1,929 results on '"Driver, Simon"'
Search Results
352. Deepest Near-IR Surface Photometry of Galaxies in the Local Sphere of Influence
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Kirby, Emma, Jerjen, Helmut, Ryder, Stuart, Driver, Simon, Jerjen, H., editor, and Koribalski, Bärbel Silvia, editor
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- 2008
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353. MEASURING STRUCTURAL PROPERTIES OF GALAXIES IN THE LOCAL UNIVERSE
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Allen, Paul D., Driver, Simon P., Liske, Jochen, Graham, Alister W., and DE JONG, R. S., editor
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- 2007
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354. Intensity of overground robotic exoskeleton training in two persons with motor-complete tetraplegia: a case series.
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Bosteder, Katelyn D., Moore, Ashlyn, Weeks, Ariana, Dawkins, Jonathan D., Trammell, Molly, Driver, Simon, Hamilton, Rita, and Swank, Chad
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- 2023
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355. Physical activity and perceived barriers in individuals with moderate‐to‐severe traumatic brain injury.
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Pham, Tri, Green, Rachel, Neaves, Stephanie, Hynan, Linda S., Bell, Kathleen R., Juengst, Shannon B., Zhang, Rong, Driver, Simon, and Ding, Kan
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BRAIN injuries ,PHYSICAL activity ,OLDER people ,MIDDLE-aged persons ,AGE groups - Abstract
Introduction: Regular physical activity (PA), especially aerobic exercise, may benefit cognitive function in middle‐aged and older adults, but promoting regular PA in individuals with traumatic brain injury (TBI) remains a challenge. Objective: To characterize PA and perceived barriers to PA in younger (<45 years) and middle age and older (≥45 years) individuals ≥1 year after moderate‐to‐severe TBI. Design: Multicenter survey study. Setting: Community. Participants: Persons who met the following criteria were included in the study: (1) 18 years and older; (2) English speaking; (3) History of moderate‐to‐severe TBI; (4) Followed in a TBI Model Systems Center for at least 1 year; and (5) Able to complete the survey independently. Intervention: Not applicable. Main Outcome Measure(s): PA level measured by Rapid Assessment of Physical Activity questionnaire (RAPA) and self‐reported barriers to PA. Results: A total of 472 participants completed the survey (response rate of 21%). More individuals in the younger group (<45 years old) met Centers for Disease Control and Prevention (CDC) recommended aerobic PA guidelines compared to the middle‐aged and older group (≥ 45 years old) (62% vs 36%, p <.001). Lack of motivation, lack of time, and fatigue were the most reported barriers. Perceived barriers to PA varied by age and PA level: the middle‐aged and older individuals (≥ 45 years old) were more likely to report no barriers and inactive individuals (RAPA ≤5) more likely to report lack of motivation and money, pain, and lack of resources. Conclusion: Participants ≥45 years of age were less likely to meet the CDC PA guidelines than younger individuals after moderate‐to‐severe TBI. Because perceived barriers to PA varied between age groups and PA levels, individualized approaches may be needed to promote PA in this population. [ABSTRACT FROM AUTHOR]
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- 2023
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356. Galaxy And Mass Assembly (GAMA): Data Release 4 and the z < 0.1 total and z < 0.08 morphological galaxy stellar mass functions
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Driver, Simon P., Bellstedt, Sabine, Robotham, Aaron S.G., Baldry, Ivan K., Davies, Luke J., Liske, Jochen, Obreschkow, Danail, Taylor, Edward N., Wright, Angus H., Alpaslan, Mehmet, Bamford, Steven P., Bauer, Amanda E., Bland-Hawthorn, Joss, Bilicki, Maciej, Brough, Sarah, Casura, Sarah, Cluver, Michelle E., Colless, Matthew, Conselice, Christopher J., Croom, Scott M., Dogruel, Burak, Drinkwater, Michael J., Dvornik, Andrej, Farrow, Daniel J., Frenk, Carlos S., Giblin, Benjamin, Graham, Alister W., Grootes, Meiert W., Gunawardhana, Madusha L.P., Hashemizadeh, Abdolhosein, Heymans, Catherine, Hildebrandt, Hendrik, Holwerda, Benne W., Hopkins, Andrew M., Jarrett, Tom H., Kelvin, Lee S., Koushan, Soheil, Kuijken, Konrad, Lange, Rebecca, Loveday, Jon, Mahajan, Smriti, Meyer, Martin, Moffett, Amanda J., Napolitano, Nicola R., Norberg, Peder, Owers, Matt S., Radovich, Mario, Raouf, Mojtaba, Peacock, John A., Phillipps, Steven, Pimbblet, Kevin A., Popescu, Cristina, Said, Khaled, Sansom, Anne E., Seibert, Mark, Sutherland, Will J., Thorne, Jessica E., Tuffs, Richard J., Turner, Ryan, and Wilkins, Steve M.
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Space and Planetary Science ,Astronomy and Astrophysics - Abstract
In Galaxy And Mass Assembly Data Release 4 (GAMA DR4), we make available our full spectroscopic redshift sample. This includes 248 682 galaxy spectra, and, in combination with earlier surveys, results in 330 542 redshifts across five sky regions covering ∼250 deg2. The redshift density, is the highest available over such a sustained area, has exceptionally high completeness (95 per cent to rKiDS = 19.65 mag), and is well-suited for the study of galaxy mergers, galaxy groups, and the low redshift (z < 0.25) galaxy population. DR4 includes 32 value-added tables or Data Management Units (DMUs) that provide a number of measured and derived data products including GALEX, ESO KiDS, ESO VIKING, WISE, and HerschelSpace Observatory imaging. Within this release, we provide visual morphologies for 15 330 galaxies to z < 0.08, photometric redshift estimates for all 18 million objects to rKiDS ∼25 mag, and stellar velocity dispersions for 111 830 galaxies. We conclude by deriving the total galaxy stellar mass function (GSMF) and its sub-division by morphological class (elliptical, compact-bulge and disc, diffuse-bulge and disc, and disc only). This extends our previous measurement of the total GSMF down to 106.75 M$⊙, h70-2 and we find a total stellar mass density of ρ∗ = (2.97 ± 0.04) × 108 M⊙ h70 Mpc-3 or Ω *=(2.17 ± 0.03) × 10-3, h70-1. We conclude that at z < 0.1, the Universe has converted 4.9 ± 0.1 per cent of the baryonic mass implied by big bang Nucleosynthesis into stars that are gravitationally bound within the galaxy population.
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- 2022
357. Bulges in a cosmological context
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Driver, Simon
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Galaxy bulges - Abstract
Review presentation at the ESO Bulges 2022 online conference.
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- 2022
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358. Physical activity and perceived barriers in individuals with moderate‐to‐severe traumatic brain injury
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Pham, Tri, primary, Green, Rachel, additional, Neaves, Stephanie, additional, Hynan, Linda S., additional, Bell, Kathleen R., additional, Juengst, Shannon B., additional, Zhang, Rong, additional, Driver, Simon, additional, and Ding, Kan, additional
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- 2022
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359. Efficacy of the Diabetes Prevention Program Group Lifestyle Balance Program Modified for Individuals with TBI (GLB-TBI): Results from a 12-month Randomized Controlled Trial
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Driver, Simon, primary, McShan, Evan, additional, Swank, Chad, additional, Calhoun, Stephanie, additional, Bennett, Monica, additional, Callender, Librada, additional, Holden, Alexandria, additional, Juengst, Shannon, additional, Bell, Kathleen, additional, Douglas, Megan, additional, Kramer, Kaye, additional, and Dubiel, Randi, additional
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- 2022
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360. Foundational ingredients of robotic gait training for people with incomplete spinal cord injury during inpatient rehabilitation (FIRST): A randomized controlled trial protocol
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Swank, Chad, primary, Holden, Alexandria, additional, McDonald, Lacy, additional, Driver, Simon, additional, Callender, Librada, additional, Bennett, Monica, additional, and Sikka, Seema, additional
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- 2022
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361. Systematic Framework to Classify the Status of Research on Spinal Cord Injury and Physical Activity
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Nery, Mara B., Driver, Simon, and Vanderbom, Kerri A.
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- 2013
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362. Review of the Status of Physical Activity Research for Individuals With Traumatic Brain Injury
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Pawlowski, Jill, Dixon-Ibarra, Alicia, and Driver, Simon
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- 2013
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363. The Global, Local and Cluster Galaxy Luminosity Function
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Driver, Simon, De Propris, Roberto, Lobo, Catarina, editor, Serote Roos, Margarida, editor, and Biviano, Andrea, editor
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- 2003
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364. Development of a Conceptual Model to Predict Physical Activity Participation in Adults with Brain Injuries
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Driver, Simon
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The purpose was to examine psychosocial factors that influence the physical activity behaviors of adults with brain injuries. Two differing models, based on Harter's model of self-worth, were proposed to examine the relationship between perceived competence, social support, physical self-worth, affect, and motivation. Adults numbering 384 with brain injuries completed a series of questionnaires measuring each psychosocial variable. The structural analysis indicated a nonsignificant chi squared value and good fit indices for model two which included affect as the mediating variable. Findings indicate that affect is critical in shaping the physical activity cognitions and behaviors of adults with brain injuries. Suggestions are made on practical ways to enhance affect and subsequently physical activity participation. (Contains 2 tables and 2 figures.)
