# Metallicity

(Redirected from Population III)
The globular cluster M80. Stars in globular clusters are mainly older metal-poor members of Population II.

In astronomy and physical cosmology, the metallicity or Z, is the proportion of its matter making up the chemical elements in stars or other kinds of astronomical objects, excluding their hydrogen (X) and helium (Y).[1][2] Most of the physical matter in the universe is in the form of hydrogen and helium, so astronomers conveniently use the blanket term "metal" to describe all other elements.[3] For example, stars or nebulae that are relatively rich in carbon, nitrogen, oxygen, and neon would be "metal-rich" in astrophysical terms, even though those elements are non-metals in chemistry. This term should not be confused with the usual physical definition of solid metals.

Metallicity in stars and other astronomical objects is an approximate estimation of their chemical abundances that change over time by the mechanisms of stellar evolution,[4] and therefore provide an indication of age.[5] In cosmological terms, the universe is also chemically evolving. According to the Big Bang Theory, the early universe first consisted of hydrogen and helium, with trace amounts of lithium and beryllium, but with no heavier elements. Through the process of stellar evolution, where stars at the end of their lives discard most of their mass by stellar winds or explode as supernovae, the metal content of the Galaxy and the Universe increases.[6] It is then assumed, that older generations of stars generally have lower metallicities than the current younger generation stars.[7]

Observed changes in the chemical abundances of different types of stars, based on the spectral peculiarities that were later attributed to metallicity, lead astronomer Walter Baade in 1944 to propose the existence of different populations of stars in galaxies.[8] These became commonly known as Population I and Population II stars. Another kind of stellar population was introduced in 1978, known as Population III stars,[9] [10] appearing for the first time in a paper title in 1980.[11] These extremely metal poor stars were theorised to have been the first born stars created in the Universe.

## Definition

Stellar composition, as determined by spectroscopy, is usually simply defined by the parameters X, Y and Z. Here X is the fractional percentage of Hydrogen, Y is the fractional percentage of Helium, and all the remaining chemical elements as the fractional percentage, Z. It is simply defined as;

$X + Y + Z = 1.00$

In most stars, nebulae and other astronomical sources, hydrogen and helium are the two dominant elements. The hydrogen mass fraction is generally expressed as $X\equiv \frac{m_\mathrm{H}}{M}$ where $M$ is the total mass of the system and $m_\mathrm{H}$ the fractional mass of the hydrogen it contains. Similarly, the helium mass fraction is denoted as $Y\equiv \frac{m_\mathrm{He}}{M}$. The remainder of the elements are collectively referred to as 'metals', and the metallicity—the mass fraction of elements heavier than helium—can be calculated as

$Z = \sum_{i>\mathrm{He}} \frac{m_i}{M} = 1 - X - Y.$

For the Sun, these parameters are often assumed to have the following approximate values,[12] although recent research shows that lower values for $Z_\mathrm{sun}$ might be more appropriate:[13][14]

Description Solar value
Hydrogen mass fraction $X_\mathrm{sun} = 0.73$
Helium mass fraction $Y_\mathrm{sun} = 0.25$
Metallicity $Z_\mathrm{sun} = 0.02$

For many astronomical objects the metallicity cannot be measured directly. Instead, proxies are used to obtain an indirect estimate. For example, an observer might measure the iron content of a galaxy (for example using the brightness of an iron emission line) directly, then compare that value with models to estimate the total metallicity.

