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71 results on '"Casey, A. R."'

1. Stellar spots cause measurable variations in atmospheric metallicity

Author: Wilson, Tanner A. and Casey, Andrew R.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: To accurately measure a star's atmospheric parameters and chemical abundances, it is crucial to have high-quality spectra. Analysing the detailed chemical abundances of groups of stars can help us better understand nucleosynthesis, galactic chemical enrichment, and stellar evolution. In this study, we explored whether stellar spots can affect a star's inferred metallicity and, if so, where the impact is the strongest. To investigate this, we created synthetic infrared spectra that included stellar spots for a sample of main-sequence stars younger than the sun. We then applied two models to the data: one that accounted for spots and one that did not. From this, we can determine the bias introduced when fitting spotted spectra with a non-spotted model and how this bias varies with different parameters. Our findings revealed that fitting spotted spectra with a non-spotted model can introduce a scatter of up to 0.05 dex in the inferred metallicity, especially for stars with high levels of spot coverage. This bias is similar in magnitude to other relevant effects, such as atomic diffusion, radiative levitation, or non-local thermodynamic equilibrium. We also found that the effect is most pronounced in young stars and decreases with age. These results suggest that stellar spots can introduce a systematic uncertainty in metallicity that is not currently accounted for in spectroscopic analysis. This could potentially limit scientific inferences for population-level studies of young stars and differential abundance analyses., 9 pages, 7 Figures
Published: 2023

2. The Gaia-ESO Survey: homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, A. J., Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A, Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., Van der Swaelmen, M., Mikolaitis, Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
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: The Gaia-ESO Survey is a public spectroscopic survey that has targeted $\gtrsim10^5$ stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its public final release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O ($T_\mathrm{eff} \sim 30,000-52,000$~K) all the way to K-M ($\gtrsim$3,500~K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different type. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, e.g., activity and accretion indicators in young stars and membership probability in star clusters for more than 114,000 stars. The spectral analysis is coordinated by a number of Working Groups (WGs) within the Survey, which specialise in the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all Survey results are placed on a common scale to arrive at a single set of recommended results for all Survey collaborators to use. We also present some general quality and consistency checks performed over all Survey results., A&A accepted, minor revision, 36 pages, 38 figures
Published: 2023

3. Data Driven Optical Cool Dwarf Chemistry & the Giant Planet–[Fe/H] Correlation

Author: Rains, Adam D., Nordlander, Thomas, Casey, Andrew R., Žerjal, Maruša, Ireland, Michael J., and Bessell, Michael S.
Subjects: low-mass stars, spectroscopy, cool dwarf stars, data driven, stellar chemistry, fundamental parameters
Abstract: Detailed chemical studies of Solar-type stars have long been routine in stellar astrophysics, making possible studies in Galactic chemodynamics and exoplanet demographics. However, a similar understanding of the chemistry of M and late-K dwarfs—the most common stars in the Galaxy and most likely to host planets—has been greatly hampered by the complex molecular chemistry of their cool atmospheres. Here we present a new implementation of the Cannon, a data-driven model widely used in stellar astrophysics, developed for low–medium resolution optical (400–700nm) cool dwarf spectra. Our novel four parameter implementation in Teff, log g, [Fe/H], and [Ti/H] models both label uncertainties and missing labels, and is trained on 121 cool dwarf benchmarks—21 of which have literature elemental abundances measured from a warmer binary companion. Under leave-one-out cross-validation, we recover Teff, [Fe/H], and [Ti/H] with precisions of 2%, ±0.12 dex, and ±0.09 dex respectively, a precision which allows insight into the giant planet–[Fe/H] correlation for our sample of 65 TESS candidate planet hosts. Our work highlights the importance of precisely known benchmark systems; the promise of data-driven models for chemical analysis of the rich, but challenging to model, optical spectra of cool stars; and the utility of both in studying exoplanet demographics in the era of TESS and Gaia., {"references":["Rains, A. D. et al. (2021), MNRAS, 504, 5788"]}
Published: 2023
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4. Data Driven Optical Cool Dwarf Chemistry & the Giant Planet–[Fe/H] Correlation

Author: Rains, Adam D., Nordlander, Thomas, Casey, Andrew R., Žerjal, Maruša, Ireland, Michael J., Bessell, Michael S., Brun, Allan Sacha, Bouvier, Jérôme, and Petit, Pascal
Subjects: low-mass stars, spectroscopy, cool dwarf stars, data driven, stellar chemistry, fundamental parameters
Abstract: Detailed chemical studies of Solar-type stars have long been routine in stellar astrophysics, making possible studies in Galactic chemodynamics and exoplanet demographics. However, a similar understanding of the chemistry of M and late-K dwarfs—the most common stars in the Galaxy and most likely to host planets—has been greatly hampered by the complex molecular chemistry of their cool atmospheres. Here we present a new implementation of the Cannon, a data-driven model widely used in stellar astrophysics, developed for low–medium resolution optical (400–700nm) cool dwarf spectra. Our novel four parameter implementation in Teff, log g, [Fe/H], and [Ti/H] models both label uncertainties and missing labels, and is trained on 121 cool dwarf benchmarks—21 of which have literature elemental abundances measured from a warmer binary companion. Under leave-one-out cross-validation, we recover Teff, [Fe/H], and [Ti/H] with precisions of 2%, ±0.12 dex, and ±0.09 dex respectively, a precision which allows insight into the giant planet–[Fe/H] correlation for our sample of 65 TESS candidate planet hosts. Our work highlights the importance of precisely known benchmark systems; the promise of data-driven models for chemical analysis of the rich, but challenging to model, optical spectra of cool stars; and the utility of both in studying exoplanet demographics in the era of TESS and Gaia.
Published: 2023
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5. Estimating the selection function of Gaia DR3 sub-samples

Author: Castro-Ginard, A., Brown, A. G. A., Kostrzewa-Rutkowska, Z., Cantat-Gaudin, T., Drimmel, R., Oh, S., Belokurov, V., Casey, A. R., Fouesneau, M., Khanna, S., Price-Whelan, A. M., and Rix, H. W.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: Understanding which sources are present in an astronomical catalogue and which are not is crucial for the accurate interpretation of astronomical data. In particular, for the multidimensional Gaia data, filters and cuts on different parameters or measurements introduces a selection function that may unintentionally alter scientific conclusions in subtle ways. We aim to develop a methodology to estimate the selection function for different sub-samples of stars in the Gaia catalogue. Comparing the number of stars in a given sub-sample to those in the overall Gaia catalogue, provides an estimate of the sub-sample membership probability, as a function of sky position, magnitude and colour. This estimate must differentiate the stochastic absence of sub-sample stars from selection effects. When multiplied with the overall Gaia catalogue selection function this provides the total selection function of the sub-sample. We present the method by estimating the selection function of the sources in Gaia DR3 with heliocentric radial velocity measurements. We also compute the selection function for the stars in the Gaia-Sausage/Enceladus sample, confirming that the apparent asymmetry of its debris across the sky is merely caused by selection effects. The developed method estimates the selection function of the stars present in a sub-sample of Gaia data, given that the sub-sample is completely contained in the Gaia parent catalogue (for which the selection function is known). This tool is made available in a GaiaUnlimited Python package., Comment: 13 pages, 12 figures. Submitted to A&A
Published: 2023
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6. The Eighteenth Data Release of the Sloan Digital Sky Surveys: Targeting and First Spectra from SDSS-V

Author: Almeida, Andrés, Anderson, Scott F., Argudo-Fernández, Maria, Badenes, Carles, Barger, Kat, Barrera-Ballesteros, Jorge K., Bender, Chad F., Benitez, Erika, Besser, Felipe, Bizyaev, Dmitry, Blanton, Michael R., Bochanski, John, Bovy, Jo, Brandt, William Nielsen, Brownstein, Joel R., Buchner, Johannes, Bulbul, Esra, Burchett, Joseph N., Díaz, Mariana Cano, Carlberg, Joleen K., Casey, Andrew R., Chandra, Vedant, Cherinka, Brian, Chiappini, Cristina, Coker, Abigail A., Comparat, Johan, Conroy, Charlie, Contardo, Gabriella, Cortes, Arlin, Covey, Kevin, Crane, Jeffrey D., Cunha, Katia, Dabbieri, Collin, Davidson Jr., James W., Davis, Megan C., De Lee, Nathan, Delgado, José Eduardo Méndez, Demasi, Sebastian, Di Mille, Francesco, Donor, John, Dow, Peter, Dwelly, Tom, Eracleous, Mike, Eriksen, Jamey, Fan, Xiaohui, Farr, Emily, Frederick, Sara, Fries, Logan, Frinchaboy, Peter, Gaensicke, Boris T., Ge, Junqiang, Ávila, Consuelo González, Grabowski, Katie, Grier, Catherine, Guiglion, Guillaume, Gupta, Pramod, Hall, Patrick, Hawkins, Keith, Hayes, Christian R., Hermes, J. J., Hernández-García, Lorena, Hogg, David W., Holtzman, Jon A., Ibarra-Medel, Hector Javier, Ji, Alexander, Jofre, Paula, Johnson, Jennifer A., Jones, Amy M., Kinemuchi, Karen, Kluge, Matthias, Koekemoer, Anton, Kollmeier, Juna A., Kounkel, Marina, Krishnarao, Dhanesh, Krumpe, Mirko, Lacerna, Ivan, Lago, Paulo Jakson Assuncao, Laporte, Chervin, Liu, Ang, Liu, Chao, Liu, Xin, Lopes, Alexandre Roman, Macktoobian, Matin, Majewski, Steven R., Malanushenko, Viktor, Maoz, Dan, Masseron, Thomas, Masters, Karen L., Matijevic, Gal, McBride, Aidan, Medan, Ilija, Merloni, Andrea, Morrison, Sean, Myers, Natalie, Mészáros, Szabolcs, Negrete, C. Alenka, Nidever, David L., Nitschelm, Christian, Oravetz, Audrey, Oravetz, Daniel, Pan, Kaike, Peng, Yingjie, Pinsonneault, Marc H., Pogge, Rick, Qiu, Dan, Queiroz, Anna Barbara de Andrade, Ramirez, Solange V., Rix, Hans-Walter, Rosso, Daniela Fernández, Runnoe, Jessie, Salvato, Mara, Sanchez, Sebastian F., Santana, Felipe A., Saydjari, Andrew, Sayres, Conor, Schlaufman, Kevin C., Schneider, Donald P., Schwope, Axel, Serna, Javier, Shen, Yue, Sobeck, Jennifer, Song, Ying-Yi, Souto, Diogo, Spoo, Taylor, Stassun, Keivan G., Steinmetz, Matthias, Straumit, Ilya, Stringfellow, Guy, Sánchez-Gallego, José, Taghizadeh-Popp, Manuchehr, Tayar, Jamie, Thakar, Ani, Tissera, Patricia B., Tkachenko, Andrew, Toledo, Hector Hernandez, Trakhtenbrot, Benny, Trincado, Jose G. Fernandez, Troup, Nicholas, Trump, Jonathan R., Tuttle, Sarah, Ulloa, Natalie, Vazquez-Mata, Jose Antonio, Alfaro, Pablo Vera, Villanova, Sandro, Wachter, Stefanie, Weijmans, Anne-Marie, Wheeler, Adam, Wilson, John, Wojno, Leigh, Wolf, Julien, Xue, Xiang-Xiang, Ybarra, Jason E., Zari, Eleonora, and Zasowski, Gail
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The eighteenth data release of the Sloan Digital Sky Surveys (SDSS) is the first one for SDSS-V, the fifth generation of the survey. SDSS-V comprises three primary scientific programs, or "Mappers": Milky Way Mapper (MWM), Black Hole Mapper (BHM), and Local Volume Mapper (LVM). This data release contains extensive targeting information for the two multi-object spectroscopy programs (MWM and BHM), including input catalogs and selection functions for their numerous scientific objectives. We describe the production of the targeting databases and their calibration- and scientifically-focused components. DR18 also includes ~25,000 new SDSS spectra and supplemental information for X-ray sources identified by eROSITA in its eFEDS field. We present updates to some of the SDSS software pipelines and preview changes anticipated for DR19. We also describe three value-added catalogs (VACs) based on SDSS-IV data that have been published since DR17, and one VAC based on the SDSS-V data in the eFEDS field., Comment: Accepted to ApJS
Published: 2023
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7. Many Roads Lead to Lithium: Formation Pathways For Lithium-Rich Red Giants

Author: Sayeed, Maryum, Ness, Melissa K., Montet, Benjamin T., Cantiello, Matteo, Casey, Andrew R., Buder, Sven, Bedell, Megan, Breivik, Katelyn, Metzger, Brian D., Martell, Sarah L., and McGee-Gold, Leah
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: Stellar models predict that lithium (Li) inside a star is destroyed during the first dredge-up phase, yet 1.2% of red giant stars are Li-rich. We aim to uncover possible origins of this population, by analysing 1155 Li-rich giants (A(Li) $\geq$ 1.5) in GALAH DR3. To expose peculiar traits of Li-rich stars, we construct a reference sample of Li-normal (doppelg\"anger) stars with matched evolutionary state and fiducial supernova abundances. Comparing Li-rich and doppelg\"anger spectra reveals systematic differences in the H-$\alpha$ and Ca-triplet line profiles associated with the velocity broadening measurement. We also find twice as many Li-rich stars appear to be fast rotators (2% with $v_\textrm{broad} \gtrsim 20$ km s$^{-1}$) compared to doppelg\"angers. On average, Li-rich stars have higher abundances than their doppelg\"angers, for a subset of elements, and Li-rich stars at the base of RGB have higher mean $s-$process abundances ($\geq 0.05$ dex for Ba, Y, Zr), relative to their doppelg\"angers. External mass-transfer from intermediate-mass AGB companions could explain this signature. Additional companion analysis excludes binaries with mass ratios $\gtrsim$ 0.5 at $\gtrsim$ 7 AU. We also discover that highly Ba-enriched stars are missing from the Li-rich population, possibly due to low-mass AGB companions which preclude Li-enrichment. Finally, we confirm a prevalence of Li-rich stars on the red clump that increases with lithium, which supports an evolutionary state mechanism for Li-enhancement. Multiple culprits, including binary spin-up and mass-transfer, are therefore likely mechanisms of Li-enrichment., Comment: 29 pages, 19 figures, 6 tables. Submitted to ApJ
Published: 2023
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8. Iron-rich Metal-poor Stars and the Astrophysics of Thermonuclear Events Observationally Classified as Type Ia Supernovae. I. Establishing the Connection

Author: Reggiani, Henrique, Schlaufman, Kevin C., and Casey, Andrew R.
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: The progenitor systems and explosion mechanisms responsible for the thermonuclear events observationally classified as Type Ia supernovae are uncertain and difficult to uniquely constrain using traditional observations of Type Ia supernova host galaxies, progenitors, light curves, and remnants. For the subset of thermonuclear events that are prolific producers of iron, we use published theoretical nucleosynthetic yields to identify a set of elemental abundance ratios infrequently observed in metal-poor stars but shared across a range of progenitor systems and explosion mechanisms: [Na,Mg,Co/Fe], Accepted for publication at AJ
Published: 2023
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9. The GALAH Survey: chemical tagging and chrono-chemodynamics of accreted halo stars with GALAH+ DR3 and Gaia eDR3

