IMPORTANCE More than 70% of patients with resistant hypertension have obstructive sleep apnea (OSA). However, there is little evidence about the effect of continuous positive airway pressure (CPAP) ...treatment on blood pressure in patients with resistant hypertension. OBJECTIVE To assess the effect of CPAP treatment on blood pressure values and nocturnal blood pressure patterns in patients with resistant hypertension and OSA. DESIGN, SETTING, AND PARTICIPANTS Open-label, randomized, multicenter clinical trial of parallel groups with blinded end point design conducted in 24 teaching hospitals in Spain involving 194 patients with resistant hypertension and an apnea-hypopnea index (AHI) of 15 or higher. Data were collected from June 2009 to October 2011. INTERVENTIONS CPAP or no therapy while maintaining usual blood pressure control medication. MAIN OUTCOMES AND MEASURES The primary end point was the change in 24-hour mean blood pressure after 12 weeks. Secondary end points included changes in other blood pressure values and changes in nocturnal blood pressure patterns. Both intention-to-treat (ITT) and per-protocol analyses were performed. RESULTS A total of 194 patients were randomly assigned to receive CPAP (n = 98) or no CPAP (control; n = 96). The mean AHI was 40.4 (SD, 18.9) and an average of 3.8 antihypertensive drugs were taken per patient. Baseline 24-hour mean blood pressure was 103.4 mm Hg; systolic blood pressure (SBP), 144.2 mm Hg; and diastolic blood pressure (DBP), 83 mm Hg. At baseline, 25.8% of patients displayed a dipper pattern (a decrease of at least 10% in the average nighttime blood pressure compared with the average daytime blood pressure). The percentage of patients using CPAP for 4 or more hours per day was 72.4%. When the changes in blood pressure over the study period were compared between groups by ITT, the CPAP group achieved a greater decrease in 24-hour mean blood pressure (3.1 mm Hg 95% CI, 0.6 to 5.6; P = .02) and 24-hour DBP (3.2 mm Hg 95% CI, 1.0 to 5.4; P = .005), but not in 24-hour SBP (3.1 mm Hg 95% CI, −0.6 to 6.7; P = .10) compared with the control group. Moreover, the percentage of patients displaying a nocturnal blood pressure dipper pattern at the 12-week follow-up was greater in the CPAP group than in the control group (35.9% vs 21.6%; adjusted odds ratio OR, 2.4 95% CI, 1.2 to 5.1; P = .02). There was a significant positive correlation between hours of CPAP use and the decrease in 24-hour mean blood pressure (r = 0.29, P = .006), SBP (r = 0.25; P = .02), and DBP (r = 0.30, P = .005). CONCLUSIONS AND RELEVANCE Among patients with OSA and resistant hypertension, CPAP treatment for 12 weeks compared with control resulted in a decrease in 24-hour mean and diastolic blood pressure and an improvement in the nocturnal blood pressure pattern. Further research is warranted to assess longer-term health outcomes. TRIAL REGISTRATION clinicaltrials.gov Identifier: NCT00616265
The miniJPAS survey González Delgado, R. M.; Díaz-García, L. A.; de Amorim, A. ...
