The origin of [C II] 157 μm emission in a five-component interstellar medium : the case of NGC 3184 and NGC 628

With its relatively low ionization potential, C+ can be found throughout the interstellar medium (ISM) and provides one of the main cooling channels of the ISM via the [C II] 157 mu m emission. While the strength of the [C II] line correlates with the star formation rate, the contributions of the various gas phases to the [C II] emission on galactic scales are not well established. In this study we establish an empirical multi-component model of the ISM, including dense H II regions, dense photon dissociation regions (PDRs), the warm ionized medium (WIM), low density and G(0). surfaces of molecular clouds (SfMCs), and the cold neutral medium (CNM). We test our model on ten luminous regions within the two nearby galaxies NGC 3184 and NGC 628. on angular scales of 500-600 pc. Both galaxies are part of the Herschel. key program. KINGFISH,. and are complemented by a large set of ancillary ground-and space-based data. The five modeled phases together reproduce the observed [C II] emission quite well, overpredicting the total flux slightly (about 45%) averaged over all regions. We find that dense PDRs are the dominating component, contributing 68% of the [C II] flux on average, followed by the WIM and the SfMCs, with mean contributions of about half of the contribution from dense PDRs, each. CNM and dense H II regions are only minor contributors with less than 5% each. These estimates are averaged over the selected regions, but the relative contributions of the various phases to the [C II] flux vary significantly between these regions

The Herschel Exploitation of Local Galaxy Andromeda (HELGA) II: Dust and Gas in Andromeda

We present an analysis of the dust and gas in Andromeda, using Herschel images sampling the entire far-infrared peak. We fit a modified-blackbody model to ~4000 quasi-independent pixels with spatial resolution of ~140pc and find that a variable dust-emissivity index (beta) is required to fit the data. We find no significant long-wavelength excess above this model suggesting there is no cold dust component. We show that the gas-to-dust ratio varies radially, increasing from ~20 in the center to ~70 in the star-forming ring at 10kpc, consistent with the metallicity gradient. In the 10kpc ring the average beta is ~1.9, in good agreement with values determined for the Milky Way (MW). However, in contrast to the MW, we find significant radial variations in beta, which increases from 1.9 at 10kpc to ~2.5 at a radius of 3.1kpc and then decreases to 1.7 in the center. The dust temperature is fairly constant in the 10kpc ring (ranging from 17-20K), but increases strongly in the bulge to ~30K. Within 3.1kpc we find the dust temperature is highly correlated with the 3.6 micron flux, suggesting the general stellar population in the bulge is the dominant source of dust heating there. At larger radii, there is a weak correlation between the star formation rate and dust temperature. We find no evidence for 'dark gas' in M31 in contrast to recent results for the MW. Finally, we obtained an estimate of the CO X-factor by minimising the dispersion in the gas-to-dust ratio, obtaining a value of (1.9+/-0.4)x10^20 cm^-2 [K kms^-1]^-1.Comment: 19 pages, 18 figures. Submitted to ApJ April 2012; Accepted July 201

Perfil epidemiológico de pacientes com fissura labiopalatinas atendidos em um hospital de referência do interior de Alagoas

Objetivo: Traçar um perfil epidemiológico e socioeconômico de pacientes com fissuras labiopalatinas atendidos em um hospital de referência do interior de Alagoas. Materiais e Métodos:  Trata-se de um estudo transversal analítico descritivo, onde foi realizada a consulta aos prontuários de pacientes com fissura labiopalatina no ano de 2019 em um hospital de referência do interior de Alagoas. Variáveis como: idade, gênero, tipo de fissura, renda familiar, grau de escolaridade dos pais, acesso a terapias complementares e o CPOD foram coletados. Foi realizada uma análise estatística descritiva bem como análises através do teste exato de Fisher ou qui-quadrado e t de Student. Resultados: Ao todo foram analisados 32 prontuários observando-se uma predominância do gênero masculino (67,7%), e de etnia parda (45,2%). A maior parte dos pacientes (56,7%) relataram que possuíam renda familiar entre 1 a 3 salários mínimos e 36,7% menos de 1 salário mínimo. As fissuras unilaterais foram mais prevalentes (65,4%,) sendo o lado esquerdo mais afetado (76,5%). A maioria dos pacientes não realizou terapia com fonoaudiólogo ou ortodontista (61,3% e 61,5% respectivamente). Não foi observada relação estatisticamente significante entre o índice CPO-D, renda familiar e escolaridade dos pais (p > 0,05). Considerações finais: O tratamento de fissuras labiopalatinas é multidisciplinar, longo e de alto custo. É necessário a criação de centros de tratamento especialmente em regiões com baixo IDH, melhorando o acesso e a assistência a saúde desses pacientes, minimizando as sequelas e melhorando sua qualidade de vida

Elaboração de fichas técnicas de preparações à base de Ora-Pro-Nóbis: o valor nutricional da PANC brasileira / Elaboration of technical sheets of preparations based on Ora-Pro-Nóbis: the nutritional value of the brazilian UFP

