发表机构
University of Padova; Institute of Space Sciences (ICE, CSIC); Instituto de Astrofísica de Canarias; Universidad de La Laguna; Steward Observatory and Department of Astronomy, University of Arizona; Universidad de Córdoba（帕多瓦大学; 空间科学研究所; 加那利天体物理研究所; 拉古纳大学; 亚利桑那大学斯图尔德天文台及天文系; 科尔多瓦大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文研究超深光学成像中银河卷云污染问题，发现赫歇尔远红外示踪虽可识别卷云，但分辨率限制使极限面亮度仅达28 mag/arcsec$^2$，远浅于LIGHTS和LSST的30.5 mag/arcsec$^2$深度，凸显现有远红外数据的根本局限，需更高分辨率示踪剂。
AI 中文摘要
当前及即将开展的深光学成像巡天正达到比30 mag/arcsec$^2$更暗的面亮度水平，在此水平下，银河卷云发射成为显著的污染源。这对极低面亮度河外星系结构的研究构成了重大挑战。我们研究了由赫歇尔250 $\mu$m波段示踪的远红外发射与斯隆\textit{g}波段和\textit{r}波段光学面亮度之间的关系。我们发现，对于$\mu_g\gtrsim$~27 mag/arcsec$^2$的银河卷云，假设尘埃光学薄，线性关系与数据一致，光学卷云发射约占远红外通量的$\sim$0.1\\%。使用赫歇尔远红外数据示踪银河卷云可使其在大范围内被识别，但代价是显著降低空间分辨率。这一限制引入了源混淆，并限制了可在光学数据中稳健探测的有效面亮度深度。我们表明，当使用赫歇尔250 $\mu$m数据对卷云发射进行建模时，极限面亮度为$\mu_V\sim$~28 mag/arcsec$^2$，明显浅于LIGHTS或10年叠加LSST（$\mu_V\sim$~30.5 mag/arcsec$^2$）等巡天的标称深度。这些结果凸显了在超深光学成像中利用现有远红外数据进行卷云抑制的根本局限性，并强调需要更高分辨率的卷云示踪剂以充分利用即将开展的巡天的深度。
英文摘要
Current and forthcoming deep optical imaging surveys are reaching surface brightness levels fainter than 30 mag/arcsec$^2$, where Galactic cirrus emission becomes a significant contaminant. This poses a major challenge for the study of extremely low-surface-brightness extragalactic structures. We investigate the relationship between far-infrared emission, as traced by the Herschel 250 $μ$m band, and optical surface brightness in the Sloan \textit{g}- and \textit{r}-bands. We find that, for Galactic cirrus with $μ_g\gtrsim$~27 mag/arcsec$^2$, a linear relation is consistent with the data, assuming optically thin dust, with optical cirrus emission amounting to $\sim$0.1\% of the far-infrared flux. Using Herschel far-infrared data to trace Galactic cirrus enables its identification over wide areas, but at the cost of significantly reducing spatial resolution. This limitation introduces source confusion and restricts the effective surface brightness depth that can be robustly probed in optical data. We show that, when cirrus emission is modeled using Herschel 250 $μ$m data, the limiting surface brightness is $μ_V\sim$~28 mag/arcsec$^2$, substantially shallower than the nominal depth of surveys such as LIGHTS or the 10-year coadd LSST ($μ_V\sim$~30.5 mag/arcsec$^2$). These results highlight a fundamental limitation in the use of currently available far-infrared data for cirrus mitigation in ultra-deep optical imaging, and emphasize the need for higher-resolution cirrus tracers to fully exploit the depth of upcoming surveys.
CommentsAccepted for publication in A&A. Fig.5 summarizes our modeling approach & Fig.6 shows the outcome of our Galactic Cirrus removal method
