Search

We present the first observational infrared luminosity function (IRLF) measurement in the Epoch of Reionization (EoR) based on a ultraviolet (UV)-selected galaxy sample with the Atacama Large Millimeter Array (ALMA) spectroscopic observations. Our analysis is based on the ALMA large program Reionization Era Bright Emission Line Survey (REBELS), which targets 42 galaxies at z = 6.4–7.7 with [C ii] 158 $\rm{\mu m}$ line scans. 16 sources exhibit dust detection, 15 of which are also spectroscopically confirmed through the [C ii] line. The infrared (IR) luminosities of the sample range from log LIR/L⊙ = 11.4 to 12.2. Using the UV luminosity function as a proxy to derive the effective volume for each of our target sources, we derive IRLF estimates, both for detections and for the full sample including IR luminosity upper limits. The resulting IRLFs are well reproduced by a Schechter function with the characteristic luminosity of $\log L_{*}/\mathrm{ L}_\odot =11.6^{+0.2}_{-0.1}$ . Our observational results are in broad agreement with the average of predicted IRLFs from simulations at z ∼ 7. Conversely, our IRLFs lie significantly below lower redshift estimates, suggesting a rapid evolution from z ∼ 4 to z ∼ 7, into the reionization epoch. The IR obscured contribution to the cosmic star formation rate density at z ∼ 7 amounts to $\mathrm{log(SFRD/{\rm M}_{\odot }\,yr^{-1}\,Mpc^{-3}) = -2.66^{+0.17}_{-0.14} }$ that is at least ∼10 per cent of UV-based estimates. We conclude that the presence of dust is already abundant in the EoR and discuss the possibility of unveiling larger samples of dusty galaxies with future ALMA and JWST observations.

We present a high sensitivity, ground-based spectral line survey of low-J carbon monoxide (CO(Jup → Jup − 1) with Jup = 1, 2, 3) and neutral carbon [CI] 3P1−3P0 ([CI](1–0)) in 36 local ultra-luminous infrared galaxies (ULIRGs) and 4 additional LIRGs, all of which have previous Herschel OH 119 μm observations. The study is based on new single-dish observations conducted with the Atacama Pathfinder Experiment (APEX) and complemented with archival APEX and Atacama Large Millimeter Array (ALMA and ACA) data. Our methods are optimized for a multi-tracer study of the total molecular line emission from these ULIRGs, including any extended low-surface-brightness components. We find a tight correlation between the CO and [CI] line luminosities, which suggests that the emission from CO(1–0) (and CO(2–1)) arises from similar regions as the [CI](1–0), at least when averaged over galactic scales. By using [CI] to compute molecular gas masses, we estimate a median CO-to-H2 conversion factor of ⟨αCO⟩ = 1.7 ± 0.5 M⊙ (K km s−1pc2)−1 for ULIRGs. We derive median galaxy-integrated CO line ratios of 〈r21〉 = LCO(2-1)′/LCO(1-0)′ = 1.09, 〈r31〉 = LCO(3-2)′/LCO(1-0)′ = 0.76, and 〈r32〉 = LCO(3-2)′/LCO(2-1)′ = 0.76, significantly higher than normal star-forming galaxies, confirming the exceptional molecular gas properties of ULIRGs. We find that the r21 and r32 ratios are poor tracers of CO excitation in ULIRGs, while r31 shows a positive trend with LIR and star formation rates and a negative trend with the H2 gas depletion timescales (τdep). Our investigation of CO line ratios as a function of gas kinematics shows no clear trends, except for a positive relation between r21 and σv, which can be explained by CO opacity effects. These ULIRGs are also characterized by high L[CI](1-0)′/LCO(1-0)′ ratios, with a measured median value of ⟨rCICO⟩ = 0.18, higher than values from previous interferometric studies that were affected by missing [CI] line flux. The rCICO values do not show a significant correlation with any of the galaxy properties investigated, including OH outflow velocities and equivalent widths. We find that the widths of [CI](1–0) lines are ∼10% smaller than those of CO lines, and that this discrepancy becomes more significant in ULIRGs with broad lines (σv > 150 km s−1) and when considering the high-v wings of the lines. This suggests that the low optical depth of [CI] can challenge its detection in diffuse, low-surface-brightness outflows and, therefore, its use as a tracer of CO-dark H2 gas in these components. Finally, we find that higher LAGN are associated with longer τdep, consistent with the hypothesis that active galactic nucleus feedback may reduce the efficiency of star formation. Our study highlights the need for sensitive single-dish multi-tracer H2 surveys of ULIRGs that are able to recover the flux that is missed by interferometers, especially in the high-frequency lines such as [CI]. The Atacama Large Aperture Submillimeter Telescope (AtLAST) will be transformational for this field.

We present Atacama Large Millimeter/Submillimeter Array (ALMA) [CII] and $\sim158$ $\rm\mu m$ continuum observations of REBELS-25, a massive, morphologically complex ultra-luminous infrared galaxy (ULIRG; $L_{\rm IR}=1.5^{+0.8}_{-0.5}\times10^{12}$ L$_\odot$) at $z=7.31$, spectroscopically confirmed by the Reionization Era Bright Emission Line Survey (REBELS) ALMA Large Programme. REBELS-25 has a significant stellar mass of $M_{*}=8^{+4}_{-2}\times10^{9}$ M$_\odot$. From dust-continuum and ultraviolet observations, we determine a total obscured + unobscured star formation rate of SFR $=199^{+101}_{-63}$ M$_\odot$ yr$^{-1}$. This is about four times the SFR estimated from an extrapolated main-sequence. We also infer a [CII]-based molecular gas mass of $M_{\rm H_2}=5.1^{+5.1}_{-2.6}\times10^{10}$ $M_\odot$, implying a molecular gas depletion time of $ t_{\rm depl, H_2}=0.3^{+0.3}_{-0.2}$ Gyr. We observe a [CII] velocity gradient consistent with disc rotation, but given the current resolution we cannot rule out a more complex velocity structure such as a merger. The spectrum exhibits excess [CII] emission at large positive velocities ($\sim500$ km s$^{-1}$), which we interpret as either a merging companion or an outflow. In the outflow scenario, we derive a lower limit of the mass outflow rate of 200 M$_\odot$ yr$^{-1}$, which is consistent with expectations for a star formation-driven outflow. Given its large stellar mass, SFR and molecular gas reservoir $\sim700$ Myr after the Big Bang, we explore the future evolution of REBELS-25. Considering a simple, conservative model assuming an exponentially declining star formation history, constant star formation efficiency, and no additional gas inflow, we find that REBELS-25 has the potential to evolve into a galaxy consistent with the properties of high-mass quiescent galaxies recently observed at $z\sim4$., Comment: Accepted for publication in MNRAS. 21 pages, 8 figures

