2016A&A...596A..78H


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.12CEST08:23:29

2016A&A...596A..78H - Astronomy and Astrophysics, volume 596A, 78-78 (2016/12-1)

Optical polarization of high-energy BL Lacertae objects.

HOVATTA T., LINDFORS E., BLINOV D., PAVLIDOU V., NILSSON K., KIEHLMANN S., ANGELAKIS E., FALLAH RAMAZANI V., LIODAKIS I., MYSERLIS I., PANOPOULOU G.V. and PURSIMO T.

Abstract (from CDS):

Context. We investigate the optical polarization properties of high-energy BL Lac objects using data from the RoboPol blazar monitoring program and the Nordic Optical Telescope.
Aims. We wish to understand if there are differences between the BL Lac objects that have been detected with the current-generation TeV instruments and those objects that have not yet been detected.
Methods. We used a maximum-likelihood method to investigate the optical polarization fraction and its variability in these sources. In order to study the polarization position angle variability, we calculated the time derivative of the electric vector position angle (EVPA) change. We also studied the spread in the Stokes Q/I-U/I plane and rotations in the polarization plane.
Results. The mean polarization fraction of the TeV-detected BL Lacs is 5%, while the non-TeV sources show a higher mean polarization fraction of 7%. This difference in polarization fraction disappears when the dilution by the unpolarized light of the host galaxy is accounted for. The TeV sources show somewhat lower fractional polarization variability amplitudes than the non-TeV sources. Also the fraction of sources with a smaller spread in the Q/I-U/I plane and a clumped distribution of points away from the origin, possibly indicating a preferred polarization angle, is larger in the TeV than in the non-TeV sources. These differences between TeV and non-TeV samples seem to arise from differences between intermediate and high spectral peaking sources instead of the TeV detection. When the EVPA variations are studied, the rate of EVPA change is similar in both samples. We detect significant EVPA rotations in both TeV and non-TeV sources, showing that rotations can occur in high spectral peaking BL Lac objects when the monitoring cadence is dense enough. Our simulations show that we cannot exclude a random walk origin for these rotations.
Conclusions. These results indicate that there are no intrinsic differences in the polarization properties of the TeV-detected and non-TeV-detected high-energy BL Lac objects. This suggests that the polarization properties are not directly related to the TeV-detection, but instead the TeV loudness is connected to the general flaring activity, redshift, and the synchrotron peak location.

Abstract Copyright: © ESO, 2016

Journal keyword(s): polarization - BL Lacertae objects: general - galaxies: jets

VizieR on-line data: <Available at CDS (J/A+A/596/A78): sources.dat tev.dat ctrl.dat>

