Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 660588.0, MPI für Astronomie / Publikationen_mpia
Chandra X-ray observations of the redshift 1.53 radio-loud quasar 3C 270.1
Authors:Wilkes, B. J.; Lal, D. V.; Worrall, D. M.; Birkinshaw, M.; Haas, M.; Willner, S. P.; Antonucci, R.; Ashby, M. L. N.; Avara, M.; Barthel, P.; Chini, R.; Fazio, G. G.; Hardcastle, M.; Lawrence, C.; Leipski, C.; Ogle, P.; Schulz, B.
Date of Publication (YYYY-MM-DD):2012
Journal Abbrev.:The Astrophysical Journal
Volume:745
Issue / Number:1
Start Page:id. 84
Audience:Not Specified
Abstract / Description:Chandra X-ray observations of the high redshift (z = 1.532) radio-loud quasar 3C 270.1 in 2008 February show the nucleus to have a power-law spectrum, Γ = 1.66 ± 0.08, typical of a radio-loud quasar, and a marginally detected Fe Kα emission line. The data also reveal extended X-ray emission, about half of which is associated with the radio emission from this source. The southern emission is co-spatial with the radio lobe and peaks at the position of the double radio hot spot. Modeling this hot spot, including Spitzer upper limits, rules out synchrotron emission from a single power-law population of electrons, favoring inverse Compton emission with a field of ~11 nT, roughly a third of the equipartition value. The northern emission is concentrated close to the location of a 40° bend where the radio jet is presumed to encounter an external medium. It can be explained by inverse Compton emission involving cosmic microwave background photons with a field of ~3 nT, a factor of 7-10 below the equipartition value. The remaining, more diffuse X-ray emission is harder (HR = -0.09 ± 0.22). With only 22.8 ± 5.6 counts, the spectral form cannot be constrained. Assuming thermal emission with a temperature of 4 keV yields an estimate for the luminosity of 1.8× 1044 erg s-1, consistent with the luminosity-temperature relation of lower-redshift clusters. However, deeper Chandra X-ray observations are required to delineate the spatial distribution and better constrain the spectrum of the diffuse emission to verify that we have detected X-ray emission from a high-redshift cluster.
Free Keywords:quasars: individual: 3C 270.1; X-rays: galaxies: clusters
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://cdsads.u-strasbg.fr/abs/2012ApJ...745...84W
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.