We present the average [C ii] 158 μm emission line sizes of UV-bright star-forming galaxies at z ∼ 7. Our results are derived from a stacking analysis of [C ii] 158 μm emission lines and dust continua observed by the Atacama Large Millimeter/submillimeter Array (ALMA), taking advantage of the large program Reionization Era Bright Emission Line Survey. We find that the average [C ii] emission at z ∼ 7 has an effective radius r e of 2.2 ± 0.2 kpc. It is ≳2× larger than the dust continuum and the rest-frame UV emission, in agreement with recently reported measurements for z ≲ 6 galaxies. Additionally, we compared the average [C ii] size with 4 < z < 6 galaxies observed by the ALMA Large Program to INvestigate [C ii] at Early times (ALPINE). By analyzing [C ii] sizes of 4 < z < 6 galaxies in two redshift bins, we find an average [C ii] size of r e = 2.2 ± 0.2 kpc and r e = 2.5 ± 0.2 kpc for z ∼ 5.5 and z ∼ 4.5 galaxies, respectively. These measurements show that star-forming galaxies, on average, show no evolution in the size of the [C ii] 158 μm emitting regions at redshift between z ∼ 7 and z ∼ 4. This finding suggests that the star-forming galaxies could be morphologically dominated by gas over a wide redshift range.

The neutral atomic gas content of individual galaxies at large cosmological distances has until recently been difficult to measure due to the weakness of the hyperfine H i 21 cm transition. Here we estimate the H i gas mass of a sample of main-sequence star-forming galaxies at z ∼ 6.5–7.8 surveyed for [C ii] 158 μm emission as part of the Reionization Era Bright Emission Line Survey (REBELS), using a recent calibration of the [C ii]-to-H i conversion factor. We find that the H i gas mass excess in galaxies increases as a function of redshift, with an average of M Hi /M ⋆ ≈ 10, corresponding to H i gas mass fractions of f Hi = M Hi /(M ⋆ + M Hi ) = 90%, at z ≈ 7. Based on the [C ii] 158 μm luminosity function (LF) derived from the same sample of galaxies, we further place constraints on the cosmic H i gas mass density in galaxies (ρ Hi ) at this redshift, which we measure to be ρ H I = 7.1 − 3.0 + 6.4 × 10 6 M ⊙ Mpc − 3 . This estimate is substantially lower by a factor of ≈10 than that inferred from an extrapolation of damped Lyα absorber (DLA) measurements and largely depends on the exact [C ii] LF adopted. However, we find this decrease in ρ Hi to be consistent with recent simulations and argue that this apparent discrepancy is likely a consequence of the DLA sight lines predominantly probing the substantial fraction of H i gas in high-z galactic halos, whereas [C ii] traces the H i in the ISM associated with star formation. We make predictions for this buildup of neutral gas in galaxies as a function of redshift, showing that at z ≳ 5, only ≈10% of the cosmic H i gas content is confined in galaxies and associated with the star-forming ISM.

High-redshift observations are often biased towards massive and bright galaxies that are not necessarily representative of the full population. In order to accurately study galaxy evolution and mass assembly at these redshifts, observations of ``normal'' main sequence galaxies are required. Here we present Atacama Large Millimeter/Submillimeter Array (ALMA) 0.3" resolution observations of the [CII] emission line at 158$\mu$m of HZ7, a main sequence galaxy at $z=5.25$. Comparing to archival rest-frame UV observations taken by the Hubble Space Telescope (HST), we find strong evidence of the existence of extended [CII] emission, which we estimate to be twice the size of the rest-frame UV emission, yielding one of the first high-redshift objects where a clear signature of a [CII] ``Halo'' has been detected to date. For a matched S\'ersic profile with n = 1, we measured a [CII] effective radius of $0.50\pm 0.04$" (3.07$\pm 0.25$ kpc) and an average rest-frame UV effective radius of $0.2\pm0.04$" ($1.48\pm0.16$ kpc). The [CII] morphology and kinematics of the system suggest a merging event resulting in a non rotating disk system. This event could be responsible for the extended [CII] emission. Alternatively, some potential obscured emission could also explain the [CII] to UV size ratio. These results contribute to the growing consensus with respect to the existence of extended [CII] emission around galaxies., Comment: 8 pages, 6 figures. Accepted to be published in MNRAS

We present results from the first public data release of the MaNGA-ARO Survey of CO Targets (MASCOT), focusing our study on galaxies whose star formation rates and stellar masses place them below the ridge of the star-forming main sequence. In optically selected type 2 AGN/low-ionization nuclear emission regions (LINERs)/Composites, we find an empirical relation between gas-phase metallicity gradients ∇Z and global molecular gas depletion times tdep=MH2/SFR with ‘more quenched’ systems showing flatter/positive gradients. Our results are based on the O3N2 metallicity diagnostic (applied to star-forming regions within a given galaxy), which was recently suggested to also be robust against emission by diffuse ionized gas (DIG) and LINERs. We conduct a systematic investigation into possible drivers of the observed ∇Z − tdep relation (ouflows, gas accretion, in situ star formation, mergers, and morphology). We find a strong relation between ∇Z or tdep and centralized outflow strength traced by the [O III] velocity broadening. We also find signatures of suppressed star formation in the outskirts in AGN-like galaxies with long depletion times and an enhancement of metals in the outer regions. We find no evidence of inflows impacting the metallicity gradients, and none of our results are found to be significantly affected by merger activity or morphology. We thus conclude that the observed ∇Z–tdep relation may stem from a combination of metal redistribution via weak feedback, and a connection to in situ star formation via a resolved mass-metallicity–SFR relation. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society., DW and CB are supported through the Emmy Noether Programme of the German Research Foundation. MA acknowledges support from FONDECYT grant 1211951, CONICYT + PCI + INSTITUTO MAX PLANCK DE ASTRONOMIA MPG190030, CONICYT+PCI + REDES 190194, and ANID BASAL project FB210003. WB acknowledges support from the ERC Advanced Grant 695671, ‘QUENCH’ and from the Science and Technology Facilities Council (STFC). Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High Performance Computing at the University of Utah., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).