### Calculation

The metallicity is often expressed as "[Fe/H]", which represents the logarithm of the ratio of a star's iron abundance compared to that of the Sun (iron is not the most abundant heavy element, but it is among the easiest to measure with spectral data in the visible spectrum). The formula for the logarithm is expressed thus:

$[\mathrm{Fe}/\mathrm{H}] = \log_{10}{\left(\frac{N_{\mathrm{Fe}}}{N_{\mathrm{H}}}\right)_\mathrm{star}} - \log_{10}{\left(\frac{N_{\mathrm{Fe}}}{N_{\mathrm{H}}}\right)_\mathrm{sun}}$

where $N_{\mathrm{Fe}}$ and $N_{\mathrm{H}}$ are the number of iron and hydrogen atoms per unit of volume respectively. The unit often used for metallicity is the "dex" which is a (now-deprecated) contraction of 'decimal exponent'.[15] By this formulation, stars with a higher metallicity than the Sun have a positive logarithmic value, whereas those with a lower metallicity than the Sun have a negative value. The logarithm is based on powers of 10; stars with a value of +1 have ten times the metallicity of the Sun (101). Conversely, those with a value of −1 have one tenth (10−1), whereas those with −2 have a hundredth (10−2), and so on.[3] Young Population I stars have significantly higher iron-to-hydrogen ratios than older Population II stars. Primordial Population III stars are estimated to have a metallicity of less than −6.0, that is, less than a millionth of the abundance of iron which is found in the Sun.[citation needed]

This same sort of notation is used to express differences in the individual elements from the solar proportion. For example, the notation "[O/Fe]" represents the difference in the logarithm of the star's oxygen abundance compared to that of the Sun and the logarithm of the star's iron abundance compared to the Sun:

$[\mathrm{O}/\mathrm{Fe}] = \log_{10}{\left(\frac{N_{\mathrm{O}}}{N_{\mathrm{Fe}}}\right)_\mathrm{star}} - \log_{10}{\left(\frac{N_{\mathrm{O}}}{N_{\mathrm{Fe}}}\right)_\mathrm{sun}}$
$= \left[\log_{10}{\left(\frac{N_{\mathrm{O}}}{N_{\mathrm{H}}}\right)_\mathrm{star}} - \log_{10}{\left(\frac{N_{\mathrm{O}}}{N_{\mathrm{H}}}\right)_\mathrm{sun}}\right] - \left[\log_{10}{\left(\frac{N_{\mathrm{Fe}}}{N_{\mathrm{H}}}\right)_\mathrm{star}} - \log_{10}{\left(\frac{N_{\mathrm{Fe}}}{N_{\mathrm{H}}}\right)_\mathrm{sun}}\right].$

The point of this notation is that if a mass of gas is diluted with pure hydrogen, then its [Fe/H] value will decrease (because there are fewer iron atoms per hydrogen atom after the dilution), but for all other elements X, the [X/Fe] ratios will remain unchanged. By contrast, if a mass of gas is polluted with some amount of pure oxygen, then its [Fe/H] will remain unchanged but its [O/Fe] ratio will increase. In general, a given stellar nucleosynthetic process alters the proportions of only a few elements or isotopes, so a star or gas sample with nonzero [X/Fe] values may be showing the signature of particular nuclear processes.

### Relation between Z and [Fe/H]

These two ways of expressing the metallic content of a star are related through the equation:

$\log_{10}\left(\frac{Z/X}{Z_\mathrm{sun}/X_\mathrm{sun}}\right) = [\mathrm{M}/\mathrm{H}]$

where [M/H] is the star's total metal abundance (i.e. all elements heavier than helium) defined as a more general expression than the one for [Fe/H]:

$[\mathrm{M}/\mathrm{H}] = \log_{10}{\left(\frac{N_{\mathrm{M}}}{N_{\mathrm{H}}}\right)_\mathrm{star}} - \log_{10}{\left(\frac{N_{\mathrm{M}}}{N_{\mathrm{H}}}\right)_\mathrm{sun}} .$

The iron abundance and the total metal abundance are often assumed to be related through a constant A as:

$[\mathrm{M}/\mathrm{H}] = A*[\mathrm{Fe}/\mathrm{H}]$

where A assumes values between 0.9 and 1. Using the formulas presented above, the relation between Z and [Fe/H] can finally be written as:

$\log_{10}\left(\frac{Z/X}{Z_\mathrm{sun}/X_\mathrm{sun}}\right) = A*[\mathrm{Fe}/\mathrm{H}].$

## Stellar populations

Stellar populations were categorized as I and II in 1944 by Walter Baade, then later in 1978, was added Population III. By coincidence, each group has decreasing metal content and increasing age. Hence the first stars in the Universe (low metal content) were population III, and recent stars (high metallicity) are population I.

