标题： BOOMERanG 2003飞行任务的仪器、方法、亮度和偏振图 显示英文标题

标题： Instrument, Method, Brightness and Polarization Maps from the 2003 flight of BOOMERanG

摘要： 我们介绍了BOOMERanG-03实验以及2003年为期14天的气球飞行期间获得的微波天空斯托克斯参数I、Q、U的地图。调查了南天的三个区域：一个深度调查（约90平方度）和一个浅度调查（约750平方度）位于高银纬（两者都以RA ~ 5.5小时，dec ~ -45度为中心），以及一个约300平方度的银河平面调查，位于RA ~ 9.1小时，dec ~ -47度。 所有三次调查都在三个宽频带中心频率145 GHz、245 GHz和345 GHz下进行，角分辨率为~10'。 145 GHz的斯托克斯I图主要由宇宙微波背景（CMB）温度各向异性主导，这些各向异性被高信噪比映射。 测量到的各向异性模式与BOOMERanG-98和WMAP在同一区域测得的模式一致。 当斯托克斯Q和U的145 GHz图进行功率谱分析时，提供了CMB偏振的一个稳健统计检测。 这种偏振的幅度与在$\Lambda$冷暗物质（CDM）宇宙学情景中的CMB一致。 在145 GHz的CMB调查中，发现天体物理前景的强度和偏振相对于宇宙学信号可以忽略不计。 在245 GHz和345 GHz处，我们检测到与IRAS/DIRBE 3000 GHz地图相关的星际尘埃（ISD）发射，并给出了任何非CMB成分的上限。 我们还展示了银河平面调查部分的强度图。 这些图与不同星际成分的监测器进行比较，表明该地区存在多种发射机制。 显示英文摘要

摘要： We present the BOOMERanG-03 experiment and maps of the Stokes parameters I, Q, U of the microwave sky obtained during a 14 day balloon flight in 2003. Three regions of the southern sky were surveyed: a deep survey (~ 90 square degrees) and a shallow survey (~ 750 square degrees) at high Galactic latitudes (both centered at RA ~ 5.5 h, dec ~ -45 deg) and a survey of ~ 300 square degrees across the Galactic plane at RA ~ 9.1 h, dec ~ -47 deg. All three surveys were carried out in three wide frequency bands centered at 145, 245 and 345 GHz, with an angular resolution of ~ 10'. The 145 GHz maps of Stokes I are dominated by Cosmic Microwave Background (CMB) temperature anisotropy, which is mapped with high signal to noise ratio. The measured anisotropy pattern is consistent with the pattern measured in the same region by BOOMERanG-98 and by WMAP. The 145 GHz maps of Stokes Q and U provide a robust statistical detection of polarization of the CMB when subjected to a power spectrum analysis. This amplitude of the polarization is consistent with that of the CMB in the $\Lambda$CDM cosmological scenario. At 145 GHz, in the CMB surveys, the intensity and polarization of the astrophysical foregrounds are found to be negligible with respect to the cosmological signal. At 245 and 345 GHz we detect ISD emission correlated to the 3000 GHz IRAS/DIRBE maps, and give upper limits for any other non-CMB component. We also present intensity maps of the surveyed section of the Galactic plane. These are compared to monitors of different interstellar components, showing that a variety of emission mechanisms is present in that region.