Table 3: Line fluxes and extinction for circumnuclear regions of spiral galaxies and starbursts.
Source Aperture a $F_{\lambda}$ b $F_{\rm H\alpha}$ b $A_{\rm V}$ c $\log[Q_{\rm Lyc}]$ d References e
  (arcsec) ( $10^{-17}~{\rm W~m^{-2}}$) ( $10^{-16}~{\rm W~m^{-2}}$) (mag) ( $\log[{\rm s^{-1}}]$)  
Circumnuclear regions of spiral galaxies
NGC 986 23.6, $4 \times 4$ ... 10.2 2.5 53.57 1, 2
NGC 1097 45 ... 39.2 1.9 53.55 3, 4
NGC 1365 40.0, 23.5 Br$\gamma$: 19.6 35.8, 28.4 2.9 53.95 5, 6
NGC 4102 starburst Pa$\beta$/Br$\gamma$: 12.1/6.0 ... 7.2 53.55 7
NGC 4293 32.4 Pa$\alpha$: 10.7 0.76 3.8 52.59 8, 9
NGC 4691 56.5, 23.5 Br$\gamma$: 3.76 8.59, 7.18 2.4 53.45 10, 11
NGC 5194 90 ... 38.6 2.8 53.29 12, 13
NGC 5236 41.2, 23.5 Br$\gamma$: 19.6 75.7, 60.6 1.7 52.79 5, 14
NGC 6946 35.3, 23.5 Br$\gamma$: 6.1 8.64, 5.80 3.5 52.58 5, 15
NGC 7552 21.8, $14 \times 20$ Br$\alpha$: 44.0 30.3, 29.4 2.1 53.75 1, 16
NGC 7771 starburst ring Pa$\beta$/Br$\gamma$: 4.0/1.5 ... 5.2 53.91 17
Starburst galaxies
NGC 253 15, $2.4 \times 12$ Br$\gamma$: 91.6 ... 8.5 53.13 18
NGC 520 17.7, $6 \times 8$ Br$\gamma$: 1.9 0.52, 0.15 7.4 54.03 19, 20
NGC 1808 20 (total) Br$\gamma$: 31.0 ... 4 53.72 21
NGC 3034 30.0 ... ... 52 (MIX) $^{\dagger}$ 54.09 22
IC 342 $17 \times 17$, $14 \times 20$ Br$\gamma$: 17.0; Br$\alpha$: 70.0 ... 5.2 $^{\dagger}$ 52.48 16, 23
LIRGs/ULIRGs
NGC 3256 $\approx$20 (total), $3.5\hbox{$^{\prime\prime}$ }\times 3.5\hbox{$^{\prime\prime}$ }$ Br$\gamma$: 15.0 ... 5.3 54.54 24, 25
NGC 6240 total Br$\gamma$: 3.1; Pa$\beta$: 4.1 ... 10.1 54.91 26, 27
IRAS 23128-5919 total, S. nucleus Pa$\alpha$: 8.0 1.76, 0.93 3.0 54.74 28, 29
Arp 220 total Br$\alpha$: 21.0; Br$\gamma$: 0.59 ... 40.1 $^{\dagger}$ 55.33 30, 31
a
Rectangular dimensions or diameter of the photometric aperture. When two values are given, the first one refers to the primary flux (H$\alpha$ when present) and the second one to the hydrogen line decrement used to estimate the extinction. The aperture adopted for the size normalization is given in Table 2.
b
Observed line fluxes used to derive the extinction and/or the ionizing photon flux. When two H$\alpha$ fluxes are given, they correspond to the two apertures used for photometry and extinction estimation, respectively.
c
Derived or adopted extinction for a uniform foreground screen (UFS) model except when "MIX'' indicates that a homogeneous mixture of dust and sources is assumed.
d
Derived or adopted intrinsic Lyman continuum photon rate.
