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Dataset results
122 results for “SMC”
Photometric detection of internal gravity waves in upper main-sequence stars. IV. Comparable stochastic low-frequency variability in SMC, LMC, and Galactic massive stars
<p>Supporting data for peer-reviewed publication entitled: 'Photometric detection of internal gravity waves in upper main-sequence stars. IV. Comparable stochastic low-frequency variability in SMC, LMC, and Galactic massive stars', published in A&A. For the purpose of open access, the authors have applied a CC BY licence to the author accepted manuscript version and made it publicly available: <a href="https://arxiv.org/abs/2410.12726">https://arxiv.org/abs/2410.12726</a></p> <p>Evolutionary models and stability window calculations courtesy of Jermyn et al. 2022 (DOI: <a href="https://iopscience.iop.org/article/10.3847/1538-4357/ac4e89">10.3847/1538-4357/ac4e89</a>) are publicly available via: <a href="https://github.com/adamjermyn/conv_trends">https://github.com/adamjermyn/conv_trends</a></p> <p>TESS full-frame image data are publicly available from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI): <a href="https://archive.stsci.edu/missions-and-data/tess">https://archive.stsci.edu/missions-and-data/tess</a></p> <p>TESS light curves (provided in this repository) were extracted using the publicly available tglc (Han & Brandt 2023; DOI: <a href="https://iopscience.iop.org/article/10.3847/1538-3881/acaaa7">10.3847/1538-3881/acaaa7</a>) software package: <a href="https://github.com/TeHanHunter/TESS_Gaia_Light_Curve">https://github.com/TeHanHunter/TESS_Gaia_Light_Curve </a></p> <p>SLF variability parameters (provided in this repository; cf. Tables 1 and 2 of the paper) were obtained using GP regression with the publicly available celerite2 (Foreman-Mackey et al. 2017; DOI: <a href="https://iopscience.iop.org/article/10.3847/1538-3881/aa9332">10.3847/1538-3881/aa9332</a>) software package: <a href="https://celerite2.readthedocs.io/en/latest/">https://celerite2.readthedocs.io/en/latest/</a> and confidence intervals were obtained using the publicly available pymc3 (Salvatier et al. 2016; <a href="https://doi.org/10.7717/peerj-cs.55">https://doi.org/10.7717/peerj-cs.55</a>) software package: <a href="https://github.com/pymc-devs/pymc">https://github.com/pymc-devs/pymc</a></p> <p>This research was supported in part by the National Science Foundation (NSF) under Grant Number NSF PHY-1748958; the Research Foundation Flanders (FWO) with grant agreement numbers 1286521N, 11F7120N, and V411621N; UK Research and Innovation (UKRI) in the form of a Frontier Research grant under the UK government's ERC Horizon Europe funding guarantee (SYMPHONY; grant number: EP/Y031059/1); a Royal Society University Research Fellowship (URF; grant number: URF\R1\231631); and the KU Leuven Research Council (grant number C16/18/005: PARADISE).</p>
The Quest for the Missing Dust: New Herschel Maps of Local Group Galaixes (LMC, SMC, M31, M33) that Restore Previously-Missed Extended Emission, Along With SED-Fitting Results, Hydrogen Gas Maps, and Swift UV Observations
<p>Here we provide the data products from publications:</p> <p>Clark, C.J.R., et al., <em>The Quest for the Missing Dust: I – Restoring Large Scale Emission in Herschel Maps of Local Group Galaxies</em>, ApJ 921 35</p> <p>Clark, C.J.R., et al., <em>The Quest for the Missing Dust: II – Two Orders of Magnitude of Evolution in the Dust-to-Gas Ratio Resolved Within Local Group Galaxies</em>, ApJ 946 42</p> <p>This data concerns four Local Group galaxies: the Large Magellanic Cloud (LMC), the Small Magellanic Cloud (SMC), M31, and M33.</p> <p> </p> <p>For each galaxy, we provide our new Herschel maps, as described in the above publications, which were combined in Fourier space ('feathered') with Planck, IRAS, and COBE data, in order to restore extended emission that was removed from previous Herschel reductions for these galaxies.</p> <p>For each galaxy, we provide this new Herschel data for 5 Hershcel bands: the PACS 100 and 160 <span>\(\mu\)</span>m bands, and the SPIRE 250, 350, and 500 <span>\(\mu\)</span>m bands. This data is provided in FITS format, with one FITS file for each band for each galaxy. Each of these files contains 4 extensions. Extension 1 (IMAGE) provides the standard feathered map. Extension 2 (UNC) provides the uncertainty map. Extension 3 (MASK) provides a binary mask map indicating the portion of the data where reliable, fully-feathered high-resolution coverage is available. Extension 4 provides the foreground-subtracted version of the feathered map (FGND_SUB), the header of which also describes the uncertainty on that subtraction. All maps are in units of MJy/sr (except the MASK extension, which is boolean).