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Polycyclic Aromatic Hydrocarbons (PAHs) are carbon-based molecules resulting from the union of aromatic rings and related species, which are likely responsible for strong infrared emission features (3.3, 6.2, 7.7, 8.6, 11.3 and 12.7 microns). In this work, using a sample of 50 Seyfert galaxies (DL300-400) as well as neutral species. By subtracting the spectrum of the central source from the total, we compare the PAH emission in the central vs extended region of a small sample of AGN. In contrast to the findings for the central regions of AGN-dominated systems, the PAH ratios measured in the extended regions of both type 1 and type 2 Seyfert galaxies can be explained assuming similar PAH molecular size distribution and ionized fractions of molecules to those seen in central regions of star-forming galaxies (100, Comment: 29 pages, 21 figures, 6 tables, MNRAS, accepted 2021 October 22

The species Eucalyptus globulus, Eucalyptus nitens and Pinus radiata, are important supplies for the production of cellulose pulp in the world market, which can be used for the production of cellulose nanofibrils (CNFs). Understanding how the characteristics of different raw materials affect the production and final properties of nanofibrillated celluloses is very useful, both for the pulp industry and for the end user. The aim of this research was to determine how the chemical and structural differences of the commercial Kraft pulps of E. globulus, E. nitens and P. radiata affect the production and the morphological and rheological characteristics of the CNFs produced through an enzymatic-mechanical process. On one hand, the results showed that pine fibers were easier to deconstruct than eucalyptus fibers, however, pine CNFs were found to have the largest fibril width and a lower aspect ratio (length /width). On the other hand, the pulp of E. globulus, was the one that obtained a better aspect ratio and higher intrinsic viscosity.

While water is indispensable for life, around 785 million people do not have access to basic drinking water. Heavy metals present high toxicity at low concentrations, are non-biodegradable and easy to accumulate in living organisms such as human body, causing serious diseases or even death. Copper is usually found at high concentrations in wastewater due to its extensive use in several industrial applications, and effective copper removal systems must be developed. The present work aims at developing effective TEMPO-oxidized cellulose nanofibers (CNFs) based systems able to adsorb Cu(II) in adsorption columns. CNFs were partially modified with alkyl ketene dimer (AKD) to avoid regelation during flowing through the column, as it was experienced for those unmodified. Calcium alginate beads were used as reference, as there is extensive literature on their use as Cu(II) adsorbent. Breakthrough curves were obtained and modelled according to Bohart-Adams, Yoon-Nelson and Thomas models, concluding that the adsorption rate of CNFs was significantly higher than in the case of calcium alginate beads due to the negative effects of highly charged water and diffusion through the beads. In addition, CNF-based adsorption systems demonstrated to be effective, especially at the beginning of the tests, as they exhibited a well-defined sigmoidal behavior, which was not observed in the case of the calcium alginate beads. On the contrary, the adsorption capacity was higher in the case of the alginate-based system, mainly due to the higher carboxyl content and ion exchange capacity. Overall, the present work shows the feasibility of using a high-performance bio-based and nanostructured cellulose material as Cu(II) adsorbent by means of a fast, simple, and effective chemical modification based on surface esterification.

This viewpoint intends to show recent open issues of using coarse grained models in molecular dynamics simulation. It reviews the current knowledge of the comparison between experimental and simulation data of structural and physical chemical properties that depend on the hydrophilic and hydrophobic behavior of the molecule.

Several agricultural wastes, such as the residues of the winemaking industry, have been tested using traditional chemical methods of pulping aimed to obtain bleached pulp, but only low yields and poor fiber quality have been achieved so far. In this work, we evaluate a two-stage chemi-thermomechanical pulping (CTMP) to assess the feasibility to add value to the residues of the wine industry (grape stalks and vine shoots) by obtaining fibers with papermaking and/or cardboard quality. The first stage of the process evaluates different conditions with low chemical charges of Na2SO3 and/or NaOH (3 to 5% on wood basis) at different temperatures (130 to 160 °C) for 60 min. The second stage consists of a mechanical refining that converts fiber bundles and shives into pulps. CTMP pulping performed with 5% Na2SO3 at 160 °C from grape stalks and vine shoots showed the best combination of fiber quality regarding higher screened pulp yield, lower rejects and fines content, and adequate drainability. Results showed that pulp from waste lignocellulosic of the winery industry can be produced by a green approach (low chemical charge and severity in CTMP pulping) and became an alternative for paper, packaging, fiber additives, or new biobased materials.

Lignocellulose nanofibrils (LCNFs) are nano-objects produced in aqueous suspension by industrially adaptable methods, with a high yield, low production cost and the potential to replace or complement delignified cellulose nanofibrils in their current applications. To this end, it is necessary to understand how their constituents affect the production and characteristics of the final product. This review explores the most recent results on the effect of the residual amount of lignin and hemicelluloses on the properties of LCNF suspensions. In the current literature, there is a consensus on hemicelluloses, a larger amount of which favors the mechanical fibrillation process, with mannans providing the greatest benefits. Meanwhile, there is no consensus on the effect of residual lignin on mechanical fibrillation, since it can act as an antioxidant, which promotes fibrillation, or as a cementing agent, which hinders fibrillation and, therefore, the production of LCNFs.

The lipophilicity of cholesterol was investigated by using coarse-grained molecular dynamics and umbrella sampling. The previous coarse-grained cholesterol models in the literature are more hydrophobic than our model. The Gibbs free energy of transferring cholesterol from the octanol phase to water phase (Δ

Based on theoretical spectra computed using Density Functional Theory we study the properties of Polycyclic Aromatic Hydrocarbons (PAH). In particular using bin-average spectra of PAH molecules with varying number of carbons we investigate how the intensity of the mid-infrared emission bands, 3.3, 6.2, 7.7 and 11.3 microns, respond to changes in the number of carbons, charge of the molecule, and the hardness of the radiation field that impinges the molecule. We confirm that the 6.2/7.7 band ratio is a good predictor for the size of the PAH molecule (based on the number of carbons present). We also investigate the efficacy of the 11.3/3.3 ratio to trace the size of PAH molecules and note the dependence of this ratio on the hardness of the radiation field. While the ratio can potentially also be used to trace PAH molecular size, a better understanding of the impact of the underlying radiation field on the 3.3 microns feature and the effect of the extinction on the ratio should be evaluated. The newly developed diagnostics are compared to band ratios measured in a variety of galaxies observed with the Infrared Spectrograph on board the Spitzer Space Telescope. We demonstrate that the band ratios can be used to probe the conditions of the interstellar medium in galaxies and differentiate between environments encountered in normal star forming galaxies and Active Galactic Nuclei. Our work highlights the immense potential that PAH observations with the James Webb Space Telescope will have on our understanding of the PAH emission itself and of the physical conditions in galaxies near and far., Comment: 14 pages; 12 figures. Final version accepted for publication in MNRAS, accepted 2021 March 31

We present the results of an integral field spectroscopy survey of a sample of dusty (ultra) luminous infrared galaxies (U/LIRGs) at 2 < z < 2.5 using KMOS on the Very Large Telescope. The sample has been drawn from Herschel deep field surveys and benefits from ancillary multiwavelength data. Our goal is to investigate the physical characteristics, kinematics, and the drivers of star formation in the galaxies whose contribution dominates the peak of the cosmic star formation density. Two-thirds of the sample are main-sequence galaxies in contrast to the starburst nature of local U/LIRGs. Our kinematic study, unique in its focus on z ∼ 2 dusty star-forming galaxies, uses the H α emission line to find that ∼40 per cent appear to be isolated discs based on the ratio of rotational velocity to the velocity dispersion, suggesting steady-state mechanisms are sufficient to power the large star formation rates (SFRs). The ratio of obscured to unobscured star formation indicates the sample of galaxies experiences less dust obscuration compared to intermediate and local counterparts, while also hosting cooler dust than local U/LIRGs. In addition to H α we detect [N II] 6583 Å in our targets and show the gas-phase metallicities do not exhibit the metal deficiency of local U/LIRGs. These results indicate that, despite their extreme IR luminosity, the underlying mechanisms driving the massive SFRs found at cosmic noon are due to scaled up disc galaxies as opposed to mergers. We want to thank the anonymous referee for their insightful comments and suggestions that improved the quality of this paper. The analysis in this paper is based on observations made with ESO Telescopes at the La Silla Paranal Observatory under run IDs: 092.B0769(A) and 097.B-0186(A). D.R., I.G.-B., and K.G. acknowledge support from STFC through grant ST/S000488/1. G.E.M. acknowledges the Villum Fonden research grant 13160 `Gas to stars, stars to dust: tracing star formation across cosmic time' and the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation under the grant No. 140. N.T. acknowledges support from STFC through grants ST/N002717/1 and ST/S001409/1. M.P.S. acknowledges support from the Comunidad de Madrid through Atracci ' on de Talento Investigador Grant 2018-T1/TIC-11035. Peerreview

Background Resveratrol (RES) is a polyphenol which has attracted great interest in the academic and industrial communities due to its natural origin and potential health benefits. Nevertheless, the administration of RES is restrained by its properties, such as poor water solubility, lack of stability due to light-induced isomerization, as well as auto-oxidation and rapid metabolization. Therefore, recently, nanotechnology, through different approaches, emerged as a potential solution to improve RES solubility and stability enabling its therapeutic use. Scope and approach In the present review, current research findings, developments and trends regarding novel nanocarriers for RES delivery are discussed. An overview of the research progress regarding the nanoencapsulation of RES is presented. Particular focus is cast on the composition, physicochemical and surface characteristics of the myriad of nanocarriers so far produced, since these features relevantly influence the intracellular delivery of RES. Key findings and conclusions The application of nanocarriers towards RES delivery reduced the physicochemical restrictions related to the administration of this phytochemical. The improvements conveyed by nanocarriers regarding RES stability and solubility may lead to an upgrade in the in vitro and in vivo bioactivity of RES.

