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) MB (mag) log(LTIR/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
Extended Objects
1 IC 10    
2 NGC 1140      
3 NGC 1569          
4 NGC 1705          
5 NGC 2366          
6 NGC 4214  
7 NGC 4449      
8 NGC 4861  
9 NGC 5253      
10 NGC 625          
11 NGC 6822        
Compact Objects
12 Haro 11  
13 Haro 2          
14 Haro 3    
15 He 2-10  
16 HS 0017+1055            
17 HS 0052+2536          
18 HS 0822+3542              
19 HS 1222+3741            
20 HS 1236+3937              
21 HS 1304+3529            
22 HS 1319+3224            
23 HS 1330+3651          
24 HS 1442+4250              
25 HS 2352+2733            
26 I Zw 18          
27 II Zw 40      
28 Mrk 1089      
29 Mrk 1450        
30 Mrk 153          
35 Mrk 209          
36 Mrk 930      
37 Pox 186            
38 SBS 0335-052          
39 SBS 1159+545          
40 SBS 1211+540              
41 SBS 1249+493              
42 SBS 1415+437          
43 SBS 1533+574          
44 Tol 0618-402                
45 Tol 1214-277          
46 UGC 4483          
47 UGCA 20                
48 UM 133          
49

 

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.

 

Maj : 29/05/2019 (4602)

Voir aussi
(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.
 

 

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