Search

Stellar bars are common morphological structures in the local Universe: according to optical and NIR surveys, they are present in about two-thirds of disc galaxies. These elongated structures are also believed to play a crucial role in secular evolutionary processes, since they are able to efficiently redistribute gas, stars and angular momentum within their hosts, although it remains unclear whether they enhance or suppress star formation. A useful tool to investigate such an ambiguity is the Main Sequence (MS) relation, which tightly links stellar mass ($M_{\star}$) and star formation rate (SFR). The main goal of this work is to explore star formation processes in barred galaxies, in order to assess the relevance of possible bar quenching effects on the typical log-linear trend of the resolved MS. To this purpose, we carry out a spatially resolved analysis on sub-kpc scales for a sample of six nearby barred galaxies. Multi-wavelength photometric data (from far-UV to far-IR) are collected from the DustPedia database and a panchromatic Spectral Energy Distribution (SED) fitting procedure is applied on square apertures of fixed angular size (8" $\times$ 8"), making use of the magphys code. For each galaxy we obtain the distributions of stellar mass and star formation rate surface densities and relate them in the $\log \Sigma_{\star}$ - $\log \Sigma_{\rm SFR}$ plane deriving the spatially resolved MS relation. Although significant galaxy-to-galaxy variations are in place, we infer the presence of a common anti-correlation track in correspondence with the bar-hosting region, which shows systematically lower values of SFR. Such a central quiescent signature can be interpreted as the result of a bar-driven depletion of gas reservoirs and a consequent halt of star formation. This seems to point in the direction of an inside-out quenching scenario., Comment: 15 pages, 6 figures, accepted for publication in A&A

The main sequence (MS) of star-forming galaxies (SFGs) is the tight relation between the galaxy stellar mass and its star formation rate (SFR) and was observed up to z ~ 6. The MS relation can be used as a reference for understanding the differences among galaxies, characterised by different rates of stellar production (starbursts, SFGs, and passive galaxies), and those inside a galaxy made up of different components (bulge, disk, and halo). To investigate peculiar features found in our sample galaxies, we focus here on their star formation history (SFH). We performed a spectral energy distribution fitting procedure that accounted for the energetic balance between UV and far-IR radiation on a sample of eight nearby face-on spiral galaxies from the DustPedia sample. This approach allowed us to study the spatially resolved MS of the sample and to recover the past SFH. By exploiting the BAGPIPES code, we constrained the SFHs for each galaxy with a delayed exponentially declining model to derive their mass-weighted age (tMW). A central old region (tMW up to~7Gyr, consistent with the presence of a bulge for various systems) is followed by younger regions in which the disks are still forming stars (tMW~4Gyr). At larger distances, tMW increases mildly in general. Strikingly, in two galaxies (NGC4321 and NGC5194), we found a steep increase in tMW that reached levels similar to those of the bulge. These old stellar populations in the very galaxy outskirts are unexpected. We discuss their potential origin by considering the different gas phases of the source with the most prominent quenched ring, NGC4321, and argue for two main possibilities: 1) some environmental effect (e.g. starvation) or 2) the circumgalactic medium of sources outside of high-density clusters might have stopped to supply pristine gas to the galaxy (e.g. if its specific angular moment is too high for being accreted)., Comment: Accepted for publication on Astronomy and Astrophysics

Measurements of the size of dust continuum emission are an important tool for constraining the spatial extent of star formation and hence the build-up of stellar mass. Compact dust emission has generally been observed at Cosmic Noon (z~2-3). However, at earlier epochs, toward the end of the Reionization (z~4-6), only the sizes of a handful of IR-bright galaxies have been measured. In this work, we derive the dust emission sizes of main-sequence galaxies at z~5 from the ALPINE survey. We measure the dust effective radius r_e,FIR in the uv-plane in Band 7 of ALMA for seven ALPINE galaxies with resolved emission and we compare it with rest-frame UV and [CII]158$\mu$m measurements. We study the r_e,FIR-L_IR scaling relation by considering our dust size measurements and all the data in literature at z~4-6. Finally, we compare our size measurements with predictions from simulations. The dust emission in the selected ALPINE galaxies is rather extended (r_e,FIR~1.5-3 kpc), similar to [CII]158 um but a factor of ~2 larger than the rest-frame UV emission. Putting together all the measurements at z~5, spanning 2 decades in luminosity from L_IR ~ 10^11 L_sun to L_IR ~ 10^13 L_sun, the data highlight a steeply increasing trend of the r_e,FIR-L_IR relation at L_IR< 10^12 L_sun, followed by a downturn and a decreasing trend at brighter luminosities. Finally, simulations that extend up to the stellar masses of the ALPINE galaxies considered in the present work predict a sub-set of galaxies (~25% at 10^10 M_sun < M_star < 10^11 M_sun) with sizes as large as those measured., Comment: 8 pages, Accepted by A&A

Galaxy-galaxy lensing (GGL) and clustering measurements from the Dark Energy Spectroscopic Instrument Year 1 (DESI Y1) dataset promise to yield unprecedented combined-probe tests of cosmology and the galaxy-halo connection. In such analyses, it is essential to identify and characterise all relevant statistical and systematic errors. In this paper, we forecast the covariances of DESI Y1 GGL+clustering measurements and characterise the systematic bias due to redshift evolution in the lens samples. Focusing on the projected clustering and galaxy-galaxy lensing correlations, we compute a Gaussian analytical covariance, using a suite of N-body and log-normal simulations to characterise the effect of the survey footprint. Using the DESI One Percent Survey data, we measure the evolution of galaxy bias parameters for the DESI Luminous Red Galaxy (LRG) and Bright Galaxy Survey (BGS) samples. We find mild evolution in the LRGs in 0.4 < z < 0.8, subdominant compared to the expected statistical errors. For BGS, we find less evolution effects for brighter absolute magnitude cuts, at the cost of reduced sample size. We find that with a fiducial redshift bin width delta z = 0.1, evolution effects on GGL is negligible across all scales, all fiducial selection cuts, all fiducial redshift bins, given DESI Y1 sample size. Galaxy clustering is more sensitive to evolution due to the bias squared scaling. Nevertheless the redshift evolution effect is insignificant for clustering above the 1-halo scale of 0.1Mpc/h. For studies that wish to reliably access smaller scales, additional treatment of redshift evolution is likely needed. This study serves as a reference for GGL and clustering studies using the DESI Y1 sample, Comment: 19 pages, 15 figures, submitted to MNRAS

We present the first spectroscopic ALMA follow-up for a pilot sample of nine Radio-Selected NIRdark galaxies in the COSMOS field. These sources were initially selected as radio-detected sources (S(3GHz)>12.65 uJy), lacking an optical/NIR counterpart in the COSMOS2015 catalog (Ks>24.7 mag). Several studies highlighted how this selection could provide a population of highly dust-obscured, massive, and star-bursting galaxies. With these new ALMA observations, we assess the spectroscopic redshifts of this pilot sample of sources and improve the quality of the physical properties estimated through SED-fitting. Moreover, we measure the quantity of molecular gas present inside these galaxies and forecast their potential evolutionary path, finding that the RS-NIRdark galaxies could represent a likely population of high-z progenitors of the massive and passive galaxies discovered at z~3. Finally, we present some initial constraints on the kinematics of the ISM within the analyzed galaxies, reporting a high fraction (~55%) of double-peaked lines that can be interpreted as the signature of a rotating structure in our targets or with the presence of major mergers in our sample. Our results presented in this paper showcase the scientific potential of (sub)mm observations for this elusive population of galaxies and highlight the potential contribution of these sources in the evolution of the massive and passive galaxies at high-z., Comment: 16 pages, 9 figures, 5 tables. Submitted to A&A

Dusty, distant, massive ($M_*\gtrsim 10^{11}\,\rm M_\odot$) galaxies are usually found to show a remarkable star-formation activity, contributing on the order of $25\%$ of the cosmic star-formation rate density at $z\approx3$--$5$, and up to $30\%$ at $z\sim7$ from ALMA observations. Nonetheless, they are elusive in classical optical surveys, and current near-infrared surveys are able to detect them only in very small sky areas. Since these objects have low space densities, deep and wide surveys are necessary to obtain statistically relevant results about them. Euclid will be potentially capable of delivering the required information, but, given the lack of spectroscopic features at these distances within its bands, it is still unclear if it will be possible to identify and characterize these objects. The goal of this work is to assess the capability of Euclid, together with ancillary optical and near-infrared data, to identify these distant, dusty and massive galaxies, based on broadband photometry. We used a gradient-boosting algorithm to predict both the redshift and spectral type of objects at high $z$. To perform such an analysis we make use of simulated photometric observations derived using the SPRITZ software. The gradient-boosting algorithm was found to be accurate in predicting both the redshift and spectral type of objects within the Euclid Deep Survey simulated catalog at $z>2$. In particular, we study the analog of HIEROs (i.e. sources with $H-[4.5]>2.25$), combining Euclid and Spitzer data at the depth of the Deep Fields. We found that the dusty population at $3\lesssim z\lesssim 7$ is well identified, with a redshift RMS and OLF of only $0.55$ and $8.5\%$ ($H_E\leq26$), respectively. Our findings suggest that with Euclid we will obtain meaningful insights into the role of massive and dusty galaxies in the cosmic star-formation rate over time., Comment: 18 pages, 13 figures, accepted in A&A