Resveratrol (RES), also known as 3,5,4'-trihydroxystilbene, is a polyphenolic phytoalexin that has been widely researched in the past decade due to its recognized numerous biological activities. Despite the potential benefits of RES, its effective use is limited due to its poor solubility, photosensitivity and rapid metabolism, which strongly undermine RES bioavailability and bioactivity. Thereby, recently, nanotechnology appeared as a potential strategy to circumvent RES physicochemical and pharmacokinetics constrains. However, only few studies have addressed the crucial in vivo suitability of the developed delivery systems to improve RES efficacy. Facing this scenario, in the present review, it is intended to present and discuss the in vivo resveratrol bioavailability and bioactivity, following its encapsulation or conjugation in nanotechnology-based carriers, contemplating their pharmacokinetics effectiveness.

Bleached kraft pulps from Eucalyptus benthamii, E. globulus, E. nitens and E. nitens × E. globulus hybrid were prepared in laboratory scale and upgraded to dissolving-grade via cold caustic extraction (CCE) and dilute acid hydrolysis. The CCE reduced the alkali solubility (S18) of bleached kraft pulps from 11.8–16.4% to 4.5–6.3% after extraction with 5% (w/v) NaOH, and to 0.9–1.7% after extraction with 10% (w/v) NaOH. The dilute acid hydrolysis with 3% H2SO4 reduced the intrinsic viscosity of CCE-treated kraft pulps from 800–900 to 110–450 ml/g. E. nitens and E. benthamii displayed the most contrasting values for S18 and intrinsic viscosity after CCE and acid hydrolysis treatments. The X-ray diffraction results showed that the crystallinity index of bleached kraft pulps followed the order: E. benthamii > E. globulus > En × Eg > E. nitens. Regarding cellulose reactivity, the Fock reactivity of the bleached kraft pulps was in the range of 34.7–41.3%. After CCE, the pulps reactivity was reduced to 13.7–25.4%, whereas after acid hydrolysis it was increased to 40.7–87.5%. E. benthamii and E. nitens pulps showed to be the less reactive pulps after pulp activation via acid hydrolysis, whereas E. globulus and the hybrid showed to be the most reactive pulps towards xanthation. It was observed that different Eucalyptus species can lead to kraft pulps with different requirements towards xanthation, and that the inherent features of wood and how they are processed are of outmost importance for the final use of kraft-based dissolving pulp from a given wood species.

arXiv:2103.03584v1, We use the SPace Infrared telescope for Cosmology and Astrophysics (SPICA) project as a template to demonstrate how deep spectrophotometric surveys covering large cosmological volumes over extended fields (1–15 deg2) with a mid-IR imaging spectrometer (17–36 µm) in conjunction with deep photometry with a far-IR camera, at wavelengths which are not affected by dust extinction can answer the most crucial questions in current galaxy evolution studies. A SPICA-like mission will be able for the first time to provide an unobscured three-dimensional (3D, i.e. x, y, and redshift z) view of galaxy evolution back to an age of the universe of less than ∼ 2 Gyrs, in the mid-IR rest frame. This survey strategy will produce a full census of the Star Formation Rate (SFR) in the universe, using polycyclic aromatic hydrocarbons (PAH) bands and fine-structure ionic lines, reaching the characteristic knee of the galaxy luminosity function, where the bulk of the population is distributed, at any redshift up to z ∼ 3.5. Deep follow-up pointed spectroscopic observations with grating spectrometers onboard the satellite, across the full IR spectral range (17–210 µm), would simultaneously measure Black Hole Accretion Rate (BHAR), from high-ionisation fine-structure lines, and SFR, from PAH and low- to mid-ionisation lines in thousands of galaxies from solar to low metallicities, down to the knee of their luminosity functions. The analysis of the resulting atlas of IR spectra will reveal the physical processes at play in evolving galaxies across cosmic time, especially its heavily dust-embedded phase during the activity peak at the cosmic noon (z ∼ 1–3), through IR emission lines and features that are insensitive to the dust obscuration., LS and JAFO acknowledge financial support by the Agenzia Spaziale Italiana (ASI) under the research contract 2018-31-HH.0. AAH acknowledges support from grants PGC2018-094671-B-I00 (MCIU/AEI/FEDER,UE) and No. MDM-2017-0737 at Unidad de Excelencia María de Maeztu-Centro de Astrobiología (INTACSIC). FJC acknowledges financial support from the Spanish Ministry MCIU under project RTI2018-096686-B-C21 (MCIU/AEI/FEDER/UE), cofunded by FEDER funds and from the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765. HD acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under the 2014 Ramón y Cajal program RYC-2014-15686 and AYA2017-84061-P, the later one co-financed by FEDER (European Regional Development Funds). AL acknowledges the support from Comunidad de Madrid through the Atracción de Talento grant 2017-T1/TIC-5213. MPS acknowledges support from the Comunidad de Madrid, Spain, through Atracción de Talento Investigador Grant 2018-T1/TIC-11035.

Galaxies with nuclear bars are believed to efficiently drive gas inward, generating a nuclear starburst and possibly an active galactic nucleus. We confirm this scenario for the isolated, double-barred, luminous infrared galaxy ESO 320-G030 based on an analysis of Herschel and ALMA spectroscopic observations. Herschel/PACS and SPIRE observations of ESO 320-G030 show absorption or emission in 18 lines of H2O, which we combine with the ALMA H2O 4(23)-3(30) 448 GHz line (E-upper similar to 400 K) and continuum images to study the physical properties of the nuclear region. Radiative transfer models indicate that three nuclear components are required to account for the multi-transition H2O and continuum data. An envelope, with radius R similar to 130-150 pc, dust temperature T-dust approximate to 50 K, and N-H2 similar to 2x10(23) cm(-2), surrounds a nuclear disk with R similar to 40 pc that is optically thick in the far-infrared (tau (100 mu m)similar to 1.5-3, N-H2 similar to 2x10(24) cm(-2)). In addition, an extremely compact (R similar to 12 pc), warm (approximate to 100 K), and buried (tau (100 mu m)> 5, N-H2 greater than or similar to 5x10(24) cm(-2)) core component is required to account for the very high-lying H2O absorption lines. The three nuclear components account for 70% of the galaxy luminosity (SFR similar to 16-18 M-circle dot yr(-1)). The nucleus is fed by a molecular inflow observed in CO 2-1 with ALMA, which is associated with the nuclear bar. With decreasing radius (r=450-225 pc), the mass inflow rate increases up to M-inf similar to 20 M yr(-1), which is similar to the nuclear star formation rate (SFR), indicating that the starburst is sustained by the inflow. At lower r, similar to 100-150 pc, the inflow is best probed by the far-infrared OH ground-state doublets, with an estimated M-inf similar to 30 M yr(-1). The inferred short timescale of similar to 20 Myr for nuclear gas replenishment indicates quick secular evolution, and indicates that we are witnessing an intermediate stage (< 100 Myr) proto-pseudobulge fed by a massive inflow that is driven by a strong nuclear bar. We also apply the H2O model to the Herschel far-infrared spectroscopic observations of H218O, OH, 18OH, OH+, H2O+, H3O+, NH, NH2, NH3, CH, CH+, 13CH+, HF, SH, and C3, and we estimate their abundances. © ESO 2021., EG-A is grateful for the warm hospitality of the Harvard-Smithsonian Center for Astrophysics, where part of the present study was carried out, and thanks Javier Goicoechea for useful conversations on the far-IR spectrum of Sgr B2, Alex Crespo Gomez for sharing preliminary results on the stellar kinematics in ESO 320-G030, and Juan Rafael Martinez-Galarza for useful conversations on the Bayesian analysis. We thank the anonymous referee for constructive and helpful comments on the manuscript. PACS was developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE was developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ.Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00263.S and ADS/JAO.ALMA#2013.1.00271.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. Based on observations made with ESO Telescopes at the Paranal Observatory under programme ID 086.B-0901(A). EG-A is a Research Associate at the Harvard-Smithsonian Center for Astrophysics. EG-A, JM-P, and FR-V thank the Spanish Ministerio de Economia y Competitividad for support under projects ESP2017-86582-C4-1-R and PID2019-105552RB-C41. EG-A and HAS thank NASA grant ADAP NNX15AE56G. MP-S acknowledges support from the Comunidad de Madrid, Spain, through Atraccion de Talento Investigador Grant 2018-T1/TIC-11035 and PID2019-105423GA-I00 (MCIU/AEI/FEDER,UE). AA-H and SG-B acknowledge support through grant PGC2018-094671-B-I00 (MCIU/AEI/FEDER,UE). LC, AA-H, MP-S, and JM-P acknowledge support under project No. MDM-2017-0737 Unidad de Excelencia "Maria de Maeztu" - Centro de Astrobiologia (INTA-CSIC). SG-B acknowledges support from the Spanish MINECO and FEDER funding grant AYA2016-76682-C3-2-P. C.Y. acknowledges support from an ESO Fellowship. LC acknowledges support from the Spanish Ministerio de Economia y Competitividad for support under project ESP2017-83197. SC acknowledges financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This research has made use of NASA's Astrophysics Data System (ADS) and of GILDAS software.

