The miniJPAS survey: Identification and characterization of galaxy populations with the J-PAS photometric system
R. M. González Delgado, L. A. Díaz-García, A. de Amorim, G. Bruzual, R. Cid Fernandes, E. Pérez, S. Bonoli, A. J. Cenarro, P. R. T. Coelho, A. Cortesi, R. Garcí… 展开作者
R. M. González Delgado, L. A. Díaz-García, A. de Amorim, G. Bruzual, R. Cid Fernandes, E. Pérez, S. Bonoli, A. J. Cenarro, P. R. T. Coelho, A. Cortesi, R. García-Benito, R. López Fernández, G. Martínez-Solaeche, J. E. Rodríguez-Martín, G. Magris, A. Mejía-Narvaez, D. Brito-Silva, L. R. Abramo, J. M. Diego, R. A. Dupke, A. Hernán-Caballero, C. Hernández-Monteagudo, C. López-Sanjuan, A. Marín-Franch, V. Marra, M. Moles, A. Montero-Dorta, C. Queiroz, L. Sodré, J. Varela, H. Vázquez Ramió, J. M. Vílchez, P. O. Baqui, N. Benítez, D. Cristóbal-Hornillos, A. Ederoclite, C. Mendes de Oliveira, T. Civera, D. Muniesa, K. Taylor, E. Tempel, the J-PAS collaboration
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27 pages, 23 figures, 3 tables, accepted for publication in Astronomy & Astrophysics
J-PAS will soon start imaging 8000 deg2 of the northern sky with its unique set of 56 filters (R $\sim$ 60). Before, we observed 1 deg2 on the AEGIS field with an interim camera with all the J-PAS filters. With this data (miniJPAS), we aim at proving the scientific potential of J-PAS to identify and characterize the galaxy populations with the goal of performing galaxy evolution studies across cosmic time. Several SED-fitting codes are used to constrain the stellar population properties of a complete flux-limited sample (rSDSS <= 22.5 AB) of miniJPAS galaxies that extends up to z = 1. We find consistent results on the galaxy properties derived from the different codes, independently of the galaxy spectral-type or redshift. For galaxies with SNR>=10, we estimate that the J-PAS photometric system allows to derive stellar population properties with a precision that is equivalent to that obtained with spectroscopic surveys of similar SNR. By using the dust-corrected (u-r) colour-mass diagram, a powerful proxy to characterize galaxy populations, we find that the fraction of red and blue galaxies evolves with cosmic time, with red galaxies being $\sim$ 38% and $\sim$ 18% of the whole population at z = 0.1 and z = 0.5, respectively. At all redshifts, the more massive galaxies belong to the red sequence and these galaxies are typically older and more metal rich than their counterparts in the blue cloud. Our results confirm that with J-PAS data we will be able to analyze large samples of galaxies up to z $\sim$ 1, with galaxy stellar masses above of log(M$_*$/M$_{\odot}$) $\sim$ 8.9, 9.5, and 9.9 at z = 0.3, 0.5, and 0.7, respectively. The SFH of a complete sub-sample of galaxies selected at z $\sim$ 0.1 with log(M$_*$/M$_{\odot}$) > 8.3 constrain the cosmic evolution of the star formation rate density up to z $\sim$ 3 in good agreement with results from cosmological surveys.
