论文标题
第一个样本的H $α$+[O III] $λ$ 5007发射器$ z> 6 $通过JWST/NIRCAM SLITless SLITSPECTROSCOPHY：物理属性和线条光度功能
First Sample of H$α$+[O III] $λ$5007 Line Emitters at $z > 6$ Through JWST/NIRCam Slitless Spectroscopy: Physical Properties and Line Luminosity Functions
论文作者
论文摘要
我们为$ z = 6.11-6.35 $的四个发射线星系提供了一个样本，这些星系使用JWST/NIRCAM宽田slitless slitless slitless sliteblessproscopy（WFSS）模式偶然发现。其中一个（$ z = 6.11 $）先前已报道，而其他人则是新发现。这些来源是由[O III] $λ$ 5007和H $α$线的安全检测选择的，在某些情况下暂时检测到其他fainter线（例如，[O II] $λ$ 3727，[O III] $λ$λ$ 4959）。在[O III]/H $β$ - [N II]/H $α$ baldwin-phillips-terlevich图中，这些星系占据与$ z \ sim2 $ sim2 $ star形成星系相同的参数空间，表明它们与亚sall-Sall-Sall-Sall-Sall-Sall-Sall-Sall-Sall-Sall-Sall-Sall-Sarl-Sall $ 0.4 $ 0.4 $ 0.4 $ 0.4 $ 0.4 $ 0.4 $ \ s_在较低的红移下可比的恒星质量。强h $α$线的检测表明，早期宇宙中星系内的电离光子生产效率更高。我们发现[O III] $λ$ 5007线光度功能（LF）从$ z = 3 $到6，而h $α$α$α$α$α$α$ z = 2 $ to的弱或没有红移的演变。这两个LF在$ z \ sim6 $中的$ z \ sim6 $ by sim $ \ sim $ \ sim $ \ sim $ \ sim by simological Simals in ly selosmological Simerustance in ly simological Simals中。这进一步表明，在$ z \ sim6 $时，通过比较了紫外线衍生的星形构型速率密度和LY $ ly $α$光度密度，$ z \ sim6 $的全球$α$α$α$α$α$α$α$α$α$α$α$α$。我们的样本恢复了$ 66^{+128} _ { - 44} $ z的$ z = 6.0-6.6 $的$ z $ z $ z $ z $ z $ z $ z $ z的星系，恒星质量大于$ 5 \ times10^8 $ $ m _ {\ odot} $ JWST。
We present a sample of four emission-line galaxies at $z=6.11-6.35$ that were serendipitously discovered using the commissioning data for the JWST/NIRCam wide-field slitless spectroscopy (WFSS) mode. One of them (at $z=6.11$) has been reported previously while the others are new discoveries. These sources are selected by the secure detections of both [O III] $λ$5007 and H$α$ lines with other fainter lines tentatively detected in some cases (e.g., [O II] $λ$3727, [O III] $λ$4959). In the [O III]/H$β$ - [N II]/H$α$ Baldwin-Phillips-Terlevich diagram, these galaxies occupy the same parameter space as that of $z\sim2$ star-forming galaxies, indicating that they have been enriched rapidly to sub-solar metallicities ($\sim$0.4 $Z_{\odot}$), similar to galaxies with comparable stellar masses at much lower redshifts. The detection of strong H$α$ lines suggests a higher ionizing photon production efficiency within galaxies in the early Universe. We find brightening of the [O III] $λ$5007 line luminosity function (LF) from $z=3$ to 6, and weak or no redshift evolution of the H$α$ line LF from $z=2$ to 6. Both LFs are under-predicted at $z\sim6$ by a factor of $\sim$10 in certain cosmological simulations. This further indicates a global Ly$α$ photon escape fraction of 7-10% at $z\sim6$, slightly lower than previous estimates through the comparison of the UV-derived star-formation rate density and Ly$α$ luminosity density. Our sample recovers $66^{+128}_{-44}$% of $z=6.0-6.6$ galaxies in the survey volume with stellar masses greater than $5\times10^8$ $M_{\odot}$, suggesting the ubiquity of strong H$α$ and [O III] line emitters in the Epoch of Reionization, which will be further uncovered in the era of JWST.