Context. ALMA observations show that dusty, distant, massive (M* ≳ 1011 M⊙) galaxies usually have a remarkable star-formation activity, contributing of the order of 25% of the cosmic star-formation rate density at z ≈ 3–5, and up to 30% at z ∼ 7. Nonetheless, they are elusive in classical optical surveys, and current near-IR surveys are able to detect them only in very small sky areas. Since these objects have low space densities, deep and wide surveys are necessary to obtain statistically relevant results about them. Euclid will potentially be capable of delivering the required information, but, given the lack of spectroscopic features at these distances within its bands, it is still unclear if Euclid will be able to identify and characterise these objects. Aims. The goal of this work is to assess the capability of Euclid, together with ancillary optical and near-IR data, to identify these distant, dusty, and massive galaxies based on broadband photometry. Methods. We used a gradient-boosting algorithm to predict both the redshift and spectral type of objects at high z. To perform such an analysis, we made use of simulated photometric observations that mimic the Euclid Deep Survey, derived using the state-of-the-art Spectro-Photometric Realizations of Infrared-selected Targets at all-z (SPRITZ) software. Results. The gradient-boosting algorithm was found to be accurate in predicting both the redshift and spectral type of objects within the simulated Euclid Deep Survey catalogue at z > 2, while drastically decreasing the runtime with respect to spectral-energy-distribution-fitting methods. In particular, we studied the analogue of HIEROs (i.e. sources selected on the basis of a red H − [4.5]> 2.25), combining Euclid and Spitzer data at the depth of the Deep Fields. These so

Our Universe is puzzling. According to the canonical cosmological model, the Lambda Cold Dark Matter (LCDM) model, around 95\% of the Universe consists of unknown dark matter and dark energy. Despite the unknown nature of these forms of matter and energy, LCDM provides accurate predictions for a variety of observations. One of the main cosmological pillars is the large-scale distribution of galaxies and the underlying dark matter halos, as probed by surveys like The Dark Energy Spectroscopic Instrument (DESI). This Thesis aims to understand the structure and properties of dark matter halos and apply innovative techniques to test the LCDM cosmological paradigm with state-of-the-art surveys like DESI. First, I will show how various halo properties (e.g., halo mass and mass accretion rate) can be inferred from weak lensing observations of cluster-sized halos. Moreover, I will talk about the splashback feature -- a distinct drop in mass density beyond the virial radius predicted by simulations -- and the accuracy and precision with which we can detect it in real data. Finally, I will demonstrate how the most massive galaxies in the Universe present an excellent avenue for performing precision cosmology with DESI. As we enter the era of DESI, millions of galaxies in the nearby Universe will be complete down to 11.5 solar masses. I will show how this dataset will constrain key cosmological parameters while also minimizing systematics plaguing current studies.

Exceptional situations allow us to rethink sociocultural dynamics that were previously taken for granted. Architecture is often part of these processes, anticipating with its projects situations that would only occur decades later. This is the case of the Tuscolano III housing project (Rome, 1950), by Adalberto Libera, which introduces a concept of domesticity based on the dissolution between the public and the private. In this project, inhabiting is understood as a phenomenon that occurs on a neighborhood scale; and domesticity as something that expands beyond the walls of a house, and depends on a complex network of social, spatial and political relations. In Tuscolano III Libera proposes an inclusive model of the city, embracing lifestyles that were not widespread at the time, but are so in current times, such as living alone. Through this project, the article aims to investigate the anticipatory capacity of architectural design in periods of great change, as was the period of post-war reconstruction in Italy, and as is the contemporary era, with its continuing economic, political and health crises., Las situaciones excepcionales permiten replantearse dinámicas socioculturales que anteriormente se daban por sentadas. La arquitectura suele ser parte de estos procesos, anticipando con sus proyectos situaciones que sólo se producirían décadas después. Es el caso del proyecto residencial Tuscolano III (Roma, 1950), de Adalberto Libera, que introduce un concepto de domesticidad basado en la disolución entre lo público y lo privado. En este proyecto, el habitar se entiende como un fenómeno que ocurre a escala de barrio; y la domesticidad como algo que se expande más allá de los muros de una casa, y depende de una compleja red de relaciones sociales, espaciales y políticas. En Tuscolano III Libera propone un modelo inclusivo de ciudad, que abarca estilos de vida que no estaban muy extendidos en la época, pero que lo son en los tiempos actuales, como vivir solo. A través de este proyecto, el artículo se propone investigar la capacidad anticipatoria del diseño arquitectónico en periodos de grandes cambios, como fue el periodo de reconstrucción de posguerra en Italia, y como es la época contemporánea, con sus continuas crisis económicas, políticas y sanitarias.

[Resumen] El Trabajo de Fin de Grado titulado Yves Saint Laurent: arte y moda a través de 6 museos de París tiene como objetivo analizar las distintas formas en las que se vinculan el arte y la moda en la obra del diseñador francés Yves Saint Laurent que formó parte de la exposición Yves Saint Laurent aux musées celebrada en París en el año 2022. En esta exposición se presentaron prendas de Yves Saint Laurent junto a las obras de arte en las que se inspiraron en el espacio de seis museos principales de París, ofreciendo a los visitantes la oportunidad de conocer cómo el diseñador trasladó principios de las artes plásticas al campo del diseño de moda. El objetivo de este trabajo es analizar, museo por museo, cómo se relacionan diversas obras artísticas y las prendas de Yves Saint Laurent que se inspiraron en ellas, y el porqué de la elección de la sala expositiva que, en cada caso, se seleccionó para mostrar esas relaciones, haciendo así un análisis desde lo más general del espacio museístico hasta lo más específico del diseño de moda que nos permitirá observar cómo se cohesionan el arte y la moda desde un ejemplo concreto. Asimismo, ahondaremos en lo influyente que fue Yves Saint Laurent en la moda de la segunda mitad del siglo XX y cuál fue su contribución en la liberación de la mujer. Para cumplir estos objetivos, se ha llevado a cabo una búsqueda y recopilación de fuentes tanto en formato impreso como digital, con especial atención a libros y artículos periodísticos en materia de historia del arte que, junto a la información generada con motivo de la exposición (noticias, dossier de prensa, artículos de blogs,…) nos han permitido reunir abundante información para abordar el análisis planteado. A mayores, en este trabajo juegan un papel importante los recursos visuales, en especial las ilustraciones elaboradas por la autora del trabajo, ya que nos permiten entender y explicar de forma clara los vínculos identificados entre cada prenda y la/s obras pictóricas, escu, [Abstract] The Final Degree Project entitled Yves Saint Laurent: art and fashion through 6 museums in Paris aims to analyze the different ways in which art and fashion are linked in the work of the French designer Yves Saint Laurent that was part of the Yves Saint Laurent aux musées exhibition held in Paris in 2022. In this exhibition, Yves Saint Laurent garments were presented along with the works of art that inspired them in the space of the six main museums in Paris, offering visitors the opportunity to learn how the designer transferred principles of plastic arts to the field of fashion design. The objective of this project is to analyze, for each museum, how different works of art and the Yves Saint Laurent garments that were inspired by them are related, and the reason for the choice of the exhibition room that, in each case, was selected to show these relationships, thus making an analysis from the most general aspects related to the exhibition space to the most specific aspects related to fashion design that will allow us to observe how art and fashion link together from a concrete example. Likewise, we will delve into how influential Yves Saint Laurent was in the fashion world in the second half of the 20th century and what his contribution meant to the liberation of women. To meet these objectives, a search and compilation of sources has been carried out in both printed and digital formats, with special attention to books and journalistic articles about art history that, together with the information generated on the occasion of the exhibition (news, press kit, blog articles,...) have allowed us to gather abundant information to address the proposed analysis. Furthermore, visual resources play an important role regarding this matter, especially the illustrations created by the author of this project, since they help us to clearly understand and explain the links identified between each garment and the work of art that served as a reference, especially in t, [Resumo] O Traballo de Fin de Grao titulado Yves Saint Laurent: arte e moda a través de 6 museos de París ten como obxectivo analizar as distintas formas nas que se vinculan a arte e a moda na obra do deseñador francés Yves Saint Laurent que formou parte da exposición Yves Saint Laurent aux musées celebrada en París no ano 2022. Nesta exposición presentáronse pezas de Yves Saint Laurent xunto ás obras de arte nas que se inspiraron no espazo de seis museos principais de París, ofrecendo aos visitantes a oportunidade de coñecer como o deseñador trasladou principios das artes plásticas ao campo do deseño de moda. O obxectivo deste traballo é analizar, museo por museo, como se relacionan diversas obras artísticas e as pezas de Yves Saint Laurent que se inspiraron nelas, e o porqué da elección da sala expositiva que, en cada caso, seleccionouse para mostrar esas relacións, facendo así unha análise desde o máis xeral do espazo museístico ata o máis específico do deseño de moda que nos permitirá observar como se cohesionan a arte e a moda desde un exemplo concreto. Así mesmo, profundaremos no influente que foi Yves Saint Laurent na moda da segunda metade do século XX e cal foi a súa contribución na liberación da muller. Para cumprir estes obxectivos, levouse a cabo unha procura e recompilación de fontes tanto en formato impreso como dixital, con especial atención a libros e artigos xornalísticos en materia de historia da arte que, xunto á información xerada con motivo da exposición (noticias, dossier de prensa, artigos de blogues,…) permitíronnos reunir abundante información para abordar a análise exposta. A maiores, neste traballo xogan un papel importante os recursos visuais, en especial as ilustracións elaboradas pola autora do traballo, xa que nos permiten entender e explicar de forma clara os vínculos identificados entre cada peza e a/s obras pictóricas, escultóricas ou doutro tipo que lle serviron de referente, especialmente en canto a texturas, formas, cores e compo

