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This article describes a methodological experiment conducted during the 13th Annual (Virtual) Schoenberg Symposium on Manuscript Studies in the Digital Age, hosted by the University of Pennsylvania, November 18–20, 2020. The experiment consisted of a “relay style” event in which three teams transcribed, revised, and prepared for submission to this journal a full edition of the “Le Pèlerinage de Damoiselle Sapience” and other texts from UPenn Ms Codex 660, ff. 86r–95v within the three-day timespan of the conference. The project used methods typical of crowdsourcing and drew participants from all over the world and from all different stages of their careers. After one group completed its work, the results were passed into the hands of the next. The final result—in the form of a finished manuscript edition, ready for submission to Digital Medievalist—was presented on the last day of the conference. The main purpose of this experiment was to demonstrate how the work of the transcriber and editor might be structured as a short-term digital event that relied wholly on virtual interactions with both the source materials and among collaborators. This method also reveals the positive aspects of the many challenges posed by working simultaneously, remotely, and globally.

This article describes a methodological experiment conducted during the 13th Annual (Virtual) Schoenberg Symposium on Manuscript Studies in the Digital Age, hosted by the University of Pennsylvania, November 18–20, 2020. The experiment consisted of a “relay style” event in which three teams transcribed, revised, and prepared for submission to this journal a full edition of the “Le Pèlerinage de Damoiselle Sapience” and other texts from UPenn Ms Codex 660, ff. 86r–95v within the three-day timespan of the conference. The project used methods typical of crowdsourcing and drew participants from all over the world and from all different stages of their careers. After one group completed its work, the results were passed into the hands of the next. The final result—in the form of a finished manuscript edition, ready for submission to Digital Medievalist—was presented on the last day of the conference. The main purpose of this experiment was to demonstrate how the work of the transcriber and editor might be structured as a short-term digital event that relied wholly on virtual interactions with both the source materials and among collaborators. This method also reveals the positive aspects of the many challenges posed by working simultaneously, remotely, and globally.

For the past two decades, Global Navigation Satellite System (GNSS) signals have been explored in terms of Earth remote sensing. Most work has been done on the Global Positioning System (GPS) signals. GNSS signals are reflected off the surface of the Earth and can be received using a left hand polarized antenna which could offer a low cost alternative to existing remote sensing instruments. The reflected GNSS signals can, together with the direct signals, be processed to provide altitude estimations of the receiver. If reflected off for example the surface of the ocean, the reflected signal carries information about the near surface winds and surface state. Most receivers use the publicly available GPS L1 signals for processing. The newer GPS L5 signals have different signal properties than the GPS L1 signal which gives a sharper correlation waveform that should lead to higher measurement sensitivity. This thesis work consisted of building a bistatic GNSS system capable of receiving L1, L2 and L5 signals. The system was tested on a 300 meter high tower and data was collected during the ascent and descent. The data collected on the tower was processed in terms of altimetry using the Wide Area Augmentation System (WAAS) L5 signals. The bistatic system was installed in the National Oceanic and Atmospheric Administration (NOAA) hurricane hunter airplane Kermit. The system collected approximately 12 hours of direct and reflected GNSS data while flying through hurricane Rafael and Sandy. The collected flight data is in the initial stages of bistatic processing., Validerat; 20130121 (global_studentproject_submitter)

To gain insight into how genomic information is translated into cellular and developmental programs, the Drosophila model organism Encyclopedia of DNA Elements (modENCODE) project is comprehensively mapping transcripts, histone modifications, chromosomal proteins, transcription factors, replication proteins and intermediates, and nucleosome properties across a developmental time course and in multiple cell lines. We have generated more than 700 data sets and discovered protein-coding, noncoding, RNA regulatory, replication, and chromatin elements, more than tripling the annotated portion of the Drosophila genome. Correlated activity patterns of these elements reveal a functional regulatory network, which predicts putative new functions for genes, reveals stage- and tissue-specific regulators, and enables gene-expression prediction. Our results provide a foundation for directed experimental and computational studies in Drosophila and related species and also a model for systematic data integration toward comprehensive genomic and functional annotation.

Very sensitive HI 21cm observations have been made in 860 directions at dec >= -43deg in search of weak, Galactic, high-velocity HI emission lines at moderate and high Galactic latitudes. One-third of the observations were made toward extragalactic objects. The median 4-sigma detection level is NHI = 8x10^{17} cm^-2 over the 21' telescope beam. High-velocity HI emission is detected in 37% of the directions; about half of the lines could not have been seen in previous surveys. The median FWHM of detected lines is 30.3 km/s. High- velocity HI lines are seen down to the sensitivity limit of the survey implying that there are likely lines at still lower values of NHI. The weakest lines have a kinematics and distribution on the sky similar to that of the strong lines, and thus do not appear to be a new population. Most of the emission originates from objects which are extended over several degrees; few appear to be compact sources. At least 75%, and possibly as many as 90%, of the lines are associated with one of the major high-velocity complexes. The Magellanic Stream extends at least 10 deg to higher Galactic latitude than previously thought and is more extended in longitude as well. Although there are many lines with low column density, their numbers do not increase as rapidly as NHI^-1, so most of the HI mass in the high-velocity cloud phenomenon likely resides in the more prominent clouds. The bright HI features may be mere clumps within larger structures, and not independent objects., Comment: 88 pages includes 22 figures Accepted for Publication in ApJ Suppl. June 2002

Very sensitive HI 21cm observations have been made in 860 directions at dec >= -43deg in search of weak, Galactic, high-velocity HI emission lines at moderate and high Galactic latitudes. One-third of the observations were made toward extragalactic objects. The median 4-sigma detection level is NHI = 8x10^{17} cm^-2 over the 21' telescope beam. High-velocity HI emission is detected in 37% of the directions; about half of the lines could not have been seen in previous surveys. The median FWHM of detected lines is 30.3 km/s. High- velocity HI lines are seen down to the sensitivity limit of the survey implying that there are likely lines at still lower values of NHI. The weakest lines have a kinematics and distribution on the sky similar to that of the strong lines, and thus do not appear to be a new population. Most of the emission originates from objects which are extended over several degrees; few appear to be compact sources. At least 75%, and possibly as many as 90%, of the lines are associated with one of the major high-velocity complexes. The Magellanic Stream extends at least 10 deg to higher Galactic latitude than previously thought and is more extended in longitude as well. Although there are many lines with low column density, their numbers do not increase as rapidly as NHI^-1, so most of the HI mass in the high-velocity cloud phenomenon likely resides in the more prominent clouds. The bright HI features may be mere clumps within larger structures, and not independent objects., Comment: 88 pages includes 22 figures Accepted for Publication in ApJ Suppl. June 2002