J/A+A/582/A121 Dust properties in galaxies (Remy-Ruyer+, 2015)
Linking dust emission to fundamental properties in galaxies:
the low-metallicity picture.
Remy-Ruyer A., Madden S.C., Galliano F., Lebouteiller V., Baes M.,
Bendo G.J., Boselli A., Ciesla L., Cormier D., Cooray A., Cortese L.,
De Looze I., Doublier-Pritchard V., Galametz M., Jones A.P.,
Karczewski O.L., Lu N., Spinoglio L.
<Astron. Astrophys., 582, A121-121 (2015)>
=2015A&A...582A.121R 2015A&A...582A.121R (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, IR ; Interstellar medium ; Photometry, infrared
Keywords: dust, extinction - evolution - galaxies: dwarf - galaxies: evolution -
infrared: ISM - infrared: galaxies
Abstract:
In this work, we aim to provide a consistent analysis of the dust
properties from metal-poor to metal-rich environments by linking them
to fundamental galactic parameters. We consider two samples of
galaxies: the Dwarf Galaxy Survey (DGS) and the Key Insights on Nearby
Galaxies: a Far-Infrared Survey with Herschel (KINGFISH), totalling
109 galaxies, spanning almost 2dex in metallicity. We collect infrared
(IR) to submillimetre (submm) data for both samples and present the
complete data set for the DGS sample. We model the observed spectral
energy distributions (SED) with a physically-motivated dust model to
access the dust properties: dust mass, total-IR luminosity, polycyclic
aromatic hydrocarbon (PAH) mass fraction, dust temperature
distribution, and dust-to-stellar mass ratio. Using a different SED
model (modified black body), different dust composition (amorphous
carbon in lieu of graphite), or a different wavelength coverage at
submm wavelengths results in differences in the dust mass estimate of
a factor two to three, showing that this parameter is subject to
non-negligible systematic modelling uncertainties. We find half as
much dust with the amorphous carbon dust composition. For eight
galaxies in our sample, we find a rather small excess at 500µm
(≤1.5σ). We find that the dust SED of low-metallicity galaxies
is broader and peaks at shorter wavelengths compared to more
metal-rich systems, a sign of a clumpier medium in dwarf galaxies. The
PAH mass fraction and dust temperature distribution are found to be
driven mostly by the specific star formation rate, sSFR, with
secondary effects from metallicity. The correlations between
metallicity and dust mass or total-IR luminosity are direct
consequences of the stellar mass-metallicity relation. The
dust-to-stellar mass ratios of metal-rich sources follow the
well-studied trend of decreasing ratio for decreasing sSFR. The
relation is more complex for low-metallicity galaxies with high sSFR,
and depends on the chemical evolutionary stage of the source (i.e.
gas-to-dust mass ratio). Dust growth processes in the ISM play a key
role in the dust mass build-up with respect to the stellar content at
high sSFR and low metallicity. We conclude that the evolution of the
dust properties from metal-poor to metal-rich galaxies derives from a
complex interplay between star formation activity, stellar mass, and
metallicity.
