J/A+A/631/A38 Local galaxies dust properties (Lianou+, 2019)
Dust properties and star formation of approximately a thousand local galaxies.
Lianou S., Barmby P., Mosenkov A.A., Lehnert M., Karczewski O.
<Astron. Astrophys. 631, A38 (2019)>
=2019A&A...631A..38L 2019A&A...631A..38L (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Energy distributions
Keywords: dust, extinction - galaxies: evolution - galaxies: star formation -
galaxies: formation - infrared: ISM - infrared: stars
Abstract:
We derived the dust properties for 753 local galaxies and examine how
these relate to some of their physical properties. We present the
derived dust emission properties, including model spectral energy
distribution (SEDs), star formation rates (SFRs) and stellar masses,
as well as their relations.
We modelled the global dust-SEDs for 753 galaxies, treated
statistically as an ensemble within a hierarchical Bayesian dust-SED
modelling approach, so as to derive their infrared (IR) emission
properties. To create the observed dust-SEDs, we used a
multi-wavelength set of observations, ranging from near-IR to
far-IR-to-submillimeter wavelengths. The model-derived properties are
the dust masses (Mdust), the average interstellar radiation field
intensities (Uav), the mass fraction of very small dust grains
("QPAH" fraction), as well as their standard deviations. In
addition, we used mid-IR observations to derive SFR and stellar
masses, quantities independent of the dust-SED modelling.
We derive distribution functions of the properties for the galaxy
ensemble and as a function of galaxy type. The mean value of Mdust for
the early-type galaxies (ETGs) is lower than that for the late-type
and irregular galaxies (LTGs and Irs, respectively), despite ETGs and
LTGs having stellar masses spanning across the whole range observed.
The Uav and "QPAH" fraction show no difference among different
galaxy types. When fixing Uav to the Galactic value, the derived
"QPAH" fraction varies across the Galactic value (0.071). The specific
SFR increases with galaxy type, while this is not the case for the
dust-specific SFR (SFR/Mdust), showing an almost constant star
formation efficiency per galaxy type. The galaxy sample is
characterised by a tight relationship between the dust mass and the
stellar mass for the LTGs and Irs, while ETGs scatter around this
relation and tend towards smaller dust masses. While the relation
indicates that Mdust may fundamentally be linked to M*, metallicity
and Uav are the second parameter driving the scatter, which we
investigate in a forthcoming work. We used the extended
Kennicutt-Schmidt (KS) law to estimate the gas mass and the
gas-to-dust mass ratio (GDR). The gas mass derived from the extended
KS law is on average ∼20% higher than that derived from the KS law,
and a large standard deviation indicates the importance of the average
star formation present to regulate star formation and gas supply. The
average GDR for the LTGs and Irs is 370, and including the ETGs gives
an average of 550.
Description:
There are four catalogues, tables A1, A2, B1, B2 - that correspond to
the physical properties and spectral energy distributions (SEDs)
derived from Hierarchical Bayesian fitting of the observed dust-SEDs
of 753 galaxies modelled as an ensemble. Catalogues A1 & A2 correspond
to fitting the mid-IR to submillimetre part of the spectrum, while the
remaining two (B1 and B2) correspond to fitting modified blackbodies.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 134 753 Galaxy sample and derived physical properties
from the model and the calibrations
tablea2.dat 8292 548 Dust-SEDs for the galaxy sample
tableb1.dat 41 753 Dust masses and temperatures from modified
blackbody fits to the galaxy sample's SEDs
tableb2.dat 9045 548 Modified blackbody SEDs for the galaxy sample
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 23 A23 --- Name Name (name)
25- 33 F9.5 deg RAdeg Right ascension (J2000) (RA)
35- 43 F9.5 deg DEdeg Declination (J2000) (Dec)
45- 48 F4.1 --- MType Morphological type (T)
50- 55 F6.3 arcmin D25 Major axis isophote at which optical surface
brightness falls beneath 25mag/arcsec2 (D25)
57- 64 F8.5 Mpc Dist Distance (distance)
66- 71 F6.2 10+6Msun Mdust Dust mass (Mdust)
73- 77 F5.2 10+6Msun e_Mdust Standard deviation of dust mass (sigma_Mdust)
79- 86 F8.2 Sun Uav Average interstellar radiation field,
in U☉ unit (Uav)
88- 95 F8.2 Sun e_Uav Standard deviation of average interstellar
radiation field, in U☉ unit (sigma_Uav)
97-101 F5.3 --- QPAH Q-pah fraction (QPAH)
103-107 F5.3 --- e_QPAH Standard deviation of q-pah fraction
(sigma_QPAH)
109-114 F6.3 Msun/yr SFR ?=- Star formation rate (SFR_pass)
116-121 F6.3 Msun/yr e_SFR ?=- Standard deviation of star formation rate
(sigma(SFRpass))
123-128 F6.3 [Msun] log10M* ?=- Logarithm (base 10) of stellar mass
(log10(M*/Mo))
130-134 F5.3 [Msun] e_log10M* ?=- Standard deviation of the logarithm
(base 10) of stellar mass
(sigma(log10(M*/Mo))
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 E9.3 um lambda Wavelength
10-8292 753E11.4 Lsun Lum Luminosity (G1)
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- Name Name (name)
25- 30 F6.2 10+6Msun Mdust Model-derived dust mass, for the THEMIS dust
grain model (Mdust)
32- 36 F5.2 10+6Msun e_Mdust Standard deviation of dust mass (sigma_Mdust)
38- 39 I2 K T Dust Temparature (T)
41 I1 K e_T Standard deviation of the dust temperature
(sigma_T)
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Byte-by-byte Description of file: tableb2.dat
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Bytes Format Units Label Explanations
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1- 10 E10.4 um lambda Wavelength
11-9046 753E12.4 Lsun Lum Luminosity (G1)
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Global notes:
Note (G1): Luminosity of each galaxy of table A1.
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Acknowledgements:
Sophia Lianou, sophia.thl(at)gmail.com
(End) Patricia Vannier [CDS] 11-Oct-2019