Aims. We provide an in-depth analysis of the COSMOS-Web ring, an Einstein ring at z=2 that we serendipitously discovered in the COSMOS-Web survey and possibly the most distant lens discovered to date. Methods. We extract the visible and NIR photometry from more than 25 bands and we derive the photometric redshifts and physical properties of both the lens and the source with three different SED fitting codes. Using JWST/NIRCam images, we also produce two lens models to (i) recover the total mass of the lens, (ii) derive the magnification of the system, (iii) reconstruct the morphology of the lensed source, and (iv) measure the slope of the total mass density profile of the lens. Results. The lens is a very massive and quiescent (sSFR < 10^(-13) yr-1) elliptical galaxy at z = 2.02 \pm 0.02 with a total mass Mtot(

About 12 billion years ago, the Universe was first experiencing light again after the dark ages, and galaxies filled the environment with stars, metals and dust. How efficient was this process? How fast did these primordial galaxies form stars and dust? We can answer these questions by tracing the Star Formation Rate Density (SFRD) back to its widely unknown high redshift tail, traditionally observed in the Near-InfraRed (NIR), Optical and UV bands. Thus, the objects with a high amount of dust were missing. We aim to fill this knowledge gap by studying Radio Selected NIR-dark (\textit{RS-NIRdark}) sources, i.e. sources not having a counterpart at UV-to-NIR wavelengths. We widen the sample by Talia et al. (2021) from 197 to 272 objects in the COSMic evolution Survey (COSMOS) field, including also photometrically contaminated sources, previously excluded. Another important step forward consists in the visual inspection of each source in the bands from u* to MIPS-24$\mu$m. According to their "environment" in the different bands, we are able to highlight different cases of study and calibrate an appropriate photometric procedure for the objects affected by confusion issues. We estimate that the contribution of RS-NIRdark to the Cosmic SFRD at 3$<$z$<$5 is $\sim$10--25$\%$ of that based on UV-selected galaxies.

We report the identification of 15 galaxy candidates at $z\ge9$ using the initial COSMOS-Web JWST observations over 77 arcmin$^2$ through four NIRCam filters (F115W, F150W, F277W, F444W) with an overlap with MIRI (F770W) of 8.7 arcmin$^2$. We fit the sample using several publicly-available SED fitting and photometric redshift codes and determine their redshifts between $z=9.3$ and $z=10.9$ ($\langle z\rangle=10.0$), UV-magnitudes between M$_{\rm UV}$ = $-$21.2 and $-$19.5 (with $\langle $M$_{\rm UV}\rangle=-20.2$) and rest-frame UV slopes ($\langle \beta\rangle=-2.4$). These galaxies are, on average, more luminous than most $z\ge9$ candidates discovered by JWST so far in the literature, while exhibiting similar blue colors in their rest-frame UV. The rest-frame UV slopes derived from SED-fitting are blue ($\beta\sim$[$-$2.0, $-$2.7]) without reaching extremely blue values as reported in other recent studies at these redshifts. The blue color is consistent with models that suggest the underlying stellar population is not yet fully enriched in metals like similarly luminous galaxies in the lower redshift Universe. The derived stellar masses with $\langle \log_{\rm 10} ($M$_\star/$M$_\odot)\rangle\approx8-9$ are not in tension with the standard $\Lambda$CDM model and our measurement of the volume density of such UV luminous galaxies aligns well with previously measured values presented in the literature at $z\sim9-10$. Our sample of galaxies, although compact, are significantly resolved., Comment: Submitted to ApJ

We propose that observations of super-massive galaxies contain cosmological constraining power similar to conventional cluster cosmology, and we provide promising indications that the associated systematic errors are comparably easier to control. We consider a fiducial spectroscopic and stellar mass complete sample of galaxies drawn from the Dark Energy Spectroscopic Survey (DESI) and forecast how constraints on Omega_m-sigma_8 from this sample will compare with those from number counts of clusters based on richness. At fixed number density, we find that massive galaxies offer similar constraints to galaxy clusters. However, a mass-complete galaxy sample from DESI has the potential to probe lower halo masses than standard optical cluster samples (which are typically limited to richness above 20 and halo mass above 10^13.5); additionally, it is straightforward to cleanly measure projected galaxy clustering for such a DESI sample, which we show can substantially improve the constraining power on Omega_m. We also compare the constraining power of stellar mass-limited samples to those from larger but mass-incomplete samples (e.g., the DESI Bright Galaxy Survey, BGS, Sample); relative to a lower number density stellar mass-limited samples, we find that a BGS-like sample improves statistical constraints by 60% for Omega_m and 40% for sigma_8, but this uses small scale information which will be harder to model for BGS. Our initial assessment of the systematics associated with supermassive galaxy cosmology yields promising results. The proposed samples have a 10% satellite fraction, but we show that cosmological constraints may be robust to the impact of satellites. These findings motivate future work to realize the potential of super-massive galaxies to probe lower halo masses than richness-based clusters and to avoid persistent systematics associated with optical cluster finding.

The joint analysis of different cosmological probes, such as galaxy clustering and weak lensing, can potentially yield invaluable insights into the nature of the primordial Universe, dark energy and dark matter. However, the development of high-fidelity theoretical models that cover a wide range of scales and redshifts is a necessary stepping-stone. Here, we present public high-resolution weak lensing maps on the light cone, generated using the $N$-body simulation suite AbacusSummit in the Born approximation, and accompanying weak lensing mock catalogues, tuned via fits to the Early Data Release small-scale clustering measurements of the Dark Energy Spectroscopic Instrument (DESI). Available in this release are maps of the cosmic shear, deflection angle and convergence fields at source redshifts ranging from $z = 0.15$ to 2.45 with $\Delta z = 0.05$ as well as CMB convergence maps ($z \approx 1090$) for each of the 25 ${\tt base}$-resolution simulations ($L_{\rm box} = 2000\,h^{-1}{\rm Mpc}$, $N_{\rm part} = 6912^3$) as well as for the two ${\tt huge}$ simulations ($L_{\rm box} = 7500\,h^{-1}{\rm Mpc}$, $N_{\rm part} = 8640^3$) at the fiducial AbacusSummit cosmology ($Planck$ 2018). The pixel resolution of each map is 0.21 arcmin, corresponding to a HEALPiX $N_{\rm side}$ of 16384. The sky coverage of the ${\tt base}$ simulations is an octant until $z \approx 0.8$ (decreasing to about 1800 deg$^2$ at $z \approx 2.4$), whereas the ${\tt huge}$ simulations offer full-sky coverage until $z \approx 2.2$. Mock lensing source catalogues are sampled matching the ensemble properties of the Kilo-Degree Survey, Dark Energy Survey, and Hyper-Suprime Cam weak lensing datasets. The produced mock catalogues are validated against theoretical predictions for various clustering and lensing statistics such as galaxy clustering multipoles, galaxy-shear and shear-shear, showing excellent agreement., Comment: 21 pages, 13 figures, data available at https://app.globus.org/file-manager?origin_id=3dd6566c-eed2-11ed-ba43-09d6a6f08166&path=%2F

