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Are CMB derived cosmological parameters affected by foregrounds associated to nearby galaxies
No full textWe perform cosmological parameters estimation on Planck cosmic microwave background (CMB) maps masking the recently discovered foreground related to nearby spiral galaxies. In addition, we also analyze the association between these foreground regions and recent claims of cosmological causal horizons in localized CMB parameter estimates. Our analysis shows consistent cosmological parameter values regardless of the masking approach, though reduced sky areas introduce larger uncertainties. By modeling the new extragalactic foreground, we identify a resemblance with local parameter variation maps with a statistical significance at the 3σ level, suggesting that a simplified foreground model partially accounts, (40-50)% correlation with 15% uncertainty, for the observed causal horizons. These findings add new evidence to the existence of the new foreground associated with large spiral galaxies and show that estimates of cosmological parameters on smaller patches on the sky can be largely affected by these foregrounds, but that the parameters taken over the full sky are unaltered.This work was partially supported by Agencia Nacional de Promoción Científica y Tecnológica (No. PICT 2015-3098, No. PICT 2016-1975), the Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET, Argentina) and the Secretaría de Ciencia y Tecnología de la Universidad Nacional de Córdoba (SeCyT-UNC, Argentina). Results in this paper are based on observations obtained with Planck [34], an European Space Agency (ESA) science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. The simulations were performed on resources provided by UNINETT Sigma2—the National Infrastructure for High Performance Computing and Data Storage in Norway.” Some of the results in this paper have been derived using the healpix package [35]. This work used computational resources from CCAD—Universidad Nacional de Córdoba [36], which are part of SNCAD—MinCyT, República ArgentinaPeer reviewe
Identification, occurrence, and mechanism of formation of 1-acetyl-β-carbolines derived from l-tryptophan and methylglyoxal
No full textβ-Carbolines (βCs) are bioactive compounds present in foods and biological systems. This work describes the identification, occurrence, and mechanism of formation of 1-acetyl-β-carbolines (1-acetyl-βCs) that result from the reaction of l-tryptophan with the α-dicarbonyl compound methylglyoxal. Two β-carbolines are characterized as 1-acetyl-β-carboline (AβC) and 1-acetyl-β-carboline-3-carboxylic acid (AβC-COOH). Their formation was favored in acidic conditions and with increasing temperature, but 1-acetyl-βCs also formed in moderate temperatures and in a wide range of pH, including physiological conditions, and in human serum. The formation mechanism relies on tautomerism and cyclization to give 1-(1-hydroxyethyl)-3,4-dihydro-β-carboline-3-carboxylic acid intermediates followed by the oxidation of C1'-OH and aromatization to 1-acetyl-βCs. The formation of 1-acetyl-βCs took place in the reactions of fructose or glucose with tryptophan under heating and depended on the methylglyoxal released during carbohydrate degradation. Formation from carbohydrates increased at neutral or basic pH values as more methylglyoxal was released under those conditions. Thus, 1-acetyl-βCs could be advanced glycation end-products (AGEs). 1-Acetyl-βCs were identified and quantified for the first time in many foods. AβC ranged from undetectable to 250 ng/g with the highest amount detected in honey, bread, cookies, soy sauce, and coffee. On average, AβC-COOH generally appeared in lower concentrations than AβC but it ranged from undetectable to 323 ng/g with the highest levels found in soy sauce, honey, cookies, and fried bread. These results indicate that 1-acetyl-βCs could be relevant βCs in foods and in vivo.The authors thank the Agencia Estatal de Investigación (MCIN/AEI/10.13039/501100011033) for funding through the projects PID2021-127833OB-I00 (cofunded by the European Regional Development Fund (ERDF), “A way to build Europe”), and PDC2022-133269-I00 and PID2022-136438OB-I00 (funded by Recovery and Resilience Facility, RRF, NextGenerationEU). The authors thank Laura Peláez (IQM-CSIC) for HPLC–MS analyses. AP was a recipient of a Garantía Juvenil contract (Comunidad de Madrid and Fondo Social Europeo-YEI).Peer reviewe