Astronomy and astrophysics (Berlin),
05/2021, Letnik:
649
Journal Article
Recenzirano
Odprti dostop
The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) will soon start imaging thousands of square degrees of the northern sky with its unique set of 56 filters (spectral ...resolution of
R
∼ 60). Before the arrival of the final instrument, we observed 1 deg
2
on the AEGIS field with an interim camera with all the J-PAS filters. Taking advantage of these data, dubbed miniJPAS, we aim at proving the scientific potential of the J-PAS to derive the stellar population properties of galaxies via fitting codes for spectral energy distributions (SEDs), with the ultimate goal of performing galaxy evolution studies across cosmic time. One parametric (
BaySeAGal
) and three non-parametric (
MUFFIT
,
AlStar
, and
TGASPEX
) SED-fitting codes are used to constrain the stellar mass, age, metallicity, extinction, and rest-frame and dust-corrected (
u
−
r
) colours of a complete flux-limited sample (
r
SDSS
≤ 22.5 AB) of miniJPAS galaxies that extends up to
z
= 1. We generally find consistent results on the galaxy properties derived from the different codes, independently of the galaxy spectral type or redshift; this is remarkable considering that 25% of the J-spectra have signal-to-noise ratios (S/N) ∼3. For galaxies with
S
/
N
≥ 10, we estimate that the J-PAS photometric system will allow us to derive the stellar population properties of rest-frame (
u
−
r
) colour, stellar mass, extinction, and mass-weighted age with a precision of 0.04 ± 0.02 mag, 0.07 ± 0.03 dex, 0.2 ± 0.09 mag, and 0.16 ± 0.07 dex, respectively. This precision is equivalent to that obtained with spectroscopic surveys of similar S/N. By using the dust-corrected (
u
−
r
) colour–mass diagram, a powerful proxy for characterizing galaxy populations, we find: (i) that the fraction of red and blue galaxies evolves with cosmic time, with red galaxies being ∼38% and ∼18% of the whole population at
z
= 0.1 and
z
= 0.5, respectively, and (ii) consistent results between codes for the average intrinsic (
u
−
r
) colour, stellar mass, age, and stellar metallicity of blue and red galaxies and their evolution up to
z
= 1. At all redshifts, the more massive galaxies belong to the red sequence, and these galaxies are typically older and more metal-rich than their counterparts in the blue cloud. Our results confirm that with J-PAS data we will be able to analyse large samples of galaxies up to
z
∼ 1, with galaxy stellar masses above log(
M
⋆
/
M
⊙
)∼8.9, 9.5, and 9.9 at
z
= 0.3, 0.5, and 0.7, respectively. The star formation history of a complete sub-sample of galaxies selected at
z
∼ 0.1 with log(
M
⋆
/
M
⊙
) > 8.3 constrains the cosmic evolution of the star formation rate density up to
z
∼ 3, in good agreement with results from cosmological surveys.
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•The dependence between the BC-surface condition and the α-Al2O3 phase formation.•Low-temperature α-Al2O3 formation in the pre-oxidation treatments.•Influence of the grit-blasting on ...the oxidation kinetics of β-(Ni, Pt)Al System.•In the grit-blasted samples, oxidation stable-state is reached less than 2 h.•Stifle the growth of metastable θ-Al2O3 and accelerate θ- to α-Al2O3 at > 1000 °C.
The effect of surface modification by grit-blasting of β-(Ni,Pt)Al bond coats on the growth of α-Al2O3 is here presented. Thermogravimetry tests at 1000 °C, 1050 °C, 1100 °C, and 1150 °C were performed on as-aluminized and as-grit-blasted specimens under the same oxygen partial pressure (pO2 = 2.1 × 10-1 atm), where the parabolic rate constant (kp) was calculated. The oxide phase fraction was obtained from the fitting of the photo-stimulated luminescence spectroscopy (PSLS) results. A strong dependence between the surface condition of the bond coat and the α-Al2O3 phase formation was observed. The thermally treated grit-blasted samples achieved faster the steady-state (1.6 h) of the thermal growth oxide (TGO), while a treatment 2.7 times longer (4.25 h) was required for the as-aluminized specimens. This result contributes to the general understanding of the effect of the surface condition on the TGO formation during pre-oxidation treatment to promote the growth of the α-Al2O3 phase at low temperature and less time without affecting the lifetime of thermal barrier coating systems.
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•NI lesion did not affect discrimination between conspecific and object.•NI lesion impaired increased interaction to the novel vs familiar conspecific.•NI lesion produce Egr-1 ...decrease in amygdala, septum and hypothalamus.•N lesion increased Egr-1 in hippocampus.•NI neural networks contribute to social recognition in rats.
