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 B.1

DGS Spitzer/IRAC and IRS observing Log.

	IRAC	IRS

Sources	AOR key	AOR key	Extraction


Haro 11	4326400	9007104	Optimal
Haro 2	5539840	9489920	Map
Haro 3	11180288	12556288	Tapered
He 2-10	4329472	4340480	Tapered
HS 0017+1055	26387200	26393344	Optimal
HS 0052+2536	26387456	17463040	Optimal
HS 0822+3542	4328960	1763808	Optimal
HS 1222+3741	17564928	26393600	Optimal
HS 1236+3937	26387712	26393856	Optimal
HS 1304+3529	26387968	26394112	Optimal
HS 1319+3224	26388480	26394624	Optimal
HS 1330+3651	26388736	26394880	Optimal
HS 1442+4250	10388480	12562944	Optimal
HS 2352+2733^a	26388992	26395136	–
I Zw 18	4330752	16205568	Optimal
IC 10	4424960	26396672	Map
II Zw 40	4327936	9007616	Optimal
Mrk 1089	11250432	26395392	Tapered
Mrk 1450	4334336	16206080 (SL),	Optimal
		9011712 (LL)
Mrk 153	4333056	4342272	Optimal
Mrk 209	22556672	12557568	Optimal
Mrk 930	4338944	4344320	Tapered
NGC 1140	4327168	4830976	Tapered
NGC 1569	4434944	3856640	Tapered
NGC 1705	5535744	9513216	Map
NGC 2366	4436480	21920768	Map
NGC 4214^b	4457984	–	–
NGC 4449	4467456	26396928	Map
NGC 4861^c	4337408	–	–
NGC 5253	4386048	4386304	Map
NGC 625^c	22520064	–	–
NGC 6822^b^,^c	5507072	–	–
Pox 186	26389248	12629760	Optimal
SBS 0335-052	4327424	8986880	Optimal
SBS 1159+545	26389504	9008896	Optimal
SBS 1211+540	26389760	26395392	Optimal
SBS 1249+493	26390016	26395904	Optimal
SBS 1415+437	10392832	12562432 (SL),	Optimal
		8990464 (LL)
SBS 1533+574	17563904	8996352	Optimal
Tol 0618-402	4328448	8090624	Optimal
Tol 1214-277	4336384	9008128	Optimal
UGC 4483	4329728	26396160	Optimal
UGCA 20^a	26390272	26396416	–
UM 133	26390528	21922304	Map
UM 311^b	10392576	–	–
UM 448	4334592	4342784	Tapered
UM 461	4335104	16204032 (SL),	Optimal
		9006336 (LL)
VII Zw 403	4334080	9005824	Tapered

Notes.

^(a)

For these galaxies, the IRS slits are not centred on the source position and thus we do not present any IRS spectrum.

^(b)

For these galaxies, only local pointings were performed and we cannot present an IRS spectrum for the total galaxy.

^(c)

Only high resolution IRS spectra (SH and/or LH) are available.

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