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Table A.1

152 TeV sources considered in this analysis.

ID TeV source (l,b) TeV pos. err. Canonical name Type8 Flux4 (E> 100 MeV) UL4 Ext.
[deg]9 [deg] [10-7phcm-2s-1] [10-7phcm-2s-1]
1 TeVJ0006+727 119.604, 10.403 0.091 CTA 1 PWN/SNR 21.4 21.6 3.3 ± 0.2 X
2 TeVJ0013-189 74.6130,–78.0684 0.0083 SHBL J001355.9-185406 HBL 1.5
3 TeVJ0025+640 120.106, 1.451 0.026 Tycho SN, G120.1+1.4 SNR 1.6 1.6 0.7
4 TeVJ0033-193 94.171, –81.216⋆ – KUV 00311-1938 HBL 2.0
5 TeVJ0035+598 120.898, –3.018 0.030 1ES 0033+595 HBL 0.2
6 TeVJ0047-253 97.4696,–87.9672 0.0080 NGC 253 Sbs 0.6
7 TeVJ0112+227 129.14, –39.88⋆ – S2 0109+22 IBL 1.8 3.3 0.8
8 TeVJ0136+391 132.416,–22.940⋆ – RGB J0136+391 HBL 1.2 1.2 0.5
9 TeVJ0152+017 152.343,–57.561 0.030 RGB J0152+017 HBL 1.9 3.7 1.5
10 TeVJ0209+648 130.701, 3.102 0.059 3C 58 PWN 2.1 4.8 0.8
11 TeVJ0218+359 142.602,–23.487 – S3 0218+35 AGN 3.3 3.9 1.0
12 TeVJ0222+430 10 140.143,–16.767 – 3C 66A IBL 8.0 8.1 1.4 ± 0.2
13 TeVJ0223+43010 140.254,–16.772 0.048 MAGIC J0223+430 UNID 7.6 8.0 1.3 ± 0.2
14 TeVJ0232+202 152.970,–36.613 0.014 1ES 0229+200 HBL 3.1 4.2 0.9 ± 0.3
15 TeVJ0240+612 135.668, 1.113 0.034 LSI+61_303 XRB 26.7 27.0 6.5 ± 0.3
16 TeVJ0303-241 214.6296,–60.1899 0.0073 PKS 0301-243 HBL 0.9
17 TeVJ0316+413 150.183, –13.734 – IC 310 HBL 0.3
18 TeVJ0319+187 165.088, –31.708⋆ 0.034 RBS 0413 HBL 2.0 1.2
19 TeVJ0319+415 150.576,–13.261 – NGC 1275 FRI 5.5 5.5 1.0 ± 0.2
20 TeVJ0349-119 201.909, –45.704 0.011 1ES 0347-121 HBL 0.8
21 TeVJ0416+010 191.8167,–33.1581 0.0069 1ES 0414+009 HBL 2.4 3.4 1.5
22 TeVJ0449-438 248.8066,–39.9082 0.0072 PKS 0447-439 HBL 1.3 1.3 1.1
23 TeVJ0507+676 143.795, 15.890⋆ – 1ES 0502+675 HBL 0.2
24 TeVJ0521+211 11 183.6021,–8.7114 0.0080 RGB J0521.8+211 IBL 4.5 4.7 1.6 ± 0.4
25 TeVJ0525-696 280.307, –32.784⋆ – LMC N132D SNR/MC 1.0 1.0 0.6
26 TeVJ0534+220 184.5558,–5.7870 0.0070 Crab Nebula PWN 55.7 55.9 26.7 ± 0.7
27 TeVJ0535-692 279.60, –31.91 0.022 30 Dor C Superbubble 3.5 3.8 1.1
28 TeVJ0537-691 279.553, –31.750 0.010 N 157B PWN 3.4 3.7 1.1
29 TeVJ0550-322 237.562, –26.152 0.014 PKS 0548-322 HBL 0.6
30 TeVJ0616+225 189.073, 2.918 0.085 IC 443 SNR 12.9 13.2 5.0 ± 0.5 X
31 TeVJ0632+057 205.660, –1.441 0.010 HESS J0632+057 XRB 2.5 4.8 1.9
32 TeVJ0632+173 195.34, 3.78 0.50 Geminga PWN PWN 75.2 82.6 40.3 ± 0.9 X
33 TeVJ0648+152 198.99, 6.32 0.12 RX J0648.7+1516 HBL 0.7
34 TeVJ0650+250 190.282, 10.996⋆ – 1ES 0647+250 HBL 0.6
35 TeVJ0710+591 157.391, 25.421 0.027 RGB J0710+591 HBL 0.4