Social interaction involves neural activity in prefrontal cortex, septum, hippocampus, amygdala and hypothalamus. Notably, these areas all receive projections from the nucleus incertus (NI) in the pontine tegmentum. Therefore, we investigated the effect of excitotoxic lesions of NI neurons in adult male, Wistar rats on performance in a social discrimination test, and associated changes in immediate-early gene protein levels. NI was lesioned with quinolinic acid, and after recovery, rats underwent two trials in the 3-chamber test. In the first trial, NI-lesioned and sham-lesioned rats spent longer exploring a conspecific than an inanimate object. By contrast, in the second trial, NI-lesioned rats visited the familiar and novel conspecific chambers equally, whereas sham-lesioned rats spent longer engaging with the novel rat. Quantification of Fos- and Egr-1-immunoreactivity (IR) levels in brain areas implicated in social behaviour, revealed that social encounter and NI lesion produced complex, differential changes. For example, Egr-1-IR was broadly decreased in several amygdala nuclei in NI-lesioned rats relative to sham, but Fos-IR levels were unaltered. In hippocampus, NI-lesioned rats displayed decreased Fos-IR in CA2 and CA3, while Egr-1-IR was increased in the polymorphic dentate gyrus, CA1, CA2 and subiculum of NI-lesioned rats, relative to sham. Social encounter-related Egr-1-IR was also decreased in septum and anterior and lateral hypothalamus of NI-lesioned rats. Overall, these data suggest NI networks can modulate the activity of sensory, emotional and executive brain areas involved in social recognition, with a likely involvement of neuronal Egr-1 activation in amygdala, septum and hypothalamus, and Erg-1 inhibition in hippocampus.
Aims. We aim at constraining the stellar population properties of quiescent galaxies. These properties reveal how these galaxies evolved and assembled since z ∼ 1 up to the present time. Methods. ...Combining the ALHAMBRA multi-filter photo-spectra with the fitting code for spectral energy distribution MUFFIT (MUlti-Filter FITting), we built a complete catalogue of quiescent galaxies via the dust-corrected stellar mass vs. colour diagram. This catalogue includes stellar population properties, such as age, metallicity, extinction, stellar mass, and photometric redshift, retrieved from the analysis of composited populations based on two independent sets of simple stellar population (SSP) models. We developed and applied a novel methodology to provide, for the first time, the analytic probability distribution functions (PDFs) of mass-weighted age, metallicity, and extinction of quiescent galaxies as a function of redshift and stellar mass. We adopted different star formation histories to discard potential systematics in the analysis. Results. The number density of quiescent galaxies is found to increase since z ∼ 1, with a more substantial variation at lower stellar mass. Quiescent galaxies feature extinction AV < 0.6, with median values in the range AV = 0.15–0.3. At increasing stellar mass, quiescent galaxies are older and more metal rich since z ∼ 1. A detailed analysis of the PDFs reveals that the evolution of quiescent galaxies is not compatible with passive evolution and a slight decrease of 0.1–0.2 dex is hinted at median metallicity. The intrinsic dispersion of the age and metallicity PDFs show a dependence on stellar mass and/or redshift. These results are consistent with both sets of SSP models and assumptions of alternative star formation histories explored. Consequently, the quiescent population must undergo an evolutive pathway including mergers and/or remnants of star formation to reconcile the observed trends, where the “progenitor” bias should also be taken into account.
Aims.
We perform a comprehensive study of the stellar population properties (formation epoch, age, metallicity, and extinction) of quiescent galaxies as a function of size and stellar mass to ...constrain the physical mechanism governing the stellar mass assembly and the likely evolutive scenarios that explain their growth in size.
Methods.
After selecting all the quiescent galaxies from the ALHAMBRA survey by the dust-corrected stellar mass–colour diagram, we built a shared sample of ∼850 quiescent galaxies with reliable measurements of sizes from the HST. This sample is complete in stellar mass and luminosity,
I
≤ 23. The stellar population properties were retrieved using the fitting code for spectral energy distributions called MUlti-Filter FITting for stellar population diagnostics (MUFFIT) with various sets of composite stellar population models. Age, formation epoch, metallicity, and extinction were studied on the stellar mass–size plane as function of size through a Monte Carlo approach. This accounted for uncertainties and degeneracy effects amongst stellar population properties.
Results.