Author: Buder, Sven, Lind, Karin, Ness, Melissa K., Feuillet, Diane K., Horta, Danny, Monty, Stephanie, Buck, Tobias, Nordlander, Thomas, Bland-Hawthorn, Joss, Casey, Andrew R., De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Hayden, Michael R., Kos, Janez, Martell, Sarah L., Lewis, Geraint F., Lin, Jane, Schlesinger, Katharine. J., Sharma, Sanjib, Simpson, Jeffrey D., Stello, Dennis, Zucker, Daniel B., Zwitter, Tomaz, Ciuca, Ioana, Horner, Jonathan, Kobayashi, Chiaki, Ting, Yuan-Sen, Wyse, Rosemary F. G., and Collaboration, The GALAH
Subjects: Astrophysics - Solar and Stellar Astrophysics, formation [Galaxy], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), abundances [Galaxy], halo [Galaxy], FOS: Physical sciences, Astronomy and Astrophysics, kinematics and dynamics [Galaxy], Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Since the advent of $Gaia$ astrometry, it is possible to identify massive accreted systems within the Galaxy through their unique dynamical signatures. One such system, $Gaia$-Sausage-Enceladus (GSE), appears to be an early "building block" given its virial mass $> 10^{10}\,\mathrm{M_\odot}$ at infall ($z\sim1-3$). In order to separate the progenitor population from the background stars, we investigate its chemical properties with up to 30 element abundances from the GALAH+ Survey Data Release 3 (DR3). To inform our choice of elements for purely chemically selecting accreted stars, we analyse 4164 stars with low-$��$ abundances and halo kinematics. These are most different to the Milky Way stars for abundances of Mg, Si, Na, Al, Mn, Fe, Ni, and Cu. Based on the significance of abundance differences and detection rates, we apply Gaussian mixture models to various element abundance combinations. We find the most populated and least contaminated component, which we confirm to represent GSE, contains 1049 stars selected via [Na/Fe] vs. [Mg/Mn] in GALAH+ DR3. We provide tables of our selections and report the chrono-chemodynamical properties (age, chemistry, and dynamics). Through a previously reported clean dynamical selection of GSE stars, including $30 < \sqrt{J_R~/~\mathrm{kpc\,km\,s^{-1}}} < 55$, we can characterise an unprecedented 24 abundances of this structure with GALAH+ DR3. Our chemical selection allows us to prevent circular reasoning and characterise the dynamical properties of the GSE, for example mean $\sqrt{J_R~/~\mathrm{kpc\,km\,s^{-1}}} = 26_{-14}^{+9}$. We find only $(29\pm1)\%$ of the GSE stars within the clean dynamical selection region. Our methodology will improve future studies of accreted structures and their importance for the formation of the Milky Way., 29 pages, 18 figures, 6 tables; publicshed in MNRAS; all code to recreate results (based on public data described in arXiv:2011.02505) and figures available at https://github.com/svenbuder/Accreted-stars-in-GALAH-DR3
Published: 2021

10. The GALAH Survey: A New Sample of Extremely Metal-Poor Stars Using A Machine Learning Classification Algorithm

Author: Hughes, Arvind C. N., Spitler, Lee R., Zucker, Daniel B., Nordlander, Thomas, Simpson, Jeffrey, Da Costa, Gary S., Ting, Yuan-Sen, Li, Chengyuan, Bland-Hawthorn, Joss, Buder, Sven, Casey, Andrew R., De Silva, Gayandhi M., D'Orazi, Valentina, Freeman, Ken C., Hayden, Michael R., Kos, Janez, Lewis, Geraint F., Lin, Jane, Lind, Karin, Martell, Sarah L., Schlesinger, Katharine J., Sharma, Sanjib, Zwitter, Tomaz, and Collaboration, The GALAH
Subjects: Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract: Extremely Metal-Poor (EMP) stars provide a valuable probe of early chemical enrichment in the Milky Way. Here we leverage a large sample of $\sim600,000$ high-resolution stellar spectra from the GALAH survey plus a machine learning algorithm to find 54 candidates with estimated [Fe/H]~$\leq$~-3.0, 6 of which have [Fe/H]~$\leq$~-3.5. Our sample includes $\sim 20 \%$ main sequence EMP candidates, unusually high for \emp surveys. We find the magnitude-limited metallicity distribution function of our sample is consistent with previous work that used more complex selection criteria. The method we present has significant potential for application to the next generation of massive stellar spectroscopic surveys, which will expand the available spectroscopic data well into the millions of stars., 27 pages, 20 figures, accepted for publication in ApJ, candidate table available at this https://github.com/arvhug/GALAH---TSNE_EMP
Published: 2022

11. Veteran Adherence to Oral Versus Injectable Alcohol Use Disorder Medication Treatment

Author: Dorflinger, Charles, Carey, Heather, Roche, Jennifer, Burant, Christopher, LeHew, Colleen, Stewart, Hayden, Mitchell, Brian, Ayanga, Daniel, Walder, Annette, Cooler, Jordan, Wu, Shuwen, Frey, Theresa, Wenthur, Cody, Burk, Bradley, Ward, Alex, Clark, Brooke, Leung, Jonathan G, Kutzke, Jade, May, Heather P, Maehler, Colin, Kummer, Bethany, Hamner, Jennifer, Ariefdjohan, Merlin, Stutzman, Danielle L, Kicklighter, Jackson, Musco, Shaina, Singson, Grace Marielle, Pamintuan, Claire, Francisco, Janelle, Phan, Tam, Sevak, Rajkumar J, Rogan, Edward L, Kehoe, William A, Halliwell, Robert F, Kanter, Joel, Ryan, Holly, Patel, Krupa, Moukaddam, Nidal, Saunders, John, Fernandez, Luis, Shah, Asim, Wong, Jerry, Erowele, Goldina, Ruppelt, Sara, Tillery, Erika E, Baker, Joni, Loflin, Bobbi Jo, Gray, Emily, Conley, Giulia, Hembree, Amanda, Sterling, Jacyntha, Buige, Ashley N, Nguyen, Mimi, Harris, Suzanne C, Bhavsar, Nisha, Shah, Niti, Lee, Bona, Jeong, Seoyoung, Maroney, Megan E, Whalen, Eric D, Maloney, Rebecca M, Hagemeier, Nicholas E, Takamura, Kay, Rice, Amanda G, Furbish, Amelia B, Hebbard, Amy M, Ross, Clint, Cumbie, Holly, Hickey, J. Scott, Lalani, Falak, Mucha, Hannah, Saklad, Stephen R, Ma, Connie, Lee, Kelly, O’Donnell, Carolyn, Jackson, Sarah, Albee, Jennifer Nelson, Yapel, Ann, Nash, Cynthia, MacDonald, Danielle, King, Amelia, Schneiderhan, Mark, Hager, Keri, Bell Lynum, Karimah S, Nash, Abigail, Fu, Dong Jing, Ionescu, Dawn F, Sliwa, Jennifer Kern, Turkoz, Ibrahim, Dorson, Peter G, Canuso, Carla, Hsia, Stephanie, Nguyen, Julie, La, Amenda, Gruenberg, Katherine, MacDougall, Conan, Brockbank, Josh, Wong, Kara, Schultz, Erica, Pinchinat, Jessica, Thibeaux, Taylor M, McCants, Tamara, Lam, Jason, Diaz-Luna, Jose, Nguyen, Jennifer, Yokoyama, Melissa, Albiar, Olivia, Bradley, Bridget, Popish, Sarah J, Bounthavong, Mark, Lau, Marcos K, Wells, Daina L, Kay, Chad L, Harvey, Michael A, Himstreet, Julianne E, Christopher, Melissa L.D, Weeda, Erin R, McGraw, Daniel J, Gonzalez, Misty L, Pardo-Pfeiffer, Carlos, Rodeghiero, Abigail, Zhang, Lusi, Brown, Sarah Jane, Shan, Yuting, Lee, Adam M, Allen, Josiah D, Eum, Seenae, Bishop, Jeffrey R, Gonzalez, Rolando, Wahl, Kimberly, Naglich, Andrew, Ayson, Marl, Thomas, Kelan, Renfro, Mandy L, Loera, Lindsey J, Hill, Lucas G, Tirado, Carlos, Delerme, Dante, Dean, Taylor, Cullen, Marissa, Straley, Craig M, Carr, Chelsea N, Sun, Wendy, Alzouby, Hiba, Harris, Suzanne, Banker, Christopher M, Cook, Sarah F, Muir, Justin, Brodie, Daniel, Cremers, Serge, Bies, Robert R, Dzierba, Amy L, Moton, Robert, Saklad, Stephen, Ferris, Ryan E, Noble, Brie N, Hartung, Daniel M, Tjia, Jennifer, Furuno, Jon P, Ibrahim, Hajer, Duong, Dat, Malcolm, Benjamin, Gogineni, Hyma P, Zahn, Amy L, Alibeckoff, Chloe C, Connor, Sharon, Buranosky, Raquel, Livezey, Sabrina N, Daniell, Jessica, DeClercq, Josh, Choi, Leena, Zuckerman, Autumn, Shah, Nisha B, Kang, Ashley, Anksorus, Heidi, Troglin, Courtney G, Bouldin, J. Brooke, Schreiner, Shannon, McKinney, Mariah, Brown, Stacy D, Pond, Brooks B, Nguyen, Thu, Chin, Hyun Ji, Dambly, Nicolle, Augsten, Alberto, Themas, Samantha, Vicencio, Claudia, Horner, Caroline, Covert, Kelly, Lewis, Paul, Tharp, Jen, Sommi, Roger W, Bidollari, Ilda, Still, Daniel, Du, Yangchun, Yagoda, Sergey, Weiden, Peter J, Long, Katelyn, Vandiver, Emily, Johnson, Stephanie, Darazs, Brooks, Tillery, Erika, Silvia, Richard J, Lee, Kelly C, Bien, Ivy, Farahmand, Khodayar, Goldsmith, Hannah, Farrar, Mallory, Le, Hadley, Huynh, Quynh, Kim, Jane, McCausland, Kristen, Haider, Batool, White, Michelle K, O’Sullivan, Amy K, Rychlec, Kaitlin, Akerman, Sarah, Fratantonio, James, Saxon, Andrew, Thase, Michael E, Parikh, Sagar V, Maheshwari, Priya, Rothschild, Anthony J, Dunlop, Boadie W, DeBattista, Charles, Conway, Charles R, Forester, Brent P, Shelton, Richard C, Macaluso, Matthew, Brown, Krystal, Li, James, Jablonski, Michael R, Greden, John F, Gidal, Barry, Patsalos, Philip, Szaflarski, Jerzy, VanLandingham, Kevan, Critchley, David, Morrison, Gilmour, Weiss, Catherine, Meehan, Stine Rasmussen, Ouyang, John, Hobart, Mary, Rowe, William, Vanover, Kimberly E, Kane, John M, Satlin, Andrew, Durgam, Suresh, Davis, Robert E, Mates, Sharon, Correll, Christoph U, Tamminga, Carol, Rabon, Hannah, Smith, Jordan, Squires, Karrie, VanDaele, Madeline, Logan, Linda D, Zhang, Feng, DeSousa, Norberto J, Sallee, F. Randy, Lickrish, David, Incledon, Bev, Smith, Joseph L, Candon, Molly, Fadeyibi, Oluwatoyin, Connolly, K. Ryan, Lim, Suet, Neimark, Geoffrey, Mandell, David, Newcomer, John W, Silverman, Bernard, DiPetrillo, Lauren, Graham, Christine, Jiang, Ying, Simmons, Adam, Hopkinson, Craig, McDonnell, David, Kahn, Rene, King, Thomas R, Kando, Judith C, Pardo, Antonio, King, Thomas, Edwards, John B, Chen, Richard, Huo, Jason, Cutler, Andrew J, Fawver, Jay, Flanagan, Mindy, Smith, Thomas, Drouin, Michelle, Mirro, Michael, Yatham, Lakshmi N, Vieta, Eduard, McIntyre, Roger S, Jain, Rakesh, Earley, Willie R, Patel, Mehul, Brown, Lisa, Sehgal, Rahul, Yu, Ken, Al Habbab, Talal, Johnson, Holly, Dechairo, Bryan, Chen, Jack J, Singer, Carlos, Marder, Stephen R, Comella, Cynthia L, Shah, Chirag, Jimenez, Roland, Goodwin, Heather, Morrow, Gina, Tewksbury, Ashley, Waters, Kristin, Eggert, Robyn, Tallian, Kimberly, Sepulveda, Joe A, Rojas, Sarah, Sikand, Harminder, Sutera, Nathan, Iuppa, Courtney A, Nelson, Leigh Anne, Kriz, Carrie R, Burns, Nicole A, Lang, Shelby E, Elliott, Ellie S.R, Luong, Uyen, Elsobky, Teresa, Abelleira, Audrey, Awan, Sundus, Dume, Roberta, Dilich, Adam, Anderson, Mikaela, Park, Priscilla, Moehnke, Austin, Aebi, Cydreese, Feighner, Lydia, Vernon, Martein, Streit, Jessica, Kauer, Jill, Lemons, Amber, Diefenderfer, Lauren A, Moon, Joseph, Smith, Jordan O, Franck, Hugh A, Randle, C. Hope, Hedgepeth Kennedy, M. Lindsey, James, Shannon, Coplan, Benjamin, Ruekert, Laura, Puri, Shilpa, Yeleti, Ramya, Cathright, Sela, Coveart, Stephanie, Regen, Sloan, Stewart, Shannon, Stratton, Miranda, Haight, Robert, Hoeft, Dawn, Bishop, Danielle, De La Cruz, Austin, Aurelio, Mariellee, Prestenback, Autumn, Price, Paul L, Makuch, Christian X, Salisbury, Nicole M, Koch, Jessa, Palmer, Melissa C, Chace, Ashley, Price, Cristofer, Putney, Jessica, Khan, Fatima, Huntsman, Amanda, Hutcheson, Brooklyn, Hightower, Sharae, Ott, Carol A, Scott, Catherine, Balser, Amanda, Karas, Andrew, Hsu, Michael, Malin, Maureen, Robert, Sophie, Leung, Edwina, Mierzwa, Mark, Kay, Lehua, Bowling, Dalia, Allen, Sabrina, Weingartner, Melissa, Ventricelli, Daniel, Santa, Heather, Nowalk, Alexandra, Downs, George, Le, N, Mospan, C, Burton, Caitlin, Mathys, Monica, Gutierrez, Erika, Ali, Sarah, Chang, Joni, Holzum, Dorothy N, Griffith, June A, Morgan, Katherine T, Laguado, S. Andrea, Steavenson, Rosana, Mehvar, Mina, Bechtold, Carson L, Kim, Heesoo, Dopheide, Julie Ann, Anderson, Lindsey, Kleyn, Thomas, DiRenzo, Baely, Walroth, Todd, Adamczyk, Raechel, Kendrick, Jenna, Thomas, Christopher, Mailloux, Lindsay M, Haas, Matthew T, Larew, Janel M, Stohs, Matthew E, DeJongh, Beth M, Satow, Britney A, Titus-Lay, Erika, Clark, Suzanne, Dike, Dozie, Pinsonnault, John, Gamber, Joy, Roseberry, Samantha, Mitchell, Brian G, Nguyen, Mai, Willborn, Robert, Roche-Desilets, Jennifer, Dailey, Alison, Ignatowski, Michael, Routhieaux, Melanie, Kawsky, Jaclyn, Stratman, Jennifer, Corboy, Alexander, Norberte, Cherisse, Gross, Tonya, Daniel, Jeremy, Tran, Aaron N, Wary, Megan, Kostric, Anna, Schaller, Samantha, Shin, Yunjung, Maroney, Megan, Hampton, Chanese, Krieger, Kelly, Hartwig, Rachel, Thamawatanakul, Rani, Wilbur, Eileen, Shofner, Steven, Butler, Justin, Moody, Breanna, Davis, Elizabeth, Hofammann, Elizabeth, Liveoak, Katie, Mitchell, McKinley, Lebrecht, Morgan, Hawley, Joanne, Smigiel, Joe, Radtke, Michelle, Walkerly, Autumn, King, Morgan, Wakefield, Andrew, Downs, Mona, Hudson, Nancy, Burghart, Steven, Reynoldson, Jill, Booth, Macey, Ishino, Risa, Lee, Tammie, Wright, Melissa, Boggs, Angela, Kaur, Rajandeep, Patel, Parth, Smith, Thomas R, Theriault, Sarah, Okusaga, Olaoluwa, Reinstatler, Kristina, Hawk, David, Rush, Stephen, Vachuska, Michaela, Powell, Elizabeth, Lacro, Jonathan, Chehovich, Charisse, Demler, Tammie Lee, deRosas, Andrea, Trigoboff, Eileen, Taylor, Aminah, Singh, Divita, Burdge, Gary, Reynolds, Jamie, Kriz, Carrie, Burns, Nicole, Sommi, Roger, Yabs, Melanie, Sarpal, Deepak, Fabian, Tanya, Bartos, Lindsey, Tallman, Kristin, Johnson, Dara, Taylor, Daniel, Hogan, Brendon, Kwan, Peter, Bast, Aubree, Sanchez, Apolinar, Maglalang, Patricia D, Scheible, Mahli M, Skurat, McKenzie K, Jackson, Sarah K, Belknap, Jazmin N, Ostfeld, Larissa, Fahy, Megan, Nguyen, Tuyen, Bui, Hoa, Little, Meg M, Seifert, Randall, Maister, Ashley, McCarthy, Caitlin, Burger, Emily, Mullen, Sandy, Cusimano, Joseph, VandenBerg, Amy, Duquette, Meghan, Guttenberg, Viktoria, Matsunaga, Candace, White, Shelby, Richard, Andrea, Jones, Jessica, Morgan, Kaitlyn, Kelsey, Taylor, Sartin, Carrie J, Rickert, Leah, Ferrill, Laine, Vallabh, Anuja, Jhawar, Archana, Barrett, Monica, Ward, Sarah, Colvard, Michelle, Phan, Joann, Preinitz, Jennifer, Ellis, Marcus, Gibu, Matthew, Kivlehan, Audrey, Chiulli, Dana, Rhodes, Kirby, Brewer, T. Amber, Richard, Michelle, Kirwan, Brigit, Flowers, Gary, Albritton, Melinda, Sutton, Caroline M, McEachern, Sydney, Miskle, Benjamin, Barr, Rachel, Thomas, Chris, Yang, Waverly, Vogt, Caitlin, Charles, Amanda, Mathews, Alisha, Bhandari, Deepali, Olsen, Emily, Garling, Ashley, Liszka, Jessica, Goodman, Courtney S, Smith, Tammy, Barron, Ana, Williams, Andrew, Zuloaga, Andrea, Parra, Brianne, Miller, Joy, Blake, Jennifer, Toney, Gregory, Galeano, Kathleen, Morabito, Brianna, Smith, Sydney, Miller, Lindsey, Fleisch, Sheryl, Kim, Erika, Kurz, Troy, Peterson, Angela M, Gruca, Justin, McGuire, Michael, Stummer, Lauren, Yip, Agustin, Rodriguez-Villa, Fernando, Wilson, Jennifer, Sutton, Caroline, Owings, R. Laney, Herbst, Claire, Hosmer, Kane, Wulff-Burchfield, Elizabeth, Ramion, Shelby, Brown, Lauren, Shishko, Ilona, Allen, Sarah, Nichols, Taylor, Fawcett, Janet, Trent, Kelley N, Eatmon, Courtney V, Hershberger, Allie, Roads, Mary, Pittenger, Amy L, Dadebo, Victoria, Tomko, John R, Simeone, Danielle, Sherwood, Devon A, Morgan, Katherine, White, C. Whitney, Holzum, Dorothy, Adetunji, Oluwaseyi, Blalock, Meredith, Snyder, Sabrina Domicoli, Kneebusch, Jamie, Mitchell, Melissa, Butala, Niyati, McHugh, Trisha, McGuire, J Michael, Moller, Karen, Melton, Brittany, Mitchell, Melissa M, Chaplin, Kyrsten, Canto, Samantha, Hang Vu, Thi Thuy, Rey, Jose A, Elmaoued, Amre Adel, Hopper, Jessica, Do, Annette, Leckband, Susan G, Abraham, Dana L, Haught, Emma J, Kobulinsky, Lawrence R, Fabian, Tanya J, Greenwood, Jessica, Rey, Jose, Chen, Emily, Farhadian, Sanaz, Smith, Austin M, Hopkins, Tiffany M, Deardorff, O. Greg, Jenne, Victoria, Wood, Joshua, Trout, Megan, Beck, Niels C, Pals, Hale, Frazier, Erica, Cavaliere, Vincent S, DiPaula, Bethany A, Glassman, Matthew, Wehring, Heidi J, Mackowick, Marie, Park, Jaeboon, Love, Raymond C, Kelly, Deanna L, Newbold, Mervan, Fioravanti, Nicole, Brown, Matthew J, Casey, Emily R, Nadkarni, Neha, Oh, Sarah, Patel, Romi, Riedley, Taylor, Mathis, Erin, Fadden, Patrick, Madden, Cristina, Schneiderhan, Mark E, Hintsala, Madelynn, Stenehjem, David, Rufus, Krystal M, Elhakim, Athar, Zolezzi, Monica, Elamin, Waad M, Homs, Shorouk, Qubaiah, Iman K, Mahmoud, Doaa A, Tawfik, Enge M, Fritz, Merideth, Alman, Brianne, Wartman, Carolanne, Clark, Megan, Ott, Carol, Rainey, Carly A, Mann, Elise, Modany, Madison, Schoettmer, Amanda, Buckley, Tiffany, Patwardhan, Vidisha, Boyle, Cynthia J, Gardner, Kristen N, Hamby, Kerri, Ngo, Nichol, Kim, Lila Q, Chen, Steven W, Mosley, Scott, Dadiomov, David, Goldstone, Lisa W, DellaVecchia, Matthew J, Cauffield, Jacintha, Grim, Hannah, Eschler, Anna, Aladeen, Traci, Blondell, Richard, Capote, Horacio, Rainka, Michelle, Lee, Ashley, Shelley, Maria, Stoncius, Kristina, Berry, Jonathan, Doroudgar, Shadi, Johnson, Kayla, Pouliot, Jonathon, Rarrick, Christine, Hebbard, Amy, Shikwana, Sara, Koller, Katherine, Reed, Ellen, Hoefling, Austin D, Miles, Talia M, Ansara, Elayne D, Titova, Viktoriya, Kandela, Dalea, Douglass, Amber R, Ehrhard, Kimberly, Stanley, Madison, Ganihong, Carissa, Liu, Mei T, Bohnenberger, Kristin, Zuber, Nicole, Plunkett, McKenzie, Axelrod, Chelsey, Lightfoot, Myaa, Moore, Miranda, Crouse, Ericka, Olazo, Muriel, Taormina, Stephanie, Reiss, Rebecca, Denno, Nora, Johnson, Braniesha, Wilkening, Gwendolyn Lucy, Andrews, Haley, Neumeister, Kristen, Murad, Muhammad Ubaidullah, Reid, Bailey, Franco, Ashley, Stutzman, Danielle, Jorgensen, Jennifer, Basit, Saadia, Jensen, Aimee, Nadal, Celeste N, Truong, Quynh-Nhu, Jameson, Melanie, Knox, Erin D, Bota, Robert G, Wieruszewski, Patrick M, and Leung, Sarah B
Subjects: CPNP Foundation Strategic Goals Award Finalists, Therapeutic Case Report Abstracts, Original Research Abstracts, Therapeutic Case Report Award Finalists, Article, Encore Presentation Abstracts, Work in Progress Abstracts, Neuropsychology and Physiological Psychology, Original Research Award Finalists, Research Trainee Award Finalists, Pharmacology (medical), Neurology (clinical), General Pharmacology, Toxicology and Pharmaceutics, Innovative Practices Abstracts, Innovative Practices Award Finalists, Scientific Posters
Published: 2020