Computational flow cytometry immunophenotyping at diagnosis is unable to predict relapse in childhood B-cell Acute Lymphoblastic Leukemia
No full textB-cell Acute Lymphoblastic Leukemia is the most prevalent form of childhood cancer, with approximately 15% of patients undergoing relapse after initial treatment. Further advancements depend on novel therapies and more precise risk stratification criteria. In the context of computational flow cytometry and machine learning, this paper aims to explore the potential prognostic value of flow cytometry data at diagnosis, a relatively unexplored direction for relapse prediction in this disease. To this end, we collected a dataset of 252 patients from three hospitals and implemented a comprehensive pipeline for multicenter data integration, feature extraction, and patient classification, comparing the results with existing algorithms from the literature. The analysis revealed no significant differences in immunophenotypic patterns between relapse and non-relapse patients and suggests the need for alternative approaches to handle flow cytometry data in relapse prediction.This work was partially supported by project PDC2022-133520-I00 funded by Ministerio de Ciencia e Innovación/ Agencia Estatal de investigación (doi:10.13039/501100011033) and European Union NextGenerationEU/PRTR; by project PID2022-140451OA-I00 funded by Ministerio de Ciencia e Innovación/Agencia Estatal de investigación (doi:10.13039/501100011033) and ERDF A way of making Europe; and by University of Castilla-La Mancha/ERDF, A way of making Europe (Applied Research Projects) under grant 2022-GRIN-34405. The support of Fundación Española para la Ciencia y la Tecnología (FECYT project PR214), Asociación Pablo Ugarte (APU, Spain) and Junta de Andalucía (Spain) group FQM-201 is also acknowledged. This work was also subsidized in its early stages by a grant for the research and biomedical innovation in the health sciences within the framework of the Integrated Territorial Initiative (ITI) for the province of Cádiz (grant number ITI-0038-2019).Peer reviewe
The Sunrise Ultraviolet Spectropolarimeter and Imager: Instrument Description
No full textFeller, A. et al.-- Full list of authors: Feller, Alex; Gandorfer, Achim; Grauf, Bianca; Hölken, Johannes; Iglesias, Francisco A.; Korpi-Lagg, Andreas; Riethmüller, Tino L.; Staub, Jan; Fernandez-Rico, German; Castellanos Durán, Juan Sebastián; Solanki, Sami K.; Smitha, H. N.; Sant, Kamal; Barthol, Peter; Bayon Laguna, Montserrat; Bergmann, Melani; Bischoff, Jörg; Bochmann, Jan; Bruns, Stefan; Deutsch, Werner; Eberhardt, Michel; Enge, Rainer; Goodyear, Sam; Heerlein, Klaus; Heinrichs, Jan; Hirche, Dennis; Meining, Stefan; Mende, Roland; Meyer, Sabrina; Mühlhaus, Maria; Müller, Marc Ferenc; Monecke, Markus; Oberdorfer, Dietmar; Papagiannaki, Ioanna; Ramanath, Sandeep; Vergöhl, Michael; Vukadinović, Dušan; Werner, Stephan; Zerr, Andreas; Berkefeld, Thomas; Bernasconi, Pietro; Katsukawa, Yukio; del Toro Iniesta, Jose Carlos; Bell, Alexander; Carpenter, Michael; Álvarez Herrero, Alberto; Kubo, Masahito; Martínez Pillet, Valentín; Orozco Suárez, DavidThe third science flight of the balloon-borne solar observatory Sunrise carries three entirely new post-focus science instruments with spectropolarimetric capabilities, concurrently covering an extended spectral range from the near ultraviolet to the near infrared. Sampling a larger height range, from the low photosphere to the chromosphere, with the sub-arcsecond resolution provided by the 1-m Sunrise telescope, is key in understanding critical small-scale phenomena which energetically couple different layers