The stellar population properties of quiescent galaxies and their stellar mass and size since
z
∼ 1 are correlated. At fixed stellar mass, the more compact the quiescent galaxy, the older and richer in metals it is (1 Gyr and 0.1 dex, respectively). In addition, more compact galaxies may present slight lower extinctions than their more extended counterparts at the same stellar mass (< 0.1 mag). By means of studying constant regions of stellar population properties across the stellar mass–size plane, we obtained empirical relations to constrain the physical mechanism that governs the stellar mass assembly of the form
M
⋆
∝
r
c
α
, where
α
amounts to 0.50–0.55 ± 0.09. There are indications that support the idea that the velocity dispersion is tightly correlated with the stellar content of galaxies. The mechanisms driving the evolution of stellar populations can therefore be partly linked to the dynamical properties of galaxies, along with their gravitational potential.
Ni-Mo2C particles supported over hydroxyapatite were synthesized as potential catalysts to hydrogen production applications due their physiochemical properties observed in characterization results, ...this favorable for biomass gasification. Mo2C particles doped with Ni were synthesized by temperature programmed reaction method at 900 °C under hydrogen reducing atmosphere. Hydroxyapatite support was obtained from thermal extraction of bovine bones, in a temperature range from 700 to 900 °C. Ni-Mo2C impregnation over hydroxyapatite support was made by incipient humidity method. X-ray diffraction analysis determined crystallographic phases of β-Mo2C, NiC and hydroxyapatite. Though, bone organic matter degradation was observed by X-ray diffraction and confirmed by Infrared Spectroscopy with Fourier Transform (FTIR) the final structure of hydroxyapatite was maintained. Finally, textural properties analysis of support showed an increase in porosity structure with the increment of temperature. β-Mo2C and NiC were obtained with similar catalytic activity than noble metals, also nickel improves hydrocarbons bonds rupture. Hydroxyapatite showed high stability and porosity at elevated temperatures attributable to synthesis conditions.
•NiMo2C/hydroxyapatite catalysts were prepared for hydrogen production applications.•β-molybdenum carbide was obtained with different wt% Ni loading.•Porous and stable hydroxyapatite structure at high temperature was observed.•NiMo2C was successfully impregnated over hydroxyapatite support.
The miniJPAS survey González Delgado, R. M.; Rodríguez-Martín, J. E.; Díaz-García, L. A. ...
Astronomy and astrophysics (Berlin),
10/2022, Letnik:
666
Journal Article
Recenzirano
Odprti dostop
The miniJPAS survey has observed ∼1 deg
2
of the AEGIS field with 60 bands (spectral resolution of
R
∼ 60) in order to demonstrate the scientific potential of the Javalambre-Physics of the ...Accelerating Universe Astrophysical Survey (J-PAS), which will map ∼8000 deg
2
of the northern sky over the coming years. In particular, this paper demonstrates the potential of J-PAS in detecting groups with mass of up to 10
13
M
⊙
and in characterising their galaxy populations up to
z
∼ 1. The parametric code BaySeAGal is used to derive the stellar population properties by fitting the J-PAS spectral energy distribution (SED) of the galaxy members in 80 groups at
z
≤ 0.8 previously detected by the AMICO code, and of a galaxy field sample retrieved from the whole miniJPAS down to
r
< 22.75 (AB). Blue, red, quiescent, and transition (blue quiescent or green valley) galaxy populations are identified through their rest-frame (extinction-corrected) (
u
−
r
)
int
colour, galaxy stellar mass (
M
⋆
), and specific star formation rate (sSFR). We measure the abundance of these galaxies as a function of
M
⋆
and environment in order to investigate the role that groups play in quenching star formation. Our findings are as follows. (i) The fraction of red and quiescent galaxies in groups increases with
M
⋆
and is always higher in groups (28% on average) than in the field (5%). (ii) The quenched fraction excess (QFE) in groups shows a strong dependence on
M
⋆
, and increases from a few percent for galaxies with
M
⋆
< 10
10
M
⊙
to higher than 60% for galaxies with
M
⋆
> 3 × 10
11
M
⊙
. (iii) The abundance excess of transition galaxies in groups shows a modest dependence on
M
⋆
, being 5%–10% for galaxies with
M
⋆
< 10
11
M
⊙
. (iv) The fading timescale, defined as the time that galaxies in groups spend in the transition phase, is very short (< 1.5 Gyr), indicating that the star formation of galaxies in groups declines very rapidly. (v) The evolution of the galaxy quenching rate in groups shows a modest but significant evolution since
z
∼ 0.8. This latter result is compatible with the expected evolution with constant QFE = 0.4, which has been previously measured for satellites in the nearby Universe, as traced by SDSS. Further, this evolution is consistent with a scenario where the low-mass star forming galaxies in clusters at
z
= 1–1.4 are environmentally quenched, as previously reported by other surveys.
