet i skolen blir krevende. De har en offensiv og læringsorientert holdning til møtet med disse utfordringene. Når det gjelder deres eget behov for tilrettelegging og lærings-støttende tiltak, peker de i første rekke på forventninger om samarbeid med erfarne kolleger, tilpasning fra ledelsen i form av arbeids- og undervisningsplaner som de kan mestre og deltakelse i en kvalitetssikret veiledningsordning i tråd med de nasjonale prinsippene for veiledning av nyutdannede lærere. På spørsmål om hva studentene mener de vil kunne tilføre det profesjonelle fellesskapet i skolen, peker de på entusiasme og glød for elevenes læring og skolemiljø og vilje til å stimulere til elevmedvirkning og demokratiforståelse. Studentene gir også uttrykk for at de tror de kan bidra med en kritisk-analytisk og utforskende tilnærming til undervisning og læring. Både svar og kommentarer viser at svært mange av studentene primært oppfatter arbeidet med masteroppgaven som en ytterligere fordypning og spesialisering i fag.
Published: 2022

8. 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, Stephanie, 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, T. M. C., 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, Timothee, 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, Gansicke, 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, Lijuan, Huang, W., James, David, Jannuzi, Buell T., Jiang, Linhua, Joyce, Richard, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kneib, Jean-Paul, Kueter-Young, Andrea, Lan, Ting-Wen, Lauer, Tod, Guillou, Laurent Le, Suu, Auguste Le Van, Lee, Jae Hyeon, Lesser, Michael, Levasseur, Laurence Perreault, Li, Ting S., Mann, Justin L., Marshall, Bob, Martinez-Vazquez, C. E., Martini, Paul, Bourboux, Helion du Mas des, McManus, Sean, Meier, Tobias Gabriel, Menard, Brice, Metcalfe, Nigel, Munoz-Gutierrez, Andrea, Najita, Joan, Napier, Kevin, Narayan, Gautham, Newman, Jeffrey A., Nie, Jundan, Nord, Brian, Norman, Dara J., Olsen, Knut A. G., Paat, Anthony, Palanque-Delabrouille, Nathalie, Peng, Xiyan, Poppett, Claire L., Poremba, Megan R., Prakash, Abhishek, Rabinowitz, David, Raichoor, Anand, Rezaie, Mehdi, Robertson, A. N., Roe, Natalie A., Ross, Ashley J., Ross, Nicholas P., Rudnick, Gregory, Safonova, Sasha, Saha, Abhijit, Sanchez, F. Javier, Savary, Elodie, Schweiker, Heidi, Scott, Adam, Seo, Hee-Jong, Shan, Huanyuan, Silva, David R., Slepian, Zachary, Soto, Christian, Sprayberry, David, Staten, Ryan, Stillman, Coley M., Stupak, Robert J., Summers, David L., Tie, Suk Sien, Tirado, H., Vargas-Magana, Mariana, Vivas, A. Katherina, Wechsler, Risa H., Williams, Doug, Yang, Jinyi, Yang, Qian, Yapici, Tolga, Zaritsky, Dennis, Zenteno, A., Zhang, Kai, Zhang, Tianmeng, Zhou, Rongpu, Zhou, Zhimin, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Universidad Antonio Nariño (UAN), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, National University of Defense Technology [China], 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), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autónoma de Madrid (UAM), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), National Optical Astronomy Observatory (NOAO), Columbia University [New York], Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Biologie des Interactions Neurones / Glie, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM), University of Arizona, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Chimie, Modélisation et Imagerie pour la Biologie [Orsay], Université Paris-Sud - Paris 11 (UP11)-Institut Curie [Paris]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Computer Vision Center (Centre de visio per computador) (CVC), Universitat Autònoma de Barcelona (UAB), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Ministry of Education Key Laboratory of Protein Sciences, Center for Structural Biology, Laboratoire de Tribologie et Dynamique des Systèmes (LTDS), École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-École Nationale des Travaux Publics de l'État (ENTPE)-Ecole Nationale d'Ingénieurs de Saint Etienne (ENISE)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Universidad Autonoma de Madrid (UAM), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut National de la Santé et de la Recherche Médicale (INSERM), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université de Lyon-Université de Lyon-École Nationale des Travaux Publics de l'État (ENTPE)-Ecole Nationale d'Ingénieurs de Saint Etienne-Centre National de la Recherche Scientifique (CNRS), National Natural Science Foundation of China, Department of Energy (US), National Energy Research Scientific Computing Center (US), National Science Foundation (US), National Optical Astronomy Observatory (US), Lawrence Berkeley National Laboratory, Harvard University, Dey, Arjun, Schlegel, David J., Lang, Dustin, Blum, Robert, Fan, Xiaohui, Finkbeiner, Douglas, Herrera, David, Juneau, Stephanie, Landriau, Martin, Levi, Michael, McGreer, Ian, Meisner, Aaron, Moustakas, John, Nugent, Peter, Schlafly, Edward F., Walker, Alistair, Valdés, Francisco, Zou, Hu, Abolfathi, Bela, Allen, Lori, Annis, James, Ansarinejad, Behzad, Bell, Eric F., BenZvi, Segev, Beutler, Florian, Calamida, Annalisa, Carlberg, Raymond G., Casas, Richard, Castander, Francisco J., Choi, Yumi, Dickinson, Mark, Duan, Yutong, Fagrelius, Parker, Farihi, Jay, Fulmer, Leah, Gaztañaga, Enrique, George, Koshy, Gerdes, David W., Green, Gregory, James, David J., Jannuz, Buell T., Jiang, Linhua, Joyce, Richard, Karkar, Sonia, Kehoe, Robert, Lan, Ting-Wen, Lauer, Tod R., Le Guillou, Laurent, Lesser, Michael, Marshall, Robert, Martini, Paul, Mas des Bourboux, Hélion du, Metcalfe, Nigel, Narayan, Gautham, Newman, Jeffrey A., Nord, Brian, Olsen, Knut, Prakash, Abhishek, Ross, Nicholas P., Rudnick, Gregory, Safonova, Sasha, Saha, Abhijit, Schweiker, Heidi, Silva, David R., Sien, Suk, Vivas, Kathy, Yang, Jinyi, Yang, Qian, Yapici, Tolga, Zaritsky, Dennis, Zhang, Kai, Zhang, Tianmeng, Zhou, Rongpu, University of St Andrews. School of Physics and Astronomy, Dey, Arjun [0000-0002-4928-4003], Schlegel, David J. [0000-0002-5042-5088], Lang, Dustin [0000-0002-1172-0754], Blum, Robert [0000-0002-8622-4237], Fan, Xiaohui [0000-0003-3310-0131], Finkbeiner, Douglas [0000-0003-2808-275X], Herrera, David [0000-0003-2092-6727], Juneau, Stephanie [0000-0002-0000-2394], Landriau, Martin [0000-0003-1838-8528], Levi, Michael [0000-0003-1887-1018], McGreer, Ian [0000-0002-3461-5228], Meisner, Aaron [0000-0002-1125-7384], Moustakas, John [0000-0002-2733-4559], Nugent, Peter [0000-0002-3389-0586], Schlafly, Edward F. [0000-0002-3569-7421], Walker, Alistair [0000-0002-7123-8943], Valdés, Francisco [0000-0001-5567-1301], Zou, Hu [0000-0002-6684-3997], Abolfathi, Bela [0000-0003-1820-8486], Allen, Lori [0000-0002-7789-5119], Annis, James [0000-0002-0609-3987], Ansarinejad, Behzad [0000-0002-6443-3396], Bell, Eric F. [0000-0002-5564-9873], BenZvi, Segev [0000-0001-5537-4710], Beutler, Florian [0000-0003-0467-5438], Calamida, Annalisa [0000-0002-0882-7702], Carlberg, Raymond G. [0000-0002-7667-0081], Casas, Richard [0000-0002-8165-5601], Castander, Francisco J. [0000-0001-7316-4573], Choi, Yumi [0000-0003-1680-1884], Dickinson, Mark [0000-0001-5414-5131], Duan, Yutong [0000-0002-2611-0895], Fagrelius, Parker [0000-0001-6974-5826], Farihi, Jay [0000-0003-1748-602X], Fulmer, Leah [0000-0001-9247-7794], Gaztañaga, Enrique [0000-0001-9632-0815], George, Koshy [0000-0002-1734-8455], Gerdes, David W. [0000-0001-6942-2736], Green, Gregory [0000-0001-5417-2260], James, David J. [0000-0001-5160-4486], Jannuz, Buell T. [0000-0002-1578-6582], Jiang, Linhua [0000-0003-4176-6486], Joyce, Richard [0000-0003-0201-5241], Karkar, Sonia [0000-0003-2832-777X], Kehoe, Robert [0000-0002-7101-697X], Lan, Ting-Wen [0000-0001-8857-7020], Lauer, Tod R. [0000-0003-3234-7247], Le Guillou, Laurent [0000-0001-7178-8868], Lesser, Michael [0000-0002-7199-0537], Marshall, Robert [0000-0002-6880-9987], Martini, Paul [0000-0002-4279-4182], Mas des Bourboux, Hélion du [0000-0001-8955-3573], Metcalfe, Nigel [0000-0001-9034-4402], Narayan, Gautham [0000-0001-6022-0484], Newman, Jeffrey A. [0000-0001-8684-2222], Nord, Brian [0000-0001-6706-8972], Olsen, Knut [0000-0002-7134-8296], Prakash, Abhishek [0000-0003-4451-4444], Ross, Nicholas P. [0000-0003-1830-6473], Rudnick, Gregory [0000-0001-5851-1856], Safonova, Sasha [0000-0002-2240-7421], Saha, Abhijit [0000-0002-6839-4881], Schweiker, Heidi [0000-0001-9580-4869], Silva, David R. [0000-0002-7678-2155], Sien, Suk [0000-0002-5249-1353], Vivas, Kathy [0000-0003-4341-6172], Yang, Jinyi [0000-0001-5287-4242], Yang, Qian [0000-0002-6893-3742], Yapici, Tolga [0000-0002-5306-4804], Zaritsky, Dennis [0000-0002-5177-727X], Zhang, Kai [0000-0002-9808-3646], Zhang, Tianmeng [0000-0002-8531-5161], Zhou, Rongpu [0000-0001-5381-4372], Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, halo, FOS: Physical sciences, Surveys, 01 natural sciences, milky-way tomography, Footprint, Software, surveys, Observatory, 0103 physical sciences, QB Astronomy, redshift distributions, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, dark energy survey, STFC, QB, 0105 earth and related environmental sciences, Remote sensing, media_common, business.industry, RCUK, Astronomy and Astrophysics, cosmos, 3rd-DAS, Probabilistic inference, Galactic plane, streams, Photometry (astronomy), Space and Planetary Science, Sky, Satellite, digital sky survey, galaxy, Catalogs, Astrophysics - Instrumentation and Methods for Astrophysics, business, sdss, sextractor, catalogs, Geology, astro-ph.IM
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., The BASS is also supported by the External Cooperation Program of Chinese Academy of Sciences (Grant # 114A11KYSB20160057), and Chinese National Natural Science Foundation (Grant # 11433005). The Legacy Surveys imaging of the DESI footprint is supported by the Director, Office of Science, Office of High Energy Physics of the U.S. Department of Energy under Contract No. DE-AC02- 05CH11231, by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract; and by the U.S. National Science Foundation, Division of Astronomical Sciences under Contract No. AST-0950945 to NOAO. Travel and other support for the DECaLS and MzLS projects is provided by the National Optical Astronomy Observatory, the Lawrence Berkeley National Laboratory, and the DESI Project. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013) / ERC Grant Agreement n. 320964 (WDTracer). J. Moustakas gratefully acknowledges support from the National Science Foundation grant AST1616414. A. Dey thanks the Radcliffe Institute for Advanced Study for their generous support during the year these surveys were initiated. A. Dey, D. J. Schlegel, and D. Lang thank the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293, for their hospitality and support during summer 2015 during which part of this work was conducted.
Published: 2019
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9. Jupyter-Enabled Astrophysical Analysis for Researchers and Students

Author: Juneau, St��phanie, Olsen, Knut A. G., Nikutta, Robert, Jacques, Alice, and Bailey, Stephen
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies
Abstract: The advent of increasingly large and complex datasets has fundamentally altered the way that scientists conduct astronomy research. The need to work closely to the data has motivated the creation of online science platforms, which include a suite of software tools and services, therefore going beyond data storage and data access. We present two example applications of Jupyter as a part of astrophysical science platforms for professional researchers and students. First, the Astro Data Lab is developed and operated by NOIRLab with a mission to serve the astronomy community with now over 1500 registered users. Second, the Dark Energy Spectroscopic Instrument science platform serves its geographically distributed team comprising about 900 collaborators from over 90 institutions. We describe the main uses of Jupyter and the interfaces that needed to be created to embed it within science platform ecosystems. We use these examples to illustrate the broader concept of empowering researchers and providing them with access to not only large datasets but also cutting-edge software, tools, and data services without requiring any local installation, which can be relevant for a wide range of disciplines. Future advances may involve science platform networks, and tools for simultaneously developing Jupyter notebooks to facilitate collaborations., 13 pages, 4 figures. Accepted version. See Computing in Science and Engineering for the final published version: Jupyter-Enabled Astrophysical Analysis Using Data-Proximate Computing Platforms
Published: 2021

