542 research outputs found
Current Research in Egyptology 2017. Proceedings of the Eighteenth Annual Symposium, University of Naples, “L’Orientale” 3-6 May 2017
No full textA new asphalt binder parameter to predict asphalt concrete fatigue behavior
No full textSubmission published under a 24 month embargo labeled 'Closed Access', the embargo will last until 2022-12-01The student, Javier Garcia Mainieri, accepted the attached license on 2020-12-09 at 18:41.The student, Javier Garcia Mainieri, submitted this Thesis for approval on 2020-12-09 at 19:07.This Thesis was approved for publication on 2020-12-10 at 16:55.DSpace SAF Submission Ingestion Package generated from Vireo submission #16111 on 2021-03-04 at 16:33:54Made available in DSpace on 2021-03-05T21:47:36Z (GMT). No. of bitstreams: 2
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Disorders of arousal in 4 older men: evidence from clinical practice
No full textSTUDY OBJECTIVES: To describe clinical and video-polysomnographic features of disorders of arousal (DoA) in older adults. METHODS: Four consecutive male patients with nocturnal motor behaviors underwent a clinical interview, neurologic examination, laboratory tests, brain magnetic resonance imaging, and nocturnal in-laboratory or 24- to 48-hour home video polysomnography. The patients repeated an evaluation after 6 months of follow-up, including a 48-hour home video polysomnography in 2 patients. RESULTS: The patients were aged 65-72 years, and 1 patient has Parkinson disease. Sleep-related behavioral episodes had begun from 12-55 years before our observation. Three patients presented with a positive family history for DoA. Sleep motor episodes were described as suddenly raising the head or trunk, sitting in bed, screaming, speaking, gesturing, and sleepwalking (in 1 patient). When questioned, all patients seemed confused, rarely reporting any dream-like content. We recorded 25 DoA episodes of different intensity and complexity arising from nonrapid eye movement sleep. The semiology of the episodes was similar to that described in younger patients, consisting of sleep terrors and confusional arousals. All patients presented with physiological rapid eye movement sleep muscle atonia. Medication therapy reduced the frequency of the episodes in 2/4 patients. CONCLUSIONS: DoA may begin in adulthood and persist or arise in older adults, sometimes causing sleep-related injuries. Motor patterns of DoA in older adults are similar to those of younger patients. A combined clinical examination and video polysomnography recording are crucial in establishing a definitive diagnosis of nocturnal motor behavior in all older adults and especially in those affected by neurodegenerative diseases. CITATION: Loddo G, Fragiacomo F, Mainieri G, et al. Disorders of arousal in 4 older men: evidence from clinical practice. J Clin Sleep Med. 2022;18(1):129-136
K-s-band luminosity function of the z=1.237 cluster of galaxies RDCS J1252.9-2927
No full textUsing deep VLT/ISAAC near-infrared imaging data, we derive the K-s-band luminosity function (LF) of the z = 1.237 massive X-ray luminous cluster of galaxies RDCS J1252.9-2927. Photometric redshifts, derived from deep multiwavelength BVRIzJK(s) data, and calibrated using a large subset of galaxies with spectroscopic redshifts, are used to separate the cluster galaxy population from the foreground and background field galaxy population. This allows for a simultaneous determination of the characteristic magnitude K-s* and faint end slope alpha of the LF without having to make an uncertain statistical background subtraction. The derived LF is well represented by the Schechter function with K-s* = 18.54(-0.55)(+0.45) and alpha = -0.64(-0.25)(+0.27) The shape of the bright end of the derived LF is similar to that measured at similar restframe wavelengths (in the z-band) in local clusters, but the characteristic magnitude is brighter by DeltaM(z)* 1.40(-0.58)(+0.49) mag. The derived a is similar to the value derived in the K-s-band in the z = 1 cluster of galaxies MG2016+112 but is shallower (at the 2.2sigma level) than the value measured at similar restframe wavelength (in the z-band) in clusters in the local universe. The brightening of the characteristic magnitude and lack of evolution in the shape of the bright end of the LF