The DOI matches its Crossref record; 36 of the 36 references it cites were found in a registry or an index.
Metallicity Effects on Mid-Infrared Colors and the 8 μm PAH Emission in Galaxies
Open accessAbstract
We examine colors from 3.6 to 24 μm as a function of metallicity (O/H) for a sample of 34 galaxies. The galaxies range over 2 orders of magnitude in metallicity. They display an abrupt shift in the 8 μm-to-24 μm color for metallicities between one-third and one-fifth of the solar value. The mean 8-to-24 μm flux density ratio below and above 12 + log (O/H) = 8.2 is 0.08 ± 0.04 and 0.70 ± 0.53, respectively. We use mid-IR colors and spectroscopy to demonstrate that the shift is primarily due to a decrease in the 8 μm flux density, as opposed to an increase in the 24 μm flux density. This result is most simply interpreted as being due to a weakening at low metallicity of the mid-IR emission bands usually attributed to PAHs (polycyclic aromatic hydrocarbons) relative to the small-grain dust emission. However, existing empirical spectral energy distribution models cannot account for the observed short-wavelength (below 8 μm) colors of the low-metallicity galaxies merely by reducing the strength of the PAH features; some other emission source (e.g., hot dust) is required.
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Cites
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Starburst99: Synthesis Models for Galaxies with Active Star Formation
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The Infrared Spectrograph (IRS) on the Spitzer Space Telescope
Houck, J. R., Roellig, T. L., van Cleve, J., Forrest, W. J., Herter, T., Lawrence, C. R., Matthews, K., Reitsema, H. J., Soifer, B. T., Watson, D. M., et al. (2004) · The Astrophysical Journal Supplement Series · doi:10.1086/423134 · Cited by 1,526
What Powers Ultraluminous IRAS Galaxies?
Genzel, R., Lutz, D., Sturm, E., Egami, E., Kunze, D., Moorwood, A. F. M., Rigopoulou, D., Spoon, H. W. W., Sternberg, A., Tacconi‐Garman, L. E., et al. (1998) · The Astrophysical Journal · doi:10.1086/305576 · Cited by 1,157
The [ITAL]Forbidden[/ITAL] Abundance of Oxygen in the Sun
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Inferences from the Composition of Two Dwarf Blue Galaxies
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Heavy‐Element Abundances in Blue Compact Galaxies
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The Infrared Spectral Energy Distribution of Normal Star‐forming Galaxies
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Self-citationThe Primordial Helium Abundance: Systematic Effects and a New Determination
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Cited by
Star Formation in the Milky Way and Nearby Galaxies
Kennicutt, R. C., & Evans, N. J. (2012) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081811-125610 · Cited by 2,902
“…2005a; Farrah et al. 2007; Calzetti et al. 2007), but the PAH bands weaken dramatically below metal abundances of approximately 1/4 to 1/3 Z⊙ (e.g., Madden 2000; Engelbracht et al. 2005; Calzetti et al. 2007; Smith et al. 2007), rendering them problematic as quantitative SFR tracers in this regime.”
BackgroundDraine, B. T., & Li, A. (2007) · The Astrophysical Journal · doi:10.1086/511055 · Cited by 2,122
Smith, J. D. T., Draine, B. T., Dale, D. A., Moustakas, J., Kennicutt, Jr., Helou, G., Armus, L., Roussel, H., Sheth, K., Bendo, G. J., et al. (2007) · The Astrophysical Journal · doi:10.1086/510549 · Cited by 962
Self-citationCONSTRAINING THE LOW-MASS SLOPE OF THE STAR FORMATION SEQUENCE AT 0.5 <z< 2.5
Whitaker, K. E., Franx, M., Leja, J., van Dokkum, P. G., Henry, A., Skelton, R. E., Fumagalli, M., Momcheva, I. G., Brammer, G. B., Labbé, I., et al. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/795/2/104 · Cited by 854
Le Floc’h, E., Papovich, C., Dole, H., Bell, E. F., Lagache, G., Rieke, G. H., Egami, E., Perez‐Gonzalez, P. G., Alonso‐Herrero, A., Rieke, M. J., et al. (2005) · The Astrophysical Journal · doi:10.1086/432789 · Cited by 818
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Metadata
- Authors
- Engelbracht, C. W., Gordon, K. D., Rieke, G. H., Werner, M. W., Dale, D. A., & Latter, W. B.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2005-06-24
- Volume
- 628
- Issue
- 1
- Pages
- L29-L32
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2015267403
- Cited by
- 347
- References
- 36
- FWCI
- 19.72
- Type
- journal article
- Language
- en
- Open access
- bronze
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