10 research outputs found
Assessment tools for the risk of pressure injury in children: A systematic review
No full textBackground: Pressure injuries in pediatric patients are associated with increased morbidity, mortality, and prolonged hospital stays, making the identification of effective risk assessment tools critical in clinical practice. Accurate risk assessment is essential in clinical practice. Although several assessment tools exist, their applicability and effectiveness vary across pediatric populations. Objective: To identify and evaluate tools designed to assess the risk of pressure injuries in children, focusing on their characteristics, validation populations, reliability, and applicability across different clinical contexts. Design: A systematic review was conducted. Methods: This systematic review (PROSPERO: CRD42024527687) was conducted in accordance with the Cochrane Handbook. Comprehensive searches were performed in five databases—PubMed, Google Scholar, CINAHL, Web of Science, and Embase—for studies published between January 2010 and March 2024. Eligible studies included those describing the development, use, or validation of pressure injury risk assessment tools in children. Two independent reviewers conducted the selection and appraisal process. Methodological quality was assessed using the QUADAS-2 and QAREL checklists, with general reference to COSMIN guidelines. Results: Of 964 records screened, 28 studies met the inclusion criteria, encompassing research from 15 countries, with Brazil being the most represented. Studies focused on pediatric and neonatal intensive care units, general wards, and surgical units. Ten different risk assessment tools were identified, including the Braden Q, Braden QD, and Glamorgan scales. The Braden QD scale—an adaptation of the Braden Q including medical device-related risk—was the most frequently evaluated. Other tools, such as the Pediatric Pressure Ulcer Prediction and Evaluation Tool and the Braden Q+P, were specifically developed or adapted for pediatric and neonatal use. Conclusions: All identified tools demonstrated acceptable validity and inter-rater reliability. However, no single tool proved universally applicable across all pediatric contexts. The Braden QD, Braden Q, and Glamorgan scales emerged as the most comprehensive, particularly in intensive care settings, aligning with National and European Pressure Ulcer Advisory Panel recommendations. Further research is warranted to enhance tool accuracy and contextual adaptability across pediatric care environments. Guidelines: PRISMA
Efficacité d’un programme intégré d’enseignements de la recherche sur l’acquisition de compétences en recherche et les représentations d’étudiants infirmiers en formation initiale : une étude quasi-expérimentale.
No full textInternational audienc
Target product profile for a diagnostic assay to differentiate between bacterial and non-bacterial infections and reduce antimicrobial overuse in resource-limited settings: an expert consensus
No full textAcute fever is one of the most common presenting symptoms globally. In order to reduce the empiric use of antimicrobial drugs and improve outcomes, it is essential to improve diagnostic capabilities. In the absence of microbiology facilities in low-income settings, an assay to distinguish bacterial from non-bacterial causes would be a critical first step. To ensure that patient and market needs are met, the requirements of such a test should be specified in a target product profile (TPP). To identify minimal/optimal characteristics for a bacterial vs. non-bacterial fever test, experts from academia and international organizations with expertise in infectious diseases, diagnostic test development, laboratory medicine, global health, and health economics were convened. Proposed TPPs were reviewed by this working group, and consensus characteristics were defined. The working group defined non-severely ill, non-malaria infected children as the target population for the desired assay. To provide access to the most patients, the