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The galactic habitable zone in elliptical galaxies

Published online by Cambridge University Press:  16 February 2012

Falguni Suthar  and
Christopher P. McKay
Falguni Suthar
Affiliation:
Space Science Division, NASA Ames Research Center, Moffett Field, CA 94035, USA
Christopher P. McKay*
Affiliation:
Space Science Division, NASA Ames Research Center, Moffett Field, CA 94035, USA
*
e-mail: chris.mckay@nasa.gov
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Abstract

The concept of a Galactic Habitable Zone (GHZ) was introduced for the Milky Way galaxy a decade ago as an extension of the earlier concept of the Circumstellar Habitable Zone. In this work, we consider the extension of the concept of a GHZ to other types of galaxies by considering two elliptical galaxies as examples, M87 and M32. We argue that the defining feature of the GHZ is the probability of planet formation which has been assumed to depend on the metallicity. We have compared the metallicity distribution of nearby stars with the metallicity of stars with planets to document the correlation between metallicity and planet formation and to provide a comparison to other galaxies. Metallicity distribution, based on the [Fe/H] ratio to solar, of nearby stars peaks at [Fe/H]≈−0.2 dex, whereas the metallicity distribution of extrasolar planet host stars peaks at [Fe/H]≈+0.4 dex. We compare the metallicity distribution of extrasolar planet host stars with the metallicity distribution of the outer star clusters of M87 and M32. The metallicity distribution of stars in the outer regions of M87 peaks at [Fe/H]≈−0.2 dex and extends to [Fe/H]≈+0.4 dex, which seems favourable for planet formation. The metallicity distribution of stars in the outer regions of M32 peaks at [Fe/H]≈−0.2 dex and extends to a much lower [Fe/H]. Both elliptical galaxies met the criteria of a GHZ. In general, many galaxies should support habitable zones.

Keywords

GalaxiesMilky WayM32M87MetallicityExtrasolar PlanetsPlanet Formation

Information

Type
Research Article
Information
International Journal of Astrobiology , Volume 11 , Issue 3 , July 2012 , pp. 157 - 161
Copyright
Copyright © Cambridge University Press 2012

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References

Barkov, M.V., Aharonian, F.A. & Bosch-Ramon, V. (2010). Gamma-Ray flares from red giant/jet interactions in AGN. Astrophys. J. 724, 1517.CrossRefGoogle Scholar
Bodenheimer, P. et al. (1980). Calculations of the evolution of the giant planets. Icarus 41, 293.CrossRefGoogle Scholar
Castelli, A. et al. (2008). Galaxy populations in the Antlia cluster – II. Compact elliptical galaxy candidates. Mon. Not. R. Astron. Soc. 391, 685–699.CrossRefGoogle Scholar
Ćirković, M.M. (2005) Boundaries of the habitable zone: unifying dynamics, astrophysics, and astrobiology. In Dynamics of Populations of Planetary Systems, ed. Knezevic, Z. & Milani, A., pp. 113–118, Proc. IAU, Colloquium No. 197. Cambridge University Press, Cambridge.Google Scholar
Cockell, C.S. (2006). The origin and emergence of life under impact bombardment. Philos. Trans. R. Soc. Lond., B, Biol. Sci. 361, 1845–1856.CrossRefGoogle ScholarPubMed
Fischer, D. & Valenti, J. (2005). The planet-metallicity correlation. Astrophys. J. 622, 1102–1117.CrossRefGoogle Scholar
Forte, J.C., Faifer, F. & Geisler, D. (2007). A quantitative link between globular clusters and the stellar haloes in elliptical galaxies. Mon. Not. R. Astron. Soc. 382, 1947–1964.CrossRefGoogle Scholar
Freedman, W.L. (1989). Stellar content of nearby galaxies. II. The local group dwarf elliptical galaxy M32. Astron. J. 98, 1285.CrossRefGoogle Scholar
Gonzalez, G. (1997). The stellar metallicity-giant planet connection. Mon. Not. R. Astron. Soc. 285, 403–412.CrossRefGoogle Scholar
Gonzalez, G., Brownlee, D. & Ward, P. (2001). The galactic habitable zone: galactic chemical evolution. Icarus 152, 185–200.CrossRefGoogle Scholar
Grillmair, C. et al. (1996). Hubble space telescope observations of M32: the color-magnitude diagram. Astron. J. 112, 1975.CrossRefGoogle Scholar
Ibukiyama, A. (2004). Solar neighbourhood age–metallicity relation based on Hipparcos data. Publ. Astron. Soc. Australia 21, 121–125.CrossRefGoogle Scholar
Ibukiyama, A. & Arimoto, N. (2002). Hipparcos age–metallicity relation of the solar neighbourhood disk stars. Astron. Astrophys. 394, 927–941.CrossRefGoogle Scholar
Lazcano, A. & Miller, S.L. (1994). How long did it take for life to begin and evolve to cyanobacteria? J. Mol. Evol. 39, 546–554.CrossRefGoogle ScholarPubMed
Lineweaver, C.H., Fenner, Y. & Gibson, B .K. (2004). The galactic habitable zone and the age distribution of complex life in the Milky Way. Science 303, 59–62.CrossRefGoogle ScholarPubMed
McKay, C.P. (1996). Time for intelligence on other planets. In Circumstellar Habitable Zones, ed. Doyle, L.R., pp. 405–419. Travis House Publications, Menlo Park.Google Scholar
Mojzsis, S.J. et al. (1996). Evidence for life on Earth before 3800 million years ago. Nature 384, 55–59.CrossRefGoogle Scholar
Orgel, L.E. (1998). The origin of life – How long did it take? Orig. Life Evol. Biosphere 28, 91–96.CrossRefGoogle Scholar
Pasquini, L. et al. (2007). Evolved stars suggest an external origin of the enhanced metallicity in planet-hosting stars. Astron. Astrophys. 473, 979–982.CrossRefGoogle Scholar
Peña-Cabrera, G.V.Y. & Durand-Manterola, H.J. (2004). Possible biotic distribution in our galaxy. Adv. Space Res. 33, 114–117.CrossRefGoogle Scholar
Prantzos, N. (2008). On the “Galactic Habitable Zone”. Space Sci. Rev. 135, 313–322.CrossRefGoogle Scholar
Ramírez, I. et al. (2010). A possible signature of terrestrial planet formation in the chemical composition of solar analogs. Astron. Astrophys. 521, A33.CrossRefGoogle Scholar
Santos, N.C., Israelian, G. & Mayor, M. (2004). Spectroscopic [Fe/H] for 98 extra-solar planet-host stars. Exploring the probability of planet formation. Astron. Astrophys. 415, 1153–1166.CrossRefGoogle Scholar
Schidlowski, M. (1988). A 3,800-million-year isotopic record of life from carbon in sedimentary rocks. Nature 333, 313–318.CrossRefGoogle Scholar
Schlaufman, K.C. & Laughlin, G. (2011). Kepler exoplanet candidate host stars are preferentially metal rich. Astrophys. J. 738, 177.CrossRefGoogle Scholar
Sundin, M. (2006). The galactic habitable zone in barred galaxies. Int. J. Astrobiol. 5, 325–326.CrossRefGoogle Scholar
Tice, M.M. & Lowe, D.R. (2004). Photosynthetic microbial mats in the 3,416-Myr-old ocean. Nature 431, 549–552.CrossRefGoogle Scholar
Ward, P. & Brownlee, D. (2000). Rare Earth: Why Complex Life is Uncommon in the Universe. Copernicus, New York.CrossRefGoogle Scholar