of the solar atmosphere. The Sunrise UV Spectropolarimeter and Imager (SUSI) operates between 309 nm and 417 nm. A key feature of SUSI is its capability to record up to several hundred spectral lines simultaneously without the harmful effects of the Earth’s atmosphere. The rich SUSI spectra can be exploited in terms of many-line inversions. Another important innovation of the instrument is the synchronized 2D context imaging which allows to numerically correct the spectrograph scans for residual optical aberrations. In this work we describe the main design aspects of SUSI, the instrument characterization and testing, and finally its operation, expected performance and data products. © The Author(s) 2025Open Access funding enabled and organized by Projekt DEAL. The German contribution to Sunrise iii and SUSI is funded by the Strategic Innovations Fund of the President of the Max Planck Society (MPG), and by the Max-Planck-Förderstiftung with private donations by supporting members of the MPG. SUSI has also received funding from the Bundesministerium für Wirtschaft und Klimaschutz through Deutsches Zentrum für Luft- und Raumfahrt e.V. (DLR), grant. no. 50 OO 1608, and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 101097844, project WINSUN). The contributions of J. Hölken, D. Vukadinović and K. Sant are supported by the International Max Planck Research School (IMPRS) for solar system science. F. Iglesias is a member of the “Carrera del Investigador Científico” of CONICET and supported by the MPG through the Max Planck Partner Group between MPS and the University of Mendoza, Argentina. The Japanese contribution has been funded by the ISAS/JAXA Small Mission-of-Opportunity program and JSPS KAKENHI JP18H05234/JP23H01220. The Spanish contribution has been funded by the Spanish MCIN/AEI under projects RTI2018-096886-B-C5, and PID2021-125325OB-C5; and from the “Center of Excellence Severo Ochoa” awards to IAA-CSIC (SEV-2017-0709, CEX2021-001131-S), all co-funded by European ERDF funds, “A way of making Europe”.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (SEV-2017-0709).With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).Peer reviewe
Translational activity of 80S monosomes varies dramatically across different tissues
No full textTranslational regulation at the stage of initiation can impact the number of ribosomes translating each mRNA molecule. However, the translational activity of single 80S ribosomes (monosomes) on mRNA is less well understood, even though these 80S monosomes represent the dominant ribosomal complexes in vivo. Here, we used cryo-EM to determine the translational activity of 80S monosomes across different tissues in Drosophila melanogaster. We discovered that while head and embryo 80S monosomes are highly translationally active, testis and ovary 80S monosomes are translationally inactive. RNA-Seq analysis of head monosome- and polysome-translated mRNAs, revealed that head 80S monosomes preferentially translate mRNAs with TOP motifs, short 5'-UTRs, short ORFs and are enriched for the presence of uORFs. Overall, these findings highlight that regulation of translation initiation and protein synthesis is mostly performed by monosomes in head and embryo, while polysomes are the main source of protein production in testis and ovary.A.B. and M.A. were funded from BBSRC DTP, BB/M011151/1. AT was funded by Wellcome Trust 102174/B/13/Z. T.H., J.F., and J.A. were funded by BBSRC grant BB/S007407/1 and BBSRC BB/X003086/1. BF was funded by BB/X003086/1. Funding to pay the Open Access publication charges for this article was provided by Leeds University.Peer reviewe
TOI-6508 b: A massive transiting brown dwarf orbiting a low-mass star