test should be deployable to community health centers and informal health settings, and staff should require 90% and >80% for sensitivity and specificity, respectively. Other key characteristics, to account for the challenging environment at which the test is targeted, included: i) time-to-result <10 min (but maximally <2 hrs); ii) storage conditions at 0-40°C, ≤90% non-condensing humidity with a minimal shelf life of 12 months; iii) operational conditions of 5-40°C, ≤90% non-condensing humidity; and iv) minimal sample collection needs (50-100μL, capillary blood). This expert approach to define assay requirements for a bacterial vs. non-bacterial assay should guide product development, and enable targeted and timely efforts by industry partners and academic institutions
Structure-based optimization and binding assays for discovery of tau PET radiotracers: Synthesis and in vivo evaluation of [11C]Z-3272
No full textHuman tau protein has six isoforms, differing in the number of microtubule-binding repeats. Progressive supranuclear palsy (PSP) and corticobasal degeneration (CBD) are primarily 4-repeat (4R)-tauopathies, and Alzheimer’s disease (AD) and chronic traumatic encephalopathy (CTE) are mixed 3R/4R-tau. Here, a promising lead compound for positron emission tomography (PET) imaging of non-AD tauopathies (Z5873993272; (methyl-1-(5-(7-hydroxynaphthalen-2-yl)pyridin-2-yl)piperidine-4-carboxylate; Z-3272), was identified as a potential 4R-tau binding ligand through computational structure-based optimization from the 2D structure of known 4R-tau ligands, followed by iterative competition binding assays. Homologous binding assays in post-mortem AD, PSP, and CBD brain with [3H]Z-3272 provided Kd (nM) values (n = 3) of AD = 1.2 ± 0.1, PSP = 2.7 ± 0.9, and CBD = 1.7 ± 0.1. [11C]Z-3272 was synthesized by 11C-methylation, by reaction of [11C]CH3I with 1-(5-(7-hydroxynaphthalen-2-yl)pyridin-2-yl)piperidine-4-carboxylic acid with NaHCO3 in DMF at 70 ºC for 3 min. The crude product was purified by semi-preparative HPLC and formulated in saline, with an overall synthesis time of 35 min from end of bombardment. [11C]Z-3272 was isolated with a non-decay corrected radiochemical yield of 4 ± 1% (n = 4), high radiochemical purity (>95%), and high molar activity (149 ± 55.5 GBq/μmol). PET imaging following bolus injection of [11C]Z-3272 in rats showed high initial brain radioactivity (>2.3 standardized uptake values (SUV)) with moderate washout (~0.7 SUV at 60 min), however, ex vivo studies revealed the rapid formation of troublesome brain penetrant radiometabolites. Medicinal chemistry optimization is underway to improve binding affinity, selectivity, and metabolic stability.The presentation of the authors' names and (or) special characters in the title of the pdf file of the accepted manuscript may differ slightly from what is displayed on the item page. The information in the pdf file of the accepted manuscript reflects the original submission by the author
School-based prevention of teacher and parental violence against children: Study protocol of a cluster-randomized controlled trial in Tanzania
No full textMattonet K, Kabelege E, Mkinga G, et al. School-based prevention of teacher and parental violence against children: Study protocol of a cluster-randomized controlled trial in Tanzania. BMC public health. 2024;24(1): 2367 (2024).BACKGROUND: Violence against children at home and at school is particularly prevalent in Africa and is associated with adverse and persistent health effects on children. The violence prevention intervention Interaction Competencies with Children-for Teachers (ICC-T) is an effective tool to reduce violence against children by fostering teachers' non-violent communication and interaction skills. To enhance these effects, in the present study, ICC-T will be extended to parents (ICC-P) aiming to increase children's experience of consistent behavior and application of non-violent discipline strategies between teachers and parents.; METHODS: To investigate the effectiveness of the school-based