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CONCERTO: Extracting the power spectrum of the [C II ] emission line

Van Cuyck, M. ; Ponthieu, N. ; Lagache, G. ; Beelen, A. ; Béthermin, M. ; Gkogkou, A. ; Aravena, M. ; Benoit, A. ; Bounmy, J. ; Calvo, M. ; Catalano, A. ; Désert, F. X. ; Dupé, F.-X. ; Fasano, A. ; Ferrara, A. ; Goupy, J. ; Hoarau, C. ; Hu, W. ; Lambert, J.-C ; Macías-Pérez, J. F. ; Marpaud, J. ; Mellema, G. ; Monfardini, A. ; Pallottini, A.

Astronomy and astrophysics (Berlin), 2023-08, Vol.676, p.A62 [Periódico revisado por pares]

EDP Sciences

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  • Título:
    CONCERTO: Extracting the power spectrum of the [C II ] emission line
  • Autor: Van Cuyck, M. ; Ponthieu, N. ; Lagache, G. ; Beelen, A. ; Béthermin, M. ; Gkogkou, A. ; Aravena, M. ; Benoit, A. ; Bounmy, J. ; Calvo, M. ; Catalano, A. ; Désert, F. X. ; Dupé, F.-X. ; Fasano, A. ; Ferrara, A. ; Goupy, J. ; Hoarau, C. ; Hu, W. ; Lambert, J.-C ; Macías-Pérez, J. F. ; Marpaud, J. ; Mellema, G. ; Monfardini, A. ; Pallottini, A.
  • Assuntos: Astrophysics ; cosmology ; galaxies ; high-redshift ; ISM ; large-scale structure of Universe ; observations ; Physics ; star formation
  • É parte de: Astronomy and astrophysics (Berlin), 2023-08, Vol.676, p.A62
  • Descrição: Context. CONCERTO is the first experiment to perform a [C II ] line intensity mapping (LIM) survey on the COSMOS field to target z  > 5.2. Measuring the [C II ] angular power spectrum allows us to study the role of dusty star-forming galaxies in the star formation history during the epochs of Reionization and post-Reionization. The main obstacle to this measurement is the contamination by bright foregrounds: the dust continuum emission and atomic and molecular lines from foreground galaxies at z  ≲ 3. Aims. We evaluate our ability to retrieve the [C II ] signal in mock observations of the sky using the Simulated Infrared Dusty Extragalactic Sky (SIDES), which covers the mid-infrared to millimetre range. We also measure the impact of field-to-field variance on the residual foreground contamination. Methods. We compared two methods for dealing with the dust continuum emission from galaxies (i.e. the cosmic infrared background fluctuations): the standard principal component analysis (PCA) and the asymmetric re-weighted penalized least-squares (arPLS) method. For line interlopers, the strategy relies on masking low-redshift galaxies using the instrumental beam profile and external catalogues. As we do not have observations of CO or deep-enough classical CO proxies (such as L IR ), we relied on the COSMOS stellar mass catalogue, which we demonstrate to be a reliable CO proxy for masking. To measure the angular power spectrum of masked data, we adapted the P of K EstimatoR (POKER) from cosmic infrared background studies and discuss its use on LIM data. Results. The arPLS method achieves a reduction in the cosmic infrared background fluctuations to a sub-dominant level of the [C II ] power at z  ∼ 7, a factor of > 70 below our fiducial [C II ] model. When using the standard PCA, this factor is only 0.7 at this redshift. The masking lowers the power amplitude of line contamination down to 2 × 10 −2 Jy 2 sr −1 . This residual level is dominated by faint undetected sources that are not clustered around the detected (and masked) sources. For our [C II ] model, this results in a detection at z  = 5.2 with a power ratio [C II ]/(residual interlopers) = 62 ± 32 for a 22% area survey loss. However, at z  = 7, [C II ]/(residual interlopers) = 2.0 ± 1.4, due to the weak contrast between [C II ] and the residual line contamination. Thanks to the large area covered by SIDES-Uchuu, we show that the power amplitude of line residuals varies by 12–15% for z  = 5.2 − 7, which is less than the field-to-field variance affecting [C II ] power spectra. Conclusions. We present an end-to-end simulation of the extragalactic foreground removal that we ran to detect the [C II ] at high redshift via its angular power spectrum. We show that cosmic infrared background fluctuations are not a limiting foreground for [C II ] LIM. On the contrary, the CO and [C I ] line contamination severely limits our ability to accurately measure the [C II ] angular power spectrum at z  ≳ 7.
  • Editor: EDP Sciences
  • Idioma: Inglês
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