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Abstract
OBJECTIVE To update a rapid review published in 2017, which evaluated the NHS Health Check programme. METHODS An enlarged body of evidence was used to readdress six research objectives from a rapid review published in 2017, relating to the uptake, patient experiences and effectiveness of the NHS Health Check programme. Data sources included MEDLINE, PubMed, Embase, Health Management Information Consortium (HMIC), Cumulative Index of Nursing and Allied Health Literature (CINAHL), Global Health, PsycINFO, the Cochrane Library, NHS Evidence, Google Scholar, Google, ClinicalTrials.gov and the ISRCTN registry, Web of Science, Science Citation Index, The Cochrane Library, NHS Evidence, OpenGrey and hand searching article reference lists. These searches identified records from between January 1996 and December 2019. Screening, data extraction and quality appraisal using the Critical Appraisals Skills Programme checklists were performed in duplicate. Grading of Recommendations Assessment, Development and Evaluations was implemented. Data were synthesised narratively. RESULTS 697 studies were identified, and 29 new studies included in the review update. The number of published studies on the uptake, patient experiences and effectiveness of the NHS Health Check programme has increased by 43% since the rapid review published in 2017. However, findings from the original review remain largely unchanged. NHS Health Checks led to an overall increase in the detection of raised risk factors and morbidities including diabetes mellitus, hypertension, raised blood pressure, cholesterol and chronic kidney disease. Individuals most likely to attend the NHS Health Check programme included women, persons aged ≥60 years and those from more socioeconomically advantaged backgrounds. Opportunistic invitations increased uptake among men, younger persons and those with a higher deprivation level. CONCLUSIONS Although results are inconsistent between studies, the NHS Health Check programme is associated with increased detection of heightened cardiovascular disease risk factors and diagnoses. Uptake varied between population subgroups. Opportunistic invitations may increase uptake.
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Affiliation(s)
- L Tanner
- Population Health Sciences Institute, Newcastle University, Newcastle upon Tyne, UK
| | - Rpw Kenny
- Population Health Sciences Institute, Newcastle University, Newcastle upon Tyne, UK
| | - M Still
- Population Health Sciences Institute, Newcastle University, Newcastle upon Tyne, UK
| | - J Ling
- Faculty of Health Sciences and Wellbeing, University of Sunderland, Sunderland, UK
| | - F Pearson
- Population Health Sciences Institute, Newcastle University, Newcastle upon Tyne, UK
| | | | - R Bhardwaj-Gosling
- Population Health Sciences Institute, Newcastle University, Newcastle upon Tyne, UK
- Faculty of Health Sciences and Wellbeing, University of Sunderland, Sunderland, UK
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Orosz JA, Welsh WF, Carter JA, Fabrycky DC, Cochran WD, Endl M, Ford EB, Haghighipour N, MacQueen PJ, Mazeh T, Sanchis-Ojeda R, Short DR, Torres G, Agol E, Buchhave LA, Doyle LR, Isaacson H, Lissauer JJ, Marcy GW, Shporer A, Windmiller G, Barclay T, Boss AP, Clarke BD, Fortney J, Geary JC, Holman MJ, Huber D, Jenkins JM, Kinemuchi K, Kruse E, Ragozzine D, Sasselov D, Still M, Tenenbaum P, Uddin K, Winn JN, Koch DG, Borucki WJ. Kepler-47: A Transiting Circumbinary Multiplanet System. Science 2012; 337:1511-4. [DOI: 10.1126/science.1228380] [Citation(s) in RCA: 286] [Impact Index Per Article: 23.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
