Table 3
The star formation rates of NGC 4676A and NGC 4676B estimated from CALIFA and multiwavelength observations.
| Method | SFRA/ M⊙ yr-1 | SFRB/ M⊙ yr-1 |
|
|
||
| (Hα, Hβ)a | 17−35 | 3−5 |
| (Hα, mid-IR)b | 4.3−6.9 | 1.3−2.1 |
| stellar continuumc | 2.6−5 | 1−4 |
| (FUV, mid-IR)d | 6.2 | 2.3 |
| [Ne ii]e | <10.1 | <1.4 |
| (FIR, radio) f | 14 | 4 |
Notes.
Dust attenuation corrected Hα luminosity using the Balmer decrement (Sect. 6.1). The errors on the dust attenuation correction in the nucleus of NGC 4676A are likely to be significant, due to the very high dust content.
Combination of Hα and 24 μm luminosities (Smith et al. 2007).
Decomposition of the stellar continuum using starlight (Sect. 5.3).
Combination of 24 μm and FUV luminosities (Smith et al. 2010).
Mid-IR [Ne ii] emission line (Haan et al. 2011).
Combined FIR and radio continuum luminosities (Yun & Hibbard 2001).
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