Population III (Pop. III) stars, as of yet, have not been detected, however as we move into the era of extremely large telescopes this is likely to change. One likely tracer for Pop. III stars is the HeII$\lambda1640$ emission line, which will be detectable by the HARMONI spectrograph on the European Extremely Large Telescope (ELT) over a broad range of redshifts ($2\leq z\leq14$). By post-processing galaxies from the cosmological, AMR-hydrodynamical simulation NewHorizon with theoretical spectral energy distributions (SED) for Pop. III stars and radiative transfer (i.e. the Yggdrasil Models and CLOUDY look-up tables respectively) we are able to compute the flux of HeII$\lambda1640$ for individual galaxies. From mock 10 hour observations of these galaxies we show that HARMONI will be able to detect Pop. III stars in galaxies up to $z\sim10$ provided Pop. III stars have a top heavy Initial Mass Function (IMF). Furthermore, we find that should Pop. III stars instead have an IMF similar to those of the Pop. I stars, the HeII$\lambda1640$ line would only be observable for galaxies with Pop. III stellar masses in excess of $10^{7}{\,M}_\odot\,{\rm yr}^{-1}$, average stellar age $, Comment: 23 Pages, 17 Figures, Accepted for publication in Monthly Notices of the Royal Astronomical Society

arXiv:2106.08345v1, SPICA Collaboration Team., In the black hole (BH)–galaxy co-evolution framework, most of the star formation (SF) and the BH accretion are expected to take place in highly obscured conditions. The large amount of gas and dust absorbs most of the UV-to-soft-X radiation and re-emits it at longer wavelengths, mostly in the IR. Thus, obscured active galactic nuclei (AGN) are very difficult to identify in optical or X-ray bands but shine bright in the IR. Moreover, X-ray background (XRB) synthesis models predict that a large fraction of the yet-unresolved XRB is due to the most obscured (Compton thick, CT: NH ≥ 1024 cm−2) of these AGN. In this work, we investigate the synergies between putative IR missions [using SPace Infrared telescope for Cosmology and Astrophysics (SPICA), proposed for European Space Agency (ESA)/M5 but withdrawn in 2020 October, and Origins Space Telescope, OST, as ‘templates’] and the X-ray mission Athena (Advanced Telescope for High ENergy Astrophysics), which should fly in early 2030s, in detecting and characterising AGN, with a particular focus on the most obscured ones. Using an XRB synthesis model, we estimated the number of AGN and the number of those which will be detected in the X-rays by Athena. For each AGN, we associated an optical-to-Far InfraRed (FIR) spectral energy distribution (SED) from observed AGN with both X-ray data and SED decomposition and used these SEDs to check if the AGN will be detected by SPICA-like or OST at IR wavelengths. We expect that, with the deepest Athena and SPICA-like (or OST) surveys, we will be able to photometrically detect in the IR more than 90% of all the AGN (down to L2−10keV ∼ 1042 erg s−1 and up to z ∼ 10) predicted by XRB synthesis modeling, and we will detect at least half of them in the X-rays. The spectroscopic capabilities of the OST can provide ≈51 000 and ≈3 400 AGN spectra with R = 300 at 25–588µm in the wide and deep surveys, respectively, the last one up to z ≈ 4. Athena will be extremely powerful in detecting and discerning moderate- and high-luminosity AGN, allowing us to properly select AGN even when the mid-IR torus emission is ‘hidden’ by the host galaxy contribution. We will constrain the intrinsic luminosity and the amount of obscuration for ∼20% of all the AGN (and ∼50% of those with L2−10keV > 3.2 × 1043 erg s−1) using the X-ray spectra provided by Athena WFI. We find that the most obscured and elusive CT-AGN will be exquisitely sampled by SPICA-like mission or OST and that Athena will allow a fine characterisation of the most luminous ones. This will provide a significant step forward in the process of placing stronger constraints on the yet-unresolved XRB and investigating the BH accretion rate evolution up to very high redshift (z ≥ 4)., FP, CV, CG, LB, and LS acknowledge financial support by the Agenzia Spaziale Italiana (ASI) under the research contract 2018-31-HH.0. FJC acknowledges financial support from the Spanish Ministry MCIU under project RTI2018-096686-B-C21 (MCIU/AEI/FEDER/UE), cofunded by FEDER funds and from the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765. MPS acknowledges support from the Comunidad de Madrid, Spain, through Atracción de Talento Investigador Grant 2018-T1/TIC-11035 and PID2019-105423GA-I00 (MCIU/AEI/FEDER,UE). AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001.

We present the first results of the Galaxy Activity, Torus and Outflow Survey (GATOS), a project aimed at understanding the properties of the dusty molecular tori and their connection to the host galaxy in nearby Seyfert galaxies. Our project expands the range of AGN luminosities and Eddington ratios covered by previous surveys of Seyferts conducted by ALMA and allows us to study the gas feeding and feedback cycle in a combined sample of 19 Seyferts. We used ALMA to obtain new images of the emission of molecular gas and dust using the CO(3-2) and HCO+(4-3) lines as well as their underlying continuum emission at 870 microns with high spatial resolutions (0.1'' ~ 7 - 13 pc) in the CND of 10 nearby (D < 28 Mpc) Seyfert galaxies. Our new ALMA observations detect 870 micron continuum and CO line emission from spatially resolved disks located around the AGN in all the sources. The bulk of the continuum flux can be accounted for by thermal emission from dust in the majority of the targets. For most of the sources the disks show a preponderant orientation perpendicular to the AGN wind axes, as expected for dusty molecular tori. The median diameters and molecular gas masses of the tori are ~ 42 pc, and ~ 6 x 10**5 Msun, respectively. We find a positive correlation between the line-of-sight gas column densities responsible for the absorption of X-rays and the molecular gas column densities derived from CO towards the AGN in our sources. The radial distributions of molecular gas in the CND of our combined sample show signs of nuclear-scale molecular gas deficits. We also detect molecular outflows in the sources that show the most extreme nuclear-scale gas deficits in our sample. These observations find for the first time supporting evidence that the imprint of AGN feedback is more extreme in higher luminosity and/or higher Eddington ratio Seyfert galaxies., 41 pages, new version revised and accepted by A&A on the 22nd of June 2021

We analyze new high-resolution (400 pc) ∼220 GHz continuum and CO(2–1) Atacama Large Millimeter Array (ALMA) observations of a representative sample of 23 local (z 1 for 70% of the sample. Therefore, this favors the presence of an obscured active galactic nucleus (AGN) in these objects that could dominate the LIR. We also classify the ULIRG nuclei in two groups: (a) compact nuclei (rcont

HARMONI is the adaptive optics assisted, near-infrared and visible light integral field spectrograph for the Extremely Large Telescope (ELT). A first light instrument, it provides the work-horse spectroscopic capability for the ELT. As the project approaches its Final Design Review milestone, the design of the instrument is being finalized, and the plans for assembly, integration and testing are being detailed. We present an overview of the instrument's capabilities from a user perspective, provide a summary of the instrument's design, including plans for operations and calibrations, and provide a brief glimpse of the predicted performance for a specific observing scenario. The paper also provides some details of the consortium composition and its evolution since the project commenced in 2015.