</p> <p> </p> <p>We also provide the outputs of our Spectral Energy Distribution (SED) fitting to this data, as described in the publications. For each galaxy, we provide FITS files giving the median value of each parameter in each pixel, and maps of the uncertainties on those medians (being the 68.3% quantile around the median). The parameters are dust mass surface density (SED_Sigma_Mass.fits), dust temperature (SED_Temp.fits), beta 1 (SED_Beta1.fits), beta 2 (SED_Beta2.fits), break wavelength (SED_Break.fits), and 500 <span>\(\mu\)</span>m excess (SED_Excess500.fits). Each of these files contain 2 extensions. Extension 1 (median) provides the map of pixel parameter median values. Extension 2 (uncert) provides the map of uncertainties on those medians.</p> <p>Additionally, we provide the full posterior probability distribution for all SED parameters, consisting of 1000 posterior samples, for all pixels, in the form of a FITS file containing a 4-dimensional hypercube, with axes corresponding to right ascension, declination, parameters (in order: dust mass surface density, dust temperature, beta 1, beta 2, break wavelength, and 500 <span>\(\mu\)</span>m excess), and samples. This is provided as a gzip compressed FITS file for each galaxy.</p> <p>Furthermore, provide the Swift-UVOT maps used in Paper II. This data is provided for Swift-UVOT bands W1, W2, and M2. For each band, we provide a FITS file containing 3 extensions. Extension 1 (SURF_BRI) provides the map of surface brightness in MJy/sr (converted using the Swift-UVOT zero points given in Breeveld et al., 2011). Extension 2 (RATE) provides the map of count rate (in photons/sec). Extension 3 (EXP) provides the map of exposure time (in sec). The maps for the LMC and SMC are those presented in Hagen et al. (2017). The maps for M31 and M33 are were reduced following the same process as those in Hagen et al. (2017), and will be fully presented in Decleir et al. (in prep.), but are provided here for the purposes of reproducibility.</p> <p>Lastly, for each galaxy, we provide our maps of the hydrogen surface density (Sigma_H.fits), and dust-to-gas ratio (DtG.fits). None of the maps presented have had deprojection corrections applied</p> <p> </p>
Reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities"
<p>This is a reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution - IV. Grids of models at Solar, LMC, and SMC metallicities" by <a href="https://doi.org/10.1093/mnras/stac2598">Keszthelyi et al. (2022).</a></p>
Webis Search Mission Corpus 2012 (Webis-SMC-12)
<p>The Webis Search Mission Corpus 2012 (Webis-SMC-12) contains 8840 search engine interactions of 127 users. Two human annotators divided these interactions into 2881 logical sessions and 1378 missions. Cases where the annotators did not agree initially were discussed to reach a consensus.</p>
Sample data connected to Barth et al "SMC motor proteins extrude DNA asymmetrically and can switch directions"
<p>Sample data connected to Barth et al "SMC motor proteins extrude DNA asymmetrically and can switch directions"</p>
Test results from quasi-static impact tests over SMC materials reinforced with glass fibre (ramdom and textile)
<p>Test results from quasi-static impact tests over SMC materials with structural properties conceived for automotive applications, reinforced with glass fibre (samples with ramdom distribution of fibres and samples reinforced with GF textile)</p>
Results from DSC analysis over glass fibre reinforced SMC (50009092 grade by Menzolit supplier)
<p>Results from DSC analysis over glass fibre reinforced SMC automotive grade (50009092 grade provided by Menzolit supplier)</p>
Results from DSC analysis over glass fibre reinforced SMC (50007150 grade by Menzolit supplier)
<p>Results from DSC analysis over glass fibre reinforced SMC for automotive applications (50007150 grade provided by Menzolit supplier)</p>
Catalogues containing photometry in 22 passbands for 603311 LMC stars and 124578 SMC stars from Bellazzini & Pascale 2024, A&A,