We introduce a new, multi-zone chemical evolution model of the DustPedia galaxy M74, calibrated by means of MCMC methods. We take into account the observed stellar and gas density profiles and use Bayesian analysis to constrain two fundamental parameters characterising the gas accretion and star formation timescale, i.e. the infall timescale tau and the SF efficiency nu, respectively, as a function of galactocentric radius R. Our analysis supports an infall timescale increasing with R and a star formation efficiency decreasing with R, thus supporting an 'Inside-Out' formation for M74. For both tau and nu, we find a weaker radial dependence than in the Milky Way. We also investigate the dust content of M74, comparing the observed dust density profile with the results of our chemical evolution models. Various prescriptions have been considered for two key parameters, i.e. the typical dust accretion timescale and the mass of gas cleared out of the dust by a supernova remnant, regulating the dust growth and destruction rate, respectively. Two models with a different current balance between destruction and accretion, i.e. with equilibrium and dominion of accretion over destruction, can equally reproduce the observed dust profile of M74. This outlines the degeneracy between these parameters in shaping the interstellar dust content in galaxies. Our methods will be extended to more DustPedia galaxies to shed more light on the relative roles of dust production and destruction., Comment: MNRAS, accepted for publication, 19 pages, 14 figures

We analyse the molecular and atomic emission lines of 71 bright Herschel-selected galaxies between redshifts 1.4 to 4.6 detected by the Atacama Large Millimetre/submillimetre Array. These lines include a total of 156 CO, [C I], and H2O emission lines. For 46 galaxies, we detect two transitions of CO lines, and for these galaxies we find gas properties similar to those of other dusty star-forming galaxy (DSFG) samples. A comparison to photo-dissociation models suggests that most of Herschel-selected galaxies have similar interstellar medium conditions as local infrared-luminous galaxies and high-redshift DSFGs, although with denser gas and more intense far-ultraviolet radiation fields than normal star-forming galaxies. The line luminosities agree with the luminosity scaling relations across five orders of magnitude, although the star-formation and gas surface density distributions (i.e., Schmidt-Kennicutt relation) suggest a different star-formation phase in our galaxies (and other DSFGs) compared to local and low-redshift gas-rich, normal star-forming systems. The gas-to-dust ratios of these galaxies are similar to Milky Way values, with no apparent redshift evolution. Four of 46 sources appear to have CO line ratios in excess of the expected maximum (thermalized) profile, suggesting a rare phase in the evolution of DSFGs. Finally, we create a deep stacked spectrum over a wide rest-frame frequency (220-890 GHz) that reveals faint transitions from HCN and CH, in line with previous stacking experiments., Comment: 30 pages, 17 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society Main Journal. Comments are warmly welcomed

We present a novel simulation-based cosmological analysis of galaxy-galaxy lensing and galaxy redshift-space clustering. Compared to analysis methods based on perturbation theory, our simulation-based approach allows us to probe a much wider range of scales, $0.4 \, h^{-1} \, \mathrm{Mpc}$ to $63 \, h^{-1} \, \mathrm{Mpc}$, including highly non-linear scales, and marginalises over astrophysical effects such as assembly bias. We apply this framework to data from the Baryon Oscillation Spectroscopic Survey LOWZ sample cross-correlated with state-of-the-art gravitational lensing catalogues from the Kilo Degree Survey and the Dark Energy Survey. We show that gravitational lensing and redshift-space clustering when analysed over a large range of scales place tight constraints on the growth-of-structure parameter $S_8 = \sigma_8 \sqrt{\Omega_{\rm m} / 0.3}$. Overall, we infer $S_8 = 0.792 \pm 0.022$ when analysing the combination of galaxy-galaxy lensing and projected galaxy clustering and $S_8 = 0.771 \pm 0.027$ for galaxy redshift-space clustering. These findings highlight the potential constraining power of full-scale studies over studies analysing only large scales, and also showcase the benefits of analysing multiple large-scale structure surveys jointly. Our inferred values for $S_8$ fall below the value inferred from the CMB, $S_8 = 0.834 \pm 0.016$. While this difference is not statistically significant by itself, our results mirror other findings in the literature whereby low-redshift large scale structure probes infer lower values for $S_8$ than the CMB, the so-called $S_8$-tension., Comment: 22 pages, 16 figures, submitted to MNRAS, comments welcome

We present 101 and 151 GHz ALMA continuum images for 85 fields selected from Herschel observations that have 500 micron flux densities >80 mJy and 250-500 micron colours consistent with z > 2, most of which are expected to be gravitationally lensed or hyperluminous infrared galaxies. Approximately half of the Herschel 500 micron sources were resolved into multiple ALMA sources, but 11 of the 15 brightest 500 micron Herschel sources correspond to individual ALMA sources. For the 37 fields containing either a single source with a spectroscopic redshift or two sources with the same spectroscopic redshift, we examined the colour temperatures and dust emissivity indices. The colour temperatures only vary weakly with redshift and are statistically consistent with no redshift-dependent temperature variations, which generally corresponds to results from other samples selected in far-infrared, submillimetre, or millimetre bands but not to results from samples selected in optical or near-infrared bands. The dust emissivity indices, with very few exceptions, are largely consistent with a value of 2. We also compared spectroscopic redshifts to photometric redshifts based on spectral energy distribution templates designed for infrared-bright high-redshift galaxies. While the templates systematically underestimate the redshifts by ~15%, the inclusion of ALMA data decreases the scatter in the predicted redshifts by a factor of ~2, illustrating the potential usefulness of these millimetre data for estimating photometric redshifts., Comment: Accepted for publication in Monthly Notices of the Royal Astronomical Society

In the last decades, an increasing scientific interest has been growing in the elusive population of "dark" (i.e. lacking an optical/NIR counterpart) Dusty Star-Forming Galaxies (DSFGs). Although extremely promising for their likely contribution to the cosmic Star Formation Rate Density and for their possible role in the evolution of the first massive and passive galaxies around $z\sim3$, the difficulty in selecting statistically significant samples of dark DSFGs is limiting their scientific potentialities. This work presents the first panchromatic study of a sample of 263 Radio-Selected NIRdark galaxies discovered in the COSMOS field following the procedure by Talia+21. These sources are selected as radio-bright galaxies (S(3GHz)>12.65 uJy) with no counterpart in the NIR-selected COSMOS2020 catalog (Ks > 25.5 mag). For these sources, we build a new photometric catalog including accurate photometry from the optical to the radio obtained with a new deblending pipeline (PhoEBO: Photometry Extractor for Blended Objects). We employ this catalog to estimate the photo-zs and the physical properties of the galaxies through an SED-fitting procedure performed with two different codes (Magphys and Cigale). Finally, we estimate the AGN contamination in our sample by performing a series of complementary tests. The high values of the median extinction (Av ~ 4) and star formation rate (SFR ~ 500 Msun/yr) confirm the likely DSFG nature of the RS-NIRdark galaxies. The median photo-z (z~3) and the presence of a significant tail of high-z candidates (z>4.5) suggest that these sources are important contributors to the cosmic SFRD and the evolutionary path of galaxies at high redshifts., Comment: 22 pages, 9 figures, 3 tables. Accepted for publication in ApJ

We have carried out HST snapshot observations at 1.1 $\mu$m of 281 candidate strongly lensed galaxies identified in the wide-area extragalactic surveys conducted with the Herschel space observatory. Our candidates comprise systems with flux densities at $500\,\mu$m$ S_{500}\geq 80$ mJy. We model and subtract the surface brightness distribution for 130 systems, where we identify a candidate for the foreground lens candidate. After combining visual inspection, archival high-resolution observations, and lens subtraction, we divide the systems into different classes according to their lensing likelihood. We confirm 65 systems to be lensed. Of these, 30 are new discoveries. We successfully perform lens modelling and source reconstruction on 23 systems, where the foreground lenses are isolated galaxies and the background sources are detected in the HST images. All the systems are successfully modelled as a singular isothermal ellipsoid. The Einstein radii of the lenses and the magnifications of the background sources are consistent with previous studies. However, the background source circularised radii (between 0.34 kpc and 1.30 kpc) are $\sim$3 times smaller than the ones measured in the sub-mm/mm for a similarly selected and partially overlapping sample. We compare our lenses with those in the SLACS survey, confirming that our lens-independent selection is more effective at picking up fainter and diffuse galaxies and group lenses. This sample represents the first step towards characterising the near-IR properties and stellar masses of the gravitationally lensed dusty star-forming galaxies., Comment: 57 pages, 18 figures, 11 tables. Accepted for publication in MNRAS