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- 2008
365. The Evolution of Ellipticals, Spirals and Irregulars: Overcoming Selection Bias
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Driver, Simon, Cristiani, Stefano, editor, Renzini, Alvio, editor, and Williams, Robert E., editor
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- 2001
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366. An empirical measurement of the Halo Mass Function from the combination of GAMA DR4, SDSS DR12, and REFLEX II data
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Driver, Simon P., Robotham, Aaron S. G., Obreschkow, Danail, Peacock, John A., Baldry, Ivan K., Bellstedt, Sabine, Bland-Hawthorn, Joss, Brough, Sarah, Cluver, Michelle, Holwerda, Benne W., Hopkins, Andrew, Lagos, Claudia, Liske, Jochen, Loveday, Jon, Phillipps, Steven, Taylor, Edward N., Driver, Simon P., Robotham, Aaron S. G., Obreschkow, Danail, Peacock, John A., Baldry, Ivan K., Bellstedt, Sabine, Bland-Hawthorn, Joss, Brough, Sarah, Cluver, Michelle, Holwerda, Benne W., Hopkins, Andrew, Lagos, Claudia, Liske, Jochen, Loveday, Jon, Phillipps, Steven, and Taylor, Edward N.
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We construct the halo mass function (HMF) from the GAMA galaxy group catalogue over the mass range 10^12.7M_sol to 10^15.5M_sol, and find good agreement with the expectation from LambdaCDM. In comparison to previous studies, this result extends the mass range over which the HMF has now been measured over by an order of magnitude. We combine the GAMA DR4 HMF with similar data from the SDSS DR12 and REFLEX II surveys, and fit a four-parameter Murray-Robotham-Power (MRP) function, valid at z~0.1, yielding: a density normalisation of: log10 (phi Mpc^3)=-3.96[+0.55,-0.82], a high mass turn-over of: log10(M/M_sol)=14.13[+0.43,-0.40], a low mass power law slope of: alpha=-1.68[+0.21,-0.24] , and a high mass softening parameter of: beta= 0.63[+0.25,-0.11]. If we fold in the constraint on Omega_M from Planck 2018 Cosmology, we are able to reduce these uncertainties further, but this relies on the assumption that the power-law trend can be extrapolated from 10^12.7M_sol to zero mass. Throughout, we highlight the effort needed to improve on our HMF measurement: improved halo mass estimates that do not rely on calibration to simulations; reduced halo mass uncertainties needed to mitigate the strong Eddington Bias that arises from the steepness of the HMF low mass slope; and deeper wider area spectroscopic surveys. To our halo mass limit of 10^12.7 M_sol, we are directly resolving (`seeing') 41+/-5 per cent of the total mass density, i.e. Omega_[M>12.7]=0.128+/-0.016, opening the door for the direct construction of 3D dark matter mass maps at Mpc resolution., Comment: Accepted for publication in MNRAS
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- 2022
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367. The challenge of measuring and mapping the missing baryons
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Driver, Simon P. and Driver, Simon P.
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The missing baryon problem may now be resolved, but the exact location and physical properties of the diffuse component remains unclear. This problem could be tractable, but requires the combination of new galaxy redshift surveys with new X-ray and radio facilities., Comment: Published as a Comment in Nature Astronomy, August 2021, see also supporting article in Nature Portfolio: https://astronomycommunity.nature.com/videos/waves-deep
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- 2022
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368. Deep Extragalactic VIsible Legacy Survey (DEVILS): The emergence of bulges and decline of disk growth since $z = 1$
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Hashemizadeh, Abdolhosein, Driver, Simon P., Davies, Luke J. M., Robotham, Aaron S. G., Bellstedt, Sabine, Windhorst, Rogier A., Jarvis, Matt, Holwerda, Benne W., Siudek, Malgorzata, Foster, Caroline, Phillipps, Steven, Thorne, Jessica E., Wolf, Christian, Hashemizadeh, Abdolhosein, Driver, Simon P., Davies, Luke J. M., Robotham, Aaron S. G., Bellstedt, Sabine, Windhorst, Rogier A., Jarvis, Matt, Holwerda, Benne W., Siudek, Malgorzata, Foster, Caroline, Phillipps, Steven, Thorne, Jessica E., and Wolf, Christian
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The majority of the stellar mass in the Universe today resides in galaxies with two primary structural components (bulge and disk). In this work, we use the largest contiguous HST imaging region (COSMOS), the Deep Extragalactic VIsible Legacy Survey (DEVILS), and the galaxy structural fitting code {\sc ProFit}, to deconstruct $\sim 35,000$ galaxies into their sub-structures. We use this sample to determine the stellar mass density (SMD) sub-divided by structural components and its evolution since $z = 1$. We find that the majority of stellar mass at all epochs lies in disk-like structures. The SMD in the disk population increases in $z = 1-0.35$ and stabilizes/decreases to $z = 0$ (contributing $\sim 60\%$ to the total SMD at $z = 1$ and declining to $\sim 30\%$ at $z = 0$). This decline is countered by a rapid rise of the SMD in pseudo-bulge population and a consistent growth of spheroidal structures (classical bulges and ellipticals) with significant stellar mass growth in $z = 1-0.35$ and a somewhat flattened trend to $z = 0$. While the physical mechanisms for this are not obvious, the results are consistent with a transition from a Universe dominated by disk growth, to a Universe in which pseudo-bulges are emerging and spheroids are growing. Further study is required before this can be apportioned to internal secular processes, gas accretion, minor and major mergers. However, it is clear that since $z = 0.35$ the processes mentioned above now dominate over quiescent disk growth as the cosmic star-formation history declines.
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- 2022
369. The eROSITA Final Equatorial Depth Survey (eFEDS): X-ray emission around star-forming and quiescent galaxies at $0.05<z<0.3$
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Comparat, Johan, Truong, Nhut, Merloni, Andrea, Pillepich, Annalisa, Ponti, Gabriele, Driver, Simon, Bellstedt, Sabine, Liske, Joe, Aird, James, Brüggen, Marcus, Bulbul, Esra, Davies, Luke, Villalba, Justo Antonio González, Georgakakis, Antonis, Haberl, Frank, Liu, Teng, Maitra, Chandreyee, Nandra, Kirpal, Popesso, Paola, Predehl, Peter, Robotham, Aaron, Salvato, Mara, Thorne, Jessica E., Zhang, Yi, Comparat, Johan, Truong, Nhut, Merloni, Andrea, Pillepich, Annalisa, Ponti, Gabriele, Driver, Simon, Bellstedt, Sabine, Liske, Joe, Aird, James, Brüggen, Marcus, Bulbul, Esra, Davies, Luke, Villalba, Justo Antonio González, Georgakakis, Antonis, Haberl, Frank, Liu, Teng, Maitra, Chandreyee, Nandra, Kirpal, Popesso, Paola, Predehl, Peter, Robotham, Aaron, Salvato, Mara, Thorne, Jessica E., and Zhang, Yi
- Abstract
We aim at characterizing the hot phase of the Circum-Galactic Medium in a large sample of galaxies. We stack X-ray events from the SRG/eROSITA eFEDS survey around central galaxies in the GAMA 9hr field to construct radially projected soft X-ray luminosity profiles as a function of their stellar mass and specific star formation rate. We consider samples of quiescent (star-forming) galaxies in the stellar mass range $2\times 10^{10}$ -- $10^{12}$ M$_\odot$ ($3\times 10^9$ -- $6\times10^{11}$ M$_\odot$). For quiescent galaxies, the X-ray profiles are clearly extended throughout the available mass range; however, the measured profile is likely biased high due to projection effects, as these galaxies tend to live in dense and hot environments. For the most massive star forming samples ($\geq10^{11}$ M$_\odot$), there is a hint of detection of extended emission. For star-forming galaxies with $< 10^{11}$ M$_\odot$ the X-ray stacked profiles are compatible with unresolved sources and consistent with the expected emission from faint Active Galactic Nuclei and X-ray binaries. We measure for the first time the mean relation between average X-ray luminosity and stellar mass separately for quiescent and star-forming galaxies. High-mass ($\geq 10^{11}$ M$_\odot$) star-forming or quiescent galaxies follow the expected scaling of virialized hot haloes, while lower mass star-forming galaxies show a less prominent luminosity and a weaker dependence on stellar mass, consistent with empirical models of the weak AGN population. When comparing our results with state-of-the art numerical simulations, we find an overall consistency on large ($>80$ kpc) scales at masses $\geq 10^{11}$ M$_\odot$, but disagreement on the small scales, where brighter than observed compact cores are predicted. Simulations also do not predict the clear differentiation that we observe between quiescent and star-forming galaxies., Comment: 23 pages, 14 figures, 5 tables, submitted to A&A
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- 2022
370. The variation of the gas content of galaxy groups and pairs compared to isolated galaxies
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Roychowdhury, Sambit, Meyer, Martin J., Rhee, Jonghwan, Zwaan, Martin A., Chauhan, Garima, Davies, Luke J. M., Bellstedt, Sabine, Driver, Simon P., Lagos, Claudia del P., Robotham, Aaron S. G., Bland-Hawthorn, Joss, Dodson, Richard, Holwerda, Benne W., Hopkins, Andrew M., Lara-Lopez, Maritza A., Lopez-Sanchez, Angel R., Obreschkow, Danail, Rozgonyi, Kristof, Whiting, Matthew T., Wright, Angus H., Roychowdhury, Sambit, Meyer, Martin J., Rhee, Jonghwan, Zwaan, Martin A., Chauhan, Garima, Davies, Luke J. M., Bellstedt, Sabine, Driver, Simon P., Lagos, Claudia del P., Robotham, Aaron S. G., Bland-Hawthorn, Joss, Dodson, Richard, Holwerda, Benne W., Hopkins, Andrew M., Lara-Lopez, Maritza A., Lopez-Sanchez, Angel R., Obreschkow, Danail, Rozgonyi, Kristof, Whiting, Matthew T., and Wright, Angus H.
