Large-scale clustering of Lyman α emission intensity from SDSS/BOSS
Large-scale clustering of Lyman α emission intensity from SDSS/BOSS
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SDSS/BOSS 莱曼 α 发射强度的大规模聚类
DOI：
10.1093/mnras/stw204
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发表时间：
2015
影响因子：
4.8
通讯作者：
C. Yéche
中科院分区：
文献类型：
--
作者：
R. Croft;J. Miralda;Zheng Zheng;A. Bolton;K. Dawson;J. Peterson;D. York;D. Eisenstein;J. Brinkmann;J. Brownstein;T. Delubac;A. Font;J. Hamilton;K. Lee;A. Myers;N. Palanque;I. Pâris;P. Petitjean;M. Pieri;N. Ross;G. Rossi;D. Schlegel;D. Schneider;A. Slosar;J. Vázquez;M. Viel;D. Weinberg;C. Yéche
通过测量Sloan数字巡天/重子振荡光谱巡天中Ly α表面亮度与类星体的互相关，尝试性地探测了宇宙中红移z = 2-3.5的Ly α发射的大尺度结构。我们使用数百万个光谱，目标是z \textless 0.8的明亮红色星系，在从每个光谱中减去最佳拟合模型星系光谱后，作为高红移Ly α表面亮度的估计。类星体-Ly α发射互相关在尺度1上被检测到，类似于15 h（-1）Mpc，形状与Lambda CDM模型一致，Ω（m）= 0.30（-0.07）（+0.10）。这种互相关的预测幅度与平均Ly α表面亮度、\textlessmu（alpha）\textgreater、质量波动幅度以及类星体和Ly α发射偏置因子的乘积成比例。我们推断\textlessmu（alpha）\textgreater（B（alpha）/3）=（3.9 +/- 0.9）x 10（-21）erg s（-1）cm（-2）angstrom（-1）arcsec（-2），其中B（alpha）是Ly alpha发射偏置。如果恒星形成星系主导这种发射，我们发现rho（SFR）=（0.28 +/- 0.07）（3/B（alpha））yr（-1）Mpc（-3）。对于B（α）= 3，这个值是类似的30倍以上，比以前的估计，从单独检测到的Ly α发射器，但一致的总ρ（SFR）来自尘埃校正，连续紫外线星系调查，如果大多数的Ly α光子从这些星系避免尘埃吸收，并在大的气体晕扩散后重新发射。加热星系际气体的He II光电离类星体辐射或喷流可以解释检测到的相关性，和冷却辐射的气体在星系晕也可能作出贡献。我们还检测到红移空间各向异性的类星体Ly α发射互相关，发现证据在3.0西格玛水平，它是径向拉长，这可能是由辐射传输效应解释。我们的测量代表的第一个应用程序的强度映射技术的光学观测。
We present a tentative detection of the large-scale structure of Ly alpha emission in the Universe at redshifts z = 2-3.5 by measuring the cross-correlation of Ly alpha surface brightness with quasars in Sloan Digital Sky Survey/Baryon Oscillation Spectroscopic Survey. We use amillion spectra targeting luminous red galaxies at z \textless 0.8, after subtracting a best-fitting model galaxy spectrum from each one, as an estimate of the high-redshift Ly alpha surface brightness. The quasar-Ly alpha emission cross-correlation is detected on scales 1 similar to 15 h(-1) Mpc, with shape consistent with a Lambda CDM model with Omega(m) = 0.30(-0.07)(+0.10). The predicted amplitude of this cross-correlation is proportional to the product of the mean Ly alpha surface brightness, \textlessmu(alpha)\textgreater, the amplitude of mass fluctuations and the quasar and Ly alpha emission bias factors. We infer \textlessmu(alpha)\textgreater (b(alpha)/3) = (3.9 +/- 0.9) x 10(-21) erg s(-1) cm(-2) angstrom(-1) arcsec(-2), where b(alpha) is the Ly alpha emission bias. If star-forming galaxies dominate this emission, we find rho(SFR) = (0.28 +/- 0.07)(3/b(alpha)) yr(-1) Mpc(-3). For b(alpha) = 3, this value is similar to 30 times larger than previous estimates from individually detected Ly alpha emitters, but consistent with the total rho(SFR) derived from dust-corrected, continuum UV galaxy surveys, if most of the Ly alpha photons from these galaxies avoid dust absorption and are reemitted after diffusing in large gas haloes. Heating of intergalactic gas by He II photoionization from quasar radiation or jets may alternatively explain the detected correlation, and cooling radiation from gas in galactic haloes may also contribute. We also detect redshift space anisotropy of the quasar-Ly alpha emission cross-correlation, finding evidence at the 3.0 sigma level that it is radially elongated, which may be explained by radiative-transfer effects. Our measurements represent the first application of the intensity mapping technique to optical observations.
斯隆数字巡天第十次数据发布：来自 SDSS-III 阿帕奇点天文台银河演化实验的首个光谱数据
DOI：
10.1088/0067-0049/211/2/17
发表时间：
2014
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
Ahn C
通讯作者：
Ahn C
SDSS-III/BOSS 大质量星系动态特性的红移演化
DOI：
10.1088/0004-637x/789/2/92
发表时间：
2014
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Beifiori A
通讯作者：
Beifiori A