Recovery of Benthic Macroinvertebrate Communities after Restoration in Two Intensively Mined Watersheds

As the body of literature supporting watershed-scale restoration projects continues to grow, there is need for a greater understanding of the underlying mechanisms that drive it. With data spanning ten years capturing pre- and post-restoration benthic macroinvertebrate communities in two distinct watersheds of West Virginia, we seek to contribute to the developing pool of knowledge regarding these dynamics. Sites were laid out prior to remediation in such a manner as to capture the spectrum of water quality conditions present, these are divided into three treatment types: reference, treated, and abandoned mine drainage (AMD). Our objectives were to: 1) determine if previously documented trends of improvement persisted into 2018, 2) explore specific impacts on community structure, and 3) determine if distance to remediation impacted degree of recovery. We hypothesized that: 1) previously measured improvements would continue, 2) watershed-wide communities would exhibit less variation over time as they grew more similar overall to reference quality, and 3) that sites situated farther from active treatment locations would exhibit greater degrees of recovery. In order to provide meaningful and holistic interpretations of the community data collected, we analyzed how site distance from active treatment dosers impacts scores from indices of biotic integrity as well as Bray-Curtis distance coefficients on community similarity. We found that the previously documented recovery was still in evidence, however at a much lesser rate. Contrary to our other hypotheses, watershed-wide communities became generally more diverse over time; and distance to treatment yielded opposite trends in recovery between our two watersheds

A Multidimensional Conceptualization of Environmental Velocity

Environmental velocity has emerged as an important concept but remains theoretically underdeveloped, particularly with respect to its multidimensionality. In response, we develop a framework that examines the variations in velocity across multiple dimensions of the environment (homology) and the causal linkages between those velocities (coupling). We then propose four velocity regimes based on different patterns of homology and coupling and argue that the conditions of each regime have important implications for organizations

The Origin of [O II] Emission in Recently Quenched Active Galaxy Nucleus Hosts

We have employed emission-line diagnostics derived from DEIMOS and NIRSPEC spectroscopy to determine the origin of the [O II] emission line observed in six active galactic nucleus (AGN) hosts at z ~ 0.9. These galaxies are a subsample of AGN hosts detected in the Cl1604 supercluster that exhibit strong Balmer absorption lines in their spectra and appear to be in a post-starburst or post-quenched phase, if not for their [O II] emission. Examining the flux ratio of the [N II] to Hα lines, we find that in five of the six hosts the dominant source of ionizing flux is AGN continuum emission. Furthermore, we find that four of the six galaxies have over twice the [O II] line luminosity that could be generated by star formation alone given their Hα line luminosities. This strongly suggests that AGN-excited narrow-line emission is contaminating the [O II] line flux. A comparison of star formation rates calculated from extinction-corrected [O II] and Hα line luminosities indicates that the former yields a five-fold overestimate of the current activity in these galaxies. Our findings reveal the [O II] line to be a poor indicator of star formation activity in a majority of these moderate-luminosity Seyferts. This result bolsters our previous findings that an increased fraction of AGN at high redshifts is hosted by galaxies in a post-starburst phase. The relatively high fraction of AGN hosts in the Cl1604 supercluster that show signs of recently truncated star formation activity may suggest that AGN feedback plays an increasingly important role in suppressing ongoing activity in large-scale structures at high redshift

The Violent Youth of Bright and Massive Cluster Galaxies and their Maturation over 7 Billion Years

