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CASA, the Common Astronomy Software Applications, is the primary data processing software for the Atacama Large Millimeter/submillimeter Array (ALMA) and the Karl G. Jansky Very Large Array (VLA), and is frequently used also for other radio telescopes. The CASA software can handle data from single-dish, aperture-synthesis, and Very Long Baseline Interferometery (VLBI) telescopes. One of its core functionalities is to support the calibration and imaging pipelines for ALMA, VLA, VLA Sky Survey (VLASS), and the Nobeyama 45m telescope. This paper presents a high-level overview of the basic structure of the CASA software, as well as procedures for calibrating and imaging astronomical radio data in CASA. CASA is being developed by an international consortium of scientists and software engineers based at the National Radio Astronomical Observatory (NRAO), the European Southern Observatory (ESO), the National Astronomical Observatory of Japan (NAOJ), and the Joint Institute for VLBI European Research Infrastructure Consortium (JIV-ERIC), under the guidance of NRAO., Comment: Accepted for publication in PASP (20 pages, 4 figures). Joint publication with CASA-VLBI paper

Introduction Left ventricular assist devices (LVADs) play a fundamental role in treating end-stage heart failure. Outflow graft stenosis (OGS) represents a serious complication that can occur at a variable time point after the implantation, although typically of the order of months to years. Different types of OGS, both intrinsic and external, were described. Notwithstanding the etiology, this clinical scenario poses a life and health-threatening complication requiring timely and precise diagnosis followed by appropriate intervention. Case Report We present a case of a 72-years-old woman on LVAD HeartMate II (HM II) support. Three years after the index implantation, she presented with clinical symptoms of outflow graft stenosis. The patient was admitted to the hospital due to”low-flow“ alarms of HMII. The CT scan revealed distal outflow graft stenosis suggestive of kinking of the graft. Subsequent percutaneous transluminal stenting of the graft was performed. However, after the intervention, signs of hemodynamic compromise persisted. Both angiography and repeated CT scans verified peculiar pattern of the proximal shift of the stenotic segment relative to the implanted stent. Given this specific feature, a diagnosis was reclassified as a previously reported pattern of the outflow graft twist scenario, and surgical subxiphoid approach reexploration was indicated. On inspection, after disconnecting the bend relief from the pump body massive”gelly mass“ plasma transudate located in the interspace between the graft and the bend relief was observed. Immediately after removing compressing gelly mass, hemodynamic and pump parameters promptly resolved, and the bend relief was re-attached. Further patient follow-up remains uneventful to the date. Summary Our observation suggests that the diagnostic assessment of the outflow graft stenosis may be confusing and challenging. As plasma transudate likely develops over an extended period of time once a distal orifice of the bend relief already gets entrapped within the adjacent adhesion, the outflow graft may become contained within incompressible interspace while limited by tight connection to the pump body. That said, the graft constriction migration upon stenting can easily get misdiagnosed as a pattern suggestive of the intrinsic twist instead of correct”pseudotwist“ diagnosis associated with the external contained compartment compression.

We describe a new protocol deployed at the National Radio Astronomy Observatory’s Karl G. Jansky Very Large Array (VLA) to support the distribution of data in support of commensal data analysis. The protocol, vys, is designed to provide access to a high time resolution data stream while a primary observation continues with the typical (lower) time resolution data stream. This form of dual time resolution, commensal observing has been implemented to enable the search for millisecond astrophysical transient events by a new, dedicated compute cluster located at the VLA. The fast transient detection system, realfast, performs real-time analysis in situ to detect events of interest and record relatively short duration data “cut-outs” of those events. By selectively recording high time resolution data, provided by vys at rates of up to 1.4[Formula: see text]GB[Formula: see text]s[Formula: see text], realfast will reduce the recorded data volume by an estimated factor of up to 1000. This makes it possible to search for transients commensally in a high data rate stream over the thousands of hours needed to find the rarest events.

Radio interferometers have the ability to precisely localize and better characterize the properties of sources. This ability is having a powerful impact on the study of fast radio transients, where a few milliseconds of data is enough to pinpoint a source at cosmological distances. However, recording interferometric data at millisecond cadence produces a terabyte-per-hour data stream that strains networks, computing systems, and archives. This challenge mirrors that of other domains of science, where the science scope is limited by the computational architecture as much as the physical processes at play. Here, we present a solution to this problem in the context of radio transients: realfast, a commensal, fast transient search system at the Jansky Very Large Array. Realfast uses a novel architecture to distribute fast-sampled interferometric data to a 32-node, 64-GPU cluster for real-time imaging and transient detection. By detecting transients in situ, we can trigger the recording of data for those rare, brief instants when the event occurs and reduce the recorded data volume by a factor of 1000. This makes it possible to commensally search a data stream that would otherwise be impossible to record. This system will search for millisecond transients in more than 1000 hours of data per year, potentially localizing several Fast Radio Bursts, pulsars, and other sources of impulsive radio emission. We describe the science scope for realfast, the system design, expected outcomes, and ways real-time analysis can help in other fields of astrophysics., Comment: Accepted to ApJS Special Issue on Data; 11 pages, 4 figures