The Dark Energy Survey Year 3 and eBOSS: constraining galaxy intrinsic alignments across luminosity and colour space
The Dark Energy Survey Year 3 and eBOSS: constraining galaxy intrinsic alignments across luminosity and colour space
复制标题
第三年暗能量调查和 eBOSS：限制星系在亮度和色彩空间上的内在排列
DOI：
10.1093/mnras/stad2013
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发表时间：
2023
影响因子：
4.8
通讯作者：
Elvin-Poole, J.
中科院分区：
文献类型：
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作者：
Samuroff, S.;Mandelbaum, R.;Blazek, J.;Campos, A.;MacCrann, N.;Zacharegkas, G.;Amon, A.;Prat, J.;Singh, S.;Elvin-Poole, J.
我们提出了直接约束星系的内在排列（IA）使用暗能量调查年3（DES Y3），扩展重子振荡光谱调查（eBOSS），和它的前身，重子振荡光谱调查（BOSS）。我们的测量包括来自DES的测光红色序列（redMaGiC）星系，中值红移为0.2-1.0，来自eBOSS的发光红色星系，以及SDSS-III BOSS CMASS样本，平均红移为0.5。我们测量两点IA的相关性，我们适合使用一个模型，包括透镜，放大率和光度红移误差。在6 Mpch−1<rp< 70 Mpch−1的尺度上拟合，我们在每个样本中检测到IA，在5σ-22σ（假设IA的简单单参数模型）。使用这些红色样品，我们测量IA-光度关系。我们的结果与以前的结果在统计上是一致的，但提供了一个显着的改善约束力，特别是在低光度。随着精度的提高，我们看到了广泛定义的红色样本之间对颜色的可检测依赖性。未来可能需要一种比二进制红/蓝分裂更复杂的方法，该方法联合考虑IA信号中的颜色和亮度依赖性。我们还比较了每个样本在参数空间中最佳拟合点处的各种信号分量，并发现放大和透镜效应对总信号的贡献。随着精度的不断提高，在未来的直接IA测量中，肯定有必要考虑这些影响。最后，我们对eBOSS atz 0.8的发射线星系样本进行了等效测量。我们将非线性排列幅度限制为（|A1| < 0.78（95% CL）。
We present direct constraints on galaxy intrinsic alignments (IAs) using the Dark Energy Survey Year 3 (DES Y3), the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), and its precursor, the Baryon Oscillation Spectroscopic Survey (BOSS). Our measurements incorporate photometric red sequence (redMaGiC) galaxies from DES with median redshiftz∼ 0.2–1.0, luminous red galaxies from eBOSS atz∼ 0.8, and also an SDSS-III BOSS CMASS sample atz∼ 0.5. We measure two-point IA correlations, which we fit using a model that includes lensing, magnification, and photometric redshift error. Fitting on scales 6 Mpch−1<rp< 70 Mpch−1, we make a detection of IAs in each sample, at 5σ–22σ (assuming a simple one-parameter model for IAs). Using these red samples, we measure the IA–luminosity relation. Our results are statistically consistent with previous results, but offer a significant improvement in constraining power, particularly at low luminosity. With this improved precision, we see detectable dependence on colour between broadly defined red samples. It is likely that a more sophisticated approach than a binary red/blue split, which jointly considers colour and luminosity dependence in the IA signal, will be needed in future. We also compare the various signal components at the best-fitting point in parameter space for each sample, and find that magnification and lensing contributeof the total signal. As precision continues to improve, it will certainly be necessary to account for these effects in future direct IA measurements. Finally, we make equivalent measurements on a sample of emission-line galaxies from eBOSS atz∼ 0.8. We constrain the non-linear alignment amplitude to be(|A1| < 0.78 at 95 per cent CL).