Auroral emissions are expected from the footprint of Callisto in Jupiter's upper atmosphere owing to the known interaction of its atmosphere with Jupiter's magnetosphere, and from the observed auroral emissions from the footprints of the other three Galilean satellites. The mapping of Callisto along modeled magnetic field lines at Jupiter, however, places the expected footprint at the same latitude as the main auroral emissions, making it difficult to detect. We analyzed ultraviolet images of Jupiter taken using the Hubble Space Telescope/Advanced Camera for Surveys instrument during a large observing campaign in 2007. Using a coaddition method similar to one used for Enceladus, we have identified a strong candidate for the footprint of Callisto on 24 May 2007. We tested this finding by applying the same coaddition technique to a nearly identical auroral configuration on 30 May 2007 when Callisto was behind Jupiter, not visible from Earth (central meridian longitude = 22°; sub‐Callisto system III longitude = 327°). By comparing the two coadded images, we can clearly see the presence of a strongly subcorotating spot close to the expected Callisto footprint location on 24 May and its absence on 30 May. On 24 May Callisto was located in the current sheet. We also found a probable candidate on 26 May 2007 during which time Callisto was positioned below the current sheet. The measured location and intensity of the auroral emission provide important information about the interaction of Callisto with Jupiter's magnetic field, the corotating plasma, and the neutral and ionized state of the thin atmosphere of Callisto.

The edge-on galaxy NGC 891 was probed using near-infrared (NIR) imaging polarimetry in the Hband (1.6 µm) with the Mimir instrument on the 1.8 m Perkins Telescope. Polarization was detected with signal-to-noise ratio greater than three out to a surface brightness of 18.8 mag arcsec −2 . The unweighted average and dispersion in polarization percentage (P ) across the full disk were 0.7% and 0.3%, respectively, and the same quantities for polarization position angle (P.A.) were 12 • and 19 • , respectively. At least one polarization null point, where P falls nearly to zero, was detected in the NE disk but not the SW disk. Several other asymmetries in P between the northern and southern disk were found and may be related to spiral structure. Profiles of P and P.A. along the minor axis of NGC 891 suggest a transition from magnetic (B) field tracing dichroic polarization near the disk mid-plane to scattering dominated polarization off the disk mid-plane. A comparison between NIR P.A. and radio (3.6 cm) synchrotron polarization P.A. values revealed similar B-field orientations in the central-northeast region, which suggests that the hot plasma and cold, star-forming interstellar medium may share a common B-field. Disk-perpendicular polarizations previously seen at optical wavelengths are likely caused by scattered light from the bright galaxy center and are unlikely to be tracing poloidal B-fields in the outer disk.

The Galactic Plane Infrared Polarization Survey (GPIPS) seeks to characterize the magnetic field in the dusty Galactic disk using near-infrared stellar polarimetry. All GPIPS observations were completed using the 1.83 m Perkins telescope and Mimir instrument. GPIPS observations surveyed 76 deg 2 of the northern Galactic plane, from Galactic longitudes 18 to 56 • and latitudes −1 to +1 • , in the H-band (1.6 µm). Surveyed stars span 7th to 16th mag, resulting in nearly 10 million stars with measured linear polarizations. Of these stars, ones with m H < 12.5 mag and polarization percentage uncertainties under 2% were judged to be high quality and number over one million. GPIPS data reveal plane-of-sky magnetic field orientations for numerous interstellar clouds for A V values to ∼30 mag. The average sky separation of stars with m H < 12.5 mag is about 30 arcsec, or about 60 per Planck polarization resolution element. Matching to Gaia DR2 showed the brightest GPIPS stars are red giants with distances in the 0.6-7.5 kpc range. Polarization orientations are mostly parallel to the

A faint star located 2arcsec from KIC8462852 was discovered in Keck10m adaptive optics imaging in the JHK near-infrared (NIR) in 2014 by Boyajian et al. (2016). The closeness of the star to KIC8462852 suggested that the two could constitute a binary, which might have implications for the cause of the brightness dips seen by Kepler and in ground-based optical studies. Here, NIR imaging in 2017 using the Mimir instrument resolved the pair and enabled measuring their separation. The faint star had moved 67±7milliarcsec (mas) relative to KIC8462852 since 2014. The relative proper motion of the faint star is 23.9±2.6masyr−1 , for a tangential velocity of 45±5kms −1 if it is at the same 390pc distance as KIC8462852. Circular velocity at the 750au current projected separation is 1.5kms −1 , hence the star pair cannot be bound.

Objective: The purpose of the study was to implement a comprehensive adverse childhood experiences (ACEs) screening protocol in a rural Integrated Primary Care Clinic serving Latino Children utilizing implementation science as a framework. Methods: The Exploration, Preparation, Implementation, Sustainment (EPIS) framework was utilized to guide and evaluate the implementation. There were 2,347 children who were screened with the developed protocol which included screening for ACEs, psychosocial problems, adolescent depression, and parental depression. Several implementation outcomes were collected and are reported, including a list of screening barriers and adaptations, a list of developed staff training, a clinician stakeholder survey and focus group, and a patient stakeholder survey. Results: Clinicians reported being satisfied with the protocol and indicated that screenings provided new clinical information, changed their clinical care and helped to inform the medical needs of patients. Barriers included inadequate time to complete screenings and over-screening for prevalent stressors in the community. Conclusions: Implementation science provides a reliable framework for the implementation of a comprehensive ACE screening process by identifying the necessary conditions for high-quality implementation. With the appropriate resources in place, screenings are possible and enhance patient care. More attention is needed to identify primary care interventions for ACEs. Implications for Impact StatementImplementation science provides models for implementation that can improve the uptake of ACE screenings in Pediatric Primary Care settings. Integrated Care presents a comprehensive interdisciplinary approach that aids in providing appropriate responses to positive screenings.