A Dust-Penetrated Classification Scheme for Bars as Inferred from their Gravitational Force Fields

The division of galaxies into ``barred'' (SB) and ``normal'' (S) spirals is a fundamental aspect of the Hubble galaxy classification system. This ``tuning fork'' view was revised by de Vaucouleurs, whose classification volume recognized apparent ``bar strength'' (SA, SAB, SB) as a continuous property of galaxies called the ``family''. However, the SA, SAB, and SB families are purely visual judgments that can have little bearing on the actual bar strength in a given galaxy. Until very recently, published bar judgments were based exclusively on blue light images, where internal extinction or star formation can either mask a bar completely or give the false impression of a bar in a nonbarred galaxy. Near-infrared camera arrays, which principally trace the old stellar populations in both normal and barred galaxies, now facilitate a quantification of bar strength in terms of their gravitational potentials and force fields. In this paper, we show that the maximum value, Qb, of the ratio of the tangential force to the mean radial force is a quantitative measure of the strength of a bar. Qb does not measure bar ellipticity or bar shape, but rather depends on the actual forcing due to the bar embedded in its disk. We show that a wide range of true bar strengths characterizes the category ``SB'', while de Vaucouleurs category ``SAB'' corresponds to a much narrower range of bar strengths. We present Qb values for 36 galaxies, and we incorporate our bar classes into a dust-penetrated classification system for spiral galaxies.Comment: Accepted for publication in the Astrophysical Journal (LaTex, 30 pages + 3 figures); Figs. 1 and 3 are in color and are also available at http://bama.ua.edu/~rbuta/bars

Pollen morphology in the tribe Sipaneeae (Rubiaceae, Ixoroideae)

The tribe Sipaneeae has its center of diversity on the Guiana Shield (northern South America), where 9 of the 10 genera occur, and a total of 44 species. It includes the genera Chalepophyllum (3 spp.), Dendrosipanea (3 spp.), Limnosipanea (3 spp.), Maguireothamnus (3 spp.), Neblinathamnus (2 spp.), Neobertiera (5 spp.), Pteridocalyx (1 sp.), Sipanea (17 spp.), Sipaneopsis (8 spp.), and Steyermarkia (1 sp.). The pollen morphology of all the genera of the tribe was studied. For pollen preparation, nearly mature flower buds (just before anthesis) were taken from herbarium material. Pollen grains destined for light microscope (LM) studies were mounted in Kaiser’s glycerine jelly. Pollen grains for scanning electron microscope (SEM) studies were suspended in ethanol and mounted on aluminium stubs using carbon adhesive tape and coated with a platinum palladium. Values of the length of polar and equatorial axes were based on LM-measurements. In all the genera, pollen grains are released in monads, and are 3- or 4-colporate. In most genera the number of colpi are consistently 3 or 4, which represents a significant diagnostic character. The largest pollen grains are found in Maguireothamnus, which is also the genus with the largest corollas in the tribe. The second largest grains in the tribe are found in Chalepophyllum, which is the genus with the second largest corollas in the tribe. The smallest pollen grains are found in Neobertiera, Pteridocalyx, and Sipanea, which are the genera with the smallest corollas in the tribe. The exine is externally foveolate-reticulate in Chalepophyllum, Neblinathamnus, Pteridocalyx, and Sipanea, foveolate or foveolate-reticulate in Dendrosipanea, shallowly foveolate, without perforations or finely perforated in Limnosipanea, smooth or finely foveolate in Maguireothamnus, and foveolate in Neobertiera, Sipaneopsis, and Steyermarkia. Possible pollen dimorphism was observed only in populations of S. pratensis var. pratensis, in which pollen grains dimensions and external ornamentation were found to be similar

Mid-Infrared Galaxy Morphology Along the Hubble Sequence

The mid-infrared emission from 18 nearby galaxies imaged with the IRAC instrument on Spitzer Space Telescope samples the spatial distributions of the reddening-free stellar photospheric emission and the warm dust in the ISM. These two components provide a new framework for galaxy morphological classification, in which the presence of spiral arms and their emission strength relative to the starlight can be measured directly and with high contrast. Four mid-infrared classification methods are explored, three of which are based on quantitative global parameters (colors, bulge-to-disk ratio) similar to those used in the past for optical studies; in this limited sample, all correlate well with traditional B-band classification. We suggest reasons why infrared classification may be superior to optical classification.Comment: ApJS (in press), Spitzer Space Telescope Special Issue; 13 pages, LaTeX (or Latex, etc); Figure 1ab is large, color plate; full-resolution plates in .pdf format available at http://cfa-www.harvard.edu/irac/publications

Radial HI Profiles at the Periphery of Galactic Disks: The Role of Ionizing Background Radiation