Observation of the spectra of stars has revealed that the older stars have fewer heavy elements compared to the Sun. This suggests that metallicity has evolved through the generations of stars by the process of stellar evolution. On the current cosmological models, the matter created in the Big Bang was mostly hydrogen and helium, with only a very tiny fraction of light elements like lithium and beryllium. After this, when the Universe cooled sufficiently, the first stars were born, as extremely metal-poor Population III stars. Without metals, it is postulated that their stellar masses were hundreds of times that of the Sun could be formed. In turn, these massive stars evolved very quickly, whose nucleosynthesis processes quickly created the first 26 elements up to iron in the periodic table.[16][citation needed]

Current theoretical stellar models show that most high-mass Population III stars quickly exhausted their fuel and exploded in extremely energetic pair-instability supernovae. Those explosions would have thoroughly dispersed their material, ejecting metals into the interstellar medium (ISM), to be incorporated into the later generations of stars. Their destruction, suggests no galactic high-mass Population III stars are observable. However, some Population III stars might be seen in high-redshift galaxies whose light originated during the earlier history of the Universe, remaining as a future area of astronomical research.[citation needed] None have been discovered. Stars too massive to produce pair-instability supernovae would have collapsed into black holes through a process known as photodisintegration, but some matter may have escaped during this process in the form of relativistic jets, and this could have "sprayed" the first metals into the Universe.[17][18]

A rendering of Mu Arae, a metal-rich population I star.

It has been proposed that recent supernovae SN 2006gy and SN 2007bi may have been pair-instability supernovae in which such super-massive Population III stars exploded. It has been speculated that these stars could have formed relatively recently in dwarf galaxies containing primordial metal-free interstellar matter; past supernovae in these galaxies could have ejected their metal-rich contents at speeds high enough for them to escape the galaxy, keeping the metal content of the galaxy very low.[19]

The oldest observed stars, known as Population II, have very low metallicities;[20][21] as subsequent generations of stars were born they became more metal-enriched, as the gaseous clouds from which they formed received the metal-rich dust manufactured by previous generations. As those stars died, they returned metal-enriched material to the interstellar medium via planetary nebulae and supernovae, enriching the nebulae out of which the newer stars formed ever further. These youngest stars, including the Sun, therefore have the highest metal content, and are known as Population I stars.

### Population I stars

Population I, or metal-rich stars, are young stars with the highest metallicity out of all three populations. The Earth's Sun is an example of a metal-rich star. These are common in the spiral arms of the Milky Way galaxy.

Generally, the youngest stars, the extreme Population I, are found farther in and intermediate Population I stars are farther out, etc. The Sun is considered an intermediate Population I star. Population I stars have regular elliptical orbits of the galactic centre, with a low relative velocity. It was hypothesised that the high metallicity of Population I stars makes them more likely to possess planetary systems than the other two populations, because planets, particularly terrestrial planets, are thought to be formed by the accretion of metals.[22] However, observations of the Kepler data-set have found smaller planets around stars with a range of metallicities, while only larger potential gas giant planets are concentrated around stars with relatively higher metallicity, a finding that has implications for theories of gas giant formation.[23]

Between the intermediate populations I and II comes the intermediary disc population.