combined implementation of ICC-T and ICC-P, a cluster-randomized controlled trial with 16 primary schools in the urban district of Morogoro in Eastern Tanzania will be conducted. Both quantitative (structured interviews) and qualitative (focus group discussions, in-depth interviews, evaluation forms) methods will be used to investigate the effects on teachers' and parents' violence against children in home and school settings. The intervention implementation will be accompanied by a comprehensive process evaluation to assess the implementation quality of and participants' engagement with ICC-T and ICC-P. Potential downstream effects of violence reduction will be investigated by assessing the children's mental health and well-being.; DISCUSSION: The present study aims to provide evidence for the feasibility, acceptability, and effectiveness of the school-based combined implementation of ICC-T and ICC-P to reduce teacher and parental violence against children and contribute to children's well-being in home and school settings.; TRAIL REGISTRATION: The clinical trial was registered at ClinicalTrials.gov (ClinicalTrials.gov, 2024) under the identifier NCT06369025 (Hecker, Preventing Physical and Emotional Violence by Parents and Teachers in Public Schools in Tanzania (ICC-T/ICC-P_Tanz) (PreVio), 2024) on April 17, 2024. © 2024. The Author(s)
Consensus-based indicators of advanced practice nursing outcomes: Results of a Delphi study in France
No full textInternational audienceBackground: Despite one of the world's most advanced health systems, advanced practice nursing (APN) roles in France are less than a decade old. Globally, APNs strengthen access, quality, and efficiency of care, but sustaining these roles requires demonstrating outcomes meaningful to patients, providers, and policymakers. Purpose: To describe consensus among French stakeholders on patient-and system-level indicators for evaluating APN contributions. Methods: A two-round Delphi process, followed by a nominal group discussion, was conducted. Participants included APNs, nurse managers, physicians, and academics. Candidate indicators, classified using Hamric's framework, were rated on nine-point Likert scales; indicators with ≥75% agreement were validated. Findings: Forty indicators were retained across seven domains, reflecting outcomes such as patient access, continuity, quality of care, collaboration, and leadership. Discussion: Consensus indicators show how APN practice is viewed in France-focused on expertise, coordination, and integration. This aligns with global APN competencies but contrasts with physician-substitution models elsewhere. Conclusion: These validated indicators provide a foundational framework for evaluating APN contributions in France. They offer a strategic tool to support integration, and to inform policy.</div
The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems I: High-contrast Imaging of the Exoplanet HIP 65426 b from 2 to 16 μm
No full textFull list of the authors: Carter, Aarynn L.; Hinkley, Sasha; Kammerer, Jens; Skemer, Andrew; Biller, Beth A.; Leisenring, Jarron M.; Millar-Blanchaer, Maxwell A.; Petrus, Simon; Stone, Jordan M.; Ward-Duong, Kimberly; Wang, Jason J.; Girard, Julien H.; Hines, Dean C.; Perrin, Marshall D.; Pueyo, Laurent; Balmer, William O.; Bonavita, Mariangela; Bonnefoy, Mickael; Chauvin, Gael; Choquet, Elodie; Christiaens, Valentin; Danielski, Camilla; Kennedy, Grant M.; Matthews, Elisabeth C.; Miles, Brittany E.; Patapis, Polychronis; Ray, Shrishmoy; Rickman, Emily; Sallum, Steph; Stapelfeldt, Karl R.; Whiteford, Niall; Zhou, Yifan; Absil, Olivier; Boccaletti, Anthony; Booth, Mark; Bowler, Brendan P.; Chen, Christine H.; Currie, Thayne; Fortney, Jonathan J.; Grady, Carol A.; Greebaum, Alexandra Z.; Henning, Thomas; Hoch, Kielan K. W.; Janson, Markus; Kalas, Paul; Kenworthy, Matthew A.; Kervella, Pierre; Kraus, Adam L.; Lagage, Pierre-Olivier; Liu, Michael C.; Macintosh, Bruce; Marino, Sebastian; Marley, Mark S.; Marois, Christian; Matthews, Brenda C.; Mawet, Dimitri; McElwain, Michael