MINERvA High Energy Test Beam Calibration

The MINERvA experiment, housed at the Fermi National Accelerator Laboratory near Chicago, is a high-statistics experiment studying neutrino-nuclei interactions. Neutrino interaction models will be a limiting uncertainty of next generation neutrino oscillation experiments. Understanding the properties of neutrino oscillations may shine light on the matter vs anti-matter discrepancy in the universe. The data recorded by MINERvA can be compared with current neutrino interaction simulations to determine their level of agreement. Improving the agreement between simulation and data leads to improved neutrino models and reduced systematic uncertainties in neutrino oscillation measurements. Before comparisons can be made, the data collected must be calibrated. Test Beam experiments, small scale versions of the MINERvA detector, are used for in-depth analyses of various detector responses to known particles. Alignment calibration for Run 2 of Test Beam 2 was started. It was found the mapping between simulation detector components and the components on the physical detector was incorrect for the configuration of Run 2. This mapping was corrected and alignment completed. In addition, strip-to-strip calibration for uniform energy response among scintillator strips was completed. New alignment and strip-to-strip constants have been installed in the Test Beam framework for collaboration use

A repeating fast radio burst associated with a persistent radio source

The dispersive sweep of fast radio bursts (FRBs) has been used to probe the ionized baryon content of the intergalactic medium1, which is assumed to dominate the total extragalactic dispersion. Although the host-galaxy contributions to the dispersion measure appear to be small for most FRBs2, in at least one case there is evidence for an extreme magneto-ionic local environment3,4 and a compact persistent radio source5. Here we report the detection and localization of the repeating FRB 20190520B, which is co-located with a compact, persistent radio source and associated with a dwarf host galaxy of high specific-star-formation rate at a redshift of 0.241 ± 0.001. The estimated host-galaxy dispersion measure of approximately 903−111+72 parsecs per cubic centimetre, which is nearly an order of magnitude higher than the average of FRB host galaxies2,6, far exceeds the dispersion-measure contribution of the intergalactic medium. Caution is thus warranted in inferring redshifts for FRBs without accurate host-galaxy identifications

Measurement of ttˉt\bar{t} cross section in the lepton+jets channel at s=\sqrt{s} = 13 TeV with the ATLAS detector

Luminosity data collected in 2016 was analyzed for both the Beams Condition Monitor, BCM, and the LUminosity Cherenkov Integrating Detector, LUCID. The discrepancy between luminosity values of the two apparatuses was determined to be both visible interaction rate, $\mu$, and Bunch Crossing IDentification, BCID, dependent. Scale factors to make BCM in better agreement with LUCID were determined for this data. Data collected in 2015 in $\sqrt{s} = 13$ TeV with $3.2$ fb$^{-1}$ was used to analyze the 8 TeV and 13 TeV transfer functions available for use in the KLFitter tool. After comparing resultant kinematic variable distributions and resolutions, it was determined the 13 TeV transfer functions should be used for $\sqrt{s} = 13$ TeV data analyses

Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe

We present the localization and host galaxies of one repeating and two apparently non-repeating Fast Radio Bursts. FRB20180301A was detected and localized with the Karl G. Jansky Very Large Array to a star-forming galaxy at $z=0.3304$. FRB20191228A, and FRB20200906A were detected and localized by the Australian Square Kilometre Array Pathfinder to host galaxies at $z=0.2430$ and $z=0.3688$, respectively. We combine these with 13 other well-localized FRBs in the literature, and analyze the host galaxy properties. We find no significant differences in the host properties of repeating and apparently non-repeating FRBs. FRB hosts are moderately star-forming, with masses slightly offset from the star-forming main-sequence. Star formation and low-ionization nuclear emission-line region (LINER) emission are major sources of ionization in FRB host galaxies, with the former dominant in repeating FRB hosts. FRB hosts do not track stellar mass and star formation as seen in field galaxies (more than 95% confidence). FRBs are rare in massive red galaxies, suggesting that progenitor formation channels are not solely dominated by delayed channels which lag star formation by Gigayears. The global properties of FRB hosts are indistinguishable from core-collapse supernovae (CCSNe) and short gamma-ray bursts (SGRBs) hosts, and the spatial offset (from galaxy centers) of FRBs is mostly inconsistent with that of the Galactic neutron star population (95% confidence). The spatial offsets of FRBs (normalized to the galaxy effective radius) also differ from those of globular clusters (GCs) in late- and early-type galaxies with 95% confidence.Comment: 27 pages, 12 figures, 8 tables. Accepted for publication in the Astrophysical Journa