suggests that the massive cluster ellipticals that dominate the bright end of the LF were already in place at z = 1.237, while the flattening of the faint end slope suggest that clusters at z similar to 1 contains relatively smaller fractions of low mass galaxies than clusters in the local universe. The results presented in this paper are a challenge for semi analytical hierarchical models of galaxy formation which predict the characteristic magnitude to grow fainter and the faint end slope to steepen with redshift as the massive galaxies break up into their progenitors. The observed evolution is consistent with a scenario in which clusters are composed of a population of massive galaxies which formed at high redshift (z much greater than 1) and subsequently evolved passively, and a population of lower mass galaxies which are gradually accreted from the field, primarily at lower redshift (z < 1)
Iron Abundance in the Intracluster Medium at High Redshift
No full textWe present the analysis of the X-ray spectra of 18 distant clusters of galaxies with redshift 0.3 1 clusters, we also use deep XMM-Newton observations. Overall, these clusters probe the temperature range 3 keV less than or similar to kT less than or similar to 8 keV. Our analysis is aimed at deriving the iron abundance in the intracluster medium (ICM) out to the highest redshifts probed to date. Using a combined spectral fit of cluster sub-samples in different redshift bins, we investigate the evolution of the mean ICM metallicity with cosmic epoch. We find that the mean Fe abundance at [z] = 0.8 is Z = 0.25(-0.06)(+0.04) Z., consistent with the local canonical metallicity value, Z similar or equal to 0.3 Z., within the 1 sigma confidence level (c.l.). Medium- and low-temperature clusters (kT 1), we obtain a statistically significant detection of the Fe K line in only one cluster (Z > 0.10 Z. at the 90% c.l.). Combining all the current data sets from Chandra and XMM at z > 1, the average metallicity is measured to be [Z] = 0.21(-0.05)(+0.10) Z. (1 sigma error), thus suggesting no evolution of the mean iron abundance out to z similar or equal to 1.2
Deep near-infrared imaging of RDCS J1252.9-2927 at z=1.237 - The colour-magnitude diagram
No full textWe present deep Soil and ISAAC near-infrared imaging data of the X-ray luminous galaxy cluster RDCS J1252.9-2927. The ISAAC data were taken at the ESO Very Large Telescope under very good seeing conditions and reach limiting Vega magnitudes of 25.6 and 24.1 in the J- and K-s-bands respectively. The image quality is 0".45 in both passbands. We use these data to construct a colour-magnitude (C-M) diagram of galaxies that are within 20" of the Cluster center and brighter than K-s = 24, which is five magnitudes fainter than the apparent magnitude of a L* galaxy in this cluster. The C-M relation is clearly identified as an over-density of galaxies with colours near J - K-s = 1.85. The slope of the relation is -0.05 +/- 0.02 and the intrinsic scatter is 0.06 mag with a 90% confidence interval that extends from 0.04 to 0.09 mag. Both the slope and the scatter are consistent with the values measured for Clusters at lower redshifts. These quantities have not evolved from z = 0 to z = 1.24. However, significant evolution in the mean J - K-s colour is detected. On average, the galaxies in RDCS J1252.9-2927 are 0.25 mag bluer than early-type galaxies in the Coma cluster. Using instantaneous single-burst solar-metallicity models. the average age of galaxies in the center of RDCS J1252.9-2927 is 2.7 Gyrs
"The Borgia collection of Egyptian antiquities: cataloguing as a method"
No full textThe Borgia collection of Egyptian antiquities is one of the two main groups that constitute the Egyptian Collection of the National Archaeological Museum of Naples (MANN). The collection, sold by Camillo Borgia to Joachim Murat in 1815, however, is mainly linked to Cardinal Stefano Borgia (Camillo ‘s uncle) and the Danish scholar Georg Zoëga, who studied and catalogued it.
The scientific accuracy of Zoëga, motivated by the idea that we must present monuments for themselves and for their own contents and not according to individual taste and personal purposes, led him to develop a cataloguing system that made him a pioneer of a highly modern method for studying archaeological materials.