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We measure how the atomic gas (HI) fraction ($f_{HI}={\rm \frac{M_{HI}}{M_{*}}}$) of groups and pairs taken as single units vary with average stellar mass ($\langle {\rm M_*} \rangle$) and average star-formation rate ($\langle {\rm SFR} \rangle$), compared to isolated galaxies. The HI 21 cm emission observation are from (i) archival ALFALFA survey data covering three fields from the GAMA survey (provides environmental and galaxy properties), and (ii) DINGO pilot survey data of one of those fields. The mean $f_{HI}$ for different units (groups/pairs/isolated galaxies) are measured in regions of the log($\langle {\rm M_*} \rangle$) -- log($\langle {\rm SFR} \rangle$) plane, relative to the z $\sim 0$ star-forming main sequence (SFMS) of individual galaxies, by stacking $f_{HI}$ spectra of individual units. For ALFALFA, $f_{HI}$ spectra of units are measured by extracting HI spectra over the full groups/pair areas and dividing by the total stellar mass of member galaxies. For DINGO, $f_{HI}$ spectra of units are measured by co-adding HI spectra of individual member galaxies, followed by division by their total stellar mass. For all units the mean $f_{HI}$ decreases as we move to higher $\langle {\rm M_*} \rangle$ along the SFMS, and as we move from above the SFMS to below it at any $\langle {\rm M_*} \rangle$. From the DINGO-based study, mean $f_{HI}$ in groups appears to be lower compared to isolated galaxies for all $\langle {\rm M_*} \rangle$ along the SFMS. From the ALFALFA-based study we find substantially higher mean $f_{HI}$ in groups compared to isolated galaxies (values for pairs being intermediate) for ${\langle{\rm M_*}\rangle}\lesssim10^{9.5}~{\rm M_{\odot}}$, indicating the presence of substantial amounts of HI not associated with cataloged member galaxies in low mass groups., Comment: Accepted for publication in ApJ. Main text: 26 pages, 16 figures, 6 tables
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- 2022
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371. The LEGA-C and SAMI Galaxy Surveys:Quiescent Stellar Populations and the Mass-Size Plane across 6 Gyr
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Barone, Tania M., D'Eugenio, Francesco, Scott, Nicholas, Colless, Matthew, Vaughan, Sam P., Wel, Arjen van der, Fraser-McKelvie, Amelia, Graaff, Anna de, Sande, Jesse van de, Wu, Po-Feng, Bezanson, Rachel, Brough, Sarah, Bell, Eric, Croom, Scott M., Cortese, Luca, Driver, Simon, Gallazzi, Anna R., Muzzin, Adam, Sobral, David, Bland-Hawthorn, Joss, Bryant, Julia J., Goodwin, Michael, Lawrence, Jon S., Lorente, Nuria P. F., Owers, Matt S., Barone, Tania M., D'Eugenio, Francesco, Scott, Nicholas, Colless, Matthew, Vaughan, Sam P., Wel, Arjen van der, Fraser-McKelvie, Amelia, Graaff, Anna de, Sande, Jesse van de, Wu, Po-Feng, Bezanson, Rachel, Brough, Sarah, Bell, Eric, Croom, Scott M., Cortese, Luca, Driver, Simon, Gallazzi, Anna R., Muzzin, Adam, Sobral, David, Bland-Hawthorn, Joss, Bryant, Julia J., Goodwin, Michael, Lawrence, Jon S., Lorente, Nuria P. F., and Owers, Matt S.
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We investigate the change in mean stellar population age and metallicity ([Z/H]) scaling relations for quiescent galaxies from intermediate redshift ($0.60\leq z\leq0.76$) using the LEGA-C Survey, to low redshift ($0.014\leq z\leq0.10$) using the SAMI Galaxy Survey. We find that, similarly to their low-redshift counterparts, the stellar metallicity of quiescent galaxies at $0.60\leq z\leq 0.76$ closely correlates with $M_*/R_\mathrm{e}$ (a proxy for the gravitational potential or escape velocity), in that galaxies with deeper potential wells are more metal-rich. This supports the hypothesis that the relation arises due to the gravitational potential regulating the retention of metals, by determining the escape velocity required by metal-rich stellar and supernova ejecta to escape the system and avoid being recycled into later stellar generations. On the other hand, we find no correlation between stellar age and $M_*/R_\mathrm{e}^2$ (stellar mass surface density $\Sigma$) in the LEGA-C sample, despite this being a strong relation at low redshift. We consider this change in the age--$\Sigma$ relation in the context of the redshift evolution of the star-forming and quiescent populations in the mass--size plane, and find our results can be explained as a consequence of galaxies forming more compactly at higher redshifts, and remaining compact throughout their evolution. Furthermore, galaxies appear to quench at a characteristic surface density that decreases with decreasing redshift. The $z\sim 0$ age--$\Sigma$ relation is therefore a result of building up the quiescent and star-forming populations with galaxies that formed at a range of redshifts and so a range of surface densities.
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- 2022
372. JWST's PEARLS: TN J1338-1942 -- I. Extreme jet triggered star-formation in a $z=4.11$ luminous radio galaxy
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Duncan, Kenneth J., Windhorst, Rogier A., Koekemoer, Anton M., Röttgering, Huub J. A., Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Tompkins, Scott, Hutchison, Taylor A., Conselice, Christopher J., Driver, Simon P., Yan, Haojing, Adams, Nathan J., Cheng, Cheng, Coe, Dan, Diego, Jose M., Dole, Hervé, Frye, Brenda, Gim, Hansung B., Grogin, Norman A., Holwerda, Benne W., Lim, Jeremy, Marshall, Madeline A., Nonino, Mario, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Duncan, Kenneth J., Windhorst, Rogier A., Koekemoer, Anton M., Röttgering, Huub J. A., Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Tompkins, Scott, Hutchison, Taylor A., Conselice, Christopher J., Driver, Simon P., Yan, Haojing, Adams, Nathan J., Cheng, Cheng, Coe, Dan, Diego, Jose M., Dole, Hervé, Frye, Brenda, Gim, Hansung B., Grogin, Norman A., Holwerda, Benne W., Lim, Jeremy, Marshall, Madeline A., Nonino, Mario, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., and Willmer, Christopher N. A.
- Abstract
We present the first JWST observations of the $z=4.11$ luminous radio galaxy TN J1338-1942, obtained as part of the ``Prime Extragalactic Areas for Reionization and Lensing Science'' (``PEARLS'') project. Our NIRCam observations, designed to probe the key rest-frame optical continuum and emission line features at this redshift, enable resolved spectral energy distribution modelling that incorporates both a range of stellar population assumptions and radiative shock models. With an estimated stellar mass of $\log_{10}(M/\text{M}_{\odot}) \sim 10.9$, TN J1338--1942 is confirmed to be one of the most massive galaxies known at this epoch. Our observations also reveal extremely high equivalent-width nebular emission coincident with the luminous AGN jets that is best fit by radiative shocks surrounded by extensive recent star-formation. We estimate the total star-formation rate (SFR) could be as high as $\sim1600\,\text{M}_{\odot}\,\text{yr}^{-1}$, with the SFR that we attribute to the jet induced burst conservatively $\gtrsim500\,\text{M}_{\odot}\,\text{yr}^{-1}$. The mass-weighted age of the star-formation, $t_{\text{mass}} <4$ Myr, is consistent with the likely age of the jets responsible for the triggered activity and significantly younger than that measured in the core of the host galaxy. The extreme scale of the potential jet-triggered star-formation activity indicates the potential importance of positive AGN feedback in the earliest stages of massive galaxy formation, with our observations also illustrating the extraordinary prospects for detailed studies of high-redshift galaxies with JWST., Comment: 17 pages, 15 figures, Accepted for publication in MNRAS after minor revisions
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- 2022
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373. Galaxy and Mass Assembly (GAMA): Extended Intra-Group Light in a group at $z=0.2$ from deep Hyper-Suprime Cam images
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Martinez-Lombilla, Cristina, Brough, Sarah, Montes, Mireia, Baena-Galle, Roberto, Akhlaghi, Mohammad, Infante-Sainz, Raul, Driver, Simon P., Holwerda, Benne W., Pimbblet, Kevin A., Robotham, Aaron S. G., Martinez-Lombilla, Cristina, Brough, Sarah, Montes, Mireia, Baena-Galle, Roberto, Akhlaghi, Mohammad, Infante-Sainz, Raul, Driver, Simon P., Holwerda, Benne W., Pimbblet, Kevin A., and Robotham, Aaron S. G.