Observations of neutral hydrogen in spiral galaxies reveal a sharp cutoff in the radial density profile at some distance from the center. Using 22 galaxies with known HI distributions as an example, we discuss the question of whether this effect can be associated exclusively with external ionizing radiation, as is commonly assumed. We show that before the surface density reaches $\sigma_{\textrm{HI}}\le 0.5 {\cal M}_\odot/{\textrm {pc}}^2$(the same for galaxies of different types), it is hard to expect the gas to be fully ionized by background radiation. For two of 13 galaxies with a sharp drop in the HI profile, the "steepening" can actually be caused by ionization. At the same time, for the remaining galaxies, the observed cutoff in the radial HI profile is closer to the center than if it was a consequence of ionization by background radiation and, therefore, it should be caused by other factors.Comment: 15 pages, 6 figure

Analytic models and forward scattering from accelerator to cosmic-ray energies

Analytic models for hadron-hadron scattering are characterized by analytical parametrizations for the forward amplitudes and the use of dispersion relation techniques to study the total cross section $\sigma_{tot}$ and the $\rho$ parameter. In this paper we investigate four aspects related to the application of the model to $pp$ and $\bar{p}p$ scattering, from accelerator to cosmic-ray energies: 1) the effect of different estimations for $\sigma_{tot}$ from cosmic-ray experiments; 2) the differences between individual and global (simultaneous) fits to $\sigma_{tot}$ and $\rho$; 3) the role of the subtraction constant in the dispersion relations; 4) the effect of distinct asymptotic inputs from different analytic models. This is done by using as a framework the single Pomeron and the maximal Odderon parametrizations for the total cross section. Our main conclusions are the following: 1) Despite the small influence from different cosmic-ray estimations, the results allow us to extract an upper bound for the soft pomeron intercept: $1 + \epsilon = 1.094$; 2) although global fits present good statistical results, in general, this procedure constrains the rise of $\sigma_{tot}$; 3) the subtraction constant as a free parameter affects the fit results at both low and high energies; 4) independently of the cosmic-ray information used and the subtraction constant, global fits with the odderon parametrization predict that, above $\sqrt s \approx 70$ GeV, $\rho_{pp}(s)$ becomes greater than $\rho_{\bar{p}p}(s)$, and this result is in complete agreement with all the data presently available. In particular, we infer $\rho_{pp} = 0.134 \pm 0.005$ at $\sqrt s = 200$ GeV and $0.151 \pm 0.007$ at 500 GeV (BNL RHIC energies).Comment: 16 pages, 7 figures, aps-revtex, wording changes, corrected typos, to appear in Physical Review

Semi-Analytical Models for Lensing by Dark Halos: I. Splitting Angles

We use the semi-analytical approach to analyze gravitational lensing of quasars by dark halos in various cold dark matter (CDM) cosmologies, in order to determine the sensitivity of the prediction probabilities of images separations to the input assumptions regarding halos and cosmologies. The mass function of dark halos is assumed to be given by the Press-Schechter function. The mass density profile of dark halos is alternatively taken to be the singular isothermal sphere (SIS), the Navarro-Frenk-White (NFW) profile, or the generalized NFW profile. The cosmologies include: the Einstein-de Sitter model (SCDM), the open model (OCDM), and the flat \Lambda-model (LCDM). As expected, we find that the lensing probability is extremely sensitive to the mass density profile of dark halos, and somewhat less so to the mean mass density in the universe, and the amplitude of primordial fluctuations. NFW halos are very much less effective in producing multiple images than SIS halos. However, none of these models can completely explain the current observations: the SIS models predict too many large splitting lenses, while the NFW models predict too few small splitting lenses. This indicates that there must be at least two populations of halos in the universe. A combination of SIS and NFW halos can reasonably reproduce the current observations if we choose the mass for the transition from SIS to NFW to be ~ 10^{13} solar masses. Additionally, there is a tendency for CDM models to have too much power on small scales, i.e. too much mass concentration; and it appears that the cures proposed for other apparent difficulties of CDM would help here as well, an example being the warm dark matter (WDM) variant which is shown to produce large splitting lenses fewer than the corresponding CDM model by one order of magnitude.Comment: 46 pages, including 13 figures. Revised version with significant improvemen

The time-dependent localization of Ki 67 antigen-positive cells in human skin wounds

