JWST defines a new era for the data-driven approach of retrieval modelling, which has become a cornerstone tool for the statistical inference of exoplanetary and brown dwarf properties. The Early Release Science program #1386 observations of VHS 1256 b represent a huge jump in data quality, data quantity and spectral coverage for such objects. VHS 1256 b is a young, planetary mass and extremely variable companion that populates the enigmatic L/T cohort of substellar atmospheres. In this first retrieval analysis of the full 1 - 18 micron dataset, we apply the Brewster retrieval framework to the NIRSpec and MIRI spectroscopic observations of VHS 1256 b, exploring a variety of cloud species and structures. Using Delta(BIC) we find that the data is best described by a forsterite (Mg_2SiO_4) and enstatite (MgSiO_3) cloud combination. Our analysis shows a strong preference for patchy silicate cloud coverage, which aligns with VHS 1256 b's extensive and well documented spectral variability. Our retrieval is able to place constraints on the abundances of H_2O, CO, CO_2, CH_4 as well as NH_3. We also show that the retrieved parameters are sensitive to the data used and the relative signal-to-noise ratios between data from different instruments. We conclude with the next steps for the wider retrieval community to better understand young and cloudy exoplanetary atmospheres.

Debris disks, which consist of dust, planetesimals, planets, and gas, offer a unique window into the mineralogical composition of their parent bodies, especially during the critical phase of terrestrial planet formation spanning 10 yr to a few hundred million years. Observations from the Spitzer Space Telescope have unveiled thousands of debris disks, yet systematic studies remain scarce, let alone those with unsupervised clustering techniques. This study introduces CLustering UnsupErvised with Sequencer (CLUES), a novel, nonparametric, fully interpretable machine learning spectral analysis tool designed to analyze and classify the spectral data of debris disks. CLUES combines multiple unsupervised clustering methods with multiscale distance measures to discern new groupings and trends, offering insights into compositional diversity and geophysical processes within these disks. Our analysis allows us to explore a vast parameter space in debris disk mineralogy and also offers broader applications in fields such as protoplanetary disks and solar system objects. This paper details the methodology, implementation, and initial results of CLUES, setting the stage for more detailed follow-up studies focusing on debris disk mineralogy and demographics.

We present aperture masking interferometry (AMI) observations of the star HIP 65426 at 3.8 μ m, 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 0.5 λ / 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 5 σ contrast of Δ m F380M ∼ 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 8 7 − 31 + 108 au ). Our observations thus rule out companions more massive than 10–12 M Jup 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.

Debris disks, which consist of dust, planetesimals, planets, and gas, offer a unique window into the mineralogical composition of their parent bodies, especially during the critical phase of terrestrial planet formation spanning 10 to a few hundred million years. Observations from the Spitzer Space Telescope have unveiled thousands of debris disks, yet systematic studies remain scarce, let alone those with unsupervised clustering techniques. This study introduces (CLustering UnsupErvised with Sequencer), a novel, non-parametric, fully-interpretable machine-learning spectral analysis tool designed to analyze and classify the spectral data of debris disks. combines multiple unsupervised clustering methods with multi-scale distance measures to discern new groupings and trends, offering insights into compositional diversity and geophysical processes within these disks. Our analysis allows us to explore a vast parameter space in debris disk mineralogy and also offers broader applications in fields such as protoplanetary disks and solar system objects. This paper details the methodology, implementation, and initial results of , setting the stage for more detailed follow-up studies focusing on debris disk mineralogy and demographics.

We present JWST MIRI Medium Resolution Spectrograph (MRS) observations of the β Pictoris system. We detect an infrared excess from the central unresolved point source from 5 to 7.5 μ m which is indicative of dust within the inner ∼7 au of the system. We perform point-spread function (PSF) subtraction on the MRS data cubes and detect a spatially resolved dust population emitting at 5 μ m. This spatially resolved hot dust population is best explained if the dust grains are in the small grain limit (2 π a ≪ λ ). The combination of unresolved and resolved dust at 5 μ m could suggest that dust grains are being produced in the inner few astronomical units of the system and are then radiatively driven outwards, where the particles could accrete onto the known planets in the system, β Pictoris b and c. We also report the detection of an emission line at 6.986 μ m that we attribute to [Ar ii ]. We find that the [Ar ii ] emission is spatially resolved with JWST and appears to be aligned with the dust disk. Through PSF-subtraction techniques, we detect β Pictoris b at the 5 σ level in our MRS data cubes and present the first mid-infrared spectrum of the planet from 5 to 7 μ m. The planet’s spectrum is consistent with having absorption from water vapor between 5 and 6.5 μ m. We perform atmosphere model grid fitting of the spectra and photometry of β Pictoris b and find that the planet’s atmosphere likely has a substellar C/O ratio.

