On Estimation of Contamination from Hydrogen Cyanide in Carbon Monoxide Line-intensity Mapping

Chung, Dongwoo T.; Li, Tony Y.; Viero, Marco P.; Church, S.

doi:10.3847/1538-4357/aa8624

Cited by 16 publications

(12 citation statements)

References 34 publications

(147 reference statements)

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“…Spectral Foregrounds: The removal of interloper line emission is an area of active development. For CO, the contribution of interloper lines is likely negligible (Chung et al 2017). However, lower redshift CO emission (from several rotational transitions of the molecule) could represent a significant foreground for [CII].…”

Section: Resultsmentioning

confidence: 99%

Probing Cosmic Origins with CO and [C ii] Emission Lines

Dizgah

Keating

Fialkov

2019

ApJL

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Primordial non-Gaussianity is an invaluable window into the physical processes that gave rise to cosmological structure. The presence of local shape PNG imprints a distinct scale-dependent correction to the bias of dark matter tracers on large scales, which can be effectively probed via the technique of intensity mapping. Considering an upcoming generation of experiments, we demonstrate that intensity mapping of CO and [CII] emission can improve upon the current best constraints from the Planck satellite. We show that measurement of the CO intensity power spectrum by a hypothetical next stage of the ground-based COMAP experiment can achieve σ(f loc NL ) = 3.4, and that the proposed CMB satellite mission PIXIE can achieve σ(f loc NL ) = 3.9 via measurement of [CII] intensity power spectrum. Subject headings: early universe -galaxies: high-redshift -large-scale structure of universe THE LINE INTENSITY POWER SPECTRUMCO is predominantly found in the dense clouds of molecular gas (of density n ∼ 10 3 cm −3 ), while [CII]

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Section: Resultsmentioning

confidence: 99%

Probing Cosmic Origins with CO and [C ii] Emission Lines

Dizgah

Keating

Fialkov

2019

ApJL

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“…The impact of foregrounds on intensity mapping varies wildly depending on which line is being considered. CO(1-0) surveys are only mildly contaminated (Chung et al 2017), but the CO(8-7) map would have to contend with lower-order CO transitions coming from lower redshifts. It is possible that this contamination could be removed, either by masking out contaminated regions (Gong et al 2012;Sun et al 2018), or by exploiting power spectrum anisotropies (Lidz & Taylor 2016;Cheng et al 2016).…”

Section: Discussionmentioning

confidence: 99%

Coupling parsec and gigaparsec scales: primordial non-Gaussianity with multi-tracer intensity mapping

Liu,

Breysse

2020

Preprint

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Primordial non-Gaussianity (PNG) is a key probe of the origins of primordial fluctuations in the early universe. It has been shown that multi-tracer measurements of large-scale structure can produce high-precision measurements of PNG. Future line intensity mapping surveys are well-suited to these measurements owing to their ability to rapidly survey large volumes and access the large scales at which PNG becomes important. In this paper, we explore for the first time how multi-tracer PNG measurements with intensity mapping surveys depend on the sub-galactic scale physics which drives line emission. We consider an example cross-correlation between CO maps, and find that the choice of astrophysical models has a substantial impact on f NL measurements at sufficiently high signal-to-noise. This in effect creates a coupling between horizon-scale PNG measurements and the molecular cloud-scale interstellar medium. We discuss how these effects depend on noise level and survey design. We further find that the cross-correlation shot noise, an effect nearly unique to intensity mapping measurements, plays an important role in multi-tracer analyses and cannot be neglected.

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“…We therefore cannot rule out the possibility that a few extremely luminous objects are present in our field. However, models where contamination is expected to be significant require objects with HCN luminosities 10 10 K km s −1 pc 2 (Chung et al 2017). Even if such galaxies do exist, they would be so rare as to be unlikely to appear in our survey volume, therefore it seems unlikely that they contaminate the auto-power results of K16 significantly.…”

Section: Search For Interloper Line Contaminationmentioning

confidence: 96%

“…At the redshifts studied by COPSS, no significant interlopers are expected for the CO(1-0) transition (Chung et al 2017), although dense gas tracers such as HCN J=1-0 and CS J=1-0 have been proposed as a potential contaminant (Breysse et al 2015). HCN emission in our SZA data corresponds to sources at 1.5 < z < 2.3.…”

Section: Search For Interloper Line Contaminationmentioning

confidence: 99%

“…We follow the approach of Li et al (2016, hereafter L16; see also Silva et al 2015;Chung et al 2017), assign-ing CO luminosities to halo catalogs from dark matter simulations using a series of scaling relations. This approach is particularly advantageous for modeling cross correlation, as each CO emitter can be matched to other halo properties in order to construct mock galaxy catalogs for cross-correlation.…”

Section: Model Descriptionmentioning

confidence: 99%

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An Intensity Mapping Constraint on the CO-Galaxy Cross Power Spectrum at Redshift ~ 3

Keenan,

Keating,

Marrone

2021

Preprint

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The abundance of cold molecular gas plays a crucial role in models of galaxy evolution. While deep spectroscopic surveys of CO emission lines have been a primary tool for measuring this abundance, the difficulty of these observations has motivated alternative approaches to studying molecular gas content. One technique, line intensity mapping, seeks to constrain the average molecular gas properties of large samples of individually undetectable galaxies through the CO brightness power spectrum.Here we present constraints on the cross-power spectrum between CO intensity maps and optical galaxy catalogs. This cross-measurement allows us to check for systematic problems in CO intensity mapping data, and validate the data analysis used the auto-power spectrum measurement of the CO Power Spectrum Survey. We place a 2σ upper limit on the band-averaged CO-galaxy cross-power of P × < 540 µK h −3 Mpc 3 . Our measurement favors a non-zero T CO at around 90% confidence and gives an upper limit on the mean molecular gas density at z ∼ 2.6 of 7.7 × 10 8 M Mpc −3 . We forecast the expected cross-power spectrum by applying a number of literature prescriptions for the CO luminosity to halo mass relation to a suite of mock light cones. Under the most optimistic forecasts the cross-spectrum could be detected with only moderate extensions of the data used here, while more conservative models could be detected with a factor of 10 increase in sensitivity. Ongoing CO intensity mapping experiments will target fields allowing extensive cross correlation analysis and should reach the sensitivity required to detect the cross-spectrum signal.

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On Estimation of Contamination from Hydrogen Cyanide in Carbon Monoxide Line-intensity Mapping

Cited by 16 publications

References 34 publications

Probing Cosmic Origins with CO and [C ii] Emission Lines

Probing Cosmic Origins with CO and [C ii] Emission Lines

Coupling parsec and gigaparsec scales: primordial non-Gaussianity with multi-tracer intensity mapping

An Intensity Mapping Constraint on the CO-Galaxy Cross Power Spectrum at Redshift ~ 3

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