In this study we investigate the formation and evolution mechanisms of the brightest cluster galaxies (BCGs) over cosmic time. At high redshift ($z\sim0.9$), we selected BCGs and most massive cluster galaxies (MMCGs) from the Cl1604 supercluster and compared them to low-redshift ($z\sim0.1$) counterparts drawn from the MCXC meta-catalog, supplemented by SDSS imaging and spectroscopy. We observed striking differences in the morphological, color, spectral, and stellar mass properties of the BCGs/MMCGs in the two samples. High-redshift BCGs/MMCGs were, in many cases, star-forming, late-type galaxies, with blue broadband colors, properties largely absent amongst the low-redshift BCGs/MMCGs. The stellar mass of BCGs was found to increase by an average factor of $2.51\pm0.71$ from $z\sim0.9$ to $z\sim0.1$. Through this and other comparisons we conclude that a combination of major merging (mainly wet or mixed) and \emph{in situ} star formation are the main mechanisms which build stellar mass in BCGs/MMCGs. The stellar mass growth of the BCGs/MMCGs also appears to grow in lockstep with both the stellar baryonic and total mass of the cluster. Additionally, BCGs/MMCGs were found to grow in size, on average, a factor of $\sim3$, while their average S\'ersic index increased by $\sim$0.45 from $z\sim0.9$ to $z\sim0.1$, also supporting a scenario involving major merging, though some adiabatic expansion is required. These observational results are compared to both models and simulations to further explore the implications on processes which shape and evolve BCGs/MMCGs over the past $\sim$7 Gyr.Comment: Accepted for publication in MNRA

Student-Athlete School Selection: A Family Systems Theory Approach

The primary focus of this study was to examine the role family members play in the college selection process for NCAA Division III student-athletes. The role of family members in the college selection process has been studied for nonathletes, NCAA Division I athletes, NCAA Division II athletes, and at a cross-divisional level for specific NCAA sports. In such research related to intercollegiate student-athletes, research has primarily been conducted quantitatively with the use of survey techniques. Little research exists specifically exploring the role of family members in the college selection process for NCAA Division III athletes. Based on the lack of research, the overarching Division III philosophy, the pure participation rates of NCAA Division III athletes (more than 180,000 current Division III athletes), and the ideal fit of Family Systems Theory to this selection process, this research study is fitting. In this project, sixty-nine student-athletes participated in semistructured interviews at eleven different NCAA Division III institutions. Five prompts directly related to potential family influence were asked. Data were analyzed using open coding based on a priori and emergent themes. Responses are collectively summarized and representative responses are presented verbatim. Results are also discussed through the framework of Family Systems Theory and related back to previous literature on the role of the family in the college selection process

Detection and Interpretation Of Long-Lived X-Ray Quasi-Periodic Pulsations in the X-Class Solar Flare On 2013 May 14

Quasi-periodic pulsations (QPP) seen in the time derivative of the GOES soft X-ray light curves are analyzed for the near-limb X3.2 event on 14 May 2013. The pulsations are apparent for a total of at least two hours from the impulsive phase to well into the decay phase, with a total of 163 distinct pulses evident to the naked eye. A wavelet analysis shows that the characteristic time scale of these pulsations increases systematically from $\sim$25 s at 01:10 UT, the time of the GOES peak, to $\sim$100 s at 02:00 UT. A second ridge in the wavelet power spectrum, most likely associated with flaring emission from a different active region, shows an increase from $\sim$40 s at 01:40 UT to $\sim$100 s at 03:10 UT. We assume that the QPP that produced the first ridge result from vertical kink-mode oscillations of the newly formed loops following magnetic reconnection in the coronal current sheet. This allows us to estimate the magnetic field strength as a function of altitude given the density, loop length, and QPP time scale as functions of time determined from the GOES light curves and RHESSI images. The calculated magnetic field strength of the newly formed loops ranges from about $\sim$500 G at an altitude of 24 Mm to a low value of $\sim$10 G at 60 Mm, in general agreement with the expected values at these altitudes. Fast sausage mode oscillations are also discussed and cannot be ruled out as an alternate mechanism for producing the QPP

The Fourier Imaging X-ray Spectrometer (FIXS) for the Argentinian, Scout-launched satelite de Aplicaciones Cienficas-1 (SAC-1)

The Fourier Imaging X-ray Spectrometer (FIXS) is one of four instruments on SAC-1, the Argentinian satellite being proposed for launch by NASA on a Scout rocket in 1992/3. The FIXS is designed to provide solar flare images at X-ray energies between 5 and 35 keV. Observations will be made on arcsecond size scales and subsecond time scales of the processes that modify the electron spectrum and the thermal distribution in flaring magnetic structures