We include a fully coupled treatment of metal and dust enrichment into the Delphi semi-analytic model of galaxy formation to explain the dust content of 13 Lyman Break Galaxies (LBGs) detected by the Atacama Large millimetre Array (ALMA) REBELS Large Program at $z\simeq 7$. We find that the galaxy dust mass, $M_d$, is regulated by the combination of SNII dust production, astration, shock destruction, and ejection in outflows; grain growth (with a standard timescale $\tau_0= 30$ Myr) plays a negligible role. The model predicts a dust-to-stellar mass ratio of $\sim 0.07-0.1\%$ and a UV-to-total star formation rate relation such that $log (\psi_{\rm UV}) = -0.05 ~[log (\psi)]^{2} + 0.86 ~log(\psi) -0.05$ (implying that 55-80\% of the star formation is obscured) for REBELS galaxies with stellar mass $M_* = 10^{9-10} M_\odot$. This relation reconciles the intrinsic UV luminosity of LBGs with their observed luminosity function at $z=7$. However, 2 out of the 13 systems show dust-to-stellar mass ratios ($\sim 0.94-1.1\%$) that are up to $18\times$ larger than expected from the fiducial relation. Due to the physical coupling between dust and metal enrichment, even decreasing $\tau_0$ to very low values (0.3 Myr) only increases the dust-to-stellar mass ratio by a factor $ \sim 2$. Given that grain growth is not a viable explanation for such high observed ratios of the dust-to-stellar mass, we propose alternative solutions., Comment: Accepted to MNRAS

ALMA observations have revealed the presence of dust in the first generations of galaxies in the Universe. However, the dust temperature Td remains mostly unconstrained due to the few available FIR continuum data at redshift $z$ > 5. This introduces large uncertainties in several properties of high-$z$ galaxies, namely their dust masses, infrared luminosities, and obscured fraction of star formation. Using a new method based on simultaneous [C $\scriptstyle \rm II$] 158-μm line and underlying dust continuum measurements, we derive Td in the continuum and [C $\scriptstyle \rm II$] detected $z$ ≈ 7 galaxies in the ALMA Large Project REBELS sample. We find 39 < Td < 58 K, and dust masses in the narrow range Md = (0.9-3.6) × 107 M⊙. These results allow us to extend for the first time the reported Td($z$) relation into the Epoch of Reionization. We produce a new physical model that explains the increasing Td($z$) trend with the decrease of gas depletion time, tdep = Mg/SFR, induced by the higher cosmological accretion rate at early times; this hypothesis yields Td ∝ (1 + $z$)0.4. The model also explains the observed Td scatter at a fixed redshift. We find that dust is warmer in obscured sources, as a larger obscuration results in more efficient dust heating. For UV-transparent (obscured) galaxies, Td only depends on the gas column density (metallicity), $T_{\rm d} \propto N_{\rm H}^{1/6}$ (Td ∝ Z-1/6). REBELS galaxies are on average relatively transparent, with effective gas column densities around NH ≃ (0.03-1) × 1021 cm-2. We predict that other high-$z$ galaxies (e.g. MACS0416-Y1, A2744-YD4), with estimated Td ≫ 60 K, are significantly obscured, low-metallicity systems. In fact, Td is higher in metal-poor systems due to their smaller dust content, which for fixed LIR results in warmer temperatures.

We analyse FIR dust continuum measurements for 14 galaxies ($z\approx 7$) in the ALMA REBELS LP to derive their physical properties. Our model uses three input data: (a) the UV spectral slope, $\beta$, (b) the observed UV continuum flux at $1500$A, $F_{\rm UV}$, (c) the observed continuum flux at $\approx 158\mu$m, $F_{158}$, and considers Milky Way (MW) and SMC extinction curves, along with different dust geometries. We find that REBELS galaxies have (28-90.5)% of their star formation obscured; the total (UV+IR) star formation rates are in the range $31.5 < {\rm SFR}/ (M_\odot {\rm yr}^{-1}) < 129.5$. The sample-averaged dust mass and temperature are $(1.3\pm 1.1)\times 10^7 M_\odot$ and $52 \pm 11$ K, respectively. In some galaxies dust is abundant (REBELS-14, $M'_d \approx 3.4 \times 10^7 M_\odot$), or hot (REBELS-18, $T'_d \approx 67$ K). The dust distribution is compact ($ 1 M_\odot$. With the SFR predicted by the model and a MW extinction curve, REBELS galaxies detected in [CII] nicely follow the local $L_{\rm CII}-$SFR relation, and are approximately located on the Kennicutt-Schmidt relation. The sample-averaged gas depletion time is of $0.11\, y_P^{-2}$ Gyr, where $y_P$ is the ratio of the gas-to-stellar distribution radius. For some systems a solution simultaneously matching the observed ($\beta, F_{\rm UV}, F_{158}$) values cannot be found. This occurs when the index $I_m = (F_{158}/F_{\rm UV})/(\beta-\beta_{\rm int})$, where $\beta_{\rm int}$ is the intrinsic UV slope, exceeds $I_m^*\approx 1120$ for a MW curve. For these objects we argue that the FIR and UV emitting regions are not co-spatial, questioning the use of the IRX-$\beta$ relation., Comment: 22 pages, 7 figures, accepted by MNRAS. Comments welcome

