Metal enrichment processes

There are many processes that can transport gas from the galaxies to their environment and enrich the environment in this way with metals. These metal enrichment processes have a large influence on the evolution of both the galaxies and their environment. Various processes can contribute to the gas transfer: ram-pressure stripping, galactic winds, AGN outflows, galaxy-galaxy interactions and others. We review their observational evidence, corresponding simulations, their efficiencies, and their time scales as far as they are known to date. It seems that all processes can contribute to the enrichment. There is not a single process that always dominates the enrichment, because the efficiencies of the processes vary strongly with galaxy and environmental properties.Comment: 18 pages, 8 figures, accepted for publication in Space Science Reviews, special issue "Clusters of galaxies: beyond the thermal view", Editor J.S. Kaastra, Chapter 17; work done by an international team at the International Space Science Institute (ISSI), Bern, organised by J.S. Kaastra, A.M. Bykov, S. Schindler & J.A.M. Bleeke

Targeting Tax Relief at Youth Employment

Canada's Youth Hires program was a targeted employment subsidy that rebated employment insurance premiums to employers with net increases in insurable earnings for youth aged 18-24. Using a difference-in-differences approach, in each of two datasets statistically and economically significant employment impacts are observed. Most of the evidence suggests that the 2-2.4 weeks of increased employment resulted from an aggregate reduction in those not in the labour force, with at most a modest change in the unemployment rate. Many estimated effects are larger for males than females. Notably, strong evidence of displacement (substitution away from slightly older non-subsidized workers) is not observed. However, there may be a small reduction in full-time schooling for the targeted group

Gaia Early Data Release 3: The celestial reference frame (Gaia-CRF3)

Context. Gaia-CRF3 is the celestial reference frame for positions and proper motions in the third release of data from the Gaia mission, Gaia DR3 (and for the early third release, Gaia EDR3, which contains identical astrometric results). The reference frame is defined by the positions and proper motions at epoch 2016.0 for a specific set of extragalactic sources in the (E)DR3 catalogue. Aims. We describe the construction of Gaia-CRF3 and its properties in terms of the distributions in magnitude, colour, and astrometric quality. Methods. Compact extragalactic sources in Gaia DR3 were identified by positional cross-matching with 17 external catalogues of quasi-stellar objects (QSO) and active galactic nuclei (AGN), followed by astrometric filtering designed to remove stellar contaminants. Selecting a clean sample was favoured over including a higher number of extragalactic sources. For the final sample, the random and systematic errors in the proper motions are analysed, as well as the radio-optical offsets in position for sources in the third realisation of the International Celestial Reference Frame (ICRF3). Results. Gaia-CRF3 comprises about 1.6 million QSO-like sources, of which 1.2 million have five-parameter astrometric solutions in Gaia DR3 and 0.4 million have six-parameter solutions. The sources span the magnitude range G = 13-21 with a peak density at 20.6 mag, at which the typical positional uncertainty is about 1 mas. The proper motions show systematic errors on the level of 12 μas yr-1 on angular scales greater than 15 deg. For the 3142 optical counterparts of ICRF3 sources in the S/X frequency bands, the median offset from the radio positions is about 0.5 mas, but it exceeds 4 mas in either coordinate for 127 sources. We outline the future of Gaia-CRF in the next Gaia data releases. Appendices give further details on the external catalogues used, how to extract information about the Gaia-CRF3 sources, potential (Galactic) confusion sources, and the estimation of the spin and orientation of an astrometric solution

Quadro citológico vaginal, concentração plasmática de progesterona durante a gestação e medidas fetais em paca (Cuniculus paca Linnaeus, 1766)

Em 27 pacas (Cuniculus paca Linnaeus, 1766) objetivou-se descrever aos 30, 60 e 90 dias (D) de prenhez diagnosticada por ultrassonografia (US), os tipos celulares do epitélio vaginal em esfregaços vaginais, relatar as condições de abertura da vulva e as características do muco vaginal, determinar a concentração plasmática de progesterona (P4) por radioimunoensaio, e ainda, mensurar por ultrassonografia (US) o diâmetro biparietal (DBP) fetal aos 60 e 90 dias de prenhez. No D30, 40% das amostras exibiram células (com características estrogênicas) superficiais e presença de núcleos nus. Nos D60 e D90, células parabasais, intermediárias, superficiais e naviculares estavam presentes nas mesmas proporções, mas células endocervicais foram descritas em apenas 73,9% e 69% das amostras daqueles dias, respectivamente. No D30 a maior proporção de células naviculares e superficiais diferiu (p The objective of this work was to describe in 27 pacas (Cuniculus paca Linnaeus, 1766) at 30, 60 and 90 days (D) of pregnancy diagnosed by ultrasonography (U.S.) the cell types of the vaginal epithelium by vaginal smears, to report the vulva opening condition and the characteristics of vaginal mucus, to determine the progesterone (P4) serum concentration by radioimmunoassay, and also measure by ultrasound (U.S.) the fetuses biparietal diameter (BPD) at 60 and 90 days of pregnancy. At D30, 40% of the smears exhibited surface cells (with estrogenic characteristics) and of naked nuclei. At D60 and D90, parabasal, intermediate, superficial, and navicular cells were present in the same proportions, but endocervical cells were described in only 73.9% and 69% of those day's smears, respectively. At D30 the highest proportion of navicular and surface cells differed (p < 0.05) compared with other cell types. The vaginal mucus was crystalline and fluid in 100% and 70% of females at D30 and D60, respectively. It was observed the vaginal vestibule open in around 50% of females in every day of exams. Minimum detectable P4 serum concentration was obtained on 72% and 83% of females, while the averages of the BPD were 1.25 cm (± 0.16) and 2.34 cm (± 0.25) on D60 and D90, respectively. Vaginal cytology aspects at D30, D60 and D90 and BPD provide elements to contribute to pregnancy diagnosis in paca. P4 concentration shows the need of further endocrinology of pregnancy studies of paca

Gaia Early Data Release 3: acceleration of the solar system from Gaia astrometry

Stars and planetary system

The PLATO mission

PLATO (PLAnetary Transits and Oscillations of stars) is ESA’s M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2R ) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5%, 10%, 10% for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO‘s target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile towards the end of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases