Western Reports, April, 1958, Volume 07, Issue 02

Publication at Western Washington Universityhttps://cedar.wwu.edu/alumni_reports/1012/thumbnail.jp

Western Reports, December, 1957, Volume 07, Issue 01

Publication at Western Washington Universityhttps://cedar.wwu.edu/alumni_reports/1011/thumbnail.jp

Social Anxiety and Fear of Evaluation in Middle Schoolers

Social anxiety can have a significant effect on adults and adolescents alike, causing significant distress and impairment. Fear of negative evaluation has been found to be positively correlated to social anxiety in adults and adolescents. Thus, an individual who has social anxiety tends to worry that they will be judged negatively by others in social situations. More recently, fear of positive evaluation also has correlated positively to social anxiety in adults (Weeks, Heimberg, & Rodebaugh, 2008); thus, adults with social anxiety tend to also fear when they are given positive feedback, such as a compliment. This study examines the links of social anxiety to both the fear of negative evaluation and the fear of positive evaluation in an adolescent sample; social anxiety was related to both fear of negative evaluation and fear of positive evaluation in this population. In addition, this study adds to the literature by including a related type of anxiety - test anxiety, which also has a social evaluative component. Specifically, this study examined whether social anxiety acts as a moderator in the relationships between test anxiety and the fear of negative and positive evaluation. This was supported for test anxiety and the fear of negative evaluation however, was not supported for test anxiety and fear of positive evaluation. Finally, suggestions for further research and clinical implications are discussed

Coevolution of metallicity and star formation in galaxies to z=3.7: I. A fundamental plane

With the aim of understanding the coevolution of star formation rate (SFR), stellar mass (M*), and oxygen abundance (O/H) in galaxies up to redshift z=3.7, we have compiled the largest available dataset for studying Metallicity Evolution and Galaxy Assembly (MEGA); it comprises roughly 1000 galaxies with a common O/H calibration and spans almost two orders of magnitude in metallicity, a factor of 10^6 in SFR, and a factor of 10^5 in stellar mass. From a Principal Component Analysis, we find that the 3-dimensional parameter space reduces to a Fundamental Plane of Metallicity (FPZ) given by 12+log(O/H) = -0.14 log (SFR) + 0.37 log (M*) + 4.82. The mean O/H FPZ residuals are small (0.16 dex) and consistent with trends found in smaller galaxy samples with more limited ranges in M*, SFR, and O/H. Importantly, the FPZ is found to be redshift-invariant within the uncertainties. In a companion paper, these results are interpreted with an updated version of the model presented by Dayal et al. (2013).Comment: 19 pages, 10 figures, 4 tables, accepted for publication in MNRA

Building galaxies:from low-metallicity compact dwarfs to active galactic nuclei

Moderne sterrenkundige theorieën zeggen dat grote sterrenstelsels ontstaan uit het samensmelten van kleinere. Leslie Kipp Hunt deed onderzoek aan twee dwergstelsels om te kijken of dit inderdaad jonge stelsels zijn, die nog maar net begonnen zijn met het vormen van sterrren. De resultaten van haar onderzoek wijzen inderdaad in die richting. Ook deed ze statistisch onderzoek naar 1400 reuzengalaxies, met name naar de vraag hoe die groeien. Het bleek dat de groei en evolutie van die stelsels in relatie staat met de zwarte gaten in de kern van stelsel

PSD-95 Is Associated with the Postsynaptic Density and Not with the Presynaptic Membrane at Forebrain Synapses

PSD-95, a prominent protein component of the postsynaptic density (PSD) fraction from rat forebrain, has been localized by light microscopy to dendrites of hippocampal neurons (Cho et al., 1992) and to the presynaptic plexus of cerebellar basket cells (Kistner et al., 1993). Here we extend these studies to show that an affinity-purified antibody to PSD-95 labels the dendrites of most neurons in the forebrain and of a subset of neurons in the cerebellum. To confirm that PSD-95 is associated with the PSD at forebrain synapses and to clarify whether it is also associated with the presynaptic membrane, we employed immunogold electron microscopy of forebrain synaptosomes. Gold-labeled antibodies to PSD-95 labeled postsynaptic densities in both intact and lysed forebrain synaptosomes but did not label presynaptic terminals or the presynaptic membrane. The asymmetric distribution of PSD-95 at synapses contrasts with that of its homologs, disks-large and ZO-1, which are arranged symmetrically at septate and tight junctions, respectively

The Relation between Black Hole Mass, Bulge Mass, and Near-Infrared Luminosity

We present new accurate near-infrared (NIR) spheroid (bulge) structural parameters obtained by two-dimensional image analysis for all galaxies with a direct black hole (BH) mass determination. As expected, NIR bulge luminosities Lbul and BH masses are tightly correlated, and if we consider only those galaxies with secure BH mass measurement and accurate Lbul (27 objects), the spread of MBH-Lbul is similar to MBH-sigma, where sigma is the effective stellar velocity dispersion. We find an intrinsic rms scatter of ~0.3 dex in log MBH. By combining the bulge effective radii R_e measured in our analysis with sigma, we find a tight linear correlation (rms ~ 0.25 dex) between MBH and the virial bulge mass (propto R_e sigma^2), with ~ 0.002. A partial correlation analysis shows that MBH depends on both sigma and R_e, and that both variables are necessary to drive the correlations between MBH and other bulge properties.Comment: Astrophysical Journal Letters, in pres

The resolved star-formation relation in nearby active galactic nuclei

We present an analysis of the relation between star formation rate (SFR) surface density (sigmasfr) and mass surface density of molecular gas (sigmahtwo), commonly referred to as the Kennicutt-Schmidt (K-S) relation, at its intrinsic spatial scale, i.e. the size of giant molecular clouds (10-150 pc), in the central, high-density regions of four nearby low-luminosity active galactic nuclei (AGN). We used interferometric IRAM CO(1-0) and CO(2-1), and SMA CO(3-2) emission line maps to derive sigmahtwo and HST-Halpha images to estimate sigmasfr. Each galaxy is characterized by a distinct molecular SF relation at spatial scales between 20 to 200 pc. The K-S relations can be sub-linear, but also super-linear, with slopes ranging from 0.5 to 1.3. Depletion times range from 1 and 2Gyr, compatible with results for nearby normal galaxies. These findings are valid independently of which transition, CO(1-0), CO(2-1), or CO(3-2), is used to derive sigmahtwo. Because of star-formation feedback, life-time of clouds, turbulent cascade, or magnetic fields, the K-S relation might be expected to degrade on small spatial scales (<100 pc). However, we find no clear evidence for this, even on scales as small as 20 pc, and this might be because of the higher density of GMCs in galaxy centers which have to resist higher shear forces. The proportionality between sigmahtwo and sigmasfr found between 10 and 100 Msun/pc2 is valid even at high densities, 10^3 Msun/pc2. However, by adopting a common CO-to-H2 conversion factor (alpha_CO), the central regions of the galaxies have higher sigmasfr for a given gas column than those expected from the models, with a behavior that lies between the mergers/high-redshift starburst systems and the more quiescent star-forming galaxies, assuming that the first ones require a lower value of alpha_CO.Comment: 22 pages, 8 figures, Accepted for publication in Astronomy and Astrophysic