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Table A.1

TANAMI VLBI observed sources.

Namea Common namea Classb z c First epoch B16d Radio γ-ray Inside HESE(> 100 TeV)
image samplee samplef R 50

0047–579 [HB89] 0047–579 Q 1.797 Paper I Y Y
0055–328 PKS 0055–328 B 1.370 This Work Y
0144–522 PKS 0144–522 G 0.098 This Work
0208–512 [HB89] 0208–512 Q 0.999 Paper I Y Y Y
0227–369 PKS 0227–369 Q 2.115 This Work Y
0235–618 PKS 0235–618 Q 0.465 This Workh HESE-20
0244–470 PKS 0244–470 Q 1.385 This Work Y Y
0302–623 PKS 0302–623 Q 1.351 This Workh Y HESE-20
0308–611 PKS 0308–611 Q 1.480 This Workh Y HESE-20
0332–376 PMN J0334–3725 B >0.39 This Work Y
0332–403 [HB89] 0332–403 B 1.351 Paper I Y Y Y
0402–362 PKS 0402–362 Q 1.417 This Work Y Y
0405–385 [HB89] 0405–385 Q 1.285 Paper I Y
0412–536 PMNJ0413–5332 Q 1.024 This Work Y
0426–380 PKS 0426–380 Q 1.110 This Work Y Y
0438–436 [HB89] 0438–436 Q 2.863 Paper I Y Y
0447–439 PKS 0447–439 B This Work Y Y
0454–463 [HB89] 0454–463 Q 0.853 Paper I Y Y
0506–612 [HB89] 0506–612 Q 1.093 Paper I Y
0516–621 PKS 0516–621 Q 1.300 This Work Y
0518–458 Pic A G 0.035 Paper I Y
0521–365 ESO 362– G 021 G 0.055 Paper I Y Y Y
0524–485 PKS 0524–485 Q 1.300 This Work Y
0527–359 PMNJ0529–3555 U 0.323 This Work Y
0530–485 PMNJ0531–4827 Q This Work Y
0537–441 [HB89] 0537–441 Q 0.894 Paper I Y Y Y
0625–354 PKS 0625–35 B 0.055 Paper I Y Y
0637–752 [HB89] 0637–752 Q 0.653 Paper I Y Y HESE-30
0646–306 PKS 0646–306 Q 0.455 This Work HESE-39
0700–661 PKS 0700–661 B >0.39 This Work Y
0717–432 PMN J0718–4319 U This Work Y
0736–770 PKS0736–770 Q This Work Y HESE-30
0745–330 PKS0745–330 U This Work Y
0812–736 PMN J0810–7530 U This Work Y HESE-30
0902–350 1FGLJ0904.7–3514 U This Work
0943–761 PKS 0943–76 G 0.270 j
1057–797 PKS 1057–79 B 0.581 This Work Y
1101–536 PKS 1101–536 B >0.15 Krauß et al. (2015) Y HESE-4
1104–445 [HB89] 1104–445 Q 1.598 Paper I Y Y HESE-4
1144–379 [HB89] 1144–379 Q 1.048 Paper I Y
1257–326 PKS 1257–326 Q 1.256 Paper I Y
1258–321 ESO443–G024 G 0.017 This Work Y
1313–333 [HB89] 1313–333 Q 1.210 Paper I Y
1322–428 Cen A G 0.002 Paper I Y Y HESE-35
1323–526 PMN J1326–5256 B >0.24 Paper I Y HESE-35
1325–558 PMN J1329–5608 B >0.13 This Work Y Y HESE-35
1333–337 IC 4296 G 0.012 Paper I Y HESE-48
1343–601 Cen B G 0.013 This Work HESE-35
1344–376 PMN J1347–3750 Q 1.300 This Work Y HESE-48
1409–651 Circinus Galaxy G 0.001 j HESE-35
1424–418 [HB89] 1424–418 Q 1.522 Paper I Y Y Y HESE-35
1440–389 PKS 1440–389 B >0.14 This Work Y
1454–354 PKS 1454–354 Q 1.424 Paper I Y Y Y
1501–343 PMN J1505–3432 B 1.554 Paper I Y