Objective: The objective of this study was to assess the priorities of patients with epilepsy and their caring physicians with reference to the timing and severity of the disease. Methods: This is a national survey in which patients with epilepsy followed in 21 Italian epilepsy centers, and their caring physicians were asked to fill anonymous questionnaires to collect data on different aspects of the disease and their needs and priorities in its management. The collected information included demographics, clinical profile and diagnosis, treatment and outcome of epilepsy. The questions were designed to understand the expectations of the patients and their caring physicians and verify the degree of concordance between patient and doctor. The study population was divided in six prognostic categories: (1) Newly diagnosed epilepsy; (2) Absence of seizures for at least 2 years; (3) Absence of seizures for at least 1 year or occasional seizures; (4) Nondrug-resistant recurrent seizures; (5) drug-resistant seizures; (6) surgical candidate. Results: Of the 787 patients enrolled, 432 were women and 355 men aged 15 to 88 years (median 41 years). Disease duration ranged from 6 months to 75 years. The sample included 53 patients with newly diagnosed epilepsy, 283 without seizures for at least 2 years, 162 seizure-free for at least 1 year or with occasional seizures, 123 with nondrug-resistant recurrent seizures, 128 with drug-resistant seizures, and 38 surgical candidates. Significant differences were found between patients and physicians in terms of priorities and needs with reference to the management of the disease. While physicians tend to prioritize the information on the diagnosis and treatment of epilepsy depending on timing and severity, patients focus on the search of the cause, the side effects of drugs, and the effects of any new treatment on the control of seizures regardless of the prognostic category. In addition, physicians tend to undervalue the communication of

Purpose: The purpose of this study was to assess the priorities of patients with epilepsy and caring physicians and the correspondence between these priorities. Methods: In this multicenter cross-sectional study, patients with epilepsy attending 21 Italian epilepsy centers and their caring physicians filled anonymously questionnaires on the needs and priorities in the management of the disease. Included were questions on patients' demographics, diagnosis, treatment, and outcome of epilepsy. The concordance between patients and their physicians was assessed on various aspects of the diagnosis and care of the disease. Patients' satisfaction with communication, services, and patient–doctor relationship was also assessed. Results: Included were 432 women and 355 men aged 15 to 88 years (median: 41 years). Disease duration ranged from 6 months to 75 years. A structural/metabolic etiology predominated (52.7%), followed by a (presumed) genetic etiology (33.0%). Seizure remission was present in 56.5% of cases. Comorbidities requiring chronic treatment were present in 27.5%, and comorbidities affecting self-sufficiency in 9.5%. Psychiatric comorbidity was present in 35.0%. Patients' priorities included discovery of the cause (89.1%), use of right drug (98.7%), use of a drug without chronic side effects (94.0%), and a life without restrictions (90.4%). Physicians' priorities included choice of right drug (83.5%) and use of drugs without chronic side effects (86.8%). Priorities varied with patients' age, sex, education, and occupation. Patient–doctor relationships were at least good in most cases. The information imparted was considered unsatisfactory by 21–44% of cases on seizure circumstances and complications, side effects of drugs, limitations of daily activities, and management of physiologic or pathologic conditions. Patients declared overall satisfaction, except for appointments (21.5%) and emergencies (30.8%). Conclusion: Patients and physicians' priorities in the mana

The Star Formation Rate Density (SFRD) history of the Universe is well constrained up to redshift $z \sim 2$. At earlier cosmic epochs, the picture has been largely inferred from UV-selected galaxies (e.g. Lyman-break galaxies, LBGs). However, LBGs' inferred SFRs strongly depend on the assumed dust extinction correction, which is not well-constrained at high-$z$, while observations in the radio domain are not affected by this issue. In this work we measure the SFRD from a 1.4 GHz-selected sample of $\sim$600 galaxies in the GOODS-N field up to redshift $\sim 3.5$. We take into account the contribution of Active Galactic Nuclei from the Infrared-Radio correlation. We measure the radio luminosity function, fitted with a modified Schechter function, and derive the SFRD. The cosmic SFRD shows a rise up to $z \sim 2$ and then an almost flat plateau up to $z \sim 3.5$. Our SFRD is in agreement with the ones from other FIR/radio surveys and a factor 2 higher than those from LBG samples. We also estimate that galaxies lacking a counterpart in the HST/WFC3 H-band ($H$-dark) make up $\sim 25\%$ of the $\phi$-integrated SFRD relative to the full sample at z $\sim 3.2$, and up to $58\%$ relative to LBG samples., Comment: 20 pages, 11 figures. Accepted for publication in ApJ

We present spectroscopic measurements for 71 galaxies associated with 62 of the brightest high-redshift submillimeter sources from the Southern fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS), while targeting 85 sources which resolved into 142. We have obtained robust redshift measurements for all sources using the 12-m Array and an efficient tuning of ALMA to optimise its use as a redshift hunter, with 73 per cent of the sources having a robust redshift identification. Nine of these redshift identifications also rely on observations from the Atacama Compact Array. The spectroscopic redshifts span a range $1.41

We investigate the radio-far infrared (FIR) correlation for a sample of $28$ bright high-redshift ($1 \lesssim z \lesssim 4$) star-forming galaxies selected in the FIR from the Herschel-ATLAS fields as candidates to be strongly gravitationally lensed. The radio information comes either from high sensitivity dedicated ATCA observations at $2.1$ GHz or from cross-matches with the FIRST survey at $1.4$ GHz. By taking advantage of source brightness possibly enhanced by lensing magnification, we identify a weak evolution with redshift out to $z\lesssim 4$ of the FIR-to-radio luminosity ratio $q_{\rm FIR}$. We also find that the $q_{\rm FIR}$ parameter as a function of the radio power $L_{1.4\,\rm GHz}$ displays a clear decreasing trend, similarly to what is observed for optically/radio selected lensed quasars found in literature, yet covering a complementary region in the $q_{\rm FIR}-L_{1.4\,\rm GHz}$ diagram. We interpret such a behavior in the framework of an in-situ galaxy formation scenario, as a result of the transition from an early dust-obscured star-forming phase (mainly pinpointed by our FIR selection) to a late radio-loud quasar phase (preferentially sampled by the optical/radio selection)., Comment: 12 pages, 6 figures. Minor changes and references updated to match the published version

To be effective in teaching vocabulary, teachers must identify, use, and be creative in their methods. The English teacher should employ the proper teaching technique to tackle the problem of mastering vocabulary using the Show and the Tell method. This study was purposefully intended to look into the following topics: 1) the students’ vocabulary mastery before they were taught by using Show and Tell Method 2) the students’ vocabulary mastery after they were taughtwhatwiut using Show and Tell Method 3) the significant improvement of the students’ vocabulary mastery after using Show and Tell Method. It was a quasi-experimental study that used a pretest-posttest control group research design. The sample of the research is two claClassessess research, the researchers choose tclassesass consists list VII A 27 st,udstudentsnd VII B 26 students. The test was employed as a datgatheringng instrument, and it was in the form of a test that included a pre-test and a post-test. Both the experimental and control groups were given the test. Based on the findings of data analysis using the normality, homogeneity tests, anthatteststst. It can be concluded the alternative hypothesis was accepted while the null hypothesis was rejected. It means there were significant differences in vocabulary before and afteusinged the show and tells method for the first grade Junior High School (SMP) Negeri 4 Juwana. Furthermore, tusesed of the Show and Tell Method was important teaching vocabulary mastery because could help motivate vocabularies show and tell method; vocabulary mastery; in students of junior high school.

To be effective in teaching vocabulary, teachers must identify, use, and be creative in their methods. The English teacher should employ the proper teaching technique to tackle the problem of mastering vocabulary using the Show and the Tell method. This study was purposefully intended to look into the following topics: 1) the students’ vocabulary mastery before they were taught by using Show and Tell Method 2) the students’ vocabulary mastery after they were taughtwhatwiut using Show and Tell Method 3) the significant improvement of the students’ vocabulary mastery after using Show and Tell Method. It was a quasi-experimental study that used a pretest-posttest control group research design. The sample of the research is two claClassessess research, the researchers choose tclassesass consists list VII A 27 st,udstudentsnd VII B 26 students. The test was employed as a datgatheringng instrument, and it was in the form of a test that included a pre-test and a post-test. Both the experimental and control groups were given the test. Based on the findings of data analysis using the normality, homogeneity tests, anthatteststst. It can be concluded the alternative hypothesis was accepted while the null hypothesis was rejected. It means there were significant differences in vocabulary before and afteusinged the show and tells method for the first grade Junior High School (SMP) Negeri 4 Juwana. Furthermore, tusesed of the Show and Tell Method was important teaching vocabulary mastery because could help motivate vocabularies show and tell method; vocabulary mastery; in students of junior high school.

