Search

The Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) will observe several Deep Drilling Fields (DDFs) to a greater depth and with a more rapid cadence than the main survey. In this paper, we describe the 'DeepDrill' survey, which used the Spitzer Space Telescope Infrared Array Camera (IRAC) to observe three of the four currently defined DDFs in two bands, centred on 3.6 and 4.5 μm. These observations expand the area that was covered by an earlier set of observations in these three fields by the Spitzer Extragalactic Representative Volume Survey (SERVS). The combined DeepDrill and SERVS data cover the footprints of the LSST DDFs in the Extended Chandra Deep Field-South (ECDFS) field, the ELAIS-S1 field (ES1), and the XMM-Large-Scale Structure Survey field (XMM-LSS). The observations reach an approximate 5σ point-source depth of 2 μJy (corresponding to an AB magnitude of 23.1; sufficient to detect a 1011 M⊙ galaxy out to z ≈ 5) in each of the two bands over a total area of ≈ 29 deg2. The dual-band catalogues contain a total of 2.35 million sources. In this paper, we describe the observations and data products from the survey, and an overview of the properties of galaxies in the survey. We compare the source counts to predictions from the Shark semi-analytic model of galaxy formation. We also identify a population of sources with extremely red ([3.6]-[4.5] >1.2) colours which we show mostly consists of highly obscured active galactic nuclei.

Chandra data in the COSMOS, AEGIS-XD and 4 Ms Chandra Deep Field South are combined with multiwavelength photometry available in those fields to determine the rest-frame U-V versus V-J colours of X-ray AGN hosts in the redshift intervals 0.1 < z < 0.6 (mean z = 0.40) and 0.6 < z < 1.2 (mean z = 0.85). This combination of colours provides an effective and least model-dependent means of separating quiescent from star-forming, including dust reddened, galaxies. Morphological information emphasizes differences between AGN populations split by their U-V versus V-J colours. AGN in quiescent galaxies consist almost exclusively of bulges, while star-forming hosts are equally split between early-and late-type hosts. The position of AGN hosts on the U-V versus V-J diagram is then used to set limits on the accretion density of the Universe associated with evolved and star-forming systems independent of dust induced biases. It is found that most of the black hole growth at z ̃0.40 and 0.85 is associated with star-forming hosts. Nevertheless, a non-negligible fraction of the X-ray luminosity density, about 15-20 per cent, at both z = 0.40 and 0.85, is taking place in galaxies in the quiescent region of the U-V versus V-J diagram. For the low-redshift sub-sample, 0.1 < z < 0.6, we also find tentative evidence, significant at the 2σ level, that AGN split by their U-V and V-J colours have different Eddington ratio distributions. AGN in blue star-forming hosts dominate at relatively high Eddington ratios. In contrast, AGN in red quiescent hosts become increasingly important as a fraction of the total population towards low Eddington ratios. At higher redshift,z > 0.6, such differences are significant at the 2σ level only for sources with Eddington ratios ≥10-3. These findings are consistent with scenarios in which diverse accretion modes are responsible for the build-up of supermassive black holes at the centres of galaxies.We compare these results with the predictions of the GALFORM semi-analytic model for the cosmological evolution of AGN and galaxies. This model postulates two black hole fuelling modes, the first is linked to star formation events and the second takes place in passive galaxies. GALFORM predicts that a substantial fraction of the black hole growth at z < 1 is associated with quiescent galaxies, in apparent conflict with the observations. Relaxing the strong assumption of the model that passive AGN hosts have zero star formation rate could bring those predictions in better agreement with the data. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Chandra data in the COSMOS, AEGIS-XD and 4 Ms Chandra Deep Field South are combined with multiwavelength photometry available in those fields to determine the rest-frame U-V versus V-J colours of X-ray AGN hosts in the redshift intervals 0.1 < z < 0.6 (mean z = 0.40) and 0.6 < z < 1.2 (mean z = 0.85). This combination of colours provides an effective and least model-dependent means of separating quiescent from star-forming, including dust reddened, galaxies. Morphological information emphasizes differences between AGN populations split by their U-V versus V-J colours. AGN in quiescent galaxies consist almost exclusively of bulges, while star-forming hosts are equally split between early-and late-type hosts. The position of AGN hosts on the U-V versus V-J diagram is then used to set limits on the accretion density of the Universe associated with evolved and star-forming systems independent of dust induced biases. It is found that most of the black hole growth at z ̃0.40 and 0.85 is associated with star-forming hosts. Nevertheless, a non-negligible fraction of the X-ray luminosity density, about 15-20 per cent, at both z = 0.40 and 0.85, is taking place in galaxies in the quiescent region of the U-V versus V-J diagram. For the low-redshift sub-sample, 0.1 < z < 0.6, we also find tentative evidence, significant at the 2σ level, that AGN split by their U-V and V-J colours have different Eddington ratio distributions. AGN in blue star-forming hosts dominate at relatively high Eddington ratios. In contrast, AGN in red quiescent hosts become increasingly important as a fraction of the total population towards low Eddington ratios. At higher redshift,z > 0.6, such differences are significant at the 2σ level only for sources with Eddington ratios ≥10-3. These findings are consistent with scenarios in which diverse accretion modes are responsible for the build-up of supermassive black holes at the centres of galaxies.We compare these results with the predictions of the GALFORM semi-analytic model for the cosmological evolution of AGN and galaxies. This model postulates two black hole fuelling modes, the first is linked to star formation events and the second takes place in passive galaxies. GALFORM predicts that a substantial fraction of the black hole growth at z < 1 is associated with quiescent galaxies, in apparent conflict with the observations. Relaxing the strong assumption of the model that passive AGN hosts have zero star formation rate could bring those predictions in better agreement with the data. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Copyright of Brazilian Journal of Biology is the property of Instituto Internacional de Ecologia and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Copyright of Brazilian Journal of Biology is the property of Instituto Internacional de Ecologia and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

