The experimental setup, consisting of a bundle of dialysis tubing 2.5 mm in diameter 10-15 kD cutoff, mean pore size 25 A, 20 microns (dry) and 40 microns (wet) wall thickness inserted into a 1-l ...glass bioreactor supplied with oxygen and pH electrodes, a porous gas distributor, a sampling tube, and a holder for the eight pieces of dialysis tubing, was developed to investigate the properties and the microenvironment of hybridoma cells enclosed in the tubing during their batch cultivation. The concentrations of low-molecular-weight medium components were the same inside and outside the tubing, and it was possible to control the microenvironment of the cells in the tubing easily. The cell damage caused by mechanical stress was less in the dialysis tubing than in stirred spinner flasks. The influence of the initial cell density in the range from 4 X 10(5) to 1 X 10(8) cells ml-1 and the cultivation time were evaluated according to the total and viable cell concentrations and the cell/cell fragment size distributions. Furthermore, the cell membrane properties, glucose consumption rate, lactate, ammonia and lipid storage material, and the monoclonal antibody production rates as well as intracellular enzyme activities in the culture medium were measured and compared to those in reference cultures in spinner flasks with the same inoculum at low initial cell densities. In dialysis tubing in a concentration range of 5 X 10(6) to 10(8) cells ml-1, the total and viable concentrations of cells remained the same during cultivation.
Context.
The Galactic plane has been observed extensively by a large number of Galactic plane surveys from infrared to radio wavelengths at an angular resolution below 40′′. However, a 21 cm line and ...continuum survey with comparable spatial resolution is lacking.
Aims.
The first half of THOR data (
l
= 14.0°−37.9°, and
l
= 47.1°−51.2°, |
b
|≤ 1.25°) has been published in our data release 1 paper. With this data release 2 paper, we publish all the remaining spectral line data and Stokes I continuum data with high angular resolution (10′′–40′′), including a new H
I
dataset for the whole THOR survey region (
l
= 14.0−67.4° and |
b
|≤ 1.25°). As we published the results of OH lines and continuum emission elsewhere, we concentrate on the H
I
analysis in this paper.
Methods.
With the
Karl G. Jansky
Very Large Array (VLA) in C-configuration, we observed a large portion of the first Galactic quadrant, achieving an angular resolution of ≤40′′. At
L
Band, the WIDAR correlator at the VLA was set to cover the 21 cm H
I
line, four OH transitions, a series of H
nα
radio recombination lines (RRLs;
n
= 151 to 186), and eight 128 MHz-wide continuum spectral windows, simultaneously.
Results.
We publish all OH and RRL data from the C-configuration observations, and a new H
I
dataset combining VLA C+D+GBT (VLA D-configuration and GBT data are from the VLA Galactic Plane Survey) for the whole survey. The H
I
emission shows clear filamentary substructures at negative velocities with low velocity crowding. The emission at positive velocities is more smeared-out, likely due to higher spatial and velocity crowding of structures at the positive velocities. Compared to the spiral arm model of the Milky Way, the atomic gas follows the Sagittarius and Perseus Arm well, but with significant material in the inter-arm regions. With the C-configuration-only H
I
+continuum data, we produce an H
I
optical depth map of the THOR areal coverage from 228 absorption spectra with the nearest-neighbor method. With this
τ
map, we corrected the H
I
emission for optical depth, and the derived column density is 38% higher than the column density with optically thin assumption. The total H
I
mass with optical depth correction in the survey region is 4.7 × 10
8
M
⊙
, 31% more than the mass derived assuming the emission is optically thin. If we applied this 31% correction to the whole Milky Way, the total atomic gas mass would be 9.4–10.5 × 10
9
M
⊙
. Comparing the H
I
with existing CO data, we find a significant increase in the atomic-to-molecular gas ratio from the spiral arms to the inter-arm regions.
Conclusions.
The high-sensitivity and resolution THOR H
I
dataset provides an important new window on the physical and kinematic properties of gas in the inner Galaxy. Although the optical depth we derive is a lower limit, our study shows that the optical depth correction issignificant for H
I
column density and mass estimation. Together with the OH, RRL and continuum emission from the THOR survey, these new H
I
data provide the basis for high-angular-resolution studies of the interstellar medium in different phases.
