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Intensity mapping

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<div id="mw-content-text" class="mw-body-content mw-content-ltr" lang="en" dir="ltr"><div class="mw-content-ltr mw-parser-output" lang="en" dir="ltr">In cosmology, intensity mapping is an observational technique for surveying the <a href="Large-scale_structure_of_the_universe" class="mw-redirect" title="Large-scale structure of the universe">large-scale structure of the universe</a> by using the integrated <a href="Radio_waves" class="mw-redirect" title="Radio waves">radio emission</a> from unresolved gas clouds.

In its most common variant, 21 cm intensity mapping, the <a href="Hydrogen_line" title="Hydrogen line">21 cm emission line</a> of neutral hydrogen is used to trace the gas. The hydrogen follows fluctuations in the underlying cosmic density field, with regions of higher density giving rise to a higher intensity of emission. Intensity fluctuations can therefore be used to reconstruct the <a href="Matter_power_spectrum" title="Matter power spectrum">power spectrum of matter fluctuations</a>. The frequency of the emission line is <a href="Redshift" title="Redshift">redshifted</a> by the expansion of the Universe, so by using radio receivers that cover a wide frequency band, one can detect this signal as a function of redshift, and thus cosmic time. This is similar in principle to a <a href="Redshift_survey" title="Redshift survey">galaxy redshift survey</a>, with the important distinction that galaxies need to be individually detected and measured, making intensity mapping a considerably faster method.<a href="#cite_note-Bull-1">[1]</a>

<div class="mw-heading mw-heading2"><h2 id="History">History</h2></div>

<ul><li>Aug 1977: Varshalovich and Khersonskii<a href="#cite_note-2">[2]</a> calculate the effect of 21cm line absorption at high redshift on the spectrum of the CMB.</li>

<li>Aug 1996: Madau, Meiksin & Rees<a href="#cite_note-3">[3]</a> propose intensity mapping as a way of probing the <a href="Epoch_of_Reionization" class="mw-redirect" title="Epoch of Reionization">Epoch of Reionization</a>.</li>

<li>Dec 2001: Bharadwaj & Sethi<a href="#cite_note-4">[4]</a> propose using intensity maps of neutral hydrogen to observe the matter distribution in the post-reionisation epoch.</li>

<li>Jan 2004: Battye, Davies & Weller<a href="#cite_note-5">[5]</a> propose using 21 cm intensity maps to measure <a href="Dark_energy" title="Dark energy">dark energy</a>.</li>

<li>Jun 2006: Peterson, Bandura, and Pen<a href="#cite_note-6">[6]</a> propose the Hubble Sphere Hydrogen Survey</li>

<li>Mar 2009: Cosmological HI signal observed for the first time out to redshift 1.12<a href="#cite_note-7">[7]</a> by the <a href="Green_Bank_Telescope" title="Green Bank Telescope">Green Bank Telescope</a>.</li>

<li>Jan 2013: Construction begins on the <a href="Canadian_Hydrogen_Intensity_Mapping_Experiment" title="Canadian Hydrogen Intensity Mapping Experiment">CHIME experiment</a><a href="#cite_note-8">[8]</a> in <a href="British_Columbia" title="British Columbia">British Columbia</a>, Canada.</li></ul>

<div class="mw-heading mw-heading2"><h2 id="Scientific_applications">Scientific applications</h2></div>

Intensity mapping has been proposed as a way of measuring the cosmic matter density field in several different regimes.

<div class="mw-heading mw-heading3"><h3 id="Epoch_of_Reionization">Epoch of Reionization</h3></div>

Between the times of <a href="Recombination_(cosmology)" title="Recombination (cosmology)">recombination</a> and <a href="Reionization" title="Reionization">reionization</a>, the <a href="Baryon" title="Baryon">baryonic</a> content of the Universe – mostly hydrogen – existed in a neutral phase. Detecting the 21 cm emission from this time, all the way through to the end of reionization, has been proposed as a powerful way of studying early structure formation.<a href="#cite_note-Loeb-9">[9]</a> This period of the Universe's history corresponds to redshifts of <math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle z\approx 30}">

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<annotation encoding="application/x-tex">{\displaystyle z\approx 30}</annotation>

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</math><img src="./e574b148afb9c1e4b1fafdefee2a7360a20e948b.svg" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:6.512ex; height:2.176ex;" alt="{\displaystyle z\approx 30}" loading="lazy"> to <math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle z\approx 6-12}">

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<annotation encoding="application/x-tex">{\displaystyle z\approx 6-12}</annotation>

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</math><img src="./350268ba22cd8d6f4f81a9e3400ca13069d48971.svg" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.505ex; width:10.514ex; height:2.343ex;" alt="{\displaystyle z\approx 6-12}" loading="lazy">, implying a frequency range for intensity mapping experiments of 50 – 200 MHz.

<div class="mw-heading mw-heading3"><h3 id="Large-scale_structure_and_dark_energy">Large-scale structure and dark energy</h3></div>

At late times, after the Universe has <a href="Reionization" title="Reionization">reionized</a>, most of the remaining neutral hydrogen is stored in dense gas clouds called <a href="Damped_Lyman-alpha_system" title="Damped Lyman-alpha system">damped Lyman-alpha systems</a>, where it is protected from <a href="Extragalactic_background_light" title="Extragalactic background light">ionizing UV radiation</a>. These are predominantly hosted in galaxies, so the neutral hydrogen signal is effectively a tracer of the galaxy distribution.

