dataesr/scientific-paragraphs-categorization huggingface dataset:
I) Scatterplot of log 2 fold-change in expression between breast/lung cancer cell lines with and without Amp1q (x-axis) and differential dependency (i. e. , the difference between median dependency estimates in breast/lung cancer cell lines with and without Amp1q) in the DepMap CRISPR screen dataset (yaxis). Genes with a positive fold-change are colored in red, while genes with a negative fold-change are colored in blue. Genes that hit in both this dataset and the MM genomewide screens are marked with yellow stars. J) Scatterplot of log 2 fold-change in expression between breast/lung cancer cell lines with and without Amp1q (x-axis) and differential dependency (i. e. , the difference between median dependency estimates in breast/lung cancer cell lines with and without Amp1q) in the targeted shRNA screen dataset (y-axis).
F) GSEA results for the PI3K/Akt/mTOR Hallmark pathway in subclones with Amp1q across all six samples. G) Scatterplot of the median log 2 fold-change in expression between subclones with and without Amp1q (x-axis) and differential dependency (i. e. , the difference between median dependency estimates in MM cell lines with and without Amp1q) in the genome-wide MM screens (y-axis). Genes with a positive fold-change are colored in red; genes with a negative fold-change are colored in blue. Genes with a differential dependency of at least 0. 2 or genes that hit in all three datasets are labeled. H) Barplot of gene set enrichment analysis results for pathways with hypergeometric q < 0. 05. In light blue, the number of genes in the gene set (black letters); in purple, the number of hits in a given gene set (white letters).
ACKNOWLEDGEMENT The authors would like to thank the patients who participated in the PCROWD study. Additionally, the authors would like to thank  Anna V. Justis, PhD , for medical editing support, and  Sarah Nersersian, MSc , for illustration support. This research was supported in part by the  National Institutes of Health  ( R35CA2263817-01A1 ). R. S. P. is supported by the  MMRF   Research Fellowship Award , the  International Waldenstrom's Macroglobulinemia Foundation 's  Robert A. Kyle Award , the  Claudia Adams-Barr Award for Innovative Basic Cancer Research , the  Hellenic Society of Hematology , and the  International Myeloma Society. G. G. is partially supported by the  Paul C. Zamecnik Chair in Oncology at Massachusetts General Hospital Cancer Center. M. S. D. is supported by the  National Institutes of Health  ( R01CA266298-01A1 ).
G) Scatterplot of the median log 2 fold-change in expression between subclones with and without Amp1q (x-axis) and differential dependency (i. e. , the difference between median dependency estimates in MM cell lines with and without Amp1q) in the genome-wide MM screens (y-axis). Genes with a positive fold-change are colored in red; genes with a negative fold-change are colored in blue. Genes with a differential dependency of at least 0. 2 or genes that hit in all three datasets are labeled. H) Barplot of gene set enrichment analysis results for pathways with hypergeometric q < 0. 05. In light blue, the number of genes in the gene set (black letters); in purple, the number of hits in a given gene set (white letters).
Subject Selection Subjects were eligible for trial enrollment (NCT03878420) if they were at least 50 years of age, had a diagnosis of non-exudative AMD as defined by the presence of drusen and/or geographic atrophy (GA) with BCVA scores as determined by the Early Treatment Diabetic Retinopathy Study (ETDRS) Visual Acuity chart with a letter score between 50 and 80 (Snellen equivalent of 20/25 to 20/100). Subjects were excluded from enrollment with current or a history of macular neovascularization, presence of center involving GA within the central ETDRS 500 lm diameter, a history of epilepsy, other significant retinal disease or other significant disease. Subjects could use AREDS vitamin supplementation; however, no change in supplements 1 month before the study and during the study trial was allowed.
Study Design Subjects with non-exudative AMD who met the inclusion criteria, had none of the exclusion criteria and provided their written informed consent were enrolled into the study across seven centers throughout Europe (UK, France, Spain, Germany, Italy). Subjects were treated with the Valeda Light Delivery System (Valeda) and received PBM or sham treatment for a total of nine treatments over a 3-to 5-week period. There was a re-treatment period starting at the 4-month time point to include nine additional treatment visits, repeated at 8 months. Data were collected during 31 visits over the course of the 10-month study (Fig. 1 ). Subjects were assessed for standard visual outcome measurements including ETDRS BCVA, Mars letter CS, Radner reading chart and Visual Function Questionnaire-25 (VFQ-25) test at selected time intervals.
