Reionization

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In Big Bang cosmology, reionization is the process that reionized the matter in the universe after the "dark ages", and is the second of two major phase transitions of gas in the universe. As the majority of baryonic matter is in the form of hydrogen, reionization usually refers to the reionization of hydrogen gas. The primordial helium in the universe experienced the same phase changes, but at different points in the history of the universe, and is usually referred to as helium reionization.

Background[edit]

Schematic timeline of the universe, depicting reionization's place in cosmic history.

The first phase change of hydrogen in the universe was recombination, which occurred at a redshift z = 1089 (379,000 years after the Big Bang), due to the cooling of the universe to the point where the rate of recombination of electrons and protons to form neutral hydrogen was higher than the reionization rate. The universe was opaque before the recombination, due to the scattering of photons (of all wavelengths) off of free electrons (and, to a significantly lesser extent, free protons), but it became increasingly transparent as more electrons and protons combined to form neutral hydrogen atoms. While electrons in neutral hydrogen can absorb photons of some wavelengths by going to an excited state, a universe full of neutral hydrogen will be relatively opaque only at those absorbed wavelengths, but transparent throughout most of the spectrum. The Dark Ages start at that point, because there were no light sources other than the gradually darkening cosmic background radiation.

The second phase change occurred once objects started to condense in the early universe that were energetic enough to ionize neutral hydrogen. As these objects formed and radiated energy, the universe reverted from being neutral, to once again being an ionized plasma. This occurred between 150 million and one billion years after the Big Bang (at a redshift 6 < z < 20). At that time, however, matter had been diffused by the expansion of the universe, and the scattering interactions of photons and electrons were much less frequent than before electron-proton recombination. Thus a universe full of low density ionized hydrogen will remain transparent, as is the case today.

Detection methods[edit]

Looking back so far in the history of the universe presents some observational challenges. There are, however, a few observational methods for studying reionization.

Quasars and the Gunn-Peterson trough[edit]

One means of studying reionization uses the spectra of distant quasars. Quasars release an extraordinary amount of energy, meaning they are among the brightest objects in the universe. As a result, some quasars are detectable from as far back as the epoch of reionization. Quasars also happen to have relatively uniform spectral features, regardless of their position in the sky or distance from the Earth. Thus it can be inferred that any major differences between quasar spectra will be caused by the interaction of their emission with atoms along the line of sight. For wavelengths of light at the energies of one of the Lyman transitions of hydrogen, the scattering cross-section is large, meaning that even for low levels of neutral hydrogen in the intergalactic medium (IGM), absorption at those wavelengths is highly likely.

For nearby objects in the universe, spectral absorption lines are very sharp, as only photons with energies just sufficient to cause an atomic transition can cause that transition. However, the distances between quasars and the telescopes which detect them are large, which means that the expansion of the universe causes light to undergo noticeable redshifting. This means that as light from the quasar travels through the IGM and is redshifted, wavelengths which had been above the Lyman Alpha limit are stretched, and will in effect begin to fill in the Lymann absorption band. This means that instead of showing sharp spectral absorption lines, a quasar's light which has traveled through a large, spread out region of neutral hydrogen will show a Gunn-Peterson trough.[1]

The redshifting for a particular quasar provides temporal (time) information about reionization. Since an object's redshift corresponds to the time at which it emitted the light, it is possible to determine when reionization ended. Quasars below a certain redshift (closer in space and time) do not show the Gunn-Peterson trough (though they may show the Lyman-alpha forest), while quasars emitting light prior to reionization will feature a Gunn-Peterson trough. In 2001, four quasars were detected (by the Sloan Digital Sky Survey) with redshifts ranging from z = 5.82 to z = 6.28. While the quasars above z = 6 showed a Gunn-Peterson trough, indicating that the IGM was still at least partly neutral, the ones below did not, meaning the hydrogen was ionized. As reionization is expected to occur over relatively short timescales, the results suggest that the universe was approaching the end of reionization at z = 6.[2] This, in turn, suggests that the universe must still have been almost entirely neutral at z > 10.

CMB anisotropy and polarization[edit]

The anisotropy of the cosmic microwave background on different angular scales can also be used to study reionization. Photons undergo scattering when there are free electrons present, in a process known as Thomson scattering. However, as the universe expands, the density of free electrons will decrease, and scattering will occur less frequently. In the period during and after reionization, but before significant expansion had occurred to sufficiently lower the electron density, the light that composes the CMB will experience observable Thomson scattering. This scattering will leave its mark on the CMB anisotropy map, introducing secondary anisotropies (anisotropies introduced after recombination).[3] The overall effect is to erase anisotropies that occur on smaller scales. While anisotropies on small scales are erased, polarization anisotropies are actually introduced because of reionization.[4] By looking at the CMB anisotropies observed, and comparing with what they would look like had reionization not taken place, the electron column density at the time of reionization can be determined. With this, the age of the universe when reionization occurred can then be calculated.

