Dynamics of Cytoskeletal Proteins during Fcγ Receptor-mediated Phagocytosis in Macrophages

Particle ingestion by phagocytosis results from sequential rearrangements of the actin cytoskeleton and overlying membrane. To assemble a chronology of molecular events during phagosome formation and to examine the contributions of phosphoinositide 3-kinase (PI 3-kinase) to these dynamics, a method was developed for synchronizing Fcγ receptor-mediated phagocytosis by murine macrophages. Erythrocytes opsonized with complement component C3bi were bound to macrophages at 37°C, a condition that does not favor particle phagocytosis. Addition of soluble anti-erythrocyte IgG resulted in rapid opsonization of the bound erythrocytes, followed by their immediate internalization via phagocytosis. Cellular content of F-actin, as measured by binding of rhodamine-phalloidin, increased transiently during phagocytosis, and this increase was not diminished by inhibitors of PI 3-kinase. Immunofluorescence localization of myosins in macrophages fixed at various times during phagocytosis indicated that myosins II and IXb were concentrated in early phagosomes, myosin IC increased later, and myosin V appeared after phagosome closure. Other cytoskeletal proteins showed similar variations in the timing of their appearance in phagosomes. The PI 3-kinase inhibitor wortmannin did not change the dynamics of PI 3-kinase or ezrin localization but prevented the loss of PAK1 from phagosomes. These results suggest that PI 3-kinase deactivates PAK1, and that this may be needed for phagosome closure

The JCMT Plane Survey: Early results from the ℓ = 30° field

We present early results from the JCMT (James Clerk Maxwell Telescope) Plane Survey (JPS), which has surveyed the northern inner Galactic plane between longitudes ℓ = 7° and ℓ = 63° in the 850-μm continuum with SCUBA-2 (Submm Common-User Bolometer Array 2), as part of the JCMT Legacy Survey programme. Data from the ℓ = 30° survey region, which contains the massive-star-forming regions W43 and G29.96, are analysed after approximately 40 per cent of the observations had been completed. The pixel-to-pixel noise is found to be 19 mJy beam-1 after a smooth over the beam area, and the projected equivalent noise levels in the final survey are expected to be around 10 mJy beam-1. An initial extraction of compact sourceswas performed using the FELLWALKER method, resulting in the detection of 1029 sources above a 5σ surface-brightness threshold. The completeness limits in these data are estimated to be around 0.2 Jy beam-1 (peak flux density) and 0.8 Jy (integrated flux density) and are therefore probably already dominated by source confusion in this relatively crowded section of the survey. The flux densities of extracted compact sources are consistent with those of matching detections in the shallower APEX (Atacama Pathfinder Experiment) Telescope Large Area Survey of the Galaxy (ATLASGAL) survey.We analyse the virial and evolutionary state of the detected clumps in the W43 star-forming complex and find that they appear younger than the Galactic-plane average. © 2015 The Authors

IGAPS: the merged IPHAS and UVEX optical surveys of the northern Galactic plane

The INT Galactic Plane Survey (IGAPS) is the merger of the optical photometric surveys, IPHAS and UVEX, based on data from the Isaac Newton Telescope (INT) obtained between 2003 and 2018. Here, we present the IGAPS point source catalogue. It contains 295.4 million rows providing photometry in the filters, i, r, narrow-band Hα, g, and URGO. The IGAPS footprint fills the Galactic coordinate range, |b| 5σ confidence)

IGAPS: the merged IPHAS and UVEX optical surveys of the northern Galactic plane⋆

Item does not contain fulltextThe INT Galactic Plane Survey (IGAPS) is the merger of the optical photometric surveys, IPHAS and UVEX, based on data from the Isaac Newton Telescope (INT) obtained between 2003 and 2018. Here, we present the IGAPS point source catalogue. It contains 295.4 million rows providing photometry in the filters, i, r, narrow-band Hα, g, and URGO. The IGAPS footprint fills the Galactic coordinate range, |b| 5σ confidence).nul