Cerebrovascular reactivity is the change in cerebral blood flow in response to a vasodilatory or vasoconstrictive stimulus. Measuring variations of cerebrovascular reactivity between different ...regions of the brain has the potential to not only advance understanding of how the cerebral vasculature controls the distribution of blood flow but also to detect cerebrovascular pathophysiology. While there are standardized and repeatable methods for estimating the changes in cerebral blood flow in response to a vasoactive stimulus, the same cannot be said for the stimulus itself. Indeed, the wide variety of vasoactive challenges currently employed in these studies impedes comparisons between them. This review therefore critically examines the vasoactive stimuli in current use for their ability to provide a standard repeatable challenge and for the practicality of their implementation. Such challenges include induced reductions in systemic blood pressure, and the administration of vasoactive substances such as acetazolamide and carbon dioxide. We conclude that many of the stimuli in current use do not provide a standard stimulus comparable between individuals and in the same individual over time. We suggest that carbon dioxide is the most suitable vasoactive stimulus. We describe recently developed computer‐controlled MRI compatible gas delivery systems which are capable of administering reliable and repeatable vasoactive CO2 stimuli.
ABSTRACT The dust attenuation for a sample of ∼10,000 local (z 0.1) star-forming galaxies is constrained as a function of their physical properties. We utilize aperture-matched multiwavelength data ...available from the Galaxy Evolution Explorer and the Sloan Digital Sky Survey to ensure that regions of comparable size in each galaxy are being analyzed. We follow the method of Calzetti et al. and characterize the dust attenuation through the UV power-law index, β, and the dust optical depth, which is quantified using the difference in Balmer emission line optical depth, . The observed linear relationship between β and is similar to the local starburst relation, but the large scatter ( int = 0.44) suggests that there is significant variation in the local universe. We derive a selective attenuation curve over the range 1250 Å < λ < 8320 Å and find that a single attenuation curve is effective for characterizing the majority of galaxies in our sample. This curve has a slightly lower selective attenuation in the UV compared to previously determined curves. We do not see evidence to suggest that a 2175 Å feature is significant in the average attenuation curve. Significant positive correlations are seen between the amount of UV and optical reddening and galaxy metallicity, mass, star formation rate (SFR), and SFR surface density. This provides a potential tool for gauging attenuation where the stellar population is unresolved, such as at high z.
We update the spectral modeling code MAGPHYS to include a 2175 absorption feature in its UV to near-IR dust attenuation prescription. This allows us to determine the strength of this feature and the ...shape of the dust attenuation curve in ∼5000 star-forming galaxies at in the COSMOS field. We find that a 2175 absorption feature of ∼1/3 the strength of that in the Milky Way is required for models to minimize residuals. We characterize the total effective dust attenuation curves as a function of several galaxy properties and find that the UV slopes of the attenuation curve for COSMOS galaxies show a strong dependence on star formation rate (SFR) and total dust attenuation (AV), such that galaxies with higher SFR and AV have shallower curves and vice versa. These results are consistent with expectations from radiative transfer that attenuation curves become shallower as the effective dust optical depth increases. We do not find significant trends in the strength of the 2175 absorption feature as a function of galaxy properties, but this may result from the high uncertainties associated with this measurement. The updated code is publicly available online (following acceptance).
We present an enhanced version of the multiwavelength spectral modeling code MAGPHYS that allows the estimation of galaxy photometric redshift and physical properties (e.g., stellar mass, star ...formation rate, dust attenuation) simultaneously, together with robust characterization of their uncertainties. The self-consistent modeling over ultraviolet to radio wavelengths in MAGPHYS+photo-z is unique compared to standard photometric redshift codes. The broader wavelength consideration is particularly useful for breaking certain degeneracies in color versus redshift for dusty galaxies with limited observer-frame ultraviolet and optical data (or upper limits). We demonstrate the success of the code in estimating redshifts and physical properties for over 4000 infrared-detected galaxies at 0.4 < z < 6.0 in the COSMOS field with robust spectroscopic redshifts. We achieve high photo-z precision ( ), high accuracy (i.e., minimal offset biases; median(Δz/(1 + zspec)) 0.02), and low catastrophic failure rates ( 4%) over all redshifts. Interestingly, we find that a weak 2175 absorption feature in the attenuation curve models is required to remove a subtle systematic zphot offset ( ) that occurs when this feature is not included. As expected, the accuracy of derived physical properties in MAGPHYS+photo-z decreases strongly as redshift uncertainty increases. The all-in-one treatment of uncertainties afforded with this code is beneficial for accurately interpreting physical properties of galaxies in large photometric data sets. Finally, we emphasize that MAGPHYS+photo-z is not intended to replace existing photo-z codes, but rather offers flexibility to robustly interpret physical properties when spectroscopic redshifts are unavailable. The MAGPHYS+photo-z code is publicly available online.
