Chemical Self-Enrichment of HII Regions by the Wolf-Rayet Phase of an 85 Msun star

It is clear from stellar evolution and from observations of WR stars that massive stars are releasing metal-enriched gas through their stellar winds in the Wolf-Rayet phase. Although HII region spectra serve as diagnostics to determine the present-day chemical composition of the interstellar medium, it is far from being understood to what extent the HII gas is already contaminated by chemically processed stellar wind. Therefore, we analyzed our models of radiative and wind bubbles of an isolated 85 Msun star with solar metallicity (Kr\"oger et al. 2006) with respect to the chemical enrichment of the circumstellar HII region. Plausibly, the hot stellar wind bubble (SWB) is enriched with 14N during the WN phase and even much higher with 12C and 16O during the WC phase of the star. During the short period that the 85 Msun star spends in the WC stage enriched SWB material mixes with warm HII gas of solar abundances and thus enhances the metallicity in the HII region. However, at the end of the stellar lifetime the mass ratios of the traced elements N and O in the warm ionized gas are insignificantly higher than solar, whereas an enrichment of 22 % above solar is found for C. Important issues from the presented study comprise a steeper radial gradient of C than O and a decreasing effect of self-enrichment for metal-poor galaxies.Comment: 5 pages, 3 figures, accepted for publication in A&A Letter

How Functionalist and Process Approaches to Behavior Can Explain Trait Covariation

Factors identified in investigations of trait structure (e.g., the Big Five) are sometimes understood as explanations or sources of the covariation of distinct behavioral traits, as when extraversion is suggested to underlie the covariation of assertiveness and sociability. Here, we detail how trait covariation can alternatively be understood as arising from units common to functionalist and process frameworks, such as self-efficacies, expectancies, values, and goals. Specifically, the expected covariation between two behavioral traits should be increased when a specific process variable tends to indicate the functionality of both traits simultaneously. In 2 empirical illustrations, we identify a wide array of specific process variables associated with several Big Five-related behavioral traits simultaneously, and which are thus likely sources of their covariation. Many of these, such as positive interpersonal expectancies, self-regulatory skills, and preference for order, relate similarly to a broad range of trait perceptions in both studies, and across both self- and peer-reports. We also illustrate how this understanding of trait covariation provides a somewhat novel explanation of why some traits are uncorrelated. As we discuss, a functionalist understanding of trait covariation as arising through functionalist or process variables has implications for many basic issues in personality psychology, such as how personality traits should be measured, mechanisms for personality stability and change, and the nature of personality traits more generally. Includes supplementary materials

Carbohydrate Catabolism in Phaeobacter inhibens DSM 17395, a Member of the Marine Roseobacter Clade

Since genome analysis did not allow unambiguous reconstruction of transport, catabolism, and substrate-specific regulation for several important carbohydrates in Phaeobacter inhibens DSM 17395, proteomic and metabolomic analyses of N-acetylglucosamine-, mannitol-, sucrose-, glucose-, and xylose-grown cells were carried out to close this knowledge gap. These carbohydrates can pass through the outer membrane via porins identified in the outer membrane fraction. For transport across the cytoplasmic membrane, carbohydrate-specific ABC transport systems were identified. Their coding genes mostly colocalize with the respective "catabolic" and "regulatory" genes. The degradation of N-acetylglucosamine proceeds via N-acetylglucosamine-6-phosphate and glucosamine-6-phosphate directly to fructose-6-phosphate; two of the three enzymes involved were newly predicted and identified. Mannitol is catabolized via fructose, sucrose via fructose and glucose, glucose via glucose-6-phosphate, and xylose via xylulose-5-phosphate. Of the 30 proteins predicted to be involved in uptake, regulation, and degradation, 28 were identified by proteomics and 19 were assigned to their respective functions for the first time. The peripheral degradation pathways feed into the Entner-Doudoroff (ED) pathway, which is connected to the lower branch of the Embden-Meyerhof-Parnas (EMP) pathway. The enzyme constituents of these pathways displayed higher abundances in P. inhibens DSM 17395 cells grown with any of the five carbohydrates tested than in succinate-grown cells. Conversely, gluconeogenesis is turned on during succinate utilization. While tricarboxylic acid (TCA) cycle proteins remained mainly unchanged, the abundance profiles of their metabolites reflected the differing growth rates achieved with the different substrates tested. Homologs of the 74 genes involved in the reconstructed catabolic pathways and central metabolism are present in various Roseobacter clade members