W.; Metchev, Stanimir; Meyer, Michael R.; Molliere, Paul; Moran, Sarah E.; Morley, Caroline V.; Mukherjee, Sagnick; Pantin, Eric; Quirrenbach, Andreas; Rebollido, Isabel; Ren, Bin B.; Schneider, Glenn; Vasist, Malavika; Worthen, Kadin; Wyatt, Mark C.; Briesemeister, Zackery W.; Bryan, Marta L.; Calissendorff, Per; Cantalloube, Faustine; Cugno, Gabriele; De Furio, Matthew; Dupuy, Trent J.; Factor, Samuel M.; Faherty, Jacqueline K.; Fitzgerald, Michael P.; Franson, Kyle; Gonzales, Eileen C.; Hood, Callie E.; Howe, Alex R.; Kuzuhara, Masayuki; Lagrange, Anne-Marie; Lawson, Kellen; Lazzoni, Cecilia; Lew, Ben W. P.; Liu, Pengyu; Llop-Sayson, Jorge; Lloyd, James P.; Martinez, Raquel A.; Mazoyer, Johan; Palma-Bifani, Paulina; Quanz, Sascha P.; Redai, Jea Adams; Samland, Matthias; Schlieder, Joshua E.; Tamura, Motohide; Tan, Xianyu; Uyama, Taichi; Vigan, Arthur; Vos, Johanna M.; Wagner, Kevin; Wolff, Schuyler G.; Ygouf, Marie; Zhang, Xi; Zhang, Keming; Zhang, ZhoujianWe present JWST Early Release Science coronagraphic observations of the super-Jupiter exoplanet, HIP 65426b, with the Near-Infrared Camera (NIRCam) from 2 to 5 μm, and with the Mid-Infrared Instrument (MIRI) from 11 to 16 μm. At a separation of ∼0.″82 (87 − 31 + 108 au), HIP 65426b is clearly detected in all seven of our observational filters, representing the first images of an exoplanet to be obtained by JWST, and the first-ever direct detection of an exoplanet beyond 5 μm. These observations demonstrate that JWST is exceeding its nominal predicted performance by up to a factor of 10, depending on separation and subtraction method, with measured 5σ contrast limits of ∼1 × 10 and ∼2 × 10 at 1″ for NIRCam at 4.4 μm and MIRI at 11.3 μm, respectively. These contrast limits provide sensitivity to sub-Jupiter companions with masses as low as 0.3M beyond separations of ∼100 au. Together with existing ground-based near-infrared data, the JWST photometry are fit well by a BT-SETTL atmospheric model from 1 to 16 μm, and they span ∼97% of HIP 65426b's luminous range. Independent of the choice of model atmosphere, we measure an empirical bolometric luminosity that is tightly constrained between log L bol / L ⊙ = −4.31 and −4.14, which in turn provides a robust mass constraint of 7.1 ± 1.2 M . In totality, these observations confirm that JWST presents a powerful and exciting opportunity to characterize the population of exoplanets amenable to high-contrast imaging in greater detail. © 2023. The Author(s). Published by the American Astronomical Society.We are truly grateful for the countless hours that thousands of people have devoted to the design, construction, and commissioning of JWST. A.L.C. acknowledges the significant harm caused to members of the LGBTQIA+ community in the Department of State and NASA, while under the leadership of James Webb as Under Secretary of State and NASA Administrator, respectively. This project was supported by a grant from STScI (JWST-ERS-01386) under NASA contract NAS5-03127. This work benefited from the 2022 Exoplanet Summer Program in the Other Worlds Laboratory (OWL) at the University of California, Santa Cruz, a program funded by the Heising-Simons Foundation. A.L.C. and this work have greatly benefited from ExoExplorers, which is sponsored by the Exoplanets Program Analysis Group (ExoPAG) and NASA's Exoplanet Exploration Program Office (ExEP). This work has made use of the SPHERE Data Centre, jointly operated by OSUG/IPAG (Grenoble), PYTHEAS/LAM/CeSAM (Marseille), OCA/Lagrange (Nice), Observatoire de Paris/LESIA (Paris), and Observatoire de Lyon/CRAL, and is supported by a grant from Labex OSUG@2020 (Investissements d'avenirANR10 LABX56). S.P. acknowledges the support of ANID-Millennium Science Initiative Program-NCN19_171. M.B.o. acknowledges support in France from the French National Research Agency (ANR) through project grant ANR-20-CE31-0012. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (COBREX, grant agreement No. 885593; EPIC, grant agreement No. 819155)). All the JWST presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute and can be accessed via DOI: 10.17909/2bdf-3p61. This research has also made use of the NASA Astrophysics Data System Bibliographic services and the Python (Van Rossum & Drake 2009) modules listed below