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We present a pilot study to assess the potential of Hyper Suprime-Cam Public Data Release 2 (HSC-PDR2) images for the analysis of extended faint structures within groups of galaxies. We examine the intra-group light (IGL) of the group 400138 ($M_{\rm{dyn}}= 1.3 \pm 0.5 \times 10^{13} $M$_{\odot}$, $z\sim 0.2$) from the Galaxy And Mass Assembly (GAMA) survey using Hyper-Suprime Cam Subaru Strategic Program Public Data Release 2 (HSC-PDR2) images in $g$, $r$, and $i$ bands. We present the most extended IGL measurement to date, reaching down to $\mu_{g}^{\rm{lim}}=30.76$ mag arcsec$^{-2}$ ($3 \sigma$; $10 \times 10$ arcsec$^{2}$) at a semi-major axis of 275 kpc. The IGL shows mean colour values of $g-i=0.92$, $g-r=0.60$, and $r-i=0.32$ ($\pm$0.01). The IGL stellar populations are younger ($2-2.5$ Gyr) and less metal-rich ([Fe/H] $ \sim -$0.4) than those of the host group galaxies. We find a range of IGL fractions as a function of total group luminosity of $\sim 2-36 \%$ depending on the definition of IGL, with larger fractions the bluer the observation wavelength. The early-type to late-type galaxy ratio suggests that 400138 is a more evolved group, dominated by ETGs, and the IGL fraction agrees with that of other similarly evolved groups. These results are consistent with tidal stripping of the outer parts of Milky Way-like galaxies as the main driver of the IGL build-up. This is supported by the detection of substructure in the IGL towards the galaxy member 1660615 suggesting a recent interaction ($<1$ Gyr ago) of that galaxy with the core of the group., Comment: 19 pages, 8 figures, 2 tables, accepted for publication in MNRAS
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- 2022
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374. JWST's PEARLS: a new lens model for ACT-CL J0102$-$4915, 'EL Gordo', and the first red supergiant star at cosmological distances discovered by JWST
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Diego, Jose M., Meena, Ashish K., Adams, Nathan J., Broadhurst, Tom, Dai, Liang, Coe, Dan, Frye, Brenda, Kelly, Patrick, Koekemoer, Anton M., Pascale, Massimo, Willner, S. P., Zackrisson, Erik, Zitrin, Adi, Windhorst, Rogier A., Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Tompkins, Scott, Conselice, Christopher J., Driver, Simon P., Yan, Haojing, Grogin, Norman, Marshall, Madeline A., Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Bradley, Larry D., Caminha, Gabriel, Caputi, Karina, Diego, Jose M., Meena, Ashish K., Adams, Nathan J., Broadhurst, Tom, Dai, Liang, Coe, Dan, Frye, Brenda, Kelly, Patrick, Koekemoer, Anton M., Pascale, Massimo, Willner, S. P., Zackrisson, Erik, Zitrin, Adi, Windhorst, Rogier A., Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Tompkins, Scott, Conselice, Christopher J., Driver, Simon P., Yan, Haojing, Grogin, Norman, Marshall, Madeline A., Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Bradley, Larry D., Caminha, Gabriel, and Caputi, Karina
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The first JWST data on the massive colliding cluster El Gordo confirm 23 known families of multiply lensed images and identify 8 new members of these families. Based on these families, which have been confirmed spectroscopically by MUSE, we derived an initial lens model. This model guided the identification of 37 additional families of multiply lensed galaxies, among which 28 are entirely new systems, and 9 were previously known. The initial lens model determined geometric redshifts for the 37 new systems. The geometric redshifts agree reasonably well with spectroscopic or photometric redshifts when those are available. The geometric redshifts enable two additional models that include all 60 families of multiply lensed galaxies spanning a redshift range $2
0.8$ and has an estimated virial mass close the maximum mass allowed by standard cosmological models. The JWST images also reveal the presence of small-mass perturbers that produce small lensing distortions. The smallest of these is consistent with being a dwarf galaxy at $z=0.87$ and has an estimated mass of $3.8\times10^9$~\Msol, making it the smallest substructure found at $z>0.5$. The JWST images also show several candidate caustic-crossing events. One of them is detected at high significance at the expected position of the critical curve and is likely a red supergiant star at $z=2.1878$. This would be the first red supergiant found at cosmological distances. The cluster lensing should magnify background objects at $z>6$, making more of them visible than in blank fields of similar size, but there appears to be a deficiency of such objects., Comment: 27 pages, 21 figures - Published
- 2022
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375. JWST's PEARLS: A JWST/NIRCam view of ALMA sources
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Cheng, Cheng, Huang, Jia-Sheng, Smail, Ian, Yan, Haojing, Cohen, Seth H., Jansen, Rolf A., Windhorst, Rogier A., Ma, Zhiyuan, Koekemoer, Anton, Willmer, Christopher N. A., Willner, S. P., Diego, Jose M., Frye, Brenda, Conselice, Christopher J., Ferreira, Leonardo, Petric, Andreea, Yun, Min, Gim, Hansung B., Polletta, Maria del Carmen, Duncan, Kenneth J., Honor, Rachel, Holwerda, Benne W., Röttgering, Huub J. A., Hathi, Nimish P., Kamieneski, Patrick S., Adams, Nathan J., Coe, Dan, Broadhurst, Tom, Summers, Jake, Tompkins, Scott, Driver, Simon P., Grogin, Norman A., Marshall, Madeline A., Pirzkal, Nor, Robotham, Aaron, Ryan Jr, Russell E., Cheng, Cheng, Huang, Jia-Sheng, Smail, Ian, Yan, Haojing, Cohen, Seth H., Jansen, Rolf A., Windhorst, Rogier A., Ma, Zhiyuan, Koekemoer, Anton, Willmer, Christopher N. A., Willner, S. P., Diego, Jose M., Frye, Brenda, Conselice, Christopher J., Ferreira, Leonardo, Petric, Andreea, Yun, Min, Gim, Hansung B., Polletta, Maria del Carmen, Duncan, Kenneth J., Honor, Rachel, Holwerda, Benne W., Röttgering, Huub J. A., Hathi, Nimish P., Kamieneski, Patrick S., Adams, Nathan J., Coe, Dan, Broadhurst, Tom, Summers, Jake, Tompkins, Scott, Driver, Simon P., Grogin, Norman A., Marshall, Madeline A., Pirzkal, Nor, Robotham, Aaron, and Ryan Jr, Russell E.
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We report the results of James Webb Space Telescope/NIRCam observations of 19 (sub)millimeter (submm/mm) sources detected by the Atacama Large Millimeter Array (ALMA). The accurate ALMA positions allowed unambiguous identifications of their NIRCam counterparts. Taking gravitational lensing into account, these represent 16 distinct galaxies in three fields and constitute the largest sample of its kind to date. The counterparts' spectral energy distributions from rest-frame ultraviolet to near infrared provide photometric redshifts ($1
10^{10.5}$ Msol), which are similar to sub-millimeter galaxy (SMG) hosts studied previously. However, our sample is fainter in submm/mm than the classic SMG samples are, and our sources exhibit a wider range of properties. They have dust-embedded star-formation rates as low as 10 Msol yr$^{-1}$, and the sources populate both the star-forming main sequence and the quiescent categories. The deep NIRCam data allow us to study the rest-frame near-IR morphologies. Excluding two multiply imaged systems and one quasar, the majority of the remaining sources are disk-like and show either little or no disturbance. This suggests that secular growth is a potential route for the assembly of high-mass disk galaxies. While a few hosts have large disks, the majority have small disks (median half-mass radius of 1.6 kpc). At this time, it is unclear whether this is due to the prevalence of small disks at these redshifts or some unknown selection effects of deep ALMA observations. A larger sample of ALMA sources with NIRCam observations will be able to address this question., Comment: 19 pages, 11 figures, accepted by ApJL - Published
- 2022
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376. Deep Investigation of Neutral Gas Origins (DINGO): HI stacking experiments with early science data
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Rhee, Jonghwan, Meyer, Martin, Popping, Attila, Bellstedt, Sabine, Driver, Simon P., Robotham, Aaron S. G., Whiting, Matthew, Baldry, Ivan K., Brough, Sarah, Brown, Michael J. I., Bunton, John D., Dodson, Richard, Holwerda, Benne W., Hopkins, Andrew M., Koribalski, Bärbel S., Lee-Waddell, Karen, López-Sánchez, Ángel R., Loveday, Jon, Mahony, Elizabeth, Roychowdhury, Sambit, Rozgonyi, Kristóf, Staveley-Smith, Lister, Rhee, Jonghwan, Meyer, Martin, Popping, Attila, Bellstedt, Sabine, Driver, Simon P., Robotham, Aaron S. G., Whiting, Matthew, Baldry, Ivan K., Brough, Sarah, Brown, Michael J. I., Bunton, John D., Dodson, Richard, Holwerda, Benne W., Hopkins, Andrew M., Koribalski, Bärbel S., Lee-Waddell, Karen, López-Sánchez, Ángel R., Loveday, Jon, Mahony, Elizabeth, Roychowdhury, Sambit, Rozgonyi, Kristóf, and Staveley-Smith, Lister