12. The impact of the COVID-19 pandemic on academic productivity

Author: Casey, Andrew R., Mandel, Ilya, and Ray, Prasun K.
Subjects: Physics - Physics and Society, Computer Science - Digital Libraries, Economics - General Economics
Abstract: 'Publish or perish' is an expression describing the pressure on academics to consistently publish research to ensure a successful career in academia. With a global pandemic that has changed the world, how has it changed academic productivity? Here we show that academics are posting just as many publications on the arXiv pre-print server as if there were no pandemic: 168,630 were posted in 2020, a +12.6% change from 2019 and $+1.4\sigma$ deviation above the predicted 162,577 $\pm$ 4,393. However, some immediate impacts are visible in individual research fields. Conference cancellations have led to sharp drops in pre-prints, but laboratory closures have had mixed effects. Only some experimental fields show mild declines in outputs, with most being consistent on previous years or even increasing above model expectations. The most significant change is a 50% increase ($+8\sigma$) in quantitative biology research, all related to the COVID-19 pandemic. Some of these publications are by biologists using arXiv for the first time, and some are written by researchers from other fields (e.g., physicists, mathematicians). While quantitative biology pre-prints have returned to pre-pandemic levels, 20% of the research in this field is now focussed on the COVID-19 pandemic, demonstrating a strong shift in research focus., Comment: Submitted to RSOS
Published: 2021

13. Can we measure the collapse time of a post-merger remnant for a future GW170817-like event?

Author: Easter, Paul J., Lasky, Paul D., and Casey, Andrew R.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology, Astrophysics::Galaxy Astrophysics
Abstract: Measuring the collapse time of a binary neutron star merger remnant can inform the physics of extreme matter and improve modelling of short gamma-ray bursts and associated kilonova. The lifetime of the post-merger remnant directly impacts the mechanisms available for the jet launch of short gamma-ray bursts. We develop and test a method to measure the collapse time of post-merger remnants. We show that for a GW170817-like event at $\sim\!40\,$Mpc, a network of Einstein Telescope with Cosmic Explorer is required to detect collapse times of $\sim\!10\,$ms. For a two-detector network at A+ design sensitivity, post-merger remnants with collapse times of $\sim\!10\,\mathrm{ms}$ must be $\lesssim 10\,$Mpc to be measureable. This increases to $\sim\!18-26\,$Mpc if we include the proposed Neutron star Extreme Matter Observatory (NEMO), increasing the effective volume by a factor of $\sim\!30$., Comment: 9 pages, 3 figures
Published: 2021
Full Text: View/download PDF

14. The impact of the COVID-19 pandemic on academic productivity

Author: Casey, Andrew R., Mandel, Ilya, and Ray, Prasun K.
Subjects: FOS: Computer and information sciences, FOS: Economics and business, General Economics (econ.GN), FOS: Physical sciences, Digital Libraries (cs.DL), Physics and Society (physics.soc-ph)
Abstract: 'Publish or perish' is an expression describing the pressure on academics to consistently publish research to ensure a successful career in academia. With a global pandemic that has changed the world, how has it changed academic productivity? Here we show that academics are posting just as many publications on the arXiv pre-print server as if there were no pandemic: 168,630 were posted in 2020, a +12.6% change from 2019 and $+1.4��$ deviation above the predicted 162,577 $\pm$ 4,393. However, some immediate impacts are visible in individual research fields. Conference cancellations have led to sharp drops in pre-prints, but laboratory closures have had mixed effects. Only some experimental fields show mild declines in outputs, with most being consistent on previous years or even increasing above model expectations. The most significant change is a 50% increase ($+8��$) in quantitative biology research, all related to the COVID-19 pandemic. Some of these publications are by biologists using arXiv for the first time, and some are written by researchers from other fields (e.g., physicists, mathematicians). While quantitative biology pre-prints have returned to pre-pandemic levels, 20% of the research in this field is now focussed on the COVID-19 pandemic, demonstrating a strong shift in research focus., Submitted to RSOS
Published: 2021
Full Text: View/download PDF

15. Groundwater and surface-water data from the C-aquifer monitoring program, Northeastern Arizona, 2012–2019

Author: Casey J. R. Jones and Michael J. Robinson
Subjects: Hydrology, geography, geography.geographical_feature_category, Environmental science, Aquifer, Monitoring program, Surface water, Groundwater
Published: 2021

16. Analysis of Trends in Anxiety in Professional Pharmacy Students

Author: Maroney, Megan, Casey, Emily R, Bhavsar, Nisha, Nadkarni, Neha, Oh, Sarah, and Patel, Romi
Published: 2020
Full Text: View/download PDF

17. Hydrogeologic characterization of the Hualapai Plateau on the western Hualapai Indian Reservation, northwestern Arizona

Author: Casey J. R. Jones, Jon P. Mason, Bruce Gungle, Jamie P. Macy, and Donald J. Bills
Subjects: geography, Hydrogeology, Plateau, geography.geographical_feature_category, Geochemistry, Geology
Published: 2020

18. Geochemical assessment of groundwater in the Big Chino subbasin, Arizona, 2011–18

Author: Kimberly R. Beisner and Casey J. R. Jones
Subjects: Hydrology, Environmental science, Groundwater
Published: 2020