We report JWST Mid-Infrared Instrument (MIRI) Medium Resolution Spectrograph (MRS) observations of the beta Pic moving-group member, eta Tel A, along with its brown dwarf binary companion, eta Tel B. Following point-spread-function subtraction, we recover the spatially resolved flux from the debris disk around eta Tel A, along with the position of the companion exterior to the disk. We present a new 5-26 mu m epoch of spectroscopy for the disk, in which we discover a 20 mu m silicate feature, and the first ever 11-21 mu m spectrum of eta Tel B, which indicates a bare photosphere. We derive a new epoch of relative astrometry for the companion, extending the baseline of measurements to 25 yr, and find that it is currently located near the apocenter of an eccentric long-period orbit. The companion's orbit is close enough to the disk that it should significantly perturb the planetesimals within it, resulting in a detectable mid-IR pericenter glow and near alignment with the companion. Contrary to expectations, however, we find that the disk appears to be axisymmetric and potentially misaligned with the companion in the MIRI MRS data. We posit that this may be due to the presence of an additional, as-yet-undetected similar to 0.7-30 M J planet orbiting interior to the disk, with a semimajor axis of similar to 3-19 au.

Modeling observations of the archetypal debris disk around beta Pic, obtained in 2023 January with the MIRI Medium Resolution Spectrograph on board JWST, reveals significant differences compared with that obtained with the Infrared Spectrograph on board Spitzer. The bright 5-15 mu m continuum excess modeled using a similar to 600 K black body has disappeared. The previously prominent 18 and 23 mu m crystalline forsterite emission features, arising from cold dust (similar to 100 K) in the Rayleigh limit, have disappeared and been replaced by very weak features arising from the hotter 500 K dust population. Finally, the shape of the 10 mu m silicate feature has changed, consistent with a shift in the temperature of the warm dust population from similar to 300 to similar to 500 K and an increase in the crystalline fraction of the warm, silicate dust. Stellar radiation pressure may have blown both the hot and the cold crystalline dust particles observed in the Spitzer spectra out of the planetary system during the intervening 20 yr between the Spitzer and JWST observations. These results indicate that the beta Pic system has a dynamic circumstellar environment, and that periods of enhanced collisions can create large clouds of dust that sweep through the planetary system.

The unprecedented medium-resolution ( R λ ∼ 1500–3500) near- and mid-infrared (1–18 μ m) 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.

We present a JWST imaging survey of I Zw 18, the archetypal extremely metal-poor, star-forming (SF), blue compact dwarf galaxy. With an oxygen abundance of only ∼3% Z _⊙ , it is among the lowest-metallicity systems known in the local Universe, and is, therefore, an excellent accessible analog for the galactic building blocks which existed at early epochs of ionization and star formation. These JWST data provide a comprehensive infrared (IR) view of I Zw 18 with eight filters utilizing both Near Infrared Camera (F115W, F200W, F356W, and F444W) and Mid-Infrared Instrument (F770W, F1000W, F1500W, and F1800W) photometry, which we have used to identify key stellar populations that are bright in the near- and mid-IR. These data allow for a better understanding of the origins of dust and dust-production mechanisms in metal-poor environments by characterizing the population of massive, evolved stars in the red supergiant (RSG) and asymptotic giant branch (AGB) phases. In addition, it enables the identification of the brightest dust-enshrouded young stellar objects (YSOs), which provide insight into the formation of massive stars at extremely low metallicities typical of the very early Universe. This paper provides an overview of the observational strategy and data processing, and presents first science results, including identifications of dusty AGB, RSG, and bright YSO candidates. These first results assess the scientific quality of JWST data and provide a guide for obtaining and interpreting future observations of the dusty and evolved stars inhabiting compact dwarf SF galaxies in the local Universe.