On the stellar populations in NGC 185 and NGC 205, and the nuclear star cluster in NGC 205 from Hubble Space Telescope observations

[Abridged] We present a first detailed analysis of resolved stellar populations in the dwarf galaxies NGC 185 and NGC 205 based on archival V- and I-band WFPC2 pointings. For NGC 185 we deduce that star formation was probably still active about 4 x 10^8 yr ago. Key abundance-related results are: (1) We identify ancient stars with [Fe/H] <~ -1.5 dex by a well-defined horizontal branch (HB). (2) We find a prominent RGB/ faint-AGB clump/ bump- like feature with the same mean V-band magnitude as the HB, within uncertainties; from a comparison with theory, ancient stars have [Fe/H] ~ -1.5 dex, with a higher abundance level for intermediate-age stars. (3) From colour information we infer that the median [Fe/H] > -1.11 +/- 0.08 dex for ancient stars. For NGC 205, we record (m-M)o = 24.76 +/- 0.1 mag, based on the RGB I-band tip magnitude method. We find that stars were probably still forming less than 3 x 10^8 yr ago, which is compatible with star formation triggered by an interaction with M31. Key abundance-related results are: (1) The RGB/ faint-AGB is significantly skewed to redder values than that of a control field in the outskirts of M31; it probably results from a relatively narrow metallicity and or age range for a significant fraction of the dwarf's stars. (2) For ancient stars we infer from colour information that the median [Fe/H] > -1.06+/-0.04 dex. We briefly compare the stellar populations of NGC 205, NGC 185 and NGC 147. Finally, we find an apparent blue excess in the outer region of the nuclear star cluster in NGC 205. It is as compact as a typical galactic globular cluster, but is quite bright (10^6 L_solar,R); and by matching its blue colour with models, its stellar population is young, up to a few times 10^8 yr old.Comment: To appear in the May edition of the Astronomical Journal. Some figures have been degraded in quality for the purpose of submissio

Ages and Metallicities of Cluster Galaxies in a779 Using Modified Strömgren Photometry

In the quest for the formation and evolution of galaxy clusters, Rakos and co-workers introduced a spectrophotometric method using modified Strömgren photometry, but with the considerable debate toward the project's abilities, we re-introduce the system by testing for the repeatability of the modified Strömgren colors and compare them with the Strömgren colors, and check for the reproducibility of the ages and metallicities (using the Principle Component Analysis (PCA) technique and the GALEV models) for the six common galaxies in all three A779 data sets. As a result, a fair agreement between two filter systems was found to produce similar colors (with a precision of 0.09 mag in (uz - vz), 0.02 mag in (bz - yz), and 0.03 mag in (vz - vz)) and the generated ages and metallicities are also similar (with an uncertainty of 0.36 Gyr and 0.04 dex from PCA and 0.44 Gyr and 0.2 dex using the GALEV models). We infer that the technique is able to relieve the age-metallicity degeneracy by separating the age effects from the metallicity effects, but it is still unable to completely eliminate it.We further extend this paper to re-study the evolution of galaxies in the low mass, dynamically poor A779 cluster (as it was not elaborately analyzed by Rakos and co-workers in their previous work) by correlating the luminosity (mass), density, and radial distance with the estimated age, metallicity, and the star formation history. Our results distinctly show the bimodality of the young, low-mass, metal-poor population with a mean age of 6.7 Gyr (± 0.5 Gyr) and the old, high-mass, metal-rich galaxies with a mean age of 9 Gyr (± 0.5 Gyr). The method also observes the color evolution of the blue cluster galaxies to red (Butcher-Oemler phenomenon), and the downsizing phenomenon. Our analysis shows that modified Strömgren photometry is very well suited for studying low- and intermediate-z clusters, as it is capable of observing deeper with better spatial resolution at spectroscopic redshift limits, and the narrow-band filters estimate the age and metallicity with fewer uncertainties compared to other methods that study stellar population scenarios