ABSTRACT
In this paper, we present a detailed spectroscopic study of the SB1 system HD 161660. New spectroscopic observations have been obtained by us with Catania Astrophysical Observatory ...Spectropolarimeter (CAOS@OAC). Combining these observations with archive data from HARPS@3.6ESO, we derived atmospheric parameters as temperature and gravity (from the fit of Balmer lines), microturbulence and rotational velocity (from metal lines), and chemical composition. We found underabundances of helium, carbon, magnesium, sulphur and chromium, overabundances of neon, phosphorus, argon, manganese, xenon, and mercury. All other elements have solar composition. In particular, mercury abundance is derived taking into account an isotopic mixture different from the terrestrial one (essentially pure 202Hg). Considering this chemical pattern, we definitively confirm HD 161660 is an HgMn star. Further, variability of equivalent widths points out a non-homogeneous distribution of helium and magnesium over stellar surface. As to iron and phosphorus, we found a non-constant abundance with the optical depth, a result currently considered an evidence of vertical stratification. Finally, we improved the fundamental parameters characterizing the HD 161660 orbit.
The CHEOPS space mission dedicated to exoplanet follow-up was launched in December 2019, equipped with the capacity to perform photometric measurements at the 20 ppm level. As CHEOPS carries out its ...observations in a broad optical passband, it can provide insights into the reflected light from exoplanets and constrain the short-wavelength thermal emission for the hottest of planets by observing occultations and phase curves. Here, we report the first CHEOPS observation of an occultation, namely, that of the hot Jupiter WASP-189 b, a
M
P
≈ 2
M
J
planet orbiting an A-type star. We detected the occultation of WASP-189 b at high significance in individual measurements and derived an occultation depth of dF = 87.9 ± 4.3 ppm based on four occultations. We compared these measurements to model predictions and we find that they are consistent with an unreflective atmosphere heated to a temperature of 3435 ± 27 K, when assuming inefficient heat redistribution. Furthermore, we present two transits of WASP-189 b observed by CHEOPS. These transits have an asymmetric shape that we attribute to gravity darkening of the host star caused by its high rotation rate. We used these measurements to refine the planetary parameters, finding a ~25% deeper transit compared to the discovery paper and updating the radius of WASP-189 b to 1.619 ± 0.021
R
J
. We further measured the projected orbital obliquity to be
λ
= 86.4
−4.4
+2.9°
, a value that is in good agreement with a previous measurement from spectroscopic observations, and derived a true obliquity of Ψ = 85.4 ± 4.3°. Finally, we provide reference values for the photometric precision attained by the CHEOPS satellite: for the
V
= 6.6 mag star, and using a 1-h binning, we obtain a residual RMS between 10 and 17 ppm on the individual light curves, and 5.7 ppm when combining the four visits.
Abstract A consistent amount of evidence suggests that vascular factors might be involved in the pathogenesis of late onset Alzheimer's disease (LOAD). We evaluated the presence of endothelial ...dysfunction by measuring the plasma levels of soluble E-selectin and vascular cell adhesion molecule 1 (VCAM-1) in a sample of patients affected by LOAD ( n . 60) or vascular dementia (VD: n . 80). They were compared with a sample of older patients with cerebrovascular disease but not-dementia (CDND: n . 40), and with a sample of healthy older controls ( n . 30). sVCAM-1 plasma levels were higher in LOAD and VD compared with controls. Among patients (LOAD, VD, and CDND), sE-selectin levels were higher in individuals with most severe cerebrovascular disease on CT scan. At multivariate regression analysis, fasting glucose ( p < 0.05) and TNF-α levels ( p < 0.02) were positively correlated with sE-selectin levels (adjusted r2 : 20%), while sVCAM-1 was positively correlated with age ( p < 0.01), and alcohol consumption ( p : 0.03), and negatively associated with HDL-C levels ( p : 0.005), ( p < 0.01; adjusted r2 : 44%), independent of possible confounders. Increased sVCAM-1 plasma levels in LOAD and VD suggest the existence of endothelial dysfunction in both types of dementia. The possible role of E-selectin in the pathogenesis of cerebrovascular disease is also supported by our data.