Description:
For this study, we combine two samples of local galaxies observed with
Herschel: the Dwarf Galaxy Survey (DGS, Madden et al.,
2013PASP..125..600M 2013PASP..125..600M) and the Key Insights on Nearby Galaxies: a
Far-Infrared Survey with Herschel (KINGFISH, Kennicutt et al.,
2011PASP..123.1347K 2011PASP..123.1347K).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table4.dat 71 109 DGS and KINGFISH stellar mass and
star-formation parameters
table5.dat 113 48 Updated Herschel flux densities for the
DGS sample
table6.dat 97 48 Spitzer IRAC flux densities for the DGS sample
table7.dat 105 48 WISE flux densities for the DGS sample
table8.dat 127 48 2MASS and IRAS flux densities from the
literature for the DGS sample
table9.dat 97 109 DGS and KINGFISH dust parameters
tableb1.dat 60 48 DGS Spitzer/IRAC and IRS observing Log
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Sample Sample
10- 20 A11 --- Name Source name
23- 24 A2 --- l_logM* [<≥] Limit flag on logM*
25- 29 F5.2 [Msun] logM* Stellar mass (1)
31- 34 F4.2 [Msun] e_logM* ? rms uncertainty on logM*
36- 40 F5.2 [Msun/yr] logSFR ?=- Star-formation rates from
Hα+LTIR (2)
42- 45 F4.2 [Msun/yr] e_logSFR ?=- rms uncertainty on logSFR
47- 48 A2 --- l_logsSFR [<≥] Limit flag on logsSFR
49- 54 F6.2 [yr-1] logsSFR ?=- Specific star-formation rates defined
by SFR/M*
56- 59 F4.2 [yr-1] e_logsSFR ? rms uncertainty on logsSFR
62- 66 F5.2 [10-7W] logLHa ?=- Hα luminosity (3)
68 A1 --- n_logLHa [a] Note on ogLHa (4)
70- 71 I2 --- rnlogLHa ? References for n_logLHa (5)
--------------------------------------------------------------------------------
Note (1): Log of stellar masses estimated with the formula from
Eskew et al. (2012AJ....143..139E 2012AJ....143..139E).
Note (2): Log of star-formation rates from Hα+LTIR (see Sect. 2.6.1)
Note (3): Log of Hα luminosities corrected for underlying stellar
absorption, NII line contamination and foreground Galactic extinction
Note (4): a for corresponding SFRs estimated from Lee et al.
(2009, Cat. J/ApJ/706/599; see Sect. 2.6.1).
Note (5): References for Hα luminosities as follows:
1 = Schmitt et al. (2006ApJS..164...52S 2006ApJS..164...52S)
2 = Kennicutt et al. (2009, Cat. J/ApJ/703/1672)
3 = Moustakas & Kennicutt (2006, Cat. J/ApJS/164/81)
4 = Kennicutt et al. (2008, Cat. J/ApJS/178/247)
5 = Gil de Paz et al. (2003, Cat. J/ApJS/147/29)
6 = Popescu & Hopp (2000A&AS..142..247P 2000A&AS..142..247P)
7 = Iglesias-Paramo & Vilchez (1997ApJ...479..190I 1997ApJ...479..190I)
8 = Pustilnik et al. (2004A&A...425...51P 2004A&A...425...51P)
9 = Izotov et al. (1994ApJ...435..647I 1994ApJ...435..647I)
10 = Izotov & Thuan (1998ApJ...500..188I 1998ApJ...500..188I)
11 = Terlevich et al. (1991, Cat. J/A+AS/91/285)
12 = Moles et al. (1994ApJ...432..135M 1994ApJ...432..135M)
13 = Skibba et al. (2011ApJ...738...89S 2011ApJ...738...89S)
14 = Plana et al. (1998A&AS..128...75P 1998A&AS..128...75P)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Source name