In this work, we present spectra of 11 young stellar objects (YSOs) taken with the Mid-Infrared Instrument / Medium Resolution Spectroscopy (MRS) instrument on board the James Webb Space Telescope (JWST). The YSOs are located in the N79 region of the Large Magellanic Cloud (LMC), an active star-forming region with hundreds of Spitzer- and Herschel-identified YSOs and host to super star cluster (SSC) candidate H72.97-69.39. The three giant molecular clouds in N79 (East, West, and South) have varying star formation rates and stellar populations. MRS follow-up observations of four Spitzer-identified YSOs in N79 East, West, and South have revealed that what seemed to be a single, massive YSO is actually a cluster of YSOs. We discuss the emission and absorption lines of six YSOs that have complete or almost-complete spectral coverage from 4.9–27.9 μ m. YSO Y3, located in N79 East, is the youngest source in this study and likely to be less than 10,000 yr old, as inferred from the prominent CH _4 , NH _3 , CH _3 OH, CH _3 OCHO, and CO _2 ice absorption features. The most luminous source is the central ionizing YSO of SSC H72.97-69.39, Y4, which has dozens of fine-structure and H _2 emission lines. Unlike the other YSOs in this work, Y4 has no polyaromatic hydrocarbon emission lines, due to the intense ionizing radiation destroying these large carbon-chain molecules. The mass accretion rates based on the H i (7-6) line luminosities of YSOs Y1, Y2, Y4, and Y9 range between 1.22 × 10 ^−4 –1.89 × 10 ^−2 M _⊙ yr ^−1 . For the first time in the mid-infrared, we are able to resolve individual high-mass protostars forming in small clusters in an extragalactic environment like the LMC.

We present 102 embedded young stellar object (YSO) candidates associated with the H72.97-69.39 super star cluster (SSC) in the Large Magellanic Cloud (LMC). With the use of the James Webb Space Telescope Mid-Infrared Instrument (MIRI) imaging mode, we utilize an F770W - F1000W versus F1000W color-magnitude diagram to select 70 YSO candidates. An additional 27 YSO candidates are selected based on model fitting using the four MIRI imaging filters employed for this study (F770W, F1000W, F1500W, and F2100W). The central region of H72.97-69.39 is saturated in MIRI imaging, however it is covered by observations made with the Medium Resolution Spectrometer (MRS), leading to the identification of five additional massive YSOs. The total star formation rate inferred based on the 102 YSO candidates is 0.02 M circle dot yr-1, similar to other high-mass star-forming regions in the LMC which have undergone several generations of starburst events. Due to its young age, however, H72.97-69.39's stellar production rate is expected to increase. The central five YSOs identified with MRS have masses ranging from 21.1 to 40.3 M circle dot and total luminosity over 106 L circle dot, making H72.97-69.39 a very compact and luminous star-forming region similar to other known SSCs. We theorize that the central five massive YSOs were formed via filamentary collision, while other YSO candidates of varying masses were triggered by wind, radiation, and expanding H ii shells based on their spatial distribution.

NGC 6822 is a nearby (\sim490 kpc) non-interacting low-metallicity (0.2 Z_\odot) dwarf galaxy which hosts several prominent Hii regions, including sites of highly embedded active star formation. In this work, we present an imaging survey of NGC 6822 conducted with the NIRCam and MIRI instruments onboard JWST. We provide a description of the data reduction, source extraction, and stellar population identifications from combined near- and mid-infrared (IR) photometry. Our NIRCam observations reach seven magnitudes deeper than previous JHKs surveys of this galaxy, which were sensitive to just below the tip of the red giant branch (TRGB). These JWST observations thus reveal for the first time in the near-IR the red clump stellar population and extend nearly three magnitudes deeper. In the mid-IR, we observe roughly two magnitudes below the TRGB with the MIRI F770W and F1000W filters. With these improvements in sensitivity, we produce a catalogue of \sim900,000 point sources over an area of \sim 6.0 x 4.3 arcmin2. We present several NIRCam and MIRI colour-magnitude diagrams and discuss which colour combinations provide useful separations of various stellar populations to aid in future JWST observation planning. Finally, we find populations of carbon- and oxygen-rich asymptotic giant branch stars which will assist in improving our understanding of dust production in low-metallicity, early Universe analogue galaxies.