Abstract Some cytokines have been involved in the pathogenesis of late onset Alzheimer’s disease (LOAD). A possible increase in plasma cytokines levels has been reported in LOAD and vascular dementia ...(VD), but the results of previous studies are conflicting. We evaluated the plasma levels of IL-6, TNF-α, IL-1β, and IL-10 in four groups of older individuals: 60 patients with LOAD, 80 patients with VD, 40 subjects with cerebrovascular disease but without dementia (CDND), and 42 controls (C). By analysis of covariance (adjustment for age, gender, coronary heart disease, diabetes, hypertension, smoking, and alcohol consumption) we found that: • IL-1β was higher in VD, LOAD, and CDND compared with controls ( p < 0.005). • TNF-α was higher in VD and LOAD compared to C ( p < 0.05), and in VD compared to LOAD ( p < 0.03). • IL-6 was higher in VD compared with LOAD ( p < 0.03). No differences in IL-10 values were found (Kruskal–Wallis, Asymp. Sig. 0.14). By logistic regression analysis, we demonstrated that high levels (defined as above the median) of IL-1β and TNF-α, but not of IL-6, were associated with increased likelihood of having VD and LOAD compared to C, while high IL-6 levels were associated with a increased probability of having VD, compared with LOAD. Our study support the notion of a low-grade systemic inflammation in older patients with LOAD or VD, characterized by an increase in plasma IL-1β and TNF-α levels. The high IL-6 levels found in VD might be not a specific finding, as it might come from several conditions including atherosclerosis and related vascular risk factors, comorbidity, and frailty.
Context.
Gas giants orbiting close to hot and massive early-type stars can reach dayside temperatures that are comparable to those of the coldest stars. These ‘ultra-hot Jupiters’ have atmospheres ...made of ions and atomic species from molecular dissociation and feature strong day-to-night temperature gradients. Photometric observations at different orbital phases provide insights on the planet’s atmospheric properties.
Aims.
We aim to analyse the photometric observations of WASP-189 acquired with the Characterising Exoplanet Satellite (CHEOPS) to derive constraints on the system architecture and the planetary atmosphere.
Methods.
We implemented a light-curve model suited for an asymmetric transit shape caused by the gravity-darkened photosphere of the fast-rotating host star. We also modelled the reflective and thermal components of the planetary flux, the effect of stellar oblateness and light-travel time on transit-eclipse timings, the stellar activity, and CHEOPS systematics.
Results.
From the asymmetric transit, we measure the size of the ultra-hot Jupiter WASP-189 b, R
p
= 1.600
−0.016
+0.017
R
J
, with a precision of 1%, and the true orbital obliquity of the planetary system, Ψ
p
= 89.6 ± 1.2deg (polar orbit). We detect no significant hotspot offset from the phase curve and obtain an eclipse depth of δ
ecl
= 96.5
−5.0
+4.5
ppm, from which we derive an upper limit on the geometric albedo:
A
g
< 0.48. We also find that the eclipse depth can only be explained by thermal emission alone in the case of extremely inefficient energy redistribution. Finally, we attribute the photometric variability to the stellar rotation, either through superficial inhomogeneities or resonance couplings between the convective core and the radiative envelope.
Conclusions.
Based on the derived system architecture, we predict the eclipse depth in the upcoming Transiting Exoplanet Survey Satellite (TESS) observations to be up to ~165 ppm. High-precision detection of the eclipse in both CHEOPS and TESS passbands might help disentangle reflective and thermal contributions. We also expect the right ascension of the ascending node of the orbit to precess due to the perturbations induced by the stellar quadrupole moment
J
2
(oblateness).
ABSTRACT
Magnetic chemically peculiar stars of the main sequence can present rotational periods as long as many decades. Here we report the results of an observational campaign started in 2001 aimed ...at establishing these very long periods from the variability of the integrated magnetic field modulus, the so-called surface magnetic field Bs, as measured from the Zeeman splitting of the Fe ii 6149.258 Å spectral line. 36 stars have been monitored with various high-resolution spectrographs at different telescopes, totalling 412 newly collected spectra. To improve the phase coverage, we have also exploited all public archives containing high-resolution spectra, many not yet published. On the basis of these new Bs variability curves, we (1) confirm or revisit the periods of 24 stars, (2) extend the lower limits to the periods of HD 55719 (P > 38 yr), HD 165474 (P > 27 yr), and HD 177765 (P > 37 yr), (3) establish for the first time the periods of HD 29578 (P = 10.95 yr), HD 47103 (P = 17.683 d), HD 150562 (P = 5.7 yr), and HD 216018 (P = 34.044 d), and (4) set lower limits to the periods of HD 75445 (P »14 yr), HD 110066 (P » 29 yr), HD 116114 (P > 48 yr), and HD 137949 (P > 27 yr). As to γ Equ, whose period must exceed 90 yr, we point out a clear decrease in the field modulus, the maximum of which coincides within the uncertainties with the minimum of the variation in the integrated longitudinal field.