The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256–1257 b
No full textPetrus, Simon et al.-- Full list of authors: Petrus, Simon; Whiteford, Niall; Patapis, Polychronis; Biller, Beth A.; Skemer, Andrew; Hinkley, Sasha; Suárez, Genaro; Palma-Bifani, Paulina; Morley, Caroline V.; Tremblin, Pascal; Charnay, Benjamin; Vos, Johanna M.; Wang, Jason J.; Stone, Jordan M.; Bonnefoy, Mickaël; Chauvin, Gaël; Miles, Brittany E.; Carter, Aarynn L.; Lueber, Anna; Helling, Christiane; Sutlieff, Ben J.; Janson, Markus; Gonzales, Eileen C.; Hoch, Kielan K. W.; Absil, Olivier; Balmer, William O.; Boccaletti, Anthony; Bonavita, Mariangela; Booth, Mark; Bowler, Brendan P.; Briesemeister, Zackery W.; Bryan, Marta L.; Calissendorff, Per; Cantalloube, Faustine; Chen, Christine H.; Choquet, Elodie; Christiaens, Valentin; Cugno, Gabriele; Currie, Thayne; Danielski, Camilla; De Furio, Matthew; Dupuy, Trent J.; Factor, Samuel M.; Faherty, Jacqueline K.; Fitzgerald, Michael P.; Fortney, Jonathan J.; Franson, Kyle; Girard, Julien H.; Grady, Carol A.; Henning, Thomas; Hines, Dean C.; Hood, Callie E.; Howe, Alex R.; Kalas, Paul; Kammerer, Jens; Kennedy, Grant M.; Kenworthy, Matthew A.; Kervella, Pierre; Kim, Minjae; Kitzmann, Daniel; Kraus, Adam L.; Kuzuhara, Masayuki; Lagage, Pierre-Olivier; Lagrange, Anne-Marie; Lawson, Kellen; Lazzoni, Cecilia; Leisenring, Jarron M.; Lew, Ben W. P.; Liu, Michael C.; Liu, Pengyu; Llop-Sayson, Jorge; Lloyd, James P.; Macintosh, Bruce; Mâlin, Mathilde; Manjavacas, Elena; Marino, Sebastián; Marley, Mark S.; Marois, Christian; Martinez, Raquel A.; Matthews, Elisabeth C.; Matthews, Brenda C.; Mawet, Dimitri; Mazoyer, Johan; McElwain, Michael W.; Metchev, Stanimir; Meyer, Michael R.; Millar-Blanchaer, Maxwell A.; Mollière, Paul; Moran, Sarah E.; Mukherjee, Sagnick; Pantin, Eric; Perrin, Marshall D.; Pueyo, Laurent; Quanz, Sascha P.; Quirrenbach, Andreas; Ray, Shrishmoy; Rebollido, Isabel; Adams Redai, Jea; Ren, Bin B.; Rickman, Emily; Sallum, Steph; Samland, Matthias; Sargent, Benjamin; Schlieder, Joshua E.; Stapelfeldt, Karl R.; Tamura, Motohide; Tan, Xianyu; Theissen, Christopher A.; Uyama, Taichi; Vasist, Malavika; Vigan, Arthur; Wagner, Kevin; Ward-Duong, Kimberly; Wolff, Schuyler G.; Worthen, Kadin; Wyatt, Mark C.; Ygouf, Marie; Zurlo, Alice; Zhang, Xi; Zhang, Keming; Zhang, Zhoujian; Zhou, YifanThe unprecedented medium-resolution (R λ ∼ 1500–3500) near- and mid-infrared (1–18 μm) spectrum provided by JWST for the young (140 ± 20 Myr) low-mass (12–20 M Jup) L–T transition (L7) companion VHS 1256 b gives access to a catalog of molecular absorptions. In this study, we present a comprehensive analysis of this data set utilizing a forward-modeling approach applying our Bayesian framework, ForMoSA. We explore five distinct atmospheric models to assess their performance in estimating key atmospheric parameters: T eff, log(g), [M/H], C/O, γ, f sed, and R. Our findings reveal that each parameter's estimate is significantly influenced by factors such as the wavelength range considered and the model chosen for the fit. This is attributed to systematic errors in the models and their challenges in accurately replicating the complex atmospheric structure of VHS 1256 b, notably the complexity of its clouds and dust distribution. To propagate the impact of these systematic uncertainties on our atmospheric property estimates, we introduce innovative fitting methodologies based on independent fits performed on different spectral windows. We finally derived a T eff consistent with the spectral type of the target, considering its young age, which is confirmed by our estimate of log(g). Despite the exceptional data quality, attaining robust estimates for chemical abundances [M/H] and C/O, often employed as indicators of formation history, remains challenging. Nevertheless, the pioneering case