We present a performance analysis for the aperture masking interferometry (AMI) mode on board the James Webb Space Telescope Near Infrared Imager and Slitless Spectrograph (JWST/NIRISS). Thanks to self-calibrating observables, AMI accesses inner working angles down to and even within the classical diffraction limit. The scientific potential of this mode has recently been demonstrated by the Early Release Science (ERS) 1386 program with a deep search for close-in companions in the HIP 65426 exoplanetary system. As part of ERS 1386, we use the same data set to explore the random, static, and calibration errors of NIRISS AMI observables. We compare the observed noise properties and achievable contrast to theoretical predictions. We explore possible sources of calibration errors and show that differences in charge migration between the observations of HIP 65426 and point-spread function calibration stars can account for the achieved contrast curves. Lastly, we use self-calibration tests to demonstrate that with adequate calibration NIRISS F380M AMI can reach contrast levels of ∼9–10 mag at ≳ λ / D . These tests lead us to observation planning recommendations and strongly motivate future studies aimed at producing sophisticated calibration strategies taking these systematic effects into account. This will unlock the unprecedented capabilities of JWST/NIRISS AMI, with sensitivity to significantly colder, lower-mass exoplanets than lower-contrast ground-based AMI setups, at orbital separations inaccessible to JWST coronagraphy.

We present an imaging survey of the Spitzer I star-forming region in NGC 6822 conducted with the NIRCam and MIRI instruments on board JWST. Located at a distance of 490 kpc, NGC 6822 is the nearest non-interacting low-metallicity (∼0.2 Z _⊙ ) dwarf galaxy. It hosts some of the brightest known H ii regions in the local universe, including recently discovered sites of highly embedded active star formation. Of these, Spitzer I is the youngest and most active, and houses 90 color-selected candidate young stellar objects (YSOs) identified from Spitzer Space Telescope observations. We revisit the YSO population of Spitzer I with these new JWST observations. By analyzing color–magnitude diagrams constructed with NIRCam and MIRI data, we establish color selection criteria and construct spectral energy distributions to identify candidate YSOs and characterize the full population of young stars, from the most embedded phase to the more evolved stages. In this way, we have identified 140 YSOs in Spitzer I. Comparing to previous Spitzer studies of the NGC 6822 YSO population, we find that the YSOs we identify are fainter and less massive, indicating that the improved resolution of JWST allows us to resolve previously blended sources into multiple objects.

We present a JWST imaging survey with NIRCam and MIRI of NGC 346, the brightest star-forming region in the Small Magellanic Cloud (SMC). By combining aperture and point spread function (PSF) photometry of eleven wavelength bands across these two instruments, we have detected more than 200,000 unique sources. Using near-infrared (IR) color analysis, we observe various evolved and young populations, including 196 young stellar objects (YSOs) and pre-main sequence stars suitable for forthcoming spectroscopic studies. We expand upon this work, creating mid-IR color-magnitude diagrams and determining color cuts to identify 833 reddened sources which are YSO candidates. We observe that these candidate sources are spatially associated with regions of dusty, filamentary nebulosity. Furthermore, we fit model YSO spectral energy distributions (SEDs) to a selection of sources with detections across all of our MIRI bands. We classify with a high degree of confidence 23 YSOs in this sample and estimate their radii, bolometric temperatures, luminosities, and masses. We detect YSOs approaching 1 solar mass, the lowest-mass extragalactic YSOs confirmed to date.