No full textBarkaoui, Khalid et al.-- Full list of authors: Barkaoui, K.; Sebastian, D.; Zúñiga-Fernández, S.; Triaud, A. H. M. J.; Rackham, B. V.; Burgasser, A. J.; Carmichael, T. W.; Gillon, M.; Theissen, C.; Softich, E.; Rojas-Ayala, B.; Srdoc, G.; Soubkiou, A.; Fukui, A.; Timmermans, M.; Stalport, M.; Burdanov, A.; Ciardi, D. R.; Collins, K. A.; Davis, Y. T.; Davoudi, F.; de Wit, J.; Demory, B. O.; Deveny, S.; Dransfield, G.; Ducrot, E.; Florian, L.; Gan, T.; Gómez Maqueo Chew, Y.; Hooton, M. J.; Howell, S. B.; Jenkins, J. M.; Littlefield, C.; Martín, E. L.; Murgas, F.; Niraula, P.; Palle, E.; Pedersen, P. P.; Pozuelos, F. J.; Queloz, D.; Ricker, G.; Schwarz, R. P.; Seager, S.; Shporer, A.; Scott, M. G.; Stockdale, C.; Winn, J.We report the discovery of a transiting brown dwarf orbiting a low-mass star, TOI-6508 b. Today, only ∼50 transiting brown dwarfs have been discovered. TOI-6508 b was first detected with data from the Transiting Exoplanet Survey Satellite (TESS) in Sectors 10, 37 and 63. Ground-based follow-up photometric data were collected with the SPECULOOS-South (Search for habitable Planets EClipsing ULtra-cOOl Stars) and LCOGT-1m telescopes, and RV measurements were obtained with the Near InfraRed Planet Searcher (NIRPS) spectrograph. We find that TOI-6508 b has a mass of Mp = 72.5−5.1+7.6 MJup and a radius of Rp = 1.03 ± 0.03 RJup. Our modeling shows that the data are consistent with an eccentric orbit of 19 day and an eccentricity of e = 0.28−0.08+0.09. TOI-6508 b has a mass ratio of MBD/M★ = 0.40, makes it the second highest mass ratio brown dwarf that transits a low-mass star. The host has a mass of M★ = 0.174 ± 0.004 M⊙, a radius of R★ = 0.205 ± 0.006 R⊙, an effective temperature of Teff = 2930 ± 70 K, and a metallicity of [Fe/H] = −0.22 ± 0.08. This makes TOI-6508 b an interesting discovery that has come to light in a region still sparsely populated. © The Authors 2025The postdoctoral fellowship of KB is funded by F.R.S.- FNRS grant T.0109.20 and by the Francqui Foundation. This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral Grant awarded to MT. MG is F.R.S.-FNRS Research Director. Author F.J.P acknowledges financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033 and Ministe- rio de Ciencia e Innovación through the project PID2022-137241NB-C43. This material is based upon work supported by the National Aeronautics and Space Administration under Agreement No. 80NSSC21K0593 for the program “Alien Earths”. The results reported herein benefited from collaborations and/or information exchange within NASA’s Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA’s Science Mission Directorate. Based on observations collected at the European Southern Observatory under ESO programme 113.27QV.001. Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under contract 80HQTR24DA010 with the National Aeronautics and Space Administration. Funding for the TESS mission is provided by NASA’s Science Mission Directorate. KAC acknowledges support from the TESS mission via subaward s3449 from MIT. This paper made use of data collected by the TESS mission, obtained from the Mikulski Archive for Space Telescopes MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Based on data collected by the SPECULOOS-South Observatory at the ESO Paranal Observatory in Chile. The ULiege’s contribution to SPECULOOS has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013) (grant Agreement n° 336480/SPECULOOS), from the Balzan Prize and Francqui Foundations, from the Belgian Scientific Research Foundation (F.R.S.-FNRS; grant n° T.0109.20), from the University of Liege, and from the ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. The Birmingham contribution is in part funded by the European Union’s Horizon 2020 research and innovation programme (grant’s agreement n° 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant nos. ST/S00193X/1, ST/W000385/1 and ST/Y001710/1). The Cambridge contribution is supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. Some of the observations in this paper made use of the High-Resolution Imaging instrument Zorro and were obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Zorro was mounted on the Gemini South telescope of the international Gemini Observatory, a program of NSF’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tec- nologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea).With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).Peer reviewe