The Atacama Large Millimetre/submillimetre Array (ALMA) is the world's most advanced radio interferometric facility, producing science data with an average rate of about 1 TB per day. After a process of calibration, imaging and quality assurance, the scientific data are stored in the ALMA Science Archive (ASA), along with the corresponding raw data, making the ASA an invaluable resource for original astronomical research. Due to their complexity, each ALMA data set has the potential for scientific results that go well beyond the ideas behind the original proposal that led to each observation. For this reason, the European ALMA Regional Centre initiated the High-Level Data Products initiative to develop science-oriented data products derived from data sets publicly available in the ASA, that go beyond the formal ALMA deliverables. The first instance of this initiative is the creation of a catalogue of submillimetre (submm) detections of Sloan Digital Sky Survey (SDSS) quasars from the SDSS Data Release 14 that lie in the aggregate ALMA footprint observed since ALMA Cycle 0. The ALMA fluxes are extracted in an automatic fashion, using the ALMA Data Mining Toolkit. All extractions above a signal-to-noise cut of 3.5 are considered, they have been visually inspected and the reliable detections are presented in a catalogue of 376 entries, corresponding to 275 unique quasars. Interesting targets found in the process, i.e. lensed or jetted quasars as well as quasars with nearby submm counterparts are highlighted, to facilitate further studies or potential follow up observations. [ABSTRACT FROM AUTHOR]

Copyright of Brazilian Journal of Biology is the property of Instituto Internacional de Ecologia and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Historically, GHz radio emission has been used extensively to characterize the star-formation activity in galaxies. In this work, we look for empirical relationships amongst the radio luminosity, the infrared luminosity, and the CO-based molecular gas mass. We assemble a sample of 278 nearby galaxies with measurements of radio continuum and total infrared emission, and the 12CO J = 1–0 emission line. We find a correlation between the radio continuum and the CO emission line (with a scatter of 0.36 dex), in a large sample of different kinds of galaxies. Making use of this correlation, we explore the evolution of the molecular gas mass function and the cosmological molecular gas mass density in six redshift bins up to z = 1.5. These results agree with previous semi-analytic predictions and direct measurements: the cosmic molecular gas density increases up to z = 1.5. In addition, we find a single plane across five orders of magnitude for the explored luminosities, with a scatter of 0.27 dex. These correlations are sufficiently robust to be used for samples where no CO measurements exist. [ABSTRACT FROM AUTHOR]

