在这个光谱学研究的婴儿大质量星团，我们发现，连续发射的电离气体竞争对手的恒星光度在光学波长。此外，我们发现星云线发射在许多常用的宽带HST滤波器，包括F814 W I波段，F555 W V波段和F435 W B波段是显着的。NGC 4449中的两个年轻的大质量星团（YMC）是在Reines等人（2008 a）在对银河系中的射电探测到的星团进行光度学研究时发现F814 W I波段过剩后进行光谱观测的目标。光谱是用3.5米APO望远镜上的双成像光谱仪获得的。我们补充这些数据与HST和SDSS测光。通过比较我们的数据Starburst 99和GALEV模型，我们发现，在我们的观测中，星云的连续辐射与恒星光的竞争，并在U-和I-波段的相对贡献是最大的，那里的Balmer和Paschen跳跃的位置。光谱还表现出强的线发射，包括HST F814 W I带中的[SIII] 9069，9532线。我们发现，星云连续谱和线发射的结合可以解释Reines等人（2008 a）发现的F814 W I波段过剩。在努力提供一个基准，估计电离气体排放的影响测光观测的YMC，我们计算的恒星连续，星云连续，和发射线的总通量的3百万岁的集群通过各种HST过滤器/仪器组合，包括过滤器在WFC 3的相对贡献。在比较YMC的观测与演化合成模型时，我们敦促谨慎，因为星云发射可能对年轻（<500万年）星团的大小和颜色产生很大影响，显著影响推断的性质，如年龄，质量和亮度。（节录）
英文摘要：
In this spectroscopic study of infant massive star clusters, we find that continuum emission from ionized gas rivals the stellar luminosity at optical wavelengths. In addition, we find that nebular line emission is significant in many commonly used broad-band HST filters including the F814W I-band, the F555W V-band and the F435W B-band. Two young massive clusters (YMCs) in NGC 4449 were targeted for spectroscopic observations after Reines et al. (2008a) discovered an F814W I-band excess in their photometric study of radio-detected clusters in the galaxy. The spectra were obtained with the Dual Imaging Spectrograph on the 3.5 m APO telescope. We supplement these data with HST and SDSS photometry. By comparing our data to the Starburst99 and GALEV models, we find that nebular continuum emission competes with the stellar light in our observations and that the relative contribution is largest in the U- and I-bands, where the Balmer and Paschen jumps are located. The spectra also exhibit strong line emission including the [SIII] 9069,9532 lines in the HST F814W I-band. We find that the combination of nebular continuum and line emission can account for the F814W I-band excess found by Reines et al. (2008a). In an effort to provide a benchmark for estimating the impact of ionized gas emission on photometric observations of YMCs, we compute the relative contributions of the stellar continuum, nebular continuum, and emission lines to the total flux of a 3 Myr-old cluster through various HST filter/instrument combinations, including filters in the WFC3. We urge caution when comparing observations of YMCs to evolutionary synthesis models since nebular emission can have a large impact on magnitudes and colors of young (< 5 Myr) clusters, significantly affecting inferred properties such as ages, masses and extinctions. (Abridged)
Nebular continuum in high-redshift galaxies with JWST
Instituto de Astrofísica e Ciências do Espaço, Universidade de Lisboa - OAL（空间科学与天体物理研究所，里斯本大学）；Departamento de Física, Faculdade de Ciências da Universidade de Lisboa（里斯本大学理学院物理系）；Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto – CAUP（波尔图大学空间科学与天体物理研究所）
A hot, nebular-dominated galaxy interacting with a pristine PopIII system uncovered by JWST
Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；DTU Space, Technical University of Denmark（丹麦技术大学空间科学中心）
The AURORA Survey: Multiple Balmer and Paschen Emission Lines for Individual Star-forming Galaxies at z=1.5-4.4. II. Implications for Nebular Dust Corrections, Nebular SFRs, and Differential Reddening
University of California, Riverside（加州大学河滨分校）；University of California, Los Angeles（加州大学洛杉矶分校）；University of California, Davis（加州大学戴维斯分校）；University of Arizona（亚利桑那大学）；Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；California Institute of Technology（加州理工学院）；University College London（伦敦大学学院）
Possible photometric signatures of nebular-dominated emission in $1.5 < z < 8.5$ JADES galaxies
University of Oxford（牛津大学）；University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Jodrell Bank Centre for Astrophysics, University of Manchester（曼彻斯特大学乔德雷尔银行天体物理学中心）；Scuola Normale Superiore（比萨高等师范学院）
A Galaxy with an Extremely Blue UV Slope $β=-3$ at $z=9.25$ Identified by JWST Spectroscopy: Evidence for a Weak Nebular Continuum and Efficient Ionizing Photon Escape?