10. NOIRLab Astro Data Archive

Author: McManus, Sean and Olsen, Knut
Abstract: An archive of raw, reduced, and high-level data products is critical to maximizing the scientific productivity of an observatory. Archives act as multipliers of scientific impact and accessibility and prepare their communities to become frontline users of observatory facilities. The NOIRLab Community Science and Data Center (CSDC) maintains a multi-petabytescale library spanning 25+ years of data taken at Cerro Tololo InterAmerican Observatory (CTIO) and Kitt Peak National Observatory (KPNO).
Published: 2021
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11. News from the Magellanic Clouds

Author: Vivas, Kathy, Nidever, David, Olsen, Knut, Ruiz-Lara, Tomas, Massana, Pol, and Bell, Cameron
Abstract: The Survey of the MAgellanic Stellar History (SMASH; [1]) was designed to study in depth the two largest satellites of the Milky Way, the Magellanic Clouds. This survey, with the Dark Energy Camera (DECam; which is funded mainly by the US Department of Energy), mapped 480 square degrees (distributed over 2,400 square degrees in and around the Clouds) in five photometric bands (ugriz) down to magnitude ~24 in each band. All of the observations were released in SMASH DR2 [2] and are available via NOIRLab’s Astro Data Lab. Although the observations were collected during the period 2013–2016, the SMASH collaboration continues exploiting the rich dataset. We report here three new exciting results from the survey.
Published: 2021
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12. The impact of frailty on ICU and 30-day mortality and the level of care in very elderly patients (≥ 80 years)

