Attenuation proxy hidden in surface brightness -- colour diagrams. A new strategy for the LSST era.
Attenuation proxy hidden in surface brightness -- colour diagrams. A new strategy for the LSST era.
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隐藏在表面亮度中的衰减代理——彩色图表。
DOI：
10.1051/0004-6361/202348432
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发表时间：
2024
影响因子：
6.5
通讯作者：
Malek K
中科院分区：
文献类型：
--
作者：
Malek K
目标 未来的大型天空调查，例如传统时空调查 (LSST)，将为数十亿个物体提供光学光度测量。对星系物理特性的可靠估计需要有关尘埃衰减的信息，这些信息通常来自紫外线 (UV) 和红外线 (IR) 数据。本文旨在仅根据光学数据构建远紫外（FUV）衰减（AFUVp）的代理，从而能够快速估计缺乏紫外或红外数据的星系的恒星形成率（SFR）。这将加速和改进对数十亿个类 LSST 观测星系（仅在光学波段观测）的关键物理特性的估计。方法为了模拟 LSST 观测，我们使用了斯隆数字巡天 (SDSS) 光度目录第 12 版的深度全色光学覆盖范围，并辅以来自 GALEX-SDSS-WISE 传统目录 (GSWLC) 的 SDSS 星系估计物理特性和获得的倾角信息来自 SDSS 数据发布 7。我们将样本限制在 0.025–0.1 光谱红移范围，并研究了从光谱能量分布 (SED) 获得的恒星形成星系的 FUV 范围内的表面亮度、颜色和尘埃衰减之间的关系。结果尘埃衰减与 u 和 r 波段 (u−r) 之间测量的颜色以及 u 波段 (μu) 中的表面亮度最相关。我们为恒星形成主序带上的星系提供尘埃衰减代理。该关系可用于 LSST 或任何其他类型的宽带光学测量。发现 SFR 的目录值与使用仅光学 SDSS 数据和 AFUVpprior 计算的值之间的平均比率，计算公式为 ΔSFR = log(SFRthis work/SFRGSWLC)，小于 0.1 dex，而没有先验的运行会导致 SFR 高估大于 0.3 dex。 AFUV的存在与否对恒星质量（Mstar）估计的影响可以忽略不计（ΔMstar的范围是0到-0.15 dex）。结论我们注意到AFUV对于低红移主序星系是可靠的。即将进行的 LSST 深钻场深度光学观测也具有多波长数据，这将使人们能够校准所获得的较高红移星系的关系，并可能将研究扩展到其他类型的星系，例如远离主序的早期型星系。
AimsLarge future sky surveys, such as the Legacy Survey of Space and Time (LSST), will provide optical photometry for billions of objects. Reliable estimation of the physical properties of galaxies requires information about dust attenuation, which is usually derived from ultraviolet (UV) and infrared (IR) data. This paper aims to construct a proxy for the far-UV (FUV) attenuation (AFUVp) from the optical data alone, enabling the rapid estimation of the star formation rate (SFR) for galaxies that lack UV or IR data. This will accelerate and improve the estimation of key physical properties of billions of LSST–like observed galaxies (observed in the optical bands only).MethodsTo mimic LSST observations, we used the deep panchromatic optical coverage of the Sloan Digital Sky Survey (SDSS) Photometric Catalogue, Data Release 12, complemented by the estimated physical properties for the SDSS galaxies from the GALEX-SDSS-WISE Legacy Catalog (GSWLC) and inclination information obtained from the SDSS Data Release 7. We restricted our sample to the 0.025–0.1 spectroscopic redshift range and investigated relations among surface brightness, colours, and dust attenuation in the FUV range for star-forming galaxies obtained from the spectral energy distribution (SED).ResultsDust attenuation is best correlated with colour measured betweenuandrbands (u−r) and the surface brightness in theuband (μu). We provide a dust attenuation proxy for galaxies on the star-forming main sequence. This relation can be used for the LSST or any other type of broadband optical survey. The mean ratio between the catalogue values of SFRs and those estimated using optical-only SDSS data with theAFUVpprior calculated as ΔSFR = log(SFRthis work/SFRGSWLC) is found to be less than 0.1 dex, while runs without priors result in an SFR overestimation larger than 0.3 dex. The presence or absence of theAFUVphas a negligible influence on the stellar mass (Mstar) estimation (with ΔMstarin the range from 0 to −0.15 dex).ConclusionsWe note thatAFUVpis reliable for low-redshift main sequence galaxies. Forthcoming deep optical observations of the LSST Deep Drilling Fields, which also have multi-wavelength data, will enable one to calibrate the obtained relation for higher redshift galaxies and, possibly, extend the study towards other types of galaxies, such as early-type galaxies off the main sequence.