Reconciling the results of the z ∼ 2 MOSDEF and KBSS-MOSFIRE Surveys
Reconciling the results of the z ∼ 2 MOSDEF and KBSS-MOSFIRE Surveys
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协调 z ≤ 2 MOSDEF 和 KBSS-MOSFIRE 调查的结果
DOI：
10.1093/mnras/stac1115
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发表时间：
2022
影响因子：
4.8
通讯作者：
Pettini, Max
中科院分区：
文献类型：
--
作者：
Runco, Jordan N.;Reddy, Naveen A.;Shapley, Alice E.;Steidel, Charles C.;Sanders, Ryan L.;Strom, Allison L.;Coil, Alison L.;Kriek, Mariska;Mobasher, Bahram;Pettini, Max
MOSDEF和KBSS-MOSFIRE巡天的组合代表了凯克/MOSFIRE迄今为止最大的联合投资，有大约3000个星系在1.4赫兹至3.8赫兹，其中大约一半是赫兹至2赫兹。MOSDEF是光度和光谱红移的选择，具有静止光学星等限制，而KBSS-MOSFIRE主要是基于静止UV颜色和静止UV星等限制。使用一致的光谱能量分布（SED）模型以统一的方式分析两个调查，我们发现，与KBSS-MOSFIREz 2目标样本相比，MOSDEFz 2目标样本具有更高的中位数M * 和更红的restU− V颜色，以及更小的基于SED的SFR和sSFR中位数（SFR（SED）和sSFR（SED））。具体来说，MOSDEF的目标是更多的U −VandV−J≥1.25的红色星系，而KBSS-MOSFIRE包含更多的年轻星系，具有强烈的星星形成。尽管在目标样本中存在这些差异，但在以前的工作中检测和分析的具有多条发射线的调查子集更加相似。除了恒星星族年龄--即M*、SFR（SED）、sSFR（SED）、AV和UVJ颜色--之外，所有主星系的中值性质都在不确定性范围内。此外，当应用均匀发射线拟合和恒星巴尔末吸收校正技术时，在[Oiii]λ5008/H β与[Nii]λ6585/H α诊断图中，两个样本之间没有明显的偏移，与以前报道的差异相反。我们现在可以联合收割机的MOSDEF和KBSS-MOSFIRE的调查，形成最大的z 102样品与中等分辨率的静止-光学光谱和构建的基本标度关系的恒星形成星系在这个重要的时代。
The combination of the MOSDEF and KBSS-MOSFIRE surveys represents the largest joint investment of Keck/MOSFIRE time to date, with ∼3000 galaxies at 1.4 ≲z≲ 3.8, roughly half of which are atz∼ 2. MOSDEF is photometric- and spectroscopic-redshift selected with a rest-optical magnitude limit, while KBSS-MOSFIRE is primarily selected based on rest-UV colours and a rest-UV magnitude limit. Analysing both surveys in a uniform manner with consistent spectral-energy-distribution (SED) models, we find that the MOSDEFz∼ 2 targeted sample has higher medianM*and redder restU−Vcolour than the KBSS-MOSFIREz∼ 2 targeted sample, and smaller median SED-based SFR and sSFR (SFR(SED) and sSFR(SED)). Specifically, MOSDEF targeted a larger population of red galaxies withU−VandV−J≥1.25, while KBSS-MOSFIRE contains more young galaxies with intense star formation. Despite these differences in thez∼ 2 targeted samples, the subsets of the surveys with multiple emission lines detected and analysed in previous work are much more similar. All median host-galaxy properties with the exception of stellar population age – i.e.M*, SFR(SED), sSFR(SED),AV, andUVJcolours – agree within the uncertainties. Additionally, when uniform emission-line fitting and stellar Balmer absorption correction techniques are applied, there is no significant offset between both samples in the [Oiii]λ5008/H β versus [Nii]λ6585/H α diagnostic diagram, in contrast to previously reported discrepancies. We can now combine the MOSDEF and KBSS-MOSFIRE surveys to form the largestz∼ 2 sample with moderate-resolution rest-optical spectra and construct the fundamental scaling relations of star-forming galaxies during this important epoch.