2006A&A...445..843G


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.22CET21:19:45

2006A&A...445..843G - Astronomy and Astrophysics, volume 445, 843-855 (2006/1-3)

Non-thermal cosmic backgrounds from blazars: the contribution to the CMB, X-ray and γ-ray backgrounds.

GIOMMI P., COLAFRANCESCO S., CAVAZZUTI E., PERRI M. and PITTORI C.

Abstract (from CDS):

We present a new assessment of the contribution of the blazar population to the extragalactic background radiation across the electromagnetic spectrum. Our calculations rely on deep blazar radio counts that we have derived by combining several radio and multi-frequency surveys. We show that blazar emission integrated over cosmic time gives rise to a considerable broad-band non-thermal cosmic background that in some parts of the electromagnetic spectrum dominates the extragalactic brightness. We confirm that blazars are the main discrete contributors to the Cosmic Microwave Background (CMB), where we estimate that their integrated emission causes an apparent temperature increase of 5-50µK in the frequency range 50-250GHz. The CMB primordial fluctuation spectrum is contaminated starting at multipole l≃300-600, in the case of a completely random source distribution, or at lower l values if spatial clustering is present. We estimate that well over one hundred-thousand blazars will produce a significant signal in the maps of the upcoming Planck CMB anisotropy mission. Because of a tight correlation between the microwave and the X-ray flux, these sources are expected to be X-ray emitters with flux larger than a few 10–15erg/cm2/s in the soft X-ray band. A large fraction of the foreground sources in current and near-future CMB anisotropy maps could therefore be identified and removed using a multi-frequency approach, provided that a sufficiently deep all-sky X-ray survey will become available in the near future. We show further that blazars are a major constituent of all high energy extragalactic backgrounds. Their contribution is expected to be 11-12% at X-ray frequencies and possibly 100% in the ∼0.5-50MeV band. At higher energies (E>100MeV) the estimated blazar collective emission, obtained by extrapolating their integrated micro-wave flux to the γ-ray band using the SED of EGRET detected sources, overestimates the extragalactic background by a large factor, thus implying that not only blazars dominate the γ-ray sky but also that their average duty cycle at these frequencies must be rather low. Finally, we find that blazars of the HBL type may produce a significant amount of flux at TeV energies.

Abstract Copyright:

Journal keyword(s): radiation mechanisms: non-thermal - BL Lacertae objects: general - quasars: general

Simbad objects: 38

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Number of rows : 38

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 4C 15.05 Bla 02 04 50.41389571 +15 14 11.0436591   21.9 22.1 21.00   ~ 364 1
2 QSO B0208-512 BLL 02 10 46.2000629834 -51 01 01.893312084   17.10 16.93 14.82   ~ 390 1
3 4C 28.07 QSO 02 37 52.40567732 +28 48 08.9900231     18.5 16.99   ~ 513 1
4 QSO B0336-0156 QSO 03 39 30.93778751 -01 46 35.8041062   18.96 18.41 17.33   ~ 515 1
5 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1080 3
6 QSO B0454-463 QSO 04 55 50.7729726039 -46 15 58.684031092   17.89 17.4 16.87   ~ 189 1
7 QSO J0457-2324 QSO 04 57 03.1792314200 -23 24 52.020969479   18.85 18.5 16.56   ~ 345 1
8 QSO B0506-612 QSO 05 06 43.9895985805 -61 09 40.990800301   17.16 16.85 16.9   ~ 167 2
9 QSO B0537-441 BLL 05 38 50.36155219 -44 05 08.9389165   15.77 16.48 16   ~ 798 2
10 QSO J0738+1742 BLL 07 38 07.39374766 +17 42 18.9982302   16.76 16.22 15.78   ~ 901 1
11 7C 082754.29+242103.00 QSO 08 30 52.08619070 +24 10 59.8204032   17.62 17.26 16.30   ~ 472 1
12 4C 71.07 QSO 08 41 24.36526906 +70 53 42.1730054     16.5 16.8   ~ 705 1
13 QSO J0854+2006 BLL 08 54 48.8749311881 +20 06 30.642936668   15.91 15.43 15.56   ~ 2048 1
14 Mrk 421 BLL 11 04 27.3139210166 +38 12 31.798324828   13.50 12.90 8.31   ~ 2418 1
15 Ton 599 QSO 11 59 31.83390975 +29 14 43.8268741   14.80 14.41 17.652 13.39 ~ 808 1
16 QSO B1221-829 Bla 12 24 54.38185745 -83 13 10.1013254   22.5   19.7   ~ 65 2
17 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5389 1
18 PKS 1245-828 Rad 12 49 48.74 -83 04 16.2           ~ 8 2
19 3C 279 QSO 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2742 2
20 QSO B1313-333 QSO 13 16 07.98593995 -33 38 59.1725057   18.04 20.0 17.23   ~ 228 1
21 QSO B1406-076 QSO 14 08 56.48120036 -07 52 26.6664200   20.3 18.4     ~ 272 1
22 QSO B1424-41 QSO 14 27 56.29756536 -42 06 19.4375991   18.48 17.7 16.30   ~ 373 1
23 QSO J1512-0906 QSO 15 12 50.53292491 -09 05 59.8295878   16.74 16.54     ~ 1172 1
24 4C 10.45 QSO 16 08 46.203185540 +10 29 07.77583000   18.5 18.0 18.03   ~ 343 1
25 6C 161147+342017 QSO 16 13 41.0645258703 +34 12 47.911898732   17.98 17.46 17.07   ~ 584 1
26 4C 38.41 QSO 16 35 15.492970280 +38 08 04.50062279   18.14 17.97 17.25   ~ 760 1
27 AT20G J164737.7-643801 Bz? 16 47 37.7415450714 -64 38 00.261725106   20.05   18.70   ~ 21 1
28 ICRF J170336.5-621240 BLL 17 03 36.5416560197 -62 12 40.008612006   18.73   17.58   ~ 80 1
29 4C 51.37 QSO 17 40 36.9779934388 +52 11 43.411910710   18.16 18.5 16.73   ~ 365 1
30 2FGL J1815.6-6407 Bla 18 14 38.690 -64 12 10.08           ~ 20 0
31 ICRF J181935.0-634548 Sy2 18 19 35.00241 -63 45 48.1926   16.80 14.40 13.4   ~ 136 1
32 [VV2006] J192332.2-210433 QSO 19 23 32.18981466 -21 04 33.3330547   15.32 17.50 16.70   ~ 130 2
33 QSO B2052-474 QSO 20 56 16.35981874 -47 14 47.6276461   18.29 19.1 18.07   ~ 266 1
34 NAME BL Lac BLL 22 02 43.2913773726 +42 16 39.978417860   15.66 14.72     ~ 2030 1
35 QSO B2209+236 QSO 22 12 05.96631138 +23 55 40.5438272   19   19.69   ~ 195 1
36 4C 11.69 QSO 22 32 36.40890517 +11 43 50.9040717   17.75 17.33     ~ 995 2
37 3C 454.3 QSO 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2545 2
38 4C 45.51 QSO 23 54 21.68022839 +45 53 04.2365363   20.6 20.6 19.1   ~ 203 1

    Equat.    Gal    SGal    Ecl

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2021.01.22-21:19:45

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