J/A+A/609/A30 Monochromatic conversion factors to LIR & Mdust (Schreiber+, 2018)
Dust temperature and mid-to-total infrared color distributions for star-forming
galaxies at 0 < z < 4.
Schreiber C., Elbaz D., Pannella M., Wang T., Ciesla L., Franco M.
<Astron. Astrophys. 609, A30 (2018)>
=2018A&A...609A..30S 2018A&A...609A..30S (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Galaxies, IR
Keywords: galaxies: evolution - galaxies: ISM - galaxies: statistics -
infrared: galaxies - submillimeter: galaxies
Abstract:
We present a new, publicly available library of dust spectral energy
distributions (SEDs). These SEDs are characterized by only three
parameters: the dust mass (Mdust), the dust temperature (Tdust), and
the mid-to-total infrared color (IR8=LIR/L8). The latter measures the
relative contribution of polycyclic aromatic hydrocarbon (PAH)
molecules to the total infrared luminosity. We used this library to
model star-forming galaxies at 0.5<z<4 in the deep CANDELS fields,
using both individual detections and stacks of Herschel and ALMA
imaging, and extending this sample to z=0 using the Herschel Reference
Survey. At first order, the dust SED of a galaxy was observed to be
independent of stellar mass, but evolving with redshift. We found
trends of increasing Tdust and IR8 with redshift and distance from the
SFR-M* main sequence, and quantified for the first time their
intrinsic scatter. Half of the observed variations of these parameters
was captured by the above empirical relations, and after subtracting
the measurement errors we found residual scatters of
δTdust/Tdust=12% and δlogIR8=0.18dex. We observed second
order variations with stellar mass: massive galaxies
(M*>10^119M☉) at z≤1 have slightly lower temperatures
indicative of a reduced star formation efficiency, while low mass
galaxies (M*<1010M☉) at z≥1 showed reduced PAH emission,
possibly linked to their lower metallicities. Building on these
results, we constructed high-fidelity mock galaxy catalogs to predict
the accuracy of infrared luminosities and dust masses determined using
a single broadband measurement. Using a single James Webb Space
Telescope (JWST) MIRI band, we found that LIR is typically uncertain
by 0.15dex, with a maximum of 0.25dex when probing the rest-frame 8um,
and this is not significantly impacted by typical redshift
uncertainties. On the other hand, we found that ALMA bands 8 to 7 and
6 to 3 measured the dust mass at better than 0.2 and 0.15dex,
respectively, and independently of redshift, while bands 9 to 6 only
measured LIR at better than 0.2dex at z>1, 3.2, 3.8, and 5.7,
respectively. Starburst galaxies had their LIR significantly
underestimated when measured by a single JWST or ALMA band, while
their dust mass from a single ALMA band were moderately overestimated.
This dust library and the results of this paper can be used
immediately to improve the design of observing proposals, and
interpret more accurately the large amount of archival data from
Spitzer, Herschel and ALMA.
Description:
These tables contain conversion factors to translate observed fluxes
(Sν) or luminosities (ν*Lν) into total infrared luminosity (LIR)
and dust mass (Mdust). The conversion factors are provided for the
most commonly used ALMA bands (Band 3 to Band 9) and all JWST MIRI
broad bands (F777W to F2550W). These factors are tabulated as a
function of redshift. For each conversion factor, the tables also
provide the logarithmic uncertainty on the conversion (in dex), which
reflects the diversity in spectral shape. These data were calibrated
on the deep Spitzer and Herschel observations of the CANDELS fields,
as well as early ALMA observations. They are therefore valid for
galaxies of masses close to 1010M☉ and above.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 89 24 ALMA flux to LIR (LIR/Snu)
tablea2.dat 89 24 ALMA flux to Mdust (Mdust/Snu)
tablea3.dat 89 119 JWST luminosity to LIR (LIR/nuLnu)
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Byte-by-byte Description of file: tablea1.dat tablea2.dat tablea3.dat
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Bytes Format Units Label Explanations
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1- 4 F4.2 -- z Redshift
6- 11 F6.3 10+12Lsun/mJy c9 ?=- Conversion from ALMA Band 9 to LIR
13- 16 F4.2 [-] u9 ?=- Logarithmic uncertainty for ALMA Band 9
18- 23 F6.3 10+12Lsun/mJy c8 ?=- Conversion from ALMA Band 8 to LIR
25- 28 F4.2 [-] u8 ?=- Logarithmic uncertainty for ALMA Band 8
30- 35 F6.3 10+12Lsun/mJy c7 ?=- Conversion from ALMA Band 7 to LIR
37- 40 F4.2 [-] u7 ?=- Logarithmic uncertainty for ALMA Band 7
42- 47 F6.3 10+12Lsun/mJy c6 ?=- Conversion from ALMA Band 6 to LIR
49- 52 F4.2 [-] u6 ?=- Logarithmic uncertainty for ALMA Band 6
54- 59 F6.3 10+12Lsun/mJy c5 ?=- Conversion from ALMA Band 5 to LIR
61- 64 F4.2 [-] u5 ?=- Logarithmic uncertainty for ALMA Band 5
66- 71 F6.3 10+12Lsun/mJy c4 ?=- Conversion from ALMA Band 4 to LIR
73- 76 F4.2 [-] u4 ?=- Logarithmic uncertainty for ALMA Band 4
78- 84 F7.3 10+12Lsun/mJy c3 ?=- Conversion from ALMA Band 3 to LIR
86- 89 F4.2 [-] u3 ?=- Logarithmic uncertainty for ALMA Band 3
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Acknowledgements:
Corentin Schreiber, cschreib(at)strw.leidenuniv.nl
(End) Patricia Vannier [CDS] 30-Oct-2017