36 TeVJ0721+713 143.981, 28.018 ⋆ – S5 0716+714 LBL 13.8 13.9 2.6 ± 0.2
37 TeVJ0809+523 166.246, 32.935 0.048 1ES 0806+524 HBL 1.9 2.0 0.9
38 TeVJ0835-455 12 263.840,–3.073 0.034 Vela X PWN 7.9 11.2 6.2 ± 0.8 X
39 TeVJ0847+115 215.456, 30.890⋆ – RBS 0723 HBL 0.8
40 TeVJ0852-463 13 266.285,–1.241 – RX J0852.0-4622 SNR 4.0 8.5 1.5 ± 0.4 X
41 TeVJ0955+696 141.409, 40.568⋆ – M82 Sbs 0.3
42 TeVJ0958+655 145.75, 43.13⋆ – S4 0954+65 FSRQ 1.8 1.9 0.8
43 TeVJ1010-313 266.896, 20.063 0.017 1RXS J101015.9-311909 HBL 0.1
44 TeVJ1015+494 165.534, 52.712⋆ – 1ES 1011+496 HBL 2.4 2.9 1.2
45 TeVJ1018-589 284.256,–1.818 – HESS J1018-589 BIN 7.0 7.9 2.4 ± 0.4 X
46 TeVJ1023-575 284.217, –0.401 0.030 Westerlund 2 WR 2.1 3.5 1.5 X
47 TeVJ1026-582 284.798, –0.520 0.090 HESS J1026-582 PWN 0.2 X
48 TeVJ1103-234 273.188, 33.074 0.012 1ES 1101-232 HBL 0.3
49 TeVJ1104+382 179.832, 65.032 – Mrk 421 HBL 5.2 5.2 1.6 ± 0.4
50 TeVJ1119-614 292.102, –0.487 – G 292.2-0.5 PWN 2.3 4.6 1.3 X
51 TeVJ1136+676 133.453, 47.951⋆ – RXJ1136.5+6737 HBL 0.4
52 TeVJ1136+701 131.910, 45.641⋆ – Mrk 180 HBL 1.4 1.4 0.7
53 TeVJ1217+301 189.010, 82.046 0.016 1ES 1215+303 HBL 0.3
54 TeVJ1221+28214 201.734, 83.288 – W Comae IBL 1.0
55 TeVJ1221+301 186.210, 82.743 0.031 1ES 1218+304 HBL 0.2
56 TeVJ1224+21315 255.074, 81.660⋆ – 4C +21.35 FSRQ 2.6 3.5 1.7
57 TeVJ1224+246 233.952, 83.418 – MS 1221.8+2452 HBL 0.7
58 TeVJ1230+123 283.7388, 74.4946⋆ 0.0080 M 87 FRI 1.0
59 TeVJ1230+253 232.75, 84.91⋆ – S3 1227+25 IBL 2.8 3.0 1.7
60 TeVJ1256-057 305.104, 57.062 ⋆ – 3C 279 FSRQ 11.1 11.2 4.2 ± 0.5
61 TeVJ1302-638 304.187, –0.987 0.011 PSR B1259-63 XRB 0.6
62 TeVJ1303-631 304.213, –0.334 0.014 HESS J1303-631 PWN 0.4 X
63 TeVJ1315-426 307.540, 20.064 0.018 1ES 1312-423 HBL 2.4 5.1 0.9
64 TeVJ1325-430 16 309.513, 19.425 0.021 Centaurus A FRI 4.4 4.9 0.8 ± 0.2
65 TeVJ1356-645 309.812, –2.494 0.034 HESS J1356-645 PWN 1.7 2.0 1.0 X
66 TeVJ1418-609 313.247, 0.150 0.030 Kookaburra (Rabbit) PWN 13.5 13.5 5.1 ± 0.4 X
67 TeVJ1420-607 313.558, 0.268 0.018 Kookaburra (PWN) PWN 1.1 X
68 TeVJ1427+238 29.472, 68.208 0.033 PKS 1424+240 IBL 1.3 1.3 1.3
69 TeVJ1427-608 314.408, –0.145 0.050 HESS J1427-608 UNID 1.2 1.2 1.1
70 TeVJ1428+426 77.487, 64.899⋆ – H 1426+428 HBL 1.0 X
71 TeVJ1442-624 315.410, –2.300 0.059 RCW 86 SNR 0.5 X
72 TeVJ1443+120 8.330, 59.840⋆ – 1ES 1440+122 IBL 0.6
73 TeVJ1443+250 34.56, 64.70⋆ – PKS 1441+25 FSRQ 0.7
74 TeVJ1457-594 318.36, –0.43 0.14 G 318.2+0.1 SNR/MC 0.2 X
75 TeVJ1459-608 317.748,–1.704 0.030 HESS J1458-608 PWN 5.6 5.8 1.5 ± 0.3 X
76 TeVJ1502-419 327.580, 14.571 – SN 1006 SNR 0.3