Dusty star-forming galaxies (DSFGs) detected at z > 4 provide important examples of the first generations of massive galaxies. However, few examples with spectroscopic confirmation are currently known, with Hershel struggling to detect significant numbers of z > 6 DSFGs. NGP6_D1 is a bright 850 |$\mathrm{ \mu}$| m source (12.3 ± 2.5 mJy) with no counterparts at shorter wavelengths (a SPIRE dropout). Interferometric observations confirm it is a single source, with no evidence for any optical or NIR emission, or nearby likely foreground lensing sources. No >3σ detected lines are seen in both LMT Redshift Search Receiver and IRAM 30 m EMIR spectra of NGP6_D1 across 32 GHz of bandwidth despite reaching detection limits of |$\sim 1\, \mathrm{mJy}/500 \, \mathrm{km~s}^{-1}$|⁠ , so the redshift remains unknown. Template fitting suggests that NGP6_D1 is most likely between z  = 5.8 and 8.3. SED analysis finds that NGP6_D1 is a ULIRG, with a dust mass ∼108–109 M⊙ and a star-formation rate of ∼500 M⊙ yr−1. We place upper limits on the gas mass of NGP6_D1 of M H 2 <(1.1 ± 3.5) × 1011 M⊙, consistent with a gas-to-dust ratio of ∼100–1000. We discuss the nature of NGP6_D1 in the context of the broader sub-mm population, and find that comparable SPIRE dropouts account for ∼20 per cent of all SCUBA-2 detected sources, but with a similar flux density distribution to the general population. [ABSTRACT FROM AUTHOR]

We present Atacama Large Millimeter/submillimeter Array (ALMA) resolved observations of molecular gas in galaxies up to |$z$| = 0.35 to characterize the role of global galactic dynamics on the global interstellar medium properties. These observations consist of a sub-sample of 39 galaxies taken from the Valparaíso ALMA Line Emission Survey (VALES). From the CO(J = 1–0) emission line, we quantify the kinematic parameters by modelling the velocity fields. We find that the infrared (IR) luminosity increases with the rotational to dispersion velocity ratio (V rot/σ |$v$| , corrected for inclination). We find a dependence between V rot/σ |$v$| and the [C ii ]/IR ratio, suggesting that the so-called [C ii ] deficit is related to the dynamical state of the galaxies. We find that global pressure support is needed to reconcile the dynamical mass estimates with the stellar masses in our systems with low V rot/σ |$v$| values. The star formation rate (SFR) is weakly correlated with the molecular gas fraction (⁠|$f_{\rm H_2}$|⁠) in our sample, suggesting that the release of gravitational energy from cold gas may not be the main energy source of the turbulent motions seen in the VALES galaxies. By defining a proxy of the 'star formation efficiency' (SFE) parameter as the SFR divided by the CO luminosity (SFE′ ≡ SFR/ L |$^{\prime }_{\rm CO}$|⁠), we find a constant SFE′ per crossing time (t cross). We suggest that t crossmay be the controlling time-scale in which the star formation occurs in dusty |$z$| ∼ 0.03–0.35 galaxies. [ABSTRACT FROM AUTHOR]

