arXiv 2202.066422022-02-14astro-ph.GA

MUSE-Wide和MUSE-Deep中Lyman $α$发射体的等效宽度

Equivalent widths of Lyman $α$ emitters in MUSE-Wide and MUSE-Deep

J. Kerutt, L. Wisotzki, A. Verhamme, K. B. Schmidt, F. Leclercq, E. C. Herenz, T. Urrutia, T. Garel, T. Hashimoto, M. Maseda, J. Matthee, H. Kusakabe, J. Schaye… 展开作者

J. Kerutt, L. Wisotzki, A. Verhamme, K. B. Schmidt, F. Leclercq, E. C. Herenz, T. Urrutia, T. Garel, T. Hashimoto, M. Maseda, J. Matthee, H. Kusakabe, J. Schaye, J. Richard, B. Guiderdoni, V. Mauerhofer, T. Nanayakkara, E. Vitte

备注：: 28 pages, 21 + 1 figures, 7 + 1 tables, accepted for publication in A&A
发表信息：: A&A 659, A183 (2022)
DOI：: 10.1051/0004-6361/202141900

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摘要：

本研究的目的是更好地了解莱曼$α$休息帧等效宽度（EW $_0$）和光谱特性以及紫外线（UV）连续形态之间的连接，通过获得可靠的EW $_0$直方图的星系的统计样本，并通过评估具有大的等效宽度的对象的分数。我们使用MUSE的积分场光谱与哈勃太空望远镜（HST）的宽带数据相结合来测量EW $_0$。我们分析了$1920$ Lyman $α$发射体（LAEs）的发射线，这些发射体在全博物馆范围（1小时曝光时间）和博物馆深度（10小时曝光时间）调查中检测到，并在存档的HST数据中发现了紫外连续谱对应物。我们使用Galfit软件拟合UV连续光度图像以获得关于剩余UV发射的形态信息，并拟合从MUSE获得的光谱以确定莱曼$α$线的双峰分数、不对称性、半峰全宽和通量。两次调查显示了不同的Lyman $α$ EW $_0$直方图。在MUSE-Wide中，对象的$20\%$具有EW $_0 > 240$，而这一部分仅是MUSE-Deep中的$11\%$和全样本的$\approx 16\%$。这包括没有HST连续对应物的物体（我们样本的三分之一），我们给出了EW $_0$的下限。具有最高安全测量的EW $_0$的对象具有EW $_0=589 \pm 193$值（最高下限为EW $_0=4464$值）。我们研究了EW $_0$和Lyman $α$光谱或UV连续形态学性质之间的联系。在研究EW $_0$分布时，必须考虑勘测深度。我们发现，在一般情况下，高EW $_0$对象可以有一个广泛的光谱和紫外线形态学特性，这可能反映了高EW $_0$值的根本原因是同样不同的。（节略）

英文摘要：

The aim of this study is to better understand the connection between the Lyman $α$ rest-frame equivalent width (EW$_0$) and spectral properties as well as ultraviolet (UV) continuum morphology by obtaining reliable EW$_0$ histograms for a statistical sample of galaxies and by assessing the fraction of objects with large equivalent widths. We used integral field spectroscopy from MUSE combined with broad-band data from the Hubble Space Telescope (HST) to measure EW$_0$. We analysed the emission lines of $1920$ Lyman $α$ emitters (LAEs) detected in the full MUSE-Wide (one hour exposure time) and MUSE-Deep (ten hour exposure time) surveys and found UV continuum counterparts in archival HST data. We fitted the UV continuum photometric images using the Galfit software to gain morphological information on the rest-UV emission and fitted the spectra obtained from MUSE to determine the double peak fraction, asymmetry, full-width at half maximum, and flux of the Lyman $α$ line. The two surveys show different histograms of Lyman $α$ EW$_0$. In MUSE-Wide, $20\%$ of objects have EW$_0 > 240$ Å, while this fraction is only $11\%$ in MUSE-Deep and $\approx 16\%$ for the full sample. This includes objects without HST continuum counterparts (one-third of our sample), for which we give lower limits for EW$_0$. The object with the highest securely measured EW$_0$ has EW$_0=589 \pm 193$ Å (the highest lower limit being EW$_0=4464$ Å). We investigate the connection between EW$_0$ and Lyman $α$ spectral or UV continuum morphological properties. The survey depth has to be taken into account when studying EW$_0$ distributions. We find that in general, high EW$_0$ objects can have a wide range of spectral and UV morphological properties, which might reflect that the underlying causes for high EW$_0$ values are equally varied. (abridged)

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