“BC03”的版本间差异
无编辑摘要 |
无编辑摘要 |
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| （未显示同一用户的1个中间版本） | |||
| 第2行： | 第2行： | ||
:AIR = VAC / (1.0 + 2.735182E-4 + 131.4182 / VAC^2 + 2.76249E8 / VAC^4) |
:AIR = VAC / (1.0 + 2.735182E-4 + 131.4182 / VAC^2 + 2.76249E8 / VAC^4) |
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:AIRTOVAC可转换 |
:AIRTOVAC可转换 |
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*3323-9301 |
*3323-9301采样率1A，分辨率3A（FWHM） |
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* http://www.bruzual.org/bc03/doc/bc03.pdf |
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*As noted by Asari et al. (2007), the Bruzual & Charlot (2003) models have a low amplitude hump in the ∼100 Å interval around |
*As noted by Asari et al. (2007), the Bruzual & Charlot (2003) models have a low amplitude hump in the ∼100 Å interval around |
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Hβ, such that Hβ emission often sits in a slightly negative valley in the observed minus model spectrum (an artefact of the STELIB |
Hβ, such that Hβ emission often sits in a slightly negative valley in the observed minus model spectrum (an artefact of the STELIB |
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library, which disappears when using models based on the MILES library of Sanchez-Bl ´ azquez et al. 2006). Asari et al. (2007) found ´ |
library, which disappears when using models based on the [[MILES]] library of Sanchez-Bl ´ azquez et al. 2006). Asari et al. (2007) found ´ |
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this effect to be unimportant for their Hβ measurements, but their analysis focused on SF galaxies, which tend to have strong Hβ. Here |
this effect to be unimportant for their Hβ measurements, but their analysis focused on SF galaxies, which tend to have strong Hβ. Here |
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it has a larger impact, since we are specifically interested in galaxies with intrinsically weak Hβ. To alleviate this problem, the Hβ flux |
it has a larger impact, since we are specifically interested in galaxies with intrinsically weak Hβ. To alleviate this problem, the Hβ flux |
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2024年6月30日 (日) 09:14的最新版本
- AIR 波长，SDSS的谱是真空波长
- AIR = VAC / (1.0 + 2.735182E-4 + 131.4182 / VAC^2 + 2.76249E8 / VAC^4)
- AIRTOVAC可转换
- 3323-9301采样率1A，分辨率3A（FWHM）
- http://www.bruzual.org/bc03/doc/bc03.pdf
- As noted by Asari et al. (2007), the Bruzual & Charlot (2003) models have a low amplitude hump in the ∼100 Å interval around
Hβ, such that Hβ emission often sits in a slightly negative valley in the observed minus model spectrum (an artefact of the STELIB library, which disappears when using models based on the MILES library of Sanchez-Bl ´ azquez et al. 2006). Asari et al. (2007) found ´ this effect to be unimportant for their Hβ measurements, but their analysis focused on SF galaxies, which tend to have strong Hβ. Here it has a larger impact, since we are specifically interested in galaxies with intrinsically weak Hβ. To alleviate this problem, the Hβ flux measurements were performed with respect to a local ‘continuum’ in the residual spectrum. No such systematic residual is found for other emission lines, whose measurement does not require the extra care devoted to Hβ.