Suchergebnisse

We use three semi-analytical models (SAMs) of galaxy formation and evolution run on the same 1 h(-1) Gpc MultiDark Planck2 cosmological simulation to investigate the properties of [O II] emission line galaxies at redshift z similar to 1. We compare model predictions with different observational data sets, including DEEP2-FIREFLY galaxies with absolute magnitudes. We estimate the [O II] luminosity (L[O II]) of our model galaxies using the public code GET EMLINES, which ideally assumes as input the instantaneous star formation rates (SFRs). This property is only available in one of the SAMs under consideration, while the others provide average SFRs, as most models do. We study the feasibility of inferring galaxies' L[O II] from average SFRs in post-processing. We find that the result is accurate for model galaxies with dust attenuated L[O II] less than or similar to 10(42.2) erg s(-1) ( 10(40.4) erg s(-1) remains overall unchanged on scales above 1 h(-1) Mpc, independently of the L[O II] computation. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society ; GFandVGPacknowledge support from the University of Portsmouth through the Dennis Sciama Fellowship award. VGP acknowledges support from the European Research Council under the European Union's Horizon 2020 research and innovation programme (grant agreement No 769130). DS is funded by the Spanish Ministry of Economy and Competitiveness (MINECO) under the 2014 Severo Ochoa Predoctoral Training Programme. DS also wants to thank the Mamua Cafe Bar-team for their kind (g)astronomical support. DS and FP acknowledge funding support from the MINECO grant AYA2014-60641-C2-1-P. AO acknowledges support from the Spanish Ministerio de Economia y Competitividad (MINECO) project No. AYA2015-66211-C2-P-2, and funding from the European Union Horizon 2020 research and innovation programme under grant agreement No. 734374. SAC acknowledges funding from Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET, PIP0387), Agencia Nacional de Promocion Cientifica y Tecnologica (ANPCyT, PICT-2013-0317), and Universidad Nacional de La Plata (11-G124 and 11-G150), Argentina. CVMacknowledges CONICET, Argentina, for the supporting fellowship. AK is supported by the MINECO and the Fondo Europeo de Desarrollo Regional (FEDER, UE) in Spain through grant AYA2015-63810-P as well as by the MICIU/FEDER through grant number PGC2018-094975-C21. He further acknowledges support from the Spanish Red Consolider MultiDark FPA2017-90566-REDC and thanks Christopher Cross for sailing. ARHS acknowledges receipt of the Jim Buckee Fellowship at ICRAR-UWA. GF, VGP and DS wish to thank La Plata Astronomical Observatory for hosting the MultiDark Galaxies workshop in September 2016, during which this work was started. The authors thank the FIREFLY team and the anonymous referee for providing insightful comments. The analysis of DEEP2 data using the FIREFLY code was done on the Sciama High Performance Compute cluster which is supported by the ICG, SEPNet and the University of Portsmouth (UK). The CosmoSim database used in this paper is a service by the Leibniz-Institute for Astrophysics Potsdam (AIP). The MultiDark database was developed in cooperation with the Spanish MultiDark Consolider Project CSD200900064. The authors gratefully acknowledge the Gauss Centre for Supercomputing e.V. (www.gauss-centre.eu) and the Partnership for Advanced Supercomputing in Europe (PRACE, www.praceri.eu) for funding the MultiDark simulation project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre (LRZ, www.lrz.de).The authors thank New Mexico State University (USA) and Instituto de Astrof ' isica de Andalucia CSIC (Spain) for hosting the SKIES& UNIVERSES database for cosmological simulation products. This work has benefited from the publicly available software tools and packages: MATPLOTLIB14 2012-2016 (Hunter 2007); PYTHON SOFTWARE FOUNDATION15 19902017, version 2.7., PYTHONBREW16; we use whenever possible in this work a colour-blind friendly colour palette17 for our plots. ; Peer reviewed