Unveiling the small-scale web around galaxies with miniJPAS and DESI
Max-Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（理化学研究所木下原宇宙起源研究核心理论中心（ Kavli IPMU）、东京大学宇宙射线研究所、东京大学）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；IKERBASQUE, Basque Foundation for Science（伊克尔巴斯基克科学基金会）；Hamburger Sternwarte, Universität Hamburg（汉堡天文台，汉堡大学）；Instituto de Astrofísica de Andalucía (IAA-CSIC)（安达卢西亚天体物理学研究所）；Tartu Observatory, University of Tartu（塔尔图天文台，塔尔图大学）；Estonian Academy of Sciences（爱沙尼亚科学院）；Departamento de Física Matemática, Instituto de Física, Universidade de São Paulo（圣保罗大学数学物理系、物理研究所）；Observatori Astronòmic de la Universitat de València（瓦伦西亚大学天文台）；Departament d’Astronomia i Astrofísica, Universitat de València（瓦伦西亚大学天文学与天体物理学系）；Departamento de Física, Universidade Federal do Espírito Santo（圣埃斯皮里图联邦大学物理系）
The miniJPAS survey: Dissecting galaxy properties across environments with spatially resolved photometry
Universidade Federal de Santa Catarina（圣卡塔琳娜联邦大学）；University of Heidelberg（海德堡大学）；Instituto de Física de Cantabria (CSIC-UC)（坎塔布里亚物理研究所）；Unidad Asociada “Grupo de Astrofísica Extragaláctica y Cosmología”, IFCA-CSIC/Universitat de València（IFCA-CSIC/瓦伦西亚大学联合单位“河外天体物理学与宇宙学组”）；Instituto de Física, Universidade de São Paulo（圣保罗大学物理研究所）；Observatório Nacional – MCTI (ON)（国家天文台）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；IKERBASQUE, Basque Foundation for Science（伊克尔巴斯克，巴斯克科学基金会）；Centro de Estudios de Física del Cosmos de Aragón (CEFCA)（阿拉贡宇宙物理学研究中心）
Exploring the spatially-resolved capabilities of the J-PAS survey with Py2DJPAS
Universidade Federal de Santa Catarina（圣卡塔琳娜联邦大学）；Instituto de Física de Cantabria (CSIC-UC)（坎塔布里亚物理研究所）；Universitat de València（瓦伦西亚大学）；University of Vienna（维也纳大学）；Universidade de São Paulo（圣保罗大学）；Observatório Nacional – MCTI (ON)（国家天文台）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；IKERBASQUE, Basque Foundation for Science（伊克拉巴斯基克，巴斯克科学基金会）；Centro de Estudios de Física del Cosmos de Aragón (CEFCA)（阿拉贡宇宙物理学研究中心）
J-PAS: A value-added catalogue of optical line intensities for nebular emission galaxies (JOLINES)
Unidad Asociada CEFCA--IAA（CEFCA-IAA联合单位）；Institute of Science and Technology Austria (ISTA)（奥地利科学技术研究院）；INAF--Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天文台与空间科学部）；Department of Astrophysics, University of Vienna（维也纳大学天体物理系）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；Universidad de La Laguna（拉古纳大学）；National Astronomical Observatory of China, Chinese Academy of Sciences（中国科学院国家天文台）；Instruments4
Toward Bayesian photometric cosmic chronometers: Application to VIPERS
Institute of Space Sciences (ICE, CSIC)（空间科学研究所）；Institut d´Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院）；Institute of Cosmology and Gravitation (ICG), University of Portsmouth（朴茨茅斯大学宇宙学与引力研究所）；Department of Astronomy, Tsinghua University（清华大学天文系）；Instituto de Astrofísica de Canarias (IAC)（加那利天体物理研究所）；Universidad de La Laguna (ULL)（拉古纳大学）；European Space Agency (ESA)（欧洲航天局）；European Space Astronomy Centre (ESAC)（欧洲空间天文中心）
Correction to the photometric colors of the Gaia Data Release 2 with the stellar color regression method
第二次盖亚数据发布（DR 2）提供了整个天空的精确和均匀的测光数据，达到了G，GRP和GBP通带前所未有的毫量级（mmag）水平。然而，在10 mmag水平上存在的星等依赖系统效应限制了其在科学开发中的力量。在这项工作中，使用大约50万颗与LAMOST DR 5相同的恒星，我们应用基于光谱的恒星颜色回归方法来校准Gaia G-GRP和GBP-GRP的颜色。以前所未有的精度约1毫等，系统的趋势与G星等揭示了两种颜色的非常详细，反映了仪器配置的变化。对GBP-GRP和亮度大于G~11.5等的恒星，发现了颜色依赖的趋势，刻度一般可达20 mmag，变化范围为几mmag/mag，给出了Gaia DR 2的修正色图，并简要讨论了一些应用。
Galaxy spectroscopy without spectra: Galaxy properties from photometric images with conditional diffusion models
University of Bern（伯尔尼大学）；Ludwig-Maximilians Universität München（慕尼黑大学）；INAF - Astronomical Observatory of Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；INFN - Sezione di Napoli（意大利国家核物理研究所那不勒斯分所）；University Federico II（那不勒斯费德里科二世大学）；University of Bologna（博洛尼亚大学）；ARTORG Center（ARTORG中心）；AIMI