To be effective in teaching vocabulary, teachers must identify, use, and be creative in their methods. The English teacher should employ the proper teaching technique to tackle the problem of mastering vocabulary using the Show and the Tell method. This study was purposefully intended to look into the following topics: 1) the students’ vocabulary mastery before they were taught by using Show and Tell Method 2) the students’ vocabulary mastery after they were taughtwhatwiut using Show and Tell Method 3) the significant improvement of the students’ vocabulary mastery after using Show and Tell Method. It was a quasi-experimental study that used a pretest-posttest control group research design. The sample of the research is two claClassessess research, the researchers choose tclassesass consists list VII A 27 st,udstudentsnd VII B 26 students. The test was employed as a datgatheringng instrument, and it was in the form of a test that included a pre-test and a post-test. Both the experimental and control groups were given the test. Based on the findings of data analysis using the normality, homogeneity tests, anthatteststst. It can be concluded the alternative hypothesis was accepted while the null hypothesis was rejected. It means there were significant differences in vocabulary before and afteusinged the show and tells method for the first grade Junior High School (SMP) Negeri 4 Juwana. Furthermore, tusesed of the Show and Tell Method was important teaching vocabulary mastery because could help motivate vocabularies show and tell method; vocabulary mastery; in students of junior high school.

We present spectroscopic measurements for 71 galaxies associated with 62 of the brightest high-redshift submillimetre sources from the Southern fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS), while targeting 85 sources which resolved into 142. We have obtained robust redshift measurements for all sources using the 12-m Array and an efficient tuning of ALMA to optimize its use as a redshift hunter, with 73 per cent of the sources having a robust redshift identification. Nine of these redshift identifications also rely on observations from the Atacama Compact Array. The spectroscopic redshifts span a range 1.41 < z < 4.53 with a mean value of 2.75, and the CO emission line full-width at half-maxima range between $\rm 110\, km\, s^{-1} \lt FWHM \lt 1290\, km\, s^{-1}$ with a mean value of ∼500 km s−1, in line with other high-z samples. The derived CO(1-0) luminosity is significantly elevated relative to line-width to CO(1-0) luminosity scaling relation, which is suggestive of lensing magnification across our sources. In fact, the distribution of magnification factors inferred from the CO equivalent widths is consistent with expectations from galaxy–galaxy lensing models, though there is a hint of an excess at large magnifications that may be attributable to the additional lensing optical depth from galaxy groups or clusters.

To be effective in teaching vocabulary, teachers must identify, use, and be creative in their methods. The English teacher should employ the proper teaching technique to tackle the problem of mastering vocabulary using the Show and the Tell method. This study was purposefully intended to look into the following topics: 1) the students’ vocabulary mastery before they were taught by using Show and Tell Method 2) the students’ vocabulary mastery after they were taughtwhatwiut using Show and Tell Method 3) the significant improvement of the students’ vocabulary mastery after using Show and Tell Method. It was a quasi-experimental study that used a pretest-posttest control group research design. The sample of the research is two claClassessess research, the researchers choose tclassesass consists list VII A 27 st,udstudentsnd VII B 26 students. The test was employed as a datgatheringng instrument, and it was in the form of a test that included a pre-test and a post-test. Both the experimental and control groups were given the test. Based on the findings of data analysis using the normality, homogeneity tests, anthatteststst. It can be concluded the alternative hypothesis was accepted while the null hypothesis was rejected. It means there were significant differences in vocabulary before and afteusinged the show and tells method for the first grade Junior High School (SMP) Negeri 4 Juwana. Furthermore, tusesed of the Show and Tell Method was important teaching vocabulary mastery because could help motivate vocabularies show and tell method; vocabulary mastery; in students of junior high school.

To be effective in teaching vocabulary, teachers must identify, use, and be creative in their methods. The English teacher should employ the proper teaching technique to tackle the problem of mastering vocabulary using the Show and the Tell method. This study was purposefully intended to look into the following topics: 1) the students’ vocabulary mastery before they were taught by using Show and Tell Method 2) the students’ vocabulary mastery after they were taughtwhatwiut using Show and Tell Method 3) the significant improvement of the students’ vocabulary mastery after using Show and Tell Method. It was a quasi-experimental study that used a pretest-posttest control group research design. The sample of the research is two claClassessess research, the researchers choose tclassesass consists list VII A 27 st,udstudentsnd VII B 26 students. The test was employed as a datgatheringng instrument, and it was in the form of a test that included a pre-test and a post-test. Both the experimental and control groups were given the test. Based on the findings of data analysis using the normality, homogeneity tests, anthatteststst. It can be concluded the alternative hypothesis was accepted while the null hypothesis was rejected. It means there were significant differences in vocabulary before and afteusinged the show and tells method for the first grade Junior High School (SMP) Negeri 4 Juwana. Furthermore, tusesed of the Show and Tell Method was important teaching vocabulary mastery because could help motivate vocabularies show and tell method; vocabulary mastery; in students of junior high school.

To be effective in teaching vocabulary, teachers must identify, use, and be creative in their methods. The English teacher should employ the proper teaching technique to tackle the problem of mastering vocabulary using the Show and the Tell method. This study was purposefully intended to look into the following topics: 1) the students’ vocabulary mastery before they were taught by using Show and Tell Method 2) the students’ vocabulary mastery after they were taughtwhatwiut using Show and Tell Method 3) the significant improvement of the students’ vocabulary mastery after using Show and Tell Method. It was a quasi-experimental study that used a pretest-posttest control group research design. The sample of the research is two claClassessess research, the researchers choose tclassesass consists list VII A 27 st,udstudentsnd VII B 26 students. The test was employed as a datgatheringng instrument, and it was in the form of a test that included a pre-test and a post-test. Both the experimental and control groups were given the test. Based on the findings of data analysis using the normality, homogeneity tests, anthatteststst. It can be concluded the alternative hypothesis was accepted while the null hypothesis was rejected. It means there were significant differences in vocabulary before and afteusinged the show and tells method for the first grade Junior High School (SMP) Negeri 4 Juwana. Furthermore, tusesed of the Show and Tell Method was important teaching vocabulary mastery because could help motivate vocabularies show and tell method; vocabulary mastery; in students of junior high school.

We present spectroscopic measurements for 71 galaxies associated with 62 of the brightest high-redshift submillimetre sources from the Southern fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS), while targeting 85 sources which resolved into 142. We have obtained robust redshift measurements for all sources using the 12-m Array and an efficient tuning of ALMA to optimize its use as a redshift hunter, with 73 per cent of the sources having a robust redshift identification. Nine of these redshift identifications also rely on observations from the Atacama Compact Array. The spectroscopic redshifts span a range 1.41 < z < 4.53 with a mean value of 2.75, and the CO emission line full-width at half-maxima range between 110 km s(-1) < FWHM < 1290 km s(-1) with a mean value of similar to 500 km s(-1), in line with other high-z samples. The derived CO(1-0) luminosity is significantly elevated relative to line-width to CO(1-0) luminosity scaling relation, which is suggestive of lensing magnification across our sources. In fact, the distribution of magnification factors inferred from the CO equivalent widths is consistent with expectations from galaxy-galaxy lensing models, though there is a hint of an excess at large magnifications that may be attributable to the additional lensing optical depth from galaxy groups or clusters.

The Star Formation Rate Density (SFRD) history of the Universe is well constrained up to redshift $z \sim 2$. At earlier cosmic epochs, the picture has been largely inferred from UV-selected galaxies (e.g. Lyman-break galaxies, LBGs). However, LBGs' inferred SFRs strongly depend on the assumed dust extinction correction, which is not well-constrained at high-$z$, while observations in the radio domain are not affected by this issue. In this work we measure the SFRD from a 1.4 GHz-selected sample of $\sim$600 galaxies in the GOODS-N field up to redshift $\sim 3.5$. We take into account the contribution of Active Galactic Nuclei from the Infrared-Radio correlation. We measure the radio luminosity function, fitted with a modified Schechter function, and derive the SFRD. The cosmic SFRD shows a rise up to $z \sim 2$ and then an almost flat plateau up to $z \sim 3.5$. Our SFRD is in agreement with the ones from other FIR/radio surveys and a factor 2 higher than those from LBG samples. We also estimate that galaxies lacking a counterpart in the HST/WFC3 H-band ($H$-dark) make up $\sim 25\%$ of the $\phi$-integrated SFRD relative to the full sample at z $\sim 3.2$, and up to $58\%$ relative to LBG samples., Comment: 20 pages, 11 figures. Accepted for publication in ApJ

