Authors:
Ivano Baronchelli, Ivano Baronchelli, Ivano Baronchelli, G. Rodighiero, Harry I. Teplitz, Claudia Scarlata, Alberto Franceschini, S. Berta, Laia Barrufet, Mattia Vaccari, Mattia Vaccari, Matteo Bonato, Laure Ciesla, A. Zanella, R. Carraro, R. Carraro (...)
Ivano Baronchelli, Ivano Baronchelli, Ivano Baronchelli, G. Rodighiero, Harry I. Teplitz, Claudia Scarlata, Alberto Franceschini, S. Berta, Laia Barrufet, Mattia Vaccari, Mattia Vaccari, Matteo Bonato, Laure Ciesla, A. Zanella, R. Carraro, R. Carraro, Chiara Mancini, A. Puglisi, A. Puglisi, M. A. Malkan, Simona Mei, Simona Mei, Simona Mei, Lucia Marchetti, Lucia Marchetti, Lucia Marchetti, James W. Colbert, Chris Sedgwick, Steve Serjeant, Chris Pearson, Chris Pearson, Chris Pearson, M. Radovich, A. Grado, L. Limatola, Giovanni Covone
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Abstract:
For a sample of star forming galaxies in the redshift interval 0.15$<$z$<$0.3, we study how both the relative strength of the AGN infra-red emission, compared to that due to the star formation (SF), and the numerical fraction of AGNs, change as a function of the total stellar mass of the hosting galaxy group (M$^{*}_{\mathrm{group}}$), between $10^{10.25}$ and $10^{11.9}$M$_{\odot}$. Using a multi-component SED fitting analysis, we separate the contribution of stars, AGN torus and star formation to the total emission at different wavelengths. T (...)
For a sample of star forming galaxies in the redshift interval 0.15$<$z$<$0.3, we study how both the relative strength of the AGN infra-red emission, compared to that due to the star formation (SF), and the numerical fraction of AGNs, change as a function of the total stellar mass of the hosting galaxy group (M$^{*}_{\mathrm{group}}$), between $10^{10.25}$ and $10^{11.9}$M$_{\odot}$. Using a multi-component SED fitting analysis, we separate the contribution of stars, AGN torus and star formation to the total emission at different wavelengths. This technique is applied to a new multi-wavelength data-set in the SIMES field (23 not redundant photometric bands), spanning the wavelength range from the UV (GALEX) to the far-IR (Herschel) and including crucial AKARI and WISE mid-IR observations (4.5 \mu m$<\lambda<$24 \mu m), where the BH thermal emission is stronger. This new photometric catalog, that includes our best photo-z estimates, is released through the NASA/IPAC Infrared Science Archive (IRSA). Groups are identified through a friends of friends algorithm ($\sim$62% purity, $\sim$51% completeness). We identified a total of 45 galaxies requiring an AGN emission component, 35 of which in groups and 10 in the field. We find BHAR$\propto ($M$^{*}_{\mathrm{group}})^{1.21\pm0.27}$ and (BHAR/SFR)$\propto ($M$^{*}_{\mathrm{group}})^{1.04\pm0.24}$ while, in the same range of M$^{*}_{\mathrm{group}}$, we do not observe any sensible change in the numerical fraction of AGNs. Our results indicate that the nuclear activity (i.e. the BHAR and the BHAR/SFR ratio) is enhanced when galaxies are located in more massive and richer groups.
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