Wird der agrarpolitische Weg einer zunehmenden Beruecksichtigung ueberbetrieblicher Leistungen des Agrarsektors fortgesetzt, so sind folgende Entwicklungen denkbar: Ein Ausbau der ...produktionsungebundenen Direktfoerderungen fuehrt bei gleichzeitig stattfindenden Preissenkungen zu negativen Produktionsanreizen und damit tendentiell zu einer Reduktion agrarischer Ueberschuesse. Gewinnt die Landschaftspflegefunktion als eigenstaendige Leistungskomponente an Bedeutung, so ist mit einer zunehmenden Dualisierung der Landwirtschaft zu rechnen. Waehrend in Gunstlagen die effiziente Produktion von Nahrungsmitteln und Rohstoffen unter Beruecksichtigung oekologischer Rahmenbedingungen im Mittelpunkt steht, wird in den Berg- und Huegelregionen die Nahrungsmittelproduktion von der Erhaltung eines intakten Lebens- und Erholungsraumes abhaengen. Insbesondere ist durch den Ausbau landwirtschaftlicher Direktzahlungen mit einer Verringerung bestehender intrasektoraler Einkommensdifferentiale zu rechnen. Dies impliziert sowohl eine Umverteilung in bezug auf die agrarischen Regionen als auch bezueglich unterschiedlicher Betriebsgroessen. Dass im derzeitigen System der Agrarfoerderung dem Bereich der Landschaftspflege (noch) nicht ausreichend Rechnung getragen wird, zeigt beispielsweise eine Analyse der derzeitigen landwirtschaftlichen Foerderungsstruktur
BACKGROUND
Hypertension and metabolic syndrome (MetS) are associated with increased sympathetic activation possibly contributing to the progression of renal damage and cardiac remodeling. Renal ...sympathetic denervation (RDN) decreases sympathetic renal efferent and afferent nerve activity.
METHODS
Obese spontaneously hypertensive rats (SHRs-ob) were subjected to RDN at the age of 34 weeks (SHRs-ob + RDN) and were compared with sham-operated SHRs-ob and their normotensive lean controls (Ctrs). Blood pressure was measured by telemetry. Kidney and heart function were determined by magnetic resonance imaging (MRI). Renal and cardiac remodeling were characterized by immunohistochemical analyses. Animals were killed at the age of 48 weeks.
RESULTS
In SHRs-ob, RDN attenuated the progressive increase in blood pressure and preserved a mean blood pressure of 156±7mm Hg compared with 220±8mm Hg in sham-operated SHRs-ob at 100 days after RDN, whereas heart rate, body weight, and metabolic parameters remained unchanged. Renal catecholamine and tyrosine hydroxylase levels were significantly reduced after RDN, suggesting effective renal denervation. Progression of renal dysfunction as characterized by increased urinary albumin/creatinine ratio and reduced glomerular filtration rate were attenuated by RDN. In SHRs-ob, renal perfusion was significantly reduced and normalized by RDN. Cardiac fibrosis and cardiac diastolic dysfunction measured by MRI and invasive pressure measurements were significantly attenuated by RDN.
CONCLUSIONS
In SHRs-ob, progressive increase in blood pressure and progression of renal injury and cardiac remodelling are mediated by renal sympathetic activation as they were attenuated by RDN.
Understanding planet formation requires one to discern how dust grows in protoplanetary disks. An important parameter to measure in disks is the maximum dust grain size present. This is usually ...estimated through measurements of the dust opacity at different millimeter wavelengths assuming optically thin emission and dust opacity dominated by absorption. However, Atacama Large Millimeter/submillimeter Array (ALMA) observations have shown that these assumptions might not be correct in the case of protoplanetary disks, leading to overestimation of particle sizes and to underestimation of the disk's mass. Here, we present an analysis of high-quality ALMA and Very Large Array images of the HL Tau protoplanetary disk, covering a wide range of wavelengths, from 0.8 mm to 1 cm, and with a physical resolution of ∼7.35 au. We describe a procedure to analyze a set of millimeter images without any assumption about the optical depth of the emission, and including the effects of absorption and scattering in the dust opacity. This procedure allows us to obtain the dust temperature, the dust surface density, and the maximum particle size at each radius. In the HL Tau disk, we found that particles have already grown to a few millimeters in size. We detect differences in the dust properties between dark and bright rings, with dark rings containing low dust density and small dust particles. Different features in the HL Tau disk seem to have different origins. Planet-disk interactions can explain substructure in the external half of the disk, but the internal rings seem to be associated with the presence of snow lines of several molecules.
