Where, when, and how well people park: a phone survey and field measurements

AVM and Low Speed Maneuvers: Human Factors Issues ProjectTwo evaluations were completed to characterize where, how often, and how accurately people normally park. A telephone survey of 30 drivers examined where people park most frequently and the problems drivers have parking. The focus was on executing maneuvers, not the availability of parking. Depending on how the question was asked, approximately 74 to 84 percent of the parking events involved perpendicular parking. Of the 8 parking-related crashes reported by subjects, 6 involved backing, usually with a vehicle traveling down an aisle or backing up from a parking stall. A field survey examined the parking accuracy of 102 vehicles in Ann Arbor, Michigan, a college town. For parallel parking, drivers parked about 4 in from the curb in spaces averaging 24 feet long. For angle parking, distances to the front of the space were bimodal, with some drivers parking about 10 inches from the end of the space and others overlapping by 10 in on average. Overall, drivers parked slightly to the right of center (by 1 inch for parallel parking and 4 inches for perpendicular parking) for 8.5 feet wide spaces. Yaw angles were almost always less than 1 degree for perpendicular and angle parking, but as much as 3 degrees for parallel parking, which is a more difficult task. The data from this experiment provide both a basis for establishing the conditions for parking experiments and baseline data on how well people park without assistance.Nissan Research Centerhttp://deepblue.lib.umich.edu/bitstream/2027.42/87990/1/102765.pd

A review of bovine cases consigned under veterinary certification to emergency and casualty slaughter in Ireland during 2006 to 2008

The emergency and casualty slaughter of cattle for human consumption (in cases where animals are likely to have suffered from acute or chronic pain, respectively) in Ireland requires that the animal is accompanied to the slaughterhouse by an official veterinary certificate (VC) completed on-farm by the owner's private veterinary practitioner (PVP). No published data is currently available in Ireland based on information provided in these VCs. In this paper, we present a review of bovine cases consigned under veterinary certification to emergency and casualty slaughter in Ireland during 2006 to 2008. All VCs during the years 2006 (where available), 2007 and 2008 were collected from four large Irish slaughterhouses. The data were computerized, and analysed using descriptive and spatial methods. In total, 1,255 VCs were enrolled into the study (1,255 study animals, 1,072 study herds), 798 (63.6%) and 457 (36.4%) animals were consigned to emergency and casualty slaughter, respectively. VCs were completed throughout the year, with consigned animals travelling a mean distance of 27.2 km from farm to slaughter. The time elapsed between veterinary certification and slaughter was greater than three days for 18.2% of all study animals. In 965 (76.9%) animals, the certified suspected disability related to the locomotory system, most commonly as a result of fractures. Among animals for which data were available, 11.9% were totally condemned at post-mortem. The transport of animals with fractured limbs and/or other painful conditions is a significant animal welfare concern.Deposited by bulk impor

The Power of High Precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch stars in the Dark Energy Survey

Blue Horizontal Branch (BHB) stars, excellent distant tracers for probing the Milky Way's halo density profile, are distinguished in the $(g-r)_0$ vs $(i-z)_0$ color space from another class of stars, blue straggler stars (BSs). We develop a Bayesian mixture model to classify BHB stars using high-precision photometry data from the Dark Energy Survey Data Release 2 (DES DR2). We select $\sim2100$ highly-probable BHBs based on their $griz$ photometry and the associated uncertainties, and use these stars to map the stellar halo over the Galactocentric radial range $20 \lesssim R \lesssim 70$ kpc. After excluding known stellar overdensities, we find that the number density $n_\star$ of BHBs can be represented by a power law density profile $n_\star \propto R^{-\alpha}$ with an index of $\alpha=4.28_{-0.12}^{+0.13}$, consistent with existing literature values. In addition, we examine the impact of systematic errors and the spatial inhomogeneity on the fitted density profile. Our work demonstrates the effectiveness of high-precision $griz$ photometry in selecting BHB stars. The upcoming photometric survey from the Rubin Observatory, expected to reach depths 2-3 magnitudes greater than DES during its 10-year mission, will enable us to investigate the density profile of the Milky Way's halo out to the virial radius, unravelling the complex processes of formation and evolution in our Galaxy.Comment: 22 pages, 18 figures. Submitted AAS Journal. Comments Welcome Code used in this work can be found at: https://github.com/sazabi4/Yu2024_BHB

S5S^5: Probing the Milky Way and Magellanic Clouds potentials with the 6-D map of the Orphan-Chenab stream