We used high-spatial resolution (70 pc; 0$ {{\overset{\prime\prime}{.}}} $3) CO multi-transition (J = 1-0, 2-1, 4-3, and 6-5) ALMA data to study the physical conditions and kinematics of the cold molecular outflow in the local luminous infrared galaxy (LIRG) ESO 320-G030 (d = 48 Mpc, LIR/L = 1011.3). ESO 320-G030 is a double-barred isolated spiral, but its compact and obscured nuclear starburst (SFR ∼15 M yr-1; AV ∼40 mag) resembles those of ultra-luminous infrared galaxies (LIR/L > 1012). In the outflow, the CO(1-0)/CO(2-1) ratio is enhanced with respect to the rest of the galaxy and the CO(4-3) transition is undetected. This indicates that the outflowing molecular gas is less excited than the molecular gas in the nuclear starburst (i.e., outflow launching site) and in the galaxy disk. Non-local thermodynamic equilibrium radiative transfer modeling reveals that the properties of the molecular clouds in the outflow differ from those of the nuclear and disk clouds: The kinetic temperature is lower (Tkin ∼ 9 K) in the outflow, and the outflowing clouds have lower column densities. Assuming a 10-4 CO abundance, the large internal velocity gradients, 60-45+250 km s-1 pc-1, imply that the outflowing molecular clouds are not bound by self-gravity. All this suggests that the life-cycle (formation, collapse, dissipation) of the galaxy disk molecular clouds might differ from that of the outflowing molecular clouds which might not be able to form stars. The low kinetic temperature of the molecular outflow remains constant at radial distances between 0.3 and 1.7 kpc. This indicates that the heating by the hotter ionized outflow phase is not efficient and may favor the survival of the molecular gas phase in the outflow. The spatially resolved velocity structure of the outflow shows a 0.8 km s-1 pc-1 velocity gradient between 190 pc and 560 pc and then a constant maximum outflow velocity of about 700-800 km s-1 up to 1.7 kpc. This could be compatible with a pure gravitational evolution of the outflow, which would require coupled variations of the mass outflow rate and the outflow launching velocity distribution. Alternatively, a combination of ram pressure acceleration and cloud evaporation could explain the observed kinematics and the total size of the cold molecular phase of the outflow. © ESO 2020., MPS acknowledges support from the Comunidad de Madrid through the Atracción de Talento Investigador Grant 2018-T1/TIC11035, PID2019-105423GA-I00 (MCIU/AEI/FEDER,UE), and STFC through Grants ST/N000919/1 and ST/N002717/1. L. C. acknowledge financial support by the Spanish MICINN under Grant ESP2017-83197. A. A.-H., S. G.-B., and A. U. acknowledge support through Grant PGC2018-094671-B-I00 (MCIU/AEI/FEDER,UE). E. GA is a Research Associate at the HarvardSmithsonian Center for Astrophysics, and thanks the Spanish Ministerio de Economía y Competitividad for support under project ESP2017-86582-C4- 1-R. J. P.-L. acknowledge financial support by the Spanish MICINN under Grant AYA2017-85170-R. M. P. S., A. A.-H., L. C., J. P.-L. and S. A. work was done under project No. MDM-2017-0737 Unidad de Excelencia “María de Maeztu”- Centro de Astrobiología (INTA-CSIC). DR acknowledges support from ST/S000488/1 and the University of Oxford Fell Fund. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00263.S, ADS/JAO.ALMA#2013.1.00271.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc

AGN-driven outflows are believed to play an important role in regulating the growth of galaxies mostly via negative feedback. However, their effects on their hosts are far from clear, especially for low and moderate luminosity Seyferts. To investigate this issue, we have obtained cold molecular gas observations, traced by the CO(2-1) transition, using the NOEMA interferometer of five nearby (distances between 19 and 58 Mpc) Seyfert galaxies. The resolution of approx. 0.3-0.8 arcsec (approx. 30-100 pc) and field of view of NOEMA allowed us to study the CO(2-1) morphology and kinematics in the nuclear regions (approx. 100 pc) and up to radial distances of approx. 900 pc. We have detected CO(2-1) emission in all five galaxies with disky or circumnuclear ring like morphologies. We derived cold molecular gas masses on nuclear (approx. 100 pc) and circumnuclear (approx. 650 pc) scales in the range from $10^6$ to $10^7$M$_{\odot}$ and from $10^7$ to $10^8$ $M_{\odot}$, respectively. In all of our galaxies the bulk of this gas is rotating in the plane of the galaxy. However, non-circular motions are also present. In NGC 4253, NGC 4388 and NGC 7465, we can ascribe the streaming motions to the presence of a large-scale bar. In Mrk 1066 and NGC 4388, the non-circular motions in the nuclear regions are explained as outflowing material due to the interaction of the AGN wind with molecular gas in the galaxy disk. We conclude that for an unambiguous and precise interpretation of the kinematics of the cold molecular gas we need a detailed knowledge of the host galaxy (i.e., presence of bars, interactions, etc) as well as of the ionized gas kinematics and the ionization cone geometry., Accepted for publication in A&A, 23 pages, 17 figures

We present a method for recovering the intrinsic (extinction-corrected) luminosity of the 11.2 micron PAH band in galaxy spectra. Using 105 high S/N Spitzer/IRS spectra of star-forming galaxies, we show that the equivalent width ratio of the 12.7 and 11.2 micron PAH bands is independent on the optical depth, with small dispersion of ~5% indicative of a nearly constant intrinsic flux ratio R_int = (f_12.7/f_11.2)_int = 0.377 +/- 0.020. Conversely, the observed flux ratio, R_obs = (f_12.7/f_11.2)_obs strongly correlates with the silicate strength (S_sil) confirming that differences in R_obs reflect variation in the optical depth. The relation between R_obs and S_sil reproduces predictions for the Galactic Centre extinction law but disagrees with other laws. We calibrate the total extinction affecting the 11.2 micron PAH from R_obs, which we apply to another sample of 215 galaxies with accurate measurements of the total infrared luminosity (L_IR) to investigate the impact of extinction on L_11.2/L_IR. Correlation between L_11.2/L_IR and R_obs independently on L_IR suggests that increased extinction explains the well known decrease in the average L_11.2/L_IR at high L_IR. The extinction-corrected L_11.2 is proportional to L_IR in the range L_IR/L_sun = 10^9--10^13. These results consolidate L_11.2 as a robust tracer of star formation in galaxies., Comment: 14 pages, 9 figures, 2 tables. Accepted for publication in MNRAS

arXiv:2009.12385v1 [astro-ph.GA], We study the multiphase feedback processes in the central ∼3 kpc of the barred Seyfert 2 galaxy NGC 5643. We used observations of the cold molecular gas (ALMA CO(2−1) transition) and ionized gas (MUSE IFU optical emission lines). We studied different regions along the outflow zone, which extends out to ∼2.3 kpc in the same direction (east-west) as the radio jet, as well as nuclear and circumnuclear regions in the host galaxy disk. The CO(2−1) line profiles of regions in the outflow and spiral arms show two or more different velocity components: one associated with the host galaxy rotation, and the others with out- or inflowing material. In the outflow region, the [O III]λ5007 Å emission lines have two or more components: the narrow component traces rotation of the gas in the disk, and the others are related to the ionized outflow. The deprojected outflowing velocities of the cold molecular gas (median Vcentral ∼ 189 km s−1) are generally lower than those of the outflowing ionized gas, which reach deprojected velocities of up to 750 km s−1 close to the active galactic nucleus (AGN), and their spatial profiles follow those of the ionized phase. This suggests that the outflowing molecular gas in the galaxy disk is being entrained by the AGN wind. We derive molecular and ionized outflow masses of ∼5.2 × 107 M⊙ (αCOGalactic) and 8.5 × 104 M⊙ and molecular and ionized outflow mass rates of ∼51 M⊙ yr−1 (αCOGalactic) and 0.14 M⊙ yr−1, respectively. This means that the molecular phase dominates the outflow mass and outflow mass rate, while the kinetic power and momentum of the outflow are similar in both phases. However, the wind momentum loads (Ṗout/ṖAGN) for the molecular and ionized outflow phases are ∼27−5 (αCOGalactic and αCOULIRGs) and < 1, which suggests that the molecular phase is not momentum conserving, but the ionized phase most certainly is. The molecular gas content (Meast ∼ 1.5 × 107 M⊙; αCOGalactic) of the eastern spiral arm is approximately 50−70% of the content of the western one. We interpret this as destruction or clearing of the molecular gas produced by the AGN wind impacting in the eastern side of the host galaxy (negative feedback process). The increase in molecular phase momentum implies that part of the kinetic energy from the AGN wind is transmitted to the molecular outflow. This suggests that in Seyfert-like AGN such as NGC 5643, the radiative or quasar and the kinetic or radio AGN feedback modes coexist and may shape the host galaxies even at kiloparsec scales through both positive and (mild) negative feedback., IGB, AAH and FJC acknowledge financial support through grant PN AYA2015-64346-C2-1-P (MINECO/FEDER), funded by the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu. IGB and DR also acknowledge support from STFC through grant ST/S000488/1. DR acknowledges support from the University of Oxford John Fell Fund. AAH, SGB and MVM also acknowledge support through grant PGC2018-094671-BI00 (MCIU/AEI/FEDER,UE). AAH, MPS, MVM and AL work was done under project No. MDM-2017-0737 Unidad de Excelencia “María de Maeztu” - Centro de Astrobiología (INTA-CSIC). MPS acknowledges support from the Comunidad de Madrid, Spain, through Atracción de Talento Investigador Grant 2018- T1/TIC-11035 and PID2019-105423GA-I00 (MCIU/AEI/FEDER,UE). BG-L acknowledges support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU) and the European Regional Development Fund (FEDER) under grant with reference AYA2015- 68217-P. FJC and SM acknowledge financial support from the Spanish Ministry MCIU under project RTI2018-096686-B-C21 (MCIU/AEI/FEDER/UE), cofunded by FEDER funds and from the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765. CRA acknowledges support from the Spanish Ministry of Science, Innovation and Universities (MCIU), the Agencia Estatal de Investigación (AEI) and the Fondo Europeo de Desarrollo Regional (EU FEDER) under project AYA2016-76682-C3-2-P and PID2019-106027GB-C42. CRA also acknowledges support from the MCIU under grant RYC-2014-15779. AL acknowledges the support from Comunidad de Madrid through the Atracción de Talento grant 2017-T1/TIC-5213. CR acknowledges support from the Fondecyt Iniciacion grant 11190831.

