The Galactic Plane Infrared Polarization Survey (GPIPS): Data Release 4
The Galactic Plane Infrared Polarization Survey (GPIPS): Data Release 4
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DOI：
10.3847/1538-4365/ab9f30
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发表时间：
2012-06
期刊：
影响因子：
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通讯作者：
D. Clemens;L. Cashman;C. Cerny;A. M. El-Batal;K. Jameson;R. Marchwinski;J. Montgomery;M. Pavel;A. Pinnick;B. Taylor
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文献类型：
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作者：
D. Clemens;L. Cashman;C. Cerny;A. M. El-Batal;K. Jameson;R. Marchwinski;J. Montgomery;M. Pavel;A. Pinnick;B. Taylor
银河平面红外偏振巡天（GPIPS）试图利用近红外恒星偏振测量来描述充满尘埃的银河圆盘中的磁场。所有GPPS观测都是使用1.83米帕金斯望远镜和Mimir仪器完成的。GPPS观测测量了北方银道面76 ° 2，从银道面18°-56°，纬度-1 °到+1°，在H波段（1.6 μm）。被调查的恒星跨度7 - 16等，导致近1000万颗恒星测量线性偏振。在这些恒星中，mH < 12.5等，偏振百分比不确定度低于2%的恒星被认为是高质量的，数量超过100万。GPIPS数据揭示了AV值为12.5等的许多星际云的天平面磁场方向。mH < 12.5等的恒星的平均天空间隔约为30″，或每个普朗克偏振分辨率元件约为60。与盖亚DR 2的匹配显示，最明亮的GPIPS恒星是红巨星，距离在0.6-7.5 kpc范围内。偏振方向大多平行于银河系盘，有些区域显示出显着的方向偏离。方向的变化随银河经度的变化比随纬度的变化更强烈。在10′角尺度下，显示最大偏振分数和最西偏振位置角分布的方向被限制在大约10个与恒星形成云不相关的大的相干结构中。GPIPS的偏振和光度数据产品（数据发布4目录和图像）公开提供超过1300万颗恒星。
The Galactic Plane Infrared Polarization Survey (GPIPS) seeks to characterize the magnetic field in the dusty Galactic disk using near-infrared stellar polarimetry. All GPIPS observations were completed using the 1.83 m Perkins telescope and Mimir instrument. GPIPS observations surveyed 76 deg2 of the northern Galactic plane, from Galactic longitudes 18°–56° and latitudes −1° to +1°, in the H band (1.6 μm). Surveyed stars span 7th–16th mag, resulting in nearly 10 million stars with measured linear polarizations. Of these stars, ones with mH < 12.5 mag and polarization percentage uncertainties under 2% were judged to be high quality and number over one million. GPIPS data reveal plane-of-sky magnetic field orientations for numerous interstellar clouds for AV values to ∼30 mag. The average sky separation of stars with mH < 12.5 mag is about 30″, or about 60 per Planck polarization resolution element. Matching to Gaia DR2 showed the brightest GPIPS stars are red giants with distances in the 0.6–7.5 kpc range. Polarization orientations are mostly parallel to the Galactic disk, with some zones showing significant orientation departures. Changes in orientations are stronger as a function of Galactic longitude than of latitude. Considered at 10′ angular scales, directions that show the greatest polarization fractions and narrowest polarization position angle distributions are confined to about 10 large, coherent structures that are not correlated with star-forming clouds. The GPIPS polarimetric and photometric data products (Data Release 4 catalogs and images) are publicly available for over 13 million stars.