Linking dust emission to fundamental properties in galaxies: the low-metallicity picture

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Volume 582 (October 2015)

A&A, 582 (2015) A121

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Table 7

WISE flux densities for the DGS sample.

Source	F _3.4	F _4.6	F ₁₂	F ₂₂	Aperture radius
	[mJy]	[mJy]	[mJy]	[mJy]	[′′]


Haro11	17.9 ± 1.9	32.6 ± 3.4	353. ± 19.	2054. ± 148.	45^a, 90^b
Haro2	24.5 ± 2.6	16.5 ± 1.7	152. ± 8.	760. ± 55.	50^a, 65^b
Haro3	25.8 ± 2.7	17.7 ± 1.9	162. ± 9.	766. ± 56.	60^a
He2-10	133. ± 17.	92.7 ± 11.2	996. ± 53.	5018. ± 362.	81^b
HS0017+1055	0.16 ± 0.03	0.25 ± 0.04	3.83 ± 0.49	11.7 ± 2.0	12^a, 25^b
HS0052+2536	0.65 ± 0.08	0.52 ± 0.07	3.71 ± 0.40	16.2 ± 2.3	17^a, 23^a
HS0822+3542	0.106 ± 0.009^c	0.082 ± 0.008^c	≤0.47^c	≤3.85^c	–
HS1222+3741	0.15 ± 0.03	0.15 ± 0.03	1.0 ± 0.2^c	5.94 ± 0.73^c	14^a, –
HS1236+3937	0.22 ± 0.05	0.16 ± 0.04	≤0.65	≤2.72	15^a
HS1304+3529	0.4 ± 0.1	0.43 ± 0.09	1.78 ± 0.21^c	10.5 ± 0.9^c	18^a, –
HS1319+3224	0.06 ± 0.02	0.07 ± 0.02	≤0.70^c	≤1.93^c	12^b, –
HS1330+3651	0.51 ± 0.07	0.36 ± 0.07	1.23 ± 0.26	5.31 ± 1.26	20^a
HS1442+4250	1.20 ± 0.14	0.8 ± 0.1	1.54 ± 0.33	≤9.40	32^b
HS2352+2733	0.15 ± 0.04	0.13 ± 0.04	≤1.03^c	≤2.98^c	15^a, –
IZw18	0.33 ± 0.07	0.39 ± 0.07	0.8 ± 0.3	4.64 ± 1.19	23^b
IC 10	1454. ± 154.	917. ± 98.	3521. ± 191.	9991. ± 728.	205 × 150^b, 230^b
IIZw40	18.6 ± 2.0	19.3 ± 2.1	335. ± 18.	1540. ± 112.	45 × 33^a, 90^b
Mrk 1089	19.0 ± 2.3	13.9 ± 3.1	102. ± 6.	453. ± 34.	75^a
Mrk 1450	1.10 ± 0.12	0.73 ± 0.09	8.00 ± 0.74	49.3 ± 4.8	20^a, 40^b
Mrk 153	2.03 ± 0.23	1.34 ± 0.17	4.61 ± 0.41	28.1 ± 3.9	25^a
Mrk 209	2.61 ± 0.39	1.70 ± 0.31	7.30 ± 0.85	46.4 ± 5.4	39^a
Mrk 930	2.61 ± 0.30	2.26 ± 0.27	25.8 ± 2.6	170. ± 14.	34^b, 60^a
NGC 1140	32.7 ± 3.5	21.6 ± 2.3	94.9 ± 5.5	367. ± 28.	118^a
NGC 1569	359. ± 24.	240. ± 47.	1021. ± 116.	6971. ± 503.	120^b
NGC 1705	25.7 ± 2.7	16.1 ± 1.7	20.3 ± 1.5	46.2 ± 6.1	75 × 46^b, 72^a
NGC 2366	75.8 ± 5.7	39.4 ± 6.2	121. ± 12.	612. ± 65.	260 × 125^b, 150^a
NGC 4214	294. ± 31.	184. ± 19.	546. ± 29.	1830. ± 133.	181^a
NGC 4449	483. ± 50.	307. ± 32.	1323.8 ± 70.0	3119. ± 227.	190 × 170^a, 250^a
NGC 4861	18.1 ± 1.1	10.1 ± 1.9	52.8 ± 5.7	330. ± 26.	120 × 50^b, 120^a
NGC 5253	212. ± 22.	255. ± 27.	2002. ± 105.	10345. ± 746.	120 × 80^b, 120^a
NGC 625	106. ± 11.	64.7 ± 6.8	194. ± 11.	797. ± 59.	200 × 75
NGC 6822^d	–	–	–	–	–
Pox186	≤0.34	≤0.44	2.67 ± 0.33	11.2 ± 1.4	25^b
SBS0335-052	0.45 ± 0.05	1.45 ± 0.16	23.4 ± 1.4	67.8 ± 5.8	14^b, 35^b
SBS1159+545	≤0.09	≤0.11	1.0 ± 0.3	4.44 ± 1.38	12^a, 25^b
SBS1211+540	0.133 ± 0.009	0.10 ± 0.03	≤0.80	≤3.60	15^a
SBS1249+493	≤0.05^c	≤0.07^c	≤1.17	≤3.76	-, 20^b
SBS1415+437	0.8 ± 0.1	0.53 ± 0.08	2.30 ± 0.55	15.5 ± 2.8	28 × 15^b, 34^a
SBS1533+574	1.52 ± 0.19	1.28 ± 0.17	9.76 ± 0.84	53.3 ± 4.7	30^a, 50^b
Tol0618-402	2.33 ± 0.33	1.32 ± 0.21	≤0.71	≤1.73	18^a
Tol1214-277	≤0.13	≤0.14	0.8 ± 0.2^c	≤6.89^c	12^a, –
UGC 4483	1.12 ± 0.26	≤1.01	≤2.30	≤12.72	43 × 24
UGCA 20	0.26 ± 0.08	≤0.24	≤0.74	≤3.27	20^a
UM133	≤10.83	≤6.74	≤1.49	≤6.70	26^a
UM311	48.5 ± 3.0	29.1 ± 3.5	120. ± 7.	292. ± 25.	115^a
UM448	15.4 ± 1.6	11.7 ± 1.3	103. ± 6.	552. ± 40.	64^a
UM461	0.58 ± 0.07	0.52 ± 0.07	5.98 ± 1.02	29.4 ± 4.9	17^a, 35^b
VIIZw403	2.59 ± 0.29	1.89 ± 0.23	4.54 ± 0.61	26.3 ± 3.6	40^a

Notes. In the aperture column, a single value indicates that only one aperture has been used for the four wavelengths. Two values separated by a comma indicate that a different aperture has been used for WISE1 and WISE2 on one side (first value), and WISE3 and WISE4 on the other side (second value, see text for details). For several galaxies elliptical apertures were used to match the morphology of the source and are indicated by semi-major axis × semi-minor axis. A dash indicates that we take the profile fit photometry from the All WISE database.

^(a)

The aperture is the same as that used for IRAC or Herschel photometry.

^(b)

The aperture has been adapted to match the peculiar morphology of the source in the NIR/MIR or to avoid a contaminating source.

^(c)

This galaxy is not resolved at these wavelengths and we thus use the profile fit photometry provided by the WISE database.

^(d)

The WISE map does not cover the full galaxy. Thus we do not report flux densities for this source.

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