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DGS

The Herschel Dwarf Galaxy Survey

"The ISM in Low Metallicity Environments: Bridging the Gap Between Local Universe and Primordial Galaxies"

The Herschel Dwarf Galaxy Survey is a Guaranteed Time Key Program led by Suzanne Madden.
Abstract:
While much of what we have gleaned of the details of dust and gas properties and the processes of dust recycling and heating and cooling in galaxies has been limited to Galactic studies, with Herschel we will be able to explore these issues in low metallicity dwarf galaxies which are known by now to exhibit dust and gas properties different from more metal-rich galaxies. Because these objects are relatively nearby, it is possible to relate the observed variations in the SEDs to the actual physical phenomena occuring within the ISM of the galaxy, allowing the construction of a rich interpretative framework for unresolved, more distant galaxies in the early universe. Using the SPIRE and PACS instruments on Herschel, we propose to map the dust and gas in a 50 dwarf galaxies, sampling a broad metallicity range of 1/50 to 1/2 solar. These data, in conjunction with other ancillary data, will be used to construct the emission spectrum of the dust plus that of the gas in the most important cooling lines. The combination of these instruments onboard Herschel will provide the first opportunity to study the dust and gas in extremely low metallicity environments that have not yet experienced repeated recycling through the ISM. The interpretation of this data will open the door to comprehending primordial ISM conditions and star formation in the young universe.

Sample

The Herschel Dwarf Galaxy Survey has observed 50 galaxies, including regions of the Magellanic Clouds, Local Group galaxies, and galaxies out to a distance of 200 Mpc. They were chosen to cover a broad range of metallicities, from 1/50 to 1/2 solar. The sample was selected from surveys of metal-poor Blue Compact Dwarf galaxies and of emission line galaxies identified in the Hamburg/SAO Survey and the First and Second Byurakan Surveys.


