Table 1
List of Milky Way satellites tested for 511 keV emission and ordered by distance.
| Name | d | F511 | MDyn | MV | σ | l | b | TExp | Ref. |
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| Segue 1b | 23 | <12.4 | 0.26 | −1.5 | − | 220.48 | 50.43 | 0.16 | (1), (12), (60), (61), (62), (63) |
| Sagittarius Dwarf | 28 | 2.2(1.0) | 190 | – 13.4 | 2.3 | 5.57 | – 14.17 | 7.00 | (1), (44), (45), (46) |
| Reticulum IIc | 30 | 17.0(5.4) | 0.24 | – 2.7 | 3.1 | 266.30 | – 49.73 | 0.55 | (22), (23), (27), (42), (43) |
| Ursa Major IIc | 34 | 4.1(2.3) | 3.9 | −4.2 | 1.9 | 152.46 | 37.44 | 1.67 | (1), (57), (58), (59) |
| Segue 2c | 35 | <14.4 | 0.23 | −2.5 | − | 149.43 | −38.14 | 0.20 | (1), (48) |
| Willman 1c | 42 | 7.3(7.1) | 0.39 | −2.7 | 1.0 | 158.58 | 56.78 | 0.45 | (1), (62), (64), (65) |
| Coma Berenicesc | 44 | 1.6(1.7) | 0.94 | −4.1 | 1.0 | 241.89 | 83.61 | 2.93 | (1), (6), (12), (18) |
| Boötes III | 48 | <4.4 | >0.017 | −5.8 | − | 35.41 | 75.35 | 1.93 | (1), (8), (9), (10) |
| Boötes IIa | 49 | <5.8 | 3.3 | −2.7 | − | 353.69 | 68.87 | 1.92 | (1), (5), (6), (7) |
| Large Magellanic Cloud | 50 | <3.6 | >1500 | −18.1 | − | 280.47 | −32.89 | 4.22 | (1), (37), (38) |
| Tucana IIc | 57 | 3.8(8.4) | N / A | −3.8 | 0.5 | 328.08 | −52.32 | 0.22 | (22), (23) |
| Small Magellanic Cloud | 61 | 0.6(2.8) | 1400 | −16.8 | 0.2 | 302.80 | −44.30 | 1.38 | (1), (37), (52), (53) |
| Boötes I a c | 62 | 8.5(2.9) | 0.81 | – 6.3 | 3.0 | 358.08 | 69.62 | 1.85 | (1), (2), (3), (4) |
| Ursa Minorc | 73 | <5.8 | 9.5 | −8.8 | − | 104.97 | 44.80 | 1.30 | (1), (29) |
| Horologium Ic | 79 | 6.7(4.4) | 0.55 | −3.4 | 1.6 | 271.39 | −54.73 | 0.43 | (22), (23), (27) |
| Dracoc | 82 | <3.8 | 11 | −8.8 | − | 86.37 | 34.72 | 1.57 | (1), (19), (20), (21) |
| Phoenix II | 83 | <16.6 | N / A | −2.8 | − | 323.68 | −59.75 | 0.19 | (22), (23) |
| Sculptorc | 83 | <11.6 | 14 | −11.1 | − | 287.54 | −83.16 | 0.22 | (1), (47) |
| Sextansc | 85 | 6.5(5.3) | 10.6 | −9.3 | 1.2 | 243.50 | 42.27 | 0.12 | (1), (49), (50), (51) |
| Eridanus III | 87 | 7.3(5.1) | N / A | −2.0 | 1.5 | 274.95 | −59.60 | 0.38 | (22), (23) |
| Indus I | 100 | 6.2(3.9) | N / A | −3.5 | 1.6 | 347.15 | −42.07 | 0.26 | (23), (23) |
| Ursa Major Ic | 101 | <9.2 | 11 | −5.5 | − | 159.43 | 54.41 | 0.42 | (1), (6), (54), (55), (56) |
| Carinac | 103 | 0.6(3.6) | 6.3 | −9.1 | 0.2 | 260.11 | −22.22 | 0.66 | (1), (14), (15) |
| Pictoris I | 114 | <7.4 | N / A | −3.1 | − | 257.29 | −40.64 | 0.46 | (22), (23) |
| Grus I c | 120 | 20.8(9.1) | N / A | – 3.4 | 2.3 | 338.68 | – 58.25 | 0.12 | (22), (23) |