As part of a PhD project on the Egyptian collection of MANN, among whose main objectives is also a new exhibition proposal, consultation of archival documents - and especially of the original writings by Zoëga - is providing fundamental information about the nature and origin of some materials, as well as about their history in the context of European collectors in the late 18th and 19th centuries
Tracing the evolution in the iron content of the intra-cluster medium
No full textContext. We present a Chandra analysis of the X-ray spectra of 56 clusters of galaxies at z greater than or similar to 0.3, which cover a temperature range of 3 less than or similar to kT less than or similar to 15 keV. Aims. Our analysis is aimed at measuring the iron abundance in the intra-cluster medium (ICM) out to the highest redshift probed to date. Methods. We made use of combined spectral analysis performed over five redshift bins at 0.3 less than or similar to z less than or similar to 1.3 to estimate the average emission weighted iron abundance. We applied non-parametric statistics to assess correlations between temperature, metallicity, and redshift. Results. We find that the emission-weighted iron abundance measured within (0.15-0.3) R-vir in clusters below 5 keV is, on average, a factor of similar to 2 higher than in hotter clusters, following Z(T) similar or equal to 0.88 T-0.47 Z(circle dot), which confirms the trend seen in local samples. We also find a constant average iron abundance Z(Fe) similar or equal to 0.25 Z(circle dot) as a function of redshift, but only for clusters at z greater than or similar to 0.5. The emission-weighted iron abundance is significantly higher (Z(Fe) similar or equal to 0.4 Z(circle dot)) in the redshift range z similar or equal to 0.3-0.5, approaching the value measured locally in the inner 0.15 R-vir radii for a mix of cool-core and non cool-core clusters in the redshift range 0.1 less than or similar to z less than or similar to 0.3. The decrease in metallicity with redshift can be parametrized by a power law of the form similar to(1 + z)(-1.25). We tested our results against selection effects and the possible evolution in the occurrence of metallicity and temperature gradients in our sample, and we do not find any evidence of a significant bias associated to these effects. Conclusions. The observed evolution implies that the average iron content of the ICM at the present epoch is a factor of similar to 2 larger than at z similar or equal to 1.2. We confirm that the ICM is already significantly enriched (ZFe similar or equal to 0.25 Z(circle dot)) at a look-back time of 9 Gyr. Our data provide significant constraints on the time scales and physical processes that drive the chemical enrichment of the ICM
The correlation of narrow line emission and X-ray luminosity in active galactic nuclei
No full textAims.We combine emission line and X-ray luminosities for 45 sources
from the Chandra Deep Field South (CDF-S), and seven
HELLAS sources, to obtain a new sample of 52 X-ray selected
type-II active galactic nuclei (AGNs). Eighteen of our sources are very luminous with a typical,
absorption-corrected 2–10 keV luminosity of erg s-1 (type-II QSOs).
Methods.
We compare the emission line properties of the new sources
with emission line and X-ray luminosities of known low redshift, mostly lower luminosity AGNs
by using a composite spectrum.
Results.
We find that / and / decrease with L(2–10 keV) such that
/ .
The trend was already evident, yet neglected in past low redshift samples.
This lead to erroneous calibration of the line-to-X-ray luminosity in earlier AGN samples.
The analysis of several type-I samples shows the same trend with a similar slope
but a median / which is larger by a factor of about two compared with optically selected
type-II samples. We interpret this shift as due to additional reddening
in type-II sources and comment in general on the very large extinction in many type-II objects
and the significantly smaller average reddening of the SDSS type-II AGNs.
The decrease of / with L(2–10 keV) is
large enough to suggest that a significant fraction of high luminosity
high redshift type-II AGNs have very weak emission lines that may have
escaped detection in large samples. A related decrease of EW([O ii
Two-face(s): ionized and neutral gas winds in the local Universe
No full textWe present a comprehensive study of the Na I λ5890, 5895 (Na I D) resonant lines in the Sloan Digital Sky Survey (SDSS, DR7) spectroscopic sample to look for neutral gas outflows in the local galaxies. Individual galaxy spectra are stacked in bins of stellar mass (M⋆) and star formation rate (SFR) to investigate the dependence of galactic wind occurrence and velocity as a function of the galaxy position in the SFR-M⋆ plane. While in most cases the interstellar medium (ISM) absorption and emission lines are at the galaxy systemic velocity, in massive galaxies (M⋆ > 5 × M☉) at the high SFR tail (SFR > 10-12 M☉ yr-1) we find evidence of a significant blue-shifted Na I D absorption, which we interpret as evidence of neutral outflowing gas. The occurrence of the blue-shifted absorption in the stacked spectra does not depend on the contribution of the nuclear activity as it is observed at the same significance for purely star-forming (SF) galaxies, active galactic nuclei (AGN), and composite systems at fixed SFR. We confirm, instead, for all classes of objects a clear dependence on the galaxy disc inclination: the blueshift is the largest and the Na I D equivalent width the smallest for face-on galaxies, while the absorption feature is at the systemic velocity for edge-on systems. This indicates that the neutral outflow is mostly perpendicular or biconical with respect to the galactic disc. We also compare the kinematics of the neutral gas with the ionized gas phase as traced by the [OIII]λ5007, Hα, [NII]λ6548, and [NII]λ6584 emission lines in the same galaxy spectra. Differently for the neutral gas phase, all the emission lines show evidence of perturbed kinematics only in galaxies with a significant level of nuclear activity, and they are independent of the galactic disc inclination. This would suggest that, while neutral winds originate from the galactic disc and are powered by SF feedback, ionized outflows are instead due to AGN feedback originating from the black hole accretion disc. In both the neutral and ionized gas phases, the observed wind velocities (of the order of 100-200 kms-1) suggest that the outflowing gas remains bound to the galaxy with no definitive effect on the gas reservoir
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