The circumgalactic medium (CGM) is the location where the interplay between large-scale outflows and accretion onto galaxies occurs. Metals in different ionization states flowing between the circumgalactic and intergalactic mediums are affected by large galactic outflows and low-ionization state inflowing gas. Observational studies on their spatial distribution and their relation with galaxy properties may provide important constraints on models of galaxy formation and evolution. To provide new insights into the spatial distribution of the circumgalactic of star-forming galaxies, we select a sample of 238 close pairs at $1.5 < z, Accepted for publication in A&A

Observations of the rest-frame UV emission of high-redshift galaxies suggest that the early stages of galaxy formation involve disturbed structures. Imaging the cold interstellar medium can provide a unique view of the kinematics associated with the assembly of galaxies. In this paper, we analyzed the spatial distribution and kinematics of the cold ionized gas of the normal star-forming galaxy COS-2987030247 at z = 6.8076, based on new high-resolution observations of the [C II] 158um line emission obtained with the Atacama Large Millimeter/submillimeter Array. These observations allowed us to compare the spatial distribution and extension of the [C II] and rest-frame UV emission, model the [C II] line data-cube using 3DBarolo, and measure the [C II] luminosity and star formation rate (SFR) surface densities in the galaxy subregions. The system is found to be composed of a main central source, a fainter north extension, and candidate [C II] companions located 10-kpc away. We find similar rest-frame UV and [C II] spatial distributions, suggesting that the [C II] emission emerges from the star-forming regions. The agreement between the UV and [C II] surface brightness radial profiles rules out diffuse, extended [C II] emission in the main galaxy component. The [C II] velocity map reveals a velocity gradient in the north-south direction suggesting ordered motion, as commonly found in rotating-disk galaxies. But higher-resolution observations would be needed to rule out a compact merger scenario. Our model indicates a low average velocity dispersion, $\sigma$ < 30 km s$^{-1}$. This result implies a dispersion lower than the expected value from observations and semi-analytic models of high redshift galaxies. We argue that COS-2987030247 is a candidate rotating disk experiencing a short period of stability which will be possibly perturbed at later times by accreting sources., Comment: 13 pages (+ 8 Appendix), 15 Figures, Accepted for publication in A&A

The intensity mapping of the [CII] 158um line redshifted to the sub-mm window is a promising probe of the z>4 star formation and its spatial distribution into the large-scale structure. To prepare the first-generation experiments (e.g., CONCERTO), we need realistic simulations of the sub-mm extragalactic sky in spectroscopy. We present a new version of the SIDES simulation including the main sub-mm lines around 1mm (CO, [CII], [CI]). This approach successfully reproduces the observed line luminosity functions. We then use our simulation to generate CONCERTO-like cubes (125-305GHz) and forecast the power spectra of the fluctuations caused by the various astrophysical components at those frequencies. Depending on our assumptions on the relation between star formation rate and [CII] luminosity, and the star formation history, our predictions of the z~6 [CII] power spectrum vary by two orders of magnitude. This highlights how uncertain the predictions are and how important future measurements will be to improve our understanding of this early epoch. SIDES can reproduce the CO shot noise recently measured at ~100 GHz by the mmIME experiment. Finally, we compare the contribution of the different astrophysical components at various redshift to the power spectra. The continuum is by far the brightest, by a factor of 3 to 100 depending on the frequency. At 300GHz, the CO foreground power spectrum is higher than the [CII] one for our base scenario. At lower frequency, the contrast between [CII] and extragalactic foregrounds is even worse. Masking the known galaxies from deep surveys should allow to reduce the foregrounds to 20% of the [CII] power spectrum up to z~6.5. However, this masking method will not be sufficient at higher redshifts. The code and the products of our simulation are released publicly and can be used for both intensity mapping experiments and sub-mm continuum and line surveys., 28 pages, 19 figures, 2 tables, accepted by A&A, the code and the products are available at https://cesamsi.lam.fr/instance/sides/home

High-redshift dusty star-forming galaxies with very high star formation rates (500 -- 3000 M$_{\odot}$ yr$^{-1}$) are key to understanding the formation of the most extreme galaxies in the early Universe. Characterising the gas reservoir of these systems can reveal the driving factor behind the high star formation. Using molecular gas tracers like high-J CO lines, neutral carbon lines and the dust continuum, we can estimate the gas density and radiation field intensity in their interstellar media. In this paper, we present high resolution ($\sim$0.4$^{\prime\prime}$) observations of CO(7-6), [CI](2-1) and dust continuum of 3 lensed galaxies from the SPT-SMG sample at $z\sim$ 3 with the Atacama Large Millimeter/submillimeter Array. Our sources have high intrinsic star-formation rates ($>$850 M$_{\odot}$yr$^{-1}$) and rather short depletion timescales ($, 29 pages, 26 figures, Accepted for publication in A&A. Figure 16 and the related conclusions have been revised

Several works in the past decade have used the ratio between total (rest 8-1000$\mu$m) infrared and radio (rest 1.4~GHz) luminosity in star-forming galaxies (q$_{IR}$), often referred to as the "infrared-radio correlation" (IRRC), to calibrate radio emission as a star formation rate (SFR) indicator. Previous studies constrained the evolution of q$_{IR}$ with redshift, finding a mild but significant decline, that is yet to be understood. For the first time, we calibrate q$_{IR}$ as a function of \textit{both} stellar mass (M$_{\star}$) and redshift, starting from an M$_{\star}$-selected sample of $>$400,000 star-forming galaxies in the COSMOS field, identified via (NUV-r)/(r-J) colours, at redshifts 0.1$, Comment: Accepted for publication in A&A. 22 pages + Appendices. 24 figures, 4 tables

