CONCERTO: High-fidelity simulation of millimeter line emissions of galaxies and [CII] intensity mapping
CONCERTO: High-fidelity simulation of millimeter line emissions of galaxies and [CII] intensity mapping
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CONCERTO：星系毫米线发射的高保真模拟和 [CII] 强度映射
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发表时间：
2022
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通讯作者：
A. Weiss
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作者：
M. Béthermin;A. Gkogkou;M. V. Cuyck;G. Lagache;A. Beelen;M. Aravena;A. Benoit;J. Bounmy;M. Calvo;A. Catalano;B. D. B. D. Trenquelleon;C. Breuck;A. Fasano;A. Ferrara;J. Goupy;C. Hoarau;C. Horellou;W. Hu;A. Julia;K. Knudsen;J. Lambert;J. Macías;J. Marpaud;A. Monfardini;A. Pallottini;N. Ponthieu;Y. Roehlly;L. Vallini;F. Walter;A. Weiss
[CII] 158 μm线红移到亚毫米窗口的强度映射是探测z bbbb4恒星形成及其在大尺度结构中的空间分布的一种有希望的方法。为了准备第一代实验（例如CONCERTO），我们需要在光谱中对亚毫米星系外天空进行真实的模拟。我们提出了一个新版本的模拟星系外红外尘埃天空（SIDES）模型，其中包括1 mm左右的主要亚毫米线（CO, [CII], [CI]）。该方法成功地再现了观测到的线光度函数。然后，我们利用我们的模拟生成了类似协奏曲的立方体（125-305 GHz），并预测了在这些频率上由各种天体物理成分引起的波动的功率谱。根据我们对恒星形成速率和[CII]亮度之间关系的假设，以及恒星形成历史，我们对z ~ 6 [CII]功率谱的预测变化了两个数量级。这凸显了这些预测的不确定性，以及未来的测量对于提高我们对这个早期时代的理解是多么重要。SIDES可以再现最近通过毫米波强度映射实验（mmIME）在~ 100 GHz测量到的CO射击噪声。最后，我们比较了不同红移的天体物理成分对功率谱的贡献。到目前为止，连续体是最亮的，根据频率的不同，亮度是3到100倍。在300 GHz时，CO前景功率谱高于我们基本方案的[CII]功率谱。在较低的频率下，[CII]和河外前景之间的对比甚至更差。在深度观测中掩盖已知星系应该允许我们将前景降低到[CII]功率谱的20%，最高可达z ~ 6.5。然而，这种掩蔽方法将不足以在较高的红移。我们的模拟代码和产品是公开发布的，可以用于强度测绘实验和亚毫米连续线测量。
The intensity mapping of the [CII] 158-μm line redshifted to the submillimeter window is a promising probe of the z>4 star formation and its spatial distribution into large-scale structures. To prepare the first-generation experiments (e.g., CONCERTO), we need realistic simulations of the submillimeter extragalactic sky in spectroscopy. We present a new version of the simulated infrared dusty extragalactic sky (SIDES) model including the main submillimeter lines around 1 mm (CO, [CII], [CI]). This approach successfully reproduces the observed line luminosity functions. We then use our simulation to generate CONCERTO-like cubes (125–305 GHz) and forecast the power spectra of the fluctuations caused by the various astrophysical components at those frequencies. Depending on our assumptions on the relation between the star formation rate and [CII] luminosity, and the star formation history, our predictions of the z∼6 [CII] power spectrum vary by two orders of magnitude. This highlights how uncertain the predictions are and how important future measurements will be to improve our understanding of this early epoch. SIDES can reproduce the CO shot noise recently measured at ∼100 GHz by the millimeter-wavelength intensity mapping experiment (mmIME). Finally, we compare the contribution of the different astrophysical components at various redshifts to the power spectra. The continuum is by far the brightest, by a factor of three to 100, depending on the frequency. At 300 GHz, the CO foreground power spectrum is higher than the [CII] one for our base scenario. At lower frequencies, the contrast between [CII] and extragalactic foregrounds is even worse. Masking the known galaxies from deep surveys should allow us to reduce the foregrounds to 20 % of the [CII] power spectrum up to z∼6.5. However, this masking method will not be sufficient at higher redshifts. The code and the products of our simulation are released publicly, and can be used for both intensity mapping experiments and submillimeter continuum and line surveys.