Sodium tissue content by
Na magnetic resonance imaging (Na-MRI) has been validated in experimental and human studies. SGLT-2 inhibition blocks the reabsorption of glucose and of sodium in the ...proximal tubular cells in a 1:1 fashion. We hypothesized that SGLT-2 inhibition in patients with type 2 diabetes characterized by sodium retention leads to decreased tissue sodium content due to its pharmacological action.
In a prospective double blind, placebo controlled, cross-over trial 59 patients (61 ± 7.6 years) with type 2 diabetes were randomized to either dapagliflozin 10 mg or placebo once daily for 6 weeks each. In addition to metabolic parameters and ambulatory blood pressure (BP) we analysed the sodium content in the skin and muscles of the lower leg by Na-MRI.
Compared to baseline 6 weeks treatment with the SGLT-2 inhibitor dapagliflozin decreased fasting (132 ± 28 vs. 114 ± 19 mg/dl, p < 0.001), postprandial blood glucose (178 ± 66 mg/dl vs. 153 ± 46 mg/dl, p < 0.001), body weight (87.6 vs. 86.6 kg, p < 0.001) and systolic (129 ± 12 vs. 126 ± 11 mmHg, p = 0.010), and diastolic (77.4 ± 9 vs. 75.6 ± 8 mmHg, p = 0.024), 24-h ambulatory BP. Tissue sodium content in the skin was reduced after 6 weeks treatment with dapagliflozin compared to baseline 24.1 ± 6.6 vs. 22.7 ± 6.4 A.U.(arbitrary unit) p = 0.013. No significant reduction of tissue sodium content was observed in the muscle (M. triceps surae: 20.5 ± 3.5 vs. 20.4 ± 3.7 A.U. p = 0.801). No clear significant difference in tissue water content of muscle and skin was observed after 6 weeks of treatment with dapagliflozin, compared to baseline.
SGLT-2 inhibition with dapagliflozin resulted in a significant decrease in tissue sodium content of the skin after 6 weeks. This observation point to a decrease of total sodium content in patients with type 2 diabetes prone to cardiovascular complications, that might be mitigated by SGLT-2 inhibition. Trial registration The study was registered at http://www.clinicaltrials.gov (NCT02383238) retrospectively registered.
Molecular clouds form from the atomic phase of the interstellar medium. However, characterizing the transition between the atomic and the molecular interstellar medium (ISM) is a complex ...observational task. Here we address cloud formation processes by combining H
I
self absorption (HISA) with molecular line data. Column density probability density functions (N-PDFs) are a common tool for examining molecular clouds. One scenario proposed by numerical simulations is that the N-PDF evolves from a log-normal shape at early times to a power-law-like shape at later times. To date, investigations of N-PDFs have been mostly limited to the molecular component of the cloud. In this paper, we study the cold atomic component of the giant molecular filament GMF38.1-32.4a (GMF38a, distance = 3.4 kpc, length ~ 230 pc), calculate its N-PDFs, and study its kinematics. We identify an extended HISA feature, which is partly correlated with the
13
CO emission. The peak velocities of the HISA and
13
CO observations agree well on the eastern side of the filament, whereas a velocity offset of approximately 4 km s
−1
is found on the western side. The sonic Mach number we derive from the linewidth measurements shows that a large fraction of the HISA, which is ascribed to the cold neutral medium (CNM), is at subsonic and transonic velocities. The column density of the CNM part is on the order of 10
20
to 10
21
cm
−2
. The column density of molecular hydrogen, traced by
13
CO, is an order of magnitude higher. The N-PDFs from HISA (CNM), H
I
emission (the warm and cold neutral medium), and
13
CO (molecular component) are well described by log-normal functions, which is in agreement with turbulent motions being the main driver of cloud dynamics. The N-PDF of the molecular component also shows a power law in the high column-density region, indicating self-gravity. We suggest that we are witnessing two different evolutionary stages within the filament. The eastern subregion seems to be forming a molecular cloud out of the atomic gas, whereas the western subregion already shows high column density peaks, active star formation, and evidence of related feedback processes.