Author: Flaatten, Hans, De Lange, Dylan W., Morandi, Alessandro, Andersen, Finn H., Artigas, Antonio, Bertolini, Guido, Boumendil, Ariane, Cecconi, Maurizio, Christensen, Steffen, Faraldi, Loredana, Fjølner, Jesper, Jung, Christian, Marsh, Brian, Moreno, Rui, Oeyen, Sandra, Öhman, Christina Agwald, Pinto, Bernardo Bollen, Soliman, Ivo W., Szczeklik, Wojciech, Valentin, Andreas, Watson, Ximena, Zaferidis, Tilemachos, Guidet, Bertrand, Schmutz, René, Wimmer, Franz, Eller, Philipp, Zotter, Klemens, Swinnen, Walter, De Buysscher, Pieter, De Neve, Nikolaas, Abraham, Paul, Fleury, Yvan, Schefold, Joerg C., Biskup, Ewelina, Taliadoros, Ioannis, Piza, Petr, Lauten, Alexander, Sacher, Anna Lena, Brenner, Thorsten, Franz, Marcus, Bloos, Frank, Ebelt, Henning, Schaller, Stefan J., Fuest, Kristina, Rabe, Christian, Dieck, Thorben, Steiner, Stephan, Graf, Tobias, Nia, Amir M., Janosi, Rolf Alexander, Meybohm, Patrick, Simon, Philipp, Utzolino, Stefan, Rahmel, Tim, Barth, Eberhard, Schuster, Michael, Dey, Nilanjan, Sølling, Christoffer, Rasmussen, Bodil Steen, Rodriguez, Enver, Rebollo, Sergio, Aguilar, Gerardo, Masdeu, Gaspar, Jaimes, Marián Irazábal, Prado Mira, Ángela, Bodi, Maria A., Barea Mendoza, Jesus A., López-Cuenca, Sonia, Homez Guzman, Marcela, Rico-Feijoo, Jesús, Ibarz, Mercedes, Trenado-Alvarez, Josep, Forceville, Xavier, Besch, Guillaume, Mentec, Herve, Michel, Philippe, Mateu, Philippe, Vettoretti, Lucie, Bourenne, Jeremy, Marin, Nathalie, Guillot, Max, Aissaoui, Naida, Goulenok, Cyril, Thieulot-Rolin, Nathalie, Messika, Jonathan, Lamhaut, Lionel, Charron, Cyril, Dempsey, Ged, Mathew, Shiju J., Raj, Ashok S., Grecu, Irina, Cupitt, Jason, Lawton, Tom, Clark, Richard, Popescu, Monica, Spittle, Nick, Faulkner, Maria, Cowton, Amanda, Elloway, Esme, Williams, Patricia, Reay, Michael, Chukkambotla, Srikanth, Kumar, Ravi, Al-Subaie, Nawaf, Kent, Linda, Tamm, Tiina, Kajtor, Istvan, Burns, Karen, Pugh, Richard, Ostermann, Marlies, Kam, Elisa, Bowyer, Helen, Smith, Neil, Templeton, Maie, Henning, Jeremy, Goffin, Kelly, Kapoor, Ritoo, Laha, Shondipon, Chilton, Phil, Khaliq, Waqas, Crayford, Alison, Coetzee, Samantha, Tait, Moira, Boultoukas, Evangelos, Stoker, Wendy, Gimenez, Marc, Pope, Alan, Camsooksai, Julie, Pogson, David, Quigley, Kate, Ritzema, Jenny, Hormis, Anil, Boulanger, Carole, Balasubramaniam, M., Vamplew, Luke, Burt, Karen, Martin, Daniel, Craig, Jayne, Prowle, John, Doyle, Nanci, Shelton, Jonathon, Scott, Carmen, Donnison, Phil, Shelton, Sarah, Frey, Christian, Ryan, Christine, Spray, Dominic, Barnes, Veronica, Barnes, Kerry, Furneval, Julie, Ridgway, Stephanie, Saha, Rajnish, Clark, Thomas, Wood, James, Bolger, Clare, Bassford, Christopher, Lewandowski, john, Zhao, Xiaobei, Humphreys, Sally, Dowling, Susan, Richardson, Neil, Burtenshaw, Andrew, Stevenson, Carl, Wilcock, Danielle, Aidoni, Zoi, Aloizos, Stavros, Tasioudis, Polychronis, Lampiri, Kleri, Zisopoulou, Vasiliki, Ifigenia, Ravani, Eymorfia, Pagaki, Angela, Anttoniou, Katsoulas, Theodoros A., Kyparissi, Aikaterini, Aikaterini, Kounougeri, Marinakis, George, Tsimpoukas, Fotios, Spyropoulou, Anastasia, Zygoulis, Paris, Hayes, Ivan, Kelly, Yvelynne, Westbrook, Andrew, Fitzpatrick, Gerry, Maheshwari, Darshana, Motherway, Catherine, Gupta, Manish, Gurjar, Mohan, Maji, Ismail M, Negri, Giovanni, Spadaro, Savino, Nattino, Giuseppe, Pedeferri, Matteo, Boscolo, Annalisa, Rossi, Simona, Rossi, Maurizio, Calicchio, Giuseppe, Cubattoli, Lucia, Di Lascio, Gabriella, Barbagallo, Maria, Berruto, Francesco, Codazzi, Daniela, Bottazzi, Andrea, Fumagalli, Paolo, Negro, Giancarlo, Lupi, Giuseppe, Savelli, Flavia, Vulcano, Giuseppe A., Fumagalli, Roberto, Marudi, Andrea, Lefons, Ugo, Lembo, Rita, Babini, Maria, Paggioro, Alessandra, Parrini, Vieri, Zaccaria, Maria, Clementi, Stefano, Gigliuto, Carmelo, Facondini, Francesca, Pastorini, Simonetta, Munaron, Susanna, Calamai, Italo, Bocchi, Anna, Brizio, Elisabetta, Adorni, Adele, Bocci, Maria Grazia, Cortegiani, Andrea, Casalicchio, Tiziana, Mellea, Serena, Graziani, Elia, Barattini, Massimo, van Dijk, I., van Lelyveld-Haas, L. E. M., Ramnarain, D., Jansen, Tim, Nooteboom, Fleur, van der Voort, Peter H. J., Dieperink, Willem, de Waard, Monique C., Bormans, Laura, Hahn, Michael, Kemmerer, Nicolai, Strietzel, Hans Frank, Fehrle, Lutz, Dybwik, Knut, Legernaes, Terje, Klepstad, Pål, Olaussen, Even Braut, Olsen, Knut Inge, Børresen, Ole Marius, Bjørsvik, Geir, Maini, Sameer, Czuczwar, Miroslaw, Krawczyk, Pawel, Ziętkiewicz, Mirosław, Nowak, Łukasz R., Kotfis, Katarzyna, Cwyl, Katarzyna, Gajdosz, Ryszard, Biernawska, Jowita, Grudzień, Paweł, Nasiłowski, Paweł, Popek, Natalia, Cyrankiewicz, Waldemar, Wnuk, Marek, Maciejewski, Dariusz, Studzińska, Dorota, Zukowski, Maciej, Bernas, Szymon, Serwa, Marta, Stefaniak, Jan, Pawel, Maciejewski, Szymkowiak, Malgorzata, Adamik, Barbara, Catorze, Nuno, Castelo Branco, Miguel, Barros, Inês, Barros, Nelson, Krystopchuk, Andriy, Honrado, Teresa, Sousa, Cristina, Munoz, Francisco, Rebelo, Marta, Gomes, Rui, Nunes, Jorge, Dias, Celeste, Fernandes, Ana Margarida, Petrisor, Cristina, Constantin, Bodolea, Belskiy, Vladislav, Boskholov, Boris, Kawati, Rafael, Sivik, Joakim, Nauska, Jessica, Smole, Daniel, Parenmark, Fredric, Lyrén, Johanna, Rockstroh, Katalin, Rydén, Sara, Spångfors, Martin, Strinnholm, Morten, Walther, Sten, De Geer, Lina, Nordlund, Peter, Pålsson, Staffan, Zetterquist, Harald, Nilsson, Annika, Thiringer, Karin, Jungner, Mårten, Bark, Björn, Nordling, Berit, Sköld, Hans, Brorsson, Camilla, Persson, Stefan, Bergström, Anna, Berkius, Johan, Holmström, Johanna, Yapici, Nihan, University of Bergen (UiB), Haukeland University Hospital, University Medical Center [Utrecht], CIBER de Epidemiología y Salud Pública (CIBERESP), Istituto di Ricovero e Cura a Carattere Scientifico (IRCCS), St George’s University Hospitals, Aarhus University Hospital, Mater Misericordiae University Hospital (The Mater Hospital), NOVA Medical School - Faculdade de Ciências Médicas (NMS), Universidade Nova de Lisboa = NOVA University Lisbon (NOVA), Ghent University Hospital, Karolinska University Hospital [Stockholm], Hôpitaux Universitaires de Genève (HUG), Uniwersytet Jagielloński w Krakowie = Jagiellonian University (UJ), Institut Pierre Louis d'Epidémiologie et de Santé Publique (iPLESP), Institut National de la Santé et de la Recherche Médicale (INSERM)-Sorbonne Université (SU), Service de Réanimation Médicale [CHU Saint-Antoine], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-CHU Saint-Antoine [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Sorbonne Université (SU), Gestionnaire, Hal Sorbonne Université, Flaatten, H, De Lange, D, Morandi, A, Andersen, F, Artigas, A, Bertolini, G, Boumendil, A, Cecconi, M, Christensen, S, Faraldi, L, Fjolner, J, Jung, C, Marsh, B, Moreno, R, Oeyen, S, Ohman, C, Pinto, B, Soliman, I, Szczeklik, W, Valentin, A, Watson, X, Zaferidis, T, Guidet, B, Schmutz, R, Wimmer, F, Eller, P, Zotter, K, Swinnen, W, De Buysscher, P, De Neve, N, Abraham, P, Fleury, Y, Schefold, J, Biskup, E, Taliadoros, I, Piza, P, Lauten, A, Sacher, A, Brenner, T, Franz, M, Bloos, F, Ebelt, H, Schaller, S, Fuest, K, Rabe, C, Dieck, T, Steiner, S, Graf, T, Nia, A, Janosi, R, Meybohm, P, Simon, P, Utzolino, S, Rahmel, T, Barth, E, Schuster, M, Dey, N, Solling, C, Rasmussen, B, Rodriguez, E, Rebollo, S, Aguilar, G, Masdeu, G, Jaimes, M, Prado Mira, A, Bodi, M, Barea Mendoza, J, Lopez-Cuenca, S, Homez Guzman, M, Rico-Feijoo, J, Ibarz, M, Trenado-Alvarez, J, Forceville, X, Besch, G, Mentec, H, Michel, P, Mateu, P, Vettoretti, L, Bourenne, J, Marin, N, Guillot, M, Aissaoui, N, Goulenok, C, Thieulot-Rolin, N, Messika, J, Lamhaut, L, Charron, C, Dempsey, G, Mathew, S, Raj, A, Grecu, I, Cupitt, J, Lawton, T, Clark, R, Popescu, M, Spittle, N, Faulkner, M, Cowton, A, Elloway, E, Williams, P, Reay, M, Chukkambotla, S, Kumar, R, Al-Subaie, N, Kent, L, Tamm, T, Kajtor, I, Burns, K, Pugh, R, Ostermann, M, Kam, E, Bowyer, H, Smith, N, Templeton, M, Henning, J, Goffin, K, Kapoor, R, Laha, S, Chilton, P, Khaliq, W, Crayford, A, Coetzee, S, Tait, M, Boultoukas, E, Stoker, W, Gimenez, M, Pope, A, Camsooksai, J, Pogson, D, Quigley, K, Ritzema, J, Hormis, A, Boulanger, C, Balasubramaniam, M, Vamplew, L, Burt, K, Martin, D, Craig, J, Prowle, J, Doyle, N, Shelton, J, Scott, C, Donnison, P, Shelton, S, Frey, C, Ryan, C, Spray, D, Barnes, V, Barnes, K, Furneval, J, Ridgway, S, Saha, R, Clark, T, Wood, J, Bolger, C, Bassford, C, Lewandowski, J, Zhao, X, Humphreys, S, Dowling, S, Richardson, N, Burtenshaw, A, Stevenson, C, Wilcock, D, Aidoni, Z, Aloizos, S, Tasioudis, P, Lampiri, K, Zisopoulou, V, Ifigenia, R, Eymorfia, P, Angela, A, Katsoulas, T, Kyparissi, A, Aikaterini, K, Marinakis, G, Tsimpoukas, F, Spyropoulou, A, Zygoulis, P, Hayes, I, Kelly, Y, Westbrook, A, Fitzpatrick, G, Maheshwari, D, Motherway, C, Gupta, M, Gurjar, M, Maji, I, Negri, G, Spadaro, S, Nattino, G, Pedeferri, M, Boscolo, A, Rossi, S, Rossi, M, Calicchio, G, Cubattoli, L, Di Lascio, G, Barbagallo, M, Berruto, F, Codazzi, D, Bottazzi, A, Fumagalli, P, Negro, G, Lupi, G, Savelli, F, Vulcano, G, Fumagalli, R, Marudi, A, Lefons, U, Lembo, R, Babini, M, Paggioro, A, Parrini, V, Zaccaria, M, Clementi, S, Gigliuto, C, Facondini, F, Pastorini, S, Munaron, S, Calamai, I, Bocchi, A, Brizio, E, Adorni, A, Bocci, M, Cortegiani, A, Casalicchio, T, Mellea, S, Graziani, E, Barattini, M, van Dijk, I, van Lelyveld-Haas, L, Ramnarain, D, Jansen, T, Nooteboom, F, van der Voort, P, Dieperink, W, de Waard, M, Bormans, L, Hahn, M, Kemmerer, N, Strietzel, H, Fehrle, L, Dybwik, K, Legernaes, T, Klepstad, P, Olaussen, E, Olsen, K, Borresen, O, Bjorsvik, G, Maini, S, Czuczwar, M, Krawczyk, P, Zietkiewicz, M, Nowak, L, Kotfis, K, Cwyl, K, Gajdosz, R, Biernawska, J, Grudzien, P, Nasilowski, P, Popek, N, Cyrankiewicz, W, Wnuk, M, Maciejewski, D, Studzinska, D, Zukowski, M, Bernas, S, Serwa, M, Stefaniak, J, Pawel, M, Szymkowiak, M, Adamik, B, Catorze, N, Castelo Branco, M, Barros, I, Barros, N, Krystopchuk, A, Honrado, T, Sousa, C, Munoz, F, Rebelo, M, Gomes, R, Nunes, J, Dias, C, Fernandes, A, Petrisor, C, Constantin, B, Belskiy, V, Boskholov, B, Kawati, R, Sivik, J, Nauska, J, Smole, D, Parenmark, F, Lyren, J, Rockstroh, K, Ryden, S, Spangfors, M, Strinnholm, M, Walther, S, De Geer, L, Nordlund, P, Palsson, S, Zetterquist, H, Nilsson, A, Thiringer, K, Jungner, M, Bark, B, Nordling, B, Skold, H, Brorsson, C, Persson, S, Bergstrom, A, Berkius, J, Holmstrom, J, Yapici, N, Flaatten, Han, De Lange, Dylan W., Morandi, Alessandro, Andersen, Finn H., Artigas, Antonio, Bertolini, Guido, Boumendil, Ariane, Cecconi, Maurizio, Christensen, Steffen, Faraldi, Loredana, Fjølner, Jesper, Jung, Christian, Marsh, Brian, Moreno, Rui, Oeyen, Sandra, Öhman, Christina Agwald, Pinto, Bernardo Bollen, Soliman, Ivo W., Szczeklik, Wojciech, Valentin, Andrea, Watson, Ximena, Zaferidis, Tilemacho, Guidet, Bertrand, Schmutz, René, Wimmer, Franz, Eller, Philipp, Zotter, Klemen, Swinnen, Walter, De Buysscher, Pieter, De Neve, Nikolaa, Abraham, Paul, Fleury, Yvan, Schefold, Joerg C., Biskup, Ewelina, Taliadoros, Ioanni, Piza, Petr, Lauten, Alexander, Sacher, Anna Lena, Brenner, Thorsten, Franz, Marcu, Bloos, Frank, Ebelt, Henning, Schaller, Stefan J., Fuest, Kristina, Rabe, Christian, Dieck, Thorben, Steiner, Stephan, Graf, Tobia, Nia, Amir M., Janosi, Rolf Alexander, Meybohm, Patrick, Simon, Philipp, Utzolino, Stefan, Rahmel, Tim, Barth, Eberhard, Schuster, Michael, Dey, Nilanjan, Sølling, Christoffer, Rasmussen, Bodil Steen, Rodriguez, Enver, Rebollo, Sergio, Aguilar, Gerardo, Masdeu, Gaspar, Jaimes, Marián Irazábal, Prado Mira, Ángela, Bodi, Maria A., Barea Mendoza, Jesus A., López-Cuenca, Sonia, Homez Guzman, Marcela, Rico-Feijoo, Jesú, Ibarz, Mercede, Trenado-Alvarez, Josep, Forceville, Xavier, Besch, Guillaume, Mentec, Herve, Michel, Philippe, Mateu, Philippe, Vettoretti, Lucie, Bourenne, Jeremy, Marin, Nathalie, Guillot, Max, Aissaoui, Naida, Goulenok, Cyril, Thieulot-Rolin, Nathalie, Messika, Jonathan, Lamhaut, Lionel, Charron, Cyril, Dempsey, Ged, Mathew, Shiju J., Raj, Ashok S., Grecu, Irina, Cupitt, Jason, Lawton, Tom, Clark, Richard, Popescu, Monica, Spittle, Nick, Faulkner, Maria, Cowton, Amanda, Elloway, Esme, Williams, Patricia, Reay, Michael, Chukkambotla, Srikanth, Kumar, Ravi, Al-Subaie, Nawaf, Kent, Linda, Tamm, Tiina, Kajtor, Istvan, Burns, Karen, Pugh, Richard, Ostermann, Marlie, Kam, Elisa, Bowyer, Helen, Smith, Neil, Templeton, Maie, Henning, Jeremy, Goffin, Kelly, Kapoor, Ritoo, Laha, Shondipon, Chilton, Phil, Khaliq, Waqa, Crayford, Alison, Coetzee, Samantha, Tait, Moira, Boultoukas, Evangelo, Stoker, Wendy, Gimenez, Marc, Pope, Alan, Camsooksai, Julie, Pogson, David, Quigley, Kate, Ritzema, Jenny, Hormis, Anil, Boulanger, Carole, Balasubramaniam, M., Vamplew, Luke, Burt, Karen, Martin, Daniel, Craig, Jayne, Prowle, John, Doyle, Nanci, Shelton, Jonathon, Scott, Carmen, Donnison, Phil, Shelton, Sarah, Frey, Christian, Ryan, Christine, Spray, Dominic, Barnes, Veronica, Barnes, Kerry, Furneval, Julie, Ridgway, Stephanie, Saha, Rajnish, Clark, Thoma, Wood, Jame, Bolger, Clare, Bassford, Christopher, Lewandowski, john, Zhao, Xiaobei, Humphreys, Sally, Dowling, Susan, Richardson, Neil, Burtenshaw, Andrew, Stevenson, Carl, Wilcock, Danielle, Aidoni, Zoi, Aloizos, Stavro, Tasioudis, Polychroni, Lampiri, Kleri, Zisopoulou, Vasiliki, Ifigenia, Ravani, Eymorfia, Pagaki, Angela, Anttoniou, Katsoulas, Theodoros A., Kyparissi, Aikaterini, Aikaterini, Kounougeri, Marinakis, George, Tsimpoukas, Fotio, Spyropoulou, Anastasia, Zygoulis, Pari, Hayes, Ivan, Kelly, Yvelynne, Westbrook, Andrew, Fitzpatrick, Gerry, Maheshwari, Darshana, Motherway, Catherine, Gupta, Manish, Gurjar, Mohan, Maji, Ismail M, Negri, Giovanni, Spadaro, Savino, Nattino, Giuseppe, Pedeferri, Matteo, Boscolo, Annalisa, Rossi, Simona, Rossi, Maurizio, Calicchio, Giuseppe, Cubattoli, Lucia, Di Lascio, Gabriella, Barbagallo, Maria, Berruto, Francesco, Codazzi, Daniela, Bottazzi, Andrea, Fumagalli, Paolo, Negro, Giancarlo, Lupi, Giuseppe, Savelli, Flavia, Vulcano, Giuseppe A., Fumagalli, Roberto, Marudi, Andrea, Lefons, Ugo, Lembo, Rita, Babini, Maria, Paggioro, Alessandra, Parrini, Vieri, Zaccaria, Maria, Clementi, Stefano, Gigliuto, Carmelo, Facondini, Francesca, Pastorini, Simonetta, Munaron, Susanna, Calamai, Italo, Bocchi, Anna, Brizio, Elisabetta, Adorni, Adele, Bocci, Maria Grazia, Cortegiani, Andrea, Casalicchio, Tiziana, Mellea, Serena, Graziani, Elia, Barattini, Massimo, van Dijk, I., van Lelyveld-Haas, L.E.M., Ramnarain, D., Jansen, Tim, Nooteboom, Fleur, van der Voort, Peter H.J., Dieperink, Willem, de Waard, Monique C., Bormans, Laura, Hahn, Michael, Kemmerer, Nicolai, Strietzel, Hans Frank, Fehrle, Lutz, Dybwik, Knut, Legernaes, Terje, Klepstad, Pål, Olaussen, Even Braut, Olsen, Knut Inge, Børresen, Ole Mariu, Bjørsvik, Geir, Maini, Sameer, Czuczwar, Miroslaw, Krawczyk, Pawel, Ziętkiewicz, Mirosław, Nowak, Łukasz R., Kotfis, Katarzyna, Cwyl, Katarzyna, Gajdosz, Ryszard, Biernawska, Jowita, Grudzień, Paweł, Nasiłowski, Paweł, Popek, Natalia, Cyrankiewicz, Waldemar, Wnuk, Marek, Maciejewski, Dariusz, Studzińska, Dorota, Zukowski, Maciej, Bernas, Szymon, Serwa, Marta, Stefaniak, Jan, Pawel, Maciejewski, Szymkowiak, Malgorzata, Adamik, Barbara, Catorze, Nuno, Castelo Branco, Miguel, Barros, Inê, Barros, Nelson, Krystopchuk, Andriy, Honrado, Teresa, Sousa, Cristina, Munoz, Francisco, Rebelo, Marta, Gomes, Rui, Nunes, Jorge, Dias, Celeste, Fernandes, Ana Margarida, Petrisor, Cristina, Constantin, Bodolea, Belskiy, Vladislav, Boskholov, Bori, Kawati, Rafael, Sivik, Joakim, Nauska, Jessica, Smole, Daniel, Parenmark, Fredric, Lyrén, Johanna, Rockstroh, Katalin, Rydén, Sara, Spångfors, Martin, Strinnholm, Morten, Walther, Sten, De Geer, Lina, Nordlund, Peter, Pålsson, Staffan, Zetterquist, Harald, Nilsson, Annika, Thiringer, Karin, Jungner, Mårten, Bark, Björn, Nordling, Berit, Sköld, Han, Brorsson, Camilla, Persson, Stefan, Bergström, Anna, Berkius, Johan, Holmström, Johanna, and Yapici, Nihan
Subjects: Male, Time Factors, Outcome Assessment, Frail Elderly/statistics & numerical data, [SDV]Life Sciences [q-bio], HSJ UCI, Passive, Critical Care and Intensive Care Medicine, Frailty/classification/diagnosis/mortality/therapy, Severity of Illness Index, Severity of illne, Elderly, 0302 clinical medicine, Quality of life, Frailty, ICU, Mortality, Octogenarians, Severity of illness, Aged, 80 and over, Critical Illness, Europe, Euthanasia, Passive, Female, Frail Elderly, Geriatric Assessment, Humans, Intensive Care Units, Length of Stay, Outcome Assessment, Health Care, Proportional Hazards Models, Prospective Studies, Quality of Life, Hospital Mortality, 80 and over, 030212 general & internal medicine, Prospective cohort study, education.field_of_study, ddc:617, Mortality rate, [SDV] Life Sciences [q-bio], Length of Stay/statistics & numerical data, Cohort, Intensive Care Units/statistics & numerical data, Critical Illne, SOFA score, Human, medicine.medical_specialty, Time Factor, Intensive Care Unit, Population, INTENSIVE-CARE, Europe/epidemiology, Outcome Assessment (Health Care), 03 medical and health sciences, Octogenarian, Intensive care, Journal Article, medicine, COHORT, Octogenarinans, Intensive care medicine, education, Aged, OLDER, Euthanasia, business.industry, 030208 emergency & critical care medicine, Health Care, Prospective Studie, Critical Illness/mortality, UNIT, Emergency medicine, Proportional Hazards Model, business
Abstract: Purpose: Very old critical ill patients are a rapid expanding group in the ICU. Indications for admission, triage criteria and level of care are frequently discussed for such patients. However, most relevant outcome studies in this group frequently find an increased mortality and a reduced quality of life in survivors. The main objective was to study the impact of frailty compared with other variables with regards to short-term outcome in the very old ICU population. Methods: A transnational prospective cohort study from October 2016 to May 2017 with 30days follow-up was set up by the European Society of Intensive Care Medicine. In total 311 ICUs from 21 European countries participated. The ICUs included the first consecutive 20 very old (≥80years) patients admitted to the ICU within a 3-month inclusion period. Frailty, SOFA score and therapeutic procedures were registered, in addition to limitations of care. For measurement of frailty the Clinical Frailty Scale was used at ICU admission. The main outcomes were ICU and 30-day mortality and survival at 30days. Results: A total of 5021 patients with a median age of 84years (IQR 81–86years) were included in the final analysis, 2404 (47.9%) were women. Admission was classified as acute in 4215 (83.9%) of the patients. Overall ICU and 30-day mortality rates were 22.1% and 32.6%. During ICU stay 23.8% of the patients did not receive specific ICU procedures: ventilation, vasoactive drugs or renal replacement therapy. Frailty (values ≥5) was found in 43.1% and was independently related to 30-day survival (HR 1.54; 95% CI 1.38–1.73) for frail versus non-frail. Conclusions: Among very old patients (≥80years) admitted to the ICU, the consecutive classes in Clinical Frailty Scale were inversely associated with short-term survival. The scale had a very low number of missing data. These findings provide support to add frailty to the clinical assessment in this patient group. Trial registration: ClinicalTrials.gov (ID: NCT03134807).
Published: 2017
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13. Empirisk analyse av finansielle nøkkeltall for de største selskapene i Eurosonen