The Wilkinson Microwave Anisotropy Probe allowed that comparison to be made. The initial observations, released in 2003, suggested that reionization took place from 11 <z < 30.[5] This redshift range was in clear disagreement with the results from studying quasar spectra. However, the three year WMAP data returned a different result, with reionization beginning at z = 11 and the universe ionized by z = 7.[6] This is in much better agreement with the quasar data.

Results in 2013 from Planck mission, in combination with data from WMAP polarization, small-scale CMB experiments, and BAO measurements yield an instantaneous reionization redshift of z = 11.3 ± 1.1.[7]

The parameter usually quoted here is τ, the "optical depth to reionization," or alternatively, zre, the redshift of reionization, assuming it was an instantaneous event. While this is unlikely to be physical, since reionization was very likely not instantaneous, zre provides an estimate of the mean redshift of reionization.

21-cm line[edit]

Even with the quasar data roughly in agreement with the CMB anisotropy data, there are still a number of questions, especially concerning the energy sources of reionization and the effects on, and role of, structure formation during reionization. The 21-cm line in hydrogen is potentially a means of studying this period, as well as the "dark ages" that preceded reionization. The 21-cm line occurs in neutral hydrogen, due to differences in energy between the spin triplet and spin singlet states of the electron and proton. This transition is forbidden, meaning it occurs extremely rarely. The transition is also highly temperature dependent, meaning that as objects form in the "dark ages" and emit Lyman-alpha photons that are absorbed and re-emitted by surrounding neutral hydrogen, it will produce a 21-cm line signal in that hydrogen through Wouthuysen-Field coupling.[8][9] By studying 21-cm line emission, it will be possible to learn more about the early structures that formed. While there are currently no results, there are a few projects underway which hope to make headway in this area in the near future, such as the Precision Array for Probing the Epoch of Reionization (PAPER), Low Frequency Array (LOFAR), Murchison Widefield Array (MWA), Giant Metrewave Radio Telescope (GMRT), the Dark Ages Radio Explorer (DARE) mission, and the Large-Aperture Experiment to Detect the Dark Ages (LEDA).

Energy sources[edit]

While observations have come in which narrow the window during which the epoch of reionization could have taken place, it is still uncertain which objects provided the photons that reionized the IGM. To ionize neutral hydrogen, an energy larger than 13.6 eV is required, which corresponds to photons with a wavelength of 91.2 nm or shorter. This is in the ultraviolet part of the electromagnetic spectrum, which means that the primary candidates are all sources which produce a significant amount of energy in the ultraviolet and above. How numerous the source is must also be considered, as well as the longevity, as protons and electrons will recombine if energy is not continuously provided to keep them apart. Altogether, the critical parameter for any source considered can be summarized as its "emission rate of hydrogen-ionizing photons per unit cosmological volume."[10] With these constraints, it is expected that quasars and first generation stars and galaxies were the main sources of energy.[11]

Dwarf galaxies[edit]

Dwarf galaxies are currently the primary candidate source of ionizing photons during the epoch of reionization.[12] For most scenarios, this would require the log-slope of the UV galaxy luminosity function, often denoted α, to be steeper than it is today, approaching α = -2.[13]

Quasars[edit]

Quasars, a class of active galactic nuclei (AGN), were considered a good candidate source because they are highly efficient at converting mass to energy, and emit a great deal of light above the threshold for ionizing hydrogen. It is unknown, however, how many quasars existed prior to reionization. Only the brightest of quasars present during reionization can be detected, which means there is no direct information about dimmer quasars that existed. However, by looking at the more easily observed quasars in the nearby universe, and assuming that the luminosity function (number of quasars as a function of luminosity) during reionization will be approximately the same as it is today, it is possible to make estimates of the quasar populations at earlier times. Such studies have found that quasars do not exist in high enough numbers to reionize the IGM alone,[10][14] saying that "only if the ionizing background is dominated by low-luminosity AGNs can the quasar luminosity function provide enough ionizing photons."[15]

Population III stars[edit]

Simulated image of the first stars, 400 Myr after the Big Bang.

Population III stars are stars which have no elements more massive than hydrogen or helium. During Big Bang nucleosynthesis, the only elements that formed aside from hydrogen and helium were trace amounts of lithium. Yet quasar spectra have revealed the presence of heavy elements in the IGM at an early era. Supernova explosions produce such heavy elements, so hot, large, Population III stars which will form supernovae are a possible mechanism for reionization. While they have not been directly observed, they are consistent according to models using numerical simulation[16] and current observations.[17] A gravitationally lensed galaxy also provides indirect evidence of Population III stars.[18] Even without direct observations of Population III stars, they are a compelling source. They are more efficient and effective ionizers than Population II stars, as they emit more ionizing photons,[19] and are capable of reionizing hydrogen on their own in some reionization models with reasonable initial mass functions.[20] As a consequence, Population III stars are currently considered the most likely energy source to initiate the reionization of the universe,[21] though other sources are likely to have taken over and driven reionization to completion.