We characterize the influence that inclination has on the shape and normalization in average dust attenuation curves derived from a sample of ∼10,000 local star-forming galaxies. To do this, we ...utilize aperture-matched multiwavelength data from the Galaxy Evolution Explorer, the Sloan Digital Sky Survey, the United Kingdom Infrared Telescope, and the Two Micron All-sky Survey. We separate our sample into groups according to axial ratio (b/a) and obtain an estimate of their average total-to-selective attenuation . The attenuation curves are found to be shallower at UV wavelengths with increasing inclination, whereas the shape at longer wavelengths remains unchanged. The highest inclination subpopulation ( ) exhibits an NUV excess in its average selective attenuation, which, if interpreted as a 2175 feature, is best fit with a bump strength of 17%-26% of the MW value. No excess is apparent in the average attenuation curve of lower inclination galaxies. The differential reddening between the stellar continuum and ionized gas is found to decrease with increasing inclination. We find that higher inclination galaxies have slightly higher values of RV, although this is poorly constrained given the uncertainties. We outline possible explanations for these trends within a two component dust model (dense cloud+diffuse dust) and find that they can be naturally explained if carriers of the 2175 feature are preferentially destroyed in star-forming regions (UV-bright regions).
Abstract
We present a spatially resolved H
ii
region study of the gas-phase metallicity, ionization parameter, and interstellar medium (ISM) pressure maps of six local star-forming and face-on spiral ...galaxies from the TYPHOON program. Self-consistent metallicity, ionization parameter, and pressure maps are calculated simultaneously through an iterative process to provide useful measures of the local chemical abundance and its relation to localized ISM properties. We constrain the presence of azimuthal variations in metallicity by measuring the residual metallicity offset Δ(O/H) after subtracting the linear fits to the radial metallicity profiles. We, however, find weak evidence of azimuthal variations in most of the galaxies, with small (mean 0.03 dex) scatter. The galaxies instead reveal that H
ii
regions with enhanced and reduced abundances are found distributed throughout the disk. While the spiral pattern plays a role in organizing the ISM, it alone does not establish the relatively uniform azimuthal variations we observe. Differences in the metal abundances are more likely driven by the strong correlations with the local physical conditions. We find a strong and positive correlation between the ionization parameter and the local abundances as measured by the relative metallicity offset Δ(O/H), indicating a tight relationship between local physical conditions and their localized enrichment of the ISM. Additionally, we demonstrate the impact of unresolved observations on the measured ISM properties by rebinning the data cubes to simulate low-resolution (1 kpc) observations, typical of large IFU surveys. We find that the ionization parameter and ISM pressure diagnostics are impacted by the loss of resolution such that their measured values are larger relative to the measured values on sub-H
ii
region scales.
ABSTRACT
We present reduced images and catalogues of photometric and emission-line data (∼230 000 and ∼8000 sources, respectively) for the WFC3 (Wide Field Camera 3) Infrared Spectroscopic Parallel ...(WISP) survey. These data are made publicly available on the Mikulski Archive for Space Telescopes and include reduced images from various facilities: ground-based ugri, Hubble Space Telescope (HST) WFC3, and Spitzer IRAC (Infrared Array Camera). Coverage in at least one additional filter beyond the WFC3/IR data are available for roughly half of the fields (227 out of 483), with ∼20 per cent (86) having coverage in six or more filters from u band to IRAC 3.6 $\mu$m (0.35–3.6 $\mu$m). For the lower spatial resolution (and shallower) ground-based and IRAC data, we perform PSF (point spread function)-matched, prior-based, deconfusion photometry (i.e. forced-photometry) using the tphot software to optimally extract measurements or upper limits. We present the methodology and software used for the WISP emission-line detection and visual inspection. The former adopts a continuous wavelet transformation that significantly reduces the number of spurious sources as candidates before the visual inspection stage. We combine both WISP catalogues and perform spectral energy distribution fitting on galaxies with reliable spectroscopic redshifts and multiband photometry to measure their stellar masses. We stack WISP spectra as functions of stellar mass and redshift and measure average emission-line fluxes and ratios. We find that WISP emission-line sources are typically ‘normal’ star-forming galaxies based on the mass–excitation diagram (O iii/Hβ versus M⋆; 0.74 < zgrism < 2.31), the galaxy main sequence (SFR versus M⋆; 0.30 < zgrism < 1.45), S32 ratio versus M⋆ (0.30 < zgrism < 0.73), and O32 and R23 ratios versus M⋆ (1.27 < zgrism < 1.45).