19. Clinical spectrum and prognostic value of CNS MOG autoimmunity in adults

Author: Cobo-Calvo, A., Ruiz, A., Maillart, E., Audoin, B., Zephir, H., Bourre, B., Ciron, J., Collongues, N., Brassat, D., Cotton, F., Papeix, C., Durand-Dubief, F., Laplaud, D., Deschamps, R., Cohen, M., Biotti, D., Ayrignac, X., Tilikete, C., Thouvenot, E., Brochet, B., Dulau, C., Moreau, T., Tourbah, A., Lebranchu, P., Michel, L., Lebrun-Frenay, C., Montcuquet, A., Mathey, G., Debouverie, M., Pelletier, J., Derache, N., Coustans, M., Rollot, F., De Seze, J., Vukusic, S., Marignier, R., Casey, D. R., Maze, D. M., Olaiz, D. J., Frangoulis, D. B., Debard, N., Vukusic, P. S., Zorila, D. C., Debouverie, P. M., Guillemin, P. F., Mathey, D. G., Ziegler, A., Edan, P. G., Le Page, D. E., Leray, D. E., Muraz, R., Brassat, P. D., Clanet, P. M., Peaureaux-Averseng, D. D., Dewas, C., Brochet, P. B., Ouallet, D. J., Ruet, D. A., Kounkou, K. K., De Seze, P. J., Collongues, D. N., Berthe, C., Vermersch, P. P., Hautecoeur, P. P., Deruelle, F., Papeix, D. C., Maillard, D. E., Lubetzki, P. C., Lebrun-Frenay, D. C., Cohen, D. M., Callier, C., Derache, D. N., Droulon, K., Labauge, P. P., Ayrignac, D. X., Carra-Dalliere, D. C., Pinna, F., Moreau, P. T., Fromont, D. A., Protin, A., Michel, D. L., Wiertlewski, D. S., Jousset, N., Berger, D. E., Chamard-Witkowski, D. L., Bereau, D. M., Cappe, C., Clavelou, P. P., Taithe, D. F., Moisset, D. X., Dumont, E., Pelletier, P. J., Audoin, P. B., Rico-Lamy, D. A., Di Lelio, B., Castelnovo, D. G., Stankoff, P. B., Giannesini, D. C., Heinzlef, D. O., Fagniez, D. O., Laage, D. C., Bourre, D. B., Lefaucheur, D. R., Maltete, D. D., Vimont, C., Al Khedr, D. A., Sehaki, S., Gout, D. O., Bensa, D. C., Cabre, P. P., Kasonde, D. I., Galli, P., Magy, P. L., Montcuquet, D. A., Nicol, M., Casez, D. O., Vaillant, D. M., Diop Kane, M., Camdessanche, P. J., Visneux, V., Guennnoc, D. A., Beltran, D. S., Meunier, G., Creange, P. A., Ayache, D. S., Abdellaoui, D. M., Pottier, D. C., Slesari, D. I., Sampaio, M., Deburghraeve?, D. V., Le Port, D., Ciron, D. J., Neau, P. J., Rabois, E., Labeyrie, D. C., Patry, D. I., Lescieux, E., Nifle, D. C., Servan, D. J., Pico, P. F., Chatagner, V., Camus-Jacqmin, D. M., Henry, D. C., Bottin, D. L., Castex, C., Diallo, S. S., Brisset, J. C., Cervenansky, F., Commovick, O., Defer, P. G., Durand-Dubief, D. F., Guttmann, P. C., Tourbah, P. A., Lifticariu, D. C., Constans, D. J., Tanguy, D. J., Dousset, P. V., Tourdias, D. T., Dardel, D. P., Oesterle, D. H., Gonin, D. S., Ricolfi, D. F., Grand, D. S., Krainik, D. A., Boncoeur-Martel, D. M., Ameli, D. R., Bonhomme, D. G., Cotton, P. F., Roch, D. J., Sappey-Marinier, D. D., Brunel, H., Coze, S., Girard, Nicolas, Lehmann, P., Ranjeva, P. J., Menjot De Champfleur, Nicolas, Anxionnat, P. R., Desal, D. H., Mondot, D. L., Savatovsky, D. J., Galanaud, P. D., Pyatigorskaya, D. N., Guillevin, D. R., Pierot, D. L., Barillot, D. C., Ferre, D. J., Bannier, E., Gerardin, D. E., Boutet, D. C., Kremer, D. S., Armspach, P. J., Berry, P. I., Bonneville, P. F., Dufay, N., Zephir, D. H., Gele, P., Marignier, D. R., Fiard, G., Lehmann, S., Lommazi, S., Laplaud, P. D., Gallot, G., Thouvenot, P. E., Fontaine, P. B., Rebeix, I., Desille-Dugast, M., CHU Pitié-Salpêtrière [APHP], Centre de résonance magnétique biologique et médicale (CRMBM), Aix Marseille Université (AMU)-Assistance Publique - Hôpitaux de Marseille (APHM)-Centre National de la Recherche Scientifique (CNRS), Neurologie, maladies neuro-musculaires [Hôpital de la Timone - APHM], Aix Marseille Université (AMU)-Assistance Publique - Hôpitaux de Marseille (APHM)- Hôpital de la Timone [CHU - APHM] (TIMONE), Hôpital de Hautepierre [Strasbourg], Hôpital Purpan [Toulouse], CHU Toulouse [Toulouse], RMN et optique : De la mesure au biomarqueur, Centre de Recherche en Acquisition et Traitement de l'Image pour la Santé (CREATIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Hospices Civils de Lyon (HCL)-Université Jean Monnet [Saint-Étienne] (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Hospices Civils de Lyon (HCL)-Université Jean Monnet [Saint-Étienne] (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Département de Neuroradiologie [Centre Hospitalier Lyon Sud - HCL], Centre Hospitalier Lyon Sud [CHU - HCL] (CHLS), Hospices Civils de Lyon (HCL)-Hospices Civils de Lyon (HCL), Département de Neurologie [Paris], Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-IFR70-CHU Pitié-Salpêtrière [APHP], Department of Neurology, CHU Lyon, Centre Hospitalier Universitaire de Nice (CHU Nice), Département de neurologie [Montpellier], Université Montpellier 1 (UM1)-Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier)-Hôpital Gui de Chauliac [Montpellier]-Université de Montpellier (UM), Centre Hospitalier Régional Universitaire de Nîmes (CHRU Nîmes), Institut de Génomique Fonctionnelle (IGF), Université de Montpellier (UM)-Université Montpellier 1 (UM1)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Centre National de la Recherche Scientifique (CNRS), Neurocentre Magendie, Physiopathologie de la Plasticité Neuronale, U1215, Institut National de la Santé et de la Recherche Médicale (INSERM), Service de Neurologie générale, vasculaire et dégénérative (CHU de Dijon), Centre Hospitalier Universitaire de Dijon - Hôpital François Mitterrand (CHU Dijon), Centre Hospitalier Universitaire de Reims (CHU Reims), 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), Université Nice Sophia Antipolis - Faculté de Médecine (UNS UFR Médecine), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Centre Hospitalier Régional Universitaire de Nancy (CHRU Nancy), Service de Neurologie [Rennes], Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Hôpital Pontchaillou-CHU Pontchaillou [Rennes], Hospices Civils de Lyon (HCL), CIC Strasbourg (Centre d’Investigation Clinique Plurithématique (CIC - P) ), Université de Strasbourg (UNISTRA)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Nouvel Hôpital Civil de Strasbourg-Hôpital de Hautepierre [Strasbourg], Centre de recherche en neurosciences de Lyon (CRNL), Université de Lyon-Université de Lyon-Université Jean Monnet [Saint-Étienne] (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier), Centre hospitalier universitaire de Nantes (CHU Nantes), The Functional Electrical Neuroimaging Laboratory, Université de Lausanne (UNIL), Department of Economics, École Polytechnique, Palaiseau Cedex, 91128, France, affiliation inconnue, Alimentation et sciences sociales (ALISS), Institut National de la Recherche Agronomique (INRA), CHU Marseille, Infections Virales et Pathologie Comparée - UMR 754 (IVPC), Institut National de la Recherche Agronomique (INRA)-École pratique des hautes études (EPHE)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, ISL, Laboratoire Charles Coulomb (L2C), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM), Instituto de Tecnologia Ceramica, Universitat Jaume I, CHU Grenoble, Cellules Souches, Plasticité Cellulaire, Médecine Régénératrice et Immunothérapies (IRMB), Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Montpellier (UM), CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), Assistance Publique - Hôpitaux de Marseille (APHM)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM), Service de Neurologie [CHU Pitié-Salpêtrière], IFR70-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), Centre Hospitalier Universitaire de Nîmes (CHU Nîmes), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Service de Neurologie [Rennes] = Neurology [Rennes], CHU Pontchaillou [Rennes], Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Strasbourg (UNISTRA)-Hôpital de Hautepierre [Strasbourg]-Nouvel Hôpital Civil de Strasbourg, Institut National de la Recherche Agronomique (INRA)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Claude Bernard Lyon 1 (UCBL), Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), Centre de recherche en neurosciences de Lyon - Lyon Neuroscience Research Center (CRNL), Sorbonne Université-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Département de Neurologie [CHU Pitié-Salpêtrière], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-IFR70-CHU Pitié-Salpêtrière [AP-HP], Sorbonne Université-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université, Hôpital Gui de Chauliac [Montpellier]-Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier)-Université Montpellier 1 (UM1)-Université de Montpellier (UM), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), Centre Hospitalier Universitaire de Toulouse (CHU Toulouse), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 1 (UM1)-Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier)-Hôpital Gui de Chauliac [CHU Montpellier], Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier)-Université de Montpellier (UM), Université de Lyon-Université de Lyon-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Université de Lausanne = University of Lausanne (UNIL), Institut National de la Recherche Agronomique (INRA)-École Pratique des Hautes Études (EPHE), Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL), and Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)
Subjects: 0301 basic medicine, medicine.medical_specialty, Visual acuity, [SDV.IB.IMA]Life Sciences [q-bio]/Bioengineering/Imaging, business.industry, Hazard ratio, Encephalopathy, Myelitis, Retrospective cohort study, Lower risk, medicine.disease, 03 medical and health sciences, 030104 developmental biology, 0302 clinical medicine, Internal medicine, medicine, Optic neuritis, Neurology (clinical), medicine.symptom, 10. No inequality, business, ComputingMilieux_MISCELLANEOUS, 030217 neurology & neurosurgery, Survival analysis
Abstract: ObjectiveTo describe clinical and radiologic features associated with myelin oligodendrocyte glycoprotein antibodies (MOG-Ab) in a large French nationwide adult cohort, to assess baseline prognostic features of MOG-Ab-associated diseases after a first acute demyelinating syndrome, and to evaluate the clinical value of MOG-Ab longitudinal analysis.MethodsClinical data were obtained from 197 MOG-Ab-positive patients ≥18 years of age. Complete imaging data were available in 108, and 54 serum samples were eligible for longitudinal evaluation. For survival analysis comparison, 169 aquaporin-4 antibody (AQP4-Ab)-positive patients from the NOMADMUS database were included.ResultsMedian age at onset was 36.46 (range 18.0–76.8) years, and patients were predominantly white (92.9%) with male:female ratio, 1.1. Clinical phenotype at onset included optic neuritis or myelitis in 90.86%, isolated brainstem or encephalopathy syndromes in 6.6%, and a combination of syndromes in 2.5%. Distinctive brain MRI findings in MOG-Ab-positive patients were thalamic and pontine lesions. Cortical and leptomeningeal lesions were found in 16.3% and 6.1%, respectively. The probability of reaching a first relapse after 2 and 5 years was 44.8% and 61.8%, respectively. MOG-Ab-positive patients were at lower risk at presentation of further clinical relapse (hazard ratio [HR] 0.45, 95% confidence interval [CI] 0.26–0.79) compared to AQP4-Ab-positive individuals. MOG-Ab-positive individuals had a lower risk of reaching Disability Status Scale score of 3.0 (HR 0.46, 95% CI 0.22–0.94) and visual acuity of 20/100 (HR 0.23, 95% CI 0.07–0.72). Finally, MOG-Ab titers were higher at relapse than in remission (p = 0.009).ConclusionIn adults, MOG-Ab-associated disease extends beyond clinical and radiologic abnormalities in the optic nerve and spinal cord. Despite the relapsing course, the overall visual and motor outcome is better compared with AQP4-Ab-positive patients.
Published: 2018

20. Characterization and hydraulic behaviour of the complex karst of the Kaibab Plateau and Grand Canyon National Park, USA

Author: Sarah J. Zappitello, Natalie A. Jones, Abraham E. Springer, Casey J. R. Jones, and Benjamin W. Tobin
Subjects: Canyon, Hydrology, geography, geography.geographical_feature_category, Plateau, 010504 meteorology & atmospheric sciences, National park, 0208 environmental biotechnology, Geology, Ocean Engineering, 02 engineering and technology, Karst, 01 natural sciences, 020801 environmental engineering, 0105 earth and related environmental sciences, Water Science and Technology
Published: 2017

21. The Southern Stellar Stream Spectroscopic Survey (S⁵): Overview, Target Selection, Data Reduction, Validation, and Early Science

Author: Li, T S, Koposov, S E, Zucker, D B, Lewis, G F, Kuehn, K, Simpson, J D, Ji, A P, Shipp, N, Mao, Y-Y, Geha, M, Pace, A B, Mackey, A D, Allam, S, Tucker, D L, Da Costa, G S, Erkal, Denis, Simon, J D, Mould, J R, Martell, S L, Wan, Z, De Silva, G M, Bechtol, K, Balbinot, E, Belokurov, V, Bland-Hawthorn, J, Casey, A R, Cullinane, L, Drlica-Wagner, A, Sharma, S, Vivas, A K, Wechsler, R H, and Yanny, B
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We introduce the Southern Stellar Stream Spectroscopy Survey (S⁵), an on-going program to map the kinematics and chemistry of stellar streams in the Southern Hemisphere. The initial focus of S⁵ has been spectroscopic observations of recently identified streams within the footprint of the Dark Energy Survey (DES), with the eventual goal of surveying streams across the entire southern sky. Stellar streams are composed of material that has been tidally striped from dwarf galaxies and globular clusters and hence are excellent dynamical probes of the gravitational potential of the Milky Way, as well as providing a detailed snapshot of its accretion history. Observing with the 3.9-m Anglo-Australian Telescope’s 2-degree-Field fibre positioner and AAOmega spectrograph, and combining the precise photometry of DES DR1 with the superb proper motions from Gaia DR2, allows us to conduct an efficient spectroscopic survey to map these stellar streams. So far S⁵ has mapped 9 DES streams and 3 streams outside of DES; the former are the first spectroscopic observations of these recently discovered streams. In addition to the stream survey, we use spare fibres to undertake a Milky Way halo survey and a low-redshift galaxy survey. This paper presents an overview of the S⁵ program, describing the scientific motivation for the survey, target selection, observation strategy, data reduction and survey validation. Finally, we describe early science results on stellar streams and Milky Way halo stars drawn from the survey. Updates on S⁵, including future public data releases, can be found at http://s5collab.github.io.
Published: 2019

22. SDSS-V pioneering panoptic spectroscopy

Author: Juna Kollmeier, Anderson, S. F., Blanc, G. A., Blanton, M. R., Covey, K. R., Crane, J., Drory, N., Frinchaboy, P. M., Froning, C. S., Johnson, J. A., P Kneib, J., Kreckel, K., Merloni, A., Pellegrini, E. W., Pogge, R. W., Ramirez, S. V., Rix, H. W., Sayres, C., José Sánchez-Gallego, Yue Shen, Tkachenko, A., Trump, J. R., Tuttle, S. E., Anne-Marie Weijmans, Zasowski, G., Barbuy, B., Beaton, R. L., Bergemann, M., Bochanski, J. J., Brandt, W. N., Casey, A. R., Cherinka, B. A., Eracleous, M., Fan, X., García, R. A., Green, P. J., Hekker, S., Lane, R. R., Longa-Peña, P., Mathur, S., Meza, A., Minchev, I., Myers, A. D., Nidever, D. L., Nitschelm, C., Connell, J. E. O., Price-Whelan, A. M., Raddick, M. J., Rossi, G., Sankrit, R., Simon, J. D., Stutz, A. M., S Ting, Y., Trakhtenbrot, B., Weaver, B. A., Willmer, C. N. A., Weinberg, D. H., University of St Andrews. School of Physics and Astronomy, and University of St Andrews. Centre for Contemporary Art
Subjects: NDAS, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: This white paper presents the case for SDSS-V. SDSS-V is an unprecedented all-sky spectroscopic survey of over six million objects. It is designed to decode the history of the Milky Way galaxy, trace the emergence of the chemical elements, reveal the inner workings of galaxies and their stars, and investigate the origin of planets. Publisher PDF Non
Published: 2019

23. The Sloan Digital Sky Survey as an archetypal mid-scale program

Author: Michael Blanton, Anderson, S. F., Basu, S., Beaton, R. L., Bergemann, M., Bershady, M. A., Bochanski, J. J., Brandt, W. N., Brownstein, J., Bundy, K., Casey, A. R., Cherinka, B. A., Covey, K. R., Eracleous, M., Fan, X., Feuillet, D. K., Frinchaboy, P. M., García, R. A., Green, P. J., Johnson, J. A., Jones, A., Knapp, G., P Kneib, J., Kollmeier, J. A., Kreckel, K., Lane, R. R., Longa-Peña, P., Masters, K., Mathur, S., Merloni, A., Meza, A., Minchev, I., Nitschelm, C., Connell, J. E. O., Raddick, M. J., Ramirez, S. V., W Rix, H., Rossi, G., Sankrit, R., Shen, Y., Simon, J. D., Stutz, A. M., S Ting, Y., Trump, J. R., Tuttle, S. E., Anne-Marie Weijmans, Weaver, B. A., Weinberg, D. H., Willmer, C. N. A., Wood-Vasey, W. M., Zasowski, G., University of St Andrews. School of Physics and Astronomy, and University of St Andrews. Centre for Contemporary Art
Subjects: QC Physics, QB Astronomy, 3rd-DAS, QC, QB
Abstract: We describe the Sloan Digital Sky Survey (SDSS) as an archetypal mid-scale program, including the technical, scientific, and organizational aspects underpinning its success over the last twenty years. Based on the SDSS experience, we present six recommendations that the funding mechanisms for mid-scale programs should be designed to ensure the adoption of these recommendations. Publisher PDF Non
Published: 2019

24. HYDROLOGIC CHANGES IN THE C-AQUIFER OF NORTHEASTERN ARIZONA, 2005-2019

Author: Casey J. R. Jones
Subjects: Hydrology, geography, geography.geographical_feature_category, Aquifer, Geology
Published: 2019

25. A Sleep Medicine Curriculum for Pulmonary and Pulmonary/Critical Care Fellowship Programs: A Multisociety Expert Panel Report

Author: Schulman, David A., Piquette, Craig A., Alikhan, Mir M., Freedman, Neil, Kumar, Sunita, McCallister, Jennifer, Mokhlesi, Babak, Santamauro, Jean, Singas, Effie, Stern, Eric, Strohl, Kingman P., and Casey, Kenneth R.
Subjects: Evidence-Based Medicine, Critical Care, Delphi Technique, education, Pulmonary Medicine, Humans, Interdisciplinary Communication, Curriculum, Fellowships and Scholarships, Sleep, Quality Improvement, Education, Sleep Medicine Specialty
Abstract: BACKGROUND: Pulmonary medicine specialists find themselves responsible for the diagnosis and management of patients with sleep disorders. Despite the increasing prevalence of many of these conditions, many sleep medicine fellowship training slots go unfilled, leading to a growing gap between the volume of patients seeking care for sleep abnormalities and the number of physicians formally trained to manage them. To address this need, we convened a multisociety panel to develop a list of curricular recommendations related to sleep medicine for pulmonary fellowship training programs. METHODS: Surveys of pulmonary and pulmonary/critical care fellowship program directors and recent graduates of these programs were performed to assess the current state of sleep medicine education in pulmonary training, as well as the current scope of practice of pulmonary specialists. These data were used to inform a modified Delphi process focused on developing curricular recommendations relevant to sleep medicine. RESULTS: Surveys confirmed that pulmonary medicine specialists are often responsible for the diagnosis and treatment of a number of sleep conditions, including several that are not traditionally considered related to respiratory medicine. Through five rounds of voting, the panel crafted a list of 52 curricular competencies relevant to sleep medicine for recommended inclusion in pulmonary training programs. CONCLUSIONS: Practicing pulmonary specialists require a broad knowledge of sleep medicine to provide appropriate care to patients they will be expected to manage. Training program directors may use the list of competencies as a framework to ensure adequate mastery of important content by graduating fellows.
Published: 2018

26. The Fourteenth Data Release of the Sloan Digital Sky Survey:First Spectroscopic Data from the Extended Baryon Oscillation Spectroscopic Survey and from the Second Phase of the Apache Point Observatory Galactic Evolution Experiment