BackgroundMental health has become one of the fundamental priorities during the COVID-19 pandemic. Situations like physical distancing as well as being constantly tagged as the most vulnerable group could expose older adults to mental and psychosocial burdens. Nonetheless, there is little clarity about the impact of the COVID-19 pandemic or similar pandemics in the past on the mental illness, wellbeing, and psychosocial health of the older population compared to other age groups.ObjectivesTo describe the patterns of older adults’ mental and psychosocial health related to acute respiratory disease propagated-type epidemics and pandemics and to evaluate the differences with how other age groups respond.Eligibility criteriaquantitative and qualitative studies evaluating mental illness, wellbeing, or psychosocial health outcomes associated with respiratory propagated epidemics and pandemics exposure or periods (COVID-19, SARS-CoV, MERS, and Influenza) in people 65 years or older.Data sourceOriginal articles published until June 1st, 2020, in any language searched in the electronic healthcare and social sciences database: MEDLINE, Embase, CINAHL, PsycINFO, Scopus, WHO Global literature on coronavirus disease database, China National Knowledge Infrastructure (中国 知网 –CNKI). Furthermore, EPPI Centre’s COVID-19 living systematic map and the publicly available publication list of the COVID-19 living systematic review will be incorporated for preprints and recent COVID-19 publications.Data extractionTwo independent reviewers will extract predefined parameters. The risk of bias will be assessed.Data synthesisData synthesis will be performed according to study type and design, type of epidemic and pandemic, types of outcomes (mental health and psychosocial outcomes), and participant characteristics (e.g., sex, race, age, socioeconomic status, food security, presence of dependency in daily life activities independent/dependent older adults). Comparison between sex, race, and other age groups will be performed qualitatively, and quantitatively if enough data is available. The risk of bias and study heterogeneity will be reported for quantitative studies.ConclusionThis study will provide information to take actions to address potential mental health difficulties during the COVID-19 pandemic in older adults and to understand responses on this age group. Furthermore, it will be useful to identify potential groups that are more vulnerable or resilient to the mental-health challenges of the current worldwide pandemic.

Mental health problems are a set of high-impact conditions. People aged 60 years and over are particularly vulnerable to factors that increase their risk of experiencing mental health problems and fatal outcomes, such as suicide. Within this age group, men as a subgroup are seldom the targets of relevant public health measures. This article aims to characterize the mental health status of men aged 60 years and over in Chile by using data from population-based surveys carried out in the country: the 2003 and 2009 National Health Surveys (NHS), the 2009 National Study of Dependency in Older Persons (ENADEAM), and the 2015 National Socioeconomic Characterization Survey (CASEN). The article looks at indicators for depression and depressive symptoms, suicide, and suicidal ideation, as well as mental health visits. According to reported figures from these surveys, older men in Chile constitute the population subgroup with the highest suicide rate, the lowest reported rates of suicidal ideation and suicide attempts, and the lowest reported frequency of mental health visits. Furthermore, men report depression less often than women. These figures provide an approximate picture of the mental health profile of older men in Chile and give rise to questions regarding the relevance of current epidemiological models for the identification of mental health risk profiles in this group. They also point to the urgent need to design health programs that integrate gender considerations in order to ensure proper screening and the acceptability of potential interventions for promoting mental health and reducing risk factors among older men.Os problemas de saúde mental constituem um conjunto de enfermidades com grande repercussão. Os indivíduos de 60 anos ou acima têm vulnerabilidades específicas que aumentam o risco de apresentar problemas de saúde mental com consequências fatais, como o suicídio. O sexo masculino é um subgrupo desta faixa etária pouco considerado como alvo em particular de ações em saúde. Este artigo enfoca o caso do Chile e busca caracterizar a realidade da saúde mental dos homens idosos a partir de dados obtidos em pesquisas de base populacional realizadas no país: Enquete Nacional de Saúde (ENS) 2003–2009, Estudo Nacional de Dependência nos Idosos (ENADEAM) 2009 e Pesquisa de Caracterização Socioeconômica Nacional (CAS) 2015. São apresentados os indicadores relativos a depressão e sintomas depressivos, suicídio e ideação suicida e consultas de saúde mental. Os dados informados nas pesquisas selecionadas revelam que, no país, os homens idosos apresentam a taxa de suicídio mais alta, o menor número de casos de ideação suicida e tentativa de suicídio e a menor frequência referida de consultas de saúde mental. Igualmente, eles referem menos depressão que as mulheres. Estes dados permitem traçar um perfil da saúde mental em homens idosos no Chile e questionar a adequação dos modelos epidemiológicos atuais para identificar os perfis de risco de saúde mental neste grupo. Existe também uma necessidade premente de estabelecer programas de saúde que incorporem o fator gênero para que se possa realizar uma pesquisa adequada com aceitabilidade das possíveis intervenções para promover a saúde mental e reduzir os riscos em homens idosos.

Resumen Introducción: La depresión es la condición de salud que genera mayor carga de enfermedad, donde los adultos mayores manifiestan un gran impacto asociado a esta enfermedad. Este artículo busca describir el impacto que tienen los síntomas depresivos en la funcionalidad de la persona mayor y comprender la relación existente entre la pérdida funcional y la depresión. Metodología: Se realizó una revisión de la literatura de artículos publicados entre los años 1990 y 2016. Se realizó un análisis narrativo de la evidencia encontrada, incluyendo un total de 40 artículos. Resultados: Una de las repercusiones más importantes es la pérdida de la funcionalidad y reducción de la participación en actividades de la vida diaria, asociándose a una dependencia progresiva, mayor riesgo de caídas y temor a caerse, restricción y reducción en la participación en actividades de interés, y peores resultados en procesos de rehabilitación. De esto se desprende la necesidad de entender los síntomas depresivos en conjunto con las repercusiones funcionales en el adulto mayor, comprendiendo que existe una relación recíproca entre la capacidad que tiene la persona mayor para realizar sus actividades diarias y la presencia de síntomas depresivos. Conclusión: Considerar el impacto clínico y psicosocial que tienen la depresión en la funcionalidad de la persona mayor podría contribuir al entendimiento de los síntomas depresivos como un problema de impacto global que requiere de un abordaje integral.

