A close look at the Centaurus A group of galaxies - IV. Recent star formation histories of late-type dwarfs around CenA

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Volume 541 (May 2012)

A&A, 541 (2012) A131

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Table 2

Star formation parameters and metallicity derived for the studied galaxies.

Galaxy	⟨ SFR ⟩	b₁₀₀	b₅₀₀	b_1G	b_14G	f_1G	f_4G	f_14G	⟨ [Fe/H] ⟩	M_star^a
	(10^-2 M_⊙ yr^-1)								(dex)	(10⁷ M_⊙)

HIPASS J1348-37	0.14 ± 0.05	1.56	1.78	1.73	0.88	0.12	0.28	0.60	−1.50 ± 0.07
KK196, AM1318-444	0.20 ± 0.11	−	0.99	0.66	1.04	0.07	0.19	0.74	−1.43 ± 0.25
KK182, Cen6	0.10 ± 0.14	5.72	6.78	3.37	0.85	0.24	0.35	0.41	−1.46 ± 0.21
ESO384-16	0.60 ± 0.23	0.14	0.54	0.37	1.09	0.03	0.27	0.70	−0.97 ± 0.15
ESO269-58	6.79 ± 3.93	0.12	0.31	0.21	1.11	0.01	0.22	0.76	−0.98 ± 0.20

Notes. The columns are the following: Col. (1): name of the galaxy (ordered by increasing absolute magnitude); (2) average SFR over the whole lifetime; (3) b₁₀₀; (4) b₅₀₀; (5) b_1G; (6) b_14G; (7) f_1G; (8) f_4G; (9) f_14G; (10) average metallicity over the whole lifetime; and (11): stellar mass as integrated from our best-fit SFH (). The b parameter is the ratio of star formation rate over the indicated time period (0.1, 0.5, 1 and from 1 to 14 Gyr respectively) to the average star formation over the whole lifetime; the f parameter is the fraction of stars born in a certain time interval (0–1, 1–4 and 4–14 Gyr). In a hypothetical galaxy with constant star formation rate, f_1G = 0.07, f_4G = 0.36 and f_14G = 0.57.

^(a)

note that these are possible lower limits because of incomplete spatial coverage; moreover, these estimates depend on the modeling details, and do not take into account stars that already ended their lives

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