Browsing by Author "Boquien, M."

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    Comprehensive comparison of models for spectral energy distributions from 0.1 μm to 1mm of nearby star-forming galaxies
    (2019) Hunt, L. K.; De Looze, I; Boquien, M.; Nikutta, R.; Rossi, A.; Bianchil, S.; Dale, D. A.; Granato, G. L.; Kennicutt, R. C.; Silva, L.; Ciesla, L.; Relano, M.; Viaene, S.; Brandl, B.; Calzetti, D.; Croxall, K., V; Draine, B. T.; Galametz, M.; Gordon, K. D.; Groves, B. A.; Helou, G.; Herrera-Camus, R.; Hinz, J. L.; Koda, J.; Salim, S.; Sandstrom, K. M.; Smith, J. D.; Wilson, C. D.; Zibetti, S.
    We have fit the far-ultraviolet (FUV) to sub-millimeter (850 mu m) spectral energy distributions (SEDs) of the 61 galaxies from the Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel (KINGFISH). The fitting has been performed using three models: the Code for Investigating GALaxy Evolution (CIGALE), the GRAphite-SILicate approach (GRASIL), and the Multiwavelength Analysis of Galaxy PHYSical properties (MAGPHYS). We have analyzed the results of the three codes in terms of the SED shapes, and by comparing the derived quantities with simple "recipes" for stellar mass (M-star), star-formation rate (SFR), dust mass (M-dust), and monochromatic luminosities. Although the algorithms rely on different assumptions for star-formation history, dust attenuation and dust reprocessing, they all well approximate the observed SEDs and are in generally good agreement for the associated quantities. However, the three codes show very different behavior in the mid-infrared regime: in the 5-10 mu m region dominated by PAH emission, and also between 25 and 70 mu m where there are no observational constraints for the KINGFISH sample. We find that different algorithms give discordant SFR estimates for galaxies with low specific SFR, and that the standard recipes for calculating FUV absorption overestimate the extinction compared to the SED-fitting results. Results also suggest that assuming a "standard" constant stellar mass-to-light ratio overestimates Mstar relative to the SED fitting, and we provide new SED-based formulations for estimating Mstar from WISE W1 (3.4 mu m) luminosities and colors. From a principal component analysis of M-star, SFR, M-dust, and O/H, we reproduce previous scaling relations among Mstar, SFR, and O/H, and find that Mdust can be predicted to within similar to 0.3 dex using only M-star and SFR.
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    SDSS-IV MaNGA: A Star Formation-Baryonic Mass Relation at Kiloparsec Scales
    (2021) Barrera-Ballesteros, J. K.; Heckman, T.; Sanchez, S. F.; Drory, N.; Cruz-Gonzalez, I.; Carigi, L.; Riffel, R. A.; Boquien, M.; Tissera, P.; Bizyaev, D.; Rong, Y.; Boardman, N. F.; Hurtado, P. Alvarez
    Star formation rate density, sigma(SFR), has shown a remarkable correlation with both components of the baryonic mass kiloparsec scales (i.e., the stellar mass density and molecular gas mass density, sigma(*) and sigma(mol), respectively) for galaxies in the nearby universe. In this study, we propose an empirical relation between sigma(SFR) and the baryonic mass surface density (sigma(b) = sigma(mol,Av) + sigma(*), where sigma(mol,Av) is the molecular gas derived from the optical extinction, A(V)) at kiloparsec scales using the spatially resolved properties of the MaNGA survey, the largest sample of galaxies observed via integral field spectroscopy (similar to 8400 objects). We find that sigma(SFR) tightly correlates with sigma(b). Furthermore, we derive an empirical relation between sigma(SFR) and a second-degree polynomial of sigma(b), yielding a one-to-one relation between these two observables. Both sigma(b) and its polynomial form show a stronger correlation and smaller scatter with respect to sigma(SFR) than the relations derived using the individual components of sigma(b). Our results suggest that these three parameters are indeed physically correlated, suggesting a scenario in which the two components of the baryonic mass regulate the star formation activity at kiloparsec scales.