<p>Catalogues from the paper "The RGB Tip in the SDSS, PS1, JWST, NGRST and Euclid photometric systems. Calibration in optical passbands using Gaia DR3 synthetic photometry" by M. Bellazzini (INAF - OAS Bo) & R. Pascale (INAF - OAS Bo), A&A, in press, (<a href="https://arxiv.org/abs/2406.04781" target="_blank" rel="noopener">arXiv:2406.04781</a>). Stars have been selected from the Gaia DR3 dataset and the magnitudes has been obtained from the Gaia GSPC catalogue of from GaiaXPy as described in Gaia Collaboration 2023.</p> <div>Each catalogue contains:</div> <div> </div> <div> <ul> <li>Column 1-15, parameters directly extracted from the Gaia DR3 source catalogue, namely: source_id, ra, dec, parallax, parallax_error, pmra, pmra_error, pmdec, pmdec_error, ruwe, phot_variable_flag, and non_single_star.</li> <li>Column 16: C⋆, a parameter that is derived from phot_bp_rp_excess_factor (that, in turn, has been extracted from the Gaia DR3 source catalogue) following (Riello et al. 2021).</li> <li>Column 17: colour excess E(B-V), derived from Skowronet al. (2021) and Schlegel et al. (1998); Schlafly & Finkbeiner (2011) as described in Sect. 2.</li> <li>Columns 18-27: standardised ugriz magnitudes in the SDSS system extracted from the Gaia DR3 GSPC (Gaia Collaboration et al. 2023a) and associated uncertainties.</li> <li>Columns 28-37: standardised UBVRI magnitudes in the JKCsystem extracted from the Gaia DR3 GSPC (Gaia Collaboration et al. 2023a) and associated uncertainties.</li> <li>Columns 38-47: standardised grizy magnitudes in the PS1 system computed with GaiaXPy and associated uncertainties.</li> <li>Columns 48-51: standardised F606W, F814W magnitudes in the HST ACS-WFC system extracted from the Gaia DR3 GSPC (Gaia Collaboration et al. 2023a) and associated uncertainties.</li> <li>Columns 52-55: non-standardised F070W and F090W magnitudes in the JWST-NIRCAM system computed with GaiaXPy and associated uncertainties.</li> <li>Columns 56-59: non-standardised R062 and Z087 magnitudes in the NGRST system computed with GaiaXPy and associated uncertainties .</li> <li>Columns 60-61: non-standardised I_E magnitude in the Euclid-VIS system computed with GaiaXPy and associated uncer-tainties (in this case, not corrected for the bias described in Sect. 2.1 of Gaia Collaboration et al. 2023a, hence slightly underestimated).</li> </ul> <p><strong>It is very important to remind </strong>that u_SDSS and U_JKC magnitudes from Gaia XPSP are significantly less accurate and pre-<br>cise than all the other magnitudes included in our catalogues (see Gaia Collaboration et al. 2023a, for detailed discussion).<br>Each star can lack some of the 22 magnitudes listed in the catalogues, depending on the signal-to-noise constraints applied to the original GSPC (S/N> 30 Gaia Collaboration et al. 2023a). For example, of the 603311 stars listed in the LMC sample only 83229(85338) have valid u_SDSS (U_JKC ) magnitudes. See Bellazzini & Pascale 2024 for further details and references.</p> </div> <p><strong>We cannot give any hint or guarantee on the behaviour of the completeness of the samples</strong> as a function of the various magnitudes and colours, as well as as a function of position in the sky (see Bellazzini & Pascale 2024 for details on the selections applied).</p>
Data from: Topological DNA-binding of SMC-like RecN promotes RecA-mediated DNA double-strand break repair
<p>Bacterial RecN, closely related to the structural maintenance of chromosomes (SMC) family of proteins, functions in the repair of DNA double-strand breaks (DSBs) by homologous recombination. However, the understanding of how RecN acts in concert with the RecA recombinase to promote DSB repair remains limited. Here, we demonstrated that the purified Escherichia coli RecN protein topologically loads onto both single-stranded DNA (ssDNA) and double-stranded DNA (dsDNA) that has a preference for ssDNA. RecN topologically bound to dsDNA slides off the end of linear dsDNA, but this is prevented by RecA nucleoprotein filaments on ssDNA, thereby allowing RecN to translocate to DSBs. Furthermore, we found that, once RecN is recruited onto ssDNA, it can topologically capture a second dsDNA substrate in an ATP-dependent manner, suggesting a role in synapsis. Indeed, RecN stimulates RecA-mediated D-loop formation and subsequent strand exchange activities. Our findings provide mechanistic insights into the recruitment of RecN to DSBs and sister chromatid interactions by RecN, both of which function in RecA-mediated DSB repair.</p>
The young massive SMC cluster NGC 330 seen by MUSE. III. Stellar parameters and rotational velocities - diagnostic plots