We present a 6-D map of the Orphan-Chenab (OC) stream by combining the data from 5 years of Southern Stellar Stream Spectroscopic Survey $S^5$ observations with Gaia EDR3 data. We reconstruct the proper motion, radial velocity, distance and on-sky track of stream stars with spline models and extract the stellar density along the stream. The stream has a total luminosity of $M_V=-8.2$ and an average metallicity of $[Fe/H]=-1.9$, similar to classical MW satellites like Draco. The stream shows drastic changes in its physical width varying from 200 pc to 1 kpc, a constant line of sight velocity dispersion of 5 km/s, but an increase in the velocity dispersion along the stream near pericenter to $\sim$ 10 km/s. Despite the large apparent variation in the stellar number density along the stream, the flow rate of stars along the stream is remarkably constant. We model the 6-D stream track by a Lagrange-point stripping method with a flexible MW potential in the presence of a moving extended LMC potential. This allows us to constrain the mass profile of the MW within the distance range 15.6 < r < 55.5 kpc, with the best measured enclosed mass of $(2.85\pm 0.1)\times10^{11}\,M_\odot$ within 32.4 kpc. With the OC stream's closest approach distance to the LMC of $\sim 21$ kpc, our stream measurements are highly sensitive to the LMC mass profile with the most precise measurement of the LMC's enclosed mass being at 32.8 kpc with $M=(7.02\pm 0.9)\times10^{10}\, {M}_\odot$. We confidently detect that the LMC DM halo extends to at least 53 kpc. The fitting of the OC stream allows us to constrain the past LMC trajectory and the degree of dynamical friction it experienced. We demonstrate that the stars on the OC stream show large energy and angular momentum spreads caused by the LMC perturbation and revealing the limitations of orbital invariants for substructure identification in the MW halo.Comment: submitted to MNRAS; comments welcome; data released with the paper is available on Zenodo https://zenodo.org/record/722265

Signature of a massive rotating metal-poor star imprinted in the Phoenix stellar stream*

The Phoenix stellar stream has a low intrinsic dispersion in velocity and metallicity that implies the progenitor was probably a low mass globular cluster. In this work we use Magellan/MIKE high-dispersion spectroscopy of eight Phoenix stream red giants to confirm this scenario. In particular, we find negligible intrinsic scatter in metallicity ($\sigma(\mathrm{[Fe~II/H]}) = 0.04^{+0.11}_{-0.03}$) and a large peak-to-peak range in [Na/Fe] and [Al/Fe] abundance ratios, consistent with the light element abundance patterns seen in the most metal-poor globular clusters. However, unlike any other globular cluster, we also find an intrinsic spread in [Sr II/Fe] spanning $\sim$1 dex, while [Ba II/Fe] shows nearly no intrinsic spread ($\sigma(\mathrm{[Ba~II/H]}) = {0.03}^{+0.10}_{-0.02}$). This abundance signature is best interpreted as slow neutron capture element production from a massive fast-rotating metal-poor star ($15-20 \mathrm{M}_\odot$, $v_\mathrm{ini}/v_\mathrm{crit} = 0.4$, $[\mathrm{Fe/H}] = -3.8$). The low inferred cluster mass suggests the system would have been unable to retain supernovae ejecta, implying that any massive fast-rotating metal-poor star that enriched the interstellar medium must have formed and evolved before the globular cluster formed. Neutron capture element production from asymptotic giant branch stars or magneto-rotational instabilities in core-collapse supernovae provide poor fits to the observations. We also report one Phoenix stream star to be a lithium-rich giant ($A(\mathrm{Li}) = 3.1 \pm 0.1$). At $[\mathrm{Fe/H}] = -2.93$ it is among the most metal-poor lithium-rich giants known.Comment: Accepted to ApJ 2021-07-0

Multiple Populations and a CH Star Found in the 300S Globular Cluster Stellar Stream

Milky Way globular clusters (GCs) display chemical enrichment in a phenomenon called multiple stellar populations (MSPs). While the enrichment mechanism is not fully understood, there is a correlation between a cluster's mass and the fraction of enriched stars found therein. However, present-day GC masses are often smaller than their masses at the time of formation due to dynamical mass loss. In this work, we explore the relationship between mass and MSPs using the stellar stream 300S. We present the chemical abundances of eight red giant branch member stars in 300S with high-resolution spectroscopy from Magellan/MIKE. We identify one enriched star characteristic of MSPs and no detectable metallicity dispersion, confirming that the progenitor of 300S was a globular cluster. The fraction of enriched stars (12.5\%) observed in our 300S stars is less than the 50\% of stars found enriched in Milky Way GCs of comparable present-day mass ($\sim10^{4.5}$\msun). We calculate the mass of 300S's progenitor and compare it to the initial masses of intact GCs, finding that 300S aligns well with the trend between the system mass at formation and enrichment. 300S's progenitor may straddle the critical mass threshold for the formation of MSPs and can therefore serve as a benchmark for the stellar enrichment process. Additionally, we identify a CH star, with high abundances of \textit{s}-process elements, probably accreted from a binary companion. The rarity of such binaries in intact GCs may imply stellar streams permit the survival of binaries that would otherwise be disrupted.Comment: 15 pages, 7 tables, 8 figures. Accepted for publication in MNRA

