Carbon monoxide intensity mapping at moderate redshifts

Breysse, Patrick C.; Kovetz, Ely D.; Kamionkowski, Marc

doi:10.1093/mnras/stu1312

Cited by 76 publications

(105 citation statements)

References 25 publications

Supporting

Mentioning

103

Contrasting

Order By: Relevance

“…While the 21 cm reionization signal is brighter, the foregrounds are commensurately brighter because of the synchrotron spectral index, yielding a similar challenge. Considering CO (1-0) at 115 GHz, Breysse et al (2014) and Li et al (2015) suggest mean temperatures of 1 K m at z 3. The scales of interest at tens of arcminutes are reasonably analogous to the Cosmic Background Imager (CBI) (Pearson et al 2003), which finds fluctuations in the raw maps at the level of several hundred K m at 30 GHz.…”

Section: Review Of Continuum Foreground Levelsmentioning

confidence: 99%

“…Intensity mapping was originally developed for 21 cm radiation (Hogan & Rees 1979;Scott & Rees 1990;Madau et al 1997), but has been studied for several other lines (in increasing frequency): deuterium (Sigurdson & Furlanetto 2006) (Righi et al 2008;Carilli 2011;Lidz et al 2011;Breysse et al 2014;Li et al 2015), C II (Gong et al 2012;Silva et al 2014;Uzgil et al 2014;Yue et al 2015), Lya Pullen et al 2014), C and O fine-structure (Kusakabe & Kawasaki 2012), and X-ray lines (Hütsi et al 2012).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Interpreting the Unresolved Intensity of Cosmologically Redshifted Line Radiation

Switzer

Chang

Masui

et al. 2015

ApJ

107

View full text Add to dashboard Cite

Intensity mapping experiments survey the spectrum of diffuse line radiation rather than detect individual objects at high signal-to-noise ratio. Spectral maps of unresolved atomic and molecular line radiation contain threedimensional information about the density and environments of emitting gasand efficiently probe cosmological volumes out to high redshift. Intensity mapping survey volumes also contain all other sources of radiation at the frequencies of interest. Continuum foregrounds are typically~10 2 -10 3 times brighter than the cosmological signal. The instrumental response to bright foregrounds will produce new spectral degrees of freedom that are not known in advance, nor necessarily spectrally smooth. The intrinsic spectra of foregrounds may also not be wellknown in advance. We describe a general class of quadratic estimators to analyze data from single-dish intensity mapping experimentsand determine contaminated spectral modes from the data themselves. The key attribute of foregrounds is not that they are spectrally smooth, but instead that they have fewer bright spectral degrees of freedom than the cosmological signal. Spurious correlations between the signal and foregrounds produce additional bias. Compensation for signal attenuation must estimate and correct this bias. A successful intensity mapping experiment will control instrumental systematics that spread variance into new modes, and it must observe a large enough volume that contaminant modes can be determined independently from the signal on scales of interest.

show abstract

Section: Review Of Continuum Foreground Levelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Interpreting the Unresolved Intensity of Cosmologically Redshifted Line Radiation

Switzer

Chang

Masui

et al. 2015

ApJ

107

View full text Add to dashboard Cite

show abstract

“…It is important to note that Breysse, Kovetz, & Kamionkowski (2014) (hereafter BKK) found that the amplitude of a CO intensity mapping power spectrum is extremely uncertain, and that different models yield very different results. We have every reason to believe that the modeling of each and every signal and foreground line we discuss here is similarly uncertain.…”

Section: Introductionmentioning

confidence: 99%

Masking line foregrounds in intensity-mapping surveys

Breysse¹,

Kovetz²,

Kamionkowski³

2015

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

We address the problem of line confusion in intensity mapping surveys and explore the possibility to mitigate line foreground contamination by progressively masking the brightest pixels in the observed map. We consider experiments targeting CO(1-0) at z = 3, Lyα at z = 7, and CII at z = 7, and use simulated intensity maps, which include both clustering and shot noise components of the signal and possible foregrounds, in order to test the efficiency of our method. We find that for CO and Lyα it is quite possible to remove most of the foreground contribution from the maps via only 1%−3% pixel masking. The CII maps will be more difficult to clean, however, due to instrumental constraints and the high-intensity foreground contamination involved. While the masking procedure sacrifices much of the astrophysical information present in our maps, we demonstrate that useful cosmological information in the targeted lines can be successfully retrieved.

show abstract

“…Line brightness determined through the cross-power does not have a cosmic variance or require a detailed model of the galaxy power spectrum. 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.…”

Section: +023mentioning

confidence: 99%

“…STATISTICAL CONSTRAINTS ON THE ANISOTROPY Intensity mapping literature has described constraints primarily on the 3D power spectrum, which exploit unique tomographic capabilities (for 2D analysis, see e.g. Pullen et al 2013;Breysse et al 2014). PIXIE's 15 GHz bands give fewer modes in k than k ⊥ , and few total k modes for low-J CO transitions.…”

Section: Pixiementioning

confidence: 99%

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

Switzer

2017

ApJ

View full text Add to dashboard Cite

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.

show abstract

Carbon monoxide intensity mapping at moderate redshifts

Cited by 76 publications

References 25 publications

Interpreting the Unresolved Intensity of Cosmologically Redshifted Line Radiation

Interpreting the Unresolved Intensity of Cosmologically Redshifted Line Radiation

Masking line foregrounds in intensity-mapping surveys

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

Contact Info

Product

Resources

About