#	Object Name	RA (J2000)	Dec (J2000)	Redshift	12 + log(O/H)	D₂₅ (arcmin²)	M_B (mag)	log(L_TIR/L_?)	log(M_?/M_?)
Extended Objects
1	IC 10	00h20m17.3s	+59d18m14s	-0.0012	8.17	6.8 × 5.9	-12.43	8.22	8.60
2	NGC 1140	02h54m33.6s	-10d01m40s	0.0050	8.38	1.7 × 0.9	-18.55	9.57	9.65
3	NGC 1569	04h30m46.1s	+64d50m53s	-0.0003	8.02	3.6 × 1.8	-15.75	9.10	8.93
4	NGC 1705	04h54m13.5s	-53d21m40s	0.0021	8.27	1.9 × 1.4	-15.73	7.84	8.34
5	NGC 2366	07h28m54.7s	+69d12m57s	0.0003	7.70	8.1 × 3.3	-16.18	8.14	8.29
6	NGC 4214	12h15m39.2s	+36d19m37s	0.0010	8.26	8.5 × 6.6	-17.11	8.73	8.92
7	NGC 4449	12h28m11.1s	+44d05m37s	0.0007	8.20	6.2 × 4.4	-17.94	9.34	9.43
8	NGC 4861	12h59m02.3s	+34d51m34s	0.0028	7.89	4.0 × 1.5	-16.84	8.54	8.49
9	NGC 5253	13h39m56.0s	-31d38m24s	0.0014	8.25	5.0 × 1.9	-16.87	9.21	8.77
10	NGC 625	01h35m04.6s	-41d26m10s	0.0013	8.22	5.8 × 1.9	-16.20	8.46	8.73
11	NGC 6822	19h44m56.6s	-14d47m21s	-0.0002	7.96	15.5 × 13.5	-13.19	7.56	8.19
Compact Objects
12	Haro 11	0h36m52.5s	-33d33m19s	0.0206	8.36	0.5 × 0.4	-20.55	11.30	10.24
13	Haro 2	10h32m31.9s	+54d24m04s	0.0048	8.23	1.2 × 0.8	-18.28	9.80	9.56
14	Haro 3	10h45m22.4s	+55d57m37s	0.0031	8.28	1.2 × 0.8	-18.29	9.73	9.49
15	He 2-10	8h36m15.2s	-26d24m34s	0.0029	8.43	1.9 × 1.4	-17.25	9.74	9.50
16	HS 0017+1055	0h20m21.4s	+11d12mm21s	0.0188	7.63	-	-16.23	8.99	7.84
17	HS 0052+2536	0h54m56.4s	+25d53m08s	0.0454	8.07	-	-19.56	10.23	10.31
18	HS 0822+3542	8h25m55.5s	+35d32m32s	0.0024	7.32	0.27 × 0.11	-12.40	7.02	6.48
19	HS 1222+3741	12h24m36.7s	+37d24m37s	0.0409	7.79	0.12 × 0.11	-17.90	9.38	9.37
20	HS 1236+3937	12h39m20.1s	+39d21m05s	0.0184	7.72	0.34 × 0.09	-16.00	-	9.17
21	HS 1304+3529	13h06m24.2s	+35d13m42s	0.0165	7.93	0.28 × 0.21	-17.73	9.24	8.58
22	HS 1319+3224	13h21m19.9s	+32d08m23s	0.0182	7.81	0.14 × 0.11	-15.68	8.37	8.05
23	HS 1330+3651	13h33m08.3s	+36d36m33s	0.0167	7.98	0.29 × 0.19	-17.81	9.14	8.95
24	HS 1442+4250	14h44m12.8s	+42d37m44s	0.0021	7.60	1.13 × 0.26	-15.15	-	-
25	HS 2352+2733	23h54m56.7s	+27d49m59s	0.0276	8.40	-	-17.05	-	8.11
26	I Zw 18	9h34m02.0s	+55d14m28s	0.0025	7.14	0.3 × 0.3	-15.22	7.52	7.34
27	II Zw 40	5h55m42.6s	+3d23m32s	0.0026	8.23	0.56 × 0.22	-14.93	9.46	-
28	Mrk 1089	5h01m37.8s	-4d15m28s	0.0134	8.10	0.61 × 0.23	-20.46	10.55	10.28