See also[edit]

Notes and references[edit]

  1. ^ J.E. Gunn and B.A. Peterson (1965). "On the Density of Neutral Hydrogen in Intergalactic Space". The Astrophysical Journal 142: 1633–1641. Bibcode:1965ApJ...142.1633G. doi:10.1086/148444. 
  2. ^ R.H. Becker, et al. (2001). "Evidence For Reionization at z ~ 6: Detection of a Gunn-Peterson Trough In A z=6.28 Quasar". Astronomical Journal 122 (6): 2850–2857. arXiv:astro-ph/0108097. Bibcode:2001AJ....122.2850B. doi:10.1086/324231. 
  3. ^ Manoj Kaplinghat et al. (2003). "Probing the Reionization History of the Universe using the Cosmic Microwave Background Polarization". The Astrophysical Journal 583 (1): 24–32. arXiv:astro-ph/0207591. Bibcode:2003ApJ...583...24K. doi:10.1086/344927. 
  4. ^ Olivier Dore et al. (2007). "The Signature of Patchy Reionization in the Polarization Anisotropy of the CMB". arXiv:astro-ph/0701784.
  5. ^ A. Kogut et al. (2003). "First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Temperature-Polarization Correlation". The Astrophysical Journal Supplement Series 148 (1): 161–173. arXiv:astro-ph/0302213. Bibcode:2003ApJS..148..161K. doi:10.1086/377219. 
  6. ^ D.N. Spergel et al. (2006). "Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology". The Astrophysical Journal Supplement Series 170 (2): 377–408. arXiv:astro-ph/0603449. Bibcode:2007ApJS..170..377S. doi:10.1086/513700. 
  7. ^ http://arxiv.org/abs/1303.5062
  8. ^ Rennan Barkana and Abraham Loeb (2005). "Detecting the Earliest Galaxies through Two New Sources of 21 Centimeter Fluctuations". The Astrophysical Journal 626 (1): 1–11. arXiv:astro-ph/0410129. Bibcode:2004astro.ph.10129B. doi:10.1086/429954. 
  9. ^ Marcelo Alvarez et al. (2010). "Enhanced Detectability of Pre-reionization 21-cm Structure". arXiv:1007.0001.
  10. ^ a b Piero Madau et al. (1999). "Radiative Transfer in a Clumpy Universe. III. The Nature of Cosmological Ionizing Source". The Astrophysical Journal 514 (2): 648–659. arXiv:astro-ph/9809058. Bibcode:1999ApJ...514..648M. doi:10.1086/306975. 
  11. ^ Loeb and Barkana (2000). "In the Beginning: The First Sources of Light and the Reionization of the Universe". Physics Reports 349 (2): 125–238. arXiv:astro-ph/0010468. Bibcode:2001PhR...349..125B. doi:10.1016/S0370-1573(01)00019-9. 
  12. ^ http://adsabs.harvard.edu/abs/2012ApJ...752L...5B
  13. ^ http://adsabs.harvard.edu/abs/2012MNRAS.423..862K
  14. ^ Paul Shapiro & Mark Giroux (1987). "Cosmological H II regions and the photoionization of the intergalactic medium". The Astrophysical Journal 321: 107–112. Bibcode:1987ApJ...321L.107S. doi:10.1086/185015. 
  15. ^ Xiaohu Fan, et al. (2001). "A Survey of z>5.8 Quasars in the Sloan Digital Sky Survey. I. Discovery of Three New Quasars and the Spatial Density of Luminous Quasars at z~6". The Astronomical Journal 122 (6): 2833–2849. arXiv:astro-ph/0108063. Bibcode:2001AJ....122.2833F. doi:10.1086/324111. 
  16. ^ Nickolay Gnedin and Jeremiah Ostriker (1997). "Reionization of the Universe and the Early Production of Metals". Astrophysical Journal 486 (2): 581–598. arXiv:astro-ph/9612127. Bibcode:1997ApJ...486..581G. doi:10.1086/304548. 
  17. ^ Limin Lu et al. (1998). "The Metal Contents of Very Low Column Density Lyman-alpha Clouds: Implications for the Origin of Heavy Elements in the Intergalactic Medium". arXiv:astro-ph/9802189.
  18. ^ R. A. E. Fosbury et al. (2003). "Massive Star Formation in a Gravitationally Lensed H II Galaxy at z = 3.357". Astrophysical Journal 596 (1): 797–809. arXiv:astro-ph/0307162. Bibcode:2003ApJ...596..797F. doi:10.1086/378228. 
  19. ^ Jason Tumlinson et al. (2002). "Cosmological Reionization by the First Stars: Evolving Spectra of Population III". ASP Conference Proceedings 267: 433–434. Bibcode:2002hsw..work..433T. 
  20. ^ Aparna Venkatesan et al. (2003). "Evolving Spectra of Population III Stars: Consequences for Cosmological Reionization". Astrophysical Journal 584 (2): 621–632. arXiv:astro-ph/0206390. Bibcode:2003ApJ...584..621V. doi:10.1086/345738. 
  21. ^ Marcelo Alvarez et al. (2006). "The H II Region of the First Star". Astrophysical Journal 639 (2): 621–632. arXiv:astro-ph/0507684. Bibcode:2006ApJ...639..621A. doi:10.1086/499578. 

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