La demencia —Trastorno Neurocognitivo Mayor— se caracteriza por deterioro cognitivo adquirido y otros sintomas psicologicos y conductuales que impactan en la capacidad de la persona para responder efectivamente a las demandas del ambiente. El numero de personas con demencia aumenta de forma consistente en el mundo, volviendose una prioridad para la salud publica y elevando la urgencia de contar con estrategias para enfrentar su impacto. La investigacion cientifica biomedica, clinica y psicosocial es fundamental en toda estrategia de abordaje de la demencia. Este articulo sintetiza elementos relacionados con la inclusion de personas con demencia en investigacion cientifica desde diferentes perspectivas, incluyendo el impacto del deficit cognitivo y la jurisprudencia local. Entre los dilemas bioeticos vinculados a investigacion en demencia se encuentra la evaluacion de capacidad de consentimiento. Las leyes 20.120 y 20.584 levantan controversias en el caso de la discapacidad, atinentes a la participacion de personas con demencia en investigacion cientifica. El presente manuscrito busca aportar una sintesis de elementos clave para el analisis de la participacion de personas con demencia en investigacion cientifica.

Objective Few instruments evaluate family caregiver perceptions of challenges caring for persons with dementia and improvement or worsening in these areas. To address this measurement gap, we examine psychometric properties of a Spanish version of the 13-item Perceived Change Index (PCI-S), originally validated with English-speaking caregivers. Methods Cross-sectional study with 94 caregivers of persons with mild to moderate dementia in Chile. Interviews included caregiver demographics, burden, health perception, distress with behaviours, dementia severity, behavioural symptoms and functionality. Results Caregiver mean age was 55.9 (SD ± 14.14) years and mean years caregiving was 3 (SD ± 2.60). The scale had strong internal consistency (Cronbach α = 0.94), and inter-observer consistency (CCI = 0.99; 95% CI = 0.95–0.99). Two factors were identified: Management skills (α = 0.89), and somatic well-being and affects (α = 0.92), explaining 63% of scale variance. Significant associations supporting convergent validity were observed for PCI-S and subscales with caregiver burden (p

Erratum to: A&A, 620, A125 (2018), https://doi.org/10.1051/0004-6361/201732442

Re-admission to hospital by the elderly is a frequent event that is associated with complications. The aim of this article is to describe a randomised clinical trial protocol which has the aim of describing and comparing the impact of a home-based intervention by Occupational Therapists (OT) in the likelihood of re-admission at 6 months.Randomised controlled trial conducted in medical units of the "Hospital Clínico de la Universidad de Chile" and "Hospital de la Fuerza Aérea de Chile", with 217 patients aged 60 years or older admitted for acute or decompensated chronic disease, provided that they have a person of reference after hospital discharge. The control group consists of the usual care regarding post-discharge patients. This will be compared to the experimental group that includes a home visit from OT on two occasions over a six-month period, who will apply a multicomponent intervention. Informed consent will be requested with the sociodemographic and hospital admission information, functional (Barthel index; LawtonBrody Scale) and cognitive performance (Short Portable Mental Status Questionnaire; Functional Activities Questionnaire; Confusion Assessment Method), and comorbidity (Cumulative Illness Rating Scale for Geriatrics). Both groups will receive a telephone follow-up at 4, 12 and 24 weeks after hospital discharge.The intervention will reduce the rate of hospital re-admissions by at least 40% at 6 months compared with usual care.It will be useful to know the components that reduce the risk of hospital re-admissions and improve hospital discharge healthcare for elderly.

Estimation of rock composition in mining plants is important for determining rock size and grindability which, in turn, may improve control of the grinding process. Variations in ore grindability and size distribution directly affect a mill's power consumption and throughput. It is therefore highly desirable to develop new methods to estimate rock lithological composition remotely. In this paper, a new method for remote lithological classification based on digital image analysis is proposed. The method is based on a single digital video camera for image acquisition from rocks on a conveyor belt. Each image is broken into sub-images to extract texture information using several different spatial scales. Gabor filters are used to extract features from each sub-image for five different spatial scales and eight orientations. After feature extraction, each sub-image is classified into a lithological class using a support-vector machine (SVM). Finally, information from the contour of each rock is used to select all sub-images that fall inside the contour and vote for the rock class. The method was tested on three databases, one of them containing sub-images of 64 × 43 pixels of five ore types assigned to three grindability classes (soft, medium and hard). The second database has seven ore types containing sub-images of 60 × 40 pixels. The third database was captured with higher resolution cameras and controlled illumination with five ore types and containing sub-images of 64 × 48. The databases were divided into 2 subsets, one for training with cross validation, and the other for testing. Classification accuracy was compared with previously published results on both databases. Comparisons show that our proposed method yielded significant improvements in classification accuracy, between 8.3% and 26%, relative to previously published results.

The Kintun program is the first public health strategy specifically designed for dementia care in Chile. It was launched in 2013 in the city of Santiago with support from the National Service for the Elderly and the Municipality of Peñalolén. Using an interdisciplinary team, the program seeks to promote community integration and better support for persons with dementia and their caregivers. The multicomponent program includes: an activity-based day care center, training and education of family caregivers, home visits, and community outreach to increase dementia awareness. Case management helps to monitor ongoing needs and link families to resources. To date, 259 dyads (persons with dementia and their families) have been enrolled in the program. Due to its success in 2015, the Kintun program received funding from the Ministry of Health. This has led to the integration of previously disparate initiatives, better consistency across services, and the development of a comprehensive national dementia plan for Chile.

