Spectral distortion of the CMB by the cumulative CO emission from galaxies throughout cosmic history

Mashian, Natalie; Loeb, Abraham; Sternberg, A.

doi:10.1093/mnrasl/slw027

Cited by 14 publications

(17 citation statements)

References 42 publications

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“…The bias of emitting gas is compelling on its own as an indicator of the underlying M gas (M halo ) relation. shows PIXIE's monopole sensitivity and line brightness models from Mashian et al (2016) and Uzgil et al (2014). These are also broadly consistent with recent predictions by Serra et al (2016).…”

Section: Pixiesupporting

confidence: 87%

“…SWITZER Righi et al (2008) and Breysse et al (2014) have developed 2D anisotropy statistics for CO, and Pullen et al (2013) have considered cross-correlation with broadband CMB surveys. Mashian et al (2016) and Serra et al (2016) further calculate the global signal from CO and [C II] in the context of PIXIE. Uzgil et al (2014) The CO molecule is present in similar environments and has a lowest J = 1 − 0 excitation of hν/k B = 5.5 K. CO has a regular ladder at ≈ 115J i GHz which is excited in critical densities from 2 × 10 3 cm −3 to 1 × 10 6 cm −3 , from J = 1 − 0 to J = 10 − 9, respectively (Carilli & Walter 2013).…”

Section: +023mentioning

confidence: 99%

“…For completeness, note that CMB spectral distortion experiments have a unique sensitivity to the line emission monopole. Mashian et al (2016) first argued for PIXIE's sensitivity to global CO emission. The mean emission monopole is not a biased tracer of density, and a combination of monopole and anisotropy analysis could separate the brightness and bias.…”

Section: Pixiementioning

confidence: 99%

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Tracing the Cosmological Evolution of Stars and Cold Gas with CMB Spectral Surveys

Switzer

2017

ApJ

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A full account of galaxy evolution in the context of ΛCDM cosmology requires measurements of the average star-formation rate (SFR) and cold gas abundance across cosmic time. Emission from the CO ladder traces cold gas, and [C II] fine structure emission at 158 µm traces the SFR. Intensity mapping surveys the cumulative surface brightness of emitting lines as a function of redshift, rather than individual galaxies. CMB spectral distortion instruments are sensitive to both the mean and anisotropy of the intensity of redshifted CO and [C II] emission. Large-scale anisotropy is proportional to the product of the mean surface brightness and the line luminosity-weighted bias. The bias provides a connection between galaxy evolution and its cosmological context, and is a unique asset of intensity mapping. Cross-correlation with galaxy redshift surveys allows unambiguous measurements of redshifted line brightness despite residual continuum contamination and interlopers. Measurement of line brightness through cross-correlation also evades cosmic variance and suggests new observation strategies. Galactic foreground emission is ≈ 10 3 times larger than the expected signals, and this places stringent requirements on instrument calibration and stability. Under a range of assumptions, a linear combination of bands cleans continuum contamination sufficiently that residuals produce a modest penalty over the instrumental noise. For PIXIE, the 2σ sensitivity to CO and [C II] emission scales from ≈ 5 × 10 −2 kJy srat low redshift to ≈ 2 kJy sr −1 by reionization.

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Section: Pixiesupporting

confidence: 87%

Section: +023mentioning

confidence: 99%

Section: Pixiementioning

confidence: 99%

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Tracing the Cosmological Evolution of Stars and Cold Gas with CMB Spectral Surveys

Switzer

2017

ApJ

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“…The integrated millimeter and submillimieter line emission from early galaxies has also been recognized as a possible significant contaminant of measurements of the spectral and spatial fluctuations of the cosmic microwave background (CMB; Righi et al 2008aRighi et al , 2008bChluba & Sunyaev 2012;de Zotti et al 2015;Mashian et al 2016). For example, modeling suggests (Mashian et al 2016) that the integrated CO line emission could be significantly higher than the primordial spectral distortions due to other cosmological effects (e.g., Chluba & Sunyaev 2012;Sunyaev & Khatri 2013;Tashiro 2014), and may be measurable with next generation instruments like the Primordial Inflation Explorer (PIXIE; Kogut et al 2014).…”

Section: Introductionmentioning

confidence: 99%

“…For example, modeling suggests (Mashian et al 2016) that the integrated CO line emission could be significantly higher than the primordial spectral distortions due to other cosmological effects (e.g., Chluba & Sunyaev 2012;Sunyaev & Khatri 2013;Tashiro 2014), and may be measurable with next generation instruments like the Primordial Inflation Explorer (PIXIE; Kogut et al 2014). …”

Section: Introductionmentioning

confidence: 99%

The Alma Spectroscopic Survey in the Hubble Ultra Deep Field: Implications for Spectral Line Intensity Mapping at Millimeter Wavelengths and CMB Spectral Distortions

Carilli

Chluba

Decarli

et al. 2016

ApJ

157

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We present direct estimates of the mean sky brightness temperature in observing bands around 99 and 242 GHz due to line emission from distant galaxies. These values are calculated from the summed line emission observed in a blind, deep survey for spectral line emission from high redshift galaxies using ALMA (the ALMA spectral deep field observations "ASPECS" survey). In the 99 GHz band, the mean brightness will be dominated by rotational transitions of CO from intermediate and high redshift galaxies. In the 242 GHz band, the emission could be a combination of higher order CO lines, and possibly [C II] 158 μm line emission from very high redshift galaxies (z∼6-7). The mean line surface brightness is a quantity that is relevant to measurements of spectral distortions of the cosmic microwave background, and as a potential tool for studying large-scale structures in the early universe using intensity mapping. While the cosmic volume and the number of detections are admittedly small, this pilot survey provides a direct measure of the mean line surface brightness, independent of conversion factors, excitation, or other galaxy formation model assumptions. The mean surface brightness in the 99 GHZ band is: T B =0.94±0.09 μK. In the 242 GHz band, the mean brightness is: T B =0.55±0.033 μK. These should be interpreted as lower limits on the average sky signal, since we only include lines detected individually in the blind survey, while in a low resolution intensity mapping experiment, there will also be the summed contribution from lower luminosity galaxies that cannot be detected individually in the current blind survey.

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New horizons in cosmology with spectral distortions of the cosmic microwave background

et al. 2021

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This Voyage 2050 paper highlights the unique science opportunities using spectral distortions of the cosmic microwave background (CMB). CMB spectral distortions probe many processes throughout the history of the Universe, delivering novel information that complements past, present and future efforts with CMB anisotropy and large-scale structure studies. Precision spectroscopy, possible with existing technology, would not only provide key tests for processes expected within the cosmological standard model but also open an enormous discovery space to new physics. This offers unique scientific opportunities for furthering our understanding of inflation, recombination, reionization and structure formation as well as dark matter and particle physics. A dedicated experimental approach could open this new window to the early Universe in the decades to come, allowing us to turn the long-standing upper distortion limits obtained with COBE/FIRAS some 25 years ago into clear detections of the expected standard distortion signals and also challenge our current understanding of the laws of nature.

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Spectral distortion of the CMB by the cumulative CO emission from galaxies throughout cosmic history

Cited by 14 publications

References 42 publications

Tracing the Cosmological Evolution of Stars and Cold Gas with CMB Spectral Surveys

Tracing the Cosmological Evolution of Stars and Cold Gas with CMB Spectral Surveys

The Alma Spectroscopic Survey in the Hubble Ultra Deep Field: Implications for Spectral Line Intensity Mapping at Millimeter Wavelengths and CMB Spectral Distortions

New horizons in cosmology with spectral distortions of the cosmic microwave background

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