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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20191001T123000
DTEND;TZID=Atlantic/Canary:20191001T133000
UID:iactalks-1325
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1325
CREATED:2019-10-01T12:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Study of the diversity of AGN dust models
DESCRIPTION:Study of the diversity of AGN dust models\nDr. Omaira González
  Martín\n\n The dust component of active galactic nuclei (AGN) produces a
  broad  infrared spectral energy distribution (SED), whose power and shape
   depends on the fraction of the source absorbed, and the geometry of the 
  absorber respectively. This emitting region is expected to be  concentrat
 ed within the inner ∼5 pc of the AGN which makes almost  impossible to
  image it with the current instruments. The study of the  infrared SED by 
 comparison between infrared AGN spectra and predicted  models is one of th
 e few ways to infer the properties of the AGN dust.  We explore a set of s
 ix dusty models of AGN with available SEDs, namely  Fritz et al. (2006), N
 enkova et al. (2008B), Hoenig & Kishimoto  (2010), Siebenmorgen et al.
  (2015), Stalevski et al. (2016), and Hoenig  & Kishimoto (2017). They
  cover a wide range of morphologies, dust  distributions, and compositions
 .  We explore the discrimination among models and parameter restriction  u
 sing synthetic spectra (Gonzalez-Martin et al. 2019A), and perform  spectr
 al fitting of a sample of 110 AGN with Spitzer/IRS drawn from the  Swift/B
 AT survey (Gonzalez-Martin et al. 2019B). Our conclusion is that  most of 
 these models can be discriminated using only mid-infrared  spectroscopy as
  long as the host galaxy contribution is less than 50%.  The best model de
 scribing the sample is the clumpy disk-wind model by  Hoenig & Kishimo
 to (2017). However, large residuals are shown  irrespective of the model u
 sed, indicating that AGN dust is more complex  than models. We found that 
 the parameter space covered by models is not  completely adequate. This ta
 lk will give tips for observers and  modelers to actually answer the quest
 ion: how is the dust arrange in  AGN? This question will be one of the mai
 n subjects of future research  using JWST in the AGN field.
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