### Population II stars

Population II, or metal-poor stars, are those with relatively little metal. The idea of a relatively small amount must be kept in perspective as even metal-rich astronomical objects contain low percentages of any element other than hydrogen or helium; metals constitute only a tiny percentage of the overall chemical makeup of the Universe, even 13.8 billion years after the Big Bang. However, metal-poor objects are even more primitive. These objects formed during an earlier time of the Universe. Intermediate Population I stars are common in the bulge near the centre of our galaxy; whereas Population II stars found in the galactic halo are older and thus more metal-poor. Globular clusters also contain high numbers of Population II stars.[24] It is believed that Population II stars created all the other elements in the periodic table, except the more unstable ones. An interesting characteristic of Population II stars is that despite their lower overall metallicity, they often have a higher ratio of alpha elements (O, Si, Ne, etc.) relative to Fe as compared to Population I stars; current theory suggests this is the result of Type II supernovae being more important contributors to the interstellar medium at the time of their formation, whereas Type Ia supernovae metal enrichment came later in the Universe's evolution.[25]

Scientists have targeted these oldest stars in several different surveys, including the HK objective-prism survey of Timothy C. Beers et al. and the Hamburg-ESO survey of Norbert Christlieb et al., originally started for faint quasars. Thus far, they have uncovered and studied in detail about ten very metal-poor stars (such as Sneden's Star, Cayrel's Star, BD +17° 3248) and three of the oldest stars known to date: HE0107-5240, HE1327-2326 and HE 1523-0901. Caffau's star was identified as the most metal-poor star yet when it was found in 2012 using Sloan Digital Sky Survey data. However in February 2014 the discovery of an even lower metallicity star was announced, SMSS J031300.36-670839.3 located with the aid of SkyMapper astronomical survey data. Less extreme in their metal deficiency, but nearer and brighter and hence longer known, are HD 122563 (a red giant) and HD 140283 (a subgiant).

### Population III stars

Possible glow of Population III stars imaged by NASA's Spitzer Space Telescope.
Credit: NASA / JPL-Caltech / A. Kashlinsky (GSFC)

Population III, or extremely metal-poor stars (EMP),[26] are a hypothetical extinct population of extremely massive and hot stars with virtually no metals, except possibly for intermixing ejecta from other nearby Pop III supernovae. Their existence is inferred from cosmology, but they have not yet been observed directly. Indirect evidence for their existence has been found in a gravitationally lensed galaxy in a very distant part of the Universe.[27] They are also thought to be components of faint blue galaxies. Their existence is proposed to account for the fact that heavy elements, which could not have been created in the Big Bang, are observed in quasar emission spectra, as well as the existence of faint blue galaxies.[16] It is believed that these stars triggered a period of reionization. UDFy-38135539, a galaxy recently discovered, is believed to have been a part of this process. Some theories hold that there were two generations of Population III stars.[28]

Artist's impression of the first stars, 400 million years after the Big Bang.

Current theory is divided on whether the first stars were very massive or not - theories proposed in 2009 and 2011 suggest the first star groups might have consisted of a massive star surrounded by several smaller stars.[29][30] One theory, which seems to be borne out by computer models of star formation, is that with no heavy elements and a much warmer interstellar medium from the Big Bang, it was easy to form stars with much greater total mass than the ones visible today.[citation needed] Typical masses for Population III stars would be expected to be about several hundred solar masses, which is much larger than the current stars. Analysis of data on extremely low-metallicity Population II stars such as HE0107-5240, which are thought to contain the metals produced by Population III stars, suggest that these metal-free stars had masses of 20 to 130 solar masses instead.[31] On the other hand, analysis of globular clusters associated with elliptical galaxies suggests pair-instability supernovae, which are typically associated with very massive stars, were responsible for their metallic composition.[32] This also explains why there have been no low-mass stars with zero metallicity observed, although models have been constructed for smaller Population III stars.[33] Clusters containing zero-metallicity red dwarfs or brown dwarfs (possibly created by pair-instability supernovae[21]) have been proposed as dark matter candidates,[34][35] but searches for these and other MACHOs through gravitational microlensing have produced negative results.