Author: Vigdal-Olsen, Knut and Skarpnord Ødegård, Dani
Subjects: eurosonen, European Central Bank, VDP::Samfunnsvitenskap: 200::Økonomi: 210::Samfunnsøkonomi: 212, kvantitativ metode, Quantitative Method, Euro zone, den europeiske sentralbanken
Abstract: Spesialisering økonomistyring Som følge av fallende inflasjon og gjeldsoppbygging i Europa implementerte Den Europeiske Sentralbanken kvantitative lettelser i mellomrommet 2015 til 2018. Bakgrunnen for dette ukonvensjonelle tiltaket var å gi økt likviditet i kredittmarkedet og styrke økonomien i Eurosonen, i en situasjon hvor det Den Europeiske Sentralbanken allerede hadde brukt opp sitt vanligste virkemiddel gjennom justering av styringsrenten til under null. Kvantitative lettelser ble utført gjennom kjøp av aktiva i markedet, da primært av statsobligasjoner, og bidro til å tvinge markedsrenten enda lavere enn en videre justering av styringsrenten hadde medført. Derpå ble både yield/avkastningskrav ved obligasjoner og rentekostnader redusert for selskaper og husholdninger. I oppgaven er det utført en empirisk analyse med bruk av finansielle data fra selskaper med tilhørighet til børsindeksen Euro STOXX 50 og en kontrollgruppe med selskaper utenfor Eurosonen for å besvare forskningsspørsmålene. Euro STOXX 50 består av de største børsnoterte selskapene i Eurosonen, og representerer derfor også en stor del av økonomien i Eurosonen. I regresjonsanalysen har vi målt finansielle nøkkeltall gjennom én regnskapsbasert indikator ved Return On Assets (ROA) og én markedsbasert indikator ved Price to Book (P/B). Disse to avhengige variablene presenterer både et perspektiv av historiske nøkkeltall (ROA) og et perspektiv av fremtidig nøkkeltall (P/B). Resultatene fra analysen indikerte at: (1) Det ikke finnes grunnlag for at økte kvantitative lettelser gir bedre historiske regnskapstall (ROA) for selskaper i Eurosonen. I kontrast fant vi derimot at ved økte kvantitative lettelser, ble verdien av ROA svekket. (2) Det var en positiv korrelasjon mellom økte kvantitative lettelser og fremtidige markedsbaserte nøkkeltall (P/B). (3) Ved økt verdi av kvantitative lettelser, økte både historiske regnskapstall og de fremtidige markedstallene for selskaper utenfor Eurosonen (kontrollgruppen). Dette til tross for at kontrollgruppen ikke er tilknyttet Den Europeiske Sentralbanken. Abstract Due to declining inflation and buildup of debt in the Eurozone, the European Central Bank implemented quantitative easing in the time period from 2015 to 2018. The intention for the unconventional measure was to provide increased liquidity in the credit market and strengthen the economy of the Eurozone, in a situation where the European Central Bank had already conducted its most common measure through altering the fund rate to below zero. The quantitative easing program was executed through purchase of assets in the market, primarily through government bonds, and helped pushing the interest rate further below. Accordingly, both bond yields and interest costs were reduced for companies and households. In order to answer the research questions, an empirical analysis of financial data belonging to companies in the Euro STOXX 50 and a control group with companies outside the Eurozone was conducted. The Euro STOXX 50 consists of the largest listed companies in the Eurozone, and therefore represents a large part of the economy in the Eurozone. In the regression analysis, we measured financial key figures through one accounting-based indicator by Return On Assets (ROA) and one market-based indicator by Price to Book (P/B). These two dependent variables present both a perspective of historical key figures (ROA) and a perspective of future key figures (P/B). The results of the analysis indicated that: (1) There is no evidence to support that increased quantitative easing will provide better historical accounting figures (ROAs) for companies in the Eurozone. In contrast, we found that by increasing quantitative easing, the value of ROA was weakened. (2) There was a positive correlation between increased quantitative easing and future key figures (P/B). (3) With increased value of quantitative easing, both historical accounting figures and future market figures for companies outside the Eurozone (control group) increased. This despite that the control group is not affiliated with the European Central Bank
Published: 2020

14. The Magellanic Clouds with LSST

Author: Olsen, Knut
Abstract: The Large Synoptic Survey Telescope (LSST) will provide a massive optical imaging dataset covering roughly half the sky with over ten years of repeated observation in ugrizY. The telescope is under construction, with the survey scheduled to enter full operations in 2023. LSST has a unique role to play in surveys of the Clouds. First, its large AΩ can probe the thousands of square degrees that comprise the extended periphery of the Magellanic Clouds with unprecedented completeness and depth, allowing us to detect and map their extended disks, stellar halos, and debris from interactions with high fidelity. Second,its ability to map the entire main bodies in only a few pointings can allow us to identify and classify their extensive variable source populations with high time and areal coverage, discovering, for example, extragalactic planets, rare variables and transients, and light echoes from explosive events that occurred thousands of years ago. I will describe the science case for observing the Magellanic Clouds with LSST and the proposed adjustments to the LSST survey footprint and observing cadence that will be needed to ensure that LSST Magellanic Clouds science may be achieved.
Published: 2019
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15. A Science Platform Network to Facilitate Astrophysics in the 2020s

Author: Desai, Vandana, Allen, Mark, Arviset, Christophe, Berriman, Bruce, Chary, Ranga-Ram, Cook, David, Faisst, Andreas, Dubois-Felsmann, Gregory, Groom, Steve, Guy, Leanne, Helou, George, Imel, David, Juneau, Stéphanie, Lacy, Mark, Lemson, Gerard, Major, Brian, Mazzarella, Joe, Mcglynn, Thomas, Momcheva, Ivelina, Murphy, Eric, Olsen, Knut, Peek, Josh, Pope, Alexandra, Shupe, David, Smale, Alan, Smith, Arfon, Stickley, Nathaniel, Teplitz, Harry, Thakar, Ani, Wu, Xiuqin, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Space Astronomy Centre (ESAC), European Space Agency (ESA), California Institute of Technology (CALTECH), Remote Sensing Group, Plymouth Marine Laboratory, Caltech Department of Astronomy [Pasadena], Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS), Adler Planetarium [Chicago], Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), and Agence Spatiale Européenne = European Space Agency (ESA)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; We advocate for the adequate funding of data centers to develop and operate “science platforms”, which will provide storage and computing resources for the astronomical community to run analyses near the data. Furthermore, these platforms should be connected to enable cross-center analysis and processing.
Published: 2019

16. The Data Lab: A Science Platform for the analysis of ground-based astronomical survey data

Author: Olsen, Knut, Bolton, Adam, Juneau, Stephanie, Nikutta, Robert, Norman, Dara, Nidever, David, Ridgway, Stephen, Scott, Adam, and Weaver, Benjamin
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The next decade will feature a growing number of massive ground-based photometric, spectroscopic, and time-domain surveys, including those produced by DECam, DESI, and LSST. The NOAO Data Lab was launched in 2017 to enable efficient exploration and analysis of large surveys, with particular focus on the petabyte-scale holdings of the NOAO Archive and their associated catalogs. The Data Lab mission and future development align well with two of the NSF's Big Ideas, namely Harnessing Data for 21st Century Science and Engineering and as part of a network to contribute to Windows on the Universe: The Era of Multi-messenger Astrophysics. Along with other Science Platforms, the Data Lab will play a key role in scientific discoveries from surveys in the next decade, and will be crucial to maintaining a level playing field as datasets grow in size and complexity., 10 pages, 4 figures, Astro2020 Activities, Projects, or State of the Profession Consideration White Paper
Published: 2019

17. What Multi-band Temporal Photometry of RR Lyrae stars can tell us about the Galactic Bulge

Author: Saha, Abhijit, Vivas, K., Olszewski, E., and Olsen, Knut
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Minimum light colors of RR Lyrae stars (which are both standard color markers as well as standard candles) measured with the DECam imager on the Blanco 4m telescope at CTIO in select fields in the Galactic bulge are used to independently derive the extinction law in these visible passbands. Variations in the color-color diagrams on sub-arc-minute scales allow the construction of reddening maps that can be anchored to the RR Lyrae color scale, yielding reddening and extinction corrected color-magnitude diagrams of unprecedented clarity that reveal interesting features and characteristics of stellar populations in the bulge, including a very blue horizontal branch and surprisingly young stars with super-solar abundance. The extinction corrected RR Lyrae stars also trace the density distribution of the ancient stars, and structure in the reddening maps show remnants from the past.
Published: 2019
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18. Astro2020 Science White Paper: Science Platforms for Resolved Stellar Populations in the Next Decade

Author: Olsen, Knut A. G., Graham, Melissa, Norman, Dara, Juneau, Stephanie, and Bolton, Adam
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: Over the past decade, research in resolved stellar populations has made great strides in exploring the nature of dark matter, in unraveling the star formation, chemical enrichment, and dynamical histories of the Milky Way and nearby galaxies, and in probing fundamental physics from general relativity to the structure of stars. Large surveys have been particularly important to the biggest of these discoveries. In the coming decade, current and planned surveys will push these research areas still further through a large variety of discovery spaces, giving us unprecedented views into the low surface brightness Universe, the high surface brightness Universe, the 3D motions of stars, the time domain, and the chemical abundances of stellar populations. These discovery spaces will be opened by a diverse range of facilities, including the continuing Gaia mission, imaging machines like LSST and WFIRST, massively multiplexed spectroscopic platforms like DESI, Subaru-PFS, and MSE, and telescopes with high sensitivity and spatial resolution like JWST, the ELTs, and LUVOIR. We do not know which of these facilities will prove most critical for resolved stellar populations research in the next decade. We can predict, however, that their chance of success will be maximized by granting use of the data to broad communities, that many scientific discoveries will draw on a combination of data from them, and that advances in computing will enable increasingly sophisticated analyses of the large and complex datasets that they will produce. We recommend that Astro2020 1) acknowledge the critical role that data archives will play for stellar populations and other science in the next decade, 2) recognize the opportunity that advances in computing will bring for survey data analysis, and 3) consider investments in Science Platform technology to bring these opportunities to fruition., Comment: 7 pages, 1 figure, Astro2020 Science White Paper
Published: 2019
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19. On the nature of a shell of young stars in the outskirts of the Small Magellanic Cloud

Author: Martinez-Delgado, David, Vivas, A. Katherina, Grebel, Eva K., Gallart, Carme, Pieres, Adriano, Bell, Cameron P. M., Zivick, Paul, Lemasle, Bertrand, Johnson, L. Clifton, Carballo-Bello, Julio A., Noel, Noelia E. D., Cioni, Maria-Rosa L., Choi, Yumi, Besla, Gurtina, Schmidt, Judy, Zaritsky, Dennis, Gruendl, Robert A., Seibert, Mark, Nidever, David, Monteagudo, Laura, Monelli, Mateo, Hubl, Bernhard, van der Marel, Roeland, Ballesteros, Fernando J., Stringfellow, Guy, Walker, Alistair, Blum, Robert, Bell, Eric F., Conn, Blair C., Olsen, Knut, Martin, Nicolas, Chu, You-Hua, Inno, Laura, Boer, Thomas J. L., Kallivayalil, Nitya, De Leo, Michele, Beletsky, Yuri, Munoz, Ricardo R., Martínez-Delgado, David, Katherina Vivas, Anna, Grebel, Eva, Bell, Cameron, Clifton Johnson, Lent, Carballo-Bello, Julio, Noël, Noelia, Cioni, Maria-Rosa, Gruendl, Robert, Ballesteros, Fernando, Bell, Eric, Conn, Blair, Boer, Thomas, Neyer, Fabian, Muñoz, Ricardo, Instituto de Astrofisica de Canarias (IAC), University of Arizona, California Institute of Technology (CALTECH), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Brown Bear Foundation
Subjects: Milky Way, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, Large Magellanic Cloud, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Local Group, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Stars, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Globular cluster, Astrophysics of Galaxies (astro-ph.GA), Small Magellanic Cloud, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Understanding the evolutionary history of the Magellanic Clouds requires an in-depth exploration and characterization of the stellar content in their outer regions, which ultimately are key to tracing the epochs and nature of past interactions. We present new deep images of a shell-like over-density of stars in the outskirts of the Small Magellanic Cloud (SMC). The shell, also detected in photographic plates dating back to the fifties, is located at ~1.9 degr from the center of the SMC in the north-east direction.The structure and stellar content of this feature were studied with multi-band, optical data from the Survey of the MAgellanic Stellar History (SMASH) carried out with the Dark Energy Camera on the Blanco Telescope at Cerro Tololo Inter-American Observatory. We also investigate the kinematic of the stars in the shell using the Gaia Data Release 2. The shell is composed of a young population with an age ~ 150 Myr, with no contribution from an old population. Thus, it is hard to explain its origin as the remnant of a tidally disrupted stellar system. The spatial distribution of the young main-sequence stars shows a rich sub-structure, with a spiral arm-like feature emanating from the main shell and a separated small arc of young stars close to the globular cluster NGC 362. We find that the absolute g-band magnitude of the shell is M_{g,shell} = -10.78+/- 0.02, with a surface brightness of mu_{g,shell} = 25.81+/- 0.01 mag/arcsec^{2}. We have not found any evidence that this feature is of tidal origin or a bright part of a spiral arm-like structure. Instead, we suggest that the shell formed in a recent star formation event, likely triggered by an interaction with the Large Magellanic Cloud and/or the Milky Way, ~150 Myr ago., Comment: 16 pages, 14 figures, submitted to Astronomy & Astrophysics
Published: 2019
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20. Lærere i kombinasjonsstillinger - praksisnær teori og teorinær praksis?