1505–496 PMN J1508–4953 Q 0.776 This Work Y HESE-35
1549–790 PKS 1549–79 G 0.150 Paper I Y Y
1600–445 PMN J1604–4441 U >0.01 This Work Y
1600–489 PMN J1603–4904 G 0.230g Müller et al. (2014) Y Y
1606–667 PMN J1610–6649 U This Work Y
1610–771 [HB89] 1610–771 Q 1.710 Paper I Y Y
1613–586 PMN J1617–5848 Q This Work Y HESE-52
1646–506 PMNJ1650–5044 U 0.090 This Work Y Y HESE-52
1653–329 SwiftJ1656.3–3302 Q 2.400 Krauß et al. (2014) HESE-2, HESE-14
1714–336 PMN J1717–3342 B Paper I Y Y HESE-2, HESE-14
1716–771 PKS 1716–771 U Paper I Y
1718–649 NGC 6328 G 0.010 Paper I Y Y
1733–565 PKS 1733–56 G 0.098 Paper I Y Y HESE-52
1759–396 PMN J1802–3940 Q 1.320 Paper I Y Y HESE-2, HESE-14
1804–502 PMN J1808–5011 Q 1.606 Paper I Y HESE-2
1814–637 PKS 1814–63 G 0.063 Paper I Y
1915–458 PKS 1915–458 Q 2.470 This Work HESE-2, HESE-12
1933–400 PKS 1933–400 Q 0.965 Paper I Y HESE-2
1954–388 [HB89] 1954–388 Q 0.630 Paper I Y Y HESE-2
2004–447 PKS 2004–447 G 0.240 Schulz et al. (2016) HESE-2,HESE-12
2005–489 [HB89] 2005–489 B 0.071 Paper I Y HESE-12
2027–308 ESO 462– G 027 G 0.539 Paper I Y HESE-2
2052–474 [HB89] 2052–474 Q 1.489 Paper I Y Y Y
2106–413 [HB89] 2106–413 Q 1.058 Paper I Y Y
2123–463 PKS 2123–463 Q 1.46i This Work
2136–428 PMNJ2139–4235 B This Work Y Y
2142–758 PKS 2142–75 Q 1.139 This Work Y
2149–306 PKS 2149–306 Q 2.345 Paper I Y
2152–699 ESO 075– G 041 G 0.028 Paper I Y
2154–838 PKS 2155–83 Q This Work
2155–304 [HB89] 2155–304 B 0.116 Paper I Y Y
2204–540 [HB89] 2204–540 Q 1.206 Paper I Y Y
2326–477 [HB89] 2326–477 Q 1.299 Paper I Y Y
2355–534 [HB89] 2355–534 Q 1.006 Paper I Y

Notes.

(a)

IAU B1950 and common name.

(b)

Optical classification after Véron-Cetty & Véron (2006) and Shaw et al. (2012, 2013) with Q: quasar, B: BL Lac, G: galaxy, U: unidentified object.

(c)

Redshift.

(d)

Source included in the radio-γ correlation study of the first year of Fermi/LAT data by Böck et al. (2016, B16).

(e)

The radio-selected subsample includes all sources south of declination − 30° from the catalog of Stickel et al. (1994) above a limiting radio flux density of S5 GHz> 2 Jy with a flat radio spectrum (α> −0.5, S ~ ν+ α) between 2.7 GHz and 5 GHz (22 sources).

(f)

The γ-ray sample includes the γ-ray brightest AGN south of declination − 30° in the 3LAC catalog (22 sources).

(g)

Redshift measurement by Goldoni et al. (2016).

(h)

Results of TANAMI VLBI observations quasi-simultaneous to the IceCube events were presented in Krauß et al. (2014).

(i)

Redshift measurement by D’Ammando et al. (2012).

(j)

See Fig. 3.

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