29	Mrk 1450	11h38m35.6s	+57d52m27s	0.0032	7.84	0.40 × 0.31	-13.86	8.48	8.09
30	Mrk 153	10h49m05.0s	+52d20m08s	0.0080	7.86	0.54 × 0.30	-18.03	9.02	9.06
31	Mrk 209	12h26m16.0s	+48d29m37s	0.0009	7.74	0.8 × 0.6	-13.67	7.45	7.46
32	Mrk 930	23h31m58.3s	+28h56m50s	0.0183	8.03	0.43 × 0.43	-19.50	10.28	9.44
33	Pox 186	13h25m48.7s	-11d36m38s	0.0039	7.70	-	-12.17	7.76	7.08
34	SBS 0335-052	3h37m44.1s	-5d02m40s	0.0135	7.25	0.23 × 0.20	-16.02	9.25	8.03
35	SBS 1159+545	12h02m02.4s	+54d15m50s	0.0118	7.44	0.20 × 0.10	-15.08	8.30	7.85
36	SBS 1211+540	12h14m02.5s	+53d45m17s	0.0030	7.58	0.26 × 0.17	-13.43	7.46	7.60
37	SBS 1249+493	12h51m52.5s	+49d03m27s	0.0243	7.68	0.10 × 0.10	-	8.97	8.42
38	SBS 1415+437	14h17m01.4s	+43d30m05s	0.0020	7.55	0.75 × 0.15	-14.99	7.82	-
39	SBS 1533+574	15h34m13.8s	+57d17m06s	0.0110	8.05	0.67 × 0.67	-16.69	9.28	7.30
40	Tol 0618-402	6h20m02.6s	-40d18m09s	0.0350	8.09	0.4 × 0.3	-	-	10.43
41	Tol 1214-277	12h17m17.1s	-28d02m33s	0.0260	7.52	0.08 × 0.05
42	UGC 4483	8h37m03.0s	+69d46m31s	0.0005	7.46	1.4 × 0.7	-12.53	6.50	6.90
43	UGCA 20	1h43m14.7s	+19d58m32s	0.0017	7.50	3.1 × 0.8	-14.43	-	7.54
44	UM 133	1h44m41.3s	+4d53m26s	0.0054	7.82	1.0 × 1.0	-15.72	7.86	7.81
45	UM 311	1h15m34.4s	-0d51m46s	0.0056	8.37	0.11 × 0.10	-19.22	9.74	-
46	UM 448	11h42m12.4s	+0d20m03s	0.0186	8.32	0.4 × 0.4	-20.02	10.95	10.62
47	UM 461	11h51m33.4s	-2d22m22s	0.0035	7.73	0.30 × 0.22	-13.73	7.85	7.66
48	VII Zw 403	11h27m59.9s	+78d59m39s	-0.0003	7.66	1.4 × 0.8	-13.77	7.30	7.20
LMC and SMC regions
001	LMC - 30 Dor	05h38m42.3s	-69d06m03s	0.0009	8.5	645 × 550	-17.58	9.15	9.30
002	LMC - N11 A	04h57m16.2s	-66d23m20s	0.0009	8.5	645 × 550	-17.58	9.15	9.30
003	LMC - N11 B	04h56m51.5s	-66d24m25s	0.0009	8.5	645 × 550	-17.58	9.15	9.30
004	LMC - N11 C	04h57m48.3s	-66d28m32s	0.0009	8.5	645 × 550	-17.58	9.15	9.30
005	LMC - N11 I	04h55m44.3s	-66d34m28s	0.0009	8.5	645 × 550	-17.58	9.15	9.30
006	LMC - N158	05h39m14.0s	-69d30m18s	0.0009	8.5	645 × 550	-17.58	9.15	9.30
007	LMC - N159	05h39m52.8s	-69d45m20s	0.0009	8.5	645 × 550	-17.58	9.15	9.30
008	LMC - N160	05h39m42.2s	-69d38m51s	0.0009	8.5	645 × 550	-17.58	9.15	9.30
009	SMC - N66	00h59m25.4s	-72d10m10s	0.0005	8.0	320 × 185	-16.19	8.02	8.62

