Hard X-ray properties of radio-selected blazars. (arXiv:2004.00477v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Langejahn_M/0/1/0/all/0/1">Marcus Langejahn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kadler_M/0/1/0/all/0/1">Matthias Kadler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilms_J/0/1/0/all/0/1">Jörn Wilms</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Litzinger_E/0/1/0/all/0/1">Eugenia Litzinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kreter_M/0/1/0/all/0/1">Michael Kreter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gehrels_N/0/1/0/all/0/1">Neil Gehrels</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baumgartner_W/0/1/0/all/0/1">Wayne H. Baumgartner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Markwardt_C/0/1/0/all/0/1">Craig B. Markwardt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tueller_J/0/1/0/all/0/1">Jack Tueller</a>
Hard X-ray properties of beamed AGN have been published in the 105-month
Swift/BAT catalog, but there have not been any studies carried out so far on a
well-defined, radio-selected sample of low-peaked blazars in the hard X-ray
band.
Using the statistically complete MOJAVE-1 sample, we aim to determine the
hard X-ray properties of radio-selected blazars, including the enigmatic
gamma-ray-faint type. Also, we aim to determine the contribution of
radio-selected low-peaked blazars to the diffuse CXB.
We determined photon indices, fluxes, and luminosities in the range of 20 keV
– 100 keV of blazars and other extragalactic jets from the MOJAVE-1 sample,
derived from the 105-month Swift/BAT survey. We calculated log N-log S
distributions and the luminosity functions.
The majority of the MOJAVE-1 blazars are found to be hard X-ray emitters
albeit many at low count rates. The log N-log S distribution for the hard X-ray
emission of radio-selected blazars is clearly non-Euclidean, in contrast to the
radio flux density distribution. Approximately 0.2% of the CXB in the 20 keV –
100 keV band can be resolved into MOJAVE-1 blazars.
The peculiar log N-log S distribution disparity might be attributed to
different evolutionary paths in the X-ray and radio bands, as tested by
luminosity-function modeling. X-ray variability can be ruled out as the
dominant contributor. Low-peaked blazars constitute an intrinsically different
source population in terms of CXB contribution compared to similar studies of
X-ray-selected blazars. The hard X-ray flux and spectral index can serve as a
good proxy for the gamma-ray detection probability of individual sources.
Future observations combining deep X-ray survey, for example, with eROSITA, and
targeted gamma-ray observations with CTA can benefit strongly from the tight
connection between these high-energy bands for the different blazar
sub-classes.
Hard X-ray properties of beamed AGN have been published in the 105-month
Swift/BAT catalog, but there have not been any studies carried out so far on a
well-defined, radio-selected sample of low-peaked blazars in the hard X-ray
band.
Using the statistically complete MOJAVE-1 sample, we aim to determine the
hard X-ray properties of radio-selected blazars, including the enigmatic
gamma-ray-faint type. Also, we aim to determine the contribution of
radio-selected low-peaked blazars to the diffuse CXB.
We determined photon indices, fluxes, and luminosities in the range of 20 keV
– 100 keV of blazars and other extragalactic jets from the MOJAVE-1 sample,
derived from the 105-month Swift/BAT survey. We calculated log N-log S
distributions and the luminosity functions.
The majority of the MOJAVE-1 blazars are found to be hard X-ray emitters
albeit many at low count rates. The log N-log S distribution for the hard X-ray
emission of radio-selected blazars is clearly non-Euclidean, in contrast to the
radio flux density distribution. Approximately 0.2% of the CXB in the 20 keV –
100 keV band can be resolved into MOJAVE-1 blazars.
The peculiar log N-log S distribution disparity might be attributed to
different evolutionary paths in the X-ray and radio bands, as tested by
luminosity-function modeling. X-ray variability can be ruled out as the
dominant contributor. Low-peaked blazars constitute an intrinsically different
source population in terms of CXB contribution compared to similar studies of
X-ray-selected blazars. The hard X-ray flux and spectral index can serve as a
good proxy for the gamma-ray detection probability of individual sources.
Future observations combining deep X-ray survey, for example, with eROSITA, and
targeted gamma-ray observations with CTA can benefit strongly from the tight
connection between these high-energy bands for the different blazar
sub-classes.
http://arxiv.org/icons/sfx.gif
