J/A+A/565/A128 Dust SED in HRS nearby galaxies (Ciesla+, 2014)
Dust spectral energy distributions of nearby galaxies: an insight from the
Herschel Reference Survey.
Ciesla L., Boquien M., Boselli A., Buat V., Cortese L., Bendo G.J.,
Heinis S., Galametz M., Eales S., Smith M.W.L., Baes M., Bianchi S.,
De Looze I., di Serego Alighieri S., Galliano F., Hughes T.M., Madden S.C.,
Pierini D., Remy-Ruyer A., Spinoglio L., Vaccari M., Viaene S., Vlahakis C.
<Astron. Astrophys., 565, A128-128 (2014)>
=2014A&A...565A.128C 2014A&A...565A.128C
ADC_Keywords: Galaxies, nearby ; Photometry, infrared
Keywords: galaxies: ISM - infrared: galaxies - dust, extinction
Abstract:
Although it accounts only for a small fraction of the baryonic mass,
dust has a profound impact on the physical processes at play in
galaxies. Thus, to understand the evolution of galaxies, it is
essential not only to characterize dust properties per se, but also in
relation to global galaxy properties. To do so, we derive the dust
properties of galaxies in a volume limited, K-band selected sample,
the Herschel Reference Survey (HRS). We gather infrared photometric
data from 8µm to 500µm from Spitzer, WISE, IRAS, and Herschel
for all of the HRS galaxies. Draine & Li (2007ApJ...663..866D 2007ApJ...663..866D) models
are fit to the data from which the stellar contribution has been
carefully removed. We find that our photometric coverage is sufficient
to constrain all of the parameters of the Draine & Li models and that
a strong constraint on the 20-60µm range is mandatory to estimate
the relative contribution of the photo-dissociation regions to the
infrared spectral energy distribution (SED). The SED models tend to
systematically underestimate the observed 500µm flux densities,
especially for low-mass systems. We provide the output parameters for
all of the galaxies, i.e., the minimum intensity of the interstellar
radiation field, the fraction of polycyclic aromatic hydrocarbon
(PAH), the relative contribution of PDR and evolved stellar population
to the dust heating, the dust mass, and the infrared luminosity. For a
subsample of gas-rich galaxies, we analyze the relations between these
parameters and the main integrated properties of galaxies, such as
stellar mass, star formation rate, infrared luminosity, metallicity,
Hα and H-band surface brightness, and the far-ultraviolet
attenuation. A good correlation between the fraction of PAH and the
metallicity is found, implying a weakening of the PAH emission in
galaxies with low metallicities and, thus, low stellar masses. The
intensity of the diffuse interstellar radiation field and the H-band
and Hα surface brightnesses are correlated, suggesting that the
diffuse dust component is heated by both the young stars in
star-forming regions and the diffuse evolved population. We use these
results to provide a new set of infrared templates calibrated with
Herschel observations on nearby galaxies and a mean SED template to
provide the z=0 reference for cosmological studies. For the same
purpose, we place our sample on the SFR-M* diagram. The templates
are compared to the most popular infrared SED libraries, enlightening
a large discrepancy between all of them in the 20-100µm range.
Description:
In order to compute the IR SEDs of the HRS galaxies, we use data from
8 to 500um performing the photometry on Spitzer/IRAC and WISE
images and using measurements available in the literature from
Spitzer/MIPS, Herschel/PACS, Herschel/SPIRE, and IRAS.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea2.dat 113 319 Mid-IR photometry of the HRS galaxies
table4.dat 93 146 Estimated parameters for galaxies analyzed
in this work
tablec1.dat 93 119 *Estimated parameters for galaxies not analyzed
in this work
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Note on tablec1.dat: 20 early-type galaxies and 99 HI-deficient galaxies.
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See also:
J/PASP/122/261 : Herschel Reference Survey Sample (Boselli+, 2010)
Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- HRS [1/323] HRS galaxy number
(<[BEC2010] HRS NNN> in Simbad)
5- 10 I6 --- CGCG ?=- CGCG galaxy number (Z NNN-NNN in Simbad)
12- 15 I4 --- VCC ?=- VCC galaxy number
17- 20 I4 --- UGC ?=- UGC galaxy number
22- 25 I4 --- NGC ?=- NGC galaxy number
27- 30 I4 --- IC ?=- IC galaxy number
32 I1 --- f_S8 [0/2] Detection flag on 8um data (1=OK) (1)
34 A1 --- l_S8 [<] Limit flag on S8
35- 41 F7.2 mJy S8 ?=- Spitzer/IRAC flux density at 8um
43- 48 F6.2 mJy e_S8 ? rms uncertainty on S8
50 I1 --- f_S12 [0/2] Detection flag on 12um data (1=OK) (1)
52 A1 --- l_S12 Limit flag on S12
53- 59 F7.2 mJy S12 ?=- WISE/W3 flux density at 12um (W3 band)
61- 66 F6.2 mJy e_S12 ? rms uncertainty on S12
68 I1 --- f_S22 [0/2] Detection flag on 22um data (1=OK) (1)
70 A1 --- l_S22 Limit flag on S22
71- 77 F7.2 mJy S22 ?=- WISE/W4 flux density at 22um (W4 band)
79- 84 F6.2 mJy e_S22 ? rms uncertainty on S22
86- 91 F6.2 deg RAdeg Right ascension (J2000)
93- 97 F5.2 deg DEdeg Declination (J2000)
99-103 F5.1 arcsec a Semi-major axis of galaxy
105-109 F5.1 arcsec b Semi-minor axis of galaxy
111-113 I3 deg PA [0/270] Position angle of galaxy ellipse
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Note (1): Flag is:
0 = undetected galaxy
1 = detected galaxy
2 = galaxy or which the measurement suffers from source blending
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Byte-by-byte Description of file: table4.dat tablec1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- HRS [1/323] HRS galaxy number
(<[BEC2010] HRS NNN> in Simbad)
5- 10 I6 --- CGCG ?=- CGCG galaxy number
12- 15 I4 --- VCC ?=- VCC galaxy number
17- 20 I4 --- UGC ?=- UGC galaxy number
22- 25 I4 --- NGC ?=- NGC galaxy number
27- 30 I4 --- IC ?=- IC galaxy number
32- 39 A8 --- MType Morphological type
41- 45 F5.2 --- Umin [0.2/16.5] Intensity of the diffuse
interstellar radiation field (ISRF) (2)
47- 50 F4.2 --- e_Umin rms uncertainty on Umin
52- 55 F4.2 % qPAH [0.8/4.6] Fraction of the total grain mass
contributed by PAH containing less than
103C atoms
57- 60 F4.2 % e_qPAH rms uncertainty on qPAH
62- 66 F5.2 % gamma [0.1/15.8] Fraction of total dust mass (2)
68- 72 F5.2 % e_gamma rms uncertainty on gamma
74- 78 F5.2 [Lsun] log(LIR) [7.6/11.0] Infrared luminosity
80- 83 F4.2 [Lsun] e_log(LIR) rms uncertainty on log(LIR)
85- 88 F4.2 [Msun] log(Mdust) [5.3/8.4] Dust mass (2)
90- 93 F4.2 [Msun] e_log(Mdust) rms uncertainty on log(Mdust)
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Note (2): parameters of modelisation from Draine and Li (2007ApJ...657..810D 2007ApJ...657..810D):
Umin = Intensity of the diffuse interstellar radiation field
(dimensionless scaling factor relative to solar neihbourhood)
Mdust = total mass of dust
1-γ = fraction of the dust mass that is exposed to starlight
intensity Umin
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 29-Jul-2014