We investigated the 65, 71, 79, 84, 119, and 163 μm OH doublets of 178 local (0 < z < 0.35) galaxies. They were observed using the Herschel/Photoconductor Array Camera and Spectrometer, including Seyfert galaxies, low-ionization nuclear emission-line regions, and star-forming galaxies. We observe these doublets exclusively in absorption (OH71), primarily in absorption (OH65, OH84), mostly in emission (OH79), only in emission (OH163), and an approximately even mix of the both (OH119). In 19 galaxies we find P Cygni or reverse P Cygni line profiles in the OH doublets. We use several galaxy observables to probe spectral classification, brightness of a central active galactic nucleus (AGN)/starburst component, and radiation field strength. We find that OH79, OH119, and OH163 are more likely to display strong emission for bright, unobscured AGNs. For less luminous, obscured AGNs and nonactive galaxies, we find populations of strong absorption (OH119), weaker emission (OH163), and a mix of weak emission and weak absorption (OH79). For OH65, OH71, and OH84, we do not find significant correlations with the observables listed above. For OH79 and OH119, we find relationships with both the 9.7 μm silicate feature and Balmer decrement dust extinction tracers in which more dust leads to weaker emission/stronger absorption. The origin of emission for the observed OH doublets, whether from collisional excitation or from radiative pumping by infrared photons, is discussed., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)

Leishmaniasis, malaria, and neosporosis are parasitic diseases that affect humans and animals, causing public health problems and billions in economic losses. Despite the advances in the development of new drugs, the severe side effects of available leishmaniasis treatments, the Plasmodium spp. resistance to antimalarial drugs, and the lack of a specific treatment against neosporosis lead us to the search for new anti-protozoan molecules from underexplored sources such as the Antarctic marine environment. Herein, we describe for the first time the chemical profile of Desmarestia antarctica crude extract and fractions using GC-MS and LC-MS/MS (molecular networking) approaches, and evaluate their antiparasitic activity against Leishmania amazonensis, Neospora caninum, and multi-drug-resistant Plasmodium falciparum. Furthermore, the cytotoxicity in 3T3 BALB/c fibroblasts and Vero cells was evaluated. D. antarctica fraction E ( IC50 of 53.8±4.4 μg mL− 1 and selectivity index of 3.3) exhibited anti-promastigote activity and was fourfold more selective to L. amazonensis rather than to the host cells. D. antarctica fraction D (IC50 of 1.6±1.3 μg mL− 1 and selectivity index of 27.8), D. antarctica fraction F (IC50 of 3.1±2.1 μg mL− 1 and selectivity index of 23.1), and D. antarctica fraction H (IC50 of 3.1±2.0 μg mL− 1 and selectivity index of 12.9) presented the highest antiparasitic effects against N. caninum with no cytotoxic effects. Also, D. antarctica fraction D presented a significant antiplasmodial inhibitory effect (IC50 of 19.1±3.9 μg mL− 1 and selectivity index of 6.0). GC-MS analysis indicated palmitic acid, myristic acid, fucosterol, phthalic acid, di(2-methylbutyl) ester, loliolide, and neophytadiene as the main components in the active fractions. In addition, this is the first report of a biological screening of macroalgae secondary metabolites against N. caninum parasites.

We investigate the relation between the detection of the 11.3 μm polycyclic aromatic hydrocarbon (PAH) feature in the nuclear (∼24-230 pc) regions of 22 nearby Seyfert galaxies and the properties of the cold molecular gas. For the former we use ground-based (0.3-0.6″ resolution) mid-infrared (mid-IR) spectroscopy. The cold molecular gas is traced by ALMA and NOEMA high (0.2-1.1″) angular resolution observations of the CO(2-1) transition. Galaxies with a nuclear detection of the 11.3 μm PAH feature contain more cold molecular gas (median 1.6 × 107 MO ) and have higher column densities (N(H2) = 2 × 1023 cm-2) over the regions sampled by the mid-IR slits than those without a detection. This suggests that molecular gas plays a role in shielding the PAH molecules in the harsh environments of Seyfert nuclei. Choosing the PAH molecule naphthalene as an illustration, we compute its half-life in the nuclear regions of our sample when exposed to 2.5 keV hard X-ray photons. We estimate shorter half-lives for naphthalene in nuclei without a 11.3 μm PAH detection than in those with a detection. The Spitzer/IRS PAH ratios on circumnuclear scales (∼4″ ∼ 0.25-1.3 kpc) are in between model predictions for neutral and partly ionized PAHs. However, Seyfert galaxies in our sample with the highest nuclear H2 column densities are not generally closer to the neutral PAH tracks. This is because in the majority of our sample galaxies, the CO(2-1) emission in the inner ∼4″ is not centrally peaked and in some galaxies traces circumnuclear sites of strong star formation activity. Spatially resolved observations with the MIRI medium-resolution spectrograph on the James Webb Space Telescope will be able to distinguish the effects of an active galactic nucleus (AGN) and star formation on the PAH emission in nearby AGN., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)

A prominent jet-driven outflow of CO(2-1) molecular gas is found along the kinematic minor axis of the Seyfert 2 galaxy ESO 420-G13, at a distance of $340-600\, \rm{pc}$ from the nucleus. The wind morphology resembles a characteristic funnel shape, formed by a highly collimated filamentary emission at the base, likely tracing the jet propagation through a tenuous medium, until a bifurcation point at $440\, \rm{pc}$ where the jet hits a dense molecular core and shatters, dispersing the molecular gas into several clumps and filaments within the expansion cone. We also trace the jet in ionised gas within the inner $\lesssim 340\, \rm{pc}$ using the [NeII]$_{\rm 12.8 \mu m}$ line emission, where the molecular gas follows a circular rotation pattern. The wind outflow carries a mass of $\sim 8 \times 10^6\, \rm{M_\odot}$ at an average wind projected speed of $\sim 160\, \rm{km\,s^{-1}}$, which implies a mass outflow rate of $\sim 14\, \rm{M_\odot\,yr^{-1}}$. Based on the structure of the outflow and the budget of energy and momentum, we discard radiation pressure from the active nucleus, star formation, and supernovae as possible launching mechanisms. ESO 420-G13 is the second case after NGC 1377 where the presence of a previously unknown jet is revealed due to its interaction with the interstellar medium, suggesting that unknown jets in feeble radio nuclei might be more common than expected. Two possible jet-cloud configurations are discussed to explain the presence of an outflow at such distance from the AGN. The outflowing gas will likely not escape, thus a delay in the star formation rather than quenching is expected from this interaction, while the feedback effect would be confined within the central few hundred parsecs of the galaxy., Comment: 12 pages, 8 figures. Accepted for publication in A&A

Plants are an important source of molecules that can control acute and chronic diseases. Malaria treatment represents a successful strategy in which an infection is controlled with compounds obtained from plants (for instance, artemisinin and quinine). Natural sources are an interesting reservoir of potential molecules that can act against protozoans, especially Trypanosoma cruzi. This parasite is the causative agent of Chagas disease, whose symptomatic chronic phase leads to cardiac and digestive complications. Despite the impacting complications of this disease, only two drugs are commercially available to treat it, nifurtimox and benznidazole. Thus, novel candidates for Trypanosoma cruzi control are desirable. Among the recent advances in this field, the diterpene copalic acid and the sesquiterpene β-caryophyllene oxide purified from copaiba plants have demonstrated antipathogenic properties, including trypanocidal activity. Here, we have studied some biological properties of copalic acid and performed several chemical modifications on β-caryophyllene oxide, which afforded six derivatives. These terpenes exerted different effects on amastigotes, epimastigotes, and trypomastigotes. In addition, they also inhibited the activity of horseradish peroxidase, a heme enzyme.

We present simulated observations of gas kinematics in galaxies formed in 10 pc resolution cosmological simulations with the hydrodynamical + N-body code RAMSES, using the new RAMSES2HSIM pipeline with the simulated observing pipeline (HSIM) for the ELT HARMONI IFU spectrograph. We post-process the galaxy's gas kinematics and H{\alpha} line emission for each simulation cell, and integrate the emission to produce an extinction-corrected input cube. We then simulate observations of the input cube with HARMONI, for a range of exposure times, spatial sampling, and spectral resolution. We analyze the mock observations to recover galaxy properties such as its kinematics and compare with the known simulation values. We investigate the cause of biases between the 'real' and 'observed' kinematic values, demonstrating the sensitivity of the inferred rotation curve to knowledge of the instrument's point spread function., Comment: 29 pages aastex format, 9 figures, 3 tables. Accepted for publication in MNRAS

Cellulose nanofibers (CNFs) are becoming a topic of great interest due to their wide range of potential applications. The huge presence of carboxylic groups in TEMPO-oxidized CNFs indicate that this material could interact with cationic species in aqueous solution, such as metal ions. Nevertheless, the contact between nanofibers and water solutions requires a 3D structure to entrap and retain the nanofibers. In this sense, two different 3D structures were synthetized: CNF-calcium alginate beads and CNF-aerogels. After the synthesis and characterization of 3D structures, batch sorption studies were performed by using these sorbents to study their ability for metal removal. Equilibrium data fitted very well Langmuir and Freundlich isotherm models in the studied concentration range of copper(II) ions and confirmed that the copper sorption is a favorable process. Both new synthetized materials resulted to be effective for Cu(II) removal and maximum sorption capacity was higher for CNF-aerogels than CNF-calcium alginate beads. Finally, in this work it has been demonstrated that the synthetized 3D CNF-aerogel structure is an efficient sorbent for copper ion removal from aqueous solutions and the use of this synthetized structure for environmental decontamination opens a new opportunity to CNF applications.