77 TeVJ1503-582 319.62, 0.29 0.10 HESS J1503-582 UNID 0.2 X
78 TeVJ1506-623 317.946, –3.494 0.050 HESS J1507-622 UNID 3.1 4.3 1.2 X
79 TeVJ1512-091 351.2907, 40.1296 0.0093 PKS 1510-089 FSRQ 24.8 25.0 8.1 ± 0.4
80 TeVJ1514-591 320.324, –1.200 0.010 MSH 15-52 PWN 0.6 X
81 TeVJ1517-243 340.673, 27.577⋆ 0.014 AP Lib LBL 2.0 3.6 0.8
82 TeVJ1554-550 327.158, –1.072 0.018 G 327.1-1.1 PWN 0.3 X
83 TeVJ1555+111 21.919, 43.960 0.016 PG 1553+113 HBL 1.9 4.4 1.3
84 TeVJ1614-518 331.52, –0.58 – HESS J1614-518 UNID 0.8 X
85 TeVJ1616-508 332.39, –0.14 – HESS J1616-508 PWN 0.9 X
86 TeVJ1626-490 334.772, 0.045 0.050 HESS J1626-490 UNID 0.3
87 TeVJ1632-478 17 336.38, 0.19 – HESS J1632-478 UNID 5.6 5.7 2.2 ± 0.4 X
88 TeVJ1634-472 337.11, 0.22 – HESS J1634-472 UNID 15.4 15.7 6.3 ± 0.4 X
89 TeVJ1640-465 338.32,–0.02 – HESS J1640-465 PWN 12.3 15.2 5.1 ± 0.5 X
90 TeVJ1641-463 338.519, 0.095 0.015 HESS J1641-463 UNID 1.0
91 TeVJ1647-458 339.55, –0.35 0.12 Westerlund 1 WR 1.3 1.3 1.3 X
92 TeVJ1653+397 63.600, 38.859 – Mrk 501 HBL 3.9 5.3 1.3
93 TeVJ1702-420 344.304, –0.184 0.050 HESS J1702-420 UNID 0.2 X
94 TeVJ1708-410 345.683, –0.469 0.050 HESS J1708-410 UNID 0.4 X
95 TeVJ1708-443 343.058,–2.376 0.071 HESS J1708-443 PWN/SNR 39.8 42.3 13.6 ± 0.4 X
96 TeVJ1713-382 348.639, 0.388 0.018 CTB 37B SNR 6.5 7.8 2.6 ± 0.4 X
97 TeVJ1713-397 347.336, –0.473 – RX J1713.7-3946 SNR 3.7 7.0 2.2 X
98 TeVJ1714-385 18 348.389, 0.107 0.023 CTB 37A SNR 7.0 7.5 2.8 ± 0.4 X
99 TeVJ1718-374 349.720, 0.174 0.010 G 349.7+0.2 SNR/MC 6.2 7.6 2.6 ± 0.4
100 TeVJ1718-385 348.834,–0.488 0.034 HESS J1718-385 PWN 6.9 7.5 2.7 ± 0.4 X
101 TeVJ1725+118 34.120, 24.475⋆ – H 1722+119 HBL 0.4
102 TeVJ1728+502 77.068, 33.537 – 1ES 1727+502 HBL 0.4
103 TeVJ1729-345 353.444,–0.128 0.035 HESS J1729-345 UNID 8.0 10.3 3.6 ± 0.5 X
104 TeVJ1732-347 17 353.542,–0.670 – HESS J1731-347 SNR 7.3 10.2 3.1 ± 0.5 X
105 TeVJ1741-302 19 358.397, 0.191 – HESS J1741-302 UNID 4.3 9.6 2.1 ± 0.5
106 TeVJ1743+196 43.836, 23.339⋆ – 1ES 1741+196 HBL 0.3
107 TeVJ1745-290 359.9449, –0.0440 0.0024 HESS J1745-290 UNID 0.3
108 TeVJ1745-303 358.710,–0.640 – HESS J1745-303 SNR/MC 11.2 12.7 5.5 ± 0.5 X
109 TeVJ1747-248 3.78, 1.72 0.45 Terzan 5 GC 5.2 5.9 1.9 ± 0.4 X
110 TeVJ1747-281 0.872, 0.076 – G 0.9+0.1 PWN 0.1
111 TeVJ1800-240 5.960, –0.380 0.044 HESS J1800-240 (A+B+C) UNID 0.9 X
112 TeVJ1801-233 6.657,–0.268 0.032 W28 SNR/MC 14.0 15.0 6.5 ± 0.5 X
113 TeVJ1804-216 8.354,–0.000 – HESS J1804-216 UNID 7.5 7.8 3.4 ± 0.5 X
114 TeVJ1808-204 9.960, –0.248 0.038 HESS J1808-204 UNID 1.3
115 TeVJ1809-193 11.180, –0.088 0.050 HESS J1809-193 PWN 3.4 4.1 2.4 X
116 TeVJ1813-178 12.812,–0.026 – HESS J1813-178 PWN 4.1 4.8 1.9 ± 0.5 X
117 TeVJ1818-154 15.409, 0.161 0.014 G 15.4+0.1 PWN 1.8 9.0 1.7 X
118 TeVJ1825-137 17.711,–0.697 0.018 HESS J1825-137 PWN 8.0 11.3 3.8 ± 0.5 X
119 TeVJ1826-148 18 16.902,–1.278 0.012 LS 5039 XRB 7.7 10.7 3.3 ± 0.5
120 TeVJ1831-099 21.850, –0.109 – HESS J1831-098 PWN 1.9 4.2 1.8 X
121 TeVJ1832-093 22.476, –0.177 0.015 G 22.7-0.2 SNR/MC 1.1 1.1 1.4 X
122 TeVJ1833-106 21.511, –0.876 0.016 HESS J1833-105 UNID 2.3 3.6 1.8
123 TeVJ1834-087 23.24, –0.32 – HESS J1834-087 UNID 0.9 X
124 TeVJ1837-069 25.18,–0.11 – HESS J1837-069 UNID 4.9 7.4 2.1 ± 0.4 X
125 TeVJ1841-055 17 26.795,–0.198 0.050 HESS J1841-055 UNID 12.4 14.0 5.0 ± 0.4 X
126 TeVJ1843-030 29.033, 0.370 – HESS J1843-033 UNID 3.6 6.7 2.2
127 TeVJ1846-029 29.705, –0.240 0.011 HESS J1846-029 PWN 1.6 1.6 1.5
128 TeVJ1848-017 31.000,–0.160 – WR121a/W43 WR 3.7 4.6 1.4 ± 0.4 X
129 TeVJ1849-000 32.638, 0.526 – IGR J18490-0000 PWN 1.0
130 TeVJ1857+026 36.003, –0.061 0.039 HESS J1857+026 UNID 0.2 X
131 TeVJ1858+020 35.578, –0.581 0.050 HESS J1858+020 UNID 0.1 X
132 TeVJ1907+062 40.280,–0.688 0.020 MGRO J1908+06 UNID 12.9 13.3 4.5 ± 0.4 X
133 TeVJ1911+090 43.259,–0.189 0.071 W 49B SNR/MC 7.6 7.8 2.4 ± 0.3
134 TeVJ1912+101 44.391,–0.071 0.050 HESS J1912+101 PWN 4.1 7.6 1.3 ± 0.3 X
135 TeVJ1923+141 49.116,–0.365 0.015 W 51 SNR/MC 7.0 7.1 2.1 ± 0.3 X
136 TeVJ1930+188 54.10, 0.26 0.11 G 54.1+0.3 PWN 3.5 5.2 1.5
137 TeVJ1943+213 57.7577, –1.2928 0.0073 HESS J1943+213 HBL 0.5
138 TeVJ1959+651 98.003, 17.670⋆ – 1ES 1959+650 HBL 3.4 3.7 0.7
139 TeVJ2001+438 79.071, 7.110 – MAGIC J2001+435 HBL 4.9 4.8 0.9 ± 0.2
140 TeVJ2009-488 350.3741, –32.6052 0.0083 PKS 2005-489 HBL 0.4
141 TeVJ2016+372 74.940, 1.140 0.019 VER J2016+372 UNID 0.3
142 TeVJ2019+368 74.828, 0.417 0.090 MGRO J2019+37 PWN 24.7 25.5 6.7 ± 0.3 X
143 TeVJ2019+407 78.331, 2.489 0.035 VER J2019+407 UNID 0.1 X
144 TeVJ2032+415 80.279, 1.042 0.044 TeV J2032+4130 UNID 7.6 8.0 2.2 ± 0.3 X
145 TeVJ2158-302 17.737,–52.247 – PKS 2155-304 HBL 4.6 4.8 1.3 ± 0.3
146 TeVJ2202+422 92.590,–10.441 – BL Lacertae LBL 7.2 8.0 1.0 ± 0.2
147 TeVJ2227+608 106.35, 2.71 0.10 G 106.3+2.7 SNR 15.2 16.7 3.0 ± 0.2 X
148 TeVJ2243+203 86.567, –33.365⋆ – RGB J2243+203 HBL 0.4
149 TeVJ2250+384 98.254, –18.578 – B3 2247+381 HBL 0.2
150 TeVJ2323+588 111.735,–2.130 0.020 Cassiopeia A SNR 5.2 7.2 0.9 ± 0.2
151 TeVJ2347+517 112.73, –9.86 0.10 1ES 2344+514 HBL 0.3
152 TeVJ2359-306 12.8689,–78.0367 0.0086 H 2356-309 HBL 3.9 4.0 3.3 ± 1.0

Notes. The sources passing the detection criteria discussed in Sect. 5.2 are shown in bold. For a detailed description of the table columns please refer to the text.

(8)

TeV source classification types: PWN: Pulsar Wind Nebulae; BIN: Binary; SNR: SuperNova Remnant; Sbs: StarBursts; UNID: UNIDentified; FSRQ: Flat Spectrum Radio Quasar; HBL: High frequency peaked BL Lac object; IBL: Intermediate frequency peaked BL Lac object; LBL: Low frequency peaked BL Lac object; XRB: X-Rays Binary; WR: Wolf-Rayet star; FRI: Fanaroff–Riley type I ; GC: Globular Cluster; MC: Molecular Cloud; PSR: Pulsar. Note that the γ-ray emission detected in the search of counterparts to the TeV emission from PWN is in general due to the average (pulsar + nebula) γ-ray flux values. Timing analysis of pulsars was not performed in this paper.

(9)

The ⋆ indicates that the best-fit position of the TeV excess is not available and the position of the optical/radio known counterpart has been used.

(10)

The sources TeVJ0222+430 and TeVJ0223+430 are as close as 0.1° and therefore indistinguishable in this analysis. Their detection is counted as one.

(11)

Results of a refined MLE analysis performed using the updated AGILE best-fit position of the Crab Nebula (one of the known γ–ray sources within 10 deg from the TeV J0521+211 position) obtained in this work.

(12)

The TeV error region for the Vela X PWN does not overlap the AGILE Vela Pulsar position error, hence the Vela PSR average γ–ray flux value for a spectral index of −1.69 was subtracted in the MLE automatic analysis. However the result is affected by the very intense Vela Pulsar nearby. The Vela X accurate γ–ray flux estimate and source location by AGILE is discused in the dedicated analysis in (Pellizzoni et al. 2010).

(13)

Also in this case, the MLE automatic analysis is affected by the very intense Vela Pulsar nearby. A dedicated analysis will be performed.

(14)

Detected by AGILE during a flaring episode (Verrecchia et al. 2008).

(15)

Detected by AGILE during several flaring episodes (Bulgarelli et al. 2010; Striani et al. 2010; Verrecchia et al. 2014).

(16)

The region of the MLE analysis is not yet well modelled since this source shows a point-like core and extended emission from the lobes, which are not yet included in the AGILE reference catalogs. A dedicated analysis will be performed.

(17)

AGILE detection presented at the 32nd ICRC (Lucarelli et al. 2011).

(18)

Source located in a crowded region of the Galactic plane. The automatic MLE analysis is not reliable. A dedicated analysis will be performed.

(19)

Source located in the region near the Galactic Center. The automatic MLE analysis is not reliable. A dedicated analysis is being performed with an improved AGILE diffuse background model in the Galactic center region (Fioretti et al., in prep.).

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