Context. Dust and its emission is increasingly being used to constrain the evolutionary stage of a galaxy. A comprehensive characterization of dust, best achieved in nearby bright galaxies, is thus a highly useful resource. Aims. We aim to characterize the relationship between dust properties (mass, luminosity, and temperature) and their relationships with galaxy-wide properties (stellar, atomic, and molecular gas mass, and star formation mode). We also aim to provide equations to accurately estimate dust properties from limited observational datasets. Methods. We assemble a sample of 1630 nearby (z < 0:1) galaxies - over a large range of stellar masses (M*), star formation rates (SFR) and specific star formation rates (sSFR = SFR/M*) - for which comprehensive and uniform multi-wavelength observations are available from WISE, IRAS, Planck, and/or SCUBA. The characterization of dust emission comes from spectral energy distribution (SED) fitting using Draine & Li (2007, ApJ, 657, 810) dust models, which we parametrize using two components (warm at 45-70 K and cold at 18-31 K). The subsample of these galaxies with global measurements of CO and/or HI are used to explore the molecular and/or atomic gas content of the galaxies. Results. The total infrared luminosity (LIR), dust mass (Mdust), and dust temperature of the cold component (Tcold) form a plane that we refer to as the dust plane. A galaxy's sSFR drives its position on the dust plane: starburst (high sSFR) galaxies show higher LIR, Mdust, and Tcold compared to main sequence (typical sSFR) and passive galaxies (low sSFR). Starburst galaxies also show higher specific dust masses (Mdust/M*) and specific gas masses (Mgas/M*). We confirm earlier findings of an anti-correlation between the dust to stellar mass ratio and M*. We also find different anti-correlations depending on sSFR; the anti-correlation becomes stronger as the sSFR increases, with the spread due to different cold dust temperatures. The dust mass is more closely correlated with the total gas mass (atomic plus molecular) than with the individual atomic and molecular gas masses. Our comprehensive multiwavelength data allows us to define several equations to accurately estimate LIR, Mdust, and Tcold from one or two monochromatic luminosities in the infrared and/or sub-millimeter. Conclusions. It is possible to estimate the dust mass and infrared luminosity from a single monochromatic luminosity within the Rayleigh-Jeans tail of the dust emission, with errors of 0.12 and 0.20 dex, respectively. These errors are reduced to 0.05 and 0.10 dex, respectively, if the dust temperature of the cold component is used. The dust mass is better correlated with the total ISM mass (MISM ∝ Mdust 0:7). For galaxies with stellar masses 8.5 < log(M*/M⊙) < 11.9, the conversion factor between the single monochromatic luminosity at 850 μm and the total ISM mass (α850 μm) shows a large scatter (rms = 0.29 dex) and a weak correlation with the LIR. The star formation mode of a galaxy shows a correlation with both the gas mass and dust mass: the dustiest (high Mdust/M*) galaxies are gas-rich and show the highest SFRs. [ABSTRACT FROM AUTHOR]

Aims. This work addresses the AGN IR-selection dependency on intrinsic source luminosity and obscuration, in order to identify and characterise biases that could affect conclusions in studies. Methods. We study IR-selected AGN in the Chandra Deep Field South (CDFS) survey and in the Cosmological Survey (COSMOS). The AGN sample is divided into low and high X-ray luminosity classes and into unobscured (type-1) and obscured (type-2) classes by means of X-ray and optical spectroscopy data. Specifically in the X-ray regime, we adopt the intrinsic luminosity taking the estimated column density (NH) into account. We also take the opportunity to highlight important differences resulting from adopting different methods of assessing AGN obscuration. Results. In agreement with previous studies, we also find that AGN IR-selection efficiency shows a decrease with decreasing source AGN X-ray luminosity. For the intermediate-luminosity AGN population (43.3 <≲ log(LX [erg s-1]) <≲ 44), the efficiency also worsens with increasing obscuration (NH). The same sample also shows an evolution with cosmic time of the obscured fraction at the highest X-ray luminosities, independently of the adopted type-1/type-2 classification method. Conclusions. We confirm that AGN IR-selection is genuinely biased towards unobscured AGNe, but only at intermediate luminosities. At the highest luminosities, where AGN IR-selection is more efficient, there is no obscuration bias. We show that type-1 AGNe are intrinsically more luminous than type-2 AGNe only at z <≲ 1.6, thus resulting in more type-1 AGN being selected when the IR survey is shallower. Based on this and other studies, we conclude that deep hard-X-ray coverages, high-resolution IR imaging, or a combination of IR and radio data are required to recover the lower luminosity obscured AGN population. In addition, wide IR surveys are needed to recover the rare powerful, obscured AGN population. Finally, when the James Webb Space Telescope comes online, the broad-band filters 2.0 μm, 4.4 μm, 7.7 μm, and 18 μm will be essential for disentangling AGN from non-AGN dominated SEDs at depths where spectroscopy becomes impractical. [ABSTRACT FROM AUTHOR]