of JWST's data for VHS 1256 b has paved the way for future acquisitions of substellar spectra that will be systematically analyzed to directly compare the properties of these objects and correct the systematics in the models. © 2024. The Author(s).This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. We are truly grateful for the countless hours that thousands of people have devoted to the design, construction, and commissioning of JWST. This project was supported by a grant from STScI (JWST-ERS-01386) under NASA contract NAS5-03127. This work benefited from the 2022 Exoplanet Summer Program in the Other Worlds Laboratory (OWL) at the University of California, Santa Cruz, a program funded by the Heising-Simons Foundation. S.P. acknowledges the support of ANID, –Millennium Science Initiative Program–Center Code NCN19_171. This project received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (COBREX; grant agreement No. 885593) and from the ANR project FRAME (ANR-20-CE31-0012). J.M.V. acknowledges support from a Royal Society—Science Foundation Ireland University Research Fellowship (URF\1\221932). S.M. is supported by a Royal Society University Research Fellowship (URF-R1-221669). M.B. received funding from the European Union's Horizon 2020 research and innovation program (AtLAST; grant agreement No. 951815). R.A.M. is supported by the National Science Foundation MPS-Ascend Postdoctoral Research Fellowship under grant No. 2213312. E.G. acknowledges support from the Heising-Simons Foundation for this research. I.R. is supported by grant FJC2021-047860-I and PID2021-127289NB-I00 financed by MCIN/AEI /10.13039/501100011033 and the European Union NextGenerationEU/PRTR. A.Z. and S.P. acknowledge support from ANID—Millennium Science Initiative Program—Center Code NCN2021_080. All of the data presented in this article were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via 10.17909/ceq5-9g20.Peer reviewe
The JWST Early-release Science Program for Direct Observations of Exoplanetary Systems II: A 1 to 20 μm Spectrum of the Planetary-mass Companion VHS 1256–1257 b
No full textMiles, Brittany E. et al.--Full list of authors: Miles, Brittany E.; Biller, Beth A.; Patapis, Polychronis; Worthen., Kadin; Rickman., Emily; Hoch, Kielan K. W.; Skemer, Andrew.; Perrin, Marshall D.; Whiteford, Niall; Chen, Christine H.; Sargent, B.; Mukherjee, Sagnick; Morley, Caroline V.; Moran, Sarah E.; Bonnefoy, Mickael; Petrus, Simon; Carter, Aarynn L.; Choquet, Elodie; Hinkley, Sasha; Ward-Duong, Kimberly; Leisenring, Jarron M.; Millar-Blanchaer, Maxwell A.; Pueyo, Laurent; Ray, Shrishmoy; Sallum, Steph; Stapelfeldt, Karl R.; Stone, Jordan M.; Wang, Jason J.; Absil, Olivier; Balmer, William O.; Boccaletti, Anthony; Bonavita, Mariangela; Booth, Mark; Bowler, Brendan P.; Chauvin, Gael; Christiaens, Valentin; Currie, Thayne; Danielski, Camilla; Fortney, Jonathan J.; Girard, Julien H.; Grady, Carol A.; Greenbaum, Alexandra Z.; Henning, Thomas; Hines, Dean C.; Janson, Markus; Kalas, Paul; Kammerer, Jens; Kennedy, Grant M.; Kenworthy, Matthew A.; Kervella, Pierre; Lagage, Pierre-Olivier; Lew, Ben W. P.; Liu, Michael C.; Macintosh, Bruce; Marino, Sebastian; Marley, Mark S.; Marois, Christian; Matthews, Elisabeth C.; Matthews, Brenda C.; Mawet, Dimitri; McElwain, Michael W.; Metchev, Stanimir; Meyer, Michael R.; Molliere, Paul; Pantin, Eric; Quirrenbach, Andreas; Rebollido, Isabel; Ren, Bin B.; Schneider, Glenn; Vasist, Malavika; Wyatt, Mark C.; Zhou, Yifan; Briesemeister, Zackery W.; Bryan, Marta L.; Calissendorff, Per; Cantalloube, Faustine; Cugno, Gabriele; De Furio, Matthew; Dupuy, Trent J.; Factor, Samuel M.; Faherty, Jacqueline K.; Fitzgerald, Michael P.; Franson, Kyle; Gonzales, Eileen C.; Hood, Callie E.; Howe, Alex R.; Kraus, Adam L.; Kuzuhara, Masayuki; Lagrange, Anne-Marie; Lawson, Kellen; Lazzoni, Cecilia; Liu, Pengyu; Llop-Sayson, Jorge; Lloyd, James P.; Martinez, Raquel A.; Mazoyer, Johan; Quanz, Sascha P.; Redai, Jea Adams; Samland, Matthias; Schlieder, Joshua E.; Tamura, Motohide; Tan, Xianyu; Uyama, Taichi; Vigan, Arthur; Vos, Johanna