THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE 600 < ℓ < 8000 COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 GHz
THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE 600 < ℓ < 8000 COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 GHz
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阿塔卡马宇宙学望远镜：148 GHz 600 < ≤ < 8000 宇宙微波背景功率谱的测量
DOI：
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发表时间：
2010
期刊：
影响因子：
--
通讯作者：
the Act Collaboration
中科院分区：
文献类型：
--
作者：
J. Fowler;V. Acquaviva;P. Ade;P. Aguirre;M. Amiri;J. Appel;L. Barrientos;E. Battistelli;J. Bond;B. Brown;B. Burger;J. Chervenak;S. Das;M. Devlin;S. Dicker;W. Doriese;J. Dunkley;R. Dunner;T. Essinger;R. Fisher;A. Hajian;M. Halpern;M. Hasselfield;C. Hern'andez;G. Hilton;M. Hilton;A. Hincks;R. Hložek;K. Huffenberger;D. Hughes;J. Hughes;L. Infante;K. Irwin;R. Jimenez;J. Juin;M. Kaul;J. Klein;A. Kosowsky;J. Lau;M. Limon;Y.;R. Lupton;T. Marriage;D. Marsden;K. Martocci;P. Mauskopf;F. Menanteau;K. Moodley;H. Moseley;C. Netterfield;M. Niemack;M. Nolta;L. Page;L. Parker;B. Partridge;H. Quintana;B. Reid;N. Sehgal;J. Sievers;D. Spergel;S. Staggs;D. Swetz;E. Switzer;R. Thornton;H. Trac;C. Tucker;L. Verde;R. Warne;G. Wilson;Edward J. Wollack;Y. Zhao;the Act Collaboration
本文给出了在148 GHz观测到的宇宙微波背景辐射角功率谱的测量结果。测量使用的是由阿塔卡玛宇宙望远镜（ACT）提供的1.4角分辨率的地图。观测范围为南天228 ° 2，以南纬53°为中心，宽4.2 °。角分角标度的CMB对Silk阻尼标度、星系团的Sunyaev-Zel'dovich（SZ）效应以及射电源和尘埃星系的辐射特别敏感。在我们的地图中屏蔽了108个最亮点源之后，我们使用自适应多锥度方法估计600 <100 < 8000之间的功率谱，以最大限度地减少频谱泄漏并最大限度地利用完整的数据集。我们的绝对校准是基于天王星的观测。为了验证校准和测试我们的地图在大角度尺度下的保真度，我们将ACT地图与WMAP地图进行交叉相关，并从250 <θ < 1150恢复WMAP功率谱。CMB（10000）的丝绸阻尼尾部之外的功率与点源发射的模型一致。我们量化SZ集群的功率谱的贡献，通过拟合到标准化为σ8 = 0.8的模型。我们约束模型的振幅ASZ < 1.63（95%CL）。如果解释为σ8的测量值，则这意味着鉴于我们的SZ模型，σ SZ 8 < 0.86（95% CL）。ACT和WMAP五年资料与六参数ΛCDM模式加点源和SZ效应的联合拟合与这些结果一致。
We present a measurement of the angular power spectrum of the cosmic microwave background (CMB) radiation observed at 148 GHz. The measurement uses maps with 1.′4 angular resolution made with data from the Atacama Cosmology Telescope (ACT). The observations cover 228 deg2 of the southern sky, in a 4.°2 wide strip centered on declination 53° south. The CMB at arcminute angular scales is particularly sensitive to the Silk damping scale, to the Sunyaev–Zel'dovich (SZ) effect from galaxy clusters, and to emission by radio sources and dusty galaxies. After masking the 108 brightest point sources in our maps, we estimate the power spectrum between 600 < ℓ < 8000 using the adaptive multi-taper method to minimize spectral leakage and maximize use of the full data set. Our absolute calibration is based on observations of Uranus. To verify the calibration and test the fidelity of our map at large angular scales, we cross-correlate the ACT map to the WMAP map and recover the WMAP power spectrum from 250 < ℓ < 1150. The power beyond the Silk damping tail of the CMB (ℓ ∼ 5000) is consistent with models of the emission from point sources. We quantify the contribution of SZ clusters to the power spectrum by fitting to a model normalized to σ8 = 0.8. We constrain the model's amplitude ASZ < 1.63 (95% CL). If interpreted as a measurement of σ8, this implies σSZ8 < 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a six-parameter ΛCDM model plus point sources and the SZ effect is consistent with these results.
APEX-SZ 毫米波各向异性高功率谱的约束
DOI：
10.1088/0004-637x/701/2/1958
发表时间：
1958
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Reichardt
通讯作者：
Reichardt
影响因子：
8.7
作者：
Komatsu, E.;Smith, K. M.;Wright, E. L.
通讯作者：
Wright, E. L.
宇宙微波背景温度功率谱的小角尺度测量
DOI：
10.1088/0004-637x/700/2/l187
发表时间：
2009
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Friedman R
通讯作者：
Friedman R