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Title:
Erratum: ``Spitzer IRS Spectroscopy of IRAS-Discovered Debris Disks'' (ApJS, 166, 351, [2006])
Authors:
Chen, C. H.; Sargent, B. A.; Bohac, C.; Kim, K. H.; Leibensperger, E.; Jura, M.; Najita, J.; Forrest, W. J.; Watson, D. M.; Sloan, G. C.; Keller, L. D.
Affiliation:
AA(), AB(), AC(), AD(), AE(), AF(), AG(), AH(), AI(), AJ(), AK()
Publication:
The Astrophysical Journal Supplement Series, Volume 177, Issue 1, pp. 417-418. (ApJS Homepage)
Publication Date:
07/2008
Origin:
UCP
DOI:
10.1086/587437
Bibliographic Code:
2008ApJS..177..417C

Abstract

After publication of our manuscript (Chen et al. [ApJS, 166, 351, (2006)]), we discovered typographical errors in Table 2. A corrected version of Table 2 is supplied here. We made typographical errors in the units for the mass of forsterite, enstatite, and silica grains. The units should be 1021, 1019, and 1019 g, respectively, instead of 1020 g as reported previously. We also mis-reported the temperature of the silicate and carbon grains in our fit to the HR 7012 IRS spectrum; the grains have a temperature 550 K, not 520 K as reported previously. Lastly, the composition of the enstatite used to fit the HR 7012 spectrum is Mg0.7Fe0.3SiO3, not Mg0.7Fe0.3SiO4. In addition, we noticed an error in the minimum blow-out size for silicate, carbon, and silica grains around HD 113766 and HR 7012; the blow-out sizes are smaller than previously estimated. For HD 113766, we originally estimated minimum silicate and carbon sizes of 1.4 and 1.9 μm, respectively; we now estimate 0.35 and 0.46 μm, respectively. With the exception of forsterite, all of the grains used to model the HD 113766 spectrum are larger than the minimum grain sizes. The forsterite grains (submicron) possess radii that are similar to the minimum silicate grain size. For HR 7012, we originally estimated minimum silicate, carbon, and silica sizes of 1.1, 1.4, and 1.6 μm, respectively; we now estimate 0.9, 1.2, and 1.3 μm, respectively. The enstatite and cristobalite grains used to model the infrared HR 7012 spectrum are still smaller than the minimum grain size. We had previously concluded that the minimum grain sizes (>1 μm) were inconsistent with presence of submicron-sized grains inferred from the structure of the silicate emission features, suggesting that a recent massive collision must have occurred around HD 113766 and HR 7012. Our new minimum grain size estimates are more consistent with our models for the infrared spectra and do not require a recent massive collision around HD 113766. However, our models do indicate the presence of submicron-sized particles significantly smaller than the blow-out size around HR 7012, suggesting that a recent massive collision may have occurred in this system.

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