Simbad objects: 52

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Number of rows : 52

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 QSO B0033+595 BLL 00 35 52.554 +59 50 04.19     19.5 17.2   ~ 136 2
2 3FHL J0114.8+1324 BLL 01 14 52.7764460837 +13 25 37.530185455 17.20 16.98 16.86 17.2   ~ 39 0
3 3FHL J0136.5+3906 BLL 01 36 32.5981369228 +39 05 59.196637223     15.80 15.5   ~ 100 1
4 3FHL J0152.6+0147 BLL 01 52 39.6108342199 +01 47 17.385034188     15.12 11.8   ~ 107 1
5 3C 66A BLL 02 22 39.6111630878 +43 02 07.797284539   15.71 15.21 14.5   ~ 796 1
6 QSO B0229+200 BLL 02 32 48.6154943841 +20 17 17.493345304   18.0 18.00     ~ 259 3
7 QSO B0317+18 BLL 03 19 51.8081953152 +18 45 34.570122144     18.12     ~ 186 0
8 QSO B0414+009 BLL 04 16 52.4945787354 +01 05 23.896410061   16.86 16.38 16   ~ 244 0
9 QSO B0502+675 BLL 05 07 56.1461168342 +67 37 24.302255568     17.0 17.2   ~ 141 1
10 ICRF J052145.9+211251 BLL 05 21 45.9656490719 +21 12 51.454716382           ~ 76 1
11 87GB 064555.8+152016 BLL 06 48 47.6489790744 +15 16 24.797273299       16.2   ~ 61 0
12 QSO B0647+250 BLL 06 50 46.4902391458 +25 02 59.623980609 16.17 15.97 15.79 16.3   ~ 109 2
13 6C 070609+591309 BLL 07 10 30.0681446132 +59 08 20.369016804   17.38 16.52 15.1   ~ 182 2
14 7C 080602.89+522749.00 BLL 08 09 49.1866520010 +52 18 58.249265842   16.11 15.59 14.6   ~ 225 2
15 3FHL J0849.1+6606 Bla 08 48 54.6216986318 +66 06 09.504251737       17.2   ~ 26 1
16 3FHL J1037.6+5711 BLL 10 37 44.3078863654 +57 11 55.629763116   17.05 16.54 16.7   ~ 87 1
17 Mrk 421 BLL 11 04 27.3139210166 +38 12 31.798324828   13.50 12.90 8.31   ~ 2383 1
18 6C 113337+702604 BLL 11 36 26.4084430 +70 09 27.307497   15.16 14.49 10.51   ~ 316 1
19 6C 120027+604804 BLL 12 03 03.5067891358 +60 31 19.159546191   16.82 16.04     ~ 95 1
20 6C 121520+302351 BLL 12 17 52.0819140772 +30 07 00.636792927   16.07 15.62 13.47   ~ 406 1
21 QSO B1218+304 BLL 12 21 21.9427463316 +30 10 37.161573795   16.50 15.85 15.7   ~ 389 1
22 7C 1219+2830 BLL 12 21 31.6902446545 +28 13 58.500383827   16.81 16.11 14.24   ~ 779 1
23 QSO B1221+24 BLL 12 24 24.1863956209 +24 36 23.500844570   17.93 17.37     ~ 117 0
24 7C 1424+2401 BLL 14 27 00.3918388878 +23 48 00.035406946 14.52 14.34 14.95 14.5   ~ 287 1
25 QSO B1426+428 BLL 14 28 32.6090831425 +42 40 21.050020627   16.95 16.45 14.4   ~ 456 2
26 QSO B1440+122 BLL 14 42 48.276582 +12 00 40.37487   18.34 17.63 15.2   ~ 137 3
27 QSO B1542+614 BLL 15 42 56.9436911925 +61 29 55.347789879   16.9 16.25 16.6   ~ 96 1
28 QSO B1553+113 BLL 15 55 43.0439413597 +11 11 24.365587666 14.91 14.72 14.57 13.99   ~ 420 1
29 7C 1557+5633 BLL 15 58 48.2888061057 +56 25 14.120355021   18.08 17.54 17.2   ~ 64 1
30 3FHL J1649.4+5235 BLL 16 49 24.9913719434 +52 35 14.998703055       17   ~ 30 1
31 4C 39.49 BLL 16 53 52.21668494 +39 45 36.6089458 14.09 14.15 13.29 8.26   ~ 1914 2
32 QSO B1722+119 BLL 17 25 04.34087 +11 52 15.4688   16.29 15.77 14.45   ~ 165 1
33 6C 172704+501607 BLL 17 28 18.6239898055 +50 13 10.472390025   16.55 15.97 12.95   ~ 321 1
34 QSO B1741+196 BLL 17 43 57.8328487 +19 35 09.020130     16.80 12.7   ~ 125 1
35 3FHL J1754.1+3212 BLL 17 54 11.7992936028 +32 12 23.056109411           ~ 34 1
36 2MASS J18092544+2041308 BLL 18 09 25.4517775680 +20 41 30.905165038           ~ 26 0
37 7C 181142.79+314318.00 BLL 18 13 35.2028793055 +31 44 17.620197311     17.4 15.2   ~ 72 1
38 2MASS J18362123+3136268 BLL 18 36 21.2402542219 +31 36 26.726597152           ~ 33 1
39 3FHL J1838.8+4802 BLL 18 38 49.1551023201 +48 02 34.271793300     17.60 16.2   ~ 60 0
40 2MASS J18414705+3218389 BLL 18 41 47.0423857944 +32 18 39.145743164           ~ 31 0
41 ICRF J190311.6+554038 BLL 19 03 11.6079210800 +55 40 38.452291005   18.1   16.4   ~ 65 1
42 2FHL J1944.1+2117 AG? 19 43 56.200 +21 18 22.95           ~ 56 1
43 QSO B1959+650 BLL 19 59 59.8525497024 +65 08 54.651170114     12.8 11.21   ~ 501 2
44 MAGIC J2001+435 gam 20 01 13.50 +43 53 02.8           ~ 17 0
45 QSO B2012-017 BLL 20 15 15.1578097011 -01 37 32.562261204 18.08 17.86 17.61 16.5   ~ 70 1
46 ICRF J202235.5+761126 BLL 20 22 35.5758679021 +76 11 26.174404015     18.10 17.54   ~ 69 1
47 3FHL J2131.5-0914 BLL 21 31 35.4235494934 -09 15 23.693366736     18.00 17.5   ~ 50 0
48 3FHL J2149.8+0322 BLL 21 49 41.8699312351 +03 22 51.429181794 18.01 17.72 17.31     ~ 34 0
49 NAME BL Lac BLL 22 02 43.2913773726 +42 16 39.978417860   15.66 14.72     ~ 2006 1
50 2MASX J22500577+3824371 BLL 22 50 05.7480525271 +38 24 37.195160708     16.00 14.8   ~ 97 1
51 2FGL J2341.7+8016 BLL 23 40 54.2292443034 +80 15 16.022633243     18.90 16.8   ~ 38 0
52 QSO B2344+514 BLL 23 47 04.8376303689 +51 42 17.875387216     15.50 10.7   ~ 387 0

    Equat.    Gal    SGal    Ecl

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2020.07.12-08:23:29

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