Low-mass stars are the most numerous stellar objects in the Universe. Before the James Webb Space Telescope (JWST), we had limited knowledge of how planetary systems around low-mass stars could form at subsolar metallicities. Here we present JWST observations of NGC 346, a star-forming region in the metal-poor Small Magellanic Cloud, revealing a substantial population of subsolar-mass young stellar objects (YSOs) with an infrared excess. We notice that continuing low-mass star formation is concentrated along dust filaments. We detected roughly 500 YSOs and pre-main-sequence (PMS) stars from more than 45,000 unique sources, using all four NIRCam wide filters with deep, high-resolution imaging. From these observations, we construct detailed near-infrared colour–magnitude diagrams with which preliminary categorizations of YSO classes are made. For the youngest, most deeply embedded objects, JWST/NIRCam is ten magnitudes more sensitive than Spitzer observations at comparable wavelengths, and reaches two magnitudes fainter than Hubble Space Telescope for more evolved PMS sources, corresponding to roughly 0.1 M ⊙ . The infrared sensitivity and resolution of JWST allows us to detect embedded low-mass star formation in an extragalactic environment. Furthermore, evidence of infrared excesses and accretion suggests that the dust required for rocky planet formation is present at metallicities as low as 0.2 Z ⊙ , which are akin to those in place at cosmic noon.

JWST observations of NGC 346, a star-forming region in the metal-poor Small Magellanic Cloud, reveal a substantial population of sub-solar mass young stellar objects (YSOs) with IR excess. We detected $\sim$500 YSOs and pre main sequence (PMS) stars from more than 45,000 unique sources utilizing all four NIRCam wide filters with deep, high-resolution imaging, where ongoing low-mass star formation is concentrated along dust filaments. From these observations, we construct detailed near-IR colour-magnitude diagrams with which preliminary categorizations of YSO classes are made. For the youngest, most deeply-embedded objects, JWST/NIRCam reaches over 10 magnitudes below Spitzer observations at comparable wavelengths, and two magnitudes fainter than HST for more-evolved PMS sources, corresponding to $\sim$0.1 M$_\odot$. For the first time in an extragalactic environment, we detect embedded low-mass star-formation. Furthermore, evidence of IR excess and accretion suggests that dust required for rocky planet formation is present at metallicities as low as 0.2 $Z_\odot$.

