dc.contributor.author |
Paliya, Vaidehi S |
|
dc.date.accessioned |
2020-11-12T15:05:01Z |
|
dc.date.available |
2020-11-12T15:05:01Z |
|
dc.date.issued |
2015-05-01 |
|
dc.identifier.citation |
The Astrophysical Journal, Vol. 804, No. 1, 74 |
en_US |
dc.identifier.issn |
0004-637X |
|
dc.identifier.uri |
http://prints.iiap.res.in/handle/2248/6950 |
|
dc.description |
Restricted Access © IOP Publishing http://dx.doi.org/10.1088/0004-637X/804/1/74 |
en_US |
dc.description.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 one of the most luminous γ-ray flares ever observed from any blazar. A fast γ-ray flux rising time of ∼3 hr 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 the single-zone leptonic emission model. In all 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 suggest the enhancement in bulk Lorentz factor as a primary cause of the γ-ray flare. The high X-ray activity with a less variable γ-ray counterpart can be due to the emission region being 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. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
IOP Publishing |
en_US |
dc.subject |
Galaxies: active |
en_US |
dc.subject |
Galaxies: jets |
en_US |
dc.subject |
Galaxies: high-redshift |
en_US |
dc.subject |
Quasars: individual (S5 0836+71) |
en_US |
dc.title |
The high-redshift blazar S5 0836+71: a broadband study |
en_US |
dc.type |
Article |
en_US |