The MUSE Hubble Ultra Deep Field Survey: IV. Global properties of C III] emitters
The MUSE Hubble Ultra Deep Field Survey: IV. Global properties of C III] emitters
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MUSE 哈勃超深场巡天：IV。
DOI：
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发表时间：
2017
期刊：
影响因子：
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通讯作者：
L. Wisotzki
中科院分区：
文献类型：
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作者：
M. Maseda;J. Brinchmann;M. Franx;R. Bacon;R. Bouwens;K. Schmidt;L. Boogaard;T. Contini;A. Feltre;H. Inami;W. Kollatschny;R. Marino;J. Richard;A. Verhamme;L. Wisotzki
C III] 1907，1909发射双峰在z > 6的星系红移确认中被认为是莱曼α的替代，因为它在这些红移处不会被大部分中性的星系际介质衰减，并且被认为在这些早期宇宙时代存在的年轻的、活跃的恒星形成星系中很强。我们使用哈勃深场南（HDFS）和超深场（UDF）中覆盖2平方角分的30小时深度VLT/MUSE积分场光谱，提供了z~1.5以外的17个C III]发射星系的统计样本，实现了HDFS中~ 2 e-17 erg/s/cm^2和UDF中~ 7 e-18 erg/s/cm^2的C III]灵敏度。静止框架等效宽度范围为2至19埃。这17个星系占1.5 < z < 4之间星系样本总数的3%。它们还显示出较高的星星形成率，较低的尘埃衰减，和年轻的质量加权年龄比一般人口的星系在相同的红移。结合来自UDF中的HST/WFC 3的深无缝棱镜光谱，我们可以将静止帧紫外C III]发射与静止帧光学发射线（即[O III] 5007）联系起来，发现两者之间存在强相关性。直到我们观测到的通量极限（UDF中的棱纹数据约为1 e-18 erg/s/cm ^2），所有静止坐标系[O III] 4959，5007等效宽度超过250埃的天体，即所谓的极端发射线星系，在我们的MUSE数据中都检测到了C III]。更详细地研究在这些中等红移的C III]-发射人口将是至关重要的，以了解在宇宙早期的星系中的物理条件，并确定C III]作为红移示踪剂的效用。
The C III] 1907,1909 emission doublet has been proposed as an alternative to Lyman-alpha in redshift confirmations of galaxies at z > 6 since it is not attenuated by the largely neutral intergalactic medium at these redshifts and is believed to be strong in the young, vigorously star-forming galaxies present at these early cosmic times. We present a statistical sample of 17 C III]-emitting galaxies beyond z~1.5 using 30 hour deep VLT/MUSE integral field spectroscopy covering 2 square arcminutes in the Hubble Deep Field South (HDFS) and Ultra Deep Field (UDF), achieving C III] sensitivities of ~2e-17 erg/s/cm^2 in the HDFS and ~7e-18 erg/s/cm^2 in the UDF. The rest-frame equivalent widths range from 2 to 19 Angstroms. These 17 galaxies represent ~3% of the total sample of galaxies found between 1.5 < z < 4. They also show elevated star formation rates, lower dust attenuation, and younger mass-weighted ages than the general population of galaxies at the same redshifts. Combined with deep slitless grism spectroscopy from the HST/WFC3 in the UDF, we can tie the rest-frame ultraviolet C III] emission to rest-frame optical emission lines, namely [O III] 5007, finding a strong correlation between the two. Down to the flux limits that we observe (~1e-18 erg/s/cm^2 with the grism data in the UDF), all objects with a rest-frame [O III] 4959,5007 equivalent width in excess of 250 Angstroms, the so-called Extreme Emission Line Galaxies, have detections of C III] in our MUSE data. More detailed studies of the C III]-emitting population at these intermediate redshifts will be crucial to understand the physical conditions in galaxies at early cosmic times and to determine the utility of C III] as a redshift tracer.
影响因子：
7.9
作者：
Laporte, N.;Ellis, R. S.;Streblyanska, A.
通讯作者：
Streblyanska, A.