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opencc-by-4.0May 2020View details →

Black Swift Technologies S1 Unmanned Aircraft System Observations from LAPSE-RATE

This dataset contains meteorological data collected by Black Swift Technologies' S1 unmanned aircraft system during the 2018 LAPSE-RATE (Lower Atmospheric Profiling Studies at Elevation - a Remotely-piloted Aircraft Team Experiment) field campaign.  Questions about the dataset should be addressed to Jack Elston (elstonj@bst.aero).

opencc-by-4.0Aug 2020View details →

An interactive figure of the 2016 and 2020 X-ray light curves of LMC 1968 as observed by the XRT instrument on Swift

This repository contains all the files necessary to create the interactive figure in the Research Note ov Schwarz, Page, Kuin, & Darnley 2020. The figure was created using the <a href="https://aas-timeseries.readthedocs.io/en/latest/">aas-timeseries</a> package of the <a href="https://www.astropy.org">astropy</a> project. The file lmc68.py is the underlying python code while the two lmcrel*.csv are the input files for the 2016 and 2020 eruptions of the recurrent nova LMC 1968 as observed by the XRT instrument on board the Neil Gehrels Swift observatory. A Jupyter notebook is required to preview the interactive figure. The output from the code is saved in the interactive.tar.gz package. It consists of four files: <ul> <li>index.html</li> <li>figure.json</li> <li>data_75e74aca-09f1-4846-966e-9e33c7acc8d3.csv</li> <li>data_5402e718-01cf-4ad7-92a5-7679d4076ed5.csv</li> </ul> The first file, index.html, is the html framework that houses the interactive figure. figure.json contains the interactive figure commands while the two data*csv files are the underlying data. The interactive figure can be viewed if this package is opened on a web server.  A copy of this interactive figure is available <a href="https://authortools.aas.org/LMC1968/">here</a> so you can try it out.

opencc-by-sa-4.0Mar 2022View details →

Dependency Networks of Open Source Libraries Available Through CocoaPods, Carthage and Swift PM

Third party libraries are used to integrate existing solutions for common problems and help speed up development. The use of third party libraries, however, can carry risks, for example through vulnerabilities in these libraries. Studying the dependency networks of package managers lets us better understand and mitigate these risks. So far, the dependency networks of the three most important package managers of the Apple ecosystem, CocoaPods, Carthage and Swift PM, have not been studied. We analysed the dependencies for all publicly available open source libraries up to December 2021 and compiled a dataset containing the dependency networks of all three package managers. The dependency networks can be used to analyse how vulnerabilities are propagated through transitive dependencies. In order to ease the tracing of vulnerable libraries we also queried the NVD database and included publicly reported vulnerabilities for these libraries in the dataset.

opencc-by-4.0Dec 2022View details →

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

Here we provide the data products from publications: Clark, C.J.R., et al., The Quest for the Missing Dust: I – Restoring Large Scale Emission in Herschel Maps of Local Group Galaxies, ApJ 921 35 Clark, C.J.R., et al., The Quest for the Missing Dust: II – Two Orders of Magnitude of Evolution in the Dust-to-Gas Ratio Resolved Within Local Group Galaxies, ApJ 946 42 This data concerns four Local Group galaxies: the Large Magellanic Cloud (LMC), the Small Magellanic Cloud (SMC), M31, and M33.   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. For each galaxy, we provide this new Herschel data for 5 Hershcel bands: the PACS 100 and 160 \(\mu\)m bands, and the SPIRE 250, 350, and 500 \(\mu\)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).   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 \(\mu\)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. 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 \(\mu\)m excess), and samples. This is provided as a gzip compressed FITS file for each galaxy. 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. 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

opencc-by-4.0Jun 2020View details →

Reproduction package for the paper "The variable radio counterpart of Swift J1858.6-0814"

This is a basic reproduction package for the paper "The variable radio counterpart of Swift J1858.6-0814" by J. van den Eijnden et al. (2020). It aims to provide the data products underlying the figures in the paper, report where the analyzed observations can be accessed, and list the software used to perform the analysis.  An open access version of the paper can be found at <a href="https://arxiv.org/abs/2006.06425">https://arxiv.org/abs/2006.06425</a>.

Fig. 7. Box plots comparing average counts per 10 in Trypanosomiasis: An emerging disease in Alpine swift (Tachymarptis melba) nestlings in Switzerland?

Fig. 7. Box plots comparing average counts per 10 HPF of granulocytes, mononuclear cells, and thrombocytes between positive (n = 20) and negative (n = 20) 45- day-old Alpine swift nestlings sampled in 2022.

Fig. 5 in Trypanosomiasis: An emerging disease in Alpine swift (Tachymarptis melba) nestlings in Switzerland?

