The ALPINE-ALMA [CII] survey. No or weak evolution in the [CII]-SFR relation over the last 13 Gyr
The ALPINE-ALMA [CII] survey. No or weak evolution in the [CII]-SFR relation over the last 13 Gyr
复制标题
ALPINE-ALMA [CII] 调查。
DOI：
--
复制
发表时间：
2020
期刊：
影响因子：
--
通讯作者：
E. Zucca
中科院分区：
文献类型：
--
作者：
D. Schaerer;M. Ginolfi;M. Béthermin;Y. Fudamoto;P. Oesch;O. Fèvre;A. Faisst;P. Capak;P. Cassata;J. Silverman;Lin Yan;G. Jones;R. Amorín;S. Bardelli;M. Boquien;A. Cimatti;M. Dessauges;M. Giavalisco;N. Hathi;S. Fujimoto;E. Ibar;A. Koekemoer;G. Lagache;B. Lemaux;F. Loiacono;R. Maiolino;D. Narayanan;L. Morselli;H. Méndez;F. Pozzi;D. Riechers;M. Talia;S. Toft;L. Vallini;D. Vergani;G. Zamorani;E. Zucca
[C ii] 158µm谱线是最强的红外发射谱线之一，它被证明可以追踪到附近宇宙中星系的恒星形成速率（SFR），最高可达z ~ 2。在更高的红移和早期宇宙中是否也存在这种情况仍然存在争议。ALPINE的调查目标是118个正在形成恒星的星系。4 < z < 5。9，为用第一个统计数据集检验这个问题提供了一个新的机会。利用ALPINE数据和早期文献中的测量结果，我们研究了从z ~ 4−8整个红移范围内[C ii]亮度和SFR之间的关系。在[C ii]和尘埃连续体中都探测到高山星系，它们与局域的L ([CII]) -SFR关系一致。当使用UV SFR时，在ALMA连续统中未探测到的星系在[C ii]中被发现过亮。在考虑尘埃遮挡恒星形成后，通过两种不同的叠加方法和SED拟合得出的SFR(IR)≈SFR（UV）的平均值，ALPINE星系显示出与本地相当的L ([CII]) -SFR关系。当考虑到[C ii]未检测到时，在高z处斜率可能会稍微陡一些，尽管这仍然有些不确定。当以均匀的方式进行比较时，z bbb6 [C ii]测量值（检测和上限）与z ~ 4−6数据的行为没有很大不同。我们发现L ([CII]) / SFR对Ly α等效宽度有较弱的依赖性。最后，我们发现ALPINE源的比值L ([CII]) / L IR ~（1−3）× 10−3与较低红移的“正常”星系相当。我们的分析，包括迄今为止在z b> 4测量的最大样本（约150个星系），表明在宇宙时间的最后13 Gyr中，[C ii] -SFR关系没有或很少演变。高z星系的恒星形成，这可以通过新的ALMA和未来的JWST观测得到。
The [C ii ] 158 µ m line is one of the strongest IR emission lines, which has been shown to trace the star-formation rate (SFR) of galaxies in the nearby Universe and up to z ∼ 2. Whether this is also the case at higher redshift and in the early Universe remains debated. The ALPINE survey, which targeted 118 star-forming galaxies at 4 . 4 < z < 5 . 9, provides a new opportunity to examine this question with the first statistical dataset. Using the ALPINE data and earlier measurements from the literature we examine the relation between the [C ii ] luminosity and the SFR over the entire redshift range from z ∼ 4 − 8. ALPINE galaxies, which are both detected in [C ii ] and dust continuum, show a good agreement with the local L ([CII])–SFR relation. Galaxies undetected in the continuum with ALMA are found to be over-luminous in [C ii ], when the UV SFR is used. After accounting for dust-obscured star formation, by an amount SFR(IR) ≈ SFR(UV) on average, which results from two di ff erent stacking methods and SED fitting, the ALPINE galaxies show an L ([CII])–SFR relation comparable to the local one. When [C ii ] non-detections are taken into account, the slope may be marginally steeper at high- z , although this is still somewhat uncertain. When compared in a homogeneous manner, the z > 6 [C ii ] measurements (detections and upper limits) do not behave very di ff erently from the z ∼ 4 − 6 data. We find a weak dependence of L ([CII]) / SFR on the Ly α equivalent width. Finally, we find that the ratio L ([CII]) / L IR ∼ (1 − 3) × 10 − 3 for the ALPINE sources, comparable to that of “normal" galaxies at lower redshift. Our analysis, which includes the largest sample ( ∼ 150 galaxies) of [C ii ] measurements at z > 4 available so far, suggests no or little evolution of the [C ii ]–SFR relation over the last 13 Gyr of cosmic time. star formation in high- z galaxies, which can be obtained with new ALMA and future JWST observations.