Journal Article Corrected proof Scientific Business Abstracts Get access Keith Siew, Keith Siew University College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Vaksha Patel, Vaksha Patel University College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Jasminka Zimmermann, Jasminka Zimmermann University College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Michael Vaughan, Michael Vaughan University of Cork, Eire Search for other works by this author on: Oxford Academic PubMed Google Scholar Christopher Cheshire, Christopher Cheshire Crick Institute, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Angela Kubik, Angela Kubik NASA Ames Research Centre, USA Search for other works by this author on: Oxford Academic PubMed Google Scholar Rebecca Finch, Rebecca Finch University of Staffordshire, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Zhongwang Li, Zhongwang Li University College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Selin Altinok, Selin Altinok University North Carolina, Chapel Hill, USA Search for other works by this author on: Oxford Academic PubMed Google Scholar Willian De Silvera, Willian De Silvera University of Staffordshire, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar ... 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other works by this author on: Oxford Academic PubMed Google Scholar Michael Lean, Michael Lean University of Glasgow, Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Roy Taylor, Roy Taylor University of Glasgow, Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Naveed Sattar, Naveed Sattar University of Glasgow, Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Alasdair Mcintosh, Alasdair Mcintosh University of Glasgow, Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Wilma Leslie, Wilma Leslie University of Glasgow, Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Louise McCombie, Louise McCombie University of Glasgow, Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Naomi Brosnahan, Naomi Brosnahan University of Glasgow, Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar George Thom, George Thom University of Glasgow, Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Alison Barnes, Alison Barnes University of Glasgow, Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Keaton Irvine, Keaton Irvine University of Glasgow, Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Sarah Cook, Sarah Cook School of Public Health & National Heart and Lung InstituteImperial College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Sara Hatem, Sara Hatem Usher Institute, University of Edinburgh, Edinburgh, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Sean Scully, Sean Scully Swansea University Medical School, Swansea, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Hywel T Evans, Hywel T Evans Swansea University Medical School, Swansea, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Ian Farr, Ian Farr Swansea University Medical School, Swansea, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Chris Orton, Chris Orton Swansea University Medical School, Swansea, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar David V Ford, David V Ford Swansea University Medical School, Swansea, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Aziz Sheikh, Aziz Sheikh Usher Institute, University of Edinburgh, Edinburgh, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Jennifer K Quint, Jennifer K Quint School of Public Health & National Heart and Lung InstituteImperial College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar David Ferenbach, David Ferenbach University of Edinburgh, Edinburgh, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Lowri Allen, Lowri Allen Diabetes Research Group, Cardiff University, Cardiff, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Georgina Mortimer, Georgina Mortimer Diabetes and Metabolism, Bristol Medical School, University of Bristol, Bristol, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Rana Fareed, Rana Fareed Diabetes and Metabolism, Bristol Medical School, University of Bristol, Bristol, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Claire Williams, Claire Williams Diabetes and Metabolism, Bristol Medical School, University of Bristol, Bristol, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Steve Bain, Steve Bain Biomedical Sciences, Swansea University, Swansea, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Colin Dayan, Colin Dayan Diabetes Research Group, Cardiff University, Cardiff, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Diane Fraser, Diane Fraser Institute of Biomedical and Clinical Science, University of Exeter, Exeter, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar William Hagopian, William Hagopian Pacific North West Research Institute, Seattle, United States of America Search for other works by this author on: Oxford Academic PubMed Google Scholar Richard Oram, Richard Oram Institute of Biomedical and Clinical Science, University of Exeter, Exeter, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Kathleen Gillespie, Kathleen Gillespie Diabetes and Metabolism, Bristol Medical School, University of Bristol, Bristol, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Omid Sadeghi-Alavijeh, Omid Sadeghi-Alavijeh University College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Melanie Chan, Melanie Chan University College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Shabbir Moochhala, Shabbir Moochhala University College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Sarah Howles, Sarah Howles University of Oxford, Oxford, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Daniel Gale, Daniel Gale University College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Detlef Böckenhauer, Detlef Böckenhauer University College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Rachel Jennings, Rachel Jennings Faculty of Biology, Medicine and Health, University of Manchester, Manchester, United KingdomEndocrinology department, Manchester University NHS Foundation Trust, Manchester, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Syed Murtuza Baker, Syed Murtuza Baker Faculty of Biology, Medicine and Health, University of Manchester, Manchester, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Peyman Zarrineh, Peyman Zarrineh Faculty of Biology, Medicine and Health, University of Manchester, Manchester, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Ali Al-Banaki, Ali Al-Banaki Faculty of Biology, Medicine and Health, University of Manchester, Manchester, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Aoibheann Mullan, Aoibheann Mullan Faculty of Biology, Medicine and Health, University of Manchester, Manchester, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Maria Alexandra Goncalves, Maria Alexandra Goncalves Faculty of Biology, Medicine and Health, University of Manchester, Manchester, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Neil Hanley, Neil Hanley Faculty of Biology, Medicine and Health, University of Manchester, Manchester, United KingdomEndocrinology department, Manchester University NHS Foundation Trust, Manchester, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Caroline Watson, Caroline Watson University of Cambridge, Cambridge, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Sophia Apostolidou, Sophia Apostolidou MRC Clinical Trials Unit at UCL, Institute of Clinical Trials and Methodology, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Usha Menon, Usha Menon MRC Clinical Trials Unit at UCL, Institute of Clinical Trials and Methodology, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Jamie Blundell, Jamie Blundell University of Cambridge, Cambridge, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Claire Shovlin, Claire Shovlin National Heart and Lung Institute, Imperial College London, London, United KingdomNIHR Imperial Biomedical Research Centre, London, UKImperial College Healthcare NHS Trust, London, UK Search for other works by this author on: Oxford Academic PubMed Google Scholar Maria Bernabeu-Herrero, Maria Bernabeu-Herrero National Heart and Lung Institute, Imperial College London, London, United KingdomNIHR Imperial Biomedical Research Centre, London, UK Search for other works by this author on: Oxford Academic PubMed Google Scholar Kinshuk Jain, Kinshuk Jain National Heart and Lung Institute, Imperial College London, London, United Kingdom Search for other works by this author on: Oxford Academic PubMed Google Scholar Michaela Aldred, Michaela Aldred Indiana University School of Medicine, Indianapolis, USA Search for other works by this author on: Oxford Academic PubMed Google Scholar Adrianna Bielowka, Adrianna Bielowka National Heart and Lung Institute, Imperial College London, London, United KingdomNIHR Imperial Biomedical Research Centre, London, UK Search for other works by this author on: Oxford Academic PubMed Google Scholar Ian Mackay, Ian Mackay Charing Cross and Royal Brompton Hospitals, London, United Kingdom Search for other works by this author on: 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Universitat de Barcelona, Artificial Intelligence in Medicine Lab (BCN-AIM) Search for other works by this author on: Oxford Academic PubMed Google Scholar Andre Altman, Andre Altman Department of Medical Physics and Biomedical Engineering, Centre for Medical Image Computing (CMIC) Search for other works by this author on: Oxford Academic PubMed Google Scholar Charalambos Antoniades, Charalambos Antoniades Division of Cardiovascular Medicine, Radcliffe Department of Medicine, University of Oxford, National Institute for Health Research Oxford Biomedical Research Centre, Oxford University Hospitals NHS Foundation Trust Search for other works by this author on: Oxford Academic PubMed Google Scholar Stefan Neubauer, Stefan Neubauer Division of Cardiovascular Medicine, Radcliffe Department of Medicine, University of Oxford, National Institute for Health Research Oxford Biomedical Research Centre, Oxford University Hospitals NHS Foundation Trust Search for other works by this author on: 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on: Oxford Academic PubMed Google Scholar Elaine Butterly, Elaine Butterly University of Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Sarah Wild, Sarah Wild University of Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Frances Mair, Frances Mair University of Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Bruce Guthrie, Bruce Guthrie University of Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Katie Gillies, Katie Gillies University of Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Sophie Dias, Sophie Dias University of Glasgow, Scotland Search for other works by this author on: Oxford Academic PubMed Google Scholar Nicky Welton, Nicky Welton University of Glasgow, Scotland Search for other works by this author on: Oxford Academic 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The unprecedented medium-resolution (R 1500-3500) near- and mid-infrared (1-18um) spectrum provided by JWST for the young (140+/-20Myr) low-mass (12-20MJup) L-T transition (L7) companion VHS1256b gives access to a catalogue of molecular absorptions. In this study, we present a comprehensive analysis of this dataset utilizing a forward modelling approach, applying our Bayesian framework, ForMoSA. We explore five distinct atmospheric models to assess their performance in estimating key atmospheric parameters: Teff, log(g), [M/H], C/O, gamma, fsed, 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 VHS1256b, 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 Teff 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 VHS1256b 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.