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Derekas A, Kiss LL, Borkovits T, Huber D, Lehmann H, Southworth J, Bedding TR, Balam D, Hartmann M, Hrudkova M, Ireland MJ, Kovács J, Mező G, Moór A, Niemczura E, Sarty GE, Szabó GM, Szabó R, Telting JH, Tkachenko A, Uytterhoeven K, Benkő JM, Bryson ST, Maestro V, Simon AE, Stello D, Schaefer G, Aerts C, ten Brummelaar TA, De Cat P, McAlister HA, Maceroni C, Mérand A, Still M, Sturmann J, Sturmann L, Turner N, Tuthill PG, Christensen-Dalsgaard J, Gilliland RL, Kjeldsen H, Quintana EV, Tenenbaum P, Twicken JD. HD 181068: A Red Giant in a Triply Eclipsing Compact Hierarchical Triple System. Science 2011; 332:216-8. [DOI: 10.1126/science.1201762] [Citation(s) in RCA: 83] [Impact Index Per Article: 6.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- A. Derekas
- Department of Astronomy, Eötvös University, Budapest, Hungary
- Konkoly Observatory, Hungarian Academy of Sciences, H-1525 Budapest, Post Office Box 67, Hungary
| | - L. L. Kiss
- Konkoly Observatory, Hungarian Academy of Sciences, H-1525 Budapest, Post Office Box 67, Hungary
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia
| | - T. Borkovits
- Baja Astronomical Observatory, H-6500 Baja, Szegedi út, Kt. 766, Hungary
- Eötvös József College, H-6500 Baja, Szegedi út 2, Hungary
| | - D. Huber
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia
| | - H. Lehmann
- Thüringer Landessternwarte (TLS) Tautenburg, Karl-Schwarzschild-Observatorium, 07778 Tautenburg, Germany
| | - J. Southworth
- Astrophysics Group, Keele University, Newcastle-Under-Lyme ST5 5BG, UK
| | - T. R. Bedding
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia
| | - D. Balam
- Dominion Astrophysical Observatory (DAO), Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada
| | - M. Hartmann
- Thüringer Landessternwarte (TLS) Tautenburg, Karl-Schwarzschild-Observatorium, 07778 Tautenburg, Germany
| | - M. Hrudkova
- Thüringer Landessternwarte (TLS) Tautenburg, Karl-Schwarzschild-Observatorium, 07778 Tautenburg, Germany
| | - M. J. Ireland
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia
| | - J. Kovács
- Gothard Observatory, Eötvös University, H-9704 Szombathely, Szent Imre Herceg u. 112., Hungary
| | - Gy. Mező
- Konkoly Observatory, Hungarian Academy of Sciences, H-1525 Budapest, Post Office Box 67, Hungary
| | - A. Moór
- Konkoly Observatory, Hungarian Academy of Sciences, H-1525 Budapest, Post Office Box 67, Hungary
| | - E. Niemczura
- Astronomical Institute, Wroclaw University, Kopernika 11, 51-622 Wroclaw, Poland
| | - G. E. Sarty
- Department of Physics and Engineering Physics, University of Saskatchewan, 9 Campus Drive, Saskatoon, Saskatchewan S7N 5A5, Canada
| | - Gy. M. Szabó
- Konkoly Observatory, Hungarian Academy of Sciences, H-1525 Budapest, Post Office Box 67, Hungary
| | - R. Szabó
- Konkoly Observatory, Hungarian Academy of Sciences, H-1525 Budapest, Post Office Box 67, Hungary
| | - J. H. Telting
- Nordic Optical Telescope, Apartado 474, 38700 Santa Cruz de La Palma, Spain
| | - A. Tkachenko
- Thüringer Landessternwarte (TLS) Tautenburg, Karl-Schwarzschild-Observatorium, 07778 Tautenburg, Germany
| | - K. Uytterhoeven
- Laboratoire Astrophysique, Instrumentation, et Modélisation, Commissariat à l’Energie Atomique (CEA)/Direction des Sciences de la Matière–CNRS–Université Paris Diderot; CEA, L'institut de recherche sur les lois fondamentales de l’Univers, Service d’Astrophysique, Saclay, 91191, Gif-sur-Yvette, France
- Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg, Germany
| | - J. M. Benkő
- Konkoly Observatory, Hungarian Academy of Sciences, H-1525 Budapest, Post Office Box 67, Hungary
| | - S. T. Bryson
- National Aeronautics and Space Administration (NASA) Ames Research Center, Moffett Field, CA 94035, USA
| | - V. Maestro
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia
| | - A. E. Simon
- Konkoly Observatory, Hungarian Academy of Sciences, H-1525 Budapest, Post Office Box 67, Hungary
| | - D. Stello
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia
| | - G. Schaefer
- Center for High Angular Resolution Astronomy, Georgia State University, Post Office Box 3969, Atlanta, GA 30302–3969, USA
| | - C. Aerts
- Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium
