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Table 11

HRS galaxies with data in the literature: fluxes normalised to Hα.

K92 This
work

HRS C(Hβ) [Oii] Hβ [Oiii] [Oiii] [Nii] Hα [Nii] [Sii] [Sii] run C(Hβ) [Oii] Hβ [Oiii] [Oiii] [Nii] Hα [Nii] [Sii] [Sii]
λ3727 λ4861 λ4959 λ5007 λ6548 λ6563 λ6584 λ6717 λ6731 λ3727 λ4861 λ4959 λ5007 λ6548 λ6563 λ6584 λ6717 λ6731

4 0.13 0.07 0.20 1 0.16
20 0.30 0.80 0.28 0.13 0.39 0.06 1 0.17 0.39
275 0.00 1.15 0.37 0.14 0.43 0.07 1 0.21 0.35
295 0.46 0.25 0.25 0.01 0.04 0.12 1 0.37 0.25

J00 This
work

HRS C(Hβ) [Oii] Hβ [Oiii] [Oiii] [Nii] Hα [Nii] [Sii] [Sii] run C(Hβ) [Oii] Hβ [Oiii] [Oiii] [Nii] Hα [Nii] [Sii] [Sii]
λ3727 λ4861 λ4959 λ5007 λ6548 λ6563 λ6584 λ6717 λ6731 λ3727 λ4861 λ4959 λ5007 λ6548 λ6563 λ6584 λ6717 λ6731

29 0.58 0.68 0.23 0.11 0.21 0.06 1 0.21 0.22 0.16 1 0.32 0.58 0.28 0.07 0.20 0.07 1 0.23 0.21 0.17
35 0.56 1
64 0.92 0.70 0.19 0.10 0.15 0.05 1 0.19 0.27 0.19
67 0.12 1.32 0.32 0.22 0.51 0.04 1 0.13 0.22 0.14 1 0.19 1.31 0.31 0.15 0.50 0.04 1 0.14 0.19 0.13
271 0.97 0.71 0.18 0.14 0.17 0.05 1 0.16 0.28 0.20

MK06 This
work

HRS C(Hβ) [Oii] Hβ [Oiii] [Oiii] [Nii] Hα [Nii] [Sii] [Sii] run C(Hβ) [Oii] Hβ [Oiii] [Oiii] [Nii] Hα [Nii] [Sii] [Sii]
λ3727 λ4861 λ4959 λ5007 λ6548 λ6563 λ6584 λ6717 λ6731 λ3727 λ4861 λ4959 λ5007 λ6548 λ6563 λ6584 λ6717 λ6731

20 0.26 0.86 0.29 0.13 0.40 0.07 1 0.21 0.20 0.13
27 0.33 0.56 0.28 0.06 0.17 0.10 1 0.31 0.19 0.13
36 0.73 0.31 0.21 0.03 0.10 0.19 1 0.59 0.19 0.15
60 0.45 0.36 0.26 0.05 0.15 0.15 1 0.45 0.21 0.16 1 1.55 0.26 0.12 0.16 0.13 1 0.47 0.18 0.15
73 0.25 0.35 0.29 0.00 0.01 0.13 1 0.39 0.17 0.09
74 0.48 0.36 0.25 0.05 0.16 0.12 1 0.37 0.18 0.13 1 0.59 0.40 0.23 0.10 0.16 0.11 1 0.35 0.15 0.11
76 0.09 0.98 0.33 0.21 0.64 0.03 1 0.10 0.19 0.10 1 0.12 1.00 0.32 0.24 0.77 0.03 1 0.11 0.15 0.12
85 0.65 0.39 0.22 0.04 0.11 0.14 1 0.43 0.21 0.14
102 0.65 0.27 0.22 0.02 0.06 0.11 1 0.34 0.14 0.09 2 0.74 0.21 0.05 0.10 1 0.32 0.13 0.09
114 0.46 0.31 0.25 0.03 0.10 0.14 1 0.41 0.14 0.11 2 0.66 0.32 0.22 0.13 0.07 0.12 1 0.39 0.15 0.10
122 1.05 0.10 0.17 0.02 0.07 0.11 1 0.33 0.09 0.05 1 0.79 0.20 0.12 1 0.36 0.08 0.06
217 2.00 0.43 0.09 0.10 0.31 0.26 1 0.77 0.37 0.21 2 0.09 1 0.57 0.15 0.17
246 0.37 0.55 0.27 0.07 0.20 0.13 1 0.38 0.24 0.18 2 0.84 0.20 0.05 0.08 0.11 1 0.37 0.18 0.11
250 0.85 0.31 0.19 0.04 0.12 0.13 1 0.38 0.20 0.16
262 0.20 0.92 0.30 0.11 0.34 0.07 1 0.22 0.21 0.14 1 0.04 1.15 0.34 0.14 0.36 0.06 1 0.20 0.20 0.13
290 0.43 0.52 0.26 0.06 0.17 0.13 1 0.35 0.26 0.17 1 0.99 0.46 0.18 0.12 0.14 0.08 1 0.29 0.19 0.14