Delignified fibres from E. benthamii, E. nitens and E. smithii were treated with different NaOH concentrations (up to 30%, w/v) at two different temperatures (25 °C and 80 °C) to investigate the polymorphic and morphological variations in cellulose. The results showed that de-crystallization and the polymorphic transformation of cellulose started at 10% (w/v) NaOH. At 10% (w/v) NaOH, the cellulose II content was similar among the samples from the different species, but changes were observed in the cellulose I content and amorphous fraction. Alkalization at 25 °C had a higher de-crystallization effect than that at 80 °C. E. benthamii showed the highest cristallinity index values and E. nitens the lowest. The crystallite size of cellulose I (L(200)) increased as the NaOH concentration increased, while the temperature seemed to not have a significant influence on the L(200) variation. E. benthamii showed the highest L(200) (3.5–5.0 nm) while E. nitens showed the lowest (3.3–4.5 nm). The crystallite size of cellulose II (L(020)) was higher (4.8–5.2 nm) than that of cellulose I L(200) (3.3–5.0 nm). Alkalization at a higher temperature resulted in a higher cellulose II L(020). Morphologically, at a 0.5% NaOH concentration, the fibres were embedded in a gel-like substance, and, with the NaOH concentration above 10%, the fibres were converted into a swollen and roughened state. Thus, different Eucalyptus species at given NaOH concentrations displayed different structural features, which could lead to procedures and products with different requirements towards the manufacturing of cellulose derivatives.

We present preliminary results on the potential of HARMONI, the first light integral field spectrograph for the ELT, to explore the evolution of central super massive black holes (SMBH)—host galaxy relation in the range from z~0.7 to z~2.5. We simulated HARMONI observations of QSO+host galaxy at different redshifts, assuming different morphologies for the host galaxy. As input, we combined MUSE observations of nearby galaxies and a theoretical QSO spectrum. These were dimmed and redshifted to the desired cosmic epoch. We scaled the total host galaxy luminosity to three different values, sampling three orders of magnitude. Likewise, we assumed two different luminosities for the central QSO. Simulations were performed for the 30×60 mas2 HARMONI spatial scale and LTAO working at 0.67 arcsec seeing. The selected wavelength range (i.e., 4,700–5,300 Å at rest-frame) was sampled at the lowest HARMONI spectral resolving power (i.e., R~3,200). This configuration included all the ingredients to estimate the host galaxy parameters and the SMBH mass, as well as for assessing the morphological type of the host galaxy. BG-L and AM-I acknowledge support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU) and the European Regional Development Fund (FEDER) under grant with reference AYA2105-68217-P. MP-S acknowledges support from the Comunidad de Madrid through Atraccion de Talento Investigador Grant 2018-T1/TIC-11035 and STFC through grant ST/N000919/1. MP-S and NT acknowledge support from STFC through grant ST/N002717/1; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737). Peer review

Neutral sulphite semichemical pulping (NSSC) of Schizolobium amazonicum (Paricá), a fast-growing Amazonian tree, was compared with that of Eucalyptus grandis (eucalypt), one of the most important wood sources for the Brazilian pulp industry, and with mixtures of both woods in different proportions (mix). Wood chips prepared from 7-year old trees were steamed, cooked using the NSSC process and defibered in a 12” disc refiner in three stages. The paricá wood produced pulp of lower yield (75 %) than eucalypt (77 %) at 16 % sulfite/150 min/170 °C. The paricá and eucalypt pulps were bleached to about 68 and 74 % ISO brightness, respectively, by the QPFAS sequence. Paricá consumed more energy for refining in comparison with the eucalypt wood. The wood mix produced lower yield and brightness than the single species processed separately.

The species Eucalyptus globulus and Eucalyptus nitens have become of great importance in Chile and the world, due to their rapid growth and because compounds with greater added-value can be obtained from their waste. This study aimed at obtaining extracts rich in phenolic compounds from the bark of E. globulus and E. nitens and at evaluating the extraction kinetics and the resistance provided by these extracts to the degradation of pine wood attacked by decay fungi. For this purpose, bark samples were taken from E. nitens and E. globulus at a commercial site and then dried and ground. The extraction of the hydrophilic components was optimized by using a Box-Behnken design that considered the influence of temperature, solid/liquid ratio and methanol concentration on the maximization of the following responses: extraction yield, total phenols (Folin-Ciocalteu) and antioxidant capacity (DPPH). Under optimum conditions, the reaction kinetics of phenolic compounds at three temperatures were modeled and determined. Two antifungal assays were performed with the extracts: determination of the minimum inhibitory concentration (MIC) and a mass loss test for three decay fungi. The optimum was obtained at a solid/liquid ratio (1:60) at a 51% concentration of methanol and water for both species and at a temperature of 319 K and 326 K for E. globulus and E. nitens , respectively. The Fick diffusion model of two extractive phases successfully represented the extraction kinetics of the phenolic compounds from the eucalyptus bark at different temperatures. Bark extractions from both species were validated as possible antifungals against the fungal species. In future studies the technical-economic feasibility of replacing commercial antifungals with solutions of the extracts obtained in this study will be analyzed, taking the extraction process to a pilot scale.

We compare mid-IR and ALMA far-IR images of 12 nearby Seyferts selected from GATOS. The mid-IR unresolved emission contributes more than 60% of the nuclear emission in most galaxies. By contrast, the ALMA 870micron continuum emission is mostly resolved and typically along the torus equatorial direction (Paper I, Garcia-Burillo et al. 2021). The Eddington ratios and nuclear hydrogen column densities NH of half the sample are favorable to launching polar and/or equatorial dusty winds, according to simulations. Six show mid-IR extended emission in the polar direction as traced by the NLR and perpendicular to the ALMA emission. In a few, the nuclear NH might be too high to uplift large quantities of dusty material along the polar direction. Five galaxies have low NH and/or Eddington ratios and thus polar dusty winds are not likely. We generate new CAT3D-WIND disk-wind model images. At low wind-to-disk cloud ratios the far-IR model images have disk- and ring-like morphologies. The X-shape associated with dusty winds is seen better in the far-IR at intermediate-high inclinations for the extended-wind configurations. In most models, the mid-IR emission comes from the inner part of the disk/cone. Extended bi-conical and one-sided polar mid-IR emission is seen in extended-wind configurations and high wind-to-disk cloud ratios. When convolved to our resolution, the model images reproduce qualitative aspects of the observed morphologies. Low-intermediate wind-to-disk ratios are required to account for the large fractions of unresolved mid-IR emission. This work and Paper I provide observational support for the torus+wind scenario. The wind component is more relevant at high Eddington ratios and/or AGN luminosities, and polar dust emission is predicted at NH of up to $10^{24}$cm$^{-2}$. The torus/disk component, on the other hand, prevails at low luminosities and/or Eddington ratios. (Abridged), 27 pages, 27 figures. Accepted for publication in A&A

Cancer remains one of the deadliest diseases, and its effective diagnosis and treatment remains challenging; therefore, progress in earlier detection and improved therapeutics are urgently required. Conventional chemotherapy has only limited efficacy, suffers from non-specific toxicity and the induction of chemoresistance. Prospective templates for these are natural materials such as nanosized clay mineral structures of different shapes (platy, tubule, spherical, and fibrous) with tunable physicochemical, morphological, and structural properties. Their submicron size, individual morphology, high specific surface area, enhanced adsorption ability, cation exchange capacity, and multilayered organization of 0.7–1 nm thick single sheets have attracted considerable interest as multifunctional biocompatible nanocarriers with versatile applications in cancer research, diagnosis, and therapy. The most common nanoclay minerals studied for oncology are kaolinite, halloysite, montmorillonite, laponite, bentonite, sepiolite, palygorskite, and allophane. These multilayered minerals can act as nanocarriers (with a typical drug load of 1–10 wt%) for improved dispersibility, stabilization, sustained controlled release, and the efficient transport of a wide range of anticancer drugs to the tumor site. Nanoclays having both positive and negative surfaces possess the potential to transport proteins and DNA/RNA. Nanoclays can serve as a platform for phototherapeutic agents. Several surface engineering strategies have been devised to develop clays with biofunctionality that could benefit cancer clinical practice. This review explores the potential of nanoclays as unique crystalline materials with applications in cancer research, diagnosis, and therapy.