Author: Olsen, Knut-Rune and Lie, Anne Liv Kaarstad
Subjects: Samfunnsvitenskap: 200::Pedagogiske fag: 280 [VDP], lærere, kombinasjonsstillinger
Abstract: Høsten 2018 ble det innledet et forsøk med å opprette stillinger for lærere i kombinasjonsstillinger knyttet til grunnskolelærerutdanningen ved Universitetet i Sørøst-Norge (USN). De som ble tilsatt, arbeider til daglig i grunnskolen og har i de fleste tilfellene erfaring som praksislærere. Prosjektet er ett av flere tiltak som er knyttet til en utviklingsavtale mellom USN og Kunnskapsdepartementet, som har som formål å videreutvikle og styrke samarbeidet mellom universitetet og praksisfeltet innenfor universitetets profesjonsutdanninger. For å koordinere og lede dette arbeidet ble det opprettet en prosjektorganisasjon kalt USN Profesjon. USN Profesjon ledes av Kristin Barstad, og ordningen med kombinasjonsstillinger er ett av fire hovedsatsingsområder som omfatter både lærerutdanningene og helse- og sosialfagutdanningene ved USN. Denne rapporten tar for seg ordningen med kombinasjonsstillinger slik den har blitt gjennomført i den femårige grunnskolelærerutdanningen ved USN. Arbeidet er gjennomført i samråd med Arild Hovland, som er dekan ved Fakultet for humaniora, idrett og lærerutdanning, og Anne Fængsrud, som er visedekan for lærerutdanningen. Det empiriske grunnlaget for rapporten består i hovedsak av fokusgruppeintervjuer med lærere som er tilsatt i kombinasjonsstillinger ved hvert de fire studiestedene ved USN som tilbyr grunnskolelærerutdanning, og programkoordinatorene ved de aktuelle studiestedene. Vi retter en stor takk til alle de som på ulike måter har gjort arbeidet med denne rapporten mulig, og håper den vil stimulere til videre drøfting og kvalitetsutvikling av den femårige grunnskolelærerutdanningen ved USN.
Published: 2019

21. A Big Sky Approach to Cadence Diplomacy

Author: Olsen, Knut, Di Criscienzo, Marcella, Jones, R. Lynne, Schwamb, Megan E., Lin, Hsing Wen \\'Edward\\', Awan, Humna, Marshall, Phil, Gawiser, Eric, Bolton, Adam, and Eisenstein, Daniel
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The LSST survey was designed to deliver transformative results for four primary objectives: constraining dark energy and dark matter, taking an inventory of the Solar System, exploring the transient optical sky, and mapping the Milky Way. While the LSST Wide-Fast-Deep survey and accompanying Deep Drilling and mini-surveys will be ground-breaking for each of these areas, there remain competing demands on the survey area, depth, and temporal coverage amid a desire to maximize all three. In this white paper, we seek to address a principal source of tension between the different LSST science collaborations, that of the survey area and depth that they each need in the parts of the sky that they care about. We present simple tools which can be used to explore trades between the area surveyed by LSST and the number of visits available per field and then use these tools to propose a change to the baseline survey strategy. Specifically, we propose to reconfigure the WFD footprint to consist of low-extinction regions (limited by galactic latitude), with the number of visits per field in WFD limited by the LSST Science Requirements Document (SRD) design goal, and suggest assignment of the remaining LSST visits to the full visible LSST sky. This proposal addresses concerns with the WFD footprint raised by the DESC (as 25 percent of the current baseline WFD region is not usable for dark energy science due to MW dust extinction), eases the time required for the NES and SCP mini-surveys (since in our proposal they would partially fall into the modified WFD footprint), raises the number of visits previously assigned to the GP region, and increases the overlap with DESI and other Northern hemisphere follow-up facilities. This proposal alleviates many of the current concerns of Science Collaborations that represent the four scientific pillars of LSST and provides a Big Sky approach to cadence diplomacy., 12 page, 5 figures, submitted to Call for White Papers on LSST Cadence Optimization
Published: 2018

22. Mapping the Periphery and Variability of the Magellanic Clouds

Author: Olsen, Knut, Szkody, Paula, Cioni, Maria-Rosa, Di Criscienzo, Marcella, Musella, Ilaria, Ripepi, Vincenzo, Borsa, Francesco, Marconi, Marcella, Girardi, Leo, Pastorelli, Giada, Trabucchi, Michele, Ventura, Paolo, and Moniez, Marc
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: We propose a combination of a modified Wide-Fast-Deep survey, a mini-survey of the South Celestial Pole, and a Deep Drilling-style survey to produce a 3-D map of the Magellanic System and to provide a detailed census of the transient and variable populations in the Clouds. We support modifying the Wide-Fast-Deep survey to cover the declination range $-72.25\deg15\deg$, as proposed in a separate white paper. We additionally propose a mini-survey covering the 950$\deg^2$ with ${\rm Dec} < -72.25$ in $ugriz$ to the standard LSST single-exposure depth and with 40 visits per filter per field. Finally, we propose a mini-survey covering $\sim100 \deg^2$ of the main bodies of the Clouds with twelve total pointings, 2000 total visits per field, and shorter exposure time., Comment: 11 pages, 3 figures, submitted to Call for White Papers on LSST Cadence Optimization
Published: 2018
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23. 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

24. Datasphere 2023

Author: Bolton, Adam, Ciardi, David, and Olsen, Knut
Subjects: Big Data, LSST
Abstract: Driving the development priorities for interaction withnext generation surveys.
Published: 2016
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25. Identification of a Class of Low-Mass AGB Stars Struggling to Become Carbon Stars in the Magellanic Clouds

Author: Boyer, Martha L., Mcdonald, Iain, Srinivasan, Sundar, Zijlstra, Albert, Olsen, Knut, and {Sonneborn}, George
Subjects: variables: general [stars], Magellanic Clouds, Astrophysics::Solar and Stellar Astrophysics, low-mass [stars], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Physics and Astronomy(all), winds, outflows [stars], AGB and post-AGB [stars], Astrophysics::Galaxy Astrophysics, stars – [infrared]
Abstract: We have identified a new class of Asymptotic Giant Branch (AGB) stars in the Small and Large Magellanic Clouds (SMC/LMC) using optical to infrared photometry, light curves, and optical spectroscopy. The strong dust production and long-period pulsations of these stars indicate that they are at the very end of their AGB evolution. Period-mass-radius relations for the fundamental-mode pulsators give median current stellar masses of 1.14 solar masses in the LMC and 0.94 solar masses in the SMC (with dispersions of 0.21 and 0.18 solar masses, respectively), and models suggest initial masses of
Published: 2015
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26. Photometric Evidence of an Intermediate-age Stellar Population in the Inner Bulge of M31

Author: Dong, Hui, Li, Zhiyuan, Wang, Q. Daniel, Lauer, Tod R., Olsen, Knut A. G., Saha, Abhijit, Dalcanton, Julianne J., and Williams, Benjamin F.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: We explore the assembly history of the M31 bulge within a projected major-axis radius of 180" (~680 pc) by studying its stellar populations in Hubble Space Telescope WFC3 and ACS observations. Colors formed by comparing near-ultraviolet vs. optical bands are found to become bluer with increasing major-axis radius, which is opposite to that predicted if the sole sources of near-ultraviolet light were old extreme horizontal branch stars with a negative radial gradient in metallicity. Spectral energy distribution fits require a metal-rich intermediate-age stellar population (300 Myr to 1 Gyr old, ~solar metallicity) in addition to the dominant old population. The radial gradients in age and metallicity of the old stellar population are consistent with those in previous works. For the intermediate-age population, we find an increase in age with radius and a mass fraction that increases up to 2% at 680 pc away from the center. We exclude contamination from the M31 disk and/or halo as the main origin for this population. Our results thus suggest that intermediate-age stars exist beyond the central 5" (19 pc) of M31 and contribute ~1% of the total stellar mass in the bulge. These stars could be related to the secular growth of the M31 bulge., Accepted for publication in MNRAS, 33 pages, 10 figures
Published: 2015

27. Spectroscopy in the Era of LSST

Author: Matheson, Thomas, Fan, Xiaohui, Green, Richard, McConnachie, Alan, Newman, Jeff, Olsen, Knut, Szkody, Paula, and Wood-Vasey, W. Michael
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This report summarizes the results of the 'Spectroscopy in the Era of LSST' workshop held April 11-12, 2013 in Tucson, Arizona. At the workshop, there were breakout sessions covering four broad science topics. These were: time domain science, Galactic structure and stellar populations, galaxies and AGN, and dark energy and cosmology. We present the science cases discussed in these breakout sessions and provide a synthesis of highly desired capabilities that meet needs across all four broad topics. We also present a table that will be useful to characterize the needs of specific science cases in a format that provides a general framework for discussion of future spectroscopic capabilities., 24 pages, 1 table. More information at this URL: http://www.noao.edu/meetings/lsst-spec/
Published: 2013

28. Addressing Decadal Survey Science through Community Access to Highly Multiplexed Spectroscopy with BigBOSS on the KPNO Mayall Telescope

Author: Pilachowski, Caty, Badenes, Carles, Bailey, Stephen, Barth, Aaron, Beaton, Rachel, Bell, Eric, Bernstein, Rebecca, Bian, Fuyan, Blanton, Michael, Blum, Robert, Bolton, Adam, Bond, Howard, Brodwin, Mark, Bullock, James, Carlin, Jeff, Chary, Ranga-Ram, Cinabro, David, Cooper, Michael, Cota, Jorge L. C., Davis, Marc, Dawson, Kyle, Dey, Arjun, Donahue, Megan, Drake, Jeremy, Ellingson, Erica, Faccioli, Lorenzo, Fan, Xiaohui, Ferguson, Harry, Gawiser, Eric, Geha, Marla, Giavalisco, Mauro, Gonzalez, Anthony, Griest, Kim, Grossan, Bruce, Guhathakurta, Raja, Harding, Paul, Heap, Sara R., Ho, Shirley, Howell, Steve, Jannuzi, Buell, Kalirai, Jason, Keeney, Brian, Kewley, Lisa, Kong, Xu, Lampton, Michael, Lin, Wei-Peng, La Macorra, Axel, Macri, Lucas, Majewski, Steve, Martini, Paul, Massey, Phil, Mcswain, Virginia, Miller, Adam A., Minniti, Dante, Modjaz, Maryam, Morrison, Heather, John Moustakas, Myers, Adam, Najita, Joan, Newman, Jeffrey, Norman, Dara, Olsen, Knut, Pierce, Michael, Pope, Alexandra, Prescott, Moire, Reddy, Naveen, Reil, Kevin, Rest, Armin, Rhode, Katherine, Rockosi, Connie, Rudnick, Greg, Saha, Abhijit, Salzer, John, Sanders, David, Schlegel, David, Sesar, Branimir, Shields, Joseph, Silverman, Jeffrey, Simon, Josh, Stanford, Adam, Stern, Daniel, Storrie-Lombardi, Lisa, Suntzeff, Nicholas, Surace, Jason, Szalay, Alex, Ulmer, Melville, Weiner, Ben, Willman, Beth, Windhorst, Rogier, and Wood-Vasey, Michael
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This document summarizes the results of a community-based discussion of the potential science impact of the Mayall+BigBOSS highly multiplexed multi-object spectroscopic capability. The KPNO Mayall 4m telescope equipped with the DOE- and internationally-funded BigBOSS spectrograph offers one of the most cost-efficient ways of accomplishing many of the pressing scientific goals identified for this decade by the "New Worlds, New Horizons" report. The BigBOSS Key Project will place unprecedented constraints on cosmological parameters related to the expansion history of the universe. With the addition of an open (publicly funded) community access component, the scientific impact of BigBOSS can be extended to many important astrophysical questions related to the origin and evolution of galaxies, stars, and the IGM. Massive spectroscopy is the critical missing ingredient in numerous ongoing and planned ground- and space-based surveys, and BigBOSS is unique in its ability to provide this to the US community. BigBOSS data from community-led projects will play a vital role in the education and training of students and in maintaining US leadership in these fields of astrophysics. We urge the NSF-AST division to support community science with the BigBOSS multi-object spectrograph through the period of the BigBOSS survey in order to ensure public access to the extraordinary spectroscopic capability., Comment: 5 pages; this white paper was produced as input to the NSF-AST portfolio review
Published: 2012
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29. Surveying the Agents of Galaxy Evolution in the Tidally-Stripped, Low Metallicity Small Magellanic Cloud (SAGE-SMC). I. Overview