Subjects also underwent eye examinations, fundus photographs, Heidelberg optical coherence tomography (OCT) and fundus autofluorescence (FAF) imaging and optional Optos UWF (ultra-widefield) color and UWF autofluorescence imaging of the retina at selected time intervals. All subjects were assessed with 20 9 20-mm highspeed SD-OCT volume scans and FAF imaging using 488-nm wavelength (Spectralis OCT; Heidelberg Engineering, Heidelberg, Germany) as described previously  [21]. For the GA area and growth assessment the Heidelberg Engineering Region Finder Analyzer software (Region Finder Software; Heidelberg Engineering, Germany) was used. This software measures the areas of homogeneous FAF hypoautofluorescence in a semiautomated way, which corresponds to the GA lesions  [17]. It further allows assessment of the potential growth over time (e.
g. , Figs. 4, 5 ). The subRPE macular drusen volume was assessed within the whole 6 9 6-mm ETDRS grid, while the mean central subfield subRPE drusen thickness was analyzed within the central 1-mm ETDRS subfield. The automated and manually corrected alignment of the Bruch's membrane and the RPE of the inbuilt Heidelberg segmentation software was employed for the assessment of respective parameters. An independent, masked imaging center reviewed and graded all images to determine disease etiology and inclusion/exclusion criterion and to assess the here presented morphological changes. The primary outcome evaluated PBM effect from baseline to month 9 within PBM-treated subjects. Secondary outcomes included other investigations on patient-reported and imaging outcomes in PBM subjects and between PBM and sham groups at various time points.
In addition, patient adherence to the in-clinic treatment visits 39/week for 3-5 weeks were well attended, when possible, during extreme disruptions due to the COVID-19 pandemic. Repeat in-clinic treatment may prove problematic for patient compliance; however, the high compliance observed in the current study (when not disrupted by COVID-19) mirrors results from the prior LIGHTSITE I study  [21]. LIGHTSITE II further highlights the positive safety and tolerability of repeated PBM treatment in the eye. Limitations exist within the LIGHTSITE II study that need to be considered when interpreting the data. As mentioned, the interference from the COVID-19 pandemic significantly interrupted the study design, adherence to the proposed protocol, data collection and statistical analysis. The study was not sufficiently powered with the recruitment of 44 subjects and was considered a feasibility study with three rounds of treatment.
All subjects provided informed consent to participate in the study. Clinicaltrial. Gov Registration Identifier: NCT03878420. Data Availability. The datasets generated during and/or analyzed during the current study are available from the corresponding author on reasonable request. Open Access. This article is licensed under a Creative Commons Attribution-NonCommercial 4. 0 International License, which permits any non-commercial use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material.
The study was stopped at the rst interim analysis for futility. The risk of death was higher with the OA, but did not reach statistical signi cance, again leaving uncertainty as to how to treat patients  (52). Otherwise, there is no prospective randomized data and results other than that which will be collected in the COOL trial. Negative Pressure Peritoneal Therapy (NPPT) Newer non-commercial and commercial negative pressure peritoneal therapy (NPPT) systems are now available for OA and may reduce the risks of enterocutaneous stula and facilitate enhanced delivery of negative peritoneal pressure to the peritoneal cavity  (32, 53, 54). In one of the largest contemporary OA databases no difference in enterocutaneous stula rates were noted related to the type of temporary abdominal closure dressing used  (55).
g. antibiotic treatment, blood transfusion or parenteral nutrition; Grade IIIa = requiring surgical, endoscopic or radiologic intervention without general anesthesia and IIIb under general anesthesia; Grade IVa = life threatening complication requiring IC/ICU management with single organ dysfunction and IVb with multiorgan dysfunction; Grade V = death of patient)  (68, 69). All data are entered into a secure web application for building and managing online surveys and databases (REDCap) maintained by the University of Calgary. While the COOL Trial Case Report form is available in paper format (Figure  3. ), investigators are encouraged to submit data directly into the online format securely hosted in REDCap (R esearch E lectronic D ata Cap ture). The Case Report Form (CRF) was also recently simpli ed to become more pragmatic in anticipation of an increasingly global participation with less dedicated research administration.
