2017A&A...602A..25Z


Query : 2017A&A...602A..25Z

2017A&A...602A..25Z - Astronomy and Astrophysics, volume 602A, 25-25 (2017/6-1)

Expected signatures from hadronic emission processes in the TeV spectra of BL Lacertae objects.

ZECH A., CERRUTI M. and MAZIN D.

Abstract (from CDS):

Context. The wealth of recent data from Imaging Air Cherenkov telescopes (IACTs), ultra-high energy cosmic-ray experiments and neutrino telescopes have fuelled a renewed interest in hadronic emission models for γ-loud blazars.
Aims. We explore physically plausible solutions for a lepto-hadronic interpretation of the stationary emission from high-frequency peaked BL Lac objects (HBLs). The modelled spectral energy distributions are then searched for specific signatures at very high energies that could help to distinguish the hadronic origin of the emission from a standard leptonic scenario.
Methods. By introducing a few basic constraints on parameters of the model, such as assuming the co-acceleration of electrons and protons, we significantly reduced the number of free parameters. We then systematically explored the parameter space of the size of the emission region and its magnetic field for two bright γ-loud HBLs, PKS 2155-304 and Mrk 421. For all solutions close to equipartition between the energy densities of protons and of the magnetic field, and with acceptable jet power and light-crossing timescales, we inspected the spectral hardening in the multi-TeV domain from proton-photon induced cascades and muon-synchrotron emission inside the source. Very-high-energy spectra simulated with the available instrument functions from the future Cherenkov Telescope Array (CTA) were evaluated for detectable features as a function of exposure time, source redshift, and flux level.
Results. A range of hadronic scenarios are found to provide satisfactory solutions for the broad band emission of the sources under study. The TeV spectrum can be dominated either by proton-synchrotron emission or by muon-synchrotron emission. The solutions for HBLs cover a parameter space that is distinct from the one found for the most extreme BL Lac objects in an earlier study. Over a large range of model parameters, the spectral hardening due to internal synchrotron-pair cascades, the "cascade bump", should be detectable for acceptable exposure times with the future CTA for a few nearby and bright HBLs.

Abstract Copyright: © ESO, 2017

Journal keyword(s): radiation mechanisms: non-thermal - astroparticle physics - radiative transfer - gamma rays: galaxies - BL Lacertae objects: individual: PKS 2155-304 - BL Lacertae objects: individual: Mrk 421 - BL Lacertae objects: individual: Mrk 421

Simbad objects: 17

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Number of rows : 17
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 ICRF J015239.6+014717 BLL 01 52 39.6109440384 +01 47 17.385104112     15.12 11.8   ~ 122 1
2 QSO B0229+200 BLL 02 32 48.6148874688 +20 17 17.486717388   18.0 18.00 13.96   ~ 298 1
3 IC 310 rG 03 16 42.9787569912 +41 19 29.615579544   14.3       ~ 256 2
4 QSO B0347-121 BLL 03 49 23.1862105584 -11 59 27.366035532   18.74 18.2 17.46   ~ 209 0
5 6C 070609+591309 BLL 07 10 30.0683697888 +59 08 20.371772544   17.38 16.52 15.1   ~ 209 2
6 7C 080602.89+522749.00 BLL 08 09 49.1868285744 +52 18 58.249938744   16.11 15.59 14.6   ~ 256 2
7 Mrk 421 BLL 11 04 27.3140835504 +38 12 31.798495872   13.50 12.90 8.31   ~ 2566 1
8 6C 121520+302351 BLL 12 17 52.0819904040 +30 07 00.634936872   16.07 15.62 13.47   ~ 449 1
9 WISEA J144357.20-390840.0 BLL 14 43 57.1974184800 -39 08 40.053885612       14.7   ~ 76 1
10 4C 39.49 BLL 16 53 52.21668403 +39 45 36.6088754 14.09 14.15 13.29 8.26   ~ 2065 2
11 6C 172704+501607 BLL 17 28 18.6242294352 +50 13 10.469553996   16.55 15.97 12.95   ~ 350 1
12 QSO B1741+196 BLL 17 43 57.8330083440 +19 35 09.018846384     16.80 12.7   ~ 149 1
13 QSO B1959+650 BLL 19 59 59.8520303688 +65 08 54.652536492     12.8 11.21   ~ 571 2
14 QSO B2005-489 BLL 20 09 25.3903899240 -48 49 53.725051056   15.75 12.81 11.41   ~ 552 2
15 QSO B2155-304 BLL 21 58 52.0652249880 -30 13 32.118447792   13.36 13.09 12.62   ~ 1671 1
16 LEDA 2126234 BLL 22 50 05.7481607616 +38 24 37.193100984     16.00 14.8   ~ 117 1
17 QSO B2344+514 BLL 23 47 04.8372110928 +51 42 17.877513168     15.50 10.7   ~ 425 0

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2023.01.31-08:09:46

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