Objective
To examine the characteristics of patients who developed late onset systemic lupus erythematosus (SLE) in the GLADEL (Grupo Latino Americano de Estudio del Lupus) cohort of patients with ...SLE.
Methods
Patients with SLE of less than two years of disease duration, seen at 34 centers of nine Latin American countries, were included. Late-onset was defined as >50 years of age at time of first SLE-related symptom. Clinical and laboratory manifestations, activity index (SLEDAI), and damage index (SLICC/ACR- DI) were ascertained at time of entry and during the course (cumulative incidence). Features were compared between the two patient groups (<50 and ≥50) using descriptive statistics and hypothesis tests. Logistic regression was performed to examine the association of late-onset lupus, adjusting for other variables.
Results
Of the 1480 patients included, 102 patients (6.9 %) had late-onset SLE, 87% of which were female. Patients with late-onset SLE had a shorter follow-up (3.6 vs. 4.4 years, p < 0.002) and a longer time to diagnosis (10.1 vs. 5.8 months, p < 0.001) compared to the younger onset group. Malar rash, photosensitivity, and renal involvement were less prevalent while interstitial lung disease, pleural effusions, and sicca symptoms were more frequent in the older age group (p > 0.05). In multivariable analysis, late onset was independently associated with higher odds of ocular (OR = 3.66, 95% CI = 2.15–6.23), pulmonary (OR = 2.04, 95% CI = 1.01–4.11), and cardiovascular (OR = 1.76, 95% CI = 1.04–2.98) involvement and lower odds of cutaneous involvement (OR = 0.41, 95% CI = 0.21–0.80), number of cumulative SLE criteria (OR = 0.79, 95% CI = 0.64–0.97), use of cyclophosphamide (OR = 0.47, 95% CI = 0.24–0.95), and anti-RNP antibodies (OR = 0.43, 95% CI = 0.20–0.91). A Cox regression model revealed a higher risk of dying in older onset than the younger-onset SLE (OR = 2.61, 95% CI = 1.2–5.6).
Conclusion
Late-onset SLE in Latin Americans had a distinct disease expression compared to the younger-onset group. The disease seems to be mild with lower cumulative SLE criteria, reduced renal/mucocutaneous involvements, and less use of cyclophosphamide. Nevertheless, these patients have a higher risk of death and of ocular, pulmonary, and cardiovascular involvements.
Celotno besedilo
Dostopno za:
DOBA, IZUM, KILJ, NUK, OILJ, PILJ, PNG, SAZU, UILJ, UKNU, UL, UM, UPUK
We report on the measurement of the all-particle cosmic ray energy spectrum with the High Altitude Water Cherenkov (HAWC) Observatory in the energy range 10 to 500 TeV. HAWC is a ground-based ...air-shower array deployed on the slopes of Volcan Sierra Negra in the state of Puebla, Mexico, and is sensitive to gamma rays and cosmic rays at TeV energies. The data used in this work were taken over 234 days between June 2016 and February 2017. The primary cosmic-ray energy is determined with a maximum likelihood approach using the particle density as a function of distance to the shower core. Introducing quality cuts to isolate events with shower cores landing on the array, the reconstructed energy distribution is unfolded iteratively. The measured all-particle spectrum is consistent with a broken power law with an index of −2.49±0.01 prior to a break at (45.7±0.1) TeV, followed by an index of −2.71±0.01. The spectrum also represents a single measurement that spans the energy range between direct detection and ground-based experiments. As a verification of the detector response, the energy scale and angular resolution are validated by observation of the cosmic ray Moon shadow’s dependence on energy.
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