MeerKAT view of Hickson Compact Groups: II. HI deficiency in the cores and surrounding regions
No full textSorgho, Amidou et al.-- Full list of authors: Sorgho, A.; Verdes-Montenegro, L.; Ianjamasimanana, R.; Hess, K. M.; Jones, M. G.; Korsaga, M.; Wang, J.; Lin, X.; Solanes, J. M.; Cluver, M. E.; Cannon, J. M.; Bosma, A.; Athanassoula, E.; del Olmo, A.; Perea, J.; Moldón, J.; Wiegert, T.; Sanchez-Expósito, S.; Garrido, J.; García-Benito, R.; Józsa, G. I. G.; Borthakur, S.; Jarrett, T.; Namumba, B.; Pérez, E.; Román, J.; Smirnov, O. M.; Yun, M.Context. Hickson compact groups (HCGs) offer an ideal environment for investigating galaxy transformation as a result of interactions. It has been established that the evolutionary sequence of HCGs is marked by an intermediate stage characterised by a substantial amount of H I in their intragroup medium (IGrM) in the form of tidal tails and bridges (phase 2), rapidly followed by a final stage in which no IGrM gas is found and i which their member galaxies are highly H I deficient (phase 3).Aims. Despite numerous single-dish and interferometric H I studies on the HCGs, a clear H I picture of the groups within their large-scale environment still remains to be uncovered. Taking advantage of MeerKAT’s high column density sensitivity and large field of view, we aim to investigate the rapid transformation of HCGs from the intermediate to late phases, and establish a picture of their gas content variations in the context of their large-scale environments.Methods. We performed MeerKAT observations of six HCGs that were selected to represent the intermediate and late phases of the proposed evolutionary sequence. Combining the H I observations with data from recent wide-field optical surveys, we evaluated the H I deficiencies of galaxies in a ∼30′ radius of the HCGs.Results. We find that galaxies surrounding both phases exhibit similar distributions in their gas content. Similarly, galaxies making up the cores of phase 2 HCGs are comparable to their neighbours in terms of H I deficiencies. However, phase 3 groups are over an order of magnitude more deficient than their surroundings, supporting previous findings that late-phase HCG galaxies are more evolved than their large-scale environments. ©The Authors 2025The MeerKAT telescope is operated by the South African Radio Astronomy Observatory (SARAO), which is a facility of the National Research Foundation, an agency of the Department of Science and Innovation. This work used the Spanish Prototype of an SRC (SPSRC, Garrido et al. 2021) service and support funded by the Ministerio de Ciencia, Innovación y Universidades (MICIU), by the Junta de Andalucía, by the European Regional Development Funds (ERDF) and by the European Union NextGenerationEU/PRTR. The SPSRC acknowledges financial support from the Agencia Estatal de Investigación (AEI) through the “Centre of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (IAA-CSIC) (SEV-2017-0709) and together with the authors AS, LVM, RI, KMH, RGB, AdO, JP, SSE, JG, BN JM, TW and EP from the grant CEX2021-001131-S funded by MICIU/AEI/10.13039/501100011033. AS, LVM, RI, JG, SSE and TW acknowledge financial support from the grant PID2021-123930OB-C21 funded by MICIU/AEI and by ERDF/EU. RI acknowledges financial support from grant TED2021-130231B-I00 funded by MICIU/AEI and by the European Union NextGeneration EU/PRTR. BN acknowledges financial support from the grant PTA2023-023268-I funded by MICIU/AEI. TW acknowledges financial support from the coordination of the participation in SKA-Spain, funded by MICIU. AdO and JP acknowledge further financial support from the MICIU through project PID2022-140871NB-C21 by ERDF/EU. R.G.B. acknowledges further financial support from grant PID2022-141755NB-I00. JM acknowledges financial support from grant PID2023-147883NB-C21, funded by MICIU/AEI/10.13039/501100011033. JMS acknowledges financial support from the Spanish state agency MICIU/AEI/10.13039/501100011033 and by ERDF/EU funds