Structural and Contextual Frameworks: Distinguishing Literal from Metaphorical Depictions of Exaggerated Size

In 2016, the authors proposed the Contextual Framework and Structural Framework for understanding pictorial metaphors. These two dichotomous frameworks are especially useful for assessing the apprehension by viewers of pictorial devices that can be used either literally or metaphorically. One such pictorial device is exaggerated size—that is, depicting objects as being overly large. This pictorial device can be used metaphorically (e.g., to indicate importance) or literally (e.g., to depict a giant). We analyze three comic book covers from the Silver Age of American comic books using both frameworks to illustrate how observers distinguish metaphoric pictorial devices from literal ones

Spontaneous Isotropy Breaking: A Mechanism for CMB Multipole Alignments

We introduce a class of models in which statistical isotropy is broken spontaneously in the CMB by a non-linear response to long-wavelength fluctuations in a mediating field. These fluctuations appear as a gradient locally and pick out a single preferred direction. The non-linear response imprints this direction in a range of multipole moments. We consider two manifestations of isotropy breaking: additive contributions and multiplicative modulation of the intrinsic anisotropy. Since WMAP exhibits an alignment of power deficits, an additive contribution is less likely to produce the observed alignments than the usual isotropic fluctuations, a fact which we illustrate with an explicit cosmological model of long-wavelength quintessence fluctuations. This problem applies to other models involving foregrounds or background anisotropy that seek to restore power to the CMB. Additive models that account directly for the observed power exacerbate the low power of the intrinsic fluctuations. Multiplicative models can overcome these difficulties. We construct a proof of principle model that significantly improves the likelihood and generates stronger alignments than WMAP in 30-45% of realizations.Comment: 13 pages, 10 figure

Preparation of 9-substituted pyridine-stretched adenines and hypoxanthines

9-Methylsulfanyl pyridine-stretched adenine and hypoxanthine derivatives have been prepared via regioselective reaction of a 5-aminoimidazole with 2-(bis-methylsulfanylmethylene)malononitrile [(NC)C=C(SMe) ]. The 9-methylsulfanyl substituent can be replaced by sequential oxidation and substitution by nucleophiles including amines

Gaps and weaknesses in the global protected area network for safeguarding at-risk species

Protected areas are essential to biodiversity conservation. Creating new parks can protect larger populations and more species, yet strengthening existing parks, particularly those vulnerable to harmful human activities, is a critical but underappreciated step for safeguarding at-risk species. Here, we model the area of habitat that terrestrial mammals, amphibians, and birds have within park networks and their vulnerability to current downgrading, downsizing, or degazettement events and future land-use change. We find that roughly 70% of species analyzed have scant representation in parks, or occur within parks that are affected by shifts in formal legal protections or are vulnerable to increased human pressures. Our results also show that expanding and strengthening park networks across just 1% of the world’s land area could preserve irreplaceable habitats of 1191 species that are particularly vulnerable to extinction

Quality Assessment of Mycobacterium tuberculosis Genotyping in a Large Laboratory Network

Quality assessment exercises were conducted to evaluate the reproducibility of IS6110 DNA fingerprinting performed by eight laboratories in the National Tuberculosis Genotyping and Surveillance Network. Three panels, each with 8 to 16 isolates, were typed at all laboratories, resulting in 280 images. When the pattern obtained by the majority for each isolate was used as the standard, exact matches were obtained for 73% of patterns; 90% and 97% of patterns matched within one- and two-band differences, respectively. A second approach involved retyping of randomly selected isolates at the Centers for Disease Control and Prevention. Retyping was done for 8–19 isolates per laboratory (76 total). Paired images matched exactly for 54% of isolates and within one and two band differences, 78% and 93%, respectively. We evaluated reasons for mismatching. We also evaluated the reproducibility of spoligotyping using a test panel of 13 isolates; a discrepancy of 1 in 91 results was noted

The Extended Blue Continuum and Line Emission around the Central Radio Galaxy in Abell 2597