Author: Gordon, Karl D., Meixner, Margaret, Meade, Marilyn, Whitney, Barbara A., Engelbracht, Charles W., Bot, Caroline, Boyer, Martha L, Lawton, Brandon, Sewilo, Marta, Babler, Mr. Brian L., Bernard, Jean-Philippe, Bracker, Steve, Block, Miwa, Blum, Robert D., Bolatto, Alberto D., Bonanos, Alceste Zoe, Harris, Jason, Hora, Joseph L., Indebetouw, Remy, Misselt, Karl A., Reach, William T., Shiao, B., Tielens, Alexander, Carlson, Lynn Redding, Churchwell, Edward B., Clayton, Geoff C., Chen, C-H Rosie, Cohen, Martin, Fukui, J. Lewis, Gorjian, Varoujan, Hony, Sacha, Israel, Frank, Kemper, F., Leroy, Adam K., Li, Aigen, Madden, Suzanne C., Marble, Andrew R., McDonald, Iain, Muller, EriK, Oliveira, Joana M., Olsen, Knut A. G., Paladini, Roberta, Paradis, Deborah, Points, Sean, Robitaille, Thomas, Rubin, Douglas, Sandstrom, Karin, Simon, Joshua D., Smith, Linda J, Srinivasan, Sundar, Vijh, Uma P., Van, Dyk Schuyler D., van, Loon Jacobus Theodorus, Zaritsky, Dennis F., Kawamura, Akiko, Mizuno, Akira, Mizuno, Norikazu, Onishi, T., Sato, S., and Shibai, Hiroshi
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Star formation, Metallicity, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Interstellar medium, Spitzer Space Telescope, Space and Planetary Science, Spectral energy distribution, Astrophysics::Solar and Stellar Astrophysics, Small Magellanic Cloud, Astrophysics::Earth and Planetary Astrophysics, Large Magellanic Cloud, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 著者人数: 60名, Accepted: 2011-07-17, 資料番号: SA1003632000
Published: 2011
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30. Boevne: En kartlegging av ulike klientkategoriers evne til å nyttiggjøre seg tilbudet om kommunal bolig

Author: Olsen, Knut Harald
Subjects: boevne, sosialt arbeid, Social science: 200::Social work: 360 [VDP]
Abstract: Master's thesis in Social work Denne masteroppgaven inngår som hoveddel i gjennomføringen av masterstudiet i sosialt arbeid ved Universitetet i Stavanger. Det bærende element i masteroppgaven er undersøkelsen av boevne. Gjennomføringen av undersøkelsen står i denne sammenheng sentralt. Undersøkelsen er utført gjennom bruk av spørreskjema som er distribuert til informanter som både har erfaring og kunnskap om ulike sider ved både bostedsløshet, boevne og problematisk boadferd. Boevne er i denne besvarelsen knyttet opp mot 7 ulike klientkategorier som har utgjort bærebjelken og nærmest fungert som en rød tråd i gjennomføringen av oppgaven. De 7 klientkategoriene er: - A: Ikke-etniske nordmenn - B: Personer med psykiske problemer - C: Personer med et rus- og psykiatriproblem - D: Personer med et rusproblem - E: Eldre personer (pensjonister) - F: Aleneforsørgere - G: Ordinære familier Definisjon og valg av klientkategorier kan virke både kontroversiell og stigmatiserende, men er ut i fra en vurdering av realitetene den mest dekkende innfallsvinkelen for å analysere variasjonen i hvem som rammes av bostedsløshet for deretter å bli hjulpet inn i et egnet, kommunalt boforhold. Utviklingen av boforholdet kommer til syne gjennom klientens boevne. Den er igjen et resultat av klientens evne til å forholde seg til sitt indre og ytre bomiljø. Konkret vil det si hvordan han på den ene siden opprettholder en ansvarsbevisst holdning til å ta vare på leiligheten sin og på den annen side hvordan han forholder seg til omgivelsene og det ytre miljø. Særlig står forholdet til naboer og klientens sosialiseringsevner her sentralt. Denne boevnen kan med andre ord gi seg utslag både på positivt og negativt vis. Når boevnen svikter – det være seg i forhold til både det indre som ytre bomiljø – beveger vi oss inn i det feltet som heter problematisk boadferd. 10 Oppgavebesvarelsen tar for seg dette temaet ved å se på årsaker, konsekvenser og løsninger. Tema og problemstilling tar sitt utgangspunkt i bostedsløse sosialklienters holdninger og adferd når de har blitt tildelt og er etablert i et kommunalt boforhold. Undersøkelsen viser hvordan disse holdningene og denne adferden gjør seg gjeldende blant de syv klientkategoriene. Oppgaven består av følgende elementer: A. Oppgavens tema omhandler boevne i kommunale boforhold og de problemer og utfordringer som foreligger der. B. Oppgavens overordnede mål har vært å få frem hvilke klientkategorier som særlig kan knyttes opp mot problematisk boadferd. Gjennom beskrivelse av problemområder som vedrører de syv klientkategoriene, vil dermed også kurante tiltak bli lansert for å avhjelpe problematisk boadferd. C. Innhenting av teoretisk grunnlagsmateriale har bydd på til dels store utfordringer fordi det eksisterer heller lite av litteratur som spesifikt tar for seg boevne og problematisk boadferd. Der hvor det likevel har vært noe å hente, er gjennom ulike forskningsrapporter som i hovedsak er utarbeidet av FAFO (Fagbevegelsens senter for forskning, utredning og dokumentasjon) og NIBR (Norsk institutt for by- og regionforskning). Selv her er problematisk boadferd omtalt sporadisk. Et stikkord som går igjen i mange av forskningsrapportene er betydningen av oppfølging fra det sosiale hjelpeapparatet som bidrag til å oppnå stabilitet og forutsigbarhet i kommunale forhold. D. I bruk av metode i undersøkelsen er hensynet til både bredde og dybde forsøkt ivaretatt. Dette innebærer at undersøkelsen har i seg elementer fra både kvantitative og kvalitative tilnærminger, dvs. både bredde og dybde. E. Totalt 33 informanter deltok i undersøkelsen. Undersøkelsen bestod av i alt 4 hovedspørsmål hvorav hovedspørsmål 1 og 2 bestod av i alt 6 underspørsmål. Innsamlingen av resultater ble foretatt i løpet av vinteren 2009/2010 og resultatene blir presentert i hele sin fulle bredde i kapittel 4. Resultatene eller funnene i undersøkelsen forteller med tydelighet hvilke klientkategorier som utviser god eller mangelfull boevne. Med utgangspunkt i funnene har det vært en målsetting å gi en beskrivelse av hvordan sosialklienters boevne i deres kommunale boforhold arter seg. De funnene som er gjort, viser klart hvilke klientkategorier som skiller seg ut ved å ha åpenbare 11 problemer i forhold til sin bosituasjon. Presentasjonen av funnene i undersøkelsen er både omfattende og til dels omstendelige. Vurderingen må være slik for at hensynet til både helhet og detaljer skal bli ivaretatt. F. Konklusjonene fra funnene i undersøkelsen blir så drøftet med særlig søkelys på sosialklientens forståelse av forholdet mellom ytelse og vilkår. Avhengig av klientens sosiale, fysiske og psykiske ballast kan dette gi seg utslag i forskjellige utfordringer og løsninger. Variasjonene i problematikk er bestemmende for hvilket botiltak som kan tilbys klienten. G. Det blir så foretatt en analyse av funnene i undersøkelsen hvor det blir presentert forslag til hvordan kommunale boforhold kan utvikle seg til å bli stabile. Stikkord i denne sammenheng er oppfølging og økonomstyring som bidrag til å skape trygge og forutsigbare rammer for klientens bosituasjon.
Published: 2011

31. 'Reguleringstvil og byggeskjønn' om reguleringsgrunnlaget for byggesaks behandling med eksempler fra gammel reguleringsplan i Asker kommune, sett opp i mot en mulig eiendomsutvikling av Gnr. 61 Bnr. 130

Author: Olsen, Knut Mikkel Normann
Subjects: Asker kommune, reguleringstvil, reguleringsplan, Norge
Published: 2011

32. Stellar Clusters in M31 from PHAT: Survey Overview and First Results

Author: Johnson, L. Clifton, Seth, Anil C., Dalcanton, Julianne J., Caldwell, Nelson, Gouliermis, Dimitrios A., Hodge, Paul W., Larsen, Soeren S., Olsen, Knut A. G., Roman, Izaskun San, Sarajedini, Ata, Weisz, Daniel R., and Collaboration, the PHAT
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Panchromatic Hubble Andromeda Treasury (PHAT) is an on-going Hubble Space Telescope (HST) multi-cycle program that will image one-third of the M31 disk at high resolution, with wavelength coverage from the ultraviolet through the near-infrared. This dataset will allow for the construction of the most complete catalog of stellar clusters obtained for a spiral galaxy. Here, we provide an overview of the PHAT survey, a progress report on the status of observations and analysis, and preliminary results from the PHAT cluster program. Although only ~20% of the survey is complete, the superior resolution of HST has allowed us to identify hundreds of new intermediate and low mass clusters. As a result, the size of the cluster sample within the Year 1 survey footprint has grown by a factor of three relative to previous catalogs., Comment: 6 pages, 3 figures, proceedings of "Stellar Clusters and Associations - A RIA workshop on GAIA", 23-27 May 2011, Granada, Spain
Published: 2011
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33. A Population of Accreted SMC Stars in the LMC

Author: Olsen, Knut A. G., Zaritsky, Dennis, Blum, Robert D., Boyer, Martha L., and Gordon, Karl D.
Subjects: Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: We present an analysis of the stellar kinematics of the Large Magellanic Cloud based on ~5900 new and existing velocities of massive red supergiants, oxygen-rich and carbon-rich AGB stars, and other giants. After correcting the line-of-sight velocities for the LMC's space motion and accounting for asymmetric drift in the AGB population, we derive a rotation curve that is consistent with all of the tracers used, as well as that of published HI data. The amplitude of the rotation curve is v_0=87+/-5 km s^-1 beyond a radius R_0=2.4+/-0.1 kpc, and has a position angle of the kinematic line of nodes of theta=142 degrees +/-5 degrees. By examining the outliers from our fits, we identify a population of 376 stars, or >~5% of our sample, that have line-of-sight velocities that apparently oppose the sense of rotation of the LMC disk. We find that these kinematically distinct stars are either counter-rotating in a plane closely aligned with the LMC disk, or rotating in the same sense as the LMC disk, but in a plane that is inclined by 54 degrees +/- 2 degrees to the LMC. Their kinematics clearly link them to two known HI arms, which have previously been interpreted as being pulled out from the LMC. We measure metallicities from the Ca triplet lines of ~1000 LMC field stars and 30 stars in the kinematically distinct population. For the LMC field, we find a median [Fe/H]=-0.56 +/- 0.02 with dispersion of 0.5 dex, while for the kinematically distinct stars the median [Fe/H] is -1.25 +/- 0.13 with a dispersion of 0.7 dex. The metallicity differences provide strong evidence that the kinematically distinct population originated in the SMC. This interpretation has the consequence that the HI arms kinematically associated with the stars are likely falling into the LMC, instead of being pulled out., 12 pages, 8 color figures, accepted for publication in the Astrophysical Journal
Published: 2011
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34. The ACS Nearby Galaxy Survey Treasury V. Radial Star Formation History of NGC 300

Author: Gogarten, Stephanie M., Dalcanton, Julianne J., Williams, Benjamin F., Roskar, Rok, Holtzman, Jon, Seth, Anil C., Dolphin, Andrew, Weisz, Daniel, Cole, Andrew, Debattista, Victor P., Gilbert, Karoline M., Olsen, Knut, Skillman, Evan, de Jong, Roelof S., Karachentsev, Igor D., and Quinn, Thomas R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present new Hubble Space Telescope (HST) observations of NGC 300 taken as part of the ACS Nearby Galaxy Survey Treasury (ANGST). Individual stars are resolved in these images down to an absolute magnitude of M_F814W = 1.0 (below the red clump). We determine the star formation history of the galaxy in 6 radial bins by comparing our observed color-magnitude diagrams (CMDs) with synthetic CMDs based on theoretical isochrones. We find that the stellar disk out to 5.4 kpc is primarily old, in contrast with the outwardly similar galaxy M33. We determine the scale length as a function of age and find evidence for inside-out growth of the stellar disk: the scale length has increased from 1.1 +/- 0.1 kpc 10 Gyr ago to 1.3 +/- 0.1 kpc at present, indicating a buildup in the fraction of young stars at larger radii. As the scale length of M33 has recently been shown to have increased much more dramatically with time, our results demonstrate that two galaxies with similar sizes and morphologies can have very different histories. With an N-body simulation of a galaxy designed to be similar to NGC 300, we determine that the effects of radial migration should be minimal. We trace the metallicity gradient as a function of time and find a present day metallicity gradient consistent with that seen in previous studies. Consistent results are obtained from archival images covering the same radial extent but differing in placement and filter combination., 18 pages, 18 figures, 4 tables, accepted for publication in ApJ
Published: 2010