O instrumento que pode reunir os indicadores essenciais à produção adequada de preparações é a Ficha Técnica de Preparação (FTP) que completa, abrange todos os indicadores técnicos e ainda pode ser acrescida da análise nutricional de macro e micronutrientes e custo total. A utilização da FTP beneficia todo o preparo, facilitando a reprodução/execução da receita, e permite estimar o valor nutricional das preparações para compor planos alimentares. Dessa forma, o objetivo do presente estudo consiste em elaborar fichas técnicas de preparações à base de ora-pro-nóbis para divulgar o valor nutricional da PANC brasileira através da reprodução de receitas de baixo custo de preparações à base de ora-pro-nóbis, analisando todos os componentes da Ficha Técnica (Per Capita), pesos bruto e líquido, fatores de correção e cocção, medidas caseiras, porção, técnica de preparo, rendimento e custo, análise química dos ingredientes). Trata-se de um estudo de caráter analítico e descritivo iniciado a partir da coleta de dados teóricos sobre as preparações para a reprodução das receitas, visando a análise química das preparações à base de ora-pro-nóbis. Das 22 receitas selecionadas para compor o cardápio semanal, 19 foram reproduzidas no Laboratório de Técnica Dietética (LTD) do curso de Nutrição do CESMAC, Maceió-AL: salada de folhas cruas, omelete, ora-pro-nóbis refolgada, arroz, feijão tropeiro, sorvete, chá, purê, peixe, escondidinho de frango com ora-pro-nóbis, suchá, farofa, torta de limão e ora-pro-nóbis, bolo, frango, refrigerante, flau, vinagrete e feijão caseiro. As preparações foram distribuídas em um cardápio para cinco dias, cada um contendo: entrada, guarnição, prato principal, acompanhamento, sobremesa e bebida.  As folhas de ora-pro-nóbis foram coletadas na horta de plantas medicinais do Centro Universitário Cesmac, localizada em Marechal Deodoro-AL. Pode-se observar que o acréscimo da ora-pro-nóbis contribuiu com significativo aumento do aporte proteico das preparações, principalmente em preparações que originalmente não são tidas como fontes proteicas, como por exemplo, bebidas (chá, suchá, refrigerante caseiro), sobremesas (bolo, torta, sorvete e flau gourmet), guarnições (purê, refolgado de folhas e farofa) e acompanhamentos (arroz e feijão). Notou-se, ainda, que haveria a possibilidade de aumentar a quantidade de ora-pro-nóbis em todas as 19 preparações, de forma que não alterasse as características organolépticas das preparações e aumentasse a oferta proteica. A popularização das PANC representa ganhos importantes do ponto de vista cultural, econômico, social e nutricional, considerando a tradição no cultivo e a sua contribuição em termos nutricionais. Trata-se, portanto, de uma questão de segurança e de soberania alimentar estimular a produção e consumo das plantas alimentícias não-convencionais.

Cold dust and low [O iii]/[C ii] ratios: an evolved star-forming population at redshift 7

We present new ALMA Band 8 (rest-frame 90 μm) continuum observations of three massive (M⋆ ≈ 1010 M⊙) galaxies at z ≈ 7 previously detected in [C II]158 μm and underlying dust continuum emission in the Reionization Era Bright Emission Line Survey (REBELS). We detect dust emission from two of our targets in Band 8 (REBELS-25 and REBELS-38), while REBELS-12 remains undetected. Through optically thin modified blackbody fitting, we determine dust temperatures of Tdust ≈ 30 − 35 K in both of the dual-band detected targets, indicating they are colder than most known galaxies at z ∼ 7. Moreover, their inferred dust masses are large (Mdust ≈ 108 M⊙), albeit still consistent with models of high-redshift dust production. We furthermore target and detect [O III]88 μm emission in both REBELS-12 and REBELS-25, and find L[O III]/L[C II] ≈ 1 − 1.5 – low compared to the L[O III]/L[C II] ≳ 2 − 10 observed in the known z ≳ 6 population thus far. We argue the lower line ratios are due to a comparatively weaker ionizing radiation field resulting from the less starbursty nature of our targets, although the possibility of REBELS-12 being a merger of an [O III]-bright and [O III]-faint component prevents the unambiguous interpretation of its [O III]/[C II] ratio. Nevertheless, a low burstiness forms a natural explanation for the cold dust temperatures and low [O III]λλ4959, 5007 + Hβ equivalent widths of REBELS-25 and REBELS-38. Overall, these observations provide evidence for the existence of a massive, dust-rich galaxy population at z ≈ 7 which has previously experienced vigorous star formation, but is currently forming stars in a steady, as opposed to bursty, manner

The ALMA REBELS Survey: The First Infrared Luminosity Function Measurement at $\mathbf{z \sim 7}