M.; Wagner, Kevin; Wolff, Schuyler G.; Ygouf, Marie; Zhang, Xi; Zhang, Keming; Zhang, ZhoujianWe present the highest fidelity spectrum to date of a planetary-mass object. VHS 1256 b is a <20 MJup widely separated (∼8'', a = 150 au), young, planetary-mass companion that shares photometric colors and spectroscopic features with the directly imaged exoplanets HR 8799c, d, and e. As an L-to-T transition object, VHS 1256 b exists along the region of the color–magnitude diagram where substellar atmospheres transition from cloudy to clear. We observed VHS 1256 b with JWST's NIRSpec IFU and MIRI MRS modes for coverage from 1 to 20 μm at resolutions of ∼1000–3700. Water, methane, carbon monoxide, carbon dioxide, sodium, and potassium are observed in several portions of the JWST spectrum based on comparisons from template brown dwarf spectra, molecular opacities, and atmospheric models. The spectral shape of VHS 1256 b is influenced by disequilibrium chemistry and clouds. We directly detect silicate clouds, the first such detection reported for a planetary-mass companion. © 2023. The Author(s). Published by the American Astronomical Society.This project was supported by a grant from STScI (JWST-ERS- 01386) under NASA contract NAS5-03127. This work benefited from the 2022 Exoplanet Summer Program in the Other Worlds Laboratory (OWL) at the University of California, Santa Cruz, a program funded by the Heising-Simons Foundation. M.B. acknowledges support in France from the French National Research Agency (ANR) through project grant ANR-20-CE31-0012. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (COBREX; grant agreement n° 885593; EPIC, grant agreement n° 819155). This work has benefited from The UltracoolSheet at http://bit.ly/UltracoolSheet, maintained by Will Best, Trent Dupuy, Michael Liu, Rob Siverd, and Zhoujian Zhang, and developed from compilations by Dupuy & Liu (2012), Dupuy & Kraus (2013), Liu et al. (2016), and Best et al. (2018, 2021). S.-.P acknowledges the support of ANID—Millennium Science Initiative Program–NCN19_171. S.M. is supported by a Royal Society University Research Fellowship. C.D. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709) and the Group project Ref. PID2019-110689RB-I00/AEI/10.13039/501100011033. B.B acknowledges funding by the UK Science and Technology Facilities Council (STFC) grant no. ST/M001229/1.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (SEV-2017-0709)Peer reviewe
The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. III. Aperture Masking Interferometric Observations of the Star HIP 65426 at 3.8μm
No full textRay, Shrishmoy et al.-- Full list of authors: Ray, Shrishmoy; Sallum, Steph; Hinkley, Sasha; Sivaramkrishnan, Anand; Cooper, Rachel; Kammerer, Jens; Greebaum, Alexandra Z.; Thatte, Deeparshi; Stolker, Tomas; Lazzoni, Cecilia; Tokovinin, Andrei; de Furio, Matthew; Factor, Samuel; Meyer, Michael; Stone, Jordan M.; Carter, Aarynn; Biller, Beth; Skemer, Andrew; Suárez, Genaro; Leisenring, Jarron M.; Perrin, Marshall D.; Kraus, Adam L.; Absil, Olivier; Balmer, William O.; Boccaletti, Anthony; Bonavita, Mariangela; Bonnefoy, Mickael; Booth, Mark; Bowler, Brendan P.; Briesemeister, Zackery W.; Bryan, Marta L.; Calissendorff, Per; Cantalloube, Faustine; Chauvin, Gael; Chen, Christine H.; Choquet, Elodie; Christiaens, Valentin; Cugno, Gabriele; Currie, Thayne; Danielski, Camilla; Dupuy, Trent J.; Faherty, Jacqueline K.; Fitzgerald, Michael P.; Fortney, Jonathan J.; Franson, Kyle; Girard, Julien H.; Grady, Carol A.; Gonzales, Eileen C.; Henning, Thomas; Hines, Dean C.; Hoch, Kielan K. W.; Hood, Callie E.; Howe, Alex R.; Janson, Markus; Kalas, Paul; Kennedy, Grant M.; Kenworthy, Matthew A.; Kervella, Pierre; Kuzuhara, Masayuki; Lagrange, Anne-Marie; Lagage, Pierre-Olivier; Lawson, Kellen; Lew, Ben W. P.; Liu, Michael C.; Liu, Pengyu; Llop-Sayson, Jorge; Lloyd, James P.; Macintosh, Bruce; Marino, Sebastian; Marley, Mark S.; Marois, Christian; Martinez, Raquel A.; Matthews, Brenda C.; Matthews, Elisabeth C.; Mawet, Dimitri; Mazoyer, Johan; McElwain, Michael