CaltechAUTHORS
  A Caltech Library Service

The High Redshift Blazar S5 0836+71: A Broadband Study

Paliya, Vaidehi S. (2015) The High Redshift Blazar S5 0836+71: A Broadband Study. Astrophysical Journal, 804 (1). Art No. 74. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20160128-132317989

Full text is not posted in this repository. Consult Related URLs below.

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20160128-132317989

Abstract

A broadband study of the high redshift blazar S5 0836+71 (z = 2.172) is presented. Multi-frequency light curves show multiple episodes of X-ray and γ-ray flares, while optical-UV fluxes show little variations. During the GeV outburst, the highest γ-ray flux measured is (5.22 ± 1.10) × 10−6 ph cm^(−2) s^−1 in the range of 0.1-300 GeV, which corresponds to an isotropic γ-ray luminosity of (1.62 ± 0.44) × 1050 erg s^−1, thereby making this as one of the most luminous γ-ray flare ever observed from any blazar. A fast γ-ray flux rising time of ∼3 hours is also noticed which is probably the first measurement of hour scale variability detected from a high redshift (z > 2) blazar. The various activity states of S5 0836+71 are reproduced under the assumption of single zone leptonic emission model. In all the states, the emission region is located inside the broad line region, and the optical-UV radiation is dominated by the accretion disk emission. The modeling parameters suggests the enhancement in bulk Lorentz factor as a primary cause of the γ-ray flare. The high X-ray activity with less variable γ-ray counterpart can be due to emission region to be located relatively closer to the black hole where the dominating energy density of the disk emission results in higher X-ray flux due to inverse-Compton scattering of disk photons.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://iopscience.iop.org/article/10.1088/0004-637X/804/1/74/metaPublisherArticle
http://dx.doi.org/10.1088/0004-637X/804/1/74DOIArticle
Additional Information:© Copyright 2015 IOP Publishing. Received 2015 January 19; accepted 2015 February 25; published 2015 May 4. The author thanks the referee for constructive comments and C.S. Stalin and Sunder Sahayanathan for useful discussions. Substantial help in NuSTAR data analysis received from Michael Parker is also acknowledged. This research has made use of data, software, and/or web tools obtained from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. Part of this work is based on archival data, software, or online services provided by the ASI Science Data Center (ASDC). This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASDC, Italy. This research has also made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). Use of the Hydra cluster at the Indian Institute of Astrophysics is acknowledged.
Group:NuSTAR
Record Number:CaltechAUTHORS:20160128-132317989
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20160128-132317989
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:64051
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:28 Jan 2016 23:13
Last Modified:28 Jan 2016 23:13

Repository Staff Only: item control page