M10 This
work

HRS C(Hβ) [Oii] Hβ [Oiii] [Oiii] [Nii] Hα [Nii] [Sii] [Sii] run C(Hβ) [Oii] Hβ [Oiii] [Oiii] [Nii] Hα [Nii] [Sii] [Sii]
λ3727 λ4861 λ4959 λ5007 λ6548 λ6563 λ6584 λ6717 λ6731 λ3727 λ4861 λ4959 λ5007 λ6548 λ6563 λ6584 λ6717 λ6731

102 1.38 0.07 0.14 0.01 0.03 0.10 1 0.29 0.12 0.08 2 0.74 0.21 0.05 0.10 1 0.32 0.13 0.09
122 1.24 0.10 0.15 0.01 0.04 0.13 1 0.39 0.14 0.10 1 0.79 0.20 0.12 1 0.36 0.08 0.06
170 1.23 0.74 0.15 0.12 0.37 0.25 1 0.76 0.43 0.31 2 0.19 1 0.47 0.20 0.20
205 1.66 0.19 0.11 0.01 0.04 0.15 1 0.44 0.25 0.19 1 1.28 0.14 0.12 0.12 1 0.37 0.20 0.16
211 1.00 1 2
217 2.25 0.22 0.07 0.05 0.16 0.32 1 0.96 0.30 0.23 2 0.09 1 0.57 0.15 0.17
220 0.93 0.74 0.18 0.13 0.38 0.44 1 1.33 0.66 0.37 2 0.20 1 0.72 0.38 0.23
263 1

Notes. 

(a)

References are K92 – Kennicutt (1992b); J00 – Jansen et al. (2000); MK06 – Moustakas & Kennicutt (2006); M10 – Moustakas et al. (2010).

(b)

For consistency with our work, the original data of Kennicutt (1992b) are corrected for the underlying Balmer absorption in Hβ (5 Å) and Hα (2.8 Å). The [Oiii]λ4959 and the [Nii]λ6548 fluxes are inferred from the [Oiii]λ5007 and the [Nii]λ6584 measurements assuming a standard ratio [Oiii]λ5007/[Oiii]λ4959 = 3 and [Nii]λ6584/[Nii]λ6548 = 3 (Osterbrock & Ferland 2005). The [Sii]λ6731 flux includes the emission of both [Sii]λ6717 and [Sii]λ6731 lines.

(c)

The original data of Jansen et al. (2000) are corrected only for the underlying Balmer absorption in Hα (2.8 Å), but not for that in Hβ given that the spectral resolution of these data, comparable to our, allows the direct measurement of the underlying absorption.

(d)

The [Oiii]λ4959 and the [Nii]λ6548 fluxes of Moustakas et al. (2010) and Moustakas & Kennicutt (2006) are inferred from the [Oiii]λ5007 and the [Nii]λ6584 measurements assuming a standard ratio [Oiii]λ5007/[Oiii]λ4959 = 3 and [Nii]λ6584/[Nii]λ6548 = 3 (Osterbrock & Ferland 2005). In the original works of Moustakas et al. (2010) and Moustakas & Kennicutt (2006) fluxes are absolute values (not normalised) representative of the whole galaxies. The galaxy HRS 211 in Moustakas et al. (2010) is detected only in the Hβ line.

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