We study the contribution of hot-dust to the luminosity density of galaxies and its evolution with cosmic time. Using the Spitzer-IRAC data over an area of 1.8 deg2 covered by the Cosmic Evolution Survey (COSMOS) field, we estimate the contribution from hot-dust at rest-frame 4.2 μm (from 0 ≲ z ≲ 0.2 up to 0.5 ≲ z ≲ 0.9). This wavelength corresponds to blackbody temperature of ∼690 K. The contribution of stellar emission is estimated from the rest-frame 1.6 μm luminosity (assumed to result from stellar emission alone) and subtracted from the mid-infrared luminosity of galaxies to measure hot-dust emission. To attempt the study of the 3.3 μm polycyclic aromatic hydrocarbon (PAH) feature, we use the rest-frame 4.2 μm to infer the hot-dust flux at 3.3 μm. This study is performed for different spectral types of galaxies: early-type, late-type, starburst, and IR-selected active galactic nuclei (AGNs). We find that (1) the decrease of the hot-dust luminosity density since 0.5 ≲ z ≲ 1 is steeper (by at least 0.5 dex) compared with that of the cold-dust, giving support to the scenario where galaxy obscuration increases with redshift, as proposed in the literature; (2) hot-dust and PAH emission evolution seems to be correlated with stellar mass, where rest-frame 1.6 μm luminous non-AGN galaxies (i.e., massive systems) show a stronger decrement (with decreasing redshift) in hot-dust and PAH emission than the less luminous (less massive) non-AGN galaxies; (3) despite comprising ≲ 3% of the total sample, AGN contribute as much as a third to the hot-dust luminosity density at z < 1 and clearly dominate the bright-end of the total hot-dust luminosity density function at 0.5 ≲ z ≲ 0.9; (4) the average dust-to-total luminosity ratio increases with redshift, while PAH-to-total luminosity ratio remains fairly constant; (5) at M1.6 > –25, the dust-to-total and PAH-to-total luminosity ratios increase with decreasing luminosity, but deeper data are required to confirm this result. Future study is necessary to further enlighten the characterization of the different spectral components at play in 2-5 μm spectral regime. [ABSTRACT FROM AUTHOR]

Ultra steep spectrum (USS) radio sources have been successfully used to select powerful radio sources at high redshifts (z ≳ 2). Typically restricted to large-sky surveys and relatively bright radio flux densities, it has gradually become possible to extend the USS search to sub-mJy levels, thanks to the recent appearance of sensitive low-frequency radio facilities. Here a first detailed analysis of the nature of the faintest USS sources is presented. By using Giant Metrewave Radio Telescope and Very Large Array radio observations of the Lockman Hole at 610 MHz and 1.4 GHz, a sample of 58 USS sources, with 610 MHz integrated fluxes above 100 µJy, is assembled. Deep infrared data at 3.6 and 4.5 µm from the Spitzer Extragalactic Representative Volunte Survey (SERVS) are used to reliably identify counterparts for 48 (83%) of these sources, showing an average total magnitude of [3.6]AB = 19.8 mag. Spectroscopic redshifts for 14 USS sources, together with photometric redshift estimates, improved by the use of the deep SERVS data, for a further 19 objects, show redshifts ranging from z = 0.1 to z = 2.8, peaking at z ~ 0.6 and tailing off at high redshifts. The remaining 25 USS sources, with no redshift estimate, include the faintest 13.61 magnitudes, with 10 sources undetected at 3.6 and 4.5 µm (typically [3.6] ≳ 22-23 mag from local measurements), which suggests the likely existence of higher redshifts among the sub-mJy USS population. The comparison with the Square Kilometre Array Design Studies Simulated Skies models indicates that Fanaroff-Riley type I radio sources and radio-quiet active galactic nuclei may constitute the bulk of the faintest USS population, and raises the possibility that the high efficiency of the USS technique for the selection of high-redshift sources remains even at the sub-mJy level. [ABSTRACT FROM AUTHOR]