Author: Abolfathi , Bela, Aguado , D. S., Aguilar , Gabriela, Prieto , Carlos Allende, Almeida , Andres, Ananna , Tonima Tasnim, Anders , Friedrich, Anderson , Scott F., Andrews , Brett H., Anguiano , Borja, Aragon-Salamanca , Alfonso, Argudo-Fernandez , Maria, Armengaud , Eric, Ata , Metin, Aubourg , Eric, Avila-Reese , Vladimir, Badenes , Carles, Bailey , Stephen, Balland , Christophe, Barger , Kathleen A., Barrera-Ballesteros , Jorge, Bartosz , Curtis, Bastien , Fabienne, Bates , Dominic, Baumgarten , Falk, Bautista , Julian, Beaton , Rachael, Beers , Timothy C., Belfiore , Francesco, Bender , Chad F., Bernardi , Mariangela, Bershady , Matthew A., Beutler , Florian, Bird , Jonathan C., Bizyaev , Dmitry, Blanc , Guillermo A., Blanton , Michael R., Blomqvist , Michael, Bolton , Adam S., Boquien , Médéric, Borissova , Jura, Bovy , Jo, Diaz , Christian Andres Bradna, Brandt , William Nielsen, Brinkmann , Jonathan, Brownstein , Joel R., Bundy , Kevin, Burgasser , Adam J., Burtin , Etienne, Busca , Nicolás G., Canas , Caleb I., Cano-Diaz , Mariana, Cappellari , Michele, Carrera , Ricardo, Casey , Andrew R., Sodi , Bernardo Cervantes, Chen , Yanping, Cherinka , Brian, Chiappini , Cristina, Choi , Peter Doohyun, Chojnowski , Drew, Chuang , Chia-Hsun, Chung , Haeun, Clerc , Nicolas, Cohen , Roger E., Comerford , Julia M., Comparat , Johan, Nascimento , Janaina Correa do, da Costa , Luiz, Cousinou , Marie-Claude, Covey , Kevin, Crane , Jeffrey d., Cruz-Gonzalez , Irene, Cunha , Katia, Ilha , Gabriele da Silva, Damke , Guillermo J., Darling , Jeremy, Davidson Jr. , James W., Dawson , Kyle, Lizaola , Miguel Angel C. de Icaza, de la Macorra , Axel, De La Torre , Sylvain, De Lee , Nathan, Agathe , Victoria de Sainte, Machado , Alice Deconto, Dell'Agli , Flavia, Delubac , Timothée, Diamond-Stanic , Aleksandar M., Donor , John, Downes , Juan Jose, Drory , Niv, Bourboux , Hélion du Mas des, Duckworth , Christopher J., Dwelly , Tom, Dyer , Jamie, Ebelke , Garrett, Eigenbrot , Arthur Davis, Eisenstein , Daniel J., Elsworth , Yvonne P., Emsellem , Eric, Eracleous , Mike, Erfanianfar , Ghazaleh, Escoffier , Stéphanie, Fan , Xiaohui, Alvar , Emma Fernandez, Fernandez-Trincado , J. G., Cirolini , Rafael Fernando, Feuillet , Diane, Finoguenov , Alexis, Fleming , Scott W., Font-Ribera , Andreu, Freischlad , Gordon, Frinchaboy , Peter, Fu , Hai, Chew , Yilen Gomez Maqueo, Galbany , Lluis, Perez , Ana E. Garcia, Garcia-Dias , R., García-Hernández , D. A., Oehmichen , Luis Alberto Garma, Gaulme , Patrick, Gelfand , Joseph, Gil-Marin , Hector, Gillespie , Bruce A., Goddard , Daniel, Hernandez , Jonay I. Gonzalez, Gonzalez-Perez , Violeta, Grabowski , Kathleen, Green , Paul J., Grier , Catherine J., Gueguen , Alain, Guo , Hong, Guy , Julien, Hagen , Alex, Hall , Patrick, Harding , Paul, Hasselquist , Sten, Hawley , Suzanne, Hayes , Christian R., Hearty , Fred, Hekker , Saskia, Hernández , Jesús, Toledo , Hector Hernandez, Hogg , David W., Holley-Bockelmann , Kelly, Holtzman , Jon, Hou , Jiamin, Hsieh , Bau-Ching, Hunt , Jason A. S., Hutchinson , Timothy A., Hwang , Ho Seong, Angel , Camilo Eduardo Jimenez, Johnson , Jennifer A., Jones , Amy, Jönsson , Henrik, Jullo , Eric, Khan , Fahim Sakil, Kinemuchi , Karen, Kirkby , David, Kirkpatrick IV , Charles C., Kitaura , Francisco-Shu, Knapp , Gillian R., Kneib , Jean-Paul, Kollmeier , Juna A., Lacerna , Ivan, Lane , Richard R., Lang , Dustin, Law , David R., Goff , Jean-Marc Le, Lee , Young-Bae, Li , Hongyu, Li , Cheng, Lian , Jianhui, Liang , Yu, Lima , Marcos, Lin , Lihwai, Long , Dan, Lucatello , Sara, Lundgren , Britt, Mackereth , J. Ted, MacLeod , Chelsea L., Mahadevan , Suvrath, Maia , Marcio Antonio Geimba, Majewski , Steven, Manchado , Arturo, Maraston , Claudia, Mariappan , Vivek, Marques-Chaves , Rui, Masseron , Thomas, Masters , Karen L., Mcdermid , Richard M., McGreer , Ian D., Melendez , Matthew, Meneses-Goytia , Sofia, Merloni , Andrea, Merrifield , Michael R., Meszaros , Szabolcs, Meza , Andres, Minchev , Ivan, Minniti , Dante, Prieto , Carlos, Ananna , Tonima, Anderson , Scott, Andrews , Brett, Aragón-Salamanca , Alfonso, Argudo-Fernández , Maria, Barger , Kathleen, Beers , Timothy, Bender , Chad, Bershady , Matthew, Bird , Jonathan, Blanc , Guillermo, Blanton , Michael, Bolton , Adam, Andres , Christian, Diaz , Bradna, Brandt , William, Brownstein , Joel, Burgasser , Adam, Busca , Nicolás, Cañas , Caleb, Cano-Díaz , Mariana, Casey , Andrew, Sodi , Bernardo, Choi , Peter, 10 , Davidson, Angel , Miguel, De Icaza Lizaola , C, De Sainte , Victoria, 72 , Agathe, Machado , Alice, Dell 'agli , Flavia, Diamond-Stanic , Aleksandar, Downes , Juan, du Mas des Bourboux , Hélion, Duckworth , Christopher, Davis Eigenbrot , Arthur, Eisenstein , Daniel, Elsworth , Yvonne, Fernández Alvar , Emma, Fernández-Trincado , J., Cirolini , Rafael, Fleming , Scott, Gómez , Yilen, Chew , Maqueo, Galbany , Lluís, García Pérez , Ana, Alberto , Luis, Oehmichen , Garma, Gil-Marín , Héctor, Gillespie , Bruce, González Hernández , Jonay, Green , Paul, Grier , Catherine, Hayes , Christian, Toledo , Hector, Hogg , David, Hunt , Jason, Hutchinson , Timothy, Hwang , Ho, Jimenez Angel , Camilo, Johnson , Jennifer, Fahim , Sakil, Kirkpatrick , Charles, 94 , Iv, Knapp , Gillian, Kollmeier , Juna, Lane , Richard, Law , DAvid, Le Goff , Jean-Marc, Macleod , Chelsea, Antonio , Marcio, Maia , Geimba, Masters , Karen, Mueller , Eva-Maria, Muller-Sanchez , Francisco, Muna , Demitri, Muñoz , Ricardo, Myers , Adam, Nair , Preethi, Nandra , Kirpal, Ness , Melissa, Newman , Jeffrey, Nichol , Robert, Nidever , David, Nitschelm , Christian, Noterdaeme , Pasquier, O 'connell , Julia, Oelkers , Ryan, Oravetz , Audrey, Oravetz , Daniel, Aquino Ortíz , Erik, Osorio , Yeisson, Pace , Zach, Padilla , Nelson, Palanque-Delabrouille , Nathalie, Palicio , Pedro, Pan , Hsi-An, Pan , Kaike, Parikh , Taniya, Pâris , Isabelle, Park , Changbom, Peirani , Sebastien, Pellejero-Ibanez , Marcos, Penny , Samantha, Percival , Will, Perez-Fournon , Ismael, Petitjean , Patrick, Pieri , Matthew, Pinsonneault , Marc, Pisani , Alice, Prada , Francisco, Prakash , Abhishek, Bárbara De Andrade Queiroz , Anna, Raddick , M, Raichoor , Anand, Rembold , Sandro, Richstein , Hannah, Riffel , Rogemar, Riffel , Rogério, Rix , Hans-Walter, Robin , Annie, Torres , Sergio, Román-Zúñiga , Carlos, Ross , Ashley, Rossi , Graziano, Ruan , John, Ruggeri , Rossana, Ruiz , Jose, Salvato , Mara, Sánchez , Ariel, Sanchez , Sebastian, Sanchez Almeida , Jorge, Sánchez-Gallego , José, Antonio , Felipe, Rojas , Santana, Santiago , Basílio, Schiavon , Ricardo, Schimoia , Jaderson, Schlafly , Edward, Schlegel , David, Schneider , Donald, Schuster , William, Schwope , Axel, Seo , Hee-Jong, Serenelli , Aldo, Shen , Shiyin, Shen , Yue, Shetrone , Matthew, Shull , Michael, Aguirre , Silva, Simon , Joshua, Skrutskie , Mike, Slosar , Anže, Smethurst , Rebecca, Smith , Verne, Sobeck , Jennifer, Somers , Garrett, Souter , Barbara, Souto , Diogo, Spindler , Ashley, Stark , David, Stassun , Keivan, Steinmetz , Matthias, Stello , Dennis, Storchi-Bergmann , Thaisa, Streblyanska , Alina, Stringfellow , Guy, Suárez , Genaro, Sun , Jing, Szigeti , Laszlo, Taghizadeh-Popp , Manuchehr, talbot , michael, Tang , Baitian, Tao , Charling, Tayar , Jamie, Tembe , Mita, Teske , Johanna, Aniruddha R. , Thakar, Daniel , Thomas, Tissera , Patricia, Tojeiro , Rita, Tremonti , Christy, Troup , Nicholas W., Urry , Meg, Valenzuela , O., van den Bosch , Remco, Vargas-González , Jaime, Magaña , Mariana Vargas, Vazquez , Jose Alberto, Villanova , Sandro, Vogt , Nicole, Wake , David, Wang , Yuting, Weaver , Benjamin Alan, Weijmans , Anne-Marie, Weinberg , David H., Westfall , Kyle B., Whelan , David G., Wilcots , Eric, Wild , Vivienne, Williams , Rob A., Wilson , John, Wood-Vasey , W.M., Wylezalek , Dominika, Xiao , Ting, Yan , Renbin, Yang , Meng, Ybarra , Jason E., Yèche , Christophe, Zakamska , Nadia, Zamora , Olga, Zarrouk , Pauline, Zasowski , Gail, Zhang , Kai, Zhao , Chang, Zhao , Gong-Bo, Zheng , Zheng, Zhou , Zhi-Min, Zhu , Guangtun, Zinn , Joel C., Zou , Hu, 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), Department of Astrophysical Sciences [Princeton], Princeton University, 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), Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Université Paris Diderot - Paris 7 (UPD7), Department of Physics and Astronomy [Philadelphia], University of Pennsylvania, 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford-University of Oxford, 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), Département de Physique des Particules (ex SPP) (DPhP), 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, European Southern Observatory (ESO), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Departamento de Matemáticas [Madrid], Universidad Autónoma de Madrid (UAM), Department of Physics and Astronomy [Nashville], Vanderbilt University [Nashville], Korea Institute for Advanced Study (KIAS), Sainsbury Laboratory Cambridge University (SLCU), University of Cambridge [UK] (CAM), Wuhan University [China], Equipe de Recherche sur l’Utilisation des Données Individuelles en lien avec la Théorie Economique (ERUDITE), Université Paris-Est Marne-la-Vallée (UPEM)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12), Institute of Astronomy [Cambridge], Max-Planck-Institut für Astrophysik (MPA), Department of Physics and Astronomy [Rochester], University of Rochester [USA], Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Inflammation, Tissus épithéliaux et Cytokines (LITEC), Université de Poitiers, Recherches Epistémologiques et Historiques sur les Sciences Exactes et les Institutions Scientifiques (REHSEIS (UMR_7596)), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Universidad Politécnica de Madrid (UPM), Universidad de Jaén (UJA), Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), University of Edinburgh, Stellar Astrophysics Centre [Aarhus] (SAC), Aarhus University [Aarhus], Alfred P. Sloan Foundation, Department of Energy (US), University of Utah, AVL, AstroParticule et Cosmologie ( APC - UMR 7164 ), 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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Astronomy and Astrophysics ( PENNSYLVANIA STATE UNIVERSITY ), PennState University [Pennsylvania] ( PSU ), Université Paris Diderot - Paris 7 ( UPD7 ), University of Pennsylvania [Philadelphia], 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'Etudes Spatiales ( CNES ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), California Institute of Technology ( CALTECH ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, University of Oxford [Oxford]-University of Oxford [Oxford], Imaging Diagnostic Center, Nanfang Hospital Guangzhou, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid ( UAM ), Centre de Physique des Particules de Marseille ( CPPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Aix Marseille Université ( AMU ), Carnegie Institution of Washington, AUTRES, Département de Physique des Particules (ex SPP) ( DPP ), 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, School of Physics and Astronomy, University of Birmingham [Birmingham], European Southern Observatory ( ESO ), Département de Physique Nucléaire (ex SPhN) ( DPHN ), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules ( UTINAM ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Max-Planck-Institut für Astronomie ( MPIA ), STScI, University of California [Irvine] ( UCI ), ISO Data Centre ( ESA - Espagne ), European Space Agency ( ESA ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Lagrange de Paris, Sorbonne Universités, Research Institute of Forest Resource Information Techniques, Chinese Academy of Forestry, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Korea Institute for Advanced Study ( KIAS ), Department of Astronomy ( Ohio State University ), Ohio State University [Columbus] ( OSU ), Institute of Infection, Immunity & Inflammation, University of Glasgow, Sainsbury Laboratory Cambridge, University of Cambridge [UK] ( CAM ), Equipe de Recherche sur l’Utilisation des Données Individuelles en lien avec la Théorie Economique ( ERUDITE ), Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ) -Université Paris-Est Marne-la-Vallée ( UPEM ), Institute of Physics, Universidade de Brasilia [Brasília] ( UnB ), Department of Chemical and Biomolecular Engineering, University of California [Berkeley], Max-Planck-Institut für Astrophysik ( MPA ), Bioinformatics and Functional Genomics Research Group, Cancer Research Center (IBMCC-CIC, CSIC-USAL), University of Wisconsin-Madison [Madison], Texas Tech University Health Sciences Center, Texas Tech University [Lubbock] ( TTU ), Institute for Astronomy ( IfA ), University of Hawaii, Research Institute of Organic Agriculture ( FiBL ), Dept. of Physics, Princess Margaret Hospital, University of Toronto-Princess Margaret Hospital, J. A. Baker Institute, Cornell University, The Observatories of the Carnegie Institution for Science, Economics, Bangor, Physics Department, Carnegie Mellon University [Pittsburgh] ( CMU ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Inflammation, Tissus épithéliaux et Cytokines ( LITEC ), School of Physics, Korea Institute for Advanced Study, Korea Institute for Advanced Study-Korea Institute for Advanced Study, Recherches Epistémologiques et Historiques sur les Sciences Exactes et les Institutions Scientifiques ( REHSEIS ), Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'astrophysique de l'observatoire de Besançon ( LAOB ), Universidad Politécnica de Madrid ( UPM ), Universidad de Jaén ( UJA ), Institute of Space Sciences [Barcelona] ( ICE-CSIC ), Spanish National Research Council [Madrid] ( CSIC ), Department of Physics and Astronomy - Stellar Astrophysics Centre, Department of Physics, The Leverhulme Trust, University of St Andrews. School of Physics and Astronomy, University of St Andrews. Centre for Contemporary Art, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Département de Physique des Particules (ex SPP) (DPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universidad Autonoma de Madrid (UAM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), University of California [Irvine] (UCI), University of California-University of California, ISO Data Centre (ESA - Espagne), European Space Agency (ESA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), Universidade de Brasilia [Brasília] (UnB), University of Wisconsin-Madison, Texas Tech University [Lubbock] (TTU), Institute for Astronomy [Honolulu] (IfA), University of Hawai'i [Honolulu] (UH), Research Institute of Organic Agriculture (FiBL), University of Toronto, Bangor University, Carnegie Mellon University [Pittsburgh] (CMU), Recherches Epistémologiques et Historiques sur les Sciences Exactes et les Institutions Scientifiques (REHSEIS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), 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 Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Sorbonne Université (SU), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Université Paris-Est Marne-la-Vallée (UPEM), Research Institute of Organic Agriculture - Forschungsinstitut für biologischen Landbau (FiBL), Cornell University [New York], Carnegie Observatories, Carnegie Institution for Science [Washington], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Astrophysics, E-SCIENCE, 01 natural sciences, HISTORIES, TARGET SELECTION, Observatory, QB Astronomy, 010303 astronomy & astrophysics, R2C, QC, media_common, QB, Physics, CATALOGS, Point (typography), ~DC~, Astrophysics::Instrumentation and Methods for Astrophysics, 520 Astronomie und zugeordnete Wissenschaften, atlases, GALAXIES, X-RAY SURVEYS, BDC, Astrophysics - Instrumentation and Methods for Astrophysics, METALLICITY, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], TELESCOPE, media_common.quotation_subject, astro-ph.GA, Phase (waves), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, [ PHYS.ASTR.CO ] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Data-driven, Data cube, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, 0103 physical sciences, ddc:530, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Astronomy and Astrophysics, DAS, 115 Astronomy, Space science, Catalogues, 530 Physik, Astrophysics - Astrophysics of Galaxies, Galaxy, Baryon, QC Physics, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), ddc:520, catalogs, astro-ph.IM, SDSS-IV MANGA
Abstract: Open Access. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI., The fourth generation of the Sloan Digital Sky Survey (SDSS-IV) has been in operation since 2014 July. This paper describes the second data release from this phase, and the 14th from SDSS overall (making this Data Release Fourteen or DR14). This release makes the data taken by SDSS-IV in its first two years of operation (2014-2016 July) public. Like all previous SDSS releases, DR14 is cumulative, including the most recent reductions and calibrations of all data taken by SDSS since the first phase began operations in 2000. New in DR14 is the first public release of data from the extended Baryon Oscillation Spectroscopic Survey; the first data from the second phase of the Apache Point Observatory (APO) Galactic Evolution Experiment (APOGEE-2), including stellar parameter estimates from an innovative data-driven machine-learning algorithm known as ¿The Cannon¿ and almost twice as many data cubes from the Mapping Nearby Galaxies at APO (MaNGA) survey as were in the previous release (N = 2812 in total). This paper describes the location and format of the publicly available data from the SDSS-IV surveys. We provide references to the important technical papers describing how these data have been taken (both targeting and observation details) and processed for scientific use. The SDSS web site (www.sdss.org) has been updated for this release and provides links to data downloads, as well as tutorials and examples of data use. SDSS-IV is planning to continue to collect astronomical data until 2020 and will be followed by SDSS-V. © 2018. The American Astronomical Society.., Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org.
Published: 2018