We present the first observational infrared luminosity function (IRLF) measurement in the Epoch of Reionization (EoR) based on a UV-selected galaxy sample with ALMA spectroscopic observations. Our analysis is based on the ALMA large program Reionization Era Bright Emission Line Survey (REBELS), which targets 42 galaxies at $\mathrm{z=6.4-7.7}$ with [CII] 158\micron line scans. 16 sources exhibit a dust detection, 15 of which are also spectroscopically confirmed through the [CII] line. The IR luminosities of the sample range from $\log L_{IR}/L_\odot=11.4$ to 12.2. Using the UVLF 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 $\log L_{*}/L_\odot=11.6^{+0.2}_{-0.1}$. Our observational results are in broad agreement with the average of predicted IRLFs from simulations at $z\sim7$. Conversely, our IRLFs lie significantly below lower redshift estimates, suggesting a rapid evolution from $z\sim4$ to $z\sim7$, into the reionization epoch. The inferred obscured contribution to the cosmic star-formation rate density at $z\sim7$ amounts to $\mathrm{log(SFRD/M_{\odot}/yr/Mpc^{3}) = -2.66^{+0.17}_{-0.14} }$ which is at least $\sim$10\% 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.Comment: 9 pages, 5 figure

DustPedia: Multiwavelength photometry and imagery of 875 nearby galaxies in 42 ultraviolet-microwave bands

Aims. The DustPedia project is capitalising on the legacy of the Herschel Space Observatory, using cutting-edge modelling techniques to study dust in the 875 DustPedia galaxies – representing the vast majority of extended galaxies within 3000 km s-1 that were observed by Herschel. This work requires a database of multiwavelength imagery and photometry that greatly exceeds the scope (in terms of wavelength coverage and number of galaxies) of any previous local-Universe survey. Methods. We constructed a database containing our own custom Herschel reductions, along with standardised archival observations from GALEX, SDSS, DSS, 2MASS, WISE, Spitzer, and Planck. Using these data, we performed consistent aperture-matched photometry, which we combined with external supplementary photometry from IRAS and Planck. Results. We present our multiwavelength imagery and photometry across 42 UV-microwave bands for the 875 DustPedia galaxies. Our aperture-matched photometry, combined with the external supplementary photometry, represents a total of 21 857 photometric measurements. A typical DustPedia galaxy has multiwavelength photometry spanning 25 bands. We also present the Comprehensive & Adaptable Aperture Photometry Routine (CAAPR), the pipeline we developed to carry out our aperture-matched photometry. CAAPR is designed to produce consistent photometry for the enormous range of galaxy and observation types in our data. In particular, CAAPR is able to determine robust cross-compatible uncertainties, thanks to a novel method for reliably extrapolating the aperture noise for observations that cover a very limited amount of background. Our rich database of imagery and photometry is being made available to the community

The ALMA REBELS Survey: the first infrared luminosity function measurement at z ∼ 7

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 μm 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 logL∗/L⊙=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 log(SFRD/M⊙yr−1Mpc−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

The Interstellar Medium In Galaxies Seen A Billion Years After The Big Bang

Evolution in the measured rest frame ultraviolet spectral slope and ultraviolet to optical flux ratios indicate a rapid evolution in the dust obscuration of galaxies during the first 3 billion years of cosmic time (z>4). This evolution implies a change in the average interstellar medium properties, but the measurements are systematically uncertain due to untested assumptions, and the inability to measure heavily obscured regions of the galaxies. Previous attempts to directly measure the interstellar medium in normal galaxies at these redshifts have failed for a number of reasons with one notable exception. Here we report measurements of the [CII] gas and dust emission in 9 typical (~1-4L*) star-forming galaxies ~1 billon years after the big bang (z~5-6). We find these galaxies have >12x less thermal emission compared with similar systems ~2 billion years later, and enhanced [CII] emission relative to the far-infrared continuum, confirming a strong evolution in the interstellar medium properties in the early universe. The gas is distributed over scales of 1-8 kpc, and shows diverse dynamics within the sample. These results are consistent with early galaxies having significantly less dust than typical galaxies seen at z<3 and being comparable to local low-metallicity systems.Comment: Submitted to Nature, under review after referee report. 22 pages, 4 figures, 4 Extended Data Figures, 5 Extended Data table

The ALMA REBELS survey: the dust content of z ∼7 Lyman break galaxies

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 ≃ 7. We find that the galaxy dust mass, Md, is regulated by the combination of Type II supernova dust production, astration, shock destruction, and ejection in outflows; grain growth (with a standard time-scale τ0 = 30 Myr) plays a negligible role. The model predicts a dust-to-stellar mass ratio of ~ 0.07-0.1per cent and a UV-to-total star formation rate relation such that log(ψUV) = -0.05 [log(ψ)]2 + 0.86 log(ψ) - 0.05 (implying that 55-80 per cent of the star formation is obscured) for REBELS galaxies with stellar mass M∗ = 109-1010 M⊙. 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 (~0.94-1.1per cent) 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 τ0 to very low values (0.3 Myr) only increases the dust-to-stellar mass ratio by a factor of ∼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