The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra-猫眼课题宝

DOI：

10.3847/1538-3881/acacfc

发表时间：

2022-08

期刊：

The Astronomical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

D. Alexander;T. Davis;E. Chaussidon;V. A. Fawcett;A. González-Morales;Ting-Wen Lan;C. Yéche;S. Ahlen;J. Aguilar;E. Armengaud;S. Bailey;D. Brooks;Z. Cai;R. Canning;A. Carr;S. Chabanier;M. Cousinou;K. Dawson;A. Macorra;A. Dey;B. Dey;G. Dhungana;A. Edge;S. Eftekharzadeh;K. Fanning;J. Farr;A. Font-Ribera;J. García-Bellido;L. Garrison;E. Gaztañaga;S. Gontcho;C. Gordon;S. Gonzalez;J. Guy;H. Herrera-Alcantar;L. Jiang;S. Juneau;Naim Göksel Karaçaylı;R. Kehoe;T. Kisner;A. Kovács;M. Landriau;M. Levi;C. Magneville;P. Martini;A. Meisner;M. Mezcua;R. Miquel;P. M. Camacho;J. Moustakas;A. Muñoz‐Gutiérrez;A. Myers;S. Nadathur;L. Napolitano;J. Nie;N. Palanque-Delabrouille;Z. Pan;W. Percival;I. Pérez-Ràfols;C. Poppett;F. Prada;César Ramírez-Pérez;C. Ravoux;D. Rosario;M. Schubnell;G. Tarlé;M. Walther;B. Weiner;S. Youles;Zhi-min Zhou;H. Zou;S. Zou

暗能量光谱仪器（DESI）调查验证（SV）的一个关键组成部分是对光学光谱数据进行详细的目视检查（VI），以量化关键调查指标。本文介绍了利用深共加SV谱进行类星体巡天的VI观测结果。我们发现，大多数（约70%）的主要调查目标被光谱确认为类星体，约16%的星系，约60%的恒星和约8%的低质量光谱缺乏可靠的功能。一个不可忽略的部分的类星体被错误识别的标准光谱管道，但我们表明，大多数可以恢复使用后管道“加力”类星体识别方法。我们将这些“加力燃烧室”与我们的标准管道相结合，以创建一个修改后的管道，以增加整体类星体产量。在主要DESI调查的深度，两条管道都达到了良好的红移纯度（在3000 km s−1范围内测量到的可靠红移）为1.99%;然而，修改后的管道恢复了1.94%的目视检查类星体，而标准管道恢复了1.86%。我们证明了这两条管道分别实现了100 km s-1和170 km s-1的中值红移精度和准确度。我们构建了复合光谱来研究为什么一些类星体被标准管道遗漏，并发现它们更受宿主星系支配（即，遥远的类似物“塞弗特星系”）和/或更多的尘埃比标准管道类星体变红。我们还展示了示例光谱，以展示DESI类星体样本的整体多样性，并提供强透镜候选人，其中两个目标有助于一个单一的光谱。

A key component of the Dark Energy Spectroscopic Instrument (DESI) survey validation (SV) is a detailed visual inspection (VI) of the optical spectroscopic data to quantify key survey metrics. In this paper we present results from VI of the quasar survey using deep coadded SV spectra. We show that the majority (≈70%) of the main-survey targets are spectroscopically confirmed as quasars, with ≈16% galaxies, ≈6% stars, and ≈8% low-quality spectra lacking reliable features. A nonnegligible fraction of the quasars are misidentified by the standard spectroscopic pipeline, but we show that the majority can be recovered using post-pipeline “afterburner” quasar-identification approaches. We combine these “afterburners” with our standard pipeline to create a modified pipeline to increase the overall quasar yield. At the depth of the main DESI survey, both pipelines achieve a good-redshift purity (reliable redshifts measured within 3000 km s−1) of ≈99%; however, the modified pipeline recovers ≈94% of the visually inspected quasars, as compared to ≈86% from the standard pipeline. We demonstrate that both pipelines achieve a median redshift precision and accuracy of ≈100 km s−1 and ≈70 km s−1, respectively. We constructed composite spectra to investigate why some quasars are missed by the standard pipeline and find that they are more host-galaxy dominated (i.e., distant analogs of “Seyfert galaxies”) and/or more dust reddened than the standard-pipeline quasars. We also show example spectra to demonstrate the overall diversity of the DESI quasar sample and provide strong-lensing candidates where two targets contribute to a single spectrum.

The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra

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