We present a study of the filamentary structure in the emission from the neutral atomic hydrogen (H
I
) at 21 cm across velocity channels in the 40′′ and 1.5-km s
−1
resolution ...position-position-velocity cube, resulting from the combination of the single-dish and interferometric observations in The H
I
/OH/recombination-line survey of the inner Milky Way. Using the Hessian matrix method in combination with tools from circular statistics, we find that the majority of the filamentary structures in the H
I
emission are aligned with the Galactic plane. Part of this trend can be assigned to long filamentary structures that are coherent across several velocity channels. However, we also find ranges of Galactic longitude and radial velocity where the H
I
filamentary structures are preferentially oriented perpendicular to the Galactic plane. These are located (i) around the tangent point of the Scutum spiral arm and the terminal velocities of the Molecular Ring, around
l
≈ 28° and
v
LSR
≈ 100 km s
−1
, (ii) toward
l
≈ 45° and
v
LSR
≈ 50 km s
−1
, (iii) around the Riegel-Crutcher cloud, and (iv) toward the positive and negative terminal velocities. A comparison with numerical simulations indicates that the prevalence of horizontal filamentary structures is most likely the result of large-scale Galactic dynamics and that vertical structures identified in (i) and (ii) may arise from the combined effect of supernova (SN) feedback and strong magnetic fields. The vertical filamentary structures in (iv) can be related to the presence of clouds from extra-planar H
I
gas falling back into the Galactic plane after being expelled by SNe. Our results indicate that a systematic characterization of the emission morphology toward the Galactic plane provides an unexplored link between the observations and the dynamical behavior of the interstellar medium, from the effect of large-scale Galactic dynamics to the Galactic fountains driven by SNe.
Context Radio continuum surveys of the Galactic plane can find and characterize H II regions, supernova remnants (SNRs), planetary nebulae (PNe), and extragalactic sources. A number of surveys at ...high angular resolution (≤25″) at different wavelengths exist to study the interstellar medium (ISM), but no comparable high-resolution and high-sensitivity survey exists at long radio wavelengths around 21 cm. Aims. Our goal is to investigate the 21 cm radio continuum emission in the northern Galactic plane at < 25″ resolution. Methods We observed a large percentage of the Galactic plane in the first quadrant of the Milky Way (l = 14.0−67.4° and |b| ≤ 1.25°) with the Karl G. Jansky Very Large Array (VLA) in the C-configuration covering six continuum spectral windows (SPW). These data provide a detailed view on the compact as well as extended radio emission of our Galaxy and thousands of extragalactic background sources. Results We used the BLOBCAT software and extracted 10 916 sources. After removing spurious source detections caused by the side lobes of the synthesized beam, we classified 10 387 sources as reliable detections. We smoothed the images to a common resolution of 25″ and extracted the peak flux density of each source in each SPW to determine the spectral indices α (assuming I(ν) ∝ να). By cross-matching with catalogs of H II regions, SNRs, PNe, and pulsars, we found radio counterparts for 840 H II regions, 52 SNRs, 164 PNe, and 38 pulsars. We found 79 continuum sources that are associated with X-ray sources. We identified 699 ultra-steep spectral sources (α < −1.3) that could be high-redshift galaxies. About 9000 of the sources we extracted are not classified specifically, but based on their spatial and spectral distribution, a large percentage of these are likely to be extragalactic background sources. More than 7750 sources do not have counterparts in the SIMBAD database and more than 3760 sources do not have counterparts in the NED database. Conclusions Studying the long wavelengths centimeter continuum emission and the associated spectral indices allows us to characaterize a large percentage of Galactic and extragalactic radio sources in the area of the northern inner Milky Way. This database will be extremely useful for future studies of a diverse set of astrophysical objects.
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