Cerebrovascular reactivity (CVR) is the change in cerebral blood flow (CBF) in response to a change in a vasoactive stimulus. Paradoxical reductions in CBF in response to vasodilatory stimulation ...(‘steal’) are associated with vascular pathology. However, a pathophysiological interpretation of ‘steal’ requires a comprehensive conceptual model linking pathology and changes in blood flow. Herein, we extend a simple model explaining steal published in the late 1960s by incorporating concepts of CBF regulation from more recent studies to generate a comprehensive dynamic model. The main elements of the model are: (a) the relationship between changes in CBF and the arterial partial pressure of carbon dioxide (PaCO2) in healthy vascular regions is sigmoidal; (b) vascular regions vasodilate to compensate for decreased perfusion pressure, leading to (c) an encroachment on vasodilatory reserve and, reduced CVR; (d) a vasodilatory stimulus may increase CBF capacity above the flow capacity of major cerebral blood vessels; and (e) this limitation induces competitive intra-cerebral redistribution of flow from territories with low vasodilatory reserve to those with high reserve. We used CVR measurements generated by applying precise, computer-controlled changes in PaCO2 as the vasoactive stimulus, and measured blood oxygen level dependent (BOLD) MRI signals as high resolution surrogates of CBF to test predictions derived from this model. Subjects were 16 healthy adults and 16 patients with known cerebral steno-occlusive diseases. We observed regional sigmoidal PaCO2–BOLD response curves with a range of slopes; graded changes in PaCO2 resulted in redistributions of BOLD signal consistent with the known underlying vascular pathology and predictions of the model. We conclude that this model can be applied to provide a hemodynamic interpretation to BOLD signal changes in response to hypercapnia, and thereby aid in relating CVR maps to pathophysiological conditions.
•We develop a model of competition for blood flow among cerebrovascular regions.•The model explains cerebral blood flow vasodilatory stimulation response maps.•Experiments using BOLD MRI validate essential aspects of the conceptual model.
Objectives The aim of this study was to determine the phenotypic and genotypic resistance profiles of methicillin-resistant Staphylococcus pseudintermedius (MRSP) and to examine the clonal ...distribution in Europe and North America. Methods A total of 103 MRSP isolates from dogs isolated from several countries in Europe, the USA and Canada were characterized. Isolates were identified by PCR–restriction fragment length polymorphism (RFLP), antimicrobial susceptibility was determined by broth dilution or gradient diffusion, and antimicrobial resistance genes were detected using a microarray. Genetic diversity was assessed by multilocus sequence typing (MLST), PFGE and spa typing. Staphylococcal cassette chromosome mec (SCCmec) elements were characterized by multiplex PCR. Results Thirteen different sequence types (STs), 18 PFGE types and 8 spa types were detected. The hybrid SCCmec element II–III described in a MRSP isolate was present in 75 (72.8%) isolates. The remaining isolates either had SCCmec type III (n = 2), IV (n = 6), V (n = 14) or VII-241 (n = 4) or were non-typeable (n = 2). The most common genotypes were ST71(MLST)-J(PFGE)-t02(spa)-II–III(SCCmec) (56.3%) and ST68-C-t06-V (12.6%). In addition to mecA-mediated β-lactam resistance, isolates showed resistance to trimethoprim dfr(G) (90.3%), gentamicin/kanamycin aac(6′)-Ie–aph(2′)-Ia (88.3%), kanamycin aph(3′)-III (90.3%), streptomycin ant(6′)-Ia (90.3%), streptothricin (sat4) (90.3%), macrolides and/or lincosamides erm(B), lnu(A) (89.3%), fluoroquinolones (87.4%), tetracycline tet(M) and/or tet(K) (69.9%), chloramphenicol (catpC221) (57.3%) and rifampicin (1.9%). Conclusions Two major clonal MRSP lineages have disseminated in Europe (ST71-J-t02-II–III) and North America (ST68-C-t06-V). Regardless of their geographical or clonal origin, the isolates displayed resistance to the major classes of antibiotics used in veterinary medicine and thus infections caused by MRSP isolates represent a serious therapeutic challenge.
We characterize the near-infrared dust attenuation for a sample of ∼5500 local ( ) star-forming galaxies and obtain an estimate of their average total-to-selective attenuation . We utilize data from ...the United Kingdom Infrared Telescope and the Two-Micron All Sky Survey, which is combined with previously measured UV-optical data for these galaxies. The average attenuation curve is slightly lower in the far-ultraviolet than in local starburst galaxies by roughly 15% but appears similar at longer wavelengths with a total-to-selective normalization of . Under the assumption of energy balance, the total attenuated energy inferred from this curve is found to be broadly consistent with the observed infrared dust emission ( ) in a small sample of local galaxies for which far-infrared measurements are available. However, the significant scatter in this quantity among the sample may reflect large variations in the attenuation properties of individual galaxies. We also derive the attenuation curve for subpopulations of the main sample, separated according to mean stellar population age (via ), specific star formation rate, stellar mass, and metallicity, and find that they show only tentative trends with low significance, at least over the range that is probed by our sample. These results indicate that a single curve is reasonable for applications seeking to broadly characterize large samples of galaxies in the local universe, while applications to individual galaxies would yield large uncertainties and is not recommended.
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