The post-Herschel view of intrinsic AGN emission: constructing templates for galaxy and AGN emission at IR wavelengths

ABSTRACT Measuring the star-forming properties of active galactic nucleus (AGN) hosts is key to our understanding of galaxy formation and evolution. However, this topic remains debated, partly due to the difficulties in separating the infrared (i.e. 1–1000 ${\rm \mu m}$) emission into AGN and star-forming components. Taking advantage of archival far-infrared data from Herschel, we present a new set of AGN and galaxy infrared templates and introduce the spectral energy distribution fitting code iragnsep. Both can be used to measure infrared host galaxy properties, free of AGN contamination. To build these, we used a sample of 100 local (z < 0.3), low-to-high luminosity AGNs (i.e. Lbol$\ \sim \ 10^{42-46}$ erg s−1), selected from the 105-month Swift–BAT X-ray survey, which have archival Spitzer–IRS spectra and Herschel photometry. We first built a set of seven galaxy templates using a sample of 55 star-forming galaxies selected via infrared diagnostics. Using these templates, combined with a flexible model for the AGN contribution, we extracted the intrinsic infrared emission of our AGN sample. We further demonstrate that we can reduce the diversity in the intrinsic shapes of AGN spectral energy distributions down to a set of three AGN templates, of which two represent AGN continuum, and one represents silicate emission. Our results indicate that, on average, the contribution of AGNs to the far-infrared (λ ≳ 50 ${\rm \mu m}$) is not as high as suggested by some recent work. We further show that the need for two infrared AGN continuum templates could be related to nuclear obscuration, where one of our templates appears dominated by the emission of the extended polar dust.

MAIN STAGES OF DEVELOPMENT OF THE INFRARED DIAGNOSTICS METHOD FOR CONTROLLING THE STATE OF TECHNOLOGICAL PIPELINES

The main stages of the development of the method of infrared diagnostics for monitoring the state of technological pipelines are considered.

Infrared monitoring of the dynamics of the local temperature as a symptom of adaptation to hypoxia and efficiency of antihypoxic drugs

The literature review shows that the general body temperature and the local temperature of individual organs of humans and animals have a significant impact on their reaction to the lack of arterial blood, oxygen and anti-hypoxic and anti-ischemic agents. It is shown that human and animal body organs have different resistance to hypoxia. The least resistant to ischemia and hypoxia is the brain, and it is the first hypoxia damaged cerebral cortex. It is shown that with a lack of oxygen, the death of neurons in the brain can be effectively prevented by timely administration of oxygen to the brain and/or lowering its local temperature. However, to date, no technologies have been developed that provide an immediate increase in the concentration of oxygen and/or a decrease in the local temperature in the brain of people while maintaining their performance. Under these conditions, professor V.M. Vinogradov proposed to find the possibility of extending the life of brain cells in conditions of lack of oxygen using drugs that have been called antihypoxants. Technologies of infrared diagnostics of hypoxia, estimation of reserves of adaptation to it and ways of estimation of efficiency of antihypoxants are described.

Infrared Diagnostics of the ISM in the Circumnuclear Environments of the Youngest Radio Galaxies

Here we present a systematic analysis of the mid-infrared properties of young radio galaxies, based on lower-resolution data provided by WISE and IRAS satellites. We restrict our analysis to sources in the earliest phase of radio galaxy evolution, with corresponding ages of the radio structures ≤ 3,000 yrs. In our sample of 29 objects, we find a variety of WISE colors, which suggests that the mid-infrared continua of studied sources are not exclusively contributed to by the circumnuclear dust. A comparison of the total mid-infrared and absorption-corrected X-ray luminosities for our sample reveals a clear correlation between the two bands. This favors the scenario in which the observed X-ray emission of young radio galaxies — at least the high-luminosity ones — originates predominantly in accretion disk corona.