THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS). I. A CLOUD-SCALE/MULTI-WAVELENGTH VIEW OF THE INTERSTELLAR MEDIUM IN A GRAND-DESIGN SPIRAL GALAXY
THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS). I. A CLOUD-SCALE/MULTI-WAVELENGTH VIEW OF THE INTERSTELLAR MEDIUM IN A GRAND-DESIGN SPIRAL GALAXY
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DOI：
10.1088/0004-637x/779/1/42
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发表时间：
2013-04
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通讯作者：
E. Schinnerer;S. Meidt;J. Pety;A. Hughes;D. Colombo;S. García-Burillo;K. Schuster;G. Dumas;C. Dobbs;A. Leroy;C. Kramer;T. Thompson;M. Regan
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作者：
E. Schinnerer;S. Meidt;J. Pety;A. Hughes;D. Colombo;S. García-Burillo;K. Schuster;G. Dumas;C. Dobbs;A. Leroy;C. Kramer;T. Thompson;M. Regan
Plateau de Bure 干涉仪弧秒漩涡巡天利用两台 IRAM 望远镜绘制了 M51 中心 ∼9 kpc 中 12CO(1–0) 线发射中的分子气体，云尺度分辨率为 ∼40 pc。我们利用该数据集来定量表征分子气体（或二氧化碳排放）与星际介质、恒星形成和不同年龄的恒星种群的其他示踪剂的关系。使用二维图、极坐标互相关技术和逐像素图，我们发现：（1）（如预期的那样）分子气体的分布可以与重力势的不同组成部分联系起来； (2) CO线发射和射电连续谱之间存在物理联系的证据，这种联系似乎不是由大质量恒星引起的，而是取决于气体密度； (3)多环芳烃(PAH)与气体分子排放量之间存在密切的空间关系，但PAH排放量对气体分子质量没有预测能力； (4) I-H 颜色图是 CO 排放分布（以及较小程度的亮度）的出色预测器； (5) 由于分子气体和恒星形成区域之间复杂的空间关系（从空间到空间偏移到不存在），大质量（紫外线强）年轻恒星形成区域对中心~9 kpc 中大部分分子气体的影响并不显着。最后一点特别强调了银河环境以及潜在的引力势对于分子气体分布和恒星形成的重要性。
The Plateau de Bure Interferometer Arcsecond Whirlpool Survey has mapped the molecular gas in the central ∼9 kpc of M51 in its 12CO(1–0) line emission at a cloud-scale resolution of ∼40 pc using both IRAM telescopes. We utilize this data set to quantitatively characterize the relation of molecular gas (or CO emission) to other tracers of the interstellar medium, star formation, and stellar populations of varying ages. Using two-dimensional maps, a polar cross-correlation technique and pixel-by-pixel diagrams, we find: (1) that (as expected) the distribution of the molecular gas can be linked to different components of the gravitational potential; (2) evidence for a physical link between CO line emission and radio continuum that seems not to be caused by massive stars, but rather depends on the gas density; (3) a close spatial relation between polycyclic aromatic hydrocarbon (PAH) and molecular gas emission, but no predictive power of PAH emission for the molecular gas mass; (4) that the I − H color map is an excellent predictor of the distribution (and to a lesser degree, the brightness) of CO emission; and (5) that the impact of massive (UV-intense) young star-forming regions on the bulk of the molecular gas in central ∼9 kpc cannot be significant due to a complex spatial relation between molecular gas and star-forming regions that ranges from cospatial to spatially offset to absent. The last point, in particular, highlights the importance of galactic environment—and thus the underlying gravitational potential—for the distribution of molecular gas and star formation.