Fig. 5. Skeletal musculature of a nestling Alpine swift showing infiltrations of mononuclear inflammatory cells (A, B) and presumably extracellular, amastigote-like structures (C). Bursa fabricii of a nestling Alpine swift with depletion of the medullary follicle with lymphocytolysis (asterisk) and a distinct epithelium (arrows) (D).

Fig. 6 in Trypanosomiasis: An emerging disease in Alpine swift (Tachymarptis melba) nestlings in Switzerland?

Fig. 6. Blood smears of nestling Alpine swifts with high (A) and moderate (B) trypomastigote burdens. Close-up of a trypomastigote between erythrocytes (C).

Fig. 4 in Trypanosomiasis: An emerging disease in Alpine swift (Tachymarptis melba) nestlings in Switzerland?

Fig. 4. Distribution of louse flies on an Alpine swift nestling (A) compared with the distribution of bruising on post-mortem examination with plumage removed (B).

Fig. 3 in Trypanosomiasis: An emerging disease in Alpine swift (Tachymarptis melba) nestlings in Switzerland?

Fig. 3. Missing (left wing) and poor quality (right wing) primary feathers on a 45-day-old nestling.

Fig. 1 in Trypanosomiasis: An emerging disease in Alpine swift (Tachymarptis melba) nestlings in Switzerland?

Fig. 1. Map of Switzerland with the locations and appearance of the three evaluated colonies (A, B, C).

Figure 6 in Species limits in the African Palm Swift Cypsiurus parvus

Figure 6. Type of Cypsiurus parvus laemostigma (ZMB 49.338; above) compared to an example of C. p. gracilis (ZMB 36.546); note the plain grey breast and belly of the former (Nigel J. Collar)

Figure 5 in Species limits in the African Palm Swift Cypsiurus parvus

Figure 5. Examples in NHMUK of six taxa treated as races of African Palm Swift Cypsiurus parvus, left to right: gracilis and griveaudi (Malagasy taxa), hyphaenes, myochrous, brachypterus and parvus African taxa). Note the stronger-marked throat and breast markings and paler, scaled bellies of the Malagasy taxa, but the longer wings of griveaudi than gracilis (Nigel J. Collar, © Natural History Museum, London)

Figure 4 in Species limits in the African Palm Swift Cypsiurus parvus

Figure 4. Examples of calls uttered by three vocal groups of Cypsiurus parvus ranked from west to east (and from left to right): parvus group a: XC348468, São Tomé, P. Verbelen; b: XC346765, Namibia, P. Boesman; gracilis group c: Madagascar, M. Mills; and balasiensis group d: XC286657, India, V. Puliyeri; e: XC362689, Thailand, A. Lastukhin.

Figure 2 in Species limits in the African Palm Swift Cypsiurus parvus

Figure 2. Examples of call series (extracts to illustrate note shapes) uttered by groups of birds, for mainland races of Cypsiurus parvus. From left to right (a–d): parvus (XC356729, B. Piot), brachypterus (XC348468, P. Verbelen), myochrous (XC396390, J. Bradley), hyphaenes (XC153527, R. de By).

Figure 3 in Species limits in the African Palm Swift Cypsiurus parvus

Figure 3. Examples of calls uttered by single individuals of Malagasy races of Cypsiurus parvus. From left to right: gracilis a: XC162876, M. Nelson; b: M. Mills; c: XC125058, A. Lastukhin (cut-off at 7.8 kHz) and griveaudi d: M. Herremans (heavily filtered).

Figure 1 in Species limits in the African Palm Swift Cypsiurus parvus

Figure 1. Examples of short calls uttered by single individuals, for mainland races of Cypsiurus parvus. From left to right (a–e): parvus (XC421450, B. Piot), brachypterus (XC348468, P. Verbelen), myochrous (XC280231, P. Boesman), hyphaenes (XC346765, P. Boesman) and celer (XC280232, P. Boesman).

opencc-zeroMar 2023View details →

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ADCP data collected in the Southern California Bight by SWIFT drifters as part of the ONR "Langmuir Circulation Departmental Research Initiative (LC-DRI)"

This is the public archive for ADCP data collected with SWIFT drifters during the 'Langmuir Circulation' Office of Naval Research Departmental Research Initiative (LC-DRI) field experiment, conducted between March 19th and April 6th, 2017 in the Southern California Bight 40 km west of Catalina Island. SWIFTs were deployed and recovered from the R/V R.G. Sproul during cruise SP1709 (Cruise DOI: 10.7284/907464). SWIFTs were deployed during storms with wind speeds up to 20 m/s and sampled strong diurnal warm layers during weaker wind periods.