21 Balmer Jump Street: The Nebular Continuum at High Redshift and Implications for the Bright Galaxy Problem, UV Continuum Slopes, and Early Stellar Populations
Paschen Jumps in Little Red Dots: Evidence for Nebular Continua
Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Astrophysics, Department of Physics, University of Oxford（牛津大学物理系天体物理学）；School of Mathematics and Physics, Astrophysics Research Centre, Queen’s University Belfast（贝尔法斯特女王大学数学与物理学院天体物理学研究中心）
Cloudy-Maraston: Integrating nebular continuum and line emission with the Maraston stellar population synthesis models
Institute of Cosmology & Gravitation, University of Portsmouth（宇宙学与引力研究所，朴茨茅斯大学）；Astronomy Centre, University of Sussex（天文学中心，萨塞克斯大学）；Department of Astronomy, University of Massachusetts, Amherst（天文学系，马萨诸塞大学阿默斯特分校）；Department of Physics, University of Oxford（物理系，牛津大学）
JWST View of the Supernebula in NGC 5253. II. Nebular Lines
Tel Aviv University（特拉维夫大学）；UCLA Department of Physics and Astronomy（加州大学洛杉矶分校物理与天文学系）；Chalmers Institute of Technology（查尔姆斯理工大学）；Academia Sinica Astronomy and Astrophysics（中央研究院天文及天文物理研究所）；New Mexico Institute of Mining and Technology（新墨西哥矿业理工学院）；Instituto Nacional de Astrofísica Óptica y Electrónica（国家天体物理学、光学和电子学研究所）
Stellar Absorption Line Analysis of Local Star-Forming Galaxies: The Relation Between Stellar Mass, Metallicity, Dust Attenuation and Star Formation Rate
The Sloan Digital Sky Survey Reverberation Mapping Project: Investigation of Continuum Lag Dependence on Broad-Line Contamination and Quasar Properties
Searching for Extremely Blue UV Continuum Slopes at $z=7-11$ in JWST/NIRCam Imaging: Implications for Stellar Metallicity and Ionizing Photon Escape in Early Galaxies
The JWST/AURORA Survey: Multiple Balmer and Paschen Emission Lines for Individual Star-forming Galaxies at z=1.5-4.4. I. A Diversity of Nebular Attenuation Curves and Evidence for Non-Unity Dust Covering Fractions
University of California, Riverside（加州大学河滨分校）；University of California, Los Angeles（加州大学洛杉矶分校）；University of Kentucky（肯塔基大学）；University of Arizona（亚利桑那大学）；University College London（伦敦大学学院）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；University of Edinburgh（爱丁堡大学）；Max-Planck-Institut für extraterrestrische Physik (MPE)（马克斯·普朗克地外物理研究所）
ALMA view on the nature of the compact VLA continuum sources in the massive young stellar object G25.65+1.05
P.N. Lebedev Physical Institute of RAS（俄罗斯科学院列别杰夫物理研究所）；Kotel'nikov Institute of Radio Engineering and Electronics of RAS（俄罗斯科学院科捷利尼科夫无线电电子学研究所）；Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台）；Ural Federal University（乌拉尔联邦大学）；Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理学研究所）
Balmer Decrements and Nebular-Stellar Reddening in JADES Galaxies at $2.7<z<7$
University of California, Los Angeles（加州大学洛杉矶分校）；University of Kentucky（肯塔基大学）；University of California, Riverside（加州大学河滨分校）；University of Arizona（亚利桑那大学）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）
Physical Properties of Spectroscopically-Confirmed Galaxies at $z\ge6$. III. Stellar Populations from SED Modeling with Secure Ly$α$ Emission and Redshifts
Hitting the slopes: A spectroscopic view of UV continuum slopes of galaxies reveals a reddening at z > 9.5
University of Oxford（牛津大学）；University College London（伦敦大学学院）；University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；University of Cambridge（剑桥大学）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）；Centro de Astrobiología (CAB), CSIC–INTA（西班牙国家航空航天技术研究所与西班牙国家科学研究委员会联合天体生物学中心）；European Space Agency（欧洲航天局）