13- 14 A2 --- l_F70 [<≥] Limit flag on F70
15- 21 F7.3 Jy F70 PACS flux at 70um
23- 27 F5.3 Jy e_F70 ? rms uncertainty on F70
28 A1 --- n_F70 [b] Note on F70 (1)
30- 31 A2 --- l_F100 [<≥] Limit flag on F1000
32- 38 F7.3 Jy F100 ?=- PACS flux at 100um
40- 45 F6.3 Jy e_F100 ? rms uncertainty on F100
46 A1 --- n_F100 [b] Note on F100 (1)
48- 49 A2 --- l_F160 [<≥] Limit flag on F160
50- 56 F7.3 Jy F160 PACS flux at 160um
58- 63 F6.3 Jy e_F160 ? rms uncertainty on F160
65 A1 --- Met [SP] Map method (2)
66 A1 --- n_Met [cd] Note on Map method (1)
68- 69 A2 --- l_F250 [<≥] Limit flag on F250
70- 75 F6.3 Jy F250 ?=- SPIRE flux at 250um
77- 82 F6.3 Jy e_F250 ? rms uncertainty on F250
84- 85 A2 --- l_F350 [<≥] Limit flag on F350
86- 91 F6.3 Jy F350 ?=- SPIRE flux at 350um
93- 98 F6.3 Jy e_F350 ?=- rms uncertainty on F350
100-101 A2 --- l_F500 [<≥] Limit flag on F500
102-107 F6.3 Jy F500 ?=- SPIRE flux on F500
109-113 F5.3 Jy e_F500 ?=- rms uncertainty on F500
--------------------------------------------------------------------------------
Note (1): Notes as follows:
b = These upper limits come from the SED modelling (see Appendix E)
c = For these galaxies, the PACS map-making method was changed from
PhotProject to Scanamorphos since Remy-Ruyer et al. (2013A&A...557A..95R 2013A&A...557A..95R)
d = For these galaxies, the PACS map-making method was changed from
Scanamorphos to PhotProject since Remy-Ruyer et al. (2013A&A...557A..95R 2013A&A...557A..95R)
Note (2): Map method as follows:
P = PhotProject
S = Scanamorphos
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Source name
12 A1 --- n_Name [f] Note on IC 10 (1)
13- 14 A2 --- l_F3.6 [<≥] Limit flag on F3.6
16- 23 F8.3 mJy F3.6 ?=- IRAC flux at 3.6um
25- 31 F7.3 mJy e_F3.6 ? rms uncertainty on F3.6
33- 34 A2 --- l_F4.5 [<≥] Limit flag on F4.5
35- 42 F8.3 mJy F4.5 ?=- IRAC flux at 4.5um
44- 50 F7.3 mJy e_F4.5 ? rms uncertainty on F4.5
52- 53 A2 --- l_F5.8 [<≥] Limit flag on F5.8
54- 59 F6.2 mJy F5.8 ?=- IRAC flux at 5.8um
61- 66 F6.2 mJy e_F5.8 ? rms uncertainty on F5.8
68- 69 A2 --- l_F8.0 [<≥] Limit flag on F8.0
70- 76 F7.2 mJy F8.0 ?=- IRAC flux at 8.0um
78- 83 F6.2 mJy e_F8.0 ?=- rms uncertainty on F8.0
86- 88 I3 arcsec ApRad ?=- Aperture radius
89 A1 --- --- [x]
90- 92 I3 arcsec ApRad2 ? Second aperture radius
93 A1 --- n_ApRad [abcde] Note on ApRad (2)
95- 97 A3 --- f_ApRad [yes ] Aperture radius corrected ?
--------------------------------------------------------------------------------
Note (1): f: the IRAC maps do not cover the full galaxy. Thus we do not report
flux densities for this source.
Note (2): Notes as follows:
a = The aperture is the same as the one used for Herschel.
b = The Herschel aperture has been shorten to avoid a contaminating source.
c = The Herschel aperture has been adapted to match the peculiar morphology.
of the source in the NIR.
d = The Herschel aperture has been enlarged to encompass all of the
NIR emission.
