首页> 外文OA文献 >The CARMA Paired Antenna Calibration System: Atmospheric Phase Correction for Millimeter Wave Interferometry and its Application to Mapping the Ultraluminous Galaxy Arp 193
【2h】

The CARMA Paired Antenna Calibration System: Atmospheric Phase Correction for Millimeter Wave Interferometry and its Application to Mapping the Ultraluminous Galaxy Arp 193

机译:CARMA配对天线校准系统:毫米波干涉法的大气相位校正及其在绘制超发光星系Arp 193中的应用

代理获取
本网站仅为用户提供外文OA文献查询和代理获取服务,本网站没有原文。下单后我们将采用程序或人工为您竭诚获取高质量的原文,但由于OA文献来源多样且变更频繁,仍可能出现获取不到、文献不完整或与标题不符等情况,如果获取不到我们将提供退款服务。请知悉。

摘要

Phase fluctuations introduced by the atmosphere are the main limiting factor in attaining diffraction limited performance in extended interferometric arrays at millimeter and submillimeter wavelengths. We report the results of C-PACS, the Combined Array for Research in Millimeter-Wave Astronomy Paired Antenna Calibration System. We present a systematic study of several hundred test observations taken during the 2009–2010 winter observing season where we utilize CARMA's eight 3.5 m antennas to monitor an atmospheric calibrator while simultaneously acquiring science observations with 6.1 and 10.4 m antennas on baselines ranging from a few hundred meters to ~2 km. We find that C-PACS is systematically successful at improving coherence on long baselines under a variety of atmospheric conditions. We find that the angular separation between the atmospheric calibrator and target source is the most important consideration, with consistently successful phase correction at CARMA requiring a suitable calibrator located ≾6° away from the science target. We show that cloud cover does not affect the success of C-PACS. We demonstrate C-PACS in typical use by applying it to the observations of the nearby very luminous infrared galaxy Arp 193 in ^(12)CO(2-1) at a linear resolution of ≈70 pc (0".12 × 0".18), 3 times better than previously published molecular maps of this galaxy. We resolve the molecular disk rotation kinematics and the molecular gas distribution and measure the gas surface densities and masses on 90 pc scales. We find that molecular gas constitutes ~30% of the dynamical mass in the inner 700 pc of this object with a surface density ~10^4 M_⊙ pc^(−2); we compare these properties to those of the starburst region of NGC 253.
机译:大气引入的相位波动是在毫米和亚毫米波长的扩展干涉阵列中获得衍射受限性能的主要限制因素。我们报告C-PACS的结果,这是毫米波天文学成对天线校准系统研究的组合阵列。我们对2009-2010年冬季观测季节进行的数百项测试观测结果进行了系统的研究,我们利用CARMA的8个3.5 m天线来监测大气校准器,同时以数百个范围为基准,用6.1和10.4 m天线获取科学观测值米至〜2公里。我们发现,C-PACS在改善各种大气条件下长基线的连贯性方面取得了系统性的成功。我们发现,大气校准器和目标源之间的角度间隔是最重要的考虑因素,在CARMA上要成功地进行相位校正,就需要一个合适的校准器,该校准器应距科学目标约6°。我们证明云量不会影响C-PACS的成功。我们通过将C-PACS应用于^(12)CO(2-1)中附近非常发光的红外星系Arp 193的观测,以线性分辨率≈70pc(0“ .12×0”,来证明其在典型用途中的用途.18),比先前发布的该星系的分子图好3倍。我们解析分子盘旋转运动学和分子气体分布,并以90 pc刻度测量气体表面密度和质量。我们发现分子气体占该物体内部700 pc中动量的〜30%,表面密度为〜10 ^ 4M_⊙pc ^(-2);我们将这些特性与NGC 253的星爆区域的特性进行了比较。

相似文献

  • 外文文献
  • 中文文献
  • 专利
代理获取

客服邮箱:kefu@zhangqiaokeyan.com

京公网安备:11010802029741号 ICP备案号:京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有
  • 客服微信

  • 服务号