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Home All issues Volume 517 (July 2010) A&A, 517 (2010) A85 Full HTML
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Table 1:

Compilation of the broad-band photometric dataa for the individual galaxies analysed in this work.

Galaxy 		E(B-V) $M_B^{\rm NC}$ MB U-B B-V V-R V-J J-H H-Ks B. Age UC Age
  (a) (b) (c) (d) (d) (d) (d) (d) d) (e) (f)
HCG 31 AC 0.06 -19.18 -19.43 $-0.60 \pm 0.06$ $0.03 \pm 0.08$ $0.12 \pm 0.08$ $0.20 \pm 0.10$ $0.13 \pm 0.10$ $0.15 \pm 0.12$ 5.0 100
HCG 31 B 0.18 -17.96 -18.71 $-0.38 \pm 0.08$ $0.17 \pm 0.06$ $0.06 \pm 0.06$ $0.14 \pm 0.10$ $0.13 \pm 0.10$ $0.12 \pm 0.10$ 7.0 100
HCG 31 E 0.06 -15.51 -15.76 $-0.65 \pm 0.10$ $-0.03 \pm 0.10$ $0.20 \pm 0.09$ $0.29 \pm 0.12$ $0.05 \pm 0.10$ $0.18 \pm 0.12$ 6.0 -
HCG 31 F1 0.20 -14.93 -15.76 $-0.99 \pm 0.12$ $-0.07 \pm 0.12$ $-0.04 \pm 0.10$ $-0.17 \pm 0.14$ $0.04 \pm 0.17$ $0.29 \pm 0.30$ 2.5 0
HCG 31 F2 0.09 -13.97 -14.34 $-1.01 \pm 0.12$ $-0.09\pm0.12$ $-0.02 \pm 0.10$ $0.01 \pm 0.16$ $0.08 \pm 0.30$ $0.20 \pm 0.50$ 2.5 0
HCG 31 G 0.06 -18.63 -18.88 $-0.43 \pm 0.09$ $-0.01 \pm 0.08$ $0.14 \pm 0.08$ $0.45 \pm 0.08$ $0.12 \pm 0.10$ $0.13 \pm 0.10$ 6.0 100
Mkn 1087 0.17 -21.45 -22.15 $-0.41 \pm 0.08$ $0.17 \pm 0.08$ $0.20 \pm 0.08$ $0.52 \pm 0.06$ $0.20 \pm 0.06$ $0.16 \pm 0.06$ 6.0 100
Mkn 1087 N 0.10 -17.65 -18.06 ... $-0.05 \pm 0.06$ $0.14 \pm 0.10$ $0.21 \pm 0.08$ $0.18 \pm 0.08$ $0.13 \pm 0.08$ 7.0 -
Mkn 1087 #1 0.07g -16.05 -16.34 $-0.75 \pm 0.15$ $-0.01 \pm 0.10$ $0.10 \pm 0.08$ ... ... ... 6.0 -
Mkn 1087 #3 0.07g -16.91 -17.20 $0.08 \pm 0.30$ $0.11 \pm 0.06$ $0.26 \pm 0.06$ $0.64 \pm 0.10$ $0.50 \pm 0.20$ ... - 150
Haro 15 0.11 -20.41 -20.87 $-0.52 \pm 0.08$ $0.26 \pm 0.08$ $0.32 \pm 0.08$ $0.17 \pm 0.08$ $0.58 \pm 0.08$ $0.22 \pm 0.08$ 5.0 500
Mkn 1199 0.15 -20.06 -20.68 $-0.44 \pm 0.06$ $0.46 \pm 0.06$ $0.29 \pm 0.06$ $1.30 \pm 0.07$ $0.55 \pm 0.08$ $0.34 \pm 0.08$ 8.0 500
Mkn 1199 NE 0.11 -17.11 -17.57 $0.16 \pm 0.08$ $0.51 \pm 0.08$ $0.34 \pm 0.08$ $1.29 \pm 0.08$ $0.62 \pm 0.10$ $0.20 \pm 0.10$ 12.0 500
Mkn 5 0.20 -14.74 -15.57 $-0.41 \pm 0.06$ $0.44 \pm 0.06$ $0.30 \pm 0.06$ 0.81: $0.52 \pm 0.03$ $0.38 \pm 0.04$ 5.0 500
IRAS 08208+2816 0.17 -20.59 -21.29 $-0.49 \pm 0.06$ $0.22 \pm 0.06$ $0.35 \pm 0.08$ $1.03 \pm 0.08$ $0.54 \pm 0.08$ $0.22 \pm 0.10$ 5.5 500
IRAS 08339+6517 0.16 -20.91 -21.57 $-0.51 \pm 0.08$ $0.01 \pm 0.08$ $0.26 \pm 0.08$ $1.36 \pm 0.06$ $0.64 \pm 0.05$ $0.23 \pm 0.06$ 4.5 150
IRAS 08339+6517 C 0.13 -17.67 -18.21 $-0.16 \pm 0.10$ $0.20 \pm 0.08$ $0.26 \pm 0.08$ $1.45 \pm 0.12$ $0.21 \pm 0.25$ $0.68 \pm 0.28$ 5.5 250
POX 4 0.06 -18.54 -18.79 $-0.68 \pm 0.03$ $0.29 \pm 0.02$ $0.32 \pm 0.04$ $0.42 \pm 0.08$ $0.28 \pm 0.08$ $0.15 \pm 0.10$ 3.5 250
POX 4 Comp 0.12 -14.86 -15.36 $-0.02 \pm 0.06$ $0.25 \pm 0.02$ $0.30 \pm 0.04$ $0.87 \pm 0.10$ 0.7: 0.3: 5.0 300
UM 420 0.06 -19.30 -19.55 $-0.80 \pm 0.06$ $0.31 \pm 0.06$ $0.13 \pm 0.06$ $0.77 \pm 0.12$ $0.41 \pm 0.12$ $0.12 \pm 0.16$ 4.5 200
