Revealing the cold dust in low-metallicity environments - I. Photometry analysis of the Dwarf Galaxy Survey with Herschel

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Volume 557 (September 2013)

A&A, 557 (2013) A95

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This article has an erratum: [https://doi.org/10.1051/0004-6361/201321602e]

Table 2

PACS flux densities for the DGS galaxies.

Source	F₇₀ (Jy)	σ₇₀ (Jy)	F₁₀₀ (Jy)	σ₁₀₀ (Jy)	F₁₆₀ (Jy)	σ₁₆₀ (Jy)	Method	Circular aperture radius (′′)

Haro 11	6.14	0.31	4.96	0.25	2.42	0.12	Scanamorphos	45^b
Haro 2	4.99	0.25	5.33	0.27	3.95	0.20	Scanamorphos	50^a
Haro 3	5.30	0.26	6.41	0.32	4.83	0.24	Scanamorphos	60^a
He 2-10	25.6	1.3	26.6	1.3	18.8	0.9	Scanamorphos	108^a
HS 0017+1055	0.046	0.005	0.033	0.004	0.019	0.004	PhotProject	16^b
HS 0052+2536	0.22	0.01	0.21	0.01	0.139	0.008	PhotProject	23^a,f
HS 0822+3542	≤0.014^j	−	≤0.013^j	−	0.034	0.003	PhotProject	12^a
HS 1222+3741	0.025	0.004	≤0.036	−	≤0.022	−	PhotProject	14^b
HS 1236+3937	≤0.029	−	≤0.035	−	≤0.028	−	PhotProject	15^a
HS 1304+3529	0.121	0.007	0.150	0.009	0.069	0.005	PhotProject	18^b
HS 1319+3224	0.012	0.003	0.013	0.002	≤0.015	−	PhotProject	8^b
HS 1330+3651	0.093	0.006	0.112	0.007	0.091	0.005	PhotProject	20^b
HS 1442+4250	0.09	0.01	≤0.016	−	≤0.047	−	PhotProject	51^a
HS 2352+2733	0.039	0.003	0.016	0.002	≤0.016	−	PhotProject	15^a
I Zw 18	0.045	0.003	0.018	0.002	≤0.011	−	PhotProject	14^a
IC 10	140.	7.	207.	10.	225.	11.	Scanamorphos	306^a
II Zw 40	6.39	0.32	5.79	0.29	3.53	0.18	Scanamorphos	66^b
Mrk 1089	4.27	0.21	4.97	0.25	4.68	0.23	Scanamorphos	75^b,f
Mrk 1450	0.30	0.02	0.25	0.01	0.127	0.007	PhotProject	20^a
Mrk 153	0.28	0.02	0.30	0.02	0.137	0.009	PhotProject	35^b
Mrk 209	0.32	0.02	0.35	0.02	0.16	0.01	Scanamorphos	24^c
Mrk 930	1.19	0.06	1.40	0.07	0.98	0.05	Scanamorphos	60^b
NGC 1140	4.04	0.20	4.62	0.23	4.58	0.23	Scanamorphos	118^b
NGC 1569	60.4	3.0	57.3	2.9	39.7	2.0	Scanamorphos	150^d
NGC 1705	1.37	0.07	1.46	0.07	1.10	0.06	PhotProject ^g	72^d
NGC 2366	5.30	0.26	6.23	0.31	4.08	0.20	Scanamorphos	150^d,e
NGC 4214	24.5	1.2	32.2	1.6	33.7	1.7	Scanamorphos	300^d
NGC 4449	49.3	2.5	75.9	3.8	79.5	4.0	Scanamorphos	250^d
NGC 4861	2.31	0.12	2.17	0.11	1.99	0.10	Scanamorphos	120^d
NGC 5253	32.9	1.6	32.3	1.6	23.2	1.2	Scanamorphos	120^d
NGC 625	6.49	0.32	9.47	0.47	8.20	0.41	Scanamorphos	170^d
NGC 6822	54.9	2.8	63.6	3.2	77.1	3.9	Scanamorphos	440^d
Pox 186	0.038^j	0.005	0.052^j	0.005	0.047^j	0.004	PhotProject	16^a
SBS 0335-052	0.056	0.004	0.024^h	0.001	0.007^h	0.001	PhotProject	10^a,h
SBS 1159+545	0.019	0.003	0.019	0.003	≤0.018	−	PhotProject	8^a
SBS 1211+540	0.034	0.003	0.018	0.002	0.013	0.002	PhotProject	15^b
SBS 1249+493	0.032	0.005	≤0.034	−	≤0.042	−	PhotProject	12^b
SBS 1415+437	0.18	0.01	0.16	0.01	0.065	0.007	PhotProject	34^a
SBS 1533+574	0.19	0.01	0.24	0.01	0.19	0.01	Scanamorphos	30^a
Tol 0618-402	≤0.014	−	≤0.005	−	≤0.013	−	PhotProject	18^a
Tol 1214-277	0.017	0.003	0.018	0.002	≤0.018	−	PhotProject	12^b
UGC 4483	0.16	0.02	−ⁱ	−ⁱ	≤0.037	−	PhotProject	63^a
UGCA 20	≤0.052	−	≤0.057	−	≤0.048	−	PhotProject	20^c
UM 133	0.15^j	0.01	0.066	0.010	0.053	0.009	Scanamorphos	26^c
UM 311	2.94	0.15	5.63	0.28	6.10	0.31	Scanamorphos	140^b,f
UM 448	5.17	0.26	−	−	3.22	0.17	Scanamorphos	64^b
UM 461	0.21^j	0.01	0.145	0.009	0.113	0.007	PhotProject	17^b
VII Zw 403	0.47	0.03	0.56	0.03	0.34	0.02	PhotProject	40^c

Notes. The map making method is indicated for each galaxy as well as the radius of the circular aperture used for the flux extraction. When an upper limit is given, it is the 5σ upper limit computed in 3.1.3.

^(a,b,c)

The radius is:

^(a)

1.5 times the optical radius.

^(b)

Larger than 1.5 times the optical radius.

^(c)

Smaller than 1.5 times the optical radius.

^(d,e)

The aperture is:

^(d)

Adapted from elliptical shape.

^(e)

Off-centred to match the particular shape of the galaxy.

^(f)

These objects are galaxies within compact groups of galaxies or are parts of other galaxies and the photometry given here is for the whole group (see Sect. 3.1.1 for details).

^(g)

The Scanamorphos maps of NGC 1705 are not satisfactory because of a non-uniform background. Therefore we use the PhotProject maps. To preserve as much of the diffuse extended emission as possible we manually mask out the galaxy before performing the high pass filtering step.

^(h)

New observations were obtained for SBS 0335-052 at 100 and 160 μm with longer integration times (Sauvage et al., in prep). We chose to quote the flux density values from the newest observations for 100 and 160 μm.

⁽ⁱ⁾

Interferences on the detector are strongly polluting the map for the 100 μm observation of UGC 4483. We thus do not report any flux density nor give any 100 μm map for this galaxy.

^(j)

These flux densities might present some discrepancies with other FIR measurements (i.e. MIPS, other PACS and/or SPIRE wavelengths).

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