e = The IRAC map is smaller than the Herschel aperture. The aperture thus
had to be shorten.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Source name
12 A1 --- n_Name [d] Note on NGC 6822 (1)
14- 15 A2 --- l_F3.4 [<≥] Limit flag on F3.4
16- 23 F8.3 mJy F3.4 ? WISE flux at 3.4um
25- 31 F7.3 mJy e_F3.4 ? rms uncertainty on F3.4
32 A1 --- n_F3.4 [c] Note on F3.4 (2)
34- 35 A2 --- l_F4.6 [<≥] Limit flag on F4.6
36- 42 F7.3 mJy F4.6 ? WISE flux at 4.6um
44- 49 F6.3 mJy e_F4.6 ? rms uncertainty on F4.6
50 A1 --- n_F4.6 [c] Note on F4.6
52- 53 A2 --- l_F12 [<≥] Limit flag on F12
54- 60 F7.2 mJy F12 ? WISE flux at 12um
62- 67 F6.2 mJy e_F12 ? rms uncertainty on F12
68 A1 --- n_F12 [c] Note on F12
70- 71 A2 --- l_F22 [<≥] Limit flag on F22
72- 80 F9.3 mJy F22 ? WISE flux at 22um
82- 87 F6.2 mJy e_F22 ? rms uncertainty on F22
88 A1 --- n_F22 [c] Note on F22
92- 94 I3 arcsec ApRad12 ?=- First aperture radius or semi-major
axis (3)
95 A1 --- --- [x]
96- 98 I3 arcsec ApRad12b ? First aperture semi-minor axis (3)
99 A1 --- r_ApRad12 [ab] Note for ApRad12 (4)
100 A1 --- --- [,]
102-104 I3 arcsec ApRad34 ? Second aperture radius (3)
105 A1 --- n_ApRad34 [ab] Note for ApRad34 (4)
--------------------------------------------------------------------------------
Note (1): The WISE map does not cover the full galaxy. Thus we do not report
flux densities for this source.
Note (2): c: This galaxy is not resolved at these wavelengths and we thus use
the profile fit photometry provided by the WISE database.
Note (3): 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 x semi-minor axis.
A dash indicates that we take the profile fit photometry from the All WISE
database.
Note (4): Notes as follows:
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
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Source name
12 A1 --- n_Name [a] Note on Name (1)
14- 21 F8.3 mJy FJ ? 2MASS flux in J-band
23- 28 F6.3 mJy e_FJ ? rms uncertainty on FJ
31- 37 F7.2 mJy FH ? 2MASS flux in JH-band
39- 44 F6.2 mJy e_FH ? rms uncertainty on FH
47- 48 A2 --- l_FKs [<≥] Limit flag on FKs
49- 55 F7.2 mJy FKs ? 2MASS flux in Ks-band
57- 62 F6.2 mJy e_FKs ? rms uncertainty on FKs
64 I1 --- r_FJ [1/5]? Reference for 2MASS fluxes (1)
66- 67 A2 --- l_F12 [<≥] Limit flag on F12
68- 72 F5.3 Jy F12 ? IRAS flux at 12um
74- 78 F5.3 Jy e_F12 ? rms uncertainty on F12
79 A1 --- n_F12 [b] Note on F12 (2)
81- 82 A2 --- l_F25 [<≥] Limit flag on F25
83- 88 F6.3 Jy F25 ? IRAS flux at 25um
90- 94 F5.3 Jy e_F25 ? rms uncertainty on F15
95 A1 --- n_F25 [b] Note on F25 (2)
97- 98 A2 --- l_F60 [<≥] Limit flag on F60
99-103 F5.2 Jy F60 ? IRAS flux at 60um
105-108 F4.2 Jy e_F60 ? rms uncertainty on F60
109 A1 --- n_F60 [b] Note on F60 (2)
111-112 A2 --- l_F100 [<≥] Limit flag on F100
113-117 F5.2 Jy F100 ? IRAS flux at 100um
119-123 F5.2 Jy e_F100 ? rms uncertainty on F100
124 A1 --- n_F100 [b] Note on F100 (2)
126-127 I2 --- r_F12 [6/12]? References for IRAS fluxes (1)
--------------------------------------------------------------------------------
Note (1): References as follows:
1 = NASA/IPAC ISA 2MASS Point Source Catalog (Cat. II/246)
2 = 2MASS Extended Objects Final Release (Cat. VII/233)
3 = 2MASS Large Galaxy Atlas (Jarrett et al., 2003AJ....125..525J 2003AJ....125..525J)
4 = Engelbracht et al. (2008ApJ...678..804E 2008ApJ...678..804E)
5 = Dale et al. (2009, Cat. J/ApJ/703/517)
6 = NASA/IPAC ISA IRAS Faint Source (v2.0 1990) (Cat. II/156)
7 = IRAS Point Source (v2.1) Catalogs (Cat. II/125)
8 = Rice et al. (1988ApJS...68...91R 1988ApJS...68...91R, Cat. VII/109)
9 = Sanders et al. (2003, Cat. J/AJ/126/1607)
10 = Engelbracht et al. (2008ApJ...678..804E 2008ApJ...678..804E)
Note (2): Notes as follows:
a = The aperture used does not cover the total emission from the galaxy and
the 2MASS magnitudes reported in the database are not consistent with the
rest of the IR photometry. Thus we do not consider them for the modelling
b = This IRAS flux density is not consistent with the rest of the IR.