SBS 0926+606 A 0.08 -16.96 -17.29 $-0.75 \pm 0.06$ $0.01 \pm 0.06$ $0.14 \pm 0.06$ $0.54 \pm 0.06$ $0.21 \pm 0.06$ $0.15 \pm 0.08$ 4.8 200
SBS 0926+606 B 0.12 -16.87 -17.37 $-0.51 \pm 0.08$ $0.08 \pm 0.06$ $0.20 \pm 0.06$ $0.83 \pm 0.06$ $0.29 \pm 0.06$ $0.18 \pm 0.08$ 6.7 100
SBS 0948+532 0.24 -17.44 -18.43 $-1.20 \pm 0.06$ $-0.12 \pm 0.06$ $0.16 \pm 0.06$ ... ... ... 4.6 100
SBS 1054+365 0.02 -13.98 -14.06 $-0.34 \pm 0.06$ $0.33 \pm 0.06$ ... $0.92 \pm 0.08$ $0.38 \pm 0.12$ $0.16 \pm 0.15$ 4.9 500
SBS 1211+540 0.08 -12.94 -13.27 $-0.61 \pm 0.06$ $0.04 \pm 0.06$ $0.21 \pm 0.06$ ... ... ... 4.7 500
SBS 1319+579 0.02 -18.45 -18.53 $-0.39 \pm 0.06$ $0.34 \pm 0.06$ $0.19 \pm 0.06$ $1.03 \pm 0.08$ $0.39 \pm 0.12$ $0.16 \pm 0.20$ 3.7 300
SBS 1415+437 0.13 -14.09 -14.52 $-0.47 \pm 0.06$ $0.21 \pm 0.06$ $0.27 \pm 0.06$ $0.98 \pm 0.08$ $0.35 \pm 0.10$ 0.15: 3.6 250
III Zw 107 0.21 -19.27 -20.14 $-0.42 \pm 0.06$ $0.14 \pm 0.06$ $0.22 \pm 0.06$ $0.62 \pm 0.12$ $0.47 \pm 0.20$ 0.35$\pm$0.20 5.6 500
Tol 9 0.31 -17.98 -19.26 $-0.34 \pm 0.06$ $0.24 \pm 0.06$ $0.22 \pm 0.06$ $0.83 \pm 0.08$ $0.68 \pm 0.10$ $0.27 \pm 0.12$ 5.8 500
Tol 1457-262 Obj1 0.16 -19.07 -19.73 $-0.56 \pm 0.06$ $0.23 \pm 0.06$ $0.26 \pm 0.06$ $0.60 \pm 0.10$ $0.51 \pm 0.12$ $0.22 \pm 0.12$ 4.6 500
Tol 1457-262 Obj2 0.16g -18.31 -18.97 $-0.42 \pm 0.06$ $0.34 \pm 0.06$ $0.36 \pm 0.06$ $0.90 \pm 0.10$ $0.58 \pm 0.12$ $0.27 \pm 0.14$ 5.2 500
Tol 1457-262 #15 0.16g -15.82 -16.48 $-0.25 \pm 0.10$ $0.39 \pm 0.08$ $0.39 \pm 0.06$ $1.10 \pm 0.20$ ... ... 6.4 400
Tol 1457-262 #16 0.16g -14.03 -14.69 $-0.10 \pm 0.15$ $0.45 \pm 0.10$ $0.40 \pm 0.06$ ... ... ... 7.0 500
ESO 566-8 0.34 -19.47 -20.88 $-0.48 \pm 0.06$ $0.31 \pm 0.06$ $0.19 \pm 0.06$ $1.10 \pm 0.10$ $0.60 \pm 0.12$ $0.38 \pm 0.14$ 4.2 500
ESO 566-7 0.16 -18.69 -19.35 $-0.21 \pm 0.08$ $0.49 \pm 0.06$ $0.31 \pm 0.06$ $1.20 \pm 0.10$ $0.71 \pm 0.16$ $0.34 \pm 0.16$ 4.2 500
NGC 5253h 0.17 -17.23 -17.92 $-0.41 \pm 0.02$ $0.27 \pm 0.02$ $0.21 \pm 0.02$ $0.81 \pm 0.03$ $0.53 \pm 0.04$ $0.19 \pm 0.05$ 3.5 300

Notes.  (a) Colour excess, E(B-V), derived from our estimates of the reddening coefficient and assuming RV=3.1, E(B-V)=0.692c(H$\beta $). (b) Absolute B-magnitude, not corrected for extinction. (c) Extinction-corrected absolute B-magnitude, assuming $M_B = M_B^{\rm NC} - A_B = M_B^{\rm NC} - 3.1\times 1.337 E(B-V) = M_B^{\rm NC} - 2.868$ c(H$\beta $). (d) All colours have been corrected for both extinction and emission of the gas, see López-Sánchez, Esteban (2008). (e) Age of the most recent star-forming burst (derived using the H$\alpha $ equivalent width), in Myr. (f) Minimum age of the underlying stellar population (derived via the analysis of the low-luminosity component of the galaxy), in Myr. (g) E(B-V) was estimated only considering the extinction of the Milky Way. (h) Optical and NIR magnitudes extracted from the NED and corrected for extinction using an average value of c(H$\beta $)= 0.24, see López-Sánchez et al. (2007).




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