Well-being related to care for person with dementia (PwD) is an important health measure as it involves both negative and positive implications of caregiving. To learn about factors related to caregiver’s well-being perception, a cross-sectional study was conducted in family caregivers of older persons with mild and moderate dementia, who assisted a daycare center for dementia in Santiago, Chile, from March to July 2016. Data were collected using the following assessments: PCI (perceived wellbeing), ZBI-6 (caregiver burden), EQ-5D (health perception), GDS-Reisberg (dementia severity), NPI-Q (neuro-psychiatric behaviors and distress) and ADCS-ADL (activities of daily living). The relationship between perceived well-being and other factors was evaluated through correlations (r,s) and logistic regression models (OR). In 86 subjects, significant correlations were observed (p

We examine the behaviour of the infrared-radio correlation (IRRC) over the range 0 2 COSMOS field. We distinguish between objects where emission is believed to arise solely from star-formation, and those where an active galactic nucleus (AGN) is thought to be present. We account for non-detections in the radio or in the infrared using a doubly-censored survival analysis. We find that the IRRC of star-forming galaxies, quantified by the infrared-to-1.4 GHz radio luminosity ratio (qTIR), decreases with increasing redshift: qTIR(z) = (2.88 ± 0.03)(1 + z)- 0.19 ± 0.01. This is consistent with several previous results from the literature. Moderate-to-high radiative luminosity AGN do not follow the same qTIR(z) trend as star-forming galaxies, having a lower normalisation and steeper decrease with redshift. We cannot rule out the possibility that unidentified AGN contributions only to the radio regime may be steepening the observed qTIR(z) trend of the star-forming galaxy population. We demonstrate that the choice of the average radio spectral index directly affects the normalisation, as well as the derived trend with redshift of the IRRC. An increasing fractional contribution to the observed 3 GHz flux by free-free emission of star-forming galaxies may also affect the derived evolution. However, we find that the standard (M82-based) assumption of the typical radio spectral energy distribution (SED) for star-forming galaxies is inconsistent with our results. This suggests a more complex shape of the typical radio SED for star-forming galaxies, and that imperfect K corrections in the radio may govern the derived trend of decreasing qTIR with increasing redshift. A more detailed understanding of the radio spectrum is therefore required for robust K corrections in the radio and to fully understand the cosmic evolution of the IRRC. Lastly, we present a redshift-dependent relation between rest-frame 1.4 GHz radio luminosity and star formation rate taking the derived redshift trend into account.

Gender classification from NIR iris image is a new topic with only a few papers published. All previous work on gender-from-iris tried to find the best feature extraction techniques to represent the information of the iris texture for gender classification using normalized, encoded or periocular images. However this is a new topic in deep-learning application with soft biometric. In this chapter, we show that learning gender-iris representations through the use of deep neural networks may increase the performance obtained on these tasks. To this end, we propose the application of deep-learning methods to separate the gender-from-iris images even when the amount of learning data is limited, using an unsupervised stage with Restricted Boltzmann Machine (RBM) and a supervised stage using a Convolutional Neural Network (CNN).

An unknown lipophilic coryneform bacterium isolated from the blood cultures of a patient with bacteremia was characterized by phenotypic and molecular genetic methods. Chemical analysis revealed the presence of short chain mycolic acids consistent with the genus Corynebacterium. The DNA G+C content was 60.8 mol%. Comparative 16S rRNA gene sequence analysis demonstrated that the isolate represents a new subline within the genus Corynebacterium. The closely phylogenetic relative of the unknown bacterium was found to be C. tuscaniense (97.8% sequence similarity). Partial rpoB gene sequence revealed that strain IMMIB L-2475(T) exhibited 13.5% sequence divergence with C. tuscaniense. The unknown bacterium was distinguished from C. tuscaniense by, DNA-DNA hybridization, cellular fatty acid profiles, MALDI-TOF analyses of cell extracts and biochemical tests. Based on the phylogenetic and phenotypic criteria, it is proposed that this bacterium be classified as new species, Corynebacterium aquatimens sp. nov., and is represented by strain IMMIB L-2475(T) (=DSM 45632(T)=CCUG 61574(T)).

The Kintun Program is an innovating health intervention project launched in Chile in 2013. It aims to enhance participation of persons with dementia (PwD) in everyday activities, respite for the caregivers and improve home-based care. The program involves different components including day care center, home visits, training for caregivers, counseling and community education. These actions are developed by a multidisciplinary team. This program represents a novel approach to dementia care in Chile as a country with policies and dementia care strategies still under development. To analyze the effect of the Program Kintun on the PwD, a quasi-experimental study was conducted during the implementation of the program, with repeated measures at baseline (T.0.) and after 10–14 weeks of intervention (T1) during September 2013 and June 2014. Data were collected using: ADCS-ADL (activities of daily living), MMSE (cognition), TUG (fall risk) and NPI-Q (neuro-psychiatric behaviors and distress). Data were analyzed with t-student considering p

Face and iris localization is one of the most active research areas in image understanding for new applications in security and theft prevention, as well as in the development of human-machine interfaces. In the past, several methods for real-time face localization have been developed using face anthropometric templates which include face features such as eyes, eyebrows, nose and mouth. It has been shown that accuracy in face and iris localization is crucial to face recognition algorithms. An error of a few pixels in face or iris localization will produce significant reduction in face recognition rates. In this paper, we present a new method based on particle swarm optimization (PSO) to generate templates for frontal face localization in real time. The PSO templates were tested for face localization on the Yale B Face Database and compared to other methods based on anthropometric templates and Adaboost. Additionally, the PSO templates were compared in iris localization to a method using combined binary edge and intensity information in two subsets of the AR face database, and to a method based on SVM classifiers in a subset of the FERET database. Results show that the PSO templates exhibit better spatial selectivity for frontal faces resulting in a better performance in face localization and face size estimation. Correct face localization reached a rate of 97.4% on Yale B which was higher than 96.2% obtained with the anthropometric templates and much better than 60.5% obtained with the Adaboost face detection method. On the AR face subsets, different disparity errors were considered and for the smallest error, a 100% correct detection was reached in the AR-63 subset and 99.7% was obtained in the AR-564 subset. On the FERET subset a detection rate of 96.6% was achieved using the same criteria. In contrast to the Adaboost method, PSO templates were able to localize faces on high-contrast or poorly illuminated environments. Additionally, in comparison with the anthropometric templates, the PSO templates have fewer pixels, resulting in a 40% reduction in processing time thus making them more appropriate for real-time applications.