35. The Star Formation Histories of the Bulge and Disk of M31 from Gemini North+NIRI/Altair and HST/NICMOS

Author: Olsen, Knut A. G., Blum, Robert D., Stephens, Andrew W., Davidge, Tim J., Massey, Philip, Strom, Stephen E., and Rigaut, Francois
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We discuss H and K observations of three fields in the bulge and disk of M31 obtained with the Altair adaptive optics system and NIRI instrument on Gemini North. These are the highest resolution and deepest near-infrared observations obtained to date of the inner regions of M31, and demonstrate the promise of ground-based adaptive optics for studying the crowded regions of nearby galaxies. We have combined our observations with previously published HST/NICMOS observations of nine M31 fields and have derived the coarse star formation histories of M31's bulge and inner disk. From fits to the M_K luminosity functions, we find the stellar population mix to be dominated by old, nearly solar-metallicity stars. The old populations, which we define as having age >~6 Gyr, indeed dominate the star formation histories at all radii independent of the relative contributions of bulge and disk stars. Although all of our fields contain some bulge contribution, our results suggest that there is no age difference between the bulge and disk to the limit of our precision., 65 total pages, 22 figures, accepted for publication in the Astronomical Journal
Published: 2006

36. Star Formation Histories from HST Color-Magnitude Diagrams of Six Fields of the LMC

Author: Olsen, Knut A. G.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present results on the analysis of background field stars found in HST WFPC2 observations of six of the old globular clusters of the Large Magellanic Cloud. Treated as contaminants by the globular cluster analysts, we produce V-I,V color-magnitude diagrams of the field stars and use them to explore the LMC's star formation history. The photometry approaches V~26, well below the turnoff of an ancient ~14 Gyr LMC population of stars. We use a maximum-likelihood technique to fit model CMDs drawn from Bertelli et al. (1994) isochrones to the observed CMDs. We constrain the models by the age-metallicity relation derived from LMC clusters, test four IMF slopes, and fit for the reddening, distance modulus, and star formation rate. We find that we can just resolve structure in SFR(t) with time steps of ~0.15 in log age, implying a resolution of ~4x10^8 years at an age of 1 Gyr. For a Salpeter IMF, our derived star formation history for the NGC 1754 field is characterized by an enhanced star formation rate over the past 4 Gyr, qualitatively resembling that derived by others for a variety of LMC fields. The remaining four fields, however, appear to have had high levels of star formation activity as long as 5-8 Gyr ago; these fields lie in the LMC Bar while the NGC 1754 field lies in the disk, suggesting that the inner regions of the LMC contain significantly more older stars than the outer regions. Examining the residuals of the models and observations, we find that the old red giant branches of the models provide a poor fit to the observations, which suggests an error in the model isochrones. The effect of the disagreement appears to be to underestimate the contribution of the old population., 48 pages, 19 Postscript figures, LaTeX, accepted by the Astronomical Journal
Published: 1999

37. Echoes of Historical Supernovae in the Milky Way Galaxy

Author: Rest, Armin, Carles Badenes, Blondin, Stephane, Challis, Peter, Clocchiatti, Alejandro, Filippenko, Alex, Foley, Ryan, Huber, Mark E., Matheson, Thomas, Mazzali, Paolo, Olsen, Knut, Sauer, Daniel, Sinnott, Brendan, Smith, R. Chris, Suntzeff, Nicholas, Welch, Doug, and Bergmann, Marcel

38. The Physical Parameters of Red Supergiants: When Massive Stars Are as Cool as They Get

Author: Philip Massey, Levesque, Emily, Olsen, Knut, Plez, Bertrand, Josselin, Eric, Maeder, Andre, and Meynet, Georges

39. SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud

Author: Gordon, Karl, Babler, Brian, Bernard, Jean-Philippe, Block, Miwa, Blum, Robert, Bolatto, Alberto, Caroline Bot, Bracker, Steve, Carlson, Lynn, Churchwell, Ed, Clayton, Geoffrey, Cohen, Martin, Engelbracht, Charles, Fukui, Yasuo, Gorjian, Varoujan, Harris, Jason, Hony, Sacha, Hora, Joseph, Indebetouw, Remy, Israel, Frank, Kawamura, Akiko, Leroy, Adam, Li, Aigen, Madden, Suzanne, Markwick-Kemper, Ciska, Meade, Marilyn, Meixner, Margaret, Misselt, Karl, Mizuno, Norikazu, Mizuno, Akira, Muller, Erik, Oliveira, Joana, Olsen, Knut, Onishi, Toshikazu, Paladini, Roberta, Points, Sean, Reach, William, Robitaille, Thomas, Rubin, Douglas, Sandstrom, Karin, Sato, Shuji, Sewilo, Marta, Shibai, Hiroshi, Simon, Josh, Smith, Linda, Srinivasan, Sundar, Tielens, Xander, Dyk, Schuyler, Loon, Jacco, Vijh, Uma, Volk, Kevin, Whitney, Barbara, and Zaritsky, Dennis

40. First Results from the Survey of the MAgellanic Stellar History (SMASH)

Author: Nidever, David L., Olsen, Knut A., Gruendl, Robert A., Besla, Gurtina, Saha, Abi, Olszewski, Edward, Munoz, Ricardo, Gallart, Carme, Monelli, Matteo, Walker, Alistair R., Blum, Robert D., Kaleida, Catherine C., Vivas, Kathy, Majewski, Steven R., Zaritsky, Dennis F., Roeland van der Marel, Bell, Eric F., Conn, Blair, Stringfellow, Guy S., Jin, Shoko, Monteagudo Nervion, Lara, Cioni, Maria-Rosa, Noel, Noelia, Martin, Nicolas, Monachesi, Antonela, Boer, Thomas, Chu, You-Hua, Kim, Hwihyun, Martinez-Delgado, David, Johnson, Lent C., Kunder, Andrea, and Smash

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

Author: Desi, Collaboration, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E., Allende Prieto, Carlos, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C., Bell, Eric F., Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S., Briceno, Cesar, Brooks, David, Brownstein, Joel R., Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G., Cahn, Robert N., Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G., Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J., Cervantes-Cota, Jorge L., Claybaugh, Todd M., Close, Madeline, Coker, Carl T., Cole, Shaun, Comparat, Johan, Cooper, Andrew P., Cousinou, M. -C, Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P., Davis, Tamara M., Dawson, Kyle S., La Macorra, Axel, Vicente, Juan, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T., Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R., Finkbeiner, Douglas P., Fitzpatrick, Michael J., Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E., Fosalba, Pablo, Frenk, Carlos S., Fumagalli, Michele, Gaensicke, Boris T., Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Pietro Gentile Fusillo, Nicola, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-De-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, Guy, Julien, Habib, Salman, Heetderks, Henry, Heetderks, Ian, Heitmann, Katrin, Hellwing, Wojciech A., Herrera, David A., Ho, Shirley, Holland, Stephen, Honscheid, Klaus, Huff, Eric, Hutchinson, Timothy A., Huterer, Dragan, Hwang, Ho Seong, Illa Laguna, Joseph Maria, Ishikawa, Yuzo, Jacobs, Dianna, Jeffrey, Niall, Jelinsky, Patrick, Jennings, Elise, Jiang, Linhua, Jimenez, Jorge, Johnson, Jennifer, Joyce, Richard, Jullo, Eric, Juneau, Stéphanie, Kama, Sami, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kennamer, Noble, Kent, Stephen, Kilbinger, Martin, Kim, Alex G., Kirkby, David, Kisner, Theodore, Kitanidis, Ellie, Kneib, Jean-Paul, Koposov, Sergey, Kovacs, Eve, Koyama, Kazuya, Kremin, Anthony, Kron, Richard, Kronig, Luzius, Kueter-Young, Andrea, Lacey, Cedric G., Lafever, Robin, Lahav, Ofer, Lambert, Andrew, Lampton, Michael, Landriau, Martin, Lang, Dustin, Lauer, Tod R., Le Goff, Jean-Marc, Le Guillou, Laurent, Le Suu, Auguste, Lee, Jae Hyeon, Lee, Su-Jeong, Leitner, Daniela, Lesser, Michael, Levi, Michael E., L Huillier, Benjamin, Li, Baojiu, Liang, Ming, Lin, Huan, Linder, Eric, Loebman, Sarah R., Lukić, Zarija, Ma, Jun, Maccrann, Niall, Magneville, Christophe, Makarem, Laleh, Manera, Marc, Manser, Christopher J., Marshall, Robert, Martini, Paul, Massey, Richard, Matheson, Thomas, Mccauley, Jeremy, Mcdonald, Patrick, Mcgreer, Ian D., Meisner, Aaron, Metcalfe, Nigel, Miller, Timothy N., Miquel, Ramon, Moustakas, John, Myers, Adam, Naik, Milind, Newman, Jeffrey A., Nichol, Robert C., Nicola, Andrina, Nicolati Da Costa, Luiz, Nie, Jundan, Niz, Gustavo, Norberg, Peder, Nord, Brian, Norman, Dara, Nugent, Peter, O Brien, Thomas, Oh, Minji, Olsen, Knut A. G., Padilla, Cristobal, Padmanabhan, Hamsa, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Palmese, Antonella, Pappalardo, Daniel, Pâris, Isabelle, Park, Changbom, Patej, Anna, Peacock, John A., Peiris, Hiranya V., Peng, Xiyan, Percival, Will J., Perruchot, Sandrine, Pieri, Matthew M., Pogge, Richard, Pollack, Jennifer E., Poppett, Claire, Prada, Francisco, Prakash, Abhishek, Probst, Ronald G., Rabinowitz, David, Raichoor, Anand, Ree, Chang Hee, Refregier, Alexandre, Regal, Xavier, Reid, Beth, Reil, Kevin, Rezaie, Mehdi, Rockosi, Constance M., Roe, Natalie, Ronayette, Samuel, Roodman, Aaron, Ross, Ashley J., Ross, Nicholas P., Rossi, Graziano, Rozo, Eduardo, Ruhlmann-Kleider, Vanina, Rykoff, Eli S., Sabiu, Cristiano, Samushia, Lado, Sanchez, Eusebio, Sanchez, Javier, Schlegel, David J., Schneider, Michael, Schubnell, Michael, Secroun, Aurélia, Seljak, Uros, Seo, Hee-Jong, Serrano, Santiago, Shafieloo, Arman, Shan, Huanyuan, Sharples, Ray, Sholl, Michael J., Shourt, William V., Silber, Joseph H., Silva, David R., Sirk, Martin M., Slosar, Anze, Smith, Alex, Smoot, George F., Som, Debopam, Song, Yong-Seon, Sprayberry, David, Staten, Ryan, Stefanik, Andy, Tarle, Gregory, Sien Tie, Suk, Tinker, Jeremy L., Tojeiro, Rita, Valdes, Francisco, Valenzuela, Octavio, Valluri, Monica, Vargas-Magana, Mariana, Verde, Licia, Walker, Alistair R., Wang, Jiali, Wang, Yuting, Weaver, Benjamin A., Weaverdyck, Curtis, Wechsler, Risa H., Weinberg, David H., White, Martin, Yang, Qian, Yeche, Christophe, Zhang, Tianmeng, Zhao, Gong-Bo, Zheng, Yi, Zhou, Xu, Zhou, Zhimin, Zhu, Yaling, Zou, Hu, and Ying Zu
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.CO, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract: DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tracers of the underlying dark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the Ly-$��$ forest absorption features in their spectra, which will be used to trace the distribution of neutral hydrogen. When moonlight prevents efficient observations of the faint targets of the baseline survey, DESI will conduct a magnitude-limited Bright Galaxy Survey comprising approximately 10 million galaxies with a median $z\approx 0.2$. In total, more than 30 million galaxy and quasar redshifts will be obtained to measure the BAO feature and determine the matter power spectrum, including redshift space distortions.

42. Survey of the MAgellanic Stellar History -- SMASH

Author: Nidever, David, Olsen, Knut, Besla, Gurtina, Gruendl, Robert, Saha, Abhijit, Gallart, Carme, Olszewski, Edward W., Munoz, Ricardo, Monelli, Matteo, Kunder, Andrea, Kaleida, Catherine, Walker, Alistair, Stringfellow, Guy, Zaritsky, Dennis, Roeland van der Marel, Blum, Robert, Vivas, Kathy, Chu, You-Hua, Martin, Nicolas, Conn, Blair, Noel, Noelia, Majewski, Steven, Jin, Shoko, Kim, Hwihyun, Cioni, Maria-Rosa, Bell, Eric, Monachesi, Antonela, Boer, Thomas, and Kapteyn Astronomical Institute
Abstract: Over the last several years, various discoveries have drastically altered our view of the iconic Magellanic Clouds (MCs), the nearest interacting galaxy system. The best evidence is now that they are on first infall into the Milky Way, that their stellar populations extend much further than previously thought, and that they suffered a close collision that tore out both the well-known Magellanic Stream and a large amount of still undetected stellar debris. Here we propose a community DECam survey of the Clouds mapping 480 deg^2 (distributed over 2400 deg^2 at 20% filling factor) to 24th mag griz (and u$ 23) that will supplement the 5000 deg^2 Dark Energy Survey's partial coverage of the Magellanic periphery, allowing us to map the expected stellar debris and extended populations with unprecedented fidelity. We have already conducted a pilot project demonstrating that DECam will allow us to: (1) Map the stellar periphery of the MCs with old main-sequence turnoff stars to a surface brightness limit of 35 mag/arcsec^2, revealing relics of their formation and past interactions. (2) Identify the stellar component of the Magellanic Stream and Leading Arm for the first time, if they exist, making them the only Galactic halo tracers with both gaseous and stellar components. (3) Derive spatially-resolved star formation histories covering all ages out to large radii of the MCs that will further complement our understanding of their formation. The combination of this survey and DES data will allow us to uncover a multitude of stellar structure that will unveil the complex and dramatic history of these two dwarf galaxies, while enabling a broad spectrum of community-led projects.

43. Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE)

Author: Meixner, Margaret, Babler, Brian, Bernard, Jean-Philippe, Blum, Robert, Boulanger, Francois, Churchwell, Edward, Cohen, Martin, Engelbracht, Charles, Frogel, Jay, Fukui, Yasuo, Gallagher, Jay, Gordon, Karl, Gorjian, Varoujan, Harris, Jason, Hora, Joseph, Indebetouw, Remy, Jansen, Stephen, Kawamura, Akiko, Kelly, Douglas, Kemper, Ciska, Latter, William, Leitherer, Claus, Madden, Suzanne, Meade, Marilyn, Misselt, Karl, Mizuno, Norikazu, Mizuno, Akira, Mould, Jeremy, Nota, Antonella, Oey, Sally, Olsen, Knut, Onishi, Toshikazu, Paladini, Roberta, Panagia, Nino, Perez-Gonzalez, Pablo, Reach, William, Shibai, Hiroshi, Shuji, Sato, Linda Smith, Staveley-Smith, Lister, Tielens, Xander, Ueta, Toshiya, Dyk, Schuyler, Volk, Kevin, Werner, Michael, Whitney, Barbara, and Zaritsky, Dennis

44. Surveying Nearby Nuclear Star Clusters

Author: Seth, Anil, Blum, Robert, Neumayer, Nadine, Debattista, Victor, Michele Cappellari, Mcdermid, Richard, Olsen, Knut, Bastian, Nate, Caldwell, Nelson, Stephens, Andrew, and Puzia, Thomas

45. SAGE-Spectroscopy: The life cycle of dust and gas in the Large Magellanic Cloud

Author: Tielens, Alexander, Markwick-Kemper, Francisca, Bernard, Jean-Philippe, Blum, Robert, Cohen, Martin, Dijkstra, Catharinus, Gordon, Karl, Gorjian, Varoujan, Harris, Jason, Hony, Sacha, Hora, Joseph, Indebetouw, Remy, Lagadec, Eric, Leisenring, Jarron, Madden, Suzanne, Marengo, Massimo, Matsuura, Mikako, Meixner, Margaret, Olsen, Knut, Paladini, Roberta, Paradis, Deborah, Reach, William T., Rubin, Douglas, Sewilo, Marta, Sloan, Greg, Speck, Angela, Srinivasan, Sundar, Schuyler Van Dyk, Vijh, Uma, Volk, Kevin, Whitney, Barbara, Zijlstra, Albert, and Loon, Jacco

46. The Stellar Populations of the Milky Way and Nearby Galaxies with LSST

Author: Olsen, Knut A., Covey, K., Saha, A., Beers, T. C., Bochanski, J., Boeshaar, P., Cargile, P., Catelan, M., Burgasser, A., Cook, K., Dhital, S., Figer, D., Ivezic, Z., Kalirai, J., Mcgehee, P., Minniti, D., Pepper, J., Prsa, A., Sarajedini, A., Silva, D., J. Allyn Smith, Stassun, K., Thorman, P., Williams, B., and Lsst, Stellar Populations Collaboration

47. Understanding the Dust Shells around Magellanic Cloud Red Supergiants

Author: Geoffrey Clayton, Morris, Pat, Ercolano, Barbara, Gordon, Karl, Levesque, Emily, Massey, Phil, Morris, Patrick, Olsen, Knut, Plez, Bertrand, Silva, David, Sugerman, Ben, Welch, Doug, and Wolff, Michael

48. The DESI Experiment Part II: Instrument Design

Author: Desi, Collaboration, Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E., Allende Prieto, Carlos, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C., Bell, Eric F., Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S., Briceno, Cesar, Brooks, David, Brownstein, Joel R., Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolas G., Cahn, Robert N., Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G., Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J., Cervantes-Cota, Jorge L., Claybaugh, Todd M., Close, Madeline, Coker, Carl T., Cole, Shaun, Comparat, Johan, Cooper, Andrew P., Cousinou, M. -C, Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P., Davis, Tamara M., Dawson, Kyle S., La Macorra, Axel, Vicente, Juan, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T., Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Elliott, Ann, Escoffier, Stéphanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R., Finkbeiner, Douglas P., Fitzpatrick, Michael J., Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E., Fosalba, Pablo, Frenk, Carlos S., Fumagalli, Michele, Gaensicke, Boris T., Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Pietro Gentile Fusillo, Nicola, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-De-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, Guy, Julien, Habib, Salman, Heetderks, Henry, Heetderks, Ian, Heitmann, Katrin, Hellwing, Wojciech A., Herrera, David A., Ho, Shirley, Holland, Stephen, Honscheid, Klaus, Huff, Eric, Hutchinson, Timothy A., Huterer, Dragan, Hwang, Ho Seong, Illa Laguna, Joseph Maria, Ishikawa, Yuzo, Jacobs, Dianna, Jeffrey, Niall, Jelinsky, Patrick, Jennings, Elise, Jiang, Linhua, Jimenez, Jorge, Johnson, Jennifer, Joyce, Richard, Jullo, Eric, Juneau, Stéphanie, Kama, Sami, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kennamer, Noble, Kent, Stephen, Kilbinger, Martin, Kim, Alex G., Kirkby, David, Kisner, Theodore, Kitanidis, Ellie, Kneib, Jean-Paul, Koposov, Sergey, Kovacs, Eve, Koyama, Kazuya, Kremin, Anthony, Kron, Richard, Kronig, Luzius, Kueter-Young, Andrea, Lacey, Cedric G., Lafever, Robin, Lahav, Ofer, Lambert, Andrew, Lampton, Michael, Landriau, Martin, Lang, Dustin, Lauer, Tod R., Le Goff, Jean-Marc, Le Guillou, Laurent, Le Suu, Auguste, Lee, Jae Hyeon, Lee, Su-Jeong, Leitner, Daniela, Lesser, Michael, Levi, Michael E., L Huillier, Benjamin, Li, Baojiu, Liang, Ming, Lin, Huan, Linder, Eric, Loebman, Sarah R., Lukić, Zarija, Ma, Jun, Maccrann, Niall, Magneville, Christophe, Makarem, Laleh, Manera, Marc, Manser, Christopher J., Marshall, Robert, Martini, Paul, Massey, Richard, Matheson, Thomas, Mccauley, Jeremy, Mcdonald, Patrick, Mcgreer, Ian D., Meisner, Aaron, Metcalfe, Nigel, Miller, Timothy N., Miquel, Ramon, Moustakas, John, Myers, Adam, Naik, Milind, Newman, Jeffrey A., Nichol, Robert C., Nicola, Andrina, Nicolati Da Costa, Luiz, Nie, Jundan, Niz, Gustavo, Peder Norberg, Nord, Brian, Norman, Dara, Nugent, Peter, O Brien, Thomas, Oh, Minji, Olsen, Knut A. G., Padilla, Cristobal, Padmanabhan, Hamsa, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Palmese, Antonella, Pappalardo, Daniel, Pâris, Isabelle, Park, Changbom, Patej, Anna, Peacock, John A., Peiris, Hiranya V., Peng, Xiyan, Percival, Will J., Perruchot, Sandrine, Pieri, Matthew M., Pogge, Richard, Pollack, Jennifer E., Poppett, Claire, Prada, Francisco, Prakash, Abhishek, Probst, Ronald G., Rabinowitz, David, Raichoor, Anand, Ree, Chang Hee, Refregier, Alexandre, Regal, Xavier, Reid, Beth, Reil, Kevin, Rezaie, Mehdi, Rockosi, Constance M., Roe, Natalie, Ronayette, Samuel, Roodman, Aaron, Ross, Ashley J., Ross, Nicholas P., Rossi, Graziano, Rozo, Eduardo, Ruhlmann-Kleider, Vanina, Rykoff, Eli S., Sabiu, Cristiano, Samushia, Lado, Sanchez, Eusebio, Sanchez, Javier, Schlegel, David J., Schneider, Michael, Schubnell, Michael, Secroun, Aurélia, Seljak, Uros, Seo, Hee-Jong, Serrano, Santiago, Shafieloo, Arman, Shan, Huanyuan, Sharples, Ray, Sholl, Michael J., Shourt, William V., Silber, Joseph H., Silva, David R., Sirk, Martin M., Slosar, Anze, Smith, Alex, Smoot, George F., Som, Debopam, Song, Yong-Seon, Sprayberry, David, Staten, Ryan, Stefanik, Andy, Tarle, Gregory, Sien Tie, Suk, Tinker, Jeremy L., Tojeiro, Rita, Valdes, Francisco, Valenzuela, Octavio, Valluri, Monica, Vargas-Magana, Mariana, Verde, Licia, Walker, Alistair R., Wang, Jiali, Wang, Yuting, Weaver, Benjamin A., Weaverdyck, Curtis, Wechsler, Risa H., Weinberg, David H., White, Martin, Yang, Qian, Yeche, Christophe, Zhang, Tianmeng, Zhao, Gong-Bo, Zheng, Yi, Zhou, Xu, Zhou, Zhimin, Zhu, Yaling, Zou, Hu, Zu, Ying, Korea Astronomy and Space Science Institute (KASI), University of California [Berkeley] (UC Berkeley), University of California (UC), Boston University [Boston] (BU), Carnegie Mellon University [Pittsburgh] (CMU), University of Edinburgh, National Optical Astronomy Observatory (NOAO), Instituto de Astrofisica de Canarias (IAC), Fermi National Accelerator Laboratory (Fermilab), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Yale University [New Haven], Ohio State University [Columbus] (OSU), The University of Notre Dame [Sydney], Department of Astronomy, University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Space Sciences Laboratory [Berkeley] (SSL), University of California (UC)-University of California (UC), University of Portsmouth, Centre for Astrophysics & Supercomputing, Swinburne University of Technology (Hawthorn campus), Ecole Polytechnique Fédérale de Lausanne (EPFL), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), The University of Utah, Cerro Tololo Inter-American Observatory, University College of London [London] (UCL), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institute for Astronomy [Edinburgh] (IfA), Department of Astronomy & Astrophysics [University of Toronto], University of Toronto, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Carreterra Mexico-Toluca, Department of Physics [Durham University], Durham University, Department of Astronomy, The Ohio State University, Institute for Computational Cosmology (ICC), Instituto de Fisica Teorica C-XVI (IFT-UAM/CSIC), Universidad Autónoma de Madrid (UAM), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Department of Applied Physics, Departamento de Fisica Aplicada [Granada], Universidad de Granada = University of Granada (UGR)-Universidad de Granada = University of Granada (UGR), University of Wyoming (UW), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Arizona State University [Tempe] (ASU), Department of Physics, University of California, University of California [Los Angeles] (UCLA), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Department of Physics [Durham], University of New Hampshire (UNH), Departamento de Fisica Teorica, Korea Institute for Advanced Study (KIAS), Centre d'Immunologie et des Maladies Infectieuses (CIMI), Institut National de la Santé et de la Recherche Médicale (INSERM)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Center for Cosmology & AstroParticle Physics, Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), School of Physics and Astronomy [Nottingham], University of Nottingham, UK (UON), School of Physics, University of Waterloo [Waterloo], Department of Astronomy and Space Science [Sejong University], Sejong University, Brookhaven National Laboratory [Upton, NY] (BNL), UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY)-U.S. Department of Energy [Washington] (DOE), Department of Physics [Ann Arbor], University of St Andrews [Scotland], University of Science and Technology of China [Hefei] (USTC), Department of Computer Science and Engineering [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Karlsruhe Institute of Technology (KIT), Key Laboratory for Liquid-Solid Structural Evolution and Processing of Materials, Shandong University, National University of Defense Technology [China], Avidea Technologies, Inc, DESI Collaboration, Okayama University, University of California [Berkeley], University of California, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), University of California-University of California, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universidad Autonoma de Madrid (UAM), Universidad Nacional Autónoma de México (UNAM), Universidad de Granada (UGR)-Universidad de Granada (UGR), Harvard University [Cambridge]-Smithsonian Institution, Centre d'Immunologie et de Maladies Infectieuses (CIMI), University of California [Irvine] (UCI), U.S. Department of Energy [Washington] (DOE)-UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), and Escoffier, Stephanie
Subjects: [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.CO, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), astro-ph.IM, Astrophysics - Cosmology and Nongalactic Astrophysics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: DESI (Dark Energy Spectropic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. The DESI instrument is a robotically-actuated, fiber-fed spectrograph capable of taking up to 5,000 simultaneous spectra over a wavelength range from 360 nm to 980 nm. The fibers feed ten three-arm spectrographs with resolution $R= \lambda/\Delta\lambda$ between 2000 and 5500, depending on wavelength. The DESI instrument will be used to conduct a five-year survey designed to cover 14,000 deg$^2$. This powerful instrument will be installed at prime focus on the 4-m Mayall telescope in Kitt Peak, Arizona, along with a new optical corrector, which will provide a three-degree diameter field of view. The DESI collaboration will also deliver a spectroscopic pipeline and data management system to reduce and archive all data for eventual public use.

49. Light Echoes of Galactic Explosions and Eruptions

Author: Rest, Armin, Bianco, Federica, Chornock, Ryan, Foley, Ryan, Kunder, Andrea, Matheson, Thomas, Olsen, Knut, Prieto, Jose Luis, Sinnott, Brendan, Smith, Chris, Smith, Nathan, and Doug Welch

50. A Pilot DECam Time-Domain Survey

Author: Bloom, Joshua, Matheson, Tom, Ridgway, Steve, Miller, Adam, Klein, Christopher, Walkowicz, Lucianne, Peter Nugent, Shivvers, Isaac, Smith, Chris, Olsen, Knut, Becker, Andrew, Norman, Dara, Simcoe, Rob, Oluseyi, Hakeem, Ridgway, Susan, Saha, Abi, Richards, Joey, Cenko, S. Bradley, and Lauer, Tod R.

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