W.; Metchev, Stanimir; Meyer, Michael R.; Miles, Brittany E.; Millar-Blanchaer, Maxwell A.; Molliere, Paul; Moran, Sarah E.; Morley, Caroline V.; Mukherjee, Sagnick; Palma-Bifani, Paulina; Pantin, Eric; Patapis, Polychronis; Petrus, Simon; Pueyo, Laurent; Quanz, Sascha P.; Quirrenbach, Andreas; Rebollido, Isabel; Adams Redai, Jea; Ren, Bin B.; Rickman, Emily; Samland, Matthias; Schlieder, Joshua E.; Schneider, Glenn; Stapelfeldt, Karl R.; Tamura, Motohide; Tan, Xianyu; Uyama, Taichi; Vigan, Arthur; Vasist, Malavika; Vos, Johanna M.; Wagner, Kevin; Wang, Jason J.; Ward-Duong, Kimberly; Whiteford, Niall; Wolff, Schuyler G.; Worthen, Kadin; Wyatt, Mark C.; Ygouf, Marie; Zhang, Xi; Zhang, Keming; Zhang, Zhoujian; Zhou, Yifan; Zurlo, Alice; Sargent, B. A.; Theissen, Christopher A.; Manjavacas, Elena; Lueber, Anna; Kitzmann, Daniel; Sutlieff, Ben J.; Betti, Sarah K.We present aperture masking interferometry (AMI) observations of the star HIP 65426 at 3.8 μm, as part of the JWST Direct Imaging Early Release Science program, obtained using the Near Infrared Imager and Slitless Spectrograph instrument. This mode provides access to very small inner working angles (even separations slightly below the Michelson limit of 0.5λ/D for an interferometer), which are inaccessible with the classical inner working angles of the JWST coronagraphs. When combined with JWST's unprecedented infrared sensitivity, this mode has the potential to probe a new portion of parameter space across a wide array of astronomical observations. Using this mode, we are able to achieve a 5σ contrast of ΔmF380M ∼ 7.62 ± 0.13 mag relative to the host star at separations ≳0
07, and the contrast deteriorates steeply at separations ≲0
07. However, we detect no additional companions interior to the known companion HIP 65426b (at separation ∼0
82 or
). Our observations thus rule out companions more massive than 10–12 MJup at separations ∼10–20 au from HIP 65426, a region out of reach of ground- or space-based coronagraphic imaging. These observations confirm that the AMI mode on JWST is sensitive to planetary mass companions at close-in separations (≳0
07), even for thousands of more distant stars at ∼100 pc, in addition to the stars in the nearby young moving groups and associations, as stated in previous works. This result will allow the planning and successful execution of future observations to probe the inner regions of nearby stellar systems, opening an essentially unexplored parameter space. © 2025. The Author(s).This work is based on observations made with the NASA/
ESA/CSA JWST and obtained from the Mikulski Archive for
Space Telescopes at the Space Telescope Science Institute. The
specific observations analyzed can be accessed via 10.17909/
8by2-x206. We are truly grateful for the countless hours that
thousands of people have devoted to the design, construction,
and commissioning of JWST. We thank the anonymous referee
for comments that have been crucial toward the improvement
of this Letter. This project was supported by a grant from
STScI (JWST-ERS-01386) under NASA contract NAS5-
03127. S.R. was supported by the Global Excellence Award
at the University of Exeter. This work is based in part on
observations obtained at the Southern Astrophysical Research
(SOAR) telescope, which is a joint project of the Ministério da
Ciência, Tecnologia e Inovações (MCTI/LNA) of Brasil, the
US National Science Foundation’s NOIRLab, the University of
North Carolina at Chapel Hill (UNC), and Michigan State
University (MSU). This work has also made use of the
SPHERE Data Centre, jointly operated by OSUG/IPAG
(Grenoble), PYTHEAS/LAM/CeSAM (Marseille), OCA/
Lagrange (Nice), Observatoire de Paris/LESIA (Paris), and
Observatoire de Lyon/CRAL, as well as being supported by a
grant from Labex OSUG@2020 (Investissements d’avenir—
ANR10 LABX56). This work has benefited from the 2022
Exoplanet Summer Program in the Other Worlds Laboratory
(OWL) at the University of California, Santa Cruz, a program
funded by the Heising–Simons Foundation.Peer reviewe