We present results from detailed imaging of the centrally dominant radio elliptical galaxy in the cooling flow cluster Abell 2597, using data obtained with the Wide Field and Planetary Camera 2 (WFPC2) on the Hubble Space Telescope (HST). This object is one of the archetypal "blue-lobed" cooling flow radio elliptical galaxies, also displaying a luminous emission-line nebula, a compact radio source, and a significant dust lane and evidence of molecular gas in its center. We show that the radio source is surrounded by a complex network of emission-line filaments, some of which display a close spatial association with the outer boundary of the radio lobes. We present a detailed analysis of the physical properties of ionized and neutral gas associated with the radio lobes, and show that their properties are strongly suggestive of direct interactions between the radio plasma and ambient gas. We resolve the blue continuum emission into a series of knots and clumps, and present evidence that these are most likely due to regions of recent star formation. We investigate several possible triggering mechanisms for the star formation, including direct interactions with the radio source, filaments condensing from the cooling flow, or the result of an interaction with a gas-rich galaxy, which may also have been responsible for fueling the active nucleus. We propose that the properties of the source are plausibly explained in terms of accretion of gas by the cD during an interaction with a gas-rich galaxy, which combined with the fact that this object is located at the center of a dense, high-pressure ICM can account for the high rates of star formation and the strong confinement of the radio source.Comment: Astrophysical Journal, in press, 34 pages, includes 6 PostScript figures. Latex format, uses aaspp4.sty and epsf.sty file

Checklists and illustrative financial statements for state and local governmental units : a financial reporting practice aid, June 2007 edition

https://egrove.olemiss.edu/aicpa_indev/1941/thumbnail.jp

Quality Assurance Project Plan (QAPP) for Wetland Program Development Grant No. CD-00E00963-0

In order to evaluate overall ecological health and function of seasonal and semi-permanent wetlands in Illinois, we will sample 240 wetlands distributed across 60 state managed lands over three field seasons (2012-2014; see attached map for preliminary site locations). During each field season, we will conduct sampling on 20 state managed properties and 4 wetlands will be sampled at each site (n = 80 wetlands per season). At each wetland surveys will be conducted during four time periods over a five month span (February-June) to increase the probability of species detection. Additionally, due to fluctuations in population sizes, variability in breeding phenologies, and suspected detection rates between taxonomic groups (i.e. rare species have lower detection rates than common species), wetlands will be sampled for three nights per period (n =12 total samples in a season). By repeatedly sampling wetlands during the field season, we can estimate occupancy and detection rates using program PRESENCE 3.1. Each state managed property (and associated wetlands) will be sampled during only one field season to increase the number of overall sites sampled during the study and all wetlands will be located on Illinois Department of Natural Resources (IDNR) managed properties to ensure accessibility. Wetland health and function will be assessed by examining three critical components of wetlands ecosystems: 1) Amphibian diversity and abundance; 2) Reptile diversity and abundance; and 3) Macroinvertebrate diversity and abundance. Each of these primary components will Date: 04 January 2012 Revision 0 9 be incorporated into an index of biological integrity (IBI) to determine how well the wetland is functioning within the ecosystem.U.S. Environmental Protection Agency Wetland Program Development Grant No. CD-00E00963-0unpublishednot peer reviewedOpe

Star Formation, Radio Sources, Cooling X-ray Gas, and Galaxy Interactions in the Brightest Cluster Galaxy in 2A0335+096

We present deep emission-line imaging taken with the SOAR Optical Imaging Camera of the brightest cluster galaxy (BCG) in the nearby (z=0.035) X-ray cluster 2A0335+096. We analyze long-slit optical spectroscopy, archival VLA, Chandra X-ray, and XMM UV data. 2A0335+096 is a bright, cool-core X-ray cluster, once known as a cooling flow. Within the highly disturbed core revealed by Chandra X-ray observations, 2A0335+096 hosts a highly structured optical emission-line system. The redshift of the companion is within 100 km/s of the BCG and has certainly interacted with the BCG, and is likely bound to it. The comparison of optical and radio images shows curved filaments in H-alpha emission surrounding the resolved radio source. The velocity structure of the emission-line bar between the BCG nucleus and the companion galaxy provides strong evidence for an interaction between the two in the last ~50 Myrs. The age of the radio source is similar to the interaction time, so this interaction may have provoked an episode of radio activity. We estimate a star formation rate of >7 solar mass/yr based on the Halpha and archival UV data, a rate similar to, but somewhat lower than, the revised X-ray cooling rate of 10-30 solar masses/year estimated from XMM spectra by Peterson & workers. The Halpha nebula is limited to a region of high X-ray surface brightness and cool X-ray temperature. The detailed structures of H-alpha and X-ray gas differ. The peak of the X-ray emission is not the peak of H-alpha emission, nor does it lie in the BCG. The estimated age of the radio lobes and their interaction with the optical emission-line gas, the estimated timescale for depletion and accumulation of cold gas, and the dynamical time in the system are all similar, suggesting a common trigger mechanism.Comment: Accepted AJ, July 2007 publication. Vol 134, p. 14-2