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We present early science results from Deep Investigation of Neutral Gas Origins (DINGO), an HI survey using the Australian Square Kilometre Array Pathfinder (ASKAP). Using ASKAP sub-arrays available during its commissioning phase, DINGO early science data were taken over $\sim$ 60 deg$^{2}$ of the Galaxy And Mass Assembly (GAMA) 23 h region with 35.5 hr integration time. We make direct detections of six known and one new sources at $z < 0.01$. Using HI spectral stacking, we investigate the HI gas content of galaxies at $0.04 < z< 0.09$ for different galaxy colours. The results show that galaxy morphology based on optical colour is strongly linked to HI gas properties. To examine environmental impacts on the HI gas content of galaxies, three sub-samples are made based on the GAMA group catalogue. The average HI mass of group central galaxies is larger than those of satellite and isolated galaxies, but with a lower HI gas fraction. We derive a variety of HI scaling relations for physical properties of our sample, including stellar mass, stellar mass surface density, $NUV-r$ colour, specific star formation rate, and halo mass. We find that the derived HI scaling relations are comparable to other published results, with consistent trends also observed to $\sim$0.5 dex lower limits in stellar mass and stellar surface density. The cosmic HI densities derived from our data are consistent with other published values at similar redshifts. DINGO early science highlights the power of HI spectral stacking techniques with ASKAP., Comment: 27 pages, 25 figures, 10 tables, accepted for publication in MNRAS
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- 2022
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377. JWST's PEARLS: Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
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Windhorst, Rogier A., Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Tompkins, Scott, Conselice, Christopher J., Driver, Simon P., Yan, Haojing, Coe, Dan, Frye, Brenda, Grogin, Norman, Koekemoer, Anton, Marshall, Madeline A., O'Brien, Rosalia, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Carleton, Timothy, Diego, Jose M., Keel, William C., Porto, Paolo, Redshaw, Caleb, Scheller, Sydney, Wilkins, Stephen M., Willner, S. P., Zitrin, Adi, Adams, Nathan J., Austin, Duncan, Arendt, Richard G., Beacom, John F., Bhatawdekar, Rachana A., Bradley, Larry D., Broadhurst, Thomas J., Cheng, Cheng, Civano, Francesca, Dai, Liang, Dole, Herve, D'Silva, Jordan C. J., Duncan, Kenneth J., Fazio, Giovanni G., Ferrami, Giovanni, Ferreira, Leonardo, Finkelstein, Steven L., Furtak, Lukas J., Gim, Hansung B., Griffiths, Alex, Hammel, Heidi B., Harrington, Kevin C., Hathi, Nimish P., Holwerda, Benne W., Honor, Rachel, Huang, Jia-Sheng, Hyun, Minhee, Im, Myungshin, Joshi, Bhavin A., Kamieneski, Patrick S., Kelly, Patrick, Larson, Rebecca L., Li, Juno, Lim, Jeremy, Ma, Zhiyuan, Maksym, Peter, Manzoni, Giorgio, Meena, Ashish Kumar, Milam, Stefanie N., Nonino, Mario, Pascale, Massimo, Pierel, Justin D. R., Petric, Andreea, Polletta, Maria del Carmen, Rottgering, Huub J. A., Rutkowski, Michael J., Smail, Ian, Straughn, Amber N., Strolger, Louis-Gregory, Swirbul, Andi, Trussler, James A. A., Wang, Lifan, Welch, Brian, Wyithe, J. Stuart B., Yun, Min, Zackrisson, Erik, Zhang, Jiashuo, Zhao, Xiurui, Windhorst, Rogier A., Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Tompkins, Scott, Conselice, Christopher J., Driver, Simon P., Yan, Haojing, Coe, Dan, Frye, Brenda, Grogin, Norman, Koekemoer, Anton, Marshall, Madeline A., O'Brien, Rosalia, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Carleton, Timothy, Diego, Jose M., Keel, William C., Porto, Paolo, Redshaw, Caleb, Scheller, Sydney, Wilkins, Stephen M., Willner, S. P., Zitrin, Adi, Adams, Nathan J., Austin, Duncan, Arendt, Richard G., Beacom, John F., Bhatawdekar, Rachana A., Bradley, Larry D., Broadhurst, Thomas J., Cheng, Cheng, Civano, Francesca, Dai, Liang, Dole, Herve, D'Silva, Jordan C. J., Duncan, Kenneth J., Fazio, Giovanni G., Ferrami, Giovanni, Ferreira, Leonardo, Finkelstein, Steven L., Furtak, Lukas J., Gim, Hansung B., Griffiths, Alex, Hammel, Heidi B., Harrington, Kevin C., Hathi, Nimish P., Holwerda, Benne W., Honor, Rachel, Huang, Jia-Sheng, Hyun, Minhee, Im, Myungshin, Joshi, Bhavin A., Kamieneski, Patrick S., Kelly, Patrick, Larson, Rebecca L., Li, Juno, Lim, Jeremy, Ma, Zhiyuan, Maksym, Peter, Manzoni, Giorgio, Meena, Ashish Kumar, Milam, Stefanie N., Nonino, Mario, Pascale, Massimo, Pierel, Justin D. R., Petric, Andreea, Polletta, Maria del Carmen, Rottgering, Huub J. A., Rutkowski, Michael J., Smail, Ian, Straughn, Amber N., Strolger, Louis-Gregory, Swirbul, Andi, Trussler, James A. A., Wang, Lifan, Welch, Brian, Wyithe, J. Stuart B., Yun, Min, Zackrisson, Erik, Zhang, Jiashuo, and Zhao, Xiurui
- Abstract
We give an overview and describe the rationale, methods, and first results from NIRCam images of the JWST "Prime Extragalactic Areas for Reionization and Lensing Science" ("PEARLS") project. PEARLS uses up to eight NIRCam filters to survey several prime extragalactic survey areas: two fields at the North Ecliptic Pole (NEP); seven gravitationally lensing clusters; two high redshift proto-clusters; and the iconic backlit VV 191 galaxy system to map its dust attenuation. PEARLS also includes NIRISS spectra for one of the NEP fields and NIRSpec spectra of two high-redshift quasars. The main goal of PEARLS is to study the epoch of galaxy assembly, AGN growth, and First Light. Five fields, the JWST NEP Time-Domain Field (TDF), IRAC Dark Field (IDF), and three lensing clusters, will be observed in up to four epochs over a year. The cadence and sensitivity of the imaging data are ideally suited to find faint variable objects such as weak AGN, high-redshift supernovae, and cluster caustic transits. Both NEP fields have sightlines through our Galaxy, providing significant numbers of very faint brown dwarfs whose proper motions can be studied. Observations from the first spoke in the NEP TDF are public. This paper presents our first PEARLS observations, their NIRCam data reduction and analysis, our first object catalogs, the 0.9-4.5 $\mu$m galaxy counts and Integrated Galaxy Light. We assess the JWST sky brightness in 13 NIRCam filters, yielding our first constraints to diffuse light at 0.9-4.5 {\mu}m. PEARLS is designed to be of lasting benefit to the community., Comment: Accepted to AJ, comments welcome. We ask anyone who uses our public PEARLS (NEP TDF) data to refer to this overview paper
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- 2022
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378. Webb's PEARLS: Bright 1.5--2.0 micron Dropouts in the Spitzer/IRAC Dark Field
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Yan, Haojing, Cohen, Seth H., Windhorst, Rogier A., Jansen, Rolf A., Ma, Zhiyuan, Beacom, John F., Cheng, Cheng, Huang, Jia-Sheng, Grogin, Norman A., Willner, S. P., Yun, Min, Hammel, Heidi B., Milam, Stefanie N., Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Marshall, Madeline A., Koekemoer, Anton, Willmer, Christopher N. A., Robotham, Aaron, D'Silva, Jordan C. J., Summers, Jake, Ling, Chenxiaoji, Lim, Jeremy, Harrington, Kevin, Ferreira, Leonardo, Diego, Jose Maria, Pirzkal, Nor, Wilkins, Stephen M., Wang, Lifan, Hathi, Nimish P., Zitrin, Adi, Bhatawdekar, Rachana A., Adams, Nathan J., Furtak, Lukas J., Maksym, Peter, Rutkowski, Michael J., Fazio, Giovanni G., Yan, Haojing, Cohen, Seth H., Windhorst, Rogier A., Jansen, Rolf A., Ma, Zhiyuan, Beacom, John F., Cheng, Cheng, Huang, Jia-Sheng, Grogin, Norman A., Willner, S. P., Yun, Min, Hammel, Heidi B., Milam, Stefanie N., Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Marshall, Madeline A., Koekemoer, Anton, Willmer, Christopher N. A., Robotham, Aaron, D'Silva, Jordan C. J., Summers, Jake, Ling, Chenxiaoji, Lim, Jeremy, Harrington, Kevin, Ferreira, Leonardo, Diego, Jose Maria, Pirzkal, Nor, Wilkins, Stephen M., Wang, Lifan, Hathi, Nimish P., Zitrin, Adi, Bhatawdekar, Rachana A., Adams, Nathan J., Furtak, Lukas J., Maksym, Peter, Rutkowski, Michael J., and Fazio, Giovanni G.