photometry. Thus we do not consider it for the modelling.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table9.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Sample Sample
10- 20 A11 --- Name Source name
23- 24 A2 --- l_logMdustGr [<≥] Limit flag on logMdustGr
25- 28 F4.2 [Msun] logMdustGr ? Dust mass derived using graphite for the
carbonaceous component
29 A1 --- n_logMdustGr [a] Note on logMdustGr (4)
30- 33 F4.2 [Msun] logMdustAc ? Dust mass derived using amorphous carbons
for the carbonaceous component
35- 39 F5.2 [Lsun] logLTIR ? Total infrared luminosity, from the
best-fit model and integrated between
1 and 1000um
40 A1 --- n_logLTIR [b] Note on logLTIR (4)
41- 42 A2 --- l_fPAH [<≥] Limit flag on fPAH
43- 46 F4.2 --- fPAH ? PAH mass fraction, normalised to the
Galactic value fPAH☉=4.57%
47 A1 --- n_fPAH [c] Note on fPAH (4)
48- 53 E6.2 --- ? Mass-averaged starlight intensity (1)
55- 60 E6.2 --- sigmaU ? Standard deviation of the starlight
intensity distribution (2)
62- 65 F4.1 K Tdust ? Average dust temperature (3)
66 A1 --- n_Tdust [a] Note on Tdust (4)
68- 74 F7.2 Sun Umin ? Minimum value of the starlight intensity,
normalised to the Galactic value U☉
76- 82 E7.1 Sun DU ? Difference between the maximum and minimum
values of the starlight intensity
distribution, normalised to the Galactic
value U☉
84- 87 F4.2 --- alpha ? Index of the power law describing the
starlight intensity distribution
89- 92 F4.0 K TMIRBB ? Temperature of the additional MIR modBB
93 A1 --- --- [,]
95- 97 I3 K TMIRBBb ? Second value of temperature of the
additional MIR modBB
--------------------------------------------------------------------------------
Note (1): computed with Eq. (1), normalised to the Galactic value
U☉=2.2x10-5W/m2
Note (2): computed with Eq. (2), normalised to the Galactic value U☉
Note (3): computed by integrating Eq. (1) over T=TMWxU1/(4+β),
with β= 2.0, and TMW=19.7K from Planck Collaboration XI (2014)
Note (4): Notes as follows:
a = Dust mass and temperature obtained from a modBB fit (see Sect. 3.2.2).
b = LTIR obtained from Galametz et al. (2013MNRAS.431.1956G 2013MNRAS.431.1956G) calibrations as
no SED fit was possible for this galaxy.
c = In these galaxies the fit converges towards 0: no PAH are detected and
it is not possible to give an upper limit with the method described in
Sect. 4.3.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tableb1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Source name
12- 14 A3 --- n_Name [abc, ] Note on Name (1)
17- 24 I8 --- IRAC IRAC AOR key
26- 52 A27 --- IRS IRS AOR key
54- 60 A7 --- Ext IRS Extraction
--------------------------------------------------------------------------------
Note (1): Note s as follows:
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
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 22-Jan-2016