In this work we use seeing-limited SINFONI H- and K-band spectroscopy to analyse the spatially resolved kinematics of the stellar component in the inner r, Comment: 36 pages, 35, accepted for publication in A&A. Abstract abridged due to arXiv requirements

Brachystegia spiciformis and Pericopsis angolensis are two hardwood species found in the Miombo woodlands. The wood features, kraft pulping and strength pulp properties of both species were evaluated in order to determine their potential as raw material for papermaking. Brachystegia spiciformis wood density was 640 kg m-3 and Pericopsis angolensis was 795 kg m-3. Pericopsis angolensis wood has higher cell wall thickness and occluded fibre lumen as remarkable anatomical properties. Runkel ratio, slenderness ratio, and the coefficients of flexibility and rigidity in Brachystegia spiciformis were 1,5; 65,7; 41,2% and 29,4% while in Pericopsis angolensis these values were 17,6; 59,9; 5,4% and 47,3%, respectively. Brachystegia spiciformis has a higher cellulose content, lower hemicellulose and lignin content, and higher S/G ratio than Pericopsis angolensis. In kraft pulping, a higher demand of active alkali was needed for both species, and pulps with high kappa number (24-27) and low pulp yield (40%) were obtained. Pericopsis angolensis pulps reached tensile, tear and burst indexes of 99,6 Nm g-1; 5,9 mN.m2 g-1 and 4,9 kPa.m2 g-1, respectively. Brachystegia spiciformis pulps reached tensile, tear and burst indexes of 100,3 Nm g-1; 10,7 mN.m2 g-1 and 6,1 kPa.m2 g-1, respectively. As a conclusion, Brachystegia spiciformis wood has better pulpability than Pericopsis angolensis wood, according to its pulps properties, despite of the similar pulp yield between both species. Both species may be suitable for unbleached wrapping papers and rigid cardboards manufacturing.

The abundance of metals in galaxies is a key parameter which permits to distinguish between different galaxy formation and evolution models. Most of the metallicity determinations are based on optical line ratios. However, the optical spectral range is subject to dust extinction and, for high-z objects (z > 3), some of the lines used in optical metallicity diagnostics are shifted to wavelengths not accessible to ground based observatories. For this reason, we explore metallicity diagnostics using far-infrared (IR) line ratios which can provide a suitable alternative in such situations. To investigate these far-IR line ratios, we modeled the emission of a starburst with the photoionization code CLOUDY. The most sensitive far-IR ratios to measure metallicities are the [OIII]52$��$m and 88$��$m to [NIII]57$��$m ratios. We show that this ratio produces robust metallicities in the presence of an AGN and is insensitive to changes in the age of the ionizing stellar. Another metallicity sensitive ratio is the [OIII]88$��$m/[NII]122$��$m ratio, although it depends on the ionization parameter. We propose various mid- and far-IR line ratios to break this dependency. Finally, we apply these far-IR diagnostics to a sample of 19 local ultraluminous IR galaxies (ULIRGs) observed with Herschel and Spitzer. We find that the gas-phase metallicity in these local ULIRGs is in the range 0.7 < Z_gas/Z_sun < 1.5, which corresponds to 8.5 < 12 + log (O/H) < 8.9. The inferred metallicities agree well with previous estimates for local ULIRGs and this confirms that they lie below the local mass-metallicity relation., Accepted for publication in MNRAS; 25 pages, 19 figures

Cellulose nanofibrils (CNF) were isolated from agro-industrial waste (corn husks and oat hulls) and market kraft pulp fibres, and a detailed comparative study was performed. Initially, the raw materials were subjected to a conventional pulping process to remove lignin and hemicelluloses. The chemical pre-treatment was based on 2,2,6,6-tetramethylpiperidinyl-1-oxyl (TEMPO)-mediated oxidation and the mechanical treatment was carried out with a high-pressure homogenizer. An extensive characterization of the raw material and of the nanofibrillated celluloses was performed, considering structural and chemical aspects. CNF films were produced for their characterization by optical methods, laser profilometry (LP), scanning electron microscopy (SEM), and atomic force microscopy (AFM). Considering the same pulping and chemical pre-treatment, the analyses indicated that the oxidized corn husks fibres had higher carboxylate content and thus a larger tendency to nanofibrillate compared to the oat hulls fibres. The obtained content of carboxylic acids was directly proportional to the content of cellulose in the assessed samples, confirming the selectivity of the TEMPO-mediated oxidation. The fibrillated corn husks material had a minor fraction of residual fibres (

The morphology of cellulose nanofibrils (CNFs), the rheological characteristics of their dispersions, and the corresponding relationships, are fundamental for understanding the properties of the material. This work aims at understanding how the morphological characteristics of the CNFs affect the rheology of the dispersions in the dilute region and to establish a relationship between both properties. A strong relationship was observed between the intrinsic viscosity of the CNF dispersions and their aspect ratio, which can be correlated through the expression ρ[η]=0.051p1.85. When comparing the model obtained in this work to the wormlike chain model, it was possible to verify that these models are independent of the flexibility of the CNFs. Regarding the fibrillation process, the dynamic viscosity only reflects part of the behavior of the morphological properties of the CNFs and does not provide reliable data that would allow these characteristics to be inferred, while the intrinsic viscosity does allow this relationship.

The extreme infrared (IR) luminosity of local luminous and ultra-luminous IR galaxies (U/LIRGs; 11 < log LIR /Lsun < 12 and log LIR /Lsun > 12, respectively) is mainly powered by star-formation processes triggered by mergers or interactions. While U/LIRGs are rare locally, at z > 1, they become more common, they dominate the star-formation rate (SFR) density, and a fraction of them are found to be normal disk galaxies. Therefore, there must be an evolution of the mechanism triggering these intense starbursts with redshift. To investigate this evolution, we present new optical SWIFT integral field spectroscopic H{\alpha}+[NII] observations of a sample of 9 intermediate-z (0.2 < z < 0.4) U/LIRG systems selected from Herschel 250{\mu}m observations. The main results are the following: (a) the ratios between the velocity dispersion and the rotation curve amplitude indicate that 10-25% (1-2 out of 8) might be compatible with being isolated disks while the remaining objects are interacting/merging systems; (b) the ratio between un-obscured and obscured SFR traced by H{\alpha} and LIR, respectively, is similar in both local and these intermediate-z U/LIRGs; and (c) the ratio between 250{\mu}m and the total IR luminosities of these intermediate-z U/LIRGs is higher than that of local U/LIRGs with the same LIR . This indicates a reduced dust temperature in these intermediate-z U/LIRGs. This, together with their already measured enhanced molecular gas content, suggests that the interstellar medium conditions are different in our sample of intermediate-z galaxies when compared to local U/LIRGs., Comment: Accepted for publication in MNRAS

We characterize for the first time the torus properties of an ultra-hard X-ray (14-195 keV) volume-limited (DL < 40 Mpc) sample of 24 Seyfert (Sy) galaxies (BCS sample). The sample was selected from the Swift/BAT nine-month catalogue.We use high angular resolution nuclear infrared (IR) photometry and N-band spectroscopy, the CLUMPY torus models and a Bayesian tool to characterize the properties of the nuclear dust. In the case of the Sy1s, we estimate the accretion disc contribution to the subarcsecond resolution nuclear IR SEDs (~0.4 arcsec) which is, on average, 46 ± 28, 23 ± 13, and 11 ± 5 per cent in the J, H, and K bands, respectively. This indicates that the accretion disc templates that assume a steep fall for longer wavelengths than 1 μm might underestimate its contribution to the near-IR emission. Using both optical (broad versus narrow lines) and X-ray (unabsorbed versus absorbed) classifications, we compare the global posterior distribution of the torus model parameters. We confirm that Sy2s have larger values of the torus covering factor (CT ~ 0.95) than Sy1s (CT ~ 0.65) in our volume-limited Seyfert sample. These findings are independent of whether we use an optical or X-ray classification.We find that the torus covering factor remains essentially constant within the errors in our luminosity range and there is no clear dependence with the Eddington ratio. Finally, we find tentative evidence that even an ultra-hard X-ray selection is missing a significant fraction of highly absorbed type 2 sources with very high covering factor tori.© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society., IGB acknowledges financial support from the Instituto de Astrofisica de Canarias through Fundacion La Caixa. IGB also acknowledges Oxford University and Durham University for their hospitality during his stays in 2017 August when this project was started and 2018 May, respectively. IGB also acknowledges Cardiff University for their hospitality from 2018 May to August. CRA and IGB acknowledge financial support from the Spanish Ministry of Science and Innovation (MICINN) through project AYA2016-76682-C3-2-P. IGB, AAH, and FJC also acknowledge financial support through grant PN AYA2015-64346-C2-1-P (MINECO/FEDER). Funded by the Agencia Estatal de Investigacion, Unidad de Excelencia Maria de Maeztu. CRA also acknowledges the Ramon y Cajal Program of the Spanish Ministry of Economy and Competitiveness. MPS acknowledges support from STFC through grant ST/N000919/1. OGM thanks to the PAPIIT UNAM project IA103118. SM acknowledges financial support through grant AYA2016-76730-P (MINECO/FEDER). IM and JM acknowledge financial support from the research project AYA2016-76682-C3-1-P (AEI/FEDER, UE). LF and CP acknowledge support from the NSF- grant number 1616828.

