The ALPINE-ALMA [CII] survey
The ALPINE-ALMA [CII] survey
复制标题
DOI：
10.1051/0004-6361/202038163
复制
发表时间：
2020-04
影响因子：
6.5
通讯作者：
Y. Fudamoto;P. Oesch;A. Faisst;M. Béthermin;M. Ginolfi;Y. Khusanova;F. Loiacono;O. Fèvre;P. Capak;D. Schaerer;J. Silverman;P. Cassata;L. Yan;R. Amorín;S. Bardelli;M. Boquien;A. Cimatti;M. Dessauges-Zavadsky;S. Fujimoto;C. Gruppioni;N. Hathi;E. Ibar;G. Jones;A. Koekemoer;G. Lagache;B. Lemaux;R. Maiolino;D. Narayanan;F. Pozzi;D. Riechers;G. Rodighiero;M. Talia;S. Toft;L. Vallini;D. Vergani;G. Zamorani;E. Zucca
中科院分区：
文献类型：
--
作者：
Y. Fudamoto;P. Oesch;A. Faisst;M. Béthermin;M. Ginolfi;Y. Khusanova;F. Loiacono;O. Fèvre;P. Capak;D. Schaerer;J. Silverman;P. Cassata;L. Yan;R. Amorín;S. Bardelli;M. Boquien;A. Cimatti;M. Dessauges-Zavadsky;S. Fujimoto;C. Gruppioni;N. Hathi;E. Ibar;G. Jones;A. Koekemoer;G. Lagache;B. Lemaux;R. Maiolino;D. Narayanan;F. Pozzi;D. Riechers;G. Rodighiero;M. Talia;S. Toft;L. Vallini;D. Vergani;G. Zamorani;E. Zucca
我们展示了光谱证实的主序带上红移~4.4-5.8的恒星形成星系的尘埃衰减特性。我们的分析基于通过阿塔卡马大型毫米波阵列 (ALMA) 早期调查 [CII] 大型计划 (ALPINE) 获得的 118 个星系在静止坐标系 158μm 处的远红外连续谱观测。我们研究紫外线 (UV) 光谱斜率 (β)、恒星质量 (M⋆) 和红外线过量 (IRX = LIR/LUV) 之间的联系。在连续体中分别检测到 23 个星系，其显着性 > 3.5σ。我们使用检测和非检测进行叠加分析，以研究 z ∼ 4.4 − 5.8 的平均灰尘衰减特性。单独的检测和叠加显示，IRX-β关系 atz ∼ 5 与比通常在较低红移（z 4）下发现的更陡峭的尘埃衰减曲线一致。同样，我们发现，与之前研究的 IRX-M⋆关系 atz ≲ 4 相比，我们的星系在固定质量下具有较低的 IRX 值，平均高达 1 dex，尽管有显着的散射。这意味着恒星形成的模糊部分比较低红移时更低。我们的结果表明，UV 选择的恒星形成星系 atz ≳ 4 的尘埃特性具有以下特征：(i) 比 atz ≲ 4 更陡的衰减曲线，以及 (ii) 作为红移函数的恒星形成的尘埃遮蔽部分迅速减少。然而，即使在这个 UV 选择的样本中，大质量星系 (logM⋆/M⊙ > 10) atz ∼ 5 − 6 也已经表现出了恒星遮蔽部分。约 45% 的形成，表明在再电离时期灰尘迅速积聚。
We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of ∼4.4 − 5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158μm obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope (β), stellar mass (M⋆), and infrared excess (IRX =LIR/LUV). Twenty-three galaxies are individually detected in the continuum at > 3.5σsignificance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties atz ∼ 4.4 − 5.8. The individual detections and stacks show that the IRX–βrelation atz ∼ 5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z 4. Similarly, we find that our galaxies have lower IRX values, up to 1 dex on average, at a fixed mass compared to previously studied IRX–M⋆relations atz ≲ 4, albeit with significant scatter. This implies a lower obscured fraction of star formation than at lower redshifts. Our results suggest that dust properties of UV-selected star forming galaxies atz ≳ 4 are characterised by (i) a steeper attenuation curve than atz ≲ 4, and (ii) a rapidly decreasing dust obscured fraction of star formation as a function of redshift. Nevertheless, even among this UV-selected sample, massive galaxies (logM⋆/M⊙ > 10) atz ∼ 5 − 6 already exhibit an obscured fraction of star formation of ∼45%, indicating a rapid build-up of dust during the epoch of reionization.