We fit model spectral energy distributions to each pixel in 67 nearby (<z>=0.0057) galaxies using broadband photometry from the Sloan Digital Sky Survey and GALEX. For each galaxy, we compare the stellar mass derived by summing the mass of each pixel to that found from fitting the entire galaxy treated as an unresolved point source. We find that, while the pixel-by-pixel and unresolved masses of galaxies with low specific star formation rates (such as ellipticals and lenticulars) are in rough agreement, the unresolved mass estimate for star-forming galaxies is systematically lower then the measurement from spatially-resolved photometry. The discrepancy is strongly correlated with sSFR, with the highest sSFRs in our sample having masses underestimated by 25% (0.12 dex) when treated as point sources. We found a simple relation to statistically correct mass estimates derived from unresolved broad-band SED fitting to the resolved mass estimates: m_{resolved} = m_{unresolved}/(-0.057log(sSFR) + 0.34) where sSFR is in units of yr^{-1}. We study the effect of varying spatial resolution by degrading the image resolution of the largest images and find a sharp decrease in the pixel-by-pixel mass estimate at a physical scale of approximately 3 kpc, which is comparable to spiral arm widths. The effects we observe are consistent with the "outshining" idea which posits that the youngest stellar populations mask more massive, older -- and thus fainter -- stellar populations. Although the presence of strong dust lanes can also lead to a drastic difference between resolved and unresolved mass estimates (up to 45% or 0.3 dex) for any individual galaxy, we found that resolving dust does not affect mass estimates on average. The strong correlation between mass discrepancy and sSFR is thus most likely due to the outshining systematic bias.
Sparks II: Panchromatic SED modeling and galaxy physical properties across the starburst to post-starburst sequence
Kavli Institute for Particle Astrophysics & Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理与宇宙学研究所）；Center for Decoding the Universe, Stanford University（斯坦福大学解码宇宙中心）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理科学系）；Department of Astronomy and Astrophysics, University of California Santa Cruz（加州大学圣克鲁兹分校天文与天体物理系）；Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU)（宇宙物理与数学卡弗里研究所）；Division of Science, National Astronomical Observatory of Japan（日本国立天文台科学部）；Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理学研究所）
Uncertainties in high-$z$ galaxy properties inferred from SED fitting using JWST NIRCam photometry
Yonsei University（延世大学）；University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理研究所）；Centre de Recherche Astrophysique de Lyon UMR5574, Univ Lyon, Univ Lyon1, Ens de Lyon（里昂天体物理研究中心）
There Is More to Outshining: 2D Dust Effects on Stellar Mass Estimates at $3 \leq z < 9$ with JWST in the JADES Field
Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）；INAF – IASF Milano（意大利国家天体物理研究所米兰分部）；Department of Physics, University of Oxford（牛津大学物理系）；National Centre for Nuclear Research（国家核研究中心）；Aix Marseille Univ. CNRS, CNES, LAM（艾克斯马赛大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Max-Planck-Institut für extraterrestrische Physik (MPE)（马克斯·普朗克地外物理学研究所）
NBursts+phot: parametric recovery of galaxy star formation histories from the simultaneous fitting of spectra and broad-band spectral energy distributions
A normalizing flow approach for the inference of star cluster properties from unresolved broadband photometry I: Comparison to spectral energy distribution fitting
Universität Heidelberg（海德堡大学）；Université Côte d’Azur（蔚蓝海岸大学）；Universidad Nacional Autónoma de México（墨西哥国立自治大学）；INAF – Arcetri Astrophysical Observatory（意大利国家天体物理研究所阿切特里天文台）；University of Wyoming（怀俄明大学）；Australian National University（澳大利亚国立大学）；The Johns Hopkins University（约翰斯·霍普金斯大学）
On the Impact of Inclination-Dependent Attenuation on Derived Star Formation Histories: Results from Disk Galaxies in the Great Observatories Origins Deep Survey Fields
Comparing the Near-infrared Spectral Energy Distributions from Different Stellar Population Synthesis Models with SPHEREx Observations
Research Institute of Basic Sciences, Seoul National University（首尔大学基础科学研究院）；Seoul National University（首尔大学）；Yonsei University（延世大学）；Korea Astronomy and Space Science Institute（韩国天文与空间科学研究所）；IPAC, California Institute of Technology（加州理工学院IPAC）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；California Institute of Technology（加州理工学院）
Far-infrared to centimeter emission of very nearby galaxies with archival data
Université de Strasbourg（斯特拉斯堡大学）；CNRS（法国国家科学研究中心）；Observatoire astronomique de Strasbourg（斯特拉斯堡天文台）；Ghent University（根特大学）；IPAC, California Institute of Technology（加州理工学院/IPAC）；DLR Galileo Competence Center（德国航空航天中心伽利略能力中心）；Institut de Recherche en Astrophysique et Planétologie（天体物理学与行星学研究所在）
Synthetic JWST galaxy images in the TNG50 simulation - I. Model validation and comparison to observations
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México（墨西哥国立自治大学无线电天文学与天体物理研究所）；Harvard-Smithsonian Center for Astrophysics（哈佛-史密森尼天体物理中心）