e
References for line fluxes and extinction values (further details are given on the derivation of the data in appendix A): (1) H$\alpha$+[N II] map from Hameed & Devereux (1999) (in NED); (2) Extinction from H$\beta$/H$\alpha$ of Véron-Cetty & Véron (1986) in $4\hbox{$^{\prime\prime}$ }\times 4\hbox{$^{\prime\prime}$ }$; (3) H$\alpha$+[N II] map graciously provided by T. Storchi-Bergmann (Storchi-Bergman et al. 1996); (4) Average extinction along the starburst ring derived from the data of Kotilainen et al. (2000); (5) Br$\gamma$ flux from Puxley et al. (1988) in an effective aperture of 23.5 $^{\prime\prime}$; (6) H$\alpha$+[N II] map graciously provided by M. Naslund (Kristen et al. 1997; Lindblad 1999); (7) Br$\gamma$ and Pa$\beta$ fluxes from Roussel et al. (2003)  in $\approx$ $5\hbox{$^{\prime\prime}$ }\times 5\hbox{$^{\prime\prime}$ }$ (most of starburst enclosed); (8) Pa$\alpha$ map from Böker et al. (1999) (in NED); (9) H$\alpha$+[N II] map from Koopmann et al. (2001) (in NED); (10) Br$\gamma$ flux from Puxley et al. (1990) in an effective aperture of 23.5 $^{\prime\prime}$; (11) H$\alpha$+[N II] map graciously provided by A. García-Barreto (García-Barreto et al. 1995); (12) H$\alpha$+[N II] map from Greenawalt et al. (1998); (13) Average extinction towards H II regions from Scoville et al. (2001); (14) H$\alpha$ map graciously provided by S. Ryder via A. Vogler (Ryder et al. 1995); (15) H$\alpha$ map from Larsen & Richtler (1999) (in NED); (16) Br$\alpha$ flux from Verma et al. (2003) in $14\hbox{$^{\prime\prime}$ }\times 20\hbox{$^{\prime\prime}$ }$; (17) Br$\gamma$ and Pa$\beta$ fluxes from Dale et al. (2004) in $\approx$ $5\hbox{$^{\prime\prime}$ }\times 5\hbox{$^{\prime\prime}$ }$ (most of starburst ring enclosed); (18) Br$\gamma$ flux and extinction from Engelbracht et al. (1998); (19) Br$\gamma$ flux from Stanford (1991) in $6\hbox{$^{\prime\prime}$ }\times 8\hbox{$^{\prime\prime}$ }$; (20) H$\alpha$+[N II] map from Hibbard & van Gorkom (1996) (in NED); (21) Br$\gamma$ flux and extinction from Krabbe et al. (1994); (22) Extinction and $Q_{\rm Lyc}$ from Förster Schreiber et al. (2001); (23) Br$\gamma$ map provided by Böker (Böker et al. 1997); (24) Total Br$\gamma$ flux from Moorwood & Oliva (1994); (25) Extinction from Br$\gamma$/Pa$\beta$ of Doyon et al. (1994) in $3.5\hbox{$^{\prime\prime}$ }\times 3.5\hbox{$^{\prime\prime}$ }$; (26) Br$\gamma$ flux from Rieke et al. (1985) in 8.7 $^{\prime\prime}$; (27) Pa$\beta$ flux from Simpson et al. (1996) in a slit of width 1.5 $^{\prime\prime}$; (28) Pa$\alpha$ flux of the southern nucleus from Kawara et al. (1987); (29) H$\alpha$ fluxes of both nuclei form Duc et al. (1997) in a slit of width 1.3 $^{\prime\prime}$; (30) Br$\alpha$ flux from Sturm et al. (1996) in $14\hbox{$^{\prime\prime}$ }\times 20\hbox{$^{\prime\prime}$ }$; (31) Br$\gamma$ flux of Goldader et al. (1995) in a slit of width 0.75 $^{\prime\prime}$.
$^{\dagger}$
Values are for the GC extinction law of Lutz (1999a) when we made use of the Br$\alpha$ line at 4.05 $\mu $m (see Sect. 3.2).


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