Early Results from GLASS-JWST. VI. Extreme Rest-optical Equivalent Widths Detected in NIRISS Wide Field Slitless Spectroscopy
Early Results from GLASS-JWST. VI. Extreme Rest-optical Equivalent Widths Detected in NIRISS Wide Field Slitless Spectroscopy
复制标题
GLASS-JWST 的早期结果。
DOI：
10.3847/2041-8213/ac9f17
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发表时间：
2022
期刊：
影响因子：
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通讯作者：
C. Willott
中科院分区：
文献类型：
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作者：
K. Boyett;S. Mascia;L. Pentericci;N. Leethochawalit;M. Trenti;G. Brammer;G. Roberts;V. Strait;T. Treu;M. Bradač;K. Glazebrook;A. Acebrón;P. Bergamini;A. Calabró;M. Castellano;A. Fontana;C. Grillo;A. Henry;T. Jones;D. Marchesini;C. Mason;A. Mercurio;T. Morishita;T. Nanayakkara;P. Rosati;C. Scarlata;E. Vanzella;B. Vulcani;X. Wang;C. Willott
宽场无狭缝光谱学（WFSS）为探测恒星形成星系（SFG）中的强谱线辐射提供了一个强有力的工具，而无需预先选择目标。作为GLASS-JWST早期释放科学（ERS）计划的一部分，我们利用NIRISS（1-2.2 μm）的近红外波长能力来观察z <3.4的静止光学发射线，其深度和空间分辨率比以往任何时候都要高（Hα到z < 2.4; [O iii]+Hβ到z < 3.4）。在这封信中，我们将样本中76 1 < z 750 nm的样本的静止框架[O III]λ5007等效宽度（EW）分布限制< 3.4 SFGs in the A2744 Hubble Frontier Field and determine an abundance fraction of extreme emission line galaxies with EW >为12%。我们确定了测量的Hβ和[O III]λ5007 EW之间的强相关性，支持高[O III]λ5007 EW天体需要年轻恒星群中的大质量恒星来产生所需的高能光子来加倍吸收氧气。我们提取光谱的对象到2 mag昏暗的近红外比以前的WFSS研究与哈勃太空望远镜。因此，这项工作清楚地突出了JWST/NIRISS在拥挤的集群环境中提供高质量WFSS数据集的潜力。
Wide Field Slitless Spectroscopy (WFSS) provides a powerful tool for detecting strong line emission in star-forming galaxies (SFGs) without the need for target preselection. As part of the GLASS-JWST Early Release Science (ERS) program, we leverage the near-infrared wavelength capabilities of NIRISS (1–2.2 μm) to observe rest-optical emission lines out to z ∼ 3.4, to a depth and with a spatial resolution higher than ever before (Hα to z < 2.4; [O iii]+Hβ to z < 3.4). In this Letter we constrain the rest-frame [O III]λ5007 equivalent width (EW) distribution for a sample of 76 1 < z < 3.4 SFGs in the A2744 Hubble Frontier Field and determine an abundance fraction of extreme emission line galaxies with EW > 750Å in our sample to be 12%. We determine a strong correlation between the measured Hβ and [O III]λ5007 EWs, supporting that the high [O III]λ5007 EW objects require massive stars in young stellar populations to generate the high-energy photons needed to doubly ionize oxygen. We extracted spectra for objects up to 2 mag fainter in the near-infrared than previous WFSS studies with the Hubble Space Telescope. Thus, this work clearly highlights the potential of JWST/NIRISS to provide high-quality WFSS data sets in crowded cluster environments.
z~0.8 处最极端的线发射器
DOI：
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发表时间：
2022
期刊：
影响因子：
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作者：
Ono Yoshiaki;Itoh Ryohei;Shibuya Takatoshi;Ouchi Masami;Harikane Yuichi;Yamanaka Satoshi;Inoue Akio K.;他;Yuichi Harikane;Yuichi Harikane;Yuichi Harikane;Yuichi Harikane;Yuichi Harikane;播金優一;播金優一;播金優一;Yuichi Harikane;播金優一;播金優一;播金優一
通讯作者：
播金優一
DOI：
10.3847/1538-4365/ac5331
发表时间：
2022-01
期刊：
The Astrophysical Journal Supplement Series
影响因子：
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作者：
S. Flury;A. Jaskot;H. Ferguson;G. Worseck;Kirill Makan;J. Chisholm;A. Saldana-Lopez;D. Schaerer;Stephan McCandless;Bingjie Wang;N. Ford;T. Heckman;Z. Ji;M. Giavalisco;R. Amorín;H. Atek;J. Blaizot;S. Borthakur;C. Carr;M. Castellano;S. Cristiani;S. D. Barros;M. Dickinson;S. Finkelstein;B. Fleming;F. Fontanot;T. Garel;A. Grazian;M. Hayes;A. Henry;V. Mauerhofer;G. Micheva;M. Oey;G. Ostlin;C. Papovich;L. Pentericci;S. Ravindranath;J. Rosdahl;M. Rutkowski;P. Santini;C. Scarlata;H. Teplitz;T. Thuan;M. Trebitsch;E. Vanzella;A. Verhamme;Xinfeng Xu University of Massachusetts Amherst;Williams College;Space Telescope Science Institute;U. Potsdam;U. T. A. Austin;U. Geneva;J. University;Universidad de La Serena;Sorbonne Universit'e;U. Lyon;A. S. University;U. Minnesota;Oss. Astronomico di Roma;Osservatorio astronomico di Trieste;NOIRLab;Laboratory for Atmospheric;S. Physics;Osservatorio Astronomico di Padova;S. University;Leibniz Institute for Astrophysics Potsdam;U. Michigan;AM Texas;M. S. University;C. Tech;U. Virginia;K. Institute;Osservatoria Astronomico di Bologna
通讯作者：
S. Flury;A. Jaskot;H. Ferguson;G. Worseck;Kirill Makan;J. Chisholm;A. Saldana-Lopez;D. Schaerer;Stephan McCandless;Bingjie Wang;N. Ford;T. Heckman;Z. Ji;M. Giavalisco;R. Amorín;H. Atek;J. Blaizot;S. Borthakur;C. Carr;M. Castellano;S. Cristiani;S. D. Barros;M. Dickinson;S. Finkelstein;B. Fleming;F. Fontanot;T. Garel;A. Grazian;M. Hayes;A. Henry;V. Mauerhofer;G. Micheva;M. Oey;G. Ostlin;C. Papovich;L. Pentericci;S. Ravindranath;J. Rosdahl;M. Rutkowski;P. Santini;C. Scarlata;H. Teplitz;T. Thuan;M. Trebitsch;E. Vanzella;A. Verhamme;Xinfeng Xu University of Massachusetts Amherst;Williams College;Space Telescope Science Institute;U. Potsdam;U. T. A. Austin;U. Geneva;J. University;Universidad de La Serena;Sorbonne Universit'e;U. Lyon;A. S. University;U. Minnesota;Oss. Astronomico di Roma;Osservatorio astronomico di Trieste;NOIRLab;Laboratory for Atmospheric;S. Physics;Osservatorio Astronomico di Padova;S. University;Leibniz Institute for Astrophysics Potsdam;U. Michigan;AM Texas;M. S. University;C. Tech;U. Virginia;K. Institute;Osservatoria Astronomico di Bologna