论文标题
清除：恒星星系的气相金属性梯度在0.6 <z <2.6
CLEAR: The Gas-Phase Metallicity Gradients of Star-Forming Galaxies at 0.6 < z < 2.6
论文作者
论文摘要
我们报告以0.6 <z <2.6的264个星形星系样品样品的气相金属性梯度，该星系通过深近红外的哈勃太空望远镜静脉内无频谱测量。观察结果包括12个轨道深度/WFC3 G102 G102 GRISM光谱作为Reionization（Clear）调查时Lya排放的一部分，以及档案WFC3 G102+G141 G141 Grism光谱重叠了清晰的足迹。该样品中的大多数星系（84％）与整个质量范围的零或略有正金属梯度一致（8.5 <log m _*/m_sun <10.5）。我们测量了金属性梯度的内在种群散射，并表明它随着恒星质量的降低而增加 - 与文献中先前的报道一致，但在这里证实了更大的样本。为了理解管理这种散射的物理机制，我们在固定质量处搜索观察到的梯度和各种恒星种群特性之间的相关性。但是，我们没有发现与我们考虑的星系特性相关的证据 - 包括恒星形成率，大小，恒星形成速率表面密度和每个重力势能的恒星形成速率。我们使用观察到的这些相关性的弱点为理论模型的预测固有相关性提供材料约束。
We report on the gas-phase metallicity gradients of a sample of 264 star-forming galaxies at 0.6 < z < 2.6, measured through deep near-infrared Hubble Space Telescope slitless spectroscopy. The observations include 12-orbit depth Hubble/WFC3 G102 grism spectra taken as a part of the CANDELS Lya Emission at Reionization (CLEAR) survey, and archival WFC3 G102+G141 grism spectra overlapping the CLEAR footprint. The majority of galaxies (84%) in this sample are consistent with a zero or slightly positive metallicity gradient across the full mass range probed (8.5 < log M_*/M_sun < 10.5). We measure the intrinsic population scatter of the metallicity gradients, and show that it increases with decreasing stellar mass---consistent with previous reports in the literature, but confirmed here with a much larger sample. To understand the physical mechanisms governing this scatter, we search for correlations between the observed gradient and various stellar population properties at fixed mass. However, we find no evidence for a correlation with the galaxy properties we consider---including star-formation rates, sizes, star-formation rate surface densities, and star-formation rates per gravitational potential energy. We use the observed weakness of these correlations to provide material constraints for predicted intrinsic correlations from theoretical models.
