A901/2中发射线Galerkin的PDKEEPAAA-OSIRIS映射：IV。- 具有倾角的星形成估计的熄灭性
OMEGA - OSIRIS Mapping of Emission-line Galaxies in A901/2: IV. - Extinction of Star-Formation Estimators with Inclination
摘要：
我们研究了倾角对恒星形成星系在光谱通带中的视亮度的影响，这些通带通常被用作恒星形成的指标。作为诊断，我们使用三个通带中的质光比：280 nm处的UV连续谱、H $α$发射线和FIR 24 $μ$带。我们包括在IR/UV比（“IRX”）和IR/H $α$比的倾斜趋势的研究。我们的样本包括来自Abell 901/902星系团周围区域的几百个星系，这些星系具有哈勃太空望远镜图像中从外盘测量的深度数据和倾角。作为一个新颖的，H $α$ -和单独的NII-发射测量可调滤波器成像和包括星系的整体。在星系恒星质量超过log $M_*/M_\odot > 10$时，我们发现UV和H $α$的质光比的趋势表明，在UV和H $α$中，$\sim 1$和$\sim 0.7$分别从正面到侧面倾斜引起衰减，这意味着在侧面星系的恒星形成率将被UV中的$\sim 2.5\times$和H $α$中的$\sim 2\times$低估。我们发现在UV和H $α$的光度是很好的相关性，但光学深度的弥漫尘埃，导致倾斜的依赖似乎是较低的恒星在280 nm发射比气体云发射巴耳末线。对于星系日志$M_*/M_\odot < 9.7$，我们发现没有可测量的影响在$>0.1$马格。在24 $μ$的倾斜依赖的情况下确认，平均星系是光学薄的FIR。
英文摘要：
We study the effect of inclination on the apparent brightness of star-forming galaxies in spectral passbands that are commonly used as star-formation indicators. As diagnostics we use mass-to-light ratios in three passbands: the UV continuum at 280 nm, the H$α$ emission line, and the FIR 24$μ$-band. We include a study of inclination trends in the IR/UV ratio ("IRX") and the IR/H$α$ ratio. Our sample comprises a few hundred galaxies from the region around the clusters Abell 901/902 with deep data and inclinations measured from outer disks in Hubble Space Telescope images. As a novelty, the H$α$- and separately the NII-emission are measured by tunable-filter imaging and encompass galaxies in their entirety. At galaxy stellar masses above log $M_*/M_\odot > 10$ we find trends in the UV and H$α$ mass-to-light ratio that suggest an inclination-induced attenuation from face-on to edge-on of $\sim 1$ mag and $\sim 0.7$ mag in UV and H$α$, respectively, implying that star-formation rates of edge-on galaxies would be underestimated by $\sim 2.5\times$ in UV and $\sim 2\times$ in H$α$. We find the luminosities in UV and H$α$ to be well correlated, but the optical depth of diffuse dust that causes inclination dependence appears to be lower for stars emitting at 280 nm than for gas clouds emitting Balmer lines. For galaxies with log $M_*/M_\odot < 9.7$, we find no measurable effect at $>0.1$ mag. The absence of an inclination dependence at 24$μ$ confirms that the average galaxy is optically thin in the FIR.
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