A total of 77 human skin wounds with a post-infliction interval between 3 h and 7 months were investigated and the proliferation marker antigen Ki 67 was visualized in paraffin sections using a specific monoclonal antibody (MIB). The re-built epidermal layer covering the former lesional area showed only a few basal cells positively staining for Ki 67 antigen. No enhanced reactivity was found when compared to uninjured skin. In basal cells of the epidermis adjacent to the wound area, however, varying numbers of positive cells occurred, but no information useful for a reliable time estimation of skin wounds could be obtained due to the considerable variability in the number of Ki 67 positive epidermal basal cells found in non-damaged skin. Fibroblastic cells in the wound area revealed an increased number of Ki 67-positive sites which could first be detected in a 1.5-day-old skin lesion. Positive results could be obtained in every specimen investigated after a post-infliction interval of 6 days up to 1.5 months. Only the scar tissue of the oldest wound examined (wound age 7 months) revealed no increase in the number of positively staining fibroblasts. Therefore, positive results indicate a wound age of at least approximately 1.5 days and the lack of an increased number of positive fibroblastic cells in a sufficient number of specimens indicates at a wound age of less than 6 days, but cannot totally exclude longer post-infliction intervals

Expanding the scope of leaf symbiosis: Caballeronia endophytes in Empogona and Tricalysia (Coffeeae, Rubiaceae)

Leaf symbiosis is a remarkable phenomenon observed in Rubiaceae host plants, where they interact with bacterial endophytes residing within their leaves. Although approximately 650 species from 8 genera across 4 tribes exhibit this symbiosis, its fiill extent within Rubiaceae remains unknown. Our primary objective is to investígate the potential presence of leaf endophytes in the African plant genera Empogona and Tricalysia and, if confirmed, determine their identity. To accomplish this, we extracted total DNA from the leaves of four Coffeeae tribe species {Empogona congesta, Tricalysia hensii, T. lasiodelphys, and T. semidecidua) and sequenced it. Subsequently, we filtered out bacterial reads. Through phylogenetic analysis o f the endophytes, we were able to ascertain their identity and establish their relationship with known symbiotic organisms. Notably, all four species harboured non-nodulated leaf endophytes, specifically identified as Caballeronia. Although these endophytes are distinct from one another, they are related to other nodulated and non-nodulated endophytes. Interestingly, we did not observe any discemible phylogenetic or geographic pattems among the endophytes or their host plants. Our findings demónstrate the presence of Caballeronia endophytes in the leaves o f Empogona and Tricalysia, two genera previously not associated with leaf symbiosis. This interaction is likely to have a broader distribution, and further discoveries are inevitable in the future

NGC 1300 Dynamics: I. The gravitational potential as a tool for detailed stellar dynamics

In a series of papers we study the stellar dynamics of the grand design barred-spiral galaxy NGC~1300. In the first paper of this series we estimate the gravitational potential and we give it in a form suitable to be used in dynamical studies. The estimation is done directly from near-infrared observations. Since the 3D distribution of the luminous matter is unknown, we construct three different general models for the potential corresponding to three different assumptions for the geometry of the system, representing limiting cases. A pure 2D disc, a cylindrical geometry (thick disc) and a third case, where a spherical geometry is assumed to apply for the major part of the bar. For the potential of the disc component on the galactic plane a Fourier decomposition method is used, that allows us to express it as a sum of trigonometric terms. Both even and odd components are considered, so that the estimated potential accounts also for the observed asymmetries in the morphology. For the amplitudes of the trigonometric terms a smoothed cubic interpolation scheme is used. The total potential in each model may include two additional terms (Plummer spheres) representing a central mass concentration and a dark halo component, respectively. In all examined models, the relative force perturbation points to a strongly nonlinear gravitational field, which ranges from 0.45 to 0.8 of the axisymmetric background with the pure 2D being the most nonlinear one. We present the topological distributions of the stable and unstable Lagrangian points as a function of the pattern speed $(\Omega_p)$. In all three models there is a range of $\Omega_p$ values, where we find multiple stationary points whose stability affects the overall dynamics of the system.Comment: 14 pages, 11 figures, published in MNRA

Sapucaia nut (Lecythis pisonis Cambess) and its by-products: a promising and underutilized source of bioactive compounds. Part II: phenolic compounds profile.

In this study, the profile of the bioactive compounds of sapucaia nut (Lecythis pisonis Cambess) and its byproducts have been investigated. The phenolic profile by LC-ESI-MS/MS, the total phenolic content, the condensed tannins and the antioxidant activity of the sapucaia nut and shell were determined. 14 phenolic compounds were identified in the sapucaia nut extract, primarily phenolic acids and flavonoids. Catechin, epicatechin, myricetin, ellagic acid and ferulic acid presented significant correlation to the antioxidant activity. The sapucaia shell contained 22 phenolic compounds, 13 of which were quantified. The sapucaia shell extract showed a high content of total phenolic compounds, a high condensed tannins content, and high antioxidant activity. The higher antioxidant activity of the shell can be associated with a higher content of phenolics. Overall, it can be concluded that the sapucaia nut is a raw material rich in phenolic compounds that present high antioxidant activity. The nuts and the cake may be used as a promising raw material for the food industry, while the shells could be an alternative source of natural antioxidants. Further use in the cosmetics and pharmaceutical industry may also be envisaged. 1. Introduction Lecythis pisonis