- Abstract
Using the first epoch of four-band NIRCam observations obtained by the James Webb Space Telescope (JWST) Prime Extragalactic Areas for Reionization and Lensing Science Program in the Spitzer IRAC Dark Field, we search for F150W and F200W dropouts. In 14.2 arcmin^2, we have found eight F150W dropouts and eight F200W dropouts, all brighter than 27.5 mag (the brightest being ~24 mag) in the band to the red side of the break. As they are detected in multiple bands, these must be real objects. Their nature, however, is unclear, and characterizing their properties is important for realizing the full potential of JWST. If the observed color decrements are due to the Lyman break, these objects should be at z >~ 11.7 and z >~ 15.4, respectively. The color diagnostics show that at least four F150W dropouts are far away from the usual contaminators encountered in dropout searches (red galaxies at much lower redshifts or brown dwarf stars). While the diagnostics of the F200W dropouts are less certain due to the limited number of passbands, at least one of them is likely not a known type of contaminant, and the rest are consistent with either high-redshift galaxies with evolved stellar populations or old galaxies at z ~ 3 to 8. If a significant fraction of our dropouts are indeed at z ~ 12, we have to face the severe problem of explaining their high luminosities and number densities. Spectroscopic identifications of such objects are urgently needed., Comment: Accepted for publication in ApJL
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- 2022
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379. JWST's PEARLS: dust attenuation and gravitational lensing in the backlit-galaxy system VV 191
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Keel, William C., Windhorst, Rogier A., Jansen, Rolf A., Cohen, Seth H., Summers, Jake, Holwerda, Benne, Bradford, Sarah T., Robertson, Clayton D., Ferrami, Giovanni, Wyithe, Stuart, Yan, Haojing, Conselice, Christopher J., Driver, Simon P., Robotham, Aaron, Grogin, Norman A., Willmer, Christopher N. A., Koekemoer, Anton M., Frye, Brenda L., Hathi, Nimish P., Ryan, Jr., Russell E., Pirzkal, Nor, Marshall, Madeline A., Coe, Dan, Diego, Jose M., Broadhurst, Thomas J., Rutkowski, Michael J., Wang, Lifan, Willner, S. P., Petric, Andreea, Cheng, Cheng, Zitrin, Adi, Keel, William C., Windhorst, Rogier A., Jansen, Rolf A., Cohen, Seth H., Summers, Jake, Holwerda, Benne, Bradford, Sarah T., Robertson, Clayton D., Ferrami, Giovanni, Wyithe, Stuart, Yan, Haojing, Conselice, Christopher J., Driver, Simon P., Robotham, Aaron, Grogin, Norman A., Willmer, Christopher N. A., Koekemoer, Anton M., Frye, Brenda L., Hathi, Nimish P., Ryan, Jr., Russell E., Pirzkal, Nor, Marshall, Madeline A., Coe, Dan, Diego, Jose M., Broadhurst, Thomas J., Rutkowski, Michael J., Wang, Lifan, Willner, S. P., Petric, Andreea, Cheng, Cheng, and Zitrin, Adi
- Abstract
We derive the spatial and wavelength behavior of dust attenuation in the multiple-armed spiral galaxy VV191b using backlighting by the superimposed elliptical system VV191a in a pair with an exceptionally favorable geometry for this measurement. Imaging using JWST and HST spans the wavelength range 0.3-4.5 microns with high angular resolution, tracing the dust in detail from 0.6 to 1.5 microns. Distinct dust lanes continue well beyond the bright spiral arms, and trace a complex web, with a very sharp radial cutoff near 1.7 Petrosian radii. We present attenuation profiles and coverage statistics in each band at radii 14-21 kpc. We derive the attenuation law with wavelength; the data both within and between the dust lanes clearly favor a stronger reddening behavior (R ~ 2.0 between 0.6 and 0.9 microns, approaching unity by 1.5 microns) than found for starbursts and star-forming regions of galaxies. Power-law extinction behavior lambda^(-beta) gives beta=2.1 from 0.6-0.9 microns. R decreases at increasing wavelengths (R~1.1 between 0.9 and 1.5 microns), while beta steepens to 2.5. Mixing regions of different column density flattens the wavelength behavior, so these results suggest a different grain population than in our vicinity. The NIRCam images reveal a lens arc and counterimage from a background galaxy at z~1, spanning 90 degrees azimuthally at 2.8" from the foreground elliptical galaxy nucleus, and an additional weakly-lensed galaxy. The lens model and imaging data give a mass/light ratio 7.6 in solar units within the Einstein radius 2.0 kpc., Comment: Accepted by Astron. J. Analysis redone since submission, using updated JWST calibrations. Dust reddening behavior is steeper with wavelength and lensed galaxy redshift lower than we first derived
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- 2022
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380. Galaxy And Mass Assembly (GAMA): Bulge-disk decomposition of KiDS data in the nearby universe
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Casura, Sarah, Liske, Jochen, Robotham, Aaron S. G., Brough, Sarah, Driver, Simon P., Graham, Alister W., Häußler, Boris, Holwerda, Benne W., Hopkins, Andrew M., Kelvin, Lee S., Moffett, Amanda J., Taranu, Dan S., Taylor, Edward N., Casura, Sarah, Liske, Jochen, Robotham, Aaron S. G., Brough, Sarah, Driver, Simon P., Graham, Alister W., Häußler, Boris, Holwerda, Benne W., Hopkins, Andrew M., Kelvin, Lee S., Moffett, Amanda J., Taranu, Dan S., and Taylor, Edward N.
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We derive single S\'ersic fits and bulge-disk decompositions for 13096 galaxies at redshifts z < 0.08 in the GAMA II equatorial survey regions in the Kilo-Degree Survey (KiDS) g, r and i bands. The surface brightness fitting is performed using the Bayesian two-dimensional profile fitting code ProFit. We fit three models to each galaxy in each band independently with a fully automated Markov-chain Monte Carlo analysis: a single S\'ersic model, a S\'ersic plus exponential and a point source plus exponential. After fitting the galaxies, we perform model selection and flag galaxies for which none of our models are appropriate (mainly mergers/Irregular galaxies). The fit quality is assessed by visual inspections, comparison to previous works, comparison of independent fits of galaxies in the overlap regions between KiDS tiles and bespoke simulations. The latter two are also used for a detailed investigation of systematic error sources. We find that our fit results are robust across various galaxy types and image qualities with minimal biases. Errors given by the MCMC underestimate the true errors typically by factors 2-3. Automated model selection criteria are accurate to > 90 % as calibrated by visual inspection of a subsample of galaxies. We also present g-r component colours and the corresponding colour-magnitude diagram, consistent with previous works despite our increased fit flexibility. Such reliable structural parameters for the components of a diverse sample of galaxies across multiple bands will be integral to various studies of galaxy properties and evolution. All results are integrated into the GAMA database., Comment: 36 pages, 33 figures. Accepted for publication in MNRAS
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- 2022
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381. MIGHTEE-HI: Evolution of HI scaling relations of star-forming galaxies at $z<0.5$
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Sinigaglia, Francesco, Rodighiero, Giulia, Elson, Ed, Vaccari, Mattia, Maddox, Natasha, Frank, Bradley S., Jarvis, Matt J., Oosterloo, Tom, Davé, Romeel, Salvato, Mara, Baes, Maarten, Bellstedt, Sabine, Bisigello, Laura, Collier, Jordan D., Cook, Robin H. W., Davies, Luke J. M., Delhaize, Jacinta, Driver, Simon P., Foster, Caroline, Kurapati, Sushma, Lagos, Claudia del P., Lidman, Christopher, Piña, Pavel E. Mancera, Meyer, Martin J., Mogotsi, K. Moses, Pan, Hengxing, Ponomareva, Anastasia A., Prandoni, Isabella, Rajohnson, Sambatriniaina H. A., Robotham, Aaron S. G., Santos, Mario G., Sekhar, Srikrishna, Spekkens, Kristine, Thorne, Jessica E., van der Hulst, Jan M., Wong, O. Ivy, Sinigaglia, Francesco, Rodighiero, Giulia, Elson, Ed, Vaccari, Mattia, Maddox, Natasha, Frank, Bradley S., Jarvis, Matt J., Oosterloo, Tom, Davé, Romeel, Salvato, Mara, Baes, Maarten, Bellstedt, Sabine, Bisigello, Laura, Collier, Jordan D., Cook, Robin H. W., Davies, Luke J. M., Delhaize, Jacinta, Driver, Simon P., Foster, Caroline, Kurapati, Sushma, Lagos, Claudia del P., Lidman, Christopher, Piña, Pavel E. Mancera, Meyer, Martin J., Mogotsi, K. Moses, Pan, Hengxing, Ponomareva, Anastasia A., Prandoni, Isabella, Rajohnson, Sambatriniaina H. A., Robotham, Aaron S. G., Santos, Mario G., Sekhar, Srikrishna, Spekkens, Kristine, Thorne, Jessica E., van der Hulst, Jan M., and Wong, O. Ivy
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We present the first measurements of HI galaxy scaling relations from a blind survey at $z>0.15$. We perform spectral stacking of 9023 spectra of star-forming galaxies undetected in HI at $0.23
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- 2022
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382. SKYSURF: Constraints on Zodiacal Light and Extragalactic Background Light through Panchromatic HST All-Sky Surface-Brightness Measurements: II. First Limits on Diffuse Light at 1.25, 1.4, and 1.6 microns
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Carleton, Timothy, Windhorst, Rogier A., O'Brien, Rosalia, Cohen, Seth H., Carter, Delondrae, Jansen, Rolf, Tompkins, Scott, Arendt, Richard G., Caddy, Sarah, Grogin, Norman, Kenyon, Scott J., Koekemoer, Anton, MacKenty, John, Casertano, Stefano, Davies, Luke J. M., Driver, Simon P., Dwek, Eli, Kashlinsky, Alexander, Miles, Nathan, Pawnikar, Rushabh, Pirzkal, Nor, Robotham, Aaron, Ryan, Russell, Abate, Haley, Andras-Letanovszky, Hanga, Berkheimer, Jessica, Goisman, Zak, Henningsen, Daniel, Kramer, Darby, Rogers, Ci'mone, Swirbul, Andi, Carleton, Timothy, Windhorst, Rogier A., O'Brien, Rosalia, Cohen, Seth H., Carter, Delondrae, Jansen, Rolf, Tompkins, Scott, Arendt, Richard G., Caddy, Sarah, Grogin, Norman, Kenyon, Scott J., Koekemoer, Anton, MacKenty, John, Casertano, Stefano, Davies, Luke J. M., Driver, Simon P., Dwek, Eli, Kashlinsky, Alexander, Miles, Nathan, Pawnikar, Rushabh, Pirzkal, Nor, Robotham, Aaron, Ryan, Russell, Abate, Haley, Andras-Letanovszky, Hanga, Berkheimer, Jessica, Goisman, Zak, Henningsen, Daniel, Kramer, Darby, Rogers, Ci'mone, and Swirbul, Andi
- Abstract
We present the first results from the HST Archival Legacy project "SKYSURF." As described in Windhorst et al. 2022, SKYSURF utilizes the large HST archive to study the diffuse UV, optical, and near-IR backgrounds and foregrounds in detail. Here we utilize SKYSURF's first sky-surface brightness measurements to constrain the level of near-IR diffuse Extragalactic Background Light (EBL). Our sky-surface brightness measurements have been verified to an accuracy of better than 1%, which when combined with systematic errors associated with HST, results in sky brightness uncertainties of $\sim$2-4% $\simeq$ 0.005 MJy/sr in each image. We put limits on the amount of diffuse EBL in three near-IR filters (F125W, F140W, and F160W) by comparing our preliminary sky measurements of $> 30,000$ images to Zodiacal light models, carefully selecting the darkest images to avoid contamination from stray light. In addition, we investigate the impact that instrumental thermal emission has on our measurements, finding that it has a limited impact on F125W and F140W measurements, whereas uncertainties in the exact thermal state of HST results in significant uncertainties in the level of astrophysical diffuse light in F160W images. When compared to the Kelsall et al. (1998) Zodiacal model, an isotropic diffuse background of $30$ nW m$^{-2}$ sr$^{-1}$ remains, whereas using the Wright (1998) Zodiacal model results in no discernible diffuse background. Based primarily on uncertainties in the foreground model subtraction, we present limits on the amount of diffuse EBL of 29 nW m$^{-2}$ sr$^{-1}$, 40 nW m$^{-2}$ sr$^{-1}$, and 29 nW m$^{-2}$ sr$^{-1}$ for F125W, F140W, and F160W respectively. While this light is generally isotropic, our modeling at this point does not distinguish between a cosmological origin or a Solar System origin (such as a dim, diffuse, spherical cloud of cometary dust)., Comment: Accepted with Windhorst et al. 2022 to AJ. Main figures are Fig. 10 and 11. Comments welcome!