Detection of Population III stars is a goal of NASA's James Webb Space Telescope.[36] New spectroscopic surveys, such as SEGUE or SDSS-II, may also locate Population III stars.[citation needed]

## References

1. ^ D. Kunth & G. Östlin (2000). "The Most Metal-poor Galaxies" 10 (1). The Astronomy and Astrophysics Review. Retrieved 3 February 2015.
2. ^ W. Sutherland (26 March 2013). "The Galaxy. Chapter 4. Galactic Chemical Evolution". Retrieved 13 January 2015.
3. ^ a b John C. Martin. "What we learn from a star's metal content". New Analysis RR Lyrae Kinematics in the Solar Neighborhood. Retrieved September 7, 2005.
4. ^ McWilliam, Andrew (26 March 2013). "Abundance Ratios and galactic Chemical Evolution". Retrieved 13 January 2015.
5. ^ McWilliam, Andrew (1997-01-01). "Abundance Ratios and galactic Chemical Evolution : Age-Metallicity Relation". Retrieved 2015-01-13.
6. ^ F. Hoyle (1954). "On Nuclear Reactions Occurring in Very Hot Stars. I. the Synthesis of Elements from Carbon to Nickel.". Astrophysical Journal Supplement 1: 121–146. Bibcode:1954ApJS....1..121H. doi:10.1086/190005.
7. ^ McWilliam, Andrew (1997-01-01). "Abundance Ratios and galactic Chemical Evolution : Introduction". Retrieved 2015-01-13.
8. ^ W. Baade (1944). "The Resolution of Messier 32, NGC 205, and the Central Region of the Andromeda Nebula.". Astrophysical Journal 100: 121–146. Bibcode:1944ApJ...100..137B. doi:10.1086/144650.
9. ^ M.J. Rees (1978). "Origin of pregalactic microwave background". Nature 275: 35–37. Bibcode:1978Natur.275...35R. doi:10.1038/275035a0.
10. ^ S.D.M. White; M.J. Rees (1978). "Core condensation in heavy halos - A two-stage theory for galaxy formation and clustering". Monthly Notices Royal Astronomical Society 183: 341–358. Bibcode:1978MNRAS.183..341W.
11. ^ J.L. Puget; J. Heyvaerts (1980). "Population III stars and the shape of the cosmological black body radiation". Astronomy and Astrophysics 83: L10–L12. Bibcode:1980A&A....83L..10P.
12. ^ A. Unsöld; B. Baschek; R.C. Smith; C.A. Hein (1983). The New Cosmos. Springer New York. doi:10.1007/978-1-4757-1791-4. ISBN 978-0-387-90886-1.
13. ^ "The new solar abundances - Part I: the observations". Communications in Asteroseismology. January 2006. Retrieved 2013-06-25.
14. ^ "Solar Heavy-Element Abundance: Constraints from Frequency Separation Ratios of Low-Degree p-Modes". The Astrophysical Journal. November 2007. Retrieved 2013-06-30.
15. ^ R. Rowlett et al. (July 2005). "How Many? A Dictionary of Units of Measurement". University of North Carolina. Retrieved 3 February 2015.
16. ^ a b A. Heger; S. E. Woosley (2002). "The Nucleosynthetic Signature of Population III". Astrophysical Journal 567 (1): 532–543. arXiv:astro-ph/0107037. Bibcode:2002ApJ...567..532H. doi:10.1086/338487.
17. ^ Fryer, C. L.; Woosley, S. E.; Heger, A. (2001). "Pair-Instability Supernovae, Gravity Waves, and Gamma-Ray Transients". The Astrophysical Journal 550: 372. arXiv:astro-ph/0007176. Bibcode:2001ApJ...550..372F. doi:10.1086/319719.
18. ^ Heger, A.; Fryer, C. L.; Woosley, S. E.; Langer, N.; Hartmann, D. H. (2003). "How Massive Single Stars End Their Life". The Astrophysical Journal 591: 288. arXiv:astro-ph/0212469. Bibcode:2003ApJ...591..288H. doi:10.1086/375341.
19. ^ Stuart Clark (February 2010). "Primordial giant: The star that time forgot". New Scientist. Retrieved February 2015.