<p>This Zenodo repository hosts additional diagnostic plots for the article "<em>The young massive SMC cluster NGC 330 seen by MUSE. III. Stellar parameters and rotational velocities</em>" by Bodensteiner et al. 2023. It provides three diagnostic figures for each of the 282 stars in the sample described in the paper. Three example figures are given for one star (#654) in the Figures 2, 3, and 4 in the paper.</p> <p>Here, we provide a .zip archive with three additional figures for all other stars that are similar to the ones in the paper:</p> <ol> <li>the <strong>spectroscopic fit</strong> ("<em>id###_spec.pdf</em>"): Each panel, one for each of the six diagnostic spectral regions, shows the combined spectrum (black) and the best-fitting tlusty model (red). Grayed-out regions are only shown for comparison but were not included in the fit, which may vary from star to star.</li> <li>the <strong>photometric fit</strong> ("<em>id###_phot.pdf</em>"): The top panel shows a comparison between the observed HST fluxes (black crosses) and the flux (colored circles) computed from the best-fit model (gray line) by convolution with the HST filters (colored lines). The bottom panel gives residuals.</li> <li>the <strong>combined fit results</strong> ("<em>correlationplot_comb_id###.pdf</em>"): The diagonal gives the χ2-distribution as a function of each parameter and the panels below show 2-dimensional χ2 -maps. The red line marks the 95% confidence level.</li> </ol> <p>The star ids (###) correspond to the ones provided in Table 1 (also available at the CDS).</p>
Results from DSC analysis over SMC paste (50007150 grade by Menzolit supplier)
<p>Results from DSC analysis over SMC paste automotive grade (50007150 grade provided by Menzolit supplier)</p>
Data for SMC UV Expanded Sample paper
<p>Extinction curves used for the analysis presented in the paper titled "" by Gordon et al. (2024, ApJ, in press).</p>
X-Shooting ULLYSES: Massive Stars at low metallicity VI. Atmosphere and mass-loss properties of O-type giants in the SMC
<p>Figures from X-Shooting ULLYSES: Massive Stars at low metallicity VI. Atmosphere and mass-loss properties of O-type giants in the SMC. The individual fits of the stars and their explored parameter space. </p> <p>Caption:</p> <p>Overview of the fitting results of AV\,80. The \textit{top} part shows the line profiles included in the fitting process, with the name of each feature indicated in the bottom left. The green line shows the best fit, with the shaded region showing the 1$\sigma$ uncertainty on the model fit. The black vertical bars indicate the observed flux, with the length indicating the uncertainty. The horizontal axis shows the wavelength in \AA. The \textit{bottom} part shows the distribution of $1/\chi^2_{\rm r}$ for each parameter (indicated on the top left), with $\chi^2_{\rm r}$ the reduced $\chi^2$ value. Each scatter point indicates one {\sc Fastwind} model calculated by Kiwi-GA. The color indicates the generation in which the model was computed, with light gray the first generation and black the last. The vertical yellow line indicates the best fit value for each parameter, and the shaded regions are the 1 and 2 $\sigma$ confidence intervals. The distributions in the red shaded area are from the optical only GA fit.</p>
The Effect of a Diabetic- and a Kidney-like Environment on Gene and Protein Expression in Cultured EC and SMC
ClinicalTrials.gov study NCT01423279. IPD Sharing: Not stated. Countries: 1. Publications: 4.
CBT Plus SMC Compared to SMC for Persistent Physical Symptoms in Secondary Care (PRINCE)
ClinicalTrials.gov study NCT02426788. IPD Sharing: NO. Countries: 1. Publications: 1.
A Comparison Study of the Perclose Proglide (TM) SMC System Versus Figure-of-8- Suture Technique for Closure of Large-bore Femoral Venous Access.
ClinicalTrials.gov study NCT05859503. IPD Sharing: Not stated. Countries: 1. Publications: 6.
Assessment of a Combined Strategy of SMC + Nutrients Supplementation to Tackle Malaria and Malnutrition
ClinicalTrials.gov study NCT04238845. IPD Sharing: YES. Countries: 1. Publications: 2.
Understanding and Maximizing the Community Impact of Antimalarial Treatment (INDIE-SMC)
ClinicalTrials.gov study NCT05878366. IPD Sharing: UNDECIDED. Countries: 1. Publications: 1.
Optimization of Seasonal Malaria Chemoprevention (SMC) Delivery
ClinicalTrials.gov study NCT02646410. IPD Sharing: Not stated. Countries: 1. Publications: 2.
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