It is widely accepted that observations at mid-infrared (mid-IR) wavelengths enable the selection of galaxies with nuclear activity, which may not be revealed even in the deepest X-ray surveys. Many mid-IR color-color criteria have been explored to accomplish this goal and tested thoroughly in the literature. Besides missing many low-luminosity active galactic nuclei (AGNs), one of the main conclusions is that, with increasing redshift, the contamination by non-active galaxies becomes significant (especially at z ≳ 2.5). This is problematic for the study of the AGN phenomenon in the early universe, the main goal of many of the current and future deep extragalactic surveys. In this work new near- and mid-IR color diagnostics are explored, aiming for improved efficiency—better completeness and less contamination—in selecting AGNs out to very high redshifts. We restrict our study to the James Webb Space Telescope wavelength range (0.6-27 μm). The criteria are created based on the predictions by state-of-the-art galaxy and AGN templates covering a wide variety of galaxy properties, and tested against control samples with deep multi-wavelength coverage (ranging from the X-rays to radio frequencies). We show that the colors Ks – [4.5], [4.5] – [8.0], and [8.0] – [24] are ideal as AGN/non-AGN diagnostics at, respectively, z ≲ 1, 1 ≲ z ≲ 2.5, and z ≳ 2.5-3. However, when the source redshift is unknown, these colors should be combined. We thus develop an improved IR criterion (using Ks and IRAC bands, KI) as a new alternative at z ≲ 2.5. KI does not show improved completeness (50%-60% overall) in comparison to commonly used Infrared Array Camera (IRAC) based AGN criteria, but is less affected by non-AGN contamination (revealing a >50%-90% level of successful AGN selection). We also propose KIM (using Ks, IRAC, and MIPS 24 μm bands, KIM), which aims to select AGN hosts from local distances to as far back as the end of reionization (0 < z ≲ 7) with reduced non-AGN contamination. However, the necessary testing constraints and the small control-sample sizes prevent the confirmation of its improved efficiency at z ≳ 2.5. Overall, KIM shows a ∼30%-40% completeness and a >70%-90% level of successful AGN selection. KI and KIM are built to be reliable against a ∼10%-20% error in flux, are based on existing filters, and are suitable for immediate use. [ABSTRACT FROM AUTHOR]

Historically, GHz radio emission has been used extensively to characterize the star-formation activity in galaxies. In this work, we look for empirical relationships amongst the radio luminosity, the infrared luminosity, and the CO-based molecular gas mass. We assemble a sample of 278 nearby galaxies with measurements of radio continuum and total infrared emission, and the 12CO J = 1–0 emission line. We find a correlation between the radio continuum and the CO emission line (with a scatter of 0.36 dex), in a large sample of different kinds of galaxies. Making use of this correlation, we explore the evolution of the molecular gas mass function and the cosmological molecular gas mass density in six redshift bins up to z = 1.5. These results agree with previous semi-analytic predictions and direct measurements: the cosmic molecular gas density increases up to z = 1.5. In addition, we find a single plane across five orders of magnitude for the explored luminosities, with a scatter of 0.27 dex. These correlations are sufficiently robust to be used for samples where no CO measurements exist. [ABSTRACT FROM AUTHOR]

Spindle epithelial tumor with thymus-like element should be included in the differential diagnosis of thyroid gland cancers, particularly in medullary carcinoma, younger patients and indolent clinical presentation, because it may influence treatment and prognosis., Competing Interests: The authors declare to have no conflicts of interest in connection with this scientific work., (© 2024 The Author(s). Clinical Case Reports published by John Wiley & Sons Ltd.)

The World Health Organization (WHO) declared an international state of emergency in order to contain the rapid spread of COVID-19. To ensure that there is adherence to preventive measures by the population aimed at controlling the pandemic in Alagoas, it is expected that knowledge, behavior and practices play an important role in preventing and controlling the disease. In this sense, it becomes relevant to understand the knowledge of the population about the disease. To evaluate the knowledge, behavior and practices of social media users during social isolation to prevent the transmission of the SARS-CoV-2 in the state of Alagoas, Northeast, Brazil. A probabilistic sample was carried out across the entire territory of the state of Alagoas with those who have access to a device that accesses the internet and a cross-sectional study was carried out using an online questionnaire applied to a convenience sample, recruited between August 2021 and July 2022 by snowball sampling. The questionnaire consisted of seven sessions, the first collecting data on the socioeconomic and sociodemographic profile of the participants, and the other sessions involving knowledge, attitudes and practices, including topics related to the vaccination that had to be administered at that time. High popular knowledge about signs and symptoms, means of transmission and risk groups. Low knowledge about seeking health services. Based on the results obtained, information from official channels became relevant to better teach the population in order to reduce the impact of COVID-19.

Key Clinical Message: This rare diagnosis highlights the importance of anatomical and embryological knowledge in the differential diagnosis of neck masses., Abstract: A 41-year-old woman was referred to the head and neck surgery department because of a large midline neck mass at the level of the hyoid bone that was diagnostic for functioning thyroid tissue in a totally ectopic location., Competing Interests: The authors declare to have no conflicts of interest in connection with this scientific work., (© 2023 The Authors. Clinical Case Reports published by John Wiley & Sons Ltd.)