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- 2022
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383. SKYSURF: Constraints on Zodiacal Light and Extragalactic Background Light through Panchromatic HST All-Sky Surface-Brightness Measurements: I. Survey Overview and Methods
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Windhorst, Rogier A., Carleton, Timothy, O'Brien, Rosalia, Cohen, Seth H., Carter, Delondrae, Jansen, Rolf, Tompkins, Scott, Arendt, Richard G., Caddy, Sarah, Grogin, Norman, Koekemoer, Anton, MacKenty, John, Casertano, Stefano, Davies, Luke J. M., Driver, Simon P., Dwek, Eli, Kashlinsky, Alexander, Kenyon, Scott J., Miles, Nathan, Pirzkal, Nor, Robotham, Aaron, Ryan, Russell, Abate, Haley, Andras-Letanovszky, Hanga, Berkheimer, Jessica, Chambers, John, Gelb, Connor, Goisman, Zak, Henningsen, Daniel, Huckabe, Isabela, Kramer, Darby, Patel, Teerthal, Pawnikar, Rushabh, Pringle, Ewan, Rogers, Ci'mone, Sherman, Steven, Swirbul, Andi, Webber, Kaitlin, Windhorst, Rogier A., Carleton, Timothy, O'Brien, Rosalia, Cohen, Seth H., Carter, Delondrae, Jansen, Rolf, Tompkins, Scott, Arendt, Richard G., Caddy, Sarah, Grogin, Norman, Koekemoer, Anton, MacKenty, John, Casertano, Stefano, Davies, Luke J. M., Driver, Simon P., Dwek, Eli, Kashlinsky, Alexander, Kenyon, Scott J., Miles, Nathan, Pirzkal, Nor, Robotham, Aaron, Ryan, Russell, Abate, Haley, Andras-Letanovszky, Hanga, Berkheimer, Jessica, Chambers, John, Gelb, Connor, Goisman, Zak, Henningsen, Daniel, Huckabe, Isabela, Kramer, Darby, Patel, Teerthal, Pawnikar, Rushabh, Pringle, Ewan, Rogers, Ci'mone, Sherman, Steven, Swirbul, Andi, and Webber, Kaitlin
- Abstract
We give an overview and describe the rationale, methods, and testing of the Hubble Space Telescope (HST) Archival Legacy project "SKYSURF." SKYSURF uses HST's unique capability as an absolute photometer to measure the ~0.2-1.7 $\mu$m sky surface brightness (SB) from 249,861 WFPC2, ACS, and WFC3 exposures in ~1400 independent HST fields. SKYSURF's panchromatic dataset is designed to constrain the discrete and diffuse UV to near-IR sky components: Zodiacal Light (ZL; inner Solar System), Kuiper Belt Objects (KBOs; outer Solar System), Diffuse Galactic Light (DGL), and the discrete plus diffuse Extragalactic Background Light (EBL). We outline SKYSURF's methods to: (1) measure sky-SB levels between its detected objects; (2) measure the integrated discrete EBL, most of which comes from AB$\simeq$17-22 mag galaxies; and (3) estimate how much diffuse light may exist in addition to the extrapolated discrete galaxy counts. Simulations of HST WFC3/IR images with known sky-values and gradients, realistic cosmic ray (CR) distributions, and star plus galaxy counts were processed with nine different algorithms to measure the "Lowest Estimated Sky-SB" (LES) in each image between the discrete objects. The best algorithms recover the inserted LES values within 0.2% when there are no image gradients, and within 0.2-0.4% when there are 5-10% gradients. SKYSURF requires non-standard re-processing of these HST images that includes restoring the lowest sky-level from each visit into each drizzled image. We provide a proof of concept of our methods from the WFC3/IR F125W images, where any residual diffuse light that HST sees in excess of the Kelsall et al. (1998) Zodiacal model prediction does not depend on the total object flux that each image contains. This enables us to present our first SKYSURF results on diffuse light in Carleton et al. (2022)., Comment: Accepted to AJ; see accompanying paper Carleton et al. 2022: arXiv:2205.06347. Comments welcome!
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- 2022
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384. Seizure Prophylaxis Guidelines Following Traumatic Brain Injury: An Evaluation of Compliance
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Zaman, Anwar, Dubiel, Randi, Driver, Simon, Bennett, Monica, Diggs, Vincent, and Callender, Librada
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- 2017
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385. Improving practice with integration of patient directed activity during inpatient rehabilitation
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Trammell, Molly, Kapoor, Priyanka, Swank, Chad, and Driver, Simon
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- 2017
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386. Teaching Sport Skills to Brain-Injury Students: An Example in Swimming
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Driver, Simon and Kelly, Luke
- Abstract
The number of people who experience a brain injury increases every year, and 40 percent of all cases involve children (Hill, 1999). In fact, this high rate has led brain injury to become the most commonly acquired disability among children (Bigge, Best, & Heller, 2001), leading to a variety of primary disabilities that affect cognition, personality, speech, memory, attention, and motor ability (Finsett & Andersson, 2000). Secondary problems often result from these primary disabilities, such as immobility and other health problems associated with being sedentary, including depression, stress, and decreased social contacts. These various disabilities challenge the teachers of students with a brain injury to provide lifetime sport-skill programs, so that these students can be active in recreational settings, even after they have finished school. This article presents an example of a lifetime sport-skill program that will be helpful to general educators, physical education teachers, adapted physical education teachers, and coaches working with students who have a brain injury. The article walks the reader through the development and implementation of such a program, designed for a fictional student, Scott, who suffers from a brain injury. Although Scott is a fictional character, his disabilities and the problems he faces are typical of a student with a brain injury. Practitioners should remember that suggestions are offered as guidelines, and depending on the student, adaptations to the program design can be made as appropriate. The first part of this article provides information about the importance of collaborating with other people when creating a lifetime sport-skill program. The article then offers practical suggestions on how to design and implement such a program. (Contains 1 table.)
- Published
- 2005
387. Efficacy of the Diabetes Prevention Program Group Lifestyle Balance Program Modified for Individuals with TBI (GLB-TBI): Results from a 12-month Randomized Controlled Trial.