20. ^ Lauren J. Bryant. "What Makes Stars Tick". Indiana University Research & Creative Activity. Retrieved September 7, 2005.
21. ^ a b Salvaterra, R.; Ferrara, A.; Schneider, R. (2004). "Induced formation of primordial low-mass stars". New Astronomy 10 (2): 113. arXiv:astro-ph/0304074. Bibcode:2004NewA...10..113S. doi:10.1016/j.newast.2004.06.003.
22. ^ Charles H. Lineweaver (2000). "An Estimate of the Age Distribution of Terrestrial Planets in the Universe: Quantifying Metallicity as a Selection Effect". Icarus 151 (2): 307–313. arXiv:astro-ph/0012399. Bibcode:2001Icar..151..307L. doi:10.1006/icar.2001.6607.
23. ^ Buchhave, L.A. et al. (2012) An abundance of small exoplanets around stars with a wide range of metallicities. Nature 486:375–377
24. ^ T. S. van Albada; Norman Baker (1973). "On the Two Oosterhoff Groups of Globular Clusters". Astrophysical Journal 185: 477–498. Bibcode:1973ApJ...185..477V. doi:10.1086/152434.
25. ^ Wolfe, Gawiser, Prochaska, "DAMPED Lyalpha SYSTEMS", Annu. Rev. Astron. Astrophys. 2005. 43: 861–918 http://ned.ipac.caltech.edu/level5/Sept05/Wolfe/Wolfe3.html
26. ^ N. Tominga et al. (2007). "Supernova Nucleosynthesis in Population III 13-50 Msolar Stars and Abundance Patterns of Extremely Metal-poor Stars". Astrophysical Journal 660 (5): 516–540. arXiv:astro-ph/0701381. Bibcode:2007ApJ...660..516T. doi:10.1086/513063.
27. ^ 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.
28. ^ V. Bromm; N. Yoshida; L. Hernquist; C.F. McKee (2009). "The formation of the first stars and galaxies". Nature 459 (7243). arXiv:0905.0929v1. Bibcode:2009Natur.459...49B. doi:10.1038/nature07990.
29. ^ Nola Redd (February 2011). "The Universe's First Stars Weren't Loners After All". Space.com. Retrieved February 2015.
30. ^ Andrea Thompson (January 2009). "How Massive Stars Form: Simple Solution Found". Space.com. Retrieved February 2015.
31. ^ Umeda, Hideyuki; Nomoto, Ken'Ichi (2003). "First-generation black-hole-forming supernovae and the metal abundance pattern of a very iron-poor star". Nature 422 (6934): 871–873. arXiv:astro-ph/0301315. Bibcode:2003Natur.422..871U. doi:10.1038/nature01571. PMID 12712199.
32. ^ Puzia, Thomas H.; Kissler‐Patig, Markus; Goudfrooij, Paul (2006). "Extremely α‐Enriched Globular Clusters in Early‐Type Galaxies: A Step toward the Dawn of Stellar Populations?". The Astrophysical Journal 648: 383–388. arXiv:astro-ph/0605210. Bibcode:2006ApJ...648..383P. doi:10.1086/505679.
33. ^ Siess, Lionel; Livio, Mario; Lattanzio, John (2002). "Structure, Evolution, and Nucleosynthesis of Primordial Stars". The Astrophysical Journal 570: 329–343. arXiv:astro-ph/0201284. Bibcode:2002ApJ...570..329S. doi:10.1086/339733.
34. ^ Kerins, E. J. (1997). "Zero-metallicity very low mass stars as halo dark matter". Astronomy and Astrophysics 322: 709. arXiv:astro-ph/9610070. Bibcode:1997A&A...322..709K.
35. ^ Sanchez-Salcedo, F. J. (1997). "On the Stringent Constraint on Massive Dark Clusters in the Galactic Halo". Astrophysical Journal Letters v.487 487: L61. Bibcode:1997ApJ...487L..61S. doi:10.1086/310873.
36. ^ C-E. Rydberg; E. Zackrisson; P. Lundqvist; P. Scott (March 2013). "Detection of isolated Population III stars with the James Webb Space Telescope". MNRAS 429 (4). arXiv:1206.0007v2. Bibcode:2013MNRAS.429.3658R. doi:10.1093/mnras/sts653.