Beyond UVJ: Color Selection of Galaxies in the JWST Era
Beyond UVJ: Color Selection of Galaxies in the JWST Era
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DOI：
10.3847/1538-4357/aca294
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发表时间：
2022-07
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通讯作者：
Jacqueline Antwi-Danso;C. Papovich;J. Leja;D. Marchesini;Z. C. Marsan;N. Martis;I. Labb'e;A. Muzzin;K. Glazebrook;Caroline M. S. Straatman;K. Tran
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作者：
Jacqueline Antwi-Danso;C. Papovich;J. Leja;D. Marchesini;Z. C. Marsan;N. Martis;I. Labb'e;A. Muzzin;K. Glazebrook;Caroline M. S. Straatman;K. Tran
我们提出了一个新的休息帧颜色选择方法，使用合成的u-gs和g-iss，（ugi）s颜色来识别恒星形成和静止星系。我们的方法类似于广泛使用的U − V vs V − J（UVJ）图。然而，UVJ遭受已知的系统学。光谱活动表明，紫外线选择的z = 3的静态样本包括10%-30%的污染，来自尘埃遮蔽的星星形成和强发射线的星系。此外，在z > 3时，UVJ的颜色是外推的，因为静止框架带移动超出了3处最深带通的覆盖范围，并且可以应用于JWST时代的星系。我们应用（ugi）的选择，在0.5 < z < 6的星系从（观察）3D-HST和UltraVISTA目录，和（模拟）JAGUAR目录。我们发现外推可以影响（V-J）0色高达1等，但改变（gs-is）0色≤0.2等，即使在z = 6。虽然（ugi）s -选择的静态样品在完整性上与UVJ相当（两者在z = 3-3.5时均达到1085%-90%），但（ugi）s将静态样品中的污染物减少了近2倍，在z = 3时从1035%减少到1017%，在z = 6时从1060%减少到1033%。这导致了真假阳性比（TP/FP）的改善，其中我们发现在z = 3.5 − 6处的（ugi）s的TP/FP <2.2，而UVJ选择的样品的TP/FP < 1。这表明，在这些红移的UVJ中，污染物的数量将超过真正的静止星系，而（ugi）s将提供更高保真的样本。
We present a new rest-frame color–color selection method using synthetic u s − g s and g s − i s , (ugi) s colors to identify star-forming and quiescent galaxies. Our method is similar to the widely used U − V versus V − J (UVJ) diagram. However, UVJ suffers known systematics. Spectroscopic campaigns have shown that UVJ-selected quiescent samples at z ≳ 3 include ∼10%–30% contamination from galaxies with dust-obscured star formation and strong emission lines. Moreover, at z > 3, UVJ colors are extrapolated because the rest-frame band shifts beyond the coverage of the deepest bandpasses at 3, and can be applied to galaxies in the JWST era. We apply (ugi) s selection to galaxies at 0.5 < z < 6 from the (observed) 3D-HST and UltraVISTA catalogs, and to the (simulated) JAGUAR catalogs. We show that extrapolation can affect (V − J)0 color by up to 1 mag, but changes (gs−is)0 color by ≤0.2 mag, even at z ≃ 6. While (ugi) s -selected quiescent samples are comparable to UVJ in completeness (both achieve ∼85%–90% at z = 3–3.5), (ugi) s reduces contamination in quiescent samples by nearly a factor of 2, from ≃35% to ≃17% at z = 3, and from ≃60% to ≃33% at z = 6. This leads to improvements in the true-to-false-positive ratio (TP/FP), where we find TP/FP ≳2.2 for (ugi) s at z ≃ 3.5 − 6, compared to TP/FP < 1 for UVJ-selected samples. This indicates that contaminants will outnumber true quiescent galaxies in UVJ at these redshifts, while (ugi) s will provide higher-fidelity samples.