Funding: No funding was received for the conduct of this analysis or the preparation of this Manuscript. The COOL Investigators as an entity were supported to conduct a Protocol Development Meeting in Parma Italy on November 26 2017 through an unrestricted grant from the  Acelity Corporation  in which Inclusion Criteria for Closed Or Open after  Laparotomy (COOL) for Source Control in Severe Complicated Intra-Abdominal Sepsis  (https://clinicaltrials. gov/ct2/show/NCT03163095) trial was discussed. The  3M/Acelity Corporation  provided limited nancial support for the  COOL  trial under contract  032519-000/2050  until unilateral cancelation on August 19 2022. The COOL trial has also received unrestricted support from the  Abdominal Compartment Society  and the  Andrew W Kirkpatrick Professional Corporation.
Recent JWST/NIRCam imaging taken for the ultra-deep UNCOVER program reveals a very red dropout object at z phot ; 7. 6, triply imaged by the galaxy cluster A2744 (z d = 0. 308). All three images are very compact, i. e. , unresolved, with a delensed size upper limit of r e  35 pc. The images have apparent magnitudes of m F444W ∼ 25-26 AB, and the magnification-corrected absolute UV magnitude of the source is M UV,1450 = -16. 81 ± 0. 09. From the sum of observed fluxes and from a spectral energy distribution (SED) analysis, we obtain estimates of the bolometric luminosities of the source of L bol  10 43 erg s -1 and L bol ∼ 10 44 -10 46 erg s -1 , respectively. Based on its compact, point-like appearance, its position in color-color space, and the SED analysis, we tentatively conclude that this object is a UV-faint dust-obscured quasar-like object, i.
Data The main data set used in this work are the recent observations taken with the Near Infrared Camera (NIRCam;  Rieke et al. 2005 Rieke et al. , 2023) )  aboard JWST, carried out in the framework of the Ultra-deep NIRSpec and NIRCam ObserVations before the Epoch of Reionization (UNCOVER) program (Program ID: GO 02561; PIs: I. Labbé & R. Bezanson; Bezanson et al. 2022). The JWST UNCOVER program was designed to observe the strong lensing (SL) galaxy cluster A2744 with NIRCam to unprecedented depths in the F115W, F150W, F200W, F277W, F356W, F410M, and F444W bands and over a large area of ∼45 arcmin 2 around the cluster. A2744 has also recently been observed in two other JWST programs: the early release (ERS) survey GLASS-JWST (Program ID: ERS 1324; PI: T. Treu; Treu et al. 2022 ) and a director's discretionary time (DDT) program targeting a lensed supernova (Program ID: DD 2756; PI: P.
Kelly). The NIRCam imaging from these programs is also folded into the UNCOVER mosaics used in this work. The data were reduced and drizzled into mosaics with the Grism redshift and line analysis software for space-based spectroscopy (grizli; 30 Brammer  et al. 2022). The final mosaics used here have pixel scales of 0 02 and 0 04 in the short-and long-wavelength channels (SW and LW), respectively, and sum up ∼16 hr exposure time per filter on average, achieving 5σ depths of 29-30 AB magnitudes, or ∼32 AB with lensing magnification. A photometric catalog of objects detected in the whole UNCOVER field is also generated in the UNCOVER program and is released with its other data products  (Weaver et al. 2023). The catalog includes photometric redshift estimates for each identified object and lists the lensing magnifications from the UNCOVER lensing model  (Furtak et al.
2023c) , which is described in more detail in Section 3. 4. We refer the reader to  Bezanson et al. (2022)  and  Weaver et al. (2023)  for more details of the data reduction, field depth in the different bands, source extraction, and catalog assembly. All UNCOVER data products are publicly available on the UNCOVER website. 31 We note that the GLASS-JWST program also obtained Near-Infrared Imager and Slitless Spectrograph (NIRISS;  Doyon et al. 2012 , R. Doyon et al. 2023 , in preparation) spectroscopy of the cluster core covering wavelengths λ ∼ 1. 1-2. 2 μm. The UNCOVER program also includes spectroscopic follow-up observations with JWST's Near Infrared Spectrograph (NIRSpec;  Ferruit et al. 2022; Jakobsen et al. 2022; Böker et al. 2023) , which are scheduled for 2023 July and would allow deeper spectroscopic measurements and to longer wavelengths.