Papillary thyroid carcinoma (PTC) primarily located in the pyramidal lobe of the thyroid gland is extremely rare, therefore the clinical and pathological features are not well understood. The authors describe a case of PTC of the pyramidal lobe, in a 77-year-old woman who underwent en bloc total thyroidectomy with pyramidal lobe, hyoid bone and cervical lymph node excision. In line with the present case, current literature reports a greater presence of worse prognostic factors, namely extrathyroidal extension, advanced T stage or presence of cervical lymph node metastasis. Recently, a new classification has been suggested-Upper Neck Papillary Thyroid Cancer (UPTC)-which encompasses these carcinomas, Delphi ganglion metastases and thyroglossal duct cyst carcinomas, with potential clinical and therapeutic implications, particularly the need for orthotopic thyroidectomy. Also, the complete excision of the pyramidal lobe during thyroidectomy may influence the success of radioactive iodine therapy and the patient's follow-up surveillance., Competing Interests: The authors declare to have no conflicts of interest in connection with this scientific work., (© 2023 The Authors. Clinical Case Reports published by John Wiley & Sons Ltd.)

The nearby radio galaxy M87 is a prime target for studying black hole accretion and jet formation 1,2 . Event Horizon Telescope observations of M87 in 2017, at a wavelength of 1.3 mm, revealed a ring-like structure, which was interpreted as gravitationally lensed emission around a central black hole 3 . Here we report images of M87 obtained in 2018, at a wavelength of 3.5 mm, showing that the compact radio core is spatially resolved. High-resolution imaging shows a ring-like structure of [Formula: see text] Schwarzschild radii in diameter, approximately 50% larger than that seen at 1.3 mm. The outer edge at 3.5 mm is also larger than that at 1.3 mm. This larger and thicker ring indicates a substantial contribution from the accretion flow with absorption effects, in addition to the gravitationally lensed ring-like emission. The images show that the edge-brightened jet connects to the accretion flow of the black hole. Close to the black hole, the emission profile of the jet-launching region is wider than the expected profile of a black-hole-driven jet, suggesting the possible presence of a wind associated with the accretion flow., (© 2023. The Author(s).)

Background: Cutaneous angiosarcoma (AS) of the head and neck is a rare highly aggressive tumor, often associated with difficult local control of the disease and poor prognosis. This article describes a case of multifocal cutaneous AS of the scalp, mainly addressing its difficult surgical management and challenging reconstruction and concludes with a review of the literature., Methods: A 70-year-old Caucasian male was referred to our hospital with a growing scalp lesion initially suspected to be benign, but later diagnosed with AS., Results: The patient had tumor recurrence and a difficult reconstruction for which dermal substitutes proved very useful., Conclusion: AS can mimic a benign lesion in its early stages. Skin substitutes, namely dermal templates, can be useful to meet the complex needs of reconstruction and oncological surveillance of patients with AS., (© 2022 The Authors. Cancer Reports published by Wiley Periodicals LLC.)

The patency of the vascular access (VA) is a fight for the attending nephrologist. A retrospective observational study was conducted to compare the success rate of surgical versus endovascular technique percutaneous transluminal angioplasty (PTA) for graft thrombosis treatment. Of 3008 patients, 22.1% patients were dialyzed through grafts. Forty-five percent of all prevalent patients referred due to VA malfunction had a graft. For 18 months, 336 thrombosed grafts were submitted to surgery in 228 cases and to PTA in 126. PTA for thrombolysis included the Pharmaco-Mechanical Technique and the Arrow-Trerotola Device. Procedures were performed as outpatient, with an average delay of 1 day. Immediate success was 100% for surgery and 87.3% for PTA. The unassisted patency for thrombosed grafts for surgery/PTA was 265.12 ± 15.30/230.59 ± 19.83 days respectively, favoring surgery. The primary patency for thrombosed grafts treated by surgery/PTA at 30, 90, and 180 days was, respectively, 74.1%/81%, 63.2%/67.5%, and 53.9%/55.6% all in favor of PTA. AV grafts have a much higher rate of thrombosis than fistulas. Graft thrombosis can be dealt either by surgery or PTA, with identical success., (© 2014 Wiley Periodicals, Inc.)