As with galaxy redshift surveys, intensity mapping observations can be used to measure the geometry and expansion rate of the Universe (and therefore the properties of <a href="Dark_energy" title="Dark energy">dark energy</a><a href="#cite_note-Bull-1">[1]</a>) by using the <a href="Baryon_Acoustic_Oscillations" class="mw-redirect" title="Baryon Acoustic Oscillations">baryon acoustic oscillation</a> feature in the matter power spectrum as a <a href="Standard_ruler" title="Standard ruler">standard ruler</a>. The growth rate of structure, useful for testing <a href="Alternatives_to_general_relativity" title="Alternatives to general relativity">modifications to general relativity</a>,<a href="#cite_note-10">[10]</a> can also be measured using <a href="Peculiar_velocity" title="Peculiar velocity">redshift space distortions</a>. Both of these features are found at large scales of tens to hundreds of <a href="Megaparsec" class="mw-redirect" title="Megaparsec">megaparsecs</a>, which is why low angular resolution (unresolved) maps of neutral hydrogen are sufficient to detect them. This should be compared with the resolution of a redshift survey, which must detect individual galaxies that are typically only tens of kiloparsecs across.

Because intensity mapping surveys can be carried out much faster than conventional optical redshift surveys, it is possible to map-out significantly larger volumes of the Universe. As such, intensity mapping has been proposed as a way of measuring phenomena on extremely large scales, including <a href="Non-Gaussianity" title="Non-Gaussianity">primordial non-Gaussianity</a> from <a href="Inflation_(cosmology)" class="mw-redirect" title="Inflation (cosmology)">inflation</a><a href="#cite_note-11">[11]</a> and general relativistic corrections to the <a href="Correlation_function_(astronomy)" title="Correlation function (astronomy)">matter correlation function</a>.<a href="#cite_note-12">[12]</a>

<div class="mw-heading mw-heading3"><h3 id="Molecular_and_fine_structure_lines">Molecular and fine structure lines</h3></div>

In principle, any emission line can be used to make intensity maps if it can be detected. Other emission lines that have been proposed as cosmological tracers include:

<ul><li>Rotational transitions in molecules, such as carbon monoxide<a href="#cite_note-13">[13]</a></li>

<li>Fine structure transitions from species such as ionized carbon<a href="#cite_note-14">[14]</a></li>

<li>Lyman-alpha emission from hydrogen<a href="#cite_note-15">[15]</a></li></ul>

<div class="mw-heading mw-heading2"><h2 id="Experiments">Experiments</h2></div>

The following telescopes have either hosted intensity mapping surveys, or plan to carry them out in future.

<ul><li>TIANLAI (China) <a href="#cite_note-16">[16]</a></li>

<li><a href="BINGO_(telescope)" title="BINGO (telescope)">BINGO</a> (Brazil/Uruguay/UK)</li>

<li><a href="Canadian_Hydrogen_Intensity_Mapping_Experiment" title="Canadian Hydrogen Intensity Mapping Experiment">CHIME</a> (Canada)</li>

<li>COMAP (USA) <a href="#cite_note-17">[17]</a></li>

<li><a href="Five_hundred_meter_Aperture_Spherical_Telescope" class="mw-redirect" title="Five hundred meter Aperture Spherical Telescope">FAST</a> (China)</li>

<li><a href="Green_Bank_Telescope" title="Green Bank Telescope">Green Bank Telescope</a> (USA)</li>

<li><a rel="nofollow" class="external text" href="http://www.acru.ukzn.ac.za/~hirax">HIRAX</a> (South Africa)</li>

<li><a href="KAT7" class="mw-redirect" title="KAT7">KAT7</a> (South Africa)</li>

<li><a href="MeerKAT" title="MeerKAT">MeerKAT</a> (South Africa)<a href="#cite_note-18">[18]</a></li>

<li><a href="Parkes_radio_telescope" class="mw-redirect" title="Parkes radio telescope">Parkes radio telescope</a> (Australia)</li>

<li><a href="Precision_Array_for_Probing_the_Epoch_of_Reionization" title="Precision Array for Probing the Epoch of Reionization">PAPER</a> (USA/South Africa/Australia)</li>

<li><a href="Square_Kilometre_Array" title="Square Kilometre Array">Square Kilometre Array</a> (South Africa/Australia)</li></ul>

The <a href="Goddard_Space_Flight_Center" title="Goddard Space Flight Center">Goddard Space Flight Center</a> also host a list of intensity mapping <a rel="nofollow" class="external text" href="https://lambda.gsfc.nasa.gov/product/expt/lim_experiments.html">experiments</a>.

<div class="mw-heading mw-heading2"><h2 id="References">References</h2></div>

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</style><cite id="CITEREFBullFerreiraPatelSantos2015" class="citation journal cs1">Bull, Philip; Ferreira, Pedro G.; Patel, Prina; Santos, Mario G. (2015). "Late-time cosmology with 21cm intensity mapping experiments". The Astrophysical Journal. 803 (1): 21. <a href="ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/1405.1452">1405.1452</a>. <a href="Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2015ApJ...803...21B">2015ApJ...803...21B</a>. <a href="Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1088%2F0004-637X%2F803%2F1%2F21">10.1088/0004-637X/803/1/21</a>. <a href="S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:118350366">118350366</a>.</cite>

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<div class="mw-heading mw-heading2"><h2 id="External_links">External links</h2></div>

<ul><li><a rel="nofollow" class="external text" href="https://www2.physics.ox.ac.uk/events/2012/11/23/oxford-martin-workshop-on-intensity-mapping">Oxford Martin workshop on intensity mapping</a></li>

<li><a rel="nofollow" class="external text" href="http://zuserver2.star.ucl.ac.uk/~fba/RAS/">RAS discussion meeting on intensity mapping</a></li>

<li><a rel="nofollow" class="external text" href="http://chime.phas.ubc.ca/">CHIME experiment</a></li></ul></div><div><div class="zim-footer">

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