2022A&A...663A.129N


Query : 2022A&A...663A.129N

2022A&A...663A.129N - Astronomy and Astrophysics, volume 663A, 129-129 (2022/7-1)

Observing the inner parsec-scale region of candidate neutrino-emitting blazars.

NANCI C., GIROLETTI M., ORIENTI M., MIGLIORI G., MOLDON J., GARRAPPA S., KADLER M., ROS E., BUSON S., AN T., PEREZ-TORRES M.A., D'AMMANDO F., MOHAN P., AGUDO I., SOHN B.W., CASTRO-TIRADO A.J. and ZHANG Y.

Abstract (from CDS):


Context. Many questions concerning the nature of astrophysical counterparts of high-energy neutrinos remain unanswered. There is increasing evidence of a connection between blazar jets and neutrino events, with the flare of the γ-ray blazar TXS 0506+056 in spatial and temporal proximity of IC 170922A representing one of the most outstanding associations of high-energy neutrinos with astrophysical sources reported so far.
Aims. With the purpose of characterising potential blazar counterparts to high-energy neutrinos, we analysed the parsec-scale regions of γ-ray blazars in spatial coincidence with high-energy neutrinos, detected by the IceCube Observatory. Specifically, we intended to investigate peculiar radio properties of the candidate counterparts related to the neutrino production, such as radio flares coincident with the neutrino detection or features in jet morphology (limb brightening, transverse structures).
Methods. We collected multi-frequency, very-long-baseline interferometry (VLBI) follow-up observations of candidate counterparts of four high-energy neutrino events detected by IceCube between January 2019 and November 2020, with a focus on γ-ray-associated objects. We analysed their radio characteristics soon after the neutrino arrival in comparison with archival VLBI observations and low-frequency radio observations. We discussed our results with respect to previous statistical works and studies on the case of TXS 0506+056.
Results. We identified and analysed five potential neutrino-emitting blazars in detail. Our results suggest an enhanced state of activity for one source, PKS 1725+123. However, the lack of adequate monitoring prior to the neutrino events was a limitation in tracing radio activity and morphological changes in all the sources.
Conclusions. We suggest that PKS 1725+123 is a promising neutrino source candidate. For the other sources, our results alone do not reveal a strong connection between the radio activity state at the neutrino arrival. A larger number of VLBI and multi-wavelength follow-up observations of neutrino events are now essential to our understanding of the neutrino production mechanisms in astrophysical sources.

Abstract Copyright: © ESO 2022

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

Simbad objects: 27

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Number of rows : 27
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 M 77 Sy2 02 42 40.7091669408 -00 00 47.859690204 9.70 9.61 8.87 10.1 9.9 ~ 4597 2
2 QSO J0509+0541 BLL 05 09 25.9644373872 +05 41 35.333820420 15.32 14.95 14.78 15.12   ~ 452 2
3 IceCube-170922A ev 05 09.7 +05 43           ~ 146 0
4 WISEA J065633.43+053922.7 IR 06 56 33.43 +05 39 22.7           ~ 2 0
5 3FGL J0658.6+0636 BLL 06 58 45.0246246403 +06 37 11.471011970           ~ 44 0
6 NVSS J065916+055252 Rad 06 59 16.72 +05 52 52.9           ~ 1 0
7 7C 103457.3+285040 QSO 10 37 43.83525734 +28 34 59.4594798           ~ 21 1
8 87GB 103758.5+063247 BLL 10 40 31.6262333280 +06 17 21.764932476   20.02 16.8 19.73   ~ 29 1
9 SDSS J104516.30+275133.4 Bla 10 45 16.2975138216 +27 51 33.460668468   19.4   19.3   ~ 12 0
10 4FGL J1045.3+2751 BL? 10 45 21.7 +27 51 05           ~ 8 0
11 IceCube-190704A ev 10 47.4 +27 07           ~ 17 0
12 4FGL J1049.8+2741 rG 10 49 38.7920168088 +27 42 13.037307156           ~ 17 0
13 SDSS J105553.72+103445.9 IR 10 55 53.72208 +10 34 45.9660           ~ 1 0
14 4FGL J1055.8+1034 gam 10 56 47.790 +10 30 28.10           ~ 1 0
15 IceCube-200109A ev 10 58.0 +11 52           ~ 17 0
16 [VV2006] J110303.6+115816 QSO 11 03 03.52983866 +11 58 16.6243929   19.35 19.13     ~ 57 1
17 3FHL J1103.1+1156 Bla 11 03 05.3 +11 57 55           ~ 23 0
18 4FGL J1114.6+1225 Q? 11 14 36.7 +12 27 18           ~ 7 0
19 WISEA J111439.67+122503.7 IR 11 14 39.67 +12 25 03.7           ~ 1 0
20 QSO B1424-41 QSO 14 27 56.29756617 -42 06 19.4376238   18.48 17.7 16.30   ~ 495 1
21 QSO B1502+1041 Bla 15 04 24.97978391 +10 29 39.1985309   18.97 18.56 18.94   ~ 573 1
22 4FGL J1725.5+1312 gam 17 23 14.120 +14 21 00.62           ~ 1 0
23 1RXS J172314.4+142103 X 17 23 14.400 +14 21 02.99           ~ 2 0
24 ICRF J172807.0+121539 QSO 17 28 07.05121409 +12 15 39.4855448     20.0 19.47   ~ 82 1
25 AT 2019dsg ev 20 57 02.970 +14 12 15.86           ~ 96 0
26 IceCube-201114A ev ~ ~           ~ 26 0
27 IceCube-201021A ev ~ ~           ~ 17 0

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