We describe the case of a patient with chronic renal failure under hemodialysis for five years who, after renal transplantation, developed acute renal failure and hypertension refractory to medical therapy. Given the clinical and imaging (renal ultrasound and computed tomography) suspicion of renal artery graft thrombosis, invasive angiography was performed, which confirmed the diagnosis. The therapeutic approach consisted of percutaneous thrombus aspiration and subsequent balloon angioplasty of the entire artery, followed by stent implantation in a second procedure. The clinical course was uneventful with improvement of renal function and normalization of blood pressure. The case highlights the importance of percutaneous intervention in the management of patients with vascular complications after transplantation, with successful application of a procedure normally used in the setting of acute myocardial infarction - percutaneous thrombus aspiration and implantation of a drug-eluting vascular stent., (Copyright © 2011 Sociedade Portuguesa de Cardiologia. Published by Elsevier España. All rights reserved.)

Percutaneous peritoneal dialysis (PD) catheter manipulation successfully corrects displacement and contributes to catheter salvage. We describe a new device for the percutaneous treatment of malpositioned PD catheters, the modified Malecot introducer technique, which is an improvement over previous methods because its flexible consistency also allows the manipulation of swan-neck catheters. Twenty-one patients experienced catheter displacement managed by the new introducer: 12 males, average time in PD 13.7+/-23.2 months, six with "swan-neck" catheter, seven obese, and six with previous abdominal surgery. Catheter manipulation was technically successful in 19 of 21 cases (90.4%) by the end of the first week and in 15 cases (71.4%) at 1 month. An additional eight episodes of malposition occurred ranging from 10 to 300 days after the first manipulation. A second manipulation using the same introducer was performed and resulted in long-term patency in seven patients. No complications were reported. In the long-term follow-up, only one patient removed PD catheter for mechanical dysfunction. Overall survival of manipulated catheters was 32.7+/-23.4 months. Function at 1 month correlated with function by the first week (r=0.513; p=0.017) and the need of a second manipulation with age (r=0.494; p=0.027) but not with obesity or previous abdominal surgery. We conclude that manipulation using the modified Malecot introducer is a simple and effective procedure for the correction of malpositioned PD catheters. It also represents a new alternative for the management of displaced "swan-neck" catheters.

We report the case of a 18-year-old girl having a solid pseudopapillary pancreatic tumor. The patient underwent local enucleation of the tumor located on pancreatic head and remained free of recurrence on the 5th year of follow up. Surgical management is discussed.

Splenic metastasis is rare, and is usually associated with disseminated malignancy. The primary tumours more frequently related with splenic metastasis are lung, breast, gynaecologic, specially ovary tumours, colon, rectum and melanoma. Isolated secondary splenic disease is rare, but it is described, often associated to ovary cancer. We report a 55 years old women with parenchymal splenic metastases of serous ovary cystadenocarcinoma in the 5th follow up year. This patient had positive peritoneal washings chytology but not macroscopic disease. We discuss the secondary splenic involvement of ovary cancer, dissemination route, prognosis and role of splenectomy as treatment modality in this unusual recurrence site in ovary cancers.

We describe a retrospective analysis of 105 patients who underwent day-case laparoscopic cholecystectomy to evaluate the safety of this procedure. Selection criteria included surgical indications and admission/exclusion criteria for day-case surgery. We analysed: causes of overnight stay and readmission, need of medical or nursing care after discharge, degree of patient satisfaction and insatisfaction reasons. This study has demonstrated a low rate of overnight stay and readmission and a high degree of patient satisfaction for this procedure. We concluded that in selected patients, laparoscopic cholecystectomy as a day-case surgery is a safe procedure.

Eighteen hemodialysis patients with the diagnosis of mesenteric ischemia (MI), admitted to the Renal Service in the last 5 years, were retrospectively reviewed. All patients, 10 males and 8 females, average age 66.3 +/- 8.6 years, were complaining of acute abdominal pain without other specific clinical or laboratorial findings, had their diagnosis confirmed during laparatomy, with ischemic involvement of the ileocecal/ascendant colon area in 14 cases and the small bowel in 4. Noteworthy was the high incidence of previous dialysis-induced hypotensive episodes (10/18), the presence of leukocytosis (13/18), the high average hemoglobin level of 9.4 gr/dl, and the constant finding of non-occlusive MI. Average time in-hospital was 15.4 days (2 to 30) and the mortality--88% (16 patients). The growing incidence of MI mostly of the non-occlusive type, and its grim prognosis, calls for an early diagnosis of functional ischemic colitis, and the adoption of preventive action to avoid bowel infarction.