Studying molecular gas in the central regions of the star burst galaxies NGC4945 and Circinus enables us to characterize the physical conditions and compare them to previous local and high-z studies. We estimate temperature, molecular density and column densities of CO and atomic carbon. Using model predictions we give a range of estimated CO/C abundance ratios. Using the new NANTEN2 4m sub-millimeter telescope in Pampa La Bola, Chile, we observed for the first time CO 4-3 and [CI] 3P1-3 P0 at the centers of both galaxies at linear scale of 682 pc and 732 pc respectively. We compute the cooling curves of 12CO and 13CO using radiative transfer models and estimate the physical conditions of CO and [CI]. The centers of NGC4945 and Circinus are very [CI] bright objects, exhibiting [CI] 3P1 - 3 P0 luminosities of 91 and 67Kkms-1kpc2, respectively. The [CI] 3P1-3 P0/CO 4-3 ratio of integrated intensities are large at 1.2 in NGC4945 and 2.8 in Circinus. Combining previous CO J= 1-0, 2-1 and 3-2 and 13CO J= 1-0, 2-1 studies with our new observations, the radiative transfer calculations give a range of densities, n(H2) = 10^3-3*104^cm-3, and a wide range of kinetic temperatures, Tkin = 20 - 100K, depending on the density. Future CO J= 7-6 and [CI] 2-1 observations will be important to resolve the ambiguity in the physical conditions and confirm the model predictions.

El uso de transporte es una actividad de vital importancia para las personas mayores como elemento promotor de autonomía y participación social. El transporte urbano con frecuencia no es planificado con templando las necesidades particulares que este grupo social puede presentar, lo que puede favorecer dificultades en el desempeño durante el uso de transporte. Para el logro de un desempeño adaptativo en la actividad interactúan elementos personales, como el estado de salud y el estado funcional, con elementos ambientales, como la accesibilidad física y las actitudes de los pasajeros. Este trabajo describe el marco conceptual y metodológico implicado en el desarrollo de un instrumento de valoración que permite conocer el desempeño de las personas mayores en el uso de transporte público (EVADUT-AM). Para su diseño, se consideró hallazgos cualitativos previamente desarrollados a partir de las experiencias en uso de transporte de personas mayores que viven en la ciudad de Santiago de Chile. El instrumento está compuesto por las dimensiones preparación, acceso, y uso del transporte público. Finalmente, el artículo presenta la escala de valoración y sus instrucciones de aplicación, con el propósito de aportar con un insumo para la práctica disciplinar gerontológica. De igual modo, plantea oportunidades para la continuidad del trabajo a partir de un abordaje cuantitativo que permita validar el instrumento y evaluar sus propiedades psicométricas.

We study the physical properties of a sample of 6 SMGs in the COSMOS field, spectroscopically confirmed to lie at z>4. We use new GMRT 325 MHz and 3 GHz JVLA data to probe the rest-frame 1.4 GHz emission at z=4, and to estimate the sizes of the star-forming (SF) regions of these sources, resp. Combining our size estimates with those available in the literature for AzTEC1 and AzTEC3 we infer a median radio-emitting size for our z>4 SMGs of (0.63"+/-0.12")x(0.35"+/-0.05") or 4.1x2.3 kpc^2 (major times minor axis; assuming z=4.5) or lower if we take the two marginally resolved SMGs as unresolved. This is consistent with the sizes of SF regions in lower-redshift SMGs, and local normal galaxies, yet higher than the sizes of SF regions of local ULIRGs. Our SMG sample consists of a fair mix of compact and more clumpy systems with multiple, perhaps merging, components. With an average formation time of ~280 Myr, derived through modeling of the UV-IR SEDs, the studied SMGs are young systems. The average stellar mass, dust temperature, and IR luminosity we derive are M*~1.4x10^11 M_sun, T_dust~43 K, and L_IR~1.3x10^13L_sun, resp. The average L_IR is up to an order of magnitude higher than for SMGs at lower redshifts. Our SMGs follow the correlation between dust temperature and IR luminosity as derived for Herschel-selected 0.1=1.95+/-0.26 for our sample, compared to q~2.6 for IR luminous galaxies at z4 SMGs put them at the high end of the L_IR-T_dust distribution of SMGs, and that our SMGs form a morphologically heterogeneous sample. Thus, further in-depth analyses of large, statistical samples of high-redshift SMGs are needed to fully understand their role in galaxy formation and evolution., Comment: 16 pages, 8 figures, 6 tables; to appear in A&A

The Kintun Program is the first public center for the support of people with dementia and their carers in Chile. The program involves different components such as day care center, home visits and caregiver training. Engagement in daily activities and situations is one of the main outcomes of the program, therefore the design and implementation of activities is a major challenge. This symposium will describe the embedded rationale, learnings and recommendations from the process of design and implementation of activities at the center. Three key stages can be described in the history of the Kintun Program since 2013 until today. These stages reflect a progression from an initial structured set of group activities towards a tailored and situated frame for participation in activities. Results show benefits in the reduction of behavioral symptoms, improvement in levels of function and improved caregiver’s perception of the person with dementia’s participation at home.

In Chile most of care for persons with dementia is delivered by family relatives and research of interventions targeting caregivers of persons with dementia is very limited. This qualitative study explored perceived benefits of an education and training program for family caregivers of older persons with dementia. Setting was the Program Kintun for persons with dementia in the city of Santiago, Chile. Intervention was founded using the theoretical frame of readiness in family caregivers of persons with dementia by Gitlin et al (2014), based on a progressive cycle in the development of skills that allow caregivers to move towards higher levels of self-efficacy.

Activities developed under hazardous conditions, such as mining, require an active investment from the industry to avoid serious injuries and even loss of lives. One of the safety measures taken to address this problem is to implement a video surveillance system able to track vehicles and workers to enforce safety protocols preventing dangerous events that could lead to accidents. In this paper, we propose an intelligent video surveillance system able to detect and predict possible dangerous interactions between workers and vehicles operating on a monitored environment. Our system is able to analyze video information from one or several cameras, detects and tracks objects and emits an alarm that warns the operator on possible safety hazards. A multiclass object detection is trained to detect vehicles and people. The system object detection stage was implemented in CUDA for parallel processing to achieve real time operation. A multitracking system was implemented to track detected objects that move from one camera field of view to a neighbor camera field of view. Experiments on a monitored parking space show that our proposed system yields good performance in tracking people and vehicles, detecting close interaction and generating relevant alarms.