We investigate the radio-far infrared (FIR) correlation for a sample of $28$ bright high-redshift ($1 \lesssim z \lesssim 4$) star-forming galaxies selected in the FIR from the Herschel-ATLAS fields as candidates to be strongly gravitationally lensed. The radio information comes either from high sensitivity dedicated ATCA observations at $2.1$ GHz or from cross-matches with the FIRST survey at $1.4$ GHz. By taking advantage of source brightness possibly enhanced by lensing magnification, we identify a weak evolution with redshift out to $z\lesssim 4$ of the FIR-to-radio luminosity ratio $q_{\rm FIR}$. We also find that the $q_{\rm FIR}$ parameter as a function of the radio power $L_{1.4\,\rm GHz}$ displays a clear decreasing trend, similarly to what is observed for optically/radio selected lensed quasars found in literature, yet covering a complementary region in the $q_{\rm FIR}-L_{1.4\,\rm GHz}$ diagram. We interpret such a behavior in the framework of an in-situ galaxy formation scenario, as a result of the transition from an early dust-obscured star-forming phase (mainly pinpointed by our FIR selection) to a late radio-loud quasar phase (preferentially sampled by the optical/radio selection)., Comment: 12 pages, 6 figures. Minor changes and references updated to match the published version

We present spectroscopic measurements for 71 galaxies associated with 62 of the brightest high-redshift submillimeter sources from the Southern fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS), while targeting 85 sources which resolved into 142. We have obtained robust redshift measurements for all sources using the 12-m Array and an efficient tuning of ALMA to optimise its use as a redshift hunter, with 73 per cent of the sources having a robust redshift identification. Nine of these redshift identifications also rely on observations from the Atacama Compact Array. The spectroscopic redshifts span a range $1.41

Using the weak gravitational lensing data from the Hyper Suprime-Cam Subaru Strategic Program (HSC survey), we study the potential of different stellar mass estimates in tracing halo mass. We consider galaxies with $\log {M_{\star}/M_{\odot}}>11.5$ at 0.2 < z < 0.5 with carefully measured light profiles and clusters from the redMaPPer and CAMIRA richness-based algorithms. We devise a method (the "TopN" test) to evaluate the scatter in the halo mass-observable relation for different tracers and inter-compare halo mass proxies in four number density bins using stacked galaxy-galaxy lensing profiles. This test reveals three key findings. The stellar mass based on cModel photometry or aperture luminosity within R<30 kpc is a poor proxy of halo mass. In contrast, the stellar mass of the outer envelope is an excellent halo mass proxy. The stellar mass within R=[50,100] kpc, M*[50,100], has performance comparable to the state-of-the-art richness-based cluster finders at $\log{M_{\rm vir}/M_{\odot}}>14.0$ and could be a better halo mass tracer at lower halo masses. Finally, using N-body simulations, we find that the lensing profiles of massive halos selected by M*[50,100] are consistent with the expectation for a sample without projection or mis-centering effects. On the other hand, Richness-selected clusters display an excess at R~1 Mpc in their lensing profiles, which may suggest a more significant impact from selection biases. These results suggest that Mstar-based tracers have distinct advantages in identifying massive halos, which could open up new avenues for cluster cosmology., Comment: 28 pages, 12 figures, 1 table, 7 appendices. Submitted to MNRAS. Codes available at https://github.com/dr-guangtou/jianbing Data available at https://doi.org/10.5281/zenodo.5259075

Galaxy mergers are thought to be one of the main mechanisms of the mass assembly of galaxies. Recently, many works have suggested a possible increase in the fraction of major mergers in the early Universe, reviving the debate on which processes (e.g., cold accretion, star formation, mergers) most contribute to the mass build-up of galaxies through cosmic time. To estimate the importance of major mergers in this context, we make use of the new data collected by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE), which observed the [CII] 158 $\mu$m emission line from a sample of 75 main-sequence star-forming galaxies at 4.4 < z < 5.9. We used, for the first time, the morpho-kinematic information provided by the [CII] emission to obtain the fraction of major mergers ($f_{MM}$) at z~5. By adopting different prescriptions for the merger timescales ($T_{MM}$), we converted this fraction into the merger rate per galaxy ($R_{MM}$) and per volume ($\Gamma_{MM}$). We then combined our results with those at lower redshifts from the literature, computing the cosmic evolution of the merger fraction. This is described by a rapid increase from z~0 to higher redshifts, a peak at z~3, and a slow decrease towards earlier epochs. Depending on the timescale prescription used, this fraction translates into a merger rate ranging between ~0.1 and ~4.0 Gyr$^{-1}$ at z~5. Finally, we compare the specific star formation and star-formation rate density with the analogous quantities from major mergers. Our new ALPINE data reveal the presence of a significant merging activity in the early Universe. However, whether this population of mergers can provide a relevant contribution to the galaxy mass assembly at these redshifts and through the cosmic epochs is strongly dependent on the assumption of the merger timescale., Comment: Accepted for publication in section 4. Extragalactic astronomy of Astronomy and Astrophysics

Secondary halo properties beyond mass, such as the mass accretion rate (MAR), concentration, and the half mass scale, are essential in understanding the formation of large-scale structure and dark matter halos. In this paper, we study the impact of secondary halo properties on the galaxy-galaxy lensing observable, $\Delta\Sigma$. We build an emulator trained on N-body simulations to model $\Delta\Sigma$ and quantify the impact of different secondary parameters on the $\Delta\Sigma$ profile. We focus on the impact of MAR on $\Delta\Sigma$. We show that a 3$\sigma$ detection of variations in MAR at fixed halo mass could be achieved with the Hyper Suprime Cam survey in combination with a proxy for MAR with scatter $\sigma_{\Gamma_\mathrm{dyn}|\mathrm{obs}}<1.5$. We show that the full radial profile of $\Delta\Sigma$ depends on secondary properties at fixed halo mass. Consequently, an emulator that can perform full shape fitting yields better than 2 times improvement upon the constraints on MAR than only using the outer part of the halo. Finally, we highlight that miscentering and MAR impact the radial profile of $\Delta\Sigma$ in a similar fashion, implying that miscentering and MAR need to be modeled jointly for unbiased estimates of both effects. We show that present-day lensing data sets have the statistical capability to place constraints on halo MAR. Our analysis opens up new possibilities for observationally measuring the assembly history of the dark matter halos that host galaxies and clusters.

The dust content of normal galaxies and the dust mass density (DMD) at high-z (z>4) are unconstrained given the source confusion and the sensitivity limitations of previous observations. The ALMA Large Program to INvestigate [CII] at Early Times (ALPINE), which targeted 118 UV-selected star-forming galaxies at 4.4

Strong gravitational lensing, which can make a background source galaxy appears multiple times due to its light rays being deflected by the mass of one or more foreground lens galaxies, provides astronomers with a powerful tool to study dark matter, cosmology and the most distant Universe. PyAutoLens is an open-source Python 3.6+ package for strong gravitational lensing, with core features including fully automated strong lens modeling of galaxies and galaxy clusters, support for direct imaging and interferometer datasets and comprehensive tools for simulating samples of strong lenses. The API allows users to perform ray-tracing by using analytic light and mass profiles to build strong lens systems. Accompanying PyAutoLens is the autolens workspace (see https://github.com/Jammy2211/autolens_workspace), which includes example scripts, lens datasets and the HowToLens lectures in Jupyter notebook format which introduce non experts to strong lensing using PyAutoLens. Readers can try PyAutoLens right now by going to the introduction Jupyter notebook on Binder (see https://mybinder.org/v2/gh/Jammy2211/autolens_workspace/master) or checkout the readthedocs (see https://pyautolens.readthedocs.io/en/latest/) for a complete overview of PyAutoLens's features., Comment: 2 pages, 1 figure

Human bocaviruses (HBoVs) are recently described as human emergent viruses, especially in young children. In this study, we undertook a systematic review and meta-analysis to estimate their prevalence in Europe. PubMed, Web of Science and Scopus databases were systematically screened for clinical studies, up to October 2020. Study eligibility criteria were primary full-text articles from clinical studies, conducted using valid screening test methods and published in peer-reviewed journals, in English or Spanish and from European countries. The overall pooled prevalence, prevalence by country as well as the prevalence of HBoV as a single or co-pathogen were estimated using a random-effects model. Sub-group and meta-regression analyses explored potential sources of heterogeneity in the data. A total of 35 studies involving 32,656 subjects from 16 European countries met the inclusion criteria. Heterogeneity (I2 = 97.0%, p < .01) was seen among studies; HBoV prevalence varied from 2.0 to 45.69% with a pooled estimate of 9.57% (95%CI 7.66-11.91%). The HBoV prevalence both as a single infection (3.99%; 95%CI 2.99-5.31%) or as co-infection with other viruses (5.06%; 95%CI 3.88-6.58%) was also analysed. On a geographic level, prevalence by country did not show statistical differences, ranging from 3.24% (Greece) to 21.05% (Denmark). An odds ratio analysis was also included in order to evaluate the relevance of the variable ‘age’ as a risk factor of HBoV infection in children <5 years old. The OR value of 1.77 (95%CI 1.13-2.77; p < .01) indicated that being <5 years old is a risk factor for HBoV infection. This study showed that HBoV has a moderate prevalence among European countries

