Studies on the reactivation of bacteria photodamaged by an angular furocoumarin: Angelicin

Modelling galaxy and AGN evolution in the infrared: black hole accretion versus star formation activity

“…Spiral galaxies contribute only to very low redshifts, while SB galaxies peak at similar z to that of LLAGNs, though the number of ‘pure’ SB galaxies is much lower. The redshift distribution shown in the plot is obtained from the combination of the redshift distributions in three different surveys (COSMOS, Le Floc’h et al 2009, and GOODS‐N and ‐S, Rodighiero et al 2010), which were all in reasonably good agreement with our model.…”

“…As shown in Fig. 7, the agreement between the data and the model is remarkably good also at 24 μm, since the model is able to reproduce well the source counts, the z ‐distributions and the luminosity function in different redshift intervals (data from Rodighiero et al 2010). Note that, according to our model, the peak observed in the counts at S 24 μm ≃ 0.3 mJy is made of mainly galaxies containing a LLAGN, with a minor contribution also from the AGN2 population.…”

“…Lower panels: rest‐frame LF at 24 μm in different redshift intervals: model expectations (coloured curves as in Fig. 5) compared to observed data in the VVDS+GOODS fields (black circles; Rodighiero et al 2010).…”

“…5) and observed by Spitzer (magenta filled circles: Papovich et al 2004; green filled triangles: Shupe et al 2008; grey‐shaded area: uncertainty region of the weighted averaged counts from the two surveys). Upper right‐hand panel: redshift distribution of the 24‐μm sources to a flux density S 24 μm = 0.15 mJy: total (black line) and decomposed into populations, compared to the combined observed data (grey‐shaded area) from the COSMOS (Le Floc’h et al 2009), GOODS‐S and GOODS‐N fields (Rodighiero et al 2010). Lower panels: rest‐frame LF at 24 μm in different redshift intervals: model expectations (coloured curves as in Fig.…”

“…The 15‐μm source counts have also been constrained separately for the different populations using the ELAIS‐S1 data. The redshift and luminosity distributions have been constrained by using the ELAIS‐S1 spectroscopic redshifts (La Franca et al 2004) at 15 μm and the GOODS‐S and ‐N (Rodighiero et al 2010) and COSMOS (Le Floc’h et al 2009) spectroscopic and photometric redshifts at different flux density levels at 24 μm. Using the La Franca et al (2004) spectroscopic sample and the SED‐based classification of Gruppioni et al (2008), we have been able to separately constrain the redshift and luminosity distributions of each population at 15 μm, while at 24 μm the comparison has been performed on the total distributions only, since the 24‐μm samples available had no classified objects through SED fitting as we would need for a direct match by populations.…”