| Hercules | 136 | 9.7(5.5) | 2.6 | −6.6 | 1.8 | 28.73 | 36.87 | 0.31 | (1), (6), (12), (26) |
| Fornaxc | 139 | 16.9(9.6) | 56 | −13.4 | 1.8 | 237.10 | −65.65 | 0.11 | (1), (24), (25) |
| Canes Venatici II c | 153 | 5.0(2.2) | 0.91 | – 4.9 | 2.3 | 113.58 | 82.70 | 2.44 | (1), (6), (12), (13) |
| Leo IVc | 155 | <5.4 | 1.3 | −5.8 | − | 265.44 | 56.51 | 1.84 | (1), (6), (12), (13) |
| Pisces IIc | 182 | 2.9(4.3) | >0.0086 | −5.0 | 0.7 | 79.21 | −47.11 | 0.79 | (1), (39), (40), (41) |
| Leo Vc | 186 | 3.7(3.3) | 1.1 | −5.2 | 1.1 | 261.86 | 58.54 | 1.96 | (1), (35), (36) |
| Canes Venatici Ic | 216 | 1.2(2.2) | 19 | −8.6 | 0.6 | 74.31 | 79.82 | 1.84 | (1), (6), (11) |
| Leo IIc | 218 | 5.0(5.5) | 4.6 | −9.8 | 0.9 | 220.17 | 67.23 | 0.35 | (1), (31), (32) |
| Leo I c | 246 | 15.8(7.4) | 12 | – 12 | 2.2 | 225.99 | 49.11 | 0.12 | (1), (28), (29), (30) |
| Eridanus II | 380 | <21.6 | N / A | −6.6 | − | 249.78 | −51.65 | 0.10 | (22), (23) |
| Leo Tc | 412 | 6.1(6.5) | 3.9 | −8.0 | 1.0 | 214.85 | 43.66 | 0.19 | (1), (33), (34) |
| Phoenix I | 418 | 4.3(5.7) | 9.7 | −9.9 | 0.8 | 272.16 | −68.95 | 0.36 | (1), (66), (67), (68), (69) |
| NGC 6822 | 498 | 1.4(1.6) | 3500 | −15.2 | 0.9 | 25.34 | −18.40 | 2.25 | (1), (29), (69), (70), (71), (72) |
Notes. The measured line flux F511 is given in 10-5 ph cm-2 s-1. The values MDyn are the dynamical masses of the satellite in units of 106M⊙, MV their absolute visual magnitude, and d the distance in kpc. The significance of a possible line detection is given in units of sigma. Detections with a significance of 2σ or above are indicated in boldface. If a line is not present at all, a 2σ upper limit on the flux is given. The positions of the assumed centres of the satellites are given in galactic longitude l and latitude b in units of degrees. The effective exposure time at the position of the sources TExp is given in Ms. The parameters MDyn, MV, d, l, and b are taken from the literature (references, last column). The distances have been chosen as the given mean value from the NASA/IPAC Extragalactic Database (NED), if available.
The values for Boo I may be over- or underestimated due to source confusion with Boo II, being not separated by at least one PSF. Likewise, the value for Boo II may be wrong, too.
These galaxies have been included in the mass- and distance-weighted stacking analysis due to available dynamical mass and J-factor estimates, see Sect. 3.2.
Reference. (1) McConnachie (2012); (2) Belokurov et al. (2006); (3) Fellhauer et al. (2008