The Javalambre Photometric Local Universe Survey (J-PLUS) is an ongoing 12-band photometric optical survey, observing thousands of square degrees of the Northern Hemisphere from the dedicated JAST/T80 telescope at the Observatorio Astrofísico de Javalambre (OAJ). The T80Cam is a camera with a field of view of 2 deg 2 mounted on a telescope with a diameter of 83 cm, and is equipped with a unique system of filters spanning the entire optical range (3500-10 000 Å). This filter system is a combination of broad-, medium-, and narrow-band filters, optimally designed to extract the rest-frame spectral features (the 3700-4000 Å Balmer break region, Hδ, Ca H+K, the G band, and the Mg b and Ca triplets) that are key to characterizing stellar types and delivering a low-resolution photospectrum for each pixel of the observed sky. With a typical depth of AB ∼21.25 mag per band, this filter set thus allows for an unbiased and accurate characterization of the stellar population in our Galaxy, it provides an unprecedented 2D photospectral information for all resolved galaxies in the local Universe, as well as accurate photo-z estimates (at the δ z/(1 + z)∼0.005-0.03 precision level) for moderately bright (up to r∼20 mag) extragalactic sources. While some narrow-band filters are designed for the study of particular emission features ([O II]/λ3727, Hα/λ6563) up to z< 0.017, they also provide well-defined windows for the analysis of other emission lines at higher redshifts. As a result, J-PLUS has the potential to contribute to a wide range of fields in Astrophysics, both in the nearby Universe (Milky Way structure, globular clusters, 2D IFU-like studies, stellar populations of nearby and moderate-redshift galaxies, clusters of galaxies) and at high redshifts (emission-line galaxies at z≈0.77, 2.2, and 4.4, quasi-stellar objects, etc.). With this paper, we release the first ∼1000 deg 2 of J-PLUS data, containing about 4.3 million stars and 3.0 million galaxies at r< 21 mag. With a goal of 8500 deg 2 for the total J-PLUS footprint, these numbers are expected to rise to about 35 million stars and 24 million galaxies by the end of the survey. © ESO 2019. ; Funding for the J-PLUS Project has been provided by the Governments of Spain and Aragon through the Fondo de Inversiones de Teruel, by the Spanish Ministry of Economy and Competitiveness (MINECO; under grants AYA2012-30789, AYA2013-40611-P, AYA2015-66211-C2-1-P, AYA2015-66211-C2-2, AYA2016-77846-P, AYA2016-77237-C3-1-P, AYA2016-75931-C2-1-P, AYA2017-86274-P, AGAURgrantSGR-661/2017, andICTS-2009-14), byFAPERJ the Government of Aragon, through the Grupo de Investigacion E16_17R, and by European FEDER funding (FCDD10-4E-867, FCDD13-4E-2685). Further support has been provided by the Ramon y Cajal programmes RYC-2016-20254, RYC-2011-08262 and RYC-2011-08529. This research has made use of the Spanish Virtual Observatory (http://svo.cab.inta-csic.es) supported from the Spanish MINECO through grant AYA2014-55216. We also acknowledge Spanish CSIC (I-COOP+ 2016 program) through grant COOPB20263. The Brazilian agencies FAPESP and the National Observatory of Brazil have also contributed to this project. We acknowledge financial support from the Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro - FAPERJ (fellowship Nota 10, PDR-10), from CNPq through BP grant 312307/2015-2 and Universal Grants 459553/20143, PQ 302037/2015-2, and PDE 200289/2017-9), FINEP grants REF. 1217/13 -01.13.0279.00 and REF 0859/10 -01.10.0663.00, from FAPERJ grant E-26/202.835/2016, and CAPES (Science without Borders program, Young Talent Fellowship, BJT) through grants A062/2013 and CAPES-PNPD 2940/2011. The FAPESP grants no. 2015/12745-6, 2014/11338-5, 2014/07684-5, 2013/04582-4 and 2009/54202-8 are also acknowledged. Finally, the authors acknowledge partial support from grant PHY 14-30152; Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE), awarded by the US National Science Foundation. ; Peer Reviewed