Feedback-driven winds from star formation or active galactic nuclei might be a relevant channel for the abrupt quenching of star formation in massive galaxies. However, both observations and simulations support the idea that these processes are non-conflictingly co-evolving and self-regulating. Furthermore, evidence of disruptive events that are capable of fast quenching is rare, and constraints on their statistical prevalence are lacking. Here we present a massive starburst galaxy at redshift z = 1.4, which is ejecting 46 ± 13% of its molecular gas mass at a startling rate of ≳10,000 M⊙ yr−1. A broad component that is red-shifted from the galaxy emission is detected in four (low and high J) CO and [C i] transitions and in the ionized phase, which ensures a robust estimate of the expelled gas mass. The implied statistics suggest that similar events are potentially a major star-formation quenching channel. However, our observations provide compelling evidence that this is not a feedback-driven wind, but rather material from a merger that has been probably tidally ejected. This finding challenges some literature studies in which the role of feedback-driven winds might be overstated.

Using the weak gravitational lensing data from the Hyper Suprime-Cam Subaru Strategic Program (HSC survey), we study the potential of different stellar mass estimates in tracing halo mass. We consider galaxies with $\log {M_{\star}/M_{\odot}}>11.5$ at 0.2 < z < 0.5 with carefully measured light profiles and clusters from the redMaPPer and CAMIRA richness-based algorithms. We devise a method (the "TopN" test) to evaluate the scatter in the halo mass-observable relation for different tracers and inter-compare halo mass proxies in four number density bins using stacked galaxy-galaxy lensing profiles. This test reveals three key findings. The stellar mass based on cModel photometry or aperture luminosity within R<30 kpc is a poor proxy of halo mass. In contrast, the stellar mass of the outer envelope is an excellent halo mass proxy. The stellar mass within R=[50,100] kpc, M*[50,100], has performance comparable to the state-of-the-art richness-based cluster finders at $\log{M_{\rm vir}/M_{\odot}}>14.0$ and could be a better halo mass tracer at lower halo masses. Finally, using N-body simulations, we find that the lensing profiles of massive halos selected by M*[50,100] are consistent with the expectation for a sample without projection or mis-centering effects. On the other hand, Richness-selected clusters display an excess at R~1 Mpc in their lensing profiles, which may suggest a more significant impact from selection biases. These results suggest that Mstar-based tracers have distinct advantages in identifying massive halos, which could open up new avenues for cluster cosmology., Comment: 28 pages, 12 figures, 1 table, 7 appendices. Submitted to MNRAS. Codes available at https://github.com/dr-guangtou/jianbing Data available at https://doi.org/10.5281/zenodo.5259075

Galaxy mergers are thought to be one of the main mechanisms of the mass assembly of galaxies. Recently, many works have suggested a possible increase in the fraction of major mergers in the early Universe, reviving the debate on which processes (e.g., cold accretion, star formation, mergers) most contribute to the mass build-up of galaxies through cosmic time. To estimate the importance of major mergers in this context, we make use of the new data collected by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE), which observed the [CII] 158 $\mu$m emission line from a sample of 75 main-sequence star-forming galaxies at 4.4 < z < 5.9. We used, for the first time, the morpho-kinematic information provided by the [CII] emission to obtain the fraction of major mergers ($f_{MM}$) at z~5. By adopting different prescriptions for the merger timescales ($T_{MM}$), we converted this fraction into the merger rate per galaxy ($R_{MM}$) and per volume ($\Gamma_{MM}$). We then combined our results with those at lower redshifts from the literature, computing the cosmic evolution of the merger fraction. This is described by a rapid increase from z~0 to higher redshifts, a peak at z~3, and a slow decrease towards earlier epochs. Depending on the timescale prescription used, this fraction translates into a merger rate ranging between ~0.1 and ~4.0 Gyr$^{-1}$ at z~5. Finally, we compare the specific star formation and star-formation rate density with the analogous quantities from major mergers. Our new ALPINE data reveal the presence of a significant merging activity in the early Universe. However, whether this population of mergers can provide a relevant contribution to the galaxy mass assembly at these redshifts and through the cosmic epochs is strongly dependent on the assumption of the merger timescale., Comment: Accepted for publication in section 4. Extragalactic astronomy of Astronomy and Astrophysics

Secondary halo properties beyond mass, such as the mass accretion rate (MAR), concentration, and the half mass scale, are essential in understanding the formation of large-scale structure and dark matter halos. In this paper, we study the impact of secondary halo properties on the galaxy-galaxy lensing observable, $\Delta\Sigma$. We build an emulator trained on N-body simulations to model $\Delta\Sigma$ and quantify the impact of different secondary parameters on the $\Delta\Sigma$ profile. We focus on the impact of MAR on $\Delta\Sigma$. We show that a 3$\sigma$ detection of variations in MAR at fixed halo mass could be achieved with the Hyper Suprime Cam survey in combination with a proxy for MAR with scatter $\sigma_{\Gamma_\mathrm{dyn}|\mathrm{obs}}<1.5$. We show that the full radial profile of $\Delta\Sigma$ depends on secondary properties at fixed halo mass. Consequently, an emulator that can perform full shape fitting yields better than 2 times improvement upon the constraints on MAR than only using the outer part of the halo. Finally, we highlight that miscentering and MAR impact the radial profile of $\Delta\Sigma$ in a similar fashion, implying that miscentering and MAR need to be modeled jointly for unbiased estimates of both effects. We show that present-day lensing data sets have the statistical capability to place constraints on halo MAR. Our analysis opens up new possibilities for observationally measuring the assembly history of the dark matter halos that host galaxies and clusters.

Strong gravitational lensing, which can make a background source galaxy appears multiple times due to its light rays being deflected by the mass of one or more foreground lens galaxies, provides astronomers with a powerful tool to study dark matter, cosmology and the most distant Universe. PyAutoLens is an open-source Python 3.6+ package for strong gravitational lensing, with core features including fully automated strong lens modeling of galaxies and galaxy clusters, support for direct imaging and interferometer datasets and comprehensive tools for simulating samples of strong lenses. The API allows users to perform ray-tracing by using analytic light and mass profiles to build strong lens systems. Accompanying PyAutoLens is the autolens workspace (see https://github.com/Jammy2211/autolens_workspace), which includes example scripts, lens datasets and the HowToLens lectures in Jupyter notebook format which introduce non experts to strong lensing using PyAutoLens. Readers can try PyAutoLens right now by going to the introduction Jupyter notebook on Binder (see https://mybinder.org/v2/gh/Jammy2211/autolens_workspace/master) or checkout the readthedocs (see https://pyautolens.readthedocs.io/en/latest/) for a complete overview of PyAutoLens's features., Comment: 2 pages, 1 figure

The dust content of normal galaxies and the dust mass density (DMD) at high-z (z>4) are unconstrained given the source confusion and the sensitivity limitations of previous observations. The ALMA Large Program to INvestigate [CII] at Early Times (ALPINE), which targeted 118 UV-selected star-forming galaxies at 4.4

In this paper we present an attempt to estimate the redshift evolution of the molecular to neutral gas mass ratio within galaxies (at fixed stellar mass). For a sample of five nearby grand design spirals located on the Main Sequence (MS) of star forming galaxies, we exploit maps at 500 pc resolution of stellar mass and star formation rate ($M_{\star}$ and SFR). For the same cells, we also have estimates of the neutral ($M_{\rm HI}$) and molecular ($M_{\rm H_2}$) gas masses. To compute the redshift evolution we exploit two relations: {\it i)} one between the molecular-to-neutral mass ratio and the total gas mass ($M_{\rm gas}$), whose scatter shows a strong dependence with the distance from the spatially resolved MS, and {\it ii)} the one between $\log(M_{\rm{H_2}}/M_{\star})$ and $\log(M_{\rm{HI}}/M_{\star})$. For both methods, we find that $M_{\rm H_2}$/$M_{\rm HI}$ within the optical radius slightly decreases with redshift, contrary to common expectations of galaxies becoming progressively more dominated by molecular hydrogen at high redshifts. We discuss possible implications of this trend on our understanding of the internal working of high redshift galaxies., Comment: Letter accepted for publication on MNRAS