27. HYDROGEOLOGY OF A PERCHED AND SEMI-CONFINED KARST AQUIFER, KAIBAB PLATEAU, GRAND CANYON

Author: Casey J. R. Jones, Abraham E. Springer, Alexander J. Wood, and Benjamin W. Tobin
Subjects: Canyon, geography, Hydrogeology, geography.geographical_feature_category, Plateau, Aquifer, Karst, Geomorphology, Geology
Published: 2018

28. Cl-/HCO3- exchanger slc26a6: a pH regulator shapes the cardiac action potential

Author: Aiello, Ernesto Alejandro, Casey, Joseph R., and Álvarez, Bernardo Víctor
Subjects: Physiology, Ciencias Médicas, Sarcoplasmic reticulum, Action potentials, Ion transport
Abstract: Regulation of intracellular pH (pHi) is often considered a housekeeping function, contributing little to cardiac contractile activity. With the study published by Sirish et al. in this issue of Circulation: Arrhythmia and Electrophysiology, a Cl-/HCO3- exchanger is revealed to have a more central role in the heart., Facultad de Ciencias Médicas
Published: 2017

29. Coordinated regulation of growth, activity and transcription in natural populations of the unicellular nitrogen-fixing cyanobacterium Crocosphaera

Author: Wilson, Samuel T, Aylward, Frank O, Ribalet, Francois, Barone, Benedetto, Casey, John R, Connell, Paige E, Eppley, John M, Ferrón, Sara, Fitzsimmons, Jessica N, Hayes, Christopher T, Romano, Anna E, Turk-Kubo, Kendra A, Vislova, Alice, Armbrust, E Virginia, Caron, David A, Church, Matthew J, Zehr, Jonathan P, Karl, David M, and DeLong, Edward F
Subjects: Pacific Ocean, Nitrogen, Gene Expression Profiling, Human Genome, Bacterial, Cyanobacteria, Microbiology, Carbon, Carbon Cycle, Bacterial Proteins, Gene Expression Regulation, Medical Microbiology, Nitrogen Fixation, Genetics, Seawater, Metabolic Networks and Pathways
Abstract: © 2017 Macmillan Publishers Limited, part of Springer Nature. All rights reserved. The temporal dynamics of phytoplankton growth and activity have large impacts on fluxes of matter and energy, yet obtaining in situ metabolic measurements of sufficient resolution for even dominant microorganisms remains a considerable challenge. We performed Lagrangian diel sampling with synoptic measurements of population abundances, dinitrogen (N"2) fixation, mortality, productivity, export and transcription in a bloom of Crocosphaera over eight days in the North Pacific Subtropical Gyre (NPSG). Quantitative transcriptomic analyses revealed clear diel oscillations in transcript abundances for 34% of Crocosphaera genes identified, reflecting a systematic progression of gene expression in diverse metabolic pathways. Significant time-lagged correspondence was evident between nifH transcript abundance and maximal N"2 fixation, as well as sepF transcript abundance and cell division, demonstrating the utility of transcriptomics to predict the occurrence and timing of physiological and biogeochemical processes in natural populations. Indirect estimates of carbon fixation by Crocosphaera were equivalent to 11% of net community production, suggesting that under bloom conditions this diazotroph has a considerable impact on the wider carbon cycle. Our cross-scale synthesis of molecular, population and community-wide data underscores the tightly coordinated in situ metabolism of the keystone N"2-fixing cyanobacterium Crocosphaera, as well as the broader ecosystem-wide implications of its activities.
Published: 2017

30. The gaia -ESO survey: calibration strategy

Author: Pancino, E., Lardo, C., Altavilla, G., Marinoni, S., Ragaini, S., Cocozza, G., Bellazzini, M., Sabbi, E., Zoccali, M., Donati, P., Heiter, U., Koposov, S. E., Blomme, R., Morel, T., Símon-Díaz, S., Lobel, A., Soubiran, C., Montalban, J., Valentini, M., Casey, A. R., Blanco-Cuaresma, S., Jofré, P., Worley, C. C., Magrini, L., Hourihane, A., François, P., Feltzing, S., Gilmore, G., Randich, S., Asplund, M., Bonifacio, P., Drew, J. E., Jeffries, R. D., Micela, G., Vallenari, A., Alfaro, E. J., Allende Prieto, C., Babusiaux, C., Bensby, T., angela Bragaglia, Flaccomio, E., Hambly, N., Korn, A. J., Lanzafame, A. C., Smiljanic, R., Eck, S., Walton, N. A., Bayo, A., Carraro, G., Costado, M. T., Damiani, F., Edvardsson, B., Franciosini, E., Frasca, A., Lewis, J., Monaco, L., Morbidelli, L., Prisinzano, L., Sacco, G. G., Sbordone, L., Sousa, S. G., Zaggia, S., Koch, A., Ministero dell'Istruzione, dell'Università e della Ricerca, Knut and Alice Wallenberg Foundation, European Research Council, Swedish National Space Board, Belgian Science Policy Office, National Science Centre (Poland), European Science Foundation, Ministerio de Economía y Competitividad (España), Pancino E., Lardo C., Altavilla G., Marinoni S., Ragaini S., Cocozza G., Bellazzini M., Sabbi E., Zoccali M., Donati P., Heiter U., Koposov S.E., Blomme R., Morel T., Simon-Diaz S., Lobel A., Soubiran C., Montalban J., Valentini M., Casey A.R., Blanco-Cuaresma S., Jofre P., Worley C.C., Magrini L., Hourihane A., Francois P., Feltzing S., Gilmore G., Randich S., Asplund M., Bonifacio P., Drew J.E., Jeffries R.D., Micela G., Vallenari A., Alfaro E.J., Allende Prieto C., Babusiaux C., Bensby T., Bragaglia A., Flaccomio E., Hambly N., Korn A.J., Lanzafame A.C., Smiljanic R., Van Eck S., Walton N.A., Bayo A., Carraro G., Costado M.T., Damiani F., Edvardsson B., Franciosini E., Frasca A., Lewis J., Monaco L., Morbidelli L., Prisinzano L., Sacco G.G., Sbordone L., Sousa S.G., Zaggia S., Koch A., Institut national de recherche et de sécurité (Vandoeuvre lès Nancy) (INRS ( Vandoeuvre lès Nancy)), Royal Observatory of Belgium [Brussels] (ROB), Science et Ingénierie des Matériaux et Procédés (SIMaP ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), M2A 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Leibniz-Institut für Astrophysik Potsdam (AIP), Focas Research Institute, Dublin Institute of Technology, 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), School of Physics, Astronomy and Mathematics [Hatfield], University of Hertfordshire [Hatfield] (UH), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Economía Política y Hacienda Pública, Estadística Económica y Empresarial y Política Económica, Universidad de Castilla-La Mancha (UCLM), Department of Astronomy and Space Physics [Uppsala], Uppsala University, INAF - Osservatorio Astrofisico di Catania (OACT), Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles (ULB), University of Turin, Department of Physiology and Pharmacology, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome]-Réseau International des Instituts Pasteur (RIIP)-Institut Pasteur, Fondation Cenci Bolognetti - Istituto Pasteur Italia, Fondazione Cenci Bolognetti, Réseau International des Instituts Pasteur (RIIP), Pôle Gérontologie, and Centre Hospitalier Universitaire de Nice (CHU Nice)
Subjects: Stars: abundance, Milky Way, FOS: Physical sciences, Techniques: spectroscopic, Astrophysics, Parameter space, Surveys, 01 natural sciences, Spectral line, surveys, 0103 physical sciences, Calibration, Emission spectrum, Survey, 010303 astronomy & astrophysics, Galaxy: general, Solar and Stellar Astrophysics (astro-ph.SR), QC, general [Galaxy], QB, Physics, [PHYS]Physics [physics], Observational error, 010308 nuclear & particles physics, Techniques: radial velocitie, Stars: abundances, Astronomy and Astrophysics, Ranging, radial velocities [techniques], [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, abundances [stars], Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Techniques: radial velocities, stars: abundances, techniques: spectroscopic, techniques: radial velocities, spectroscopic [techniques], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The Gaia-ESO survey (GES) is now in its fifth and last year of observations and has produced tens of thousands of high-quality spectra of stars in all Milky Way components. This paper presents the strategy behind the selection of astrophysical calibration targets, ensuring that all GES results on radial velocities, atmospheric parameters, and chemical abundance ratios will be both internally consistent and easily comparable with other literature results, especially from other large spectroscopic surveys and from Gaia. The calibration of GES is particularly delicate because of (i) the large space of parameters covered by its targets, ranging from dwarfs to giants, from O to M stars; these targets have a large wide of metallicities and also include fast rotators, emission line objects, and stars affected by veiling; (ii) the variety of observing setups, with different wavelength ranges and resolution; and (iii) the choice of analyzing the data with many different state-of-the-art methods, each stronger in a different region of the parameter space, which ensures a better understanding of systematic uncertainties. An overview of the GES calibration and homogenization strategy is also given, along with some examples of the usage and results of calibrators in GES iDR4, which is the fourth internal GES data release and will form the basis of the next GES public data release. The agreement between GES iDR4 recommended values and reference values for the calibrating objects are very satisfactory. The average offsets and spreads are generally compatible with the GES measurement errors, which in iDR4 data already meet the requirements set by the main GES scientific goals.© ESO, 2017., This work was partly supported by the European Union FP7 program through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR) in the form of the grant >Premiale VLT 2012>. The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. S.F. and T.B. acknowledge the support from the New Milky Way project funded by a grant from the Knut and Alice Wallenberg foundation. C.L. gratefully acknowledges financial support from the European Research Council (ERC-CoG-646928, Multi-Pop, PI: N. Bastian). U.H. and A.J.K acknowledge support from the Swedish National Space Board (Rymdstyrelsen). The research of A.L. has been subsidized by the Belgian Federal Science Policy Office under contract No. BR/143/A2/BRASS. R.S. acknowledges support by the National Science Center of Poland through grant 2014/15/B/ST9/03981. C.A.P. is thankful for support from the Spanish Ministry of Economy and Competitiveness (MINECO) through grant AYA2014-56359-P.J.M. acknowledges support from the ERC Consolidator Grant funding scheme (project STARKEY, G.A. No. 615604). T.M. acknowledges financial support from Belspo for contract PRODEX Gaia-DPAC. S.G.S acknowledges the support by Fundacao para a Ciencia e Tecnologia (FCT) through national funds and a research grant (project ref. UID/FIS/04434/2013, and PTDC/FIS-AST/7073/2014). S.G.S. also acknowledge the support from FCT through Investigador FCT contract of reference IF/00028/2014 and POPH/FSE (EC) by FEDER funding through the program >Programa Operacional de Factores de Competitividade - COMPETE>. L.S. acknowledges support by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS). M.Z. acknowledges support by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS), by Fondecyt Regular 1150345 and by the BASAL CATA PFB-06. E.J.A. and M.T.C acknowledge the financial support from the Spanish Ministerio de Economia y Competitividad, through grant AYA2013-40611-P.S.Z. acknowledge the support from the INAF grant >PRIN INAF 2014>, >Star won't tell their ages to Gaia, Galactic Archaelogy with wide-area asterosismic>.
Published: 2017

31. The Gaia-ESO Survey

Author: Pancino, E., Romano, D., Tang, B., Tautvaišienė, G., Casey, A. R., Gruyters, P., Geisler, D., San Roman, I., Randich, S., Alfaro, E. J., Bragaglia, A., Flaccomio, E., Korn, A. J., Recio Blanco, A., Smiljanic, R., Carraro, Giovanni, Bayo, A., Costado, M. T., Damiani, F., Jofré, P., Lardo, C., de Laverny, P., Monaco, L., Morbidelli, L., Sbordone, L., Sousa, S. G., and Villanova, S.
Published: 2017

32. Stellar atmospheric parameters and the Gaia-ESO Survey experience with multiple analysis pipelines

Author: Smiljanic, R., Korn, A. J., Casey, A. R., and consortium, the Gaia-ESO Survey
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: To use libraries of observed stellar spectra, one needs to know the atmospheric parameters of the stars associated to those spectra. It is, however, hard to know what are the real levels of precision and accuracy of these parameters. To overcome this very same problem in a stellar survey, the Gaia-ESO Survey implements a comprehensive calibration effort together with the use of multiple parallel analysis methodologies. Here, we discuss the multiple analyses approach and the effort to understand the accuracy and precision of the provided stellar atmospheric parameters., Comment: 4 pages, 1 figure, to appear in the Proceedings of the International Workshop on Stellar Spectral Libraries 2017 held in Campos de Jordao, Brazil
Published: 2017
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33. The Gaia-ESO Survey: Structural and dynamical properties of the young cluster Chamaeleon i

