Science-advisor
REGISTER info/FAQ
Login
username
password
     
forgot password?
register here
 
Research articles
  search articles
  reviews guidelines
  reviews
  articles index
My Pages
my alerts
  my messages
  my reviews
  my favorites
 
 
Stat
Members: 3645
Articles: 2'506'133
Articles rated: 2609

27 April 2024
 
  » arxiv » 1506.6182

 Article overview



3C 273 with NuSTAR: Unveiling the AGN
Kristin K. Madsen ; Felix Fürst ; Dominic J. Walton ; Fiona A. Harrison ; David R. Ballantyne ; Steve E. Boggs ; Laura W. Brenneman ; Finn E. Christensen ; William W. Craig ; Andrew C. Fabian ; Karl Forster ; Brian W. Grefenstette ; Matteo Guainazzi ; Charles J. Hailey ; Greg M. Madejski ; Giorgio Matt ; Daniel Stern ; William W. Zhang ;
Date 20 Jun 2015
AbstractWe present results from a 244 ks $NuSTAR$ observation of 3C 273, obtained during a cross-calibration campaign with the $Chandra$, $INTEGRAL$, $Suzaku$, $Swift$, and $XMM-Newton$ observatories. We show that the spectrum, when fit with a power-law model using data from all observatories except $INTEGRAL$ over the 1-78 keV band, leaves significant residuals in the $NuSTAR$ data between 30-78 keV. The $NuSTAR$ 3-78 keV spectrum is well-described by an exponentially cutoff power-law ($Gamma = 1.646 pm 0.006$, E$_mathrm{cutoff} = 202_{-34}^{+51}$ keV) with a weak reflection component from cold, dense material. There is also evidence for a weak ($EW = 23 pm 11$ eV) neutral iron line. We interpret these features as arising from coronal emission plus reflection off an accretion disk or distant material. Beyond 80 keV $INTEGRAL$ data show clear excess flux relative to an extrapolation of the AGN model fit to $NuSTAR$. This high-energy power-law is consistent with the presence of a beamed jet, which begins to dominate over emission from the inner accretion flow at 30-40 keV. Modeling the jet as a power-law, we find the coronal component is fit by $Gamma_mathrm{AGN} = 1.638 pm 0.045$, $E_mathrm{cutfoff} = 47 pm 15$ keV, and jet photon index by $Gamma_mathrm{jet} = 1.05 pm 0.4$. We applied comptonizing coronal electron plasma models to place constraints on the plasma temperature and optical depth. Finally, we investigate the variability and find an inverse correlation between flux and $Gamma$. We interpret this hardening of the spectrum with increasing flux to be due to the jet.
Source arXiv, 1506.6182
Services Forum | Review | PDF | Favorites   
 
Visitor rating: did you like this article? no 1   2   3   4   5   yes

No review found.
 Did you like this article?

This article or document is ...
important:
of broad interest:
readable:
new:
correct:
Global appreciation:

  Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.

browser Mozilla/5.0 AppleWebKit/537.36 (KHTML, like Gecko; compatible; ClaudeBot/1.0; +claudebot@anthropic.com)






ScienXe.org
» my Online CV
» Free


News, job offers and information for researchers and scientists:
home  |  contact  |  terms of use  |  sitemap
Copyright © 2005-2024 - Scimetrica