English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/170313
logo share SHARE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL | DATACITE
Exportar a otros formatos:


Average iron line emission from distant AGN

AuthorsCorral, Amalia ; Page, M. J.; Carrera, Francisco J. ; Barcons, Xavier ; Mateos, Silvia ; Ebrero, Jacobo ; Krumpe, M.; Schwope, A.; Tedds, J. A.; Watson, M. G.
Issue Date2010
PublisherSpringer Nature
CitationHighlights of Spanish Astrophysics V: 273 (2010)
SeriesAstrophysics and Space Science Proceedings 52
AbstractWe have developed a new method to construct a high SNR X-ray average spectrum for type 1 and type 2 AGN in order to measure the main properties of the Fe Kα emission line. Our method takes into account all the possible contributions to the continuum around the emission line, and an estimate of the significance of any excursion above this continuum can be obtained from it. We applied this method to the identified AGN within AXIS and XWAS, 606 type 1 and 117 type 2 AGN, and obtained average spectra for both AGN types. We found an unresolved emission line on the final average spectrum of type 1 and 2 AGN with an EW ∼ 100 eV, corresponding to neutral or low-ionization Fe Kα emission, thus emitted far from the central source. We also found that the EW of this narrow line becomes weaker as the luminosity increases, the so-called Iwasawa–Taniguchi effect. A clear relativistic component in the Fe Kα line is not present in the average spectra and the continuum is best represented by a mixture of absorbed power laws plus a moderate reflection component for type 1 AGN. In the case of type 2 AGN, the statistics turned out to be insufficient to distinguish between a reflection component and a relativistic line. We estimated the EW of any relativistic contribution to be < 400 eV and < 300 eV at 3σ confidence level for type 1 and type 2 AGN, respectively. Our results are in excellent agreement with studies of local AGN, whereas we obtain a much lower value for the relativistic line EW than studies at higher redshifts.
DescriptionResumen del trabajo presentado al Eighth Scientific Meeting of the Spanish Astronomical Society (Sociedad Española de Astronomía, SEA), celebrado en Santander del 7 al 11 de julio de 2008.
Identifiersdoi: 10.1007/978-3-642-11250-8_36
isbn: 978-3-642-11249-2
Appears in Collections:(IFCA) Libros y partes de libros
Files in This Item:
File Description SizeFormat 
accesoRestringido.pdf15,38 kBAdobe PDFThumbnail
Show full item record
Review this work

WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.