Herschel PACS and SPIRE Observations

Our sample consist of 50 galaxies observed with PACS and SPIRE in photometry and spectroscopy (Madden et al. 2013). The spectroscopy of the extended sources was observed as part of the SHINING program (Sturm et al. 2011). The photometry of the Magellanic Clouds belongs to the HERITAGE program (Meixner et al. 2013).

Table keys: • = in our program • = in the archive • = no 70 or 100µm

PACS phot

SPIRE phot

PACS spec

SPIRE spec

Object Name

70, 100, 160

250, 350, 500

[C II]157

[O I]63

[O III]88

[O I]145

[N II]122

[N II]205

[N III]57

205-610

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Team Members

Suzanne Madden (PI)	AIM, CEA Saclay	suzanne.madden [at] cea.fr

Mélanie Chevance	Universität Heidelberg	chevance [at] uni-heidelberg.de

Diane Cormier	AIM, CEA Saclay	diane.cormier [at] cea.fr

Ilse De Looze	Universiteit Gent	ilse.delooze [at] ugent.be

Maud Galametz	AIM, CEA Saclay	maud.galametz [at] cea.fr

Frédéric Galliano	AIM, CEA Saclay	frederic.galliano [at] cea.fr

Sacha Hony	Universität Heidelberg	sacha.hony [at] free.fr

Vianney Lebouteiller	AIM, CEA Saclay	vianney.lebouteiller [at] cea.fr

Min-Young Lee	MPIfR Bonn	mlee [at] mpifr-bonn.mpg.de

Fiorella Polles	Observatoire de Paris	fiorella.polles [at] cea.fr

Aurélie Rémy-Ruyer	-----	-----

Ronin Wu	Observatoire de Meudon	ronin.wu [at] obspm.fr

and the SAG2 consortium

Publications

*2019*
♣	Cormier et al. 2019, A&A, in press The Herschel Dwarf Galaxy Survey: II. Physical conditions, origin of [CII] emission, and porosity of the multiphase low-metallicity ISM
*2018*
♣	Polles et al. 2019, A&A, 622, 119 Modeling ionized gas in low-metallicity environments: the Local Group dwarf galaxy IC10
*2017*
♣	Lebouteiller et al. 2017, A&A, 602, 45 Neutral gas heating by X-rays in primitive galaxies: Infrared observations of the blue compact dwarf I Zw 18 with Herschel
♣	Cormier et al. 2017, MNRAS, 468, 87 New ALMA constraints on the star-forming interstellar medium at low metallicity: a 50 pc view of the blue compact dwarf galaxy SBS 0335-052
*2016*
♣	Lee et al. 2016, A&A, 596, 85 Radiative and mechanical feedback into the molecular gas in the Large Magellanic Cloud. I. N159W
♣	Chevance et al. 2016, A&A, 590, 36 A milestone toward understanding PDR properties in the extreme environment of LMC-30 Doradus
*2015*
♣	Rémy-Ruyer et al. 2015, A&A, 582, 121 Linking dust emission to fundamental properties in galaxies: The low-metallicity picture
♣	Cormier et al. 2015, A&A, 578, 53 The Herschel Dwarf Galaxy Survey: I. Properties of the low-metallicity ISM from PACS spectroscopy
*2014*
♣	De Looze et al. 2014, A&A, 568, 62 The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types
♣	Cormier et al. 2014, A&A, 564, 121 The molecular gas reservoir of 6 low-metallicity galaxies from the Herschel Dwarf Galaxy Survey: A ground-based follow-up survey of CO(1-0), CO(2-1), and CO(3-2)
♣	Rémy-Ruyer et al. 2014, A&A, 564, 31 Gas-to-Dust mass ratios in galaxies over a 2 dex metallicity range
*2013*
♣	Rémy-Ruyer et al. 2013, A&A, 557, 95 Revealing the cold dust in low-metallicity environments - I. Photometry analysis of the Dwarf Galaxy Survey with Herschel
♣	Madden et al. 2013, PASP, 125, 600 An Overview of the Dwarf Galaxy Survey
♣	Karczewski et al. 2013, MNRAS, 431, 2493 A multiwavelength study of the Magellanic-type galaxy NGC 4449 - I. Modelling the spectral energy distribution, the ionization structure and the star formation history
*2012*
♣	Lebouteiller et al. 2012, A&A, 548, 91 Physical conditions in the gas phases of the giant H II region LMC-N 11 unveiled by Herschel - I. Diffuse [C II] and [O III] emission in LMC-N 11B
♣	Cormier et al. 2012, 548, 20 The nature of the interstellar medium of the starburst low-metallicity galaxy Haro 11: a multi-phase model of the infrared emission
*2010*
♣	O'Halloran et al. 2010, A&A, 518, 580 Herschel photometric observations of the low metallicity dwarf galaxy NGC 1705
♣	Cormier et al. 2010, A&A, 518, 57 The effects of star formation on the low-metallicity ISM: NGC 4214 mapped with Herschel/PACS spectroscopy
♣	Galametz et al. 2010, A&A, 518, 55 Herschel photometric observations of the nearby low metallicity irregular galaxy NGC 6822

Links

			For Herschel PACS data reduction and analysis, we used the PACSman software. It includes IDL routines for line fitting and map making. For more information, go see Vianney's website here.

			The HErschel DAtabase in Marseille (HEDAM) is the repository of several Herschel Key Programs and will soon host data products of the DGS. Access the HEDAM website here.

#4602 - Màj : 29/05/2019

• Formation des Etoiles et du Milieu Interstellaire • Star Formation and Interstellar Medium

• HERSCHEL • HERSCHEL

Voir aussi

NUAGES

(Nearby Universe Agents of Galaxy Evolution Studies)

NUAGES is a research group of the Star-formation and Interstellar Medium lab at CEA Saclay. The acronym NUAGES stands for Nearby Universe Agents of Galaxy Evolution Studies. The group focuses on the study of (nearby) galaxies with interest in topics related to the interstellar dust and gas, heating and cooling processes, ISM composition and structure, low-metallicity conditions, chemical evolution of galaxies.