through research grant PID2022-140871NB-C22 and the additional support of MICIU/AEI/10.13039/501100011033 through the Centre of Excellence María de Maeztu’s award for the Institut de Ciències del Cosmos at the Universitat de Barcelona under contract CEX2019–000918–M. EA and AB acknowledge support from the Centre National d’Etudes Spatiales (CNES), France. MEC acknowledges the support of an Australian Research Council Future Fellowship (Project No. FT170100273) funded by the Australian Government. J.R. acknowledges financial support from the Spanish Ministry of Science and Innovation through the project PID2022-138896NB-C55. OMS’s research is supported by the South African Research Chairs Initiative of the Department of Science and Technology and National Research Foundation (grant No. 81737).With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (SEV-2017-0709).With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).Peer reviewe
Selection of texts related to Latin American authors and published in the Yugoslavian journal Mostovi
No full textEsta publicación es parte del proyecto de I+D+i Escritores latinoamericanos en los países socialistas europeos durante la Guerra Fría (PID2020-113994GB-I00), financiado por MCIN/ AEI/10.13039/501100011033/.Esta publicación es parte del proyecto de I+D+i Escritores latinoamericanos en los países socialistas europeos durante la Guerra Fría (PID2020-113994GB-I00), financiado por MCIN/ AEI/10.13039/501100011033/.Peer reviewe
Supplementary Materials: Microalga Nannochloropsis gaditana as a sustainable source of bioactive peptides: A proteomic and in silico approach
No full textFigure S1: Complete Omicbox workflow followed for the proteomic functional analysis of Nannochloropsis gaditana. Figure S2: Complete functional distribution of detected proteins from Nannochloropsis gaditana biomass in cellular component functional group using gene ontology (GO). Figure S3: Complete functional distribution of detected proteins from Nannochloropsis gaditana biomass in biological process functional group using gene ontology (GO). Figure S4: Complete functional distribution of detected proteins from Nannochloropsis gaditana biomass in molecular function functional group using gene ontology (GO). Table S1. Identified proteins from Nannochloropsis gaditana.Peer reviewe
The excitation mechanism of H2 in bipolar planetary nebulae
No full textWe present near-IR K-band intermediate-dispersion spatially-resolved spectroscopic observations of a limited sample of bipolar planetary nebulae (PNe). The spectra have been used to determine the excitation mechanism of the H2 molecule using standard line ratios diagnostics. The H2 molecule is predominantly shock-excited in bipolar PNe with broad equatorial rings, whereas bipolar PNe with narrow equatorial waists present either UV excitation at their cores (e.g. Hb 12) or shock-excitation at their bipolar lobes (e.g. M1-92). The shock-excitation among bipolar PNe with ring is found to be correlated with emission in the H2 1-0 S(1) line brighter than Br γ. We have extended this investigation to other PNe with available near-IR spectroscopic observations. This confirms that bipolar PNe with equatorial rings are in average brighter in H2 than in Br γ and show dominant shock-excitation. © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.MAG and RAM-L are supported by the Spanish MICINN (Ministerio de Ciencia e Innovación) grant AYA 2011-29754-C03-02 cofunded with FEDER funds. RAM-L also acknowledges support by Mexican CONACYT (Consejo Nacional de Ciencia y Tecnología) grant no. 207706. GR-L acknowledges support from CONACYT (grant 177864), CGCI, PROMEP and SEP (Mexico). LFM is supported by the Spanish MICINN grant AYA 2011-30228-C3-01 and MINECO grant AYA 2014-57369-C3-3-P, both cofunded by FEDER funds. Based on observations made with the Italian TNG operated at the Observatorio del Roque de los Muchachos, La Palma, Spain, by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica). Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (IAA-CSIC)