DBS surgery is considered for Parkinson’s Disease patients when motor complications and consequent quality of life is no longer acceptable on optimal medical therapy prescribed by neurologists. Within the operating room, the electrode placement with the best clinical outcome for the patient is quantitatively assessed via the wrist rigidity assessment. A subjective scale is used, influenced by the neurologists’ perception and experience. Our research group has previously designed a novel, comfortable and wireless system aiming to tackle this subjectivity. This system comprised a gyroscope sensor in a textile band, placed in the patients’ hand, which communicated its measurement to a Smartphone via Bluetooth. During the wrist rigidity evaluation exam, a signal descriptor was computed from angular velocity (ω) and a polynomial mathematical model was used to classify the signals using a quantitative scale of rigidity improvement. In this present work, we aim to develop models that consider the 3-gyroscope-axes to acquire the ω and the cogwheel rigidity. Our results showed that y-gyroscope-axis remains the best way to classify the rigidity reduction, showing an accuracy of 78% and a mean error of 3.5%. According to previous results, the performance was similar and the decrease of samples to extract the ω features did not compromise system performance. The cogwheel rigidity did not improve the previous model and other gyroscope-axis beyond the y-axis decreased system performance.

The tuning of DPPC coarse grained models was successfully investigated using coarse grained molecular dynamics simulation and umbrella sampling. The octanol-water partition coefficient was measured with the slow stirring method in order to use it as reference for tuning the DPPC models in terms of their hydrophobicity. The Gibbs free energies of transferring the best fit DPPC model (C4 model) from the octanol to water phase gave −14.51 ± 0.30 kcal mol−1. The octanol/water partitioning coefficient of this DPPC model was calculated to be 10.6 ± 0.2, which is in excellent agreement with the experimental octanol/water partition coefficient, 11.50 ± 1.43. The DPPC monolayer model was validated with molecular dynamics simulations and against experiments performed in a Langmuir trough coupled with a grazing incidence X-ray off-specular scattering apparatus. The area per lipid and thickness of the DPPC bilayer model were also validated against experimental and simulated data from literature. Consequently, the tuned DPPC model is expected to have a realistic behavior in terms of its hydrophobicity and structural characteristics.

The interaction of naringin and naringenin with DPPC monolayer at the air-water interface was investigated by coarse grained molecular dynamics and grazing incidence X-ray off-specular scattering (GIXOS). By molecular dynamics, we found that the DPPC monolayer is not disturbed by the addition of flavonoids at the surface tension of 28 mN m−1. The flavonoids are located in the region of phospholipid polar heads. The GIXOS experiments show that the addition of flavonoids does not change the film thickness at the surface tension of 28 mN m-1, which is in excellent agreement with molecular dynamics simulation. Our very preliminary study indicates that DPPC may be used as a delivery system for the administration of naringenin and naringin to the lung.

We present new estimates of AGN accretion and star-formation luminosity in galaxies obtained for the local 12-$\mu$m sample of Seyfert galaxies (12MGS), by performing a detailed broad-band spectral energy distribution (SED) decomposition including the emission of stars, dust heated by star formation and a possible AGN dusty torus. Thanks to the availability of data from the X-rays to the sub-millimetre, we constrain and test the contribution of the stellar, AGN and star-formation components to the SEDs. The availability of Spitzer-IRS low resolution mid-infrared (mid-IR) spectra is crucial to constrain the dusty torus component at its peak wavelengths. The results of SED-fitting are also tested against the available information in other bands: the reconstructed AGN bolometric luminosity is compared to those derived from X-rays and from the high excitation IR lines tracing AGN activity like [Ne V] and [O IV]. The IR luminosity due to star-formation (SF) and the intrinsic AGN bolometric luminosity are shown to be strongly related to the IR line luminosity. Variations of these relations with different AGN fractions are investigated, showing that the relation dispersions are mainly due to different AGN relative contribution within the galaxy. Extrapolating these local relations between line and SF or AGN luminosities to higher redshifts, by means of recent Herschel galaxy evolution results, we then obtain mid- and far-IR line luminosity functions useful to estimate how many star-forming galaxies and AGN we expect to detect in the different lines at different redshifts and luminosities with future IR facilities (e.g., JWST, SPICA)., Comment: 27 pages, 13 figures, 7 tables. MNRAS in press

The detection of several radio-loud narrow-line Seyfert 1 (NLS1) galaxies by the Fermi Gamma-Ray Space Telescope hints at the existence of a rare, new class of gamma-ray emitting active galactic nuclei with low black hole masses. Like flat spectrum radio quasars (FSRQs), their gamma-ray emission is thought to be produced via the external Compton mechanism whereby relativistic jet electrons upscatter a photon field external to the jet, e.g. from the accretion disc, broad line region (BLR) and dusty torus, to higher energies. Here we study the origin of the gamma-ray emission in the lowest-redshift candidate among the currently-known gamma-ray emitting NLS1s, 1H 0323+342, and take a new approach. We observationally constrain the external photon field using quasi-simultaneous near-IR, optical and X-ray spectroscopy. Applying a one-zone leptonic jet model, we simulate the range of jet parameters for which this photon field, when Compton scattered to higher energies, can explain the gamma-ray emission. We find that the site of the gamma-ray emission lies well within the BLR and that the seed photons mainly originate from the accretion disc. The jet power that we determine, $1.0 \times 10^{45}$ erg s$^{-1}$, is approximately half the accretion disc luminosity. We show that this object is not simply a low-mass FSRQ, its jet is intrinsically less powerful than predicted by scaling a typical FSRQ jet by black hole mass and accretion rate. That gamma-ray emitting NLS1s appear to host underpowered jets may go some way to explaining why so few have been detected to date., Comment: 22 pages, 8 figures and 8 tables. Accepted for publication in MNRAS

In an earlier paper we modeled the far-infrared emission from a star-forming galaxy using the photoionisation code CLOUDY and presented metallicity sensitive diagnostics based on far-infrared fine structure line ratios. Here, we focus on the applicability of the [OIII]88/[NII]122 microns line ratio as a gas phase metallicity indicator in high redshift submillimetre luminous galaxies. The [OIII]88/[NII]122 microns ratio is strongly dependent on the ionization parameter (which is related to the total number of ionizing photons) as well as the gas electron density. We demonstrate how the ratio of 88/$122 continuum flux measurements can provide a reasonable estimate of the ionization parameter while the availability of the [NII]205 microns line can constrain the electron density. Using the [OIII]88/[NII]122 microns line ratios from a sample of nearby normal and star-forming galaxies we measure their gas phase metallicities and find that their mass metallicity relation is consistent with the one derived using optical emission lines. Using new, previously unpublished, Herschel spectroscopic observations of key far-infrared fine structure lines of the z~3 galaxy HLSW-01 and additional published measurements of far-infrared fine structure lines of high-z submillimetre luminous galaxies we derive gas phase metallicities using their [OIII]88/[NII]122 microns line ratio. We find that the metallicities of these z~3 submm luminous galaxies are consistent with solar metallicities and that they appear to follow the mass-metallicity relation expected for z~3 systems., Comment: 10 pages, 7 figures, MNRAS in press

We present new CO(2–1) observations of three low-z (d ∼ 350 Mpc) ultra-luminous infrared galaxy (ULIRG) systems (six nuclei) observed with the Atacama large millimeter/submillimeter array (ALMA) at high spatial resolution (∼500 pc). We detect massive cold molecular gas outflows in five out of six nuclei (Mout ∼ (0.3−5) ×108 M). These outflows are spatially resolved with deprojected effective radii between 250 pc and 1 kpc although high-velocity molecular gas is detected up to Rmax ∼ 0.5−1.8 kpc (1−6 kpc deprojected). The mass outflow rates are 12−400 M yr−1 and the inclination corrected average velocity of the outflowing gas is 350−550 km s−1 (vmax = 500−900 km s−1). The origin of these outflows can be explained by the strong nuclear starbursts although the contribution of an obscured active galactic nucleus cannot be completely ruled out. The position angle (PA) of the outflowing gas along the kinematic minor axis of the nuclear molecular disk suggests that the outflow axis is perpendicular to the disk for three of these outflows. Only in one case is the outflow PA clearly not along the kinematic minor axis, which might indicate a different outflow geometry. The outflow depletion times are 15−80 Myr. These are comparable to, although slightly shorter than, the star-formation (SF) depletion times (30−80 Myr). However, we estimate that only 15−30% of the outflowing molecular gas will escape the gravitational potential of the nucleus. The majority of the outflowing gas will return to the disk after 5−10 Myr and become available to form new stars. Therefore, these outflows will not likely completely quench the nuclear starbursts. These star-forming powered molecular outflows would be consistent with being driven by radiation pressure from young stars (i.e., momentum-driven) only if the coupling between radiation and dust increases with increasing SF rates. This can be achieved if the dust optical depth is higher in objects with higher SF. This is the case in at least one of the studied objects. Alternatively, if the outflows are mainly driven by supernovae (SNe), the coupling efficiency between the interstellar medium and SNe must increase with increasing SF levels. The relatively small sizes (, L.C., S.G.B., and A.L. acknowledge financial support by the Spanish MEC under grants ESP2015-68964 and AYA2016-76682-C3-2-P.