Multiple Populations and a CH Star Found in the 300S Globular Cluster Stellar Stream

Milky Way globular clusters (GCs) display chemical enrichment in a phenomenon called multiple stellar populations (MSPs). While the enrichment mechanism is not fully understood, there is a correlation between a cluster’s mass and the fraction of enriched stars found therein. However, present-day GC masses are often smaller than their masses at the time of formation due to dynamical mass loss. In this work, we explore the relationship between mass and MSPs using the stellar stream 300S. We present the chemical abundances of eight red giant branch member stars in 300S with high-resolution spectroscopy fromMagellan/MIKE. We identify one enriched star characteristic of MSPs and no detectable metallicity dispersion, confirming that the progenitor of 300S was a globular cluster. The fraction of enriched stars (12.5%) observed in our 300S stars is less than the 50% of stars found enriched in Milky Way GCs of comparable present-day mass (∼ 104.5 M⊙). We calculate the mass of 300S’sprogenitor and compare it to the initial masses of intact GCs, finding that 300S aligns well with the trend between the system mass at formation and enrichment. 300S’s progenitor may straddle the critical mass threshold for the formation of MSPs and can therefore serve as a benchmark for the stellar enrichment process. Additionally, we identify a CH star, with high abundancesof s-process elements, probably accreted from a binary companion. The rarity of such binaries in intact GCs may imply stellar streams permit the survival of binaries that would otherwise be disrupted

Binding of C4b-binding protein: A molecular mechanism of serum resistance of Neisseria gonorrhoeae

We screened 29 strains of Neisseria gonorrhoeae and found 16/21 strains that resisted killing by normal human serum and 0/8 serum sensitive strains that bound the complement regulator, C4b-binding protein (C4bp). Microbial surface-bound C4bp demonstrated cofactor activity. We constructed gonococcal strains with hybrid porin (Por) molecules derived from each of the major serogroups (Por1A and Por1B) of N. gonorrhoeae, and showed that the loop 1 of Por1A is required for C4bp binding. Por1B loops 5 and 7 of serum-resistant gonococci together formed a negatively charged C4bp-binding domain. C4bp-Por1B interactions were ionic in nature (inhibited by high salt or by heparin), whereas the C4bp-Por1A bond was hydrophobic. Only recombinant C4bp mutant molecules containing the NH2-terminal alpha-chain short consensus repeat (SCR1) bound to both Por1A and Por1B gonococci, suggesting that SCR1 contained Por binding sites. C4bp alpha-chain monomers did not bind gonococci, indicating that the polymeric form of C4bp was required for binding. Using fAb fragments against C4bp SCR1, C4bp binding to Por1A and Por1B strains was inhibited in a complement-dependent serum bactericidal assay. This resulted in complete killing of these otherwise fully serum resistant strains in only 10% normal serum, underscoring the importance of C4bp in mediating gonococcal serum resistance

Broken into Pieces::ATLAS and Aliqa Uma as One Single Stream

We present the first spectroscopic measurements of the ATLAS and Aliqa Uma streams from the Southern Stellar Stream Spectroscopic Survey ($S^5$), in combination with the photometric data from the Dark Energy Survey and astrometric data from $Gaia$. From the coherence of spectroscopic members in radial velocity and proper motion, we find out that these two systems are extremely likely to be one stream with discontinuity in morphology and density on the sky (the "kink" feature). We refer to this entire stream as the ATLAS-Aliqa Uma stream, or the AAU stream. We perform a comprehensive exploration of the effect of baryonic substructures and find that only an encounter with the Sagittarius dwarf $\sim 0.5$ Gyr ago can create a feature similar to the observed "kink". In addition, we also identify two gaps in the ATLAS component associated with the broadening in the stream width (the "broadening" feature). These gaps have likely been created by small mass perturbers, such as dark matter halos, as the AAU stream is the most distant cold stream known with severe variations in both the stream surface density and the stream track on the sky. With the stream track, stream distance and kinematic information, we determine the orbit of the AAU stream and find that it has been affected by the Large Magellanic Cloud, resulting in a misalignment between the proper motion and stream track. Together with the Orphan-Chenab Stream, AAU is the second stream pair that has been found to be a single stream separated into two segments by external perturbation.Comment: 33 pages, 22 figures (including 1 movie), 3 tables. Accepted for publication in Ap