PHIBSS: MOLECULAR GAS, EXTINCTION, STAR FORMATION, AND KINEMATICS IN THE z = 1.5 STAR-FORMING GALAXY EGS13011166
PHIBSS: MOLECULAR GAS, EXTINCTION, STAR FORMATION, AND KINEMATICS IN THE z = 1.5 STAR-FORMING GALAXY EGS13011166
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DOI：
10.1088/0004-637x/773/1/68
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发表时间：
2013-04
期刊：
影响因子：
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通讯作者：
R. Genzel;L. Tacconi;J. Kurk;S. Wuyts;F. Combes;J. Freundlich;A. Bolatto;M. Cooper;R. Neri
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文献类型：
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作者：
R. Genzel;L. Tacconi;J. Kurk;S. Wuyts;F. Combes;J. Freundlich;A. Bolatto;M. Cooper;R. Neri
作为“Plateau de Bure high-z，blue-sequence survey”（PHIBSS：Tacconi et al.）的一部分，我们报道了z = 1.53的大质量主序星EGS 13011166中的CO 3-2线（使用IRAM Plateau de Bure毫米干涉仪）和Hα线（使用LUCI在大双筒望远镜上）的匹配分辨率成像光谱。我们结合联合收割机这些数据与哈勃太空望远镜的V-I-J-H波段地图，推导出空间分辨的恒星表面密度，星星形成率，分子气体表面密度，光学消光，气体运动学的分布。电离和分子气体的空间分布和运动学是非常相似的，以及模拟的湍流，全球Toomre不稳定，旋转盘。恒星表面密度分布比星团静止坐标系的紫外光/可见光分布更平滑，在动力中心附近的一个模糊的恒星形成大质量凸起处达到峰值。分子气体的表面密度和有效的光学屏幕消光跟踪对方，并很好地模拟了“混合”消光模型。空间分辨分子气体与星星形成速率关系的推断斜率N = dlog β星星形式/dlog β mol气体，强烈依赖于所采用的消光模型，并且可以在0.8到1.7之间变化。对于优选的混合尘气模型，我们发现N = 1.14 ± 0.1。
We report matched resolution imaging spectroscopy of the CO 3–2 line (with the IRAM Plateau de Bure millimeter interferometer) and of the Hα line (with LUCI at the Large Binocular Telescope) in the massive z = 1.53 main-sequence galaxy EGS 13011166, as part of the “Plateau de Bure high-z, blue-sequence survey” (PHIBSS: Tacconi et al.). We combine these data with Hubble Space Telescope V–I–J–H-band maps to derive spatially resolved distributions of stellar surface density, star formation rate, molecular gas surface density, optical extinction, and gas kinematics. The spatial distribution and kinematics of the ionized and molecular gas are remarkably similar and are well modeled by a turbulent, globally Toomre unstable, rotating disk. The stellar surface density distribution is smoother than the clumpy rest-frame UV/optical light distribution and peaks in an obscured, star-forming massive bulge near the dynamical center. The molecular gas surface density and the effective optical screen extinction track each other and are well modeled by a “mixed” extinction model. The inferred slope of the spatially resolved molecular gas to star formation rate relation, N = dlogΣstar form/dlogΣmol gas, depends strongly on the adopted extinction model, and can vary from 0.8 to 1.7. For the preferred mixed dust–gas model, we find N = 1.14 ± 0.1.