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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 (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:
FileName Lrecl Records Explanations
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)
Byte-by-byte Description of file: tablea1.dat tablea2.dat tablea3.dat
Bytes Format Units Label Explanations
1- 4 F4.2 -- z Redshift 6- 11 F6.3 10+12.Lsun/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+12.Lsun/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+12.Lsun/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+12.Lsun/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+12.Lsun/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+12.Lsun/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+12.Lsun/mJy c3 ?=- Conversion from ALMA Band 3 to LIR 86- 89 F4.2 [-] u3 ?=- Logarithmic uncertainty for ALMA Band 3
Acknowledgements: Corentin Schreiber, cschreib(at)strw.leidenuniv.nl
(End) Patricia Vannier [CDS] 30-Oct-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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