- Institute for Mathematics, Astrophysics, and Particle Physics (IMAPP), Department of Astrophysics, Radboud University Nijmegen, Post Office Box 9010, NL-6500 GL Nijmegen, Netherlands
| | - T. A. ten Brummelaar
- Center for High Angular Resolution Astronomy, Georgia State University, Post Office Box 3969, Atlanta, GA 30302–3969, USA
| | - P. De Cat
- Royal Observatory of Belgium, Ringlaan 3, 1180 Brussel, Belgium
| | - H. A. McAlister
- Center for High Angular Resolution Astronomy, Georgia State University, Post Office Box 3969, Atlanta, GA 30302–3969, USA
| | - C. Maceroni
- Istituto Nazionale di Astrofisica (INAF), Osservatorio astronomico di Roma, via Frascati 33, I-00040 Monteporzio C., Italy
| | - A. Mérand
- European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago 19, Chile
| | - M. Still
- National Aeronautics and Space Administration (NASA) Ames Research Center, Moffett Field, CA 94035, USA
| | - J. Sturmann
- Center for High Angular Resolution Astronomy, Georgia State University, Post Office Box 3969, Atlanta, GA 30302–3969, USA
| | - L. Sturmann
- Center for High Angular Resolution Astronomy, Georgia State University, Post Office Box 3969, Atlanta, GA 30302–3969, USA
| | - N. Turner
- Center for High Angular Resolution Astronomy, Georgia State University, Post Office Box 3969, Atlanta, GA 30302–3969, USA
| | - P. G. Tuthill
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia
| | | | - R. L. Gilliland
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - H. Kjeldsen
- Department of Physics and Astronomy, Building 1520, Aarhus University, 8000 Aarhus C, Denmark
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Gehrels N, Sarazin CL, O'Brien PT, Zhang B, Barbier L, Barthelmy SD, Blustin A, Burrows DN, Cannizzo J, Cummings JR, Goad M, Holland ST, Hurkett CP, Kennea JA, Levan A, Markwardt CB, Mason KO, Meszaros P, Page M, Palmer DM, Rol E, Sakamoto T, Willingale R, Angelini L, Beardmore A, Boyd PT, Breeveld A, Campana S, Chester MM, Chincarini G, Cominsky LR, Cusumano G, de Pasquale M, Fenimore EE, Giommi P, Gronwall C, Grupe D, Hill JE, Hinshaw D, Hjorth J, Hullinger D, Hurley KC, Klose S, Kobayashi S, Kouveliotou C, Krimm HA, Mangano V, Marshall FE, McGowan K, Moretti A, Mushotzky RF, Nakazawa K, Norris JP, Nousek JA, Osborne JP, Page K, Parsons AM, Patel S, Perri M, Poole T, Romano P, Roming PWA, Rosen S, Sato G, Schady P, Smale AP, Sollerman J, Starling R, Still M, Suzuki M, Tagliaferri G, Takahashi T, Tashiro M, Tueller J, Wells AA, White NE, Wijers RAMJ. A short γ-ray burst apparently associated with an elliptical galaxy at redshift z = 0.225. Nature 2005; 437:851-4. [PMID: 16208363 DOI: 10.1038/nature04142] [Citation(s) in RCA: 471] [Impact Index Per Article: 24.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/31/2005] [Accepted: 08/10/2005] [Indexed: 11/08/2022]
Abstract
Gamma-ray bursts (GRBs) come in two classes: long (> 2 s), soft-spectrum bursts and short, hard events. Most progress has been made on understanding the long GRBs, which are typically observed at high redshift (z approximately 1) and found in subluminous star-forming host galaxies. They are likely to be produced in core-collapse explosions of massive stars. In contrast, no short GRB had been accurately (< 10'') and rapidly (minutes) located. Here we report the detection of the X-ray afterglow from--and the localization of--the short burst GRB 050509B. Its position on the sky is near a luminous, non-star-forming elliptical galaxy at a redshift of 0.225, which is the location one would expect if the origin of this GRB is through the merger of neutron-star or black-hole binaries. The X-ray afterglow was weak and faded below the detection limit within a few hours; no optical afterglow was detected to stringent limits, explaining the past difficulty in localizing short GRBs.
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Affiliation(s)
- N Gehrels
- NASA/Goddard Space Flight Center, Greenbelt, Maryland 20771, USA
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