ABSTRACT
We present a long-term optical spectroscopic study of the post-asymptotic giant branch (AGB) binary system 89 Herculis, with the aim to characterize the relationship between photospheric ...instabilities and dynamics in the close circumstellar environment of the system. This study is based on spectra acquired with the high-resolution Catania Astrophysical Observatory Spectropolarimeter and archive data, covering a time interval between 1978 and 2018. We find long-term changes in the radial velocity curve of the system, occurring mostly in amplitude, which correlate with the variability observed in the blueshifted absorption component of the P Cygni-like H α profile. Two possible scenarios are discussed. We also find strong splitting in the s-process elements of Ba ii 6141.713- and 6496.898-Å lines, with short-term morphological variations. A Gaussian decomposition of such profiles allows us to distinguish four shell components, two expanding and two infalling toward the central star, which are subject to the orbital motion of the system and are not affected by the long-term instabilities. Finally, we find that the numerous metal lines in emission could originate in regions of a structured circumbinary disc that have sizes proportional to the energy of the corresponding upper level transition Eup. This study demonstrates the potential of long-term high-resolution spectroscopy in linking together the instability processes occurring during the late evolutionary stages of post-AGBs and the subsequent phase of PNe.
ABSTRACT
In this paper, we present a detailed revision of the orbital parameters and the first quantitative abundance analysis of the spectroscopic triple system HD 226766. By means of a simultaneous ...fit of the radial velocities of all the three components, we derived precise orbital parameters for the system, in particular inner pair has P(d) = 31.9187 ± 0.0001, e = 0.28 ± 0.01, and MA/MB = 1.03 ± 0.03, while the C component orbits around the inner pair with a period of P(d) = 1615 ± 59 in a very eccentric orbit (e = 0.54 ± 0.11). From the fit of the Hβ and Hα profiles, we determined the effective temperatures and surface gravities of each component of the inner pair: Teff = 8600 ± 500 K and log g = 3.8 ± 0.2 for HD 226766 A and Teff = 8500 ± 400 K and log g = 4.0 ± 0.2 for HD 226766 B. In the hypothesis that component C is a main sequence star (log g = 4.0) we derived Teff = 8000 ± 500 K. Rotational velocities have been estimated by modeling the profiles of metallic lines: v sin i = 13 ± 1 km s−1 for inner pair and v sin i = 150 ± 20 km s−1 for the C component. We find that the inner pair is heterogeneous from the point of view of the chemical composition: both stars are very similar and show chemical anomalies typical of Am stars. With some hypothesis about the masses of the components, we estimated the orbital inclination angle for the inner binary, i = (47 ± 1)○, and for the outer orbit, i = (54 ± 19)○.
Montasio is a typical protected designation of origin (PDO) Italian semi-hard and semi-cooked cheese produced in northeast Italy from raw or thermized cow’s milk. The PDO label implies that the ...product has distinctive characteristics that are connected to traditional production methods. The aim of this work was to precisely characterize the volatile fraction of this Italian cheese. The volatile profile can be considered a fingerprint because the flavor of a cheese variety is the result of a specific balance between the volatile compounds produced during the ripening process. Analysis of the volatile profile of Montasio cheese was performed by solid-phase microextraction–gas chromatography. Six cheesemaking trials were performed, each in a different dairy located within the Montasio cheese production area. Cheeses were analyzed at 5 stages of ripening (60, 90, 170, 300, and 365 d). Only 11 compounds were identified and measured: 5 fatty acids, 3 alcohols, 2 ketones, and 1 ester. The limited number of volatile compounds measured in the headspace of the Montasio cheese is probably due to the specific making process of this cheese, which affects evolution of the microflora and the biochemical processes of ripening. The total volatile fraction profile progressively increased from 60 to 170 d, after which time it remained almost steady. The most important contributors were found to be ethanol, short-chain fatty acids (C2 to C6), diacetyl, and ethyl hexanoate. Ethanol and short-chain fatty acids increased up to 170 d, diacetyl increased up to 300 d and then declined, and ethyl hexanoate increased until the final stage.
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