Exploring graduate student parent experiences: How to better support and reduce attrition in an underserved population

Changes in the global economy, employer expectations, and cultural norms are causing a shift in the demographics of post-baccalaureate students. Out of necessity to support oneself in an increasingly demanding job market, female graduate student enrollment has been on the rise for a number of years. This, in combination with a general increase in the number of individuals enrolling in graduate degree programs while trying to balance the responsibility of raising children presents a growing problem for institutions of higher education. Graduate student parents are a population that requires additional and varying support services than those of the traditional graduate student. The unique challenges faced by this population can prove to be overwhelming at best, and this struggle can lead to attrition in many cases. There is a not only an absence of information regarding the best way in which to support graduate student parents, but some institutions seem to be largely unaware of the problem. James Madison University exhibits a complete lack of demographic information on its own graduate parent population, as well as a gap in an understanding of the ways in which these students could be better supported, thus reducing their risk of attrition. A mixed-methods research design that relies on survey questions addressing the experiences, perceptions, and unmet needs of graduate parents at JMU provides some of this preliminary information. Future research is needed to further qualify the services that could be provided to these students that would hold the most value for graduate parents, but survey results revealed a number of themes regarding the experiences, satisfaction, and needed support services within the population of JMU graduate student parents

No sign (yet) of intergalactic globular clusters in the Local Group

We present Gemini Multi-Object Spectrograph (GMOS) imaging of 12 candidate intergalactic globular clusters (IGCs) in the Local Group, identified in a recent survey of the Sloan Digital Sky Survey (SDSS) footprint by di Tullio Zinn & Zinn. Our image quality is sufficiently high, at ∼0.4–0.7 arcsec, that we are able to unambiguously classify all 12 targets as distant galaxies. To reinforce this conclusion we use GMOS images of globular clusters in the M31 halo, taken under very similar conditions, to show that any genuine clusters in the putative IGC sample would be straightforward to distinguish. Based on the stated sensitivity of the di Tullio Zinn & Zinn search algorithm, we conclude that there cannot be a significant number of IGCs with MV ≤ −6 lying unseen in the SDSS area if their properties mirror those of globular clusters in the outskirts of M31 – even a population of 4 would have only a ≈1 per cent chance of non-detection

Stellar metallicity gradients of Local Group dwarf galaxies

Aims. We explore correlations between the strength of metallicity gradients in Local Group dwarf galaxies and their stellar mass, star formation history timescales, and environment. Methods. We performed a homogeneous analysis of literature spectroscopic data of red giant stars and determined radial metallicity profiles for 30 Local Group dwarf galaxies. This is the largest compilation of this type to date. Results. The dwarf galaxies in our sample show a variety of metallicity profiles, most of them decreasing with radius and some with rather steep profiles. The derived metallicity gradients as a function of the half-light radius, [Fe/H](R/Re), show no statistical differences when compared with the morphological type of the galaxies, nor with their distance from the Milky Way or M31. No correlations are found with either stellar mass or star formation timescales. In particular, we do not find the linear relation between [Fe/H](R/Re) and the galaxy median age t50, which has been reported in the literature for a set of simulated systems. On the other hand, the high angular momentum in some of our galaxies does not seem to affect the gradient strengths. The strongest gradients in our sample are observed in systems that are likely to have experienced a past merger event. When these merger candidates are excluded, the analysed dwarf galaxies show mild gradients (ã-0.1 dex Re-1) with little scatter between them, regardless of their stellar mass, dynamical state, and their star formation history. These results agree well with different sets of simulations presented in the literature that were analysed using the same method as for the observed dwarf galaxies. Conclusions. The interplay between the multitude of factors that could drive the formation of metallicity gradients likely combine in complex ways to produce in general comparable mild [Fe/H](R/Re) values, regardless of stellar mass and star formation history. The strongest driver of steep gradients seems to be previous dwarf-dwarf merger events in a system