A2744 will also be observed with NIRCam as part of the JWST guaranteed time observation (GTO) program Prime Extragalactic Areas for Reionization and Lensing Science (PEARLS; Program ID: GTO 1176; PI: R. Windhorst; Windhorst et al. 2023). Ancillary data for A2744 include deep (∼29 AB) HST imaging, taken in various programs, most prominently the HFF and HST grism spectroscopy from the Grism Lens-Amplified Survey from Space survey (GLASS; PI: T. Treu; Treu et al. 2015). We also note that spectroscopy with the Multi-Unit Spectroscopic Explorer (MUSE;  Bacon et al. 2010 ) on ESO's Very Large Telescope (VLT) was used to measure the redshift for many multiply imaged galaxies in the cluster  (Mahler et al. 2018; Bergamini et al. 2023). A2744 is also part of the ALMA Frontier Fields survey  (González-López et al.
Photometry The three images of our object are detected in the UNCOVER catalog (for details, see  Weaver et al. 2023). The detection is performed on the UNCOVER mosaics corrected for intracluster light (ICL) with the Python implementation of SExtractor (SEP;  Bertin & Arnouts 1996; Barbary 2016 Barbary , 2018)). We note, however, that for images B and C, the UNCOVER catalog fluxes are heavily contaminated with light from the nearby cluster galaxy in image B (see Figure  1 ) and from a faint blue object right next to image C (also visible in Figure  1 ). In order to derive decontaminated fluxes for these two images, we measure them in a circular aperture of 0 32 diameter using photutils (v1. 6. 0;  Bradley et al. 2022)  and subtract a local background measured in an annulus around the aperture.
Lensing Magnifications and Geometric Redshift To estimate the delensed properties of the object presented here as well as to corroborate the photometric redshift estimates, we use an updated fully parametric SL model of A2744 that we recently constructed in the framework of the UNCOVER program  (Furtak et al. 2023c ; see also  Roberts-Borsani et al. 2023). The model uses a long list of spectroscopically confirmed multiply imaged systems (e. g. ,  Mahler et al. 2018; Bergamini et al. 2023 ) and additional photometric systems identified in the new UNCOVER data, in particular in the two northern subclusters. We note that this substructure only has a minor effect on the SL properties in the main cluster core though, where the object studied in this work is situated. For the lens model, cluster galaxies are each modeled as a dual pseudo-isothermal elliptical mass distribution (dPIE; see  Keeton 2001; Elíasdóttir et al.
Acknowledgments The authors would like to thank the anonymous referee for providing very useful comments, which greatly helped to improve the paper. L. F. thanks  Pierre Boldrini  for very useful discussions about high-redshift star clusters. A. Z. thanks  Erik Zackrisson  for a useful discussion regarding Population III stars. L. F. and A. Z. acknowledge support by grant No. 2020750  from the  United States-Israel Binational Science Foundation (BSF)  and grant No. 2109066  from the  United States National Science Foundation (NSF) , and by the  Ministry of Science & Technology, Israel. R. B. acknowledges support from the  Research Corporation for Scientific Advancement (RCSA)   Cottrell Scholar Award  ID No. :  27587. E. C. L. acknowledges the support of an  STFC Webb Fellowship  ( ST/W001438/1 ).
H. A. acknowledges support from  CNES (Centre National d'Etudes Spatiales). J. C. acknowledges funding from the " FirstGalaxies" Advanced Grant  from the  European Research Council (ERC)  under the  European Unionʼs Horizon 2020 research and innovation program  (grant agreement No. 789056 ). P. D. acknowledges support from the  NWO  grant No. 016. VIDI. 189. 162  ("ODIN") and from the  European Commission 's and  University of Groningen 's  CO-FUND Rosalind Franklin program. The work of C. C. W. is supported by  NOIRLab , which is managed by the  Association of Universities for Research in Astronomy (AURA)  under a cooperative agreement with the  National Science Foundation. The  Cosmic Dawn Center  (DAWN) is funded by the  Danish National Research Foundation (DNRF)  under grant # 140. Support for the program  JWST-GO-02561  was provided through a grant from the  STScI  under  NASA  contract  NAS 5-03127.
13, 31, 35 I, C, N, and H atoms are illustrated as purple, brown, blue, and pink spheres, respectively. The Pb atoms lie within black octahedra. The image was produced using VESTA. 40 gure  2. QENS data of FAPbI 3 measured on IN16B. (a) EFWS and IFWSs summed over all measured q values as a function of temperature. The EFWSs intensity is normalized to a maximum value of unity, and the IFWS intensities are multiplied by a factor of 15 for increased visibility. An elastic contribution was subtracted from the IFWS by determining the relative intensity at 4 and 10 μeV in the 2 K QENS spectrum. (b) Fit of S(q, E) measured at T = 125 K and q = 1. 75 Å -1. (c) T dependence of the quasi-elastic line width from fits to the IFWS and QENS spectra. The solid orange line represents an Arrhenius fit with an activation energy of 13 meV, and the dashed black line indicates the γ-to-β phase transition.
Fitting to an Arrhenius dependence suggests that the dynamics are characterized by an activation energy of 13 ± 4 meV, which is much lower than what was extracted from the fit to the IFWSs (about 23 meV). For comparison, the corresponding neutron data for MAPbI 3 show much better agreement with respect to the QENS line shape and FWS data; see the QENS data on MAPbI 3 , which are summarized in Figures  S3-S5. This shows that the MA cation dynamics in the orthorhombic phase of MAPbI 3 are well described by a single dynamical component that can be adequately modeled as a Lorentzian function. The worse agreement between the IFWS fit and the width extracted from the fitting of the QENS spectra for FAPbI 3 suggests that the FA cation dynamics are more complex than the MA dynamics in the γ-phase and that they are not well described by a single relaxational process.
6 MA 0. 4 PbI 3 , as measured at T = 250 K and q = 1. 61 Å -1 on IN6. Similar to the S(q, E) for FAPbI 3 and MAPbI 3 , the T = 200 K data are characterized by a large quasielastic component, and two Lorentzian functions were needed to describe the quasi-elastic scattering. The two Lorentzians exhibit average line widths of around 1. 3 and 0. 18 meV, respectively, at T = 250 K, and the line widths are essentially qindependent. One should note, however, that each Lorentzian cannot be simply related to a single dynamical process since, based on the results of FAPbI 3 and MAPbI 3 , the FA cation is expected to have at least one dynamical process and the MA cation is expected to have at least two dynamical processes under the measurement conditions. Because of the fact that they occur on similar time scales (cf.
51 Figure  5  (e) compares the EISF of FA 0. 6 MA 0. 4 PbI 3 at T = 100 K as extracted from measurements using neutrons with incident wavelengths of both 5. 1 Å (IN6) and 2. 5 Å (IN5). The data are compared to a model that assumes that only the methyl/ ammonia group of the MA cations performs the C 3 rotations. As can be seen in Figure  5  (e), the extended q-range allows for an unequivocal assignment of the observed dynamics to C 3 rotations of the MA cation. The C 3 rotations in FA 0. 6 MA 0. 4 PbI 3 have an average relaxation time of about 3 ps at 100 K, which is drastically faster than that in MAPbI 3 at the same temperature (136 ps). This may be related to the absence of a phase transition to an orthorhombic phase upon cooling FA 0. 6 MA 0. 4 PbI 3 and the increased disorder.
■ EXPERIMENTAL DETAILS The QENS experiments were performed on three different instruments: the two direct-geometry time-of-flight spectrometers IN5  54  and IN6  55  and the backscattering spectrometer IN16B  56  at the Institut Laue-Langevin (ILL), Grenoble, France. After general and instrument-specific data reductions, which are briefly outlined in the following text, the computed response function in each experiment is the dynamical structure factor, S(q, E), where q and E are the moduli of the wavevector transfer and energy transfer, respectively. The complementarity in using IN5, IN6, and IN16B is that they allow us to probe different parts of (q, E) space with different energy resolutions, meaning that information about the dynamics over a large range of time and length scales can be obtained.
IN6 was set up using an incident neutron wavelength of 5. 1 Å, which yields an E resolution at the full width at halfmaximum (fwhm) of 70 μeV. The accessible q range was ∼0. 3-2 Å -1 at the elastic line. On IN5, incident neutron wavelengths of 5 and 2. 5 Å were used. The use of 5 Å wavelength neutrons yields an E resolution at fwhm of 0. 1 meV and a q range of ∼0. 3-2. 2 Å -1 at the elastic line. The use of 2. 5 Å wavelength neutrons yields an E resolution at fwhm of 0. 62 meV and a q range of ∼0. 5-4 Å -1 at the elastic line. For both the IN6 and IN5 data, standard data reduction included normalization to a vanadium standard, background subtraction (empty sample cell), and correction of the energy-dependent efficiency of the detectors. Measurements were taken in the temperature range of 2-350 K, and the 2 K spectra were used as a resolution function in the data analysis.