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Driver, Simon, McShan, Evan, Swank, Chad, Calhoun, Stephanie, Bennett, Monica, Callender, Librada, Holden, Alexandria, Juengst, Shannon, Bell, Kathleen, Douglas, Megan, Kramer, Kaye, and Dubiel, Randi
- Subjects
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TOTAL body irradiation , *CONTROL (Psychology) , *RANDOMIZED controlled trials , *DIASTOLIC blood pressure , *ATTENTION control , *HDL cholesterol - Abstract
Background Obesity after traumatic brain injury (TBI) is a public health issue and no evidence-based weight loss interventions exist to meet the unique needs of individuals after TBI. Purpose To (a) examine the efficacy of the Diabetes Prevention Program Group Lifestyle Balance for TBI (GLB-TBI) weight-loss intervention compared to an attention control for primary (weight-loss) and secondary health outcomes; (b) determine participant compliance with the GLB-TBI; and (c) determine if compliance is associated with improved outcomes. Methods Individuals with moderate to severe TBI, age 18–64 years, ≥6 months postinjury, and body mass index of ≥25 kg/m2 were randomized to a 12-month, 22-session GLB-TBI intervention or attention control condition. Weight-loss (lbs.), anthropometric, biomarkers, and patient-reported outcomes were collected at baseline, 3, 6, and 12 months. Results The GLB-TBI group (n = 27) lost 17.8 ± 41.4lbs (7.9%) over the 12-month program and the attention control group (n = 27) lost 0 ± 55.4lbs (0%). The GLB-TBI group had significant improvements in diastolic blood pressure, triglycerides, and HDL cholesterol. GLB-TBI attendance was 89.6% and weekly self-monitoring of diet and activity was 68.8%. Relative to baseline, the GLB-TBI compliant group (≥80% attendance; ≥85% self-monitoring; n = 10) had a statistically significant decrease in weight at each assessment, the noncompliant group had a significant decrease between 6 and 12 months (n = 17), with no change in weight in the attention control group (n = 27). Conclusions Findings suggest for adults with TBI who are overweight or obese, participation in the GLB-TBI can significantly reduce weight and metabolic risk factors and increase self-reported habits for diet and exercise. [ABSTRACT FROM AUTHOR]
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- 2023
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388. Hubble Deep Fever: A Faint Galaxy Diagnosis
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Driver, Simon P., Bergeron, Jacqueline, editor, Morganti, Raffaella, editor, and Couch, Warrick J., editor
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- 1999
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389. Deep extragalactic visible legacy survey (DEVILS): the emergence of bulges and decline of disc growth since z = 1
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Hashemizadeh, Abdolhosein, primary, Driver, Simon P, additional, Davies, Luke J M, additional, Robotham, Aaron S G, additional, Bellstedt, Sabine, additional, Foster, Caroline, additional, Holwerda, Benne W, additional, Jarvis, Matt, additional, Phillipps, Steven, additional, Siudek, Malgorzata, additional, Thorne, Jessica E, additional, Windhorst, Rogier A, additional, and Wolf, Christian, additional
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- 2022
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390. Effectiveness and feasibility of the workout on wheels internet intervention (WOWii) for individuals with spinal cord injury: a randomized controlled trial
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Froehlich-Grobe, Katherine, primary, Lee, Jaehoon, additional, Ochoa, Christa, additional, Lopez, Amber, additional, Sarker, Erina, additional, Driver, Simon, additional, Shegog, Ross, additional, and Lin, Suh-Jen, additional
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- 2022
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391. An empirical measurement of the halo mass function from the combination of GAMA DR4, SDSS DR12, and REFLEX II data
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Driver, Simon P, primary, Robotham, Aaron S G, additional, Obreschkow, Danail, additional, Peacock, John A, additional, Baldry, Ivan K, additional, Bellstedt, Sabine, additional, Bland-Hawthorn, Joss, additional, Brough, Sarah, additional, Cluver, Michelle, additional, Holwerda, Benne W, additional, Hopkins, Andrew, additional, Lagos, Claudia, additional, Liske, Jochen, additional, Loveday, Jon, additional, Phillipps, Steven, additional, and Taylor, Edward N, additional
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- 2022
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392. Galaxy and Mass Assembly (GAMA): The Weak Environmental Dependence of Quasar Activity at 0.1 < z < 0.35
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Wethers, Clare F., primary, Acharya, Nischal, additional, De Propris, Roberto, additional, Kotilainen, Jari, additional, Baldry, Ivan K., additional, Brough, Sarah, additional, Driver, Simon P., additional, Graham, Alister W., additional, Holwerda, Benne W., additional, Hopkins, Andrew M., additional, López-Sánchez, Angel R., additional, Loveday, Jonathan, additional, Phillipps, Steven, additional, Pimbblet, Kevin A., additional, Taylor, Edward, additional, Wang, Lingyu, additional, and Wright, Angus H., additional
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- 2022
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393. The LEGA-C and SAMI galaxy surveys: quiescent stellar populations and the mass–size plane across 6 Gyr
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Barone, Tania M, primary, D’Eugenio, Francesco, additional, Scott, Nicholas, additional, Colless, Matthew, additional, Vaughan, Sam P, additional, van der Wel, Arjen, additional, Fraser-McKelvie, Amelia, additional, de Graaff, Anna, additional, van de Sande, Jesse, additional, Wu(吳柏鋒), Po-Feng, additional, Bezanson, Rachel, additional, Brough, Sarah, additional, Bell, Eric, additional, Croom, Scott M, additional, Cortese, Luca, additional, Driver, Simon, additional, Gallazzi, Anna R, additional, Muzzin, Adam, additional, Sobral, David, additional, Bland-Hawthorn, Joss, additional, Bryant, Julia J, additional, Goodwin, Michael, additional, Lawrence, Jon S, additional, Lorente, Nuria P F, additional, and Owers, Matt S, additional
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- 2022
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394. Feasibility and Pilot Testing of Mobile Health Apps to Supplement 2 Healthy Lifestyle Interventions in Chronic Traumatic Brain Injury
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Juengst, Shannon B., primary, McShan, Evan, additional, Conley, Michael, additional, Luu, Ivan, additional, and Driver, Simon, additional
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- 2022
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395. Galaxy And Mass Assembly (GAMA): Data Release 4 and the z < 0.1 total and z < 0.08 morphological galaxy stellar mass functions
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Driver, Simon P, primary, Bellstedt, Sabine, additional, Robotham, Aaron S G, additional, Baldry, Ivan K, additional, Davies, Luke J, additional, Liske, Jochen, additional, Obreschkow, Danail, additional, Taylor, Edward N, additional, Wright, Angus H, additional, Alpaslan, Mehmet, additional, Bamford, Steven P, additional, Bauer, Amanda E, additional, Bland-Hawthorn, Joss, additional, Bilicki, Maciej, additional, Bravo, Matías, additional, Brough, Sarah, additional, Casura, Sarah, additional, Cluver, Michelle E, additional, Colless, Matthew, additional, Conselice, Christopher J, additional, Croom, Scott M, additional, de Jong, Jelte, additional, D’Eugenio, Franceso, additional, De Propris, Roberto, additional, Dogruel, Burak, additional, Drinkwater, Michael J, additional, Dvornik, Andrej, additional, Farrow, Daniel J, additional, Frenk, Carlos S, additional, Giblin, Benjamin, additional, Graham, Alister W, additional, Grootes, Meiert W, additional, Gunawardhana, Madusha L P, additional, Hashemizadeh, Abdolhosein, additional, Häußler, Boris, additional, Heymans, Catherine, additional, Hildebrandt, Hendrik, additional, Holwerda, Benne W, additional, Hopkins, Andrew M, additional, Jarrett, Tom H, additional, Heath Jones, D, additional, Kelvin, Lee S, additional, Koushan, Soheil, additional, Kuijken, Konrad, additional, Lara-López, Maritza A, additional, Lange, Rebecca, additional, López-Sánchez, Ángel R, additional, Loveday, Jon, additional, Mahajan, Smriti, additional, Meyer, Martin, additional, Moffett, Amanda J, additional, Napolitano, Nicola R, additional, Norberg, Peder, additional, Owers, Matt S, additional, Radovich, Mario, additional, Raouf, Mojtaba, additional, Peacock, John A, additional, Phillipps, Steven, additional, Pimbblet, Kevin A, additional, Popescu, Cristina, additional, Said, Khaled, additional, Sansom, Anne E, additional, Seibert, Mark, additional, Sutherland, Will J, additional, Thorne, Jessica E, additional, Tuffs, Richard J, additional, Turner, Ryan, additional, van der Wel, Arjen, additional, van Kampen, Eelco, additional, and Wilkins, Steve M, additional
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- 2022
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396. The Variation of the Gas Content of Galaxy Groups and Pairs Compared to Isolated Galaxies
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Roychowdhury, Sambit, primary, Meyer, Martin J., additional, Rhee, Jonghwan, additional, Zwaan, Martin A., additional, Chauhan, Garima, additional, Davies, Luke J. M., additional, Bellstedt, Sabine, additional, Driver, Simon P., additional, del P. Lagos, Claudia, additional, Robotham, Aaron S. G., additional, Bland-Hawthorn, Joss, additional, Dodson, Richard, additional, Holwerda, Benne W., additional, Hopkins, Andrew M., additional, Lara-López, Maritza A., additional, López-Sánchez, Ángel R., additional, Obreschkow, Danail, additional, Rozgonyi, Kristof, additional, Whiting, Matthew T., additional, and Wright, Angus H., additional
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- 2022
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397. Usability of a two-way personalized mobile trainer system in a community-based exercise program for adults with chronic traumatic brain injury
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Ding, Kan, primary, Juengst, Shannon B., additional, Neaves, Stephanie, additional, Turki, Ahmad, additional, Wang, Chaowei, additional, Huang, Mu, additional, Pham, Tri, additional, Behbehani, Khosrow, additional, Li, Ming, additional, Hynan, Linda, additional, Driver, Simon, additional, Zhang, Rong, additional, and Bell, Kathleen R., additional
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- 2022
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398. Caught in the Act: The Identification of the Galaxies Responsible for the Faint Blue Excess
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Driver, Simon P., Windhorst, Rogier A., Griffiths, Richard E., Bender, Ralf, editor, and Davies, Roger L., editor
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- 1996
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399. Deep Extragalactic VIsible Legacy Survey (DEVILS): identification of AGN through SED fitting and the evolution of the bolometric AGN luminosity function
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Thorne, Jessica E, primary, Robotham, Aaron S G, additional, Davies, Luke J M, additional, Bellstedt, Sabine, additional, Brown, Michael J I, additional, Croom, Scott M, additional, Delvecchio, Ivan, additional, Groves, Brent, additional, Jarvis, Matt J, additional, Shabala, Stanislav S, additional, Seymour, Nick, additional, Whittam, Imogen H, additional, Bravo, Matias, additional, Cook, Robin H W, additional, Driver, Simon P, additional, Holwerda, Benne, additional, Phillipps, Steven, additional, and Siudek, Malgorzata, additional
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- 2021
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400. Review of: "Effects of Surgical Facemasks on Perceived Exertion During Submaximal Exercise in Healthy Children"
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driver, simon, primary and Brown, Katelyn, additional
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- 2021
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Catalog
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