12CO and 13CO lines, as well as a mm-wave continuum, have been observed for a sample of 22 OH/IR stars in directions within 2 degrees of the Galactic Centre. Photometry data have been gathered from the literature to construct SEDs and to determine pulsational variability. Radiative transfer models have been used to interpret the data. All stars in the sample were detected in at least one CO line, and 8 objects were detected in 324 GHz continuum. Based on luminosity criteria, the sample is divided into 17 objects that most likely lie within the inner Galactic Bulge, and 5 objects that are most likely foreground objects. The median luminosity of the inner-Galactic-Bulge objects, 5600 Lsun, corresponds to an initial mass in the range 1.2-1.6 Msun, indicating that these OH/IR stars descend from solar-type stars. The objects in this sub-sample are further divided into two classes based on their SED characteristics: 11 objects have SEDs that are well matched by models invoking dust envelopes extending from a few stellar radii and outwards, while 6 objects are better modelled as having detached dust envelopes with inner radii in the range 200-600 au and warmer central stars. The former objects have periodic variability, while the latter objects are predominantly non-periodic. The median gas-mass-loss rate, gas terminal expansion velocity, gas-to-dust mass ratio, and circumstellar 12CO/13CO abundance ratio have been estimated to be 2x10-5 Msun/yr, 18 km/s, 200 (excluding the sources with detached dust envelopes, which show markedly lower gas-to-dust ratios), and 5, respectively, for the inner-Galactic-Bulge objects. The inner-Galactic-Bulge OH/IR stars studied here constitute an excellent sample of equidistant objects for the purpose of understanding the evolution of the mass-loss-rate characteristics at the tip of the AGB.