A close look at the Centaurus A group of galaxies - II. Intermediate-age populations in early-type dwarfs

D. Crnojević; M. Rejkuba; E. K. Grebel; G. Da Costa; H. Jerjen

doi:10.1051/0004-6361/201015419

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Volume 530 (June 2011)

A&A, 530 (2011) A58

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Table 4

Magnitudes of the most luminous (in bolometric magnitude) AGB candidates for each galaxy.

Galaxy	ID	I₀	K₀	V₀ − I₀	J₀ − K₀	M_{bol, opt}	M_{bol, NIR}

CenA-dE1	420^a	23.69 ± 0.03	21.78 ± 0.11	2.20	1.58	−4.14 ± 0.18	−3.24 ± 0.24
	9323^a	23.74 ± 0.03	21.87 ± 0.20	2.32	1.65	−4.11 ± 0.18	−3.10 ± 0.25
	9248^a^b	23.66 ± 0.02	21.15 ± 0.08	1.65	1.30	−4.04 ± 0.18	−4.08 ± 0.22
	168^b	23.76 ± 0.02	21.30 ± 0.07	1.69	1.29	−3.95 ± 0.18	−3.94 ± 0.21
	329^b	23.71 ± 0.03	21.39 ± 0.07	1.62	1.36	−3.98 ± 0.18	−3.79 ± 0.22
SGC1319.1-4216	224^a	22.74 ± 0.02	21.40 ± 0.12	1.51	1.36	−4.76 ± 0.17	−3.61 ± 0.28
	1361^a^b	23.14 ± 0.02	20.08 ± 0.04	3.15	1.24	−4.75 ± 0.17	−5.05 ± 0.27
	1316^a^b	23.06 ± 0.02	19.27 ± 0.02	2.34	2.06	−4.64 ± 0.17	−5.37 ± 0.48
	1482^b	23.45 ± 0.02	20.00 ± 0.03	3.90	1.34	−4.63 ± 0.17	−5.03 ± 0.28
ESO269-066	3689^a	22.58 ± 0.01	20.15 ± 0.04	1.94	1.22	−4.89 ± 0.17	−4.86 ± 0.32
	2139^a	22.68 ± 0.01	20.24 ± 0.04	2.35	1.31	−4.89 ± 0.17	−4.58 ± 0.34
	4406^a^b	22.93 ± 0.02	19.99 ± 0.03	3.37	1.17	−4.88 ± 0.17	−5.07 ± 0.32
	3774^b	22.93 ± 0.02	19.37 ± 0.18	2.60	2.08	−4.70 ± 0.17	−5.13 ± 0.63
	3170^b	23.21 ± 0.02	19.92 ± 0.03	1.92	1.30	−4.25 ± 0.17	−5.01 ± 0.34

Notes. The columns contain: (1) galaxy name; (2) stellar ID from the combined catalog; (3) dereddened apparent I₀-band magnitude; (4) dereddened apparent K₀-band magnitude; (5) dereddened optical color; (6) dereddened NIR color; (7) absolute bolometric magnitude computed from optical values; and (8) absolute bolometric magnitude computed from NIR values. Note that the combined (ISAAC and ACS) and dereddened NIR and optical magnitudes are given with the photometric errors resulting from the photometric package.

^(a)

Among the three most luminous objects in the optical.

^(b)

Among the three most luminous objects in the NIR.

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