Author: Sacco, G. G., Spina, L., Randich, S., Palla, F., Parker, J., Jeffries, D., Jackson, R., Meyer, R., Mapelli, M., Lanzafame, C., Bonito, R., Damiani, F., Franciosini, E., Frasca, A., Klutsch, A., Prisinzano, L., Tognelli, E., Degl’Innocenti, S., Prada Moroni, P. G., Alfaro, J., Micela, G., Prusti, T., Barrado, D., Biazzo, K., Bouy, H., Bravi, L., Lopez-Santiago, J., Wright, J., Bayo, A., Gilmore, G., Bragaglia, A., Flaccomio, E., Koposov, S. E., Pancino, E., Casey, A. R., Costado, M. T., Donati, P., Hourihane, A., Jofré, P., Lardo, C., Lewis, J., Magrini, L., Monaco, L., Morbidelli, L., Sousa, S. G., Worley, C. C., Zaggia, S., Parker, R. J., Jeffries, R. D., Meyer, M. R., Lanzafame, A. C., Degl'Innocenti, S., Alfaro, E. J., Wright, N. J., Gilmore, Gerard [0000-0003-4632-0213], Koposov, Sergey [0000-0003-2644-135X], Worley, Clare [0000-0001-9310-2898], Apollo - University of Cambridge Repository, Sacco G.G., Spina L., Randich S., Palla F., Parker R.J., Jeffries R.D., Jackson R., Meyer M.R., Mapelli M., Lanzafame A.C., Bonito R., Damiani F., Franciosini E., Frasca A., Klutsch A., Prisinzano L., Tognelli E., Degl'Innocenti S., Prada Moroni P.G., Alfaro E.J., Micela G., Prusti T., Barrado D., Biazzo K., Bouy H., Bravi L., Lopez-Santiago J., Wright N.J., Bayo A., Gilmore G., Bragaglia A., Flaccomio E., Koposov S.E., Pancino E., Casey A.R., Costado M.T., Donati P., Hourihane A., Jofre P., Lardo C., Lewis J., Magrini L., Monaco L., Morbidelli L., Sousa S.G., Worley C.C., Zaggia S., Ministero dell'Istruzione, dell'Università e della Ricerca, Istituto Nazionale di Astrofisica, European Research Council, Fundação para a Ciência e a Tecnologia (Portugal), Pôle Gérontologie, Centre Hospitalier Universitaire de Nice (CHU Nice), Muséum national d'Histoire naturelle (MNHN), Watershed Associates Ltd, Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Istituto Nazionale di Astrofisica (INAF), University of Turin, INAF - Osservatorio Astrofisico di Catania (OACT), Economía Política y Hacienda Pública, Estadística Económica y Empresarial y Política Económica, Universidad de Castilla-La Mancha (UCLM), INAF - Osservatorio Astronomico di Palermo (OAPa), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), INAF - Osservatorio Astrofisico di Arcetri (OAA), M2A 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Synchrotron Radiation Facility (ESRF), Focas Research Institute, Dublin Institute of Technology, Institut national de recherche et de sécurité (Vandoeuvre lès Nancy) (INRS ( Vandoeuvre lès Nancy)), Hitotsubashi University, Department of Physiology and Pharmacology, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome]-Réseau International des Instituts Pasteur (RIIP)-Institut Pasteur, Fondation Cenci Bolognetti - Istituto Pasteur Italia, Fondazione Cenci Bolognetti, Réseau International des Instituts Pasteur (RIIP), Universidade de Sao Paulo, Instituto Ocenografico, Department of Microbiology and Molecular Genetics, Michigan State University [East Lansing], Michigan State University System-Michigan State University System, Université libre de Bruxelles (ULB), and Newcastle University [Newcastle]
Subjects: astro-ph.SR, Stellar population, open clustersand associations: individual: Chamaeleon I, Individual: Chamaeleon I [Open clusters and associations], Open clusters and associations: Individual: Chamaeleon I, Stars: Kinematics and dynamics, Stars: Pre-main sequence, Techniques: Spectroscopic, astro-ph.GA, stars: kinematics and dynamics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, stars: pre-main sequence, 01 natural sciences, Virial theorem, Kinematics and dynamics [Stars], Stars: Kinematics and dynamic, 0103 physical sciences, Cluster (physics), Mass segregation, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, QC, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB, Physics, Pre-main sequence [Stars], open clusters and associations: individual: Chamaeleon I, 010308 nuclear & particles physics, Velocity dispersion, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], techniques: spectroscopic, Star cluster, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Spectroscopic [Techniques], Equivalent width, QB799
Abstract: Investigating the physical mechanisms driving the dynamical evolution of young star clusters is fundamental to our understanding of the star formation process and the properties of the Galactic field stars. The young (~2 Myr) and partially embedded cluster Chamaeleon I is one of the closest laboratories for the study of the early stages of star cluster dynamics in a low-density environment. The aim of this work is to study the structural and kinematical properties of this cluster combining parameters from the high-resolution spectroscopic observations of the Gaia-ESO Survey with data from the literature. Our main result is the evidence of a large discrepancy between the velocity dispersion (σ = 1.14 ± 0.35 km s) of the stellar population and the dispersion of the pre-stellar cores (~0.3 km s) derived from submillimeter observations. The origin of this discrepancy, which has been observed in other young star clusters, is not clear. It has been suggested that it may be due to either the effect of the magnetic field on the protostars and the filaments or to the dynamical evolution of stars driven by two-body interactions. Furthermore, the analysis of the kinematic properties of the stellar population puts in evidence a significant velocity shift (~1 km s) between the two subclusters located around the north and south main clouds of the cluster. This result further supports a scenario where clusters form from the evolution of multiple substructures rather than from a monolithic collapse. Using three independent spectroscopic indicators (the gravity indicator γ, the equivalent width of the Li line at 6708 Å, and the Hα 10% width), we performed a new membership selection. We found six new cluster members all located in the outer region of the cluster, proving that Chamaeleon I is probably more extended than previously thought. Starting from the positions and masses of the cluster members, we derived the level of substructure Q, the surface density Σ, and the level of mass segregation Λ of the cluster. The comparison between these structural properties and the results of N-body simulations suggests that the cluster formed in a low-density environment, in virial equilibrium or a supervirial state, and highly substructured.© 2017 ESO., This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR) in the form of the grant >Premiale VLT 2012>. This work has been partially supported by PRIN-INAF-2014. The results presented here benefited from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. M.M. acknowledges financial support from the Italian Ministry of Education, University and Research (MIUR) through grant FIRB 2012 RBFR12PM1F, from INAF through grant PRIN-2014-14, and from the MERAC Foundation. S.G.S. acknowledges the support by Fundacao para a Ciencia e Tecnologia (FCT) through national funds and a research grant (project Ref. UID/FIS/04434/2013, and PTDC/FIS-AST/7073/2014). S.G.S. also acknowledge the support from FCT through Investigador FCT contract of reference IF/00028/2014 and POPH/FSE (EC) by FEDER funding through the program Programa Operacional de Factores de Competitividade COMPETE.
Published: 2017

34. SDSS-V: Pioneering Panoptic Spectroscopy

Author: Kollmeier, Juna A., Zasowski, Gail, Rix, Hans-Walter, Johns, Matt, Anderson, Scott F., Drory, Niv, Johnson, Jennifer A., Pogge, Richard W., Bird, Jonathan C., Blanc, Guillermo A., Brownstein, Joel R., Crane, Jeffrey D., Lee, Nathan M., Klaene, Mark A., Kreckel, Kathryn, Macdonald, Nick, Merloni, Andrea, Ness, Melissa K., O Brien, Thomas, Sanchez-Gallego, Jose R., Sayres, Conor C., Shen, Yue, Thakar, Ani R., Andrew Casey, Aerts, Conny, Blanton, Michael R., Eisenstein, Daniel J., Holtzman, Jon A., Maoz, Dan, Nandra, Kirpal, Rockosi, Constance, Weinberg, David H., Bovy, Jo, Casey, Andrew R., Chaname, Julio, Clerc, Nicolas, Conroy, Charlie, Eracleous, Michael, Gänsicke, Boris T., Hekker, Saskia, Horne, Keith, Kauffmann, Jens, Mcquinn, Kristen B. W., Pellegrini, Eric W., Schinnerer, Eva, Schlafly, Edward F., Schwope, Axel D., Seibert, Mark, Teske, Johanna K., and Saders, Jennifer L.
Subjects: Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: SDSS-V will be an all-sky, multi-epoch spectroscopic survey of over six million objects. It is designed to decode the history of the Milky Way, trace the emergence of the chemical elements, reveal the inner workings of stars, and investigate the origin of planets. It will also create an integral-field spectroscopic map of the gas in the Galaxy and the Local Group that is 1,000x larger than the current state of the art and at high enough spatial resolution to reveal the self-regulation mechanisms of galactic ecosystems. SDSS-V will pioneer systematic, spectroscopic monitoring across the whole sky, revealing changes on timescales from 20 minutes to 20 years. The survey will thus track the flickers, flares, and radical transformations of the most luminous persistent objects in the universe: massive black holes growing at the centers of galaxies. The scope and flexibility of SDSS-V will be unique among extant and future spectroscopic surveys: it is all-sky, with matched survey infrastructures in both hemispheres; it provides near-IR and optical multi-object fiber spectroscopy that is rapidly reconfigurable to serve high target densities, targets of opportunity, and time-domain monitoring; and it provides optical, ultra-wide-field integral field spectroscopy. SDSS-V, with its programs anticipated to start in 2020, will be well-timed to multiply the scientific output from major space missions (e.g., TESS, Gaia, eROSITA) and ground-based projects. SDSS-V builds on the 25-year heritage of SDSS's advances in data analysis, collaboration infrastructure, and product deliverables. The project is now refining its science scope, optimizing the survey strategies, and developing new hardware that builds on the SDSS-IV infrastructure. We present here an overview of the current state of these developments as we seek to build our worldwide consortium of institutional and individual members., Comment: 23-page summary of the current status of SDSS-V. See also http://www.sdss.org/future/. SDSS-V is currently seeking institutional and individual members -- join us!
Published: 2017
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35. Nasopharyngeal Bacterial Interactions in Children

Author: Xu, Qingfu, Almudervar, Anthony, Casey, Janet R., and Pichichero, Michael E.
Subjects: nasopharyngeal bacterial infections, Microbiology (medical), Staphylococcus aureus, polymicrobial colonization, Epidemiology, lcsh:Medicine, bacterial interaction, Biology, medicine.disease_cause, Article, Pneumococcal conjugate vaccine, lcsh:Infectious and parasitic diseases, Microbiology, Haemophilus influenzae, Moraxella catarrhalis, children, Moraxella (Branhamella) catarrhalis, CME, Streptococcus pneumoniae, otorhinolaryngologic diseases, Heptavalent Pneumococcal Conjugate Vaccine, medicine, lcsh:RC109-216, bacteria, Respiratory tract infections, Research, acute otitis media, lcsh:R, Environmental exposure, biology.organism_classification, Infectious Diseases, Immunology, medicine.drug
Abstract: TOC summary: Pathogen prevalence differs during periods of health and at onset of acute otitis media., Antimicrobial treatments and vaccines can alter bacterial interactions in the nasopharynx, thereby altering disease processes. To better understand these interactions, we examined colonization rates of 3 respiratory bacterial pathogens among 320 children when healthy and at onset of acute otitis media (AOM). Bacterial interactions were analyzed with a repeated measures logistic regression model. Among healthy children, Streptococcus pneumoniae and Moraxella catarrhalis were synergistically (positively) associated. Colonization with S. pneumoniae when healthy, but not at onset of AOM, was competitively (negatively) associated with Staphylococcus aureus. Among children with AOM, competitive associations were found between Haemophilus influenzae and S. pneumoniae and between H. influenzae and M. catarrhalis; rates of colonization with H. influenzae were higher. Bacterial interactions result in differing pathogen prevalence during periods of health and at onset of AOM. H. influenzae might become a more common cause of AOM among children who receive pneumococcal conjugate vaccine.
Published: 2012

36. How much can we trust high-resolution spectroscopic stellar atmospheric parameters?

Author: Blanco-Cuaresma, Sergi, Nordlander, Thomas, Heiter, Ulrike, Jofré, Paula, Masseron, Thomas, Casamiquela, Laia, Tabernero, Hugo M., Bhat, Shruthi S., Casey, Andrew R., Meléndez, Jorge, Ramírez, Ivan, and Feiden, Gregory A.
Subjects: stars, spectroscopy, radiative codes, Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: The determination of atmospheric parameters depends on the use of radiative transfer codes (among other elements such as model atmospheres) to compute synthetic spectra and/or derive abundances from equivalent widths. However, it is common to mix results from different surveys/studies where different setups were used to derive the parameters. These inhomogeneities can lead us to inaccurate conclusions. In this work, we studied one aspect of the problem: When deriving atmospheric parameters from high-resolution stellar spectra, what differences originate from the use of different radiative transfer codes?, To appear in the 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun proceeding
Published: 2016

37. The RAVE-on catalog of stellar atmospheric parameters and chemical abundances for chemo-dynamic studies in the Gaia era

Author: Casey, Andrew R
Abstract: The orbits, atmospheric parameters, chemical abundances, and ages of individual stars in the Milky Way provide the most comprehensive illustration of galaxy formation available. The Tycho-Gaia Astrometric Solution (TGAS) will deliver astrometric parameters for the largest ever sample of Milky Way stars, though its full potential cannot be realized without the addition of complementary spectroscopy. Among existing spectroscopic surveys, the RAdial Velocity Experiment (RAVE) has the largest overlap with TGAS (~206,000 stars). We present a data-driven re-analysis of 520,781 RAVE spectra using The Cannon. For red giants, we build our model using high-fidelity APOGEE stellar parameters and abundances for stars that overlap with RAVE. For main-sequence and sub-giant stars, our model uses stellar parameters from the K2/EPIC. We derive and validate effective temperature, surface gravity, and chemical abundances of up to seven elements (O, Mg, Al, Si, Ca, Fe, Ni). We report a total of 1,685,851 elemental abundances with a typical precision of 0.07 dex, a substantial improvement over previous RAVE data releases. The synthesis of RAVE-on and TGAS is the most powerful data set for chemo-dynamic analyses of the Milky Way ever produced.
Published: 2016
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38. Emerging Streptococcus pneumoniae Strains Colonizing the Nasopharynx in Children after 13-Valent (PCV13) Pneumococcal Conjugate Vaccination in Comparison to the 7-Valent (PCV7) Era, 2006-2015

Author: Kaur, Ravinder, Casey, Janet R., and Pichichero, Michael E.
Subjects: Male, Heptavalent Pneumococcal Conjugate Vaccine, Vaccination, Infant, Serogroup, Article, Pneumococcal Infections, Anti-Bacterial Agents, Pneumococcal Vaccines, Streptococcus pneumoniae, Child, Preschool, Nasopharynx, Carrier State, Drug Resistance, Bacterial, Humans, Female
Abstract: After introduction of the 7-valent pneumococcal conjugate vaccine (PCV7) in the United States in 2000, emergence of replacement serotypes occurred, leading to the introduction of a 13-valent pneumococcal conjugate vaccine (PCV13) in 2010 that contained all PCV7 serotypes plus 6 additional serotypes (1, 3, 5, 6A, 7F and 19A). Here, we describe a 9-year prospective, longitudinal study characterizing Streptococcus pneumoniae strains colonizing the nasopharynx (NP) of young children based on serotype, sequence type (ST) and antibiotic susceptibility during the PCV7 and PCV13 eras.NP samples were obtained for pneumococcal identification from prospectively followed children at 6, 9, 12, 15, 18, 24 and 30 months of age. A total of 1072 visits during the PCV7 era (June 2006 to September 2010) and 2044 visits during the PCV13 era (October 2010 to September 2015) were included from 665 children. Serotyping and multilocus sequence typing types of Streptococcus pneumoniae isolates were evaluated along with their antibiotic resistance pattern.A total of 1045 Streptococcus pneumoniae were isolated; 350 during the PCV7 era and 685 during the PCV13 era. The most common serotypes identified during the PCV7 era were 19A and 23B compared with 35B, 23B and 21 in PCV13 era. Serotypes 15A/B/C emerged in equal proportion during the PCV13 era. Serotypes 16 and 20 were only observed in the PCV13 era. NP carriage of 19A persisted 5 years after PCV13 introduction (5% of all isolates). Multilocus ST 199 remained a dominant ST during both the PCV7 and PCV13 eras, and ST558 and ST62 emerged after PCV13. Antibiotic resistance to penicillin, ceftriaxone, cefotaxime, erythromycin, tetracycline and trimethoprim/sulfamethoxazole significantly decreased from the PCV7 to the PCV13 era.Serotypes 35B, 23B, 21 and 15A/B/C rapidly emerged as NP colonizers in the early PCV13 era. Genetically divergent strains with ST558 and ST62 emerged. Resistance to common antibiotics declined after the introduction of PCV13.
Published: 2016

39. The Gaia-ESO Survey: A simple explanation for the Li-rich giant problem

Author: Casey, Andrew R., Ruchti, G., Masseron, T., Randich, S., Gilmore, G., Lind, K., Grant Kennedy, Smiljanic, R., Jofre, P., Hourihane, A., Bragaglia, A., Donati, P., Koposov, S. E., Worley, C. C., Lanzafame, A., Franciosini, E., Lewis, J. R., Magrini, L., Morbidelli, L., Sacco, G. G., Bensby, T., Carraro, G., Damiani, F., Feltzing, S., Jeffries, R. D., Korn, A. J., Lardo, C., Laverny, P., Delgado Mena, E., Costado, M. T., Flaccomio, E., Frasca, A., Monaco, L., Pancino, E., Prisinzano, L., Recio-Blanco, A., Sbordone, L., Sousa, S. G., Tautvaisiene, G., Vallenari, A., Zaggia, S., Zwitter, T., Silva Aguirre, V., Chorniy, Y., Martell, S. L., Miglo, A., Chiappini, C., Montalban, J., Morel, T., and Valentini, M.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The discovery of lithium-rich giants contradicts expectations from canonical stellar evolution. Although multiple scenarios have been proposed to preserve or produce Li, no model can explain the ensemble properties of Li-rich giants. We report on the serendipitous discovery of 20 Li-rich giants observed through the Gaia-ESO Survey. Our sample is one of the largest in the literature, and includes nine towards the CoRoT fields. We explore all mechanisms proposed to explain Li-rich giants. While the planet accretion scenario was presented to reconcile observations of Li-rich giants across the RGB/AGB, this is inconsistent with recent studies of close-in giant planets. We highlight recent observations of the difference in hot Jupiter occurrence rates around dwarf and sub-giant stars as evidence for their tidal destruction when the convective envelope expands. Therefore any close-in giant planet is likely to be engulfed well before the host evolves up the RGB/AGB. When this occurs, simulations indicate a giant planet will provide a small reservoir of unburnt Li to replenish the stellar photospheric abundance, and subsequently induce deep mixing to produce additional Li. We argue these two independent lines of evidence actually predict the existence of Li-rich giants, and suggests they should be preferentially found before the luminosity bump at near-solar metallicities, consistent with observations. This scenario explains (indeed, predicts) the majority properties of Li-rich giants, leaving a minority population of evolved metal-poor Li-rich giants which are explainable by internal mixing processes associated with late evolutionary stages, or mass transfer from more evolved AGB stars.
Published: 2016

40. UTILIZING KARST RESEARCH TO INFORM THE NEPA PROCESS AT GRAND CANYON NATIONAL PARK

Author: Benjamin W. Tobin, Edward R. Schenk, Casey J. R. Jones, Abraham E. Springer, and Hampton Childres
Subjects: Canyon, geography, geography.geographical_feature_category, National park, business.industry, Environmental protection, Process (engineering), Environmental resource management, Environmental science, business, Karst
Published: 2016

41. Chemistry of the Most Metal-poor Stars in the Bulge and the z > 10 Universe

Author: Casey, Andrew R. and Schlaufman, Kevin C.
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::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Metal-poor stars in the Milky Way are local relics of the epoch of the first stars and the first galaxies. However, a low metallicity does not prove that a star formed in this ancient era, as metal-poor stars form over a range of redshift in different environments. Theoretical models of Milky Way formation have shown that at constant metallicity, the oldest stars are those closest to the center of the Galaxy on the most tightly-bound orbits. For that reason, the most metal-poor stars in the bulge of the Milky Way provide excellent tracers of the chemistry of the high-redshift universe. We report the dynamics and detailed chemical abundances of three stars in the bulge with [Fe/H] $\lesssim-2.7$, two of which are the most metal-poor stars in the bulge in the literature. We find that with the exception of scandium, all three stars follow the abundance trends identified previously for metal-poor halo stars. These three stars have the lowest [Sc II/Fe] abundances yet seen in $��$-enhanced giant stars in the Galaxy. Moreover, all three stars are outliers in the otherwise tight [Sc II/Fe]-[Ti II/Fe] relation observed among metal-poor halo stars. Theoretical models predict that there is a 30% chance that at least one of these stars formed at $z\gtrsim15$, while there is a 70% chance that at least one formed at $10 \lesssim z \lesssim 15$. These observations imply that by $z\sim10$, the progenitor galaxies of the Milky Way had both reached [Fe/H] $\sim-3.0$ and established the abundance pattern observed in extremely metal-poor stars., Submitted to ApJ on 2014 December 23, accepted 2015 May 4th after minor revisions. ArXiv tarball includes referee report and response
Published: 2015
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42. Media and the Coverage of Psychiatry

Author: Halder, Neel, Niazi, A., Ahmed, Z., and Casey, Patricia R.
Subjects: Media, Stigma, England, Tabloids, Physical health, Broadsheets, Mental health, Newspapers, Ireland
Abstract: Background and aim: Psychiatric issues have often been a focus for the media. Studies have differed in their findings about how the subject matter is portrayed in newspapers.We compared tone and content of Irish print with the British, broadsheets and tabloids, and the coverage of physical and mental illness. Methods: A selection of Irish and British broadsheet and tabloid newspapers were examined page by page by researchers for period of 6 months. Various parameters investigated including who the authors were, commenting on the tone, focus and topic of the articles. A comparison of the parameters between the two countries was made. Results: The total numbers of newspapers studied in six months were 579. In comparison the tone of heading and article was neutral for both Irish and English articles. The tone was more negative (and sensationlist) on tabloids compared to dailies and Sunday newpapers. Predominantly for articles related to mental and physical illnesses tone of headline and article itself was neutral in daily and Sunday broadsheets and dramatic in daily tabloids. Conclusions: To ensure accuracy of information and a more balanced article, we feel more articles should be written by health care professionals themselves, especially for tabloids. Databases now exist where journalists can contact the health care professionals for various illnesses.
Published: 2014

43. The Role of a Neuropsychiatry Clinic in a Tertiary Referral Teaching Hospital: A Two-Year Study

Author: Jabbar, Faraz, Doherty, Anne, Duffy, R., Aziz, M., Casey, Patricia R., Sheehan, John D., Lynch, T., and Kelly, Brendan D.
Subjects: Psychiatry, Mental disorder, Neurology, Mental health services, Neuropsychiatry, Liaison psychiatry
Abstract: Objectives: Mental disorder is common among individuals with neurological illness. We aimed to characterise the patient population referred for psychiatry assessment at a tertiary neurology service in terms of neurological and psychiatric diagnoses and interventions provided. Methods: We studied all individuals referred for psychiatry assessment at a tertiary neurology service over a 2-year period (n= 82). Results: The most common neurological diagnoses among those referred were epilepsy (16%), Parkinson’s disease (15%) and multiple sclerosis (8%). The most common reasons for psychiatric assessment were low mood or anxiety (48%) and medically unexplained symptoms or apparent functional or psychogenic disease (21%). The most common diagnoses among those with mental disorder were mood disorders (62%), and neurotic, stress-related and somatoform disorders, including dissociative (conversion) disorders (28%). Psychiatric diagnosis was not related to gender, neurological diagnosis or psychiatric history. Conclusion: Individuals with neurological illness demonstrate significant symptoms of a range of mental disorders. There is a need for further research into the characteristics and distribution of mental disorder in individuals with neurological illness, and for the enhancement of integrated psychiatric and neurological services to address the comorbidities demonstrated in this population.
Published: 2014

44. A Tale of Tidal Tails in the Milky Way

Author: Casey, Andrew R., Keller, Stefan C, Da Costa, Gary, and Schmidt, Brian P
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astronomy, Stellar streams, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Hundreds of globular clusters and dwarf galaxies encircle the Milky Way. Many of these systems have undergone partial disruption due to tidal forces, littering the halo with stellar streams. These tidal tails are sensitive to the Galactic potential, facilitating an excellent laboratory to investigate Galaxy formation and evolution, as well as local chemical signatures of differing star formation environments. To better understand the emergence of the Milky Way, this thesis examines the dynamics and chemistry of a number of known stellar streams., Comment: PhD thesis
Published: 2014
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45. Astropy: A Community Python Package for Astronomy

Author: The Astropy Collaboration, Robitaille, Thomas P., Tollerud, Erik J., Greenfield, Perry, Droettboom, Michael, Bray, Erik, Aldcroft, Tom, Davis, Matt, Ginsburg, Adam, Price-Whelan, Adrian M., Kerzendorf, Wolfgang E., Conley, Alexander, Crighton, Neil, Barbary, Kyle, Muna, Demitri, Ferguson, Henry, Grollier, Fr��d��ric, Parikh, Madhura M., Nair, Prasanth H., G��nther, Hans M., Deil, Christoph, Woillez, Julien, Conseil, Simon, Kramer, Roban, Turner, James E. H., Singer, Leo, Fox, Ryan, Weaver, Benjamin A., Zabalza, Victor, Edwards, Zachary I., Bostroem, K. Azalee, Burke, D. J., Casey, Andrew R., Crawford, Steven M., Dencheva, Nadia, Ely, Justin, Jenness, Tim, Labrie, Kathleen, Lim, Pey Lian, Pierfederici, Francesco, Pontzen, Andrew, Ptak, Andy, Refsdal, Brian, Servillat, Mathieu, Streicher, Ole, The Astropy Collaboration, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Point spread function, 010308 nuclear & particles physics, Computer science, Coordinate system, virtual observatory tools, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Python (programming language), Virtual observatory, File format, methods: data analysis, 01 natural sciences, 3. Good health, Space and Planetary Science, methods: miscellaneous, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, computer, Instrumentation and Methods for Astrophysics (astro-ph.IM), computer.programming_language
Abstract: We present the first public version (v0.2) of the open-source and community-developed Python package, Astropy. This package provides core astronomy-related functionality to the community, including support for domain-specific file formats such as Flexible Image Transport System (FITS) files, Virtual Observatory (VO) tables, and common ASCII table formats, unit and physical quantity conversions, physical constants specific to astronomy, celestial coordinate and time transformations, world coordinate system (WCS) support, generalized containers for representing gridded as well as tabular data, and a framework for cosmological transformations and conversions. Significant functionality is under active development, such as a model fitting framework, VO client and server tools, and aperture and point spread function (PSF) photometry tools. The core development team is actively making additions and enhancements to the current code base, and we encourage anyone interested to participate in the development of future Astropy versions., Comment: Accepted for publication in Astronomy and Astrophysics. For more information about Astropy, visit http://www.astropy.org
Published: 2013

46. I'm spiritual but not religious : Implications for research and practice

Author: Casey, Patricia R.
Subjects: Religion, Psychiatry, Spirituality
Abstract: There is an assumption, amongst some mental health service users, clinicians, researchers and others, that religiousness and spirituality are the same construct. A consideration of the history of these concepts shows that, over time, each has become separated from the other. Both require careful definition. The definitions of spirituality are heterogeneous and, with important implications for research and practice, some encompass mood states. The failure to separate spirituality and religiousness, and the confounding of spirituality with mood states in some research in psychiatry, makes interpretation of the findings difficult. Greater clarity and precision will be required in future research including, if possible, attempts to provide distinctive operational definitions of spirituality and religiousness.
Published: 2013

47. The 300km/s stellar stream near Segue 1: Insights From high-resolution spectroscopy of its brightest star

Author: Frebel, Anna, Lunnan, Ragnhild, Casey, Andrew R., Norris, John E., Wyse, Rosemary F. G., and Gilmore, Gerard
Subjects: Astrophysics - Solar and Stellar Astrophysics, 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, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present a chemical abundance analysis of 300S-1, the brightest likely member star of the 300 km/s stream near the faint satellite galaxy Segue 1. From a high-resolution Magellan/MIKE spectrum we determine a metallicity of [Fe/H] = -1.46 +- 0.05 +- 0.23 (random and systematic uncertainties) for star 300S-1, and find an abundance pattern similar to typical halo stars at this metallicity. Comparing our stellar parameters to theoretical isochrones, we estimate a distance of 18 +- 7 kpc. Both the metallicity and distance estimates are in good agreement with what can be inferred from comparing the SDSS photometric data of the stream stars to globular cluster sequences. While several other structures overlap with the stream in this part of the sky, the combination of kinematic, chemical and distance information makes it unlikely that these stars are associated with either the Segue 1 galaxy, the Sagittarius stream or the Orphan stream. Streams with halo-like abundance signatures, such as the 300 km/s stream, present another observational piece for understanding the accretion history of the Galactic halo., Comment: 13 pages, emulateapj, accepted for publication in ApJ
Published: 2013
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48. Comparison of Amoxicillin/Clavulanate High Dose to Cefdinir in Treatment of Acute Otitis Media

Author: Casey, Janet R., Block, Stan, Hedrick, Jim, Almudevar, Anthony, and Pichichero, Michael E.
Subjects: Cefdinir, Infant, Amoxicillin-Potassium Clavulanate Combination, Article, Drug Administration Schedule, Anti-Bacterial Agents, Cephalosporins, Otitis Media, Treatment Outcome, Acute Disease, Humans, Single-Blind Method, Prospective Studies, Follow-Up Studies
Abstract: 10 days of amoxicillin/clavulanic acid high dose and 5 days of cefdinir have been the preferred first- or second-line antibiotics for treatment of children with acute otitis media (AOM) since 2004, as recommended by the American Academy of Pediatrics in the USA, but no head-to-head comparison study has been done.The purpose of the study was to compare the clinical efficacy of amoxicillin/clavulanic acid high-dose therapy for 10 days with cefdinir therapy for 5 days for AOM at recommended doses.This was an investigator-blind trial in young children 6-24 months old with no history of recurrent AOM who were randomly assigned to amoxicillin/clavulanic acid (80 mg/kg/day amoxicillin) or cefdinir (14 mg/kg/day), both in two divided doses. The diagnosis of AOM was based on specific clinical criteria by validated otoscopists at two AOM research centres. The outcome measure for clinical cure was resolution of all symptoms and signs of AOM except for persistence of middle-ear effusion at test-of-cure (TOC) 11-14 days after initiation of antibiotic treatment. Clinical failure was defined as persistence of symptoms and signs of AOM and the need for additional antibiotic therapy. Subjects lost to follow up or who had not taken at least 80% of the prescribed medication were classified as having an indeterminate response. Compliance was monitored using Medical Electronic Monitoring System (MEMS) caps and antibiotic bottle volume measurement at the TOC visit. A logistic regression model was used to estimate the association of age with cure rate. Full interactions in terms of age with treatment were included to estimate any age gradient differential.A total of 330 children (average age 13.1 months) with AOM were studied. At TOC, 256 children had clinical cure, 69 had clinical failure, and 5 were lost to follow-up. High-dose amoxicillin/clavulanic acid-treated children had a better cure rate (86.5%) than cefdinir-treated patients (71.0%; p = 0.001). Cefdinir was correlated with less frequent cure outcomes as children increased in age between 6 and 24 months. The odds ratios for clinical cure per increasing month of age estimated from a logistic regression model for amoxicillin/clavulanic acid high dose and cefdinir treatment groups was 0.992 (95% CI 0.932, 1.056), p 0.05 and 0.932 (95% CI 0.881, 0.986), p = 0.01. The differences in the odds ratios are significant at p 0.002, indicating a stable clinical cure rate across the ages of children studied for amoxicillin/clavulanic acid and decreasing clinical cure rates as children increased in age for cefdinir.In children with bona fide AOM for whom clinical outcomes are assessed by validated otoscopists, 10 days of high-dose amoxicillin/clavulanic acid is significantly more effective than 5 days of cefdinir as therapy for AOM. Because of the identified age effect (correlated to child weight), higher doses of cefdinir may have led to a different conclusion; 10 days of cefdinir may also have led to a different conclusion.
Published: 2012

49. Kinematics & Chemistry of Halo Substructures: The Vicinity of the Virgo Over-Density

Author: Casey, A. R., Keller, S. C., and Da Costa, G.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present observations obtained with the AAT's 2dF wide field spectrograph AAOmega of K-type stars located within a region of the sky which contains the Virgo Over-Density and the leading arm of the Sagittarius Stream. On the basis of the resulting velocity histogram we isolate halo substructures in these overlapping regions including Sagittarius and previously discovered Virgo groups. Through comparisons with N-body models of the Galaxy-Sagittarius interaction, we find a tri-axial dark matter halo is favoured and we exclude a prolate shape. This result is contradictory with other observations along the Sagittarius leading arm, which typically favour prolate models. We have also uncovered K-giant members of Sagittarius that are notably more metal poor ([Fe/H] = -1.7 +/- 0.3 dex) than previous studies. This suggests a significantly wider metallicity distribution exists in the Sagittarius Stream than formerly considered. We also present data on five carbon stars which were discovered in our sample., accepted to AJ
Published: 2012
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50. Value network orchestration of a cognitive radio platform

Author: Taparia, Ankit, Basaure, Arturo, and Casey, Thomas R.
Subjects: ddc:330
Abstract: Mobile communication industry has taken over path of platformisation in terms of service provisioning leading to emergence of different platforms. These service oriented platforms have opened up otherwise closed and vertically integrated mobile industry. However in terms of spectrum licensing and usage market structure is still relatively closed and cognitive radio (CR) technology is expected to be at forefront to solve these issues. With development of CR technologies new stakeholders are expected to emerge and join existing market players resulting in the development of a multi-sided platform. In this paper we introduce spectrum database driven CR platform as an integral part of CR ecosystem. We visualize its architecture in form of set of layered and interconnected platforms. Higher layer platform for services catering to end-users, lower layer platform for different CR access technologies and a generic CR protocol in between binding these layered platforms. In order to understand how to orchestrate the value network for different stakeholders to participate in this CR platform, we conducted interviews and identified that stakeholders are in principle willing to move out of their silos and think holistically in terms of CR platform. However political uncertainties and regulatory indecision happens to be major cause of concern hampering stakeholders to make required investments. Also observed that regulators are in position to orchestrate CR market place since their actions influence market, market participants and technology. Thus regulators are required to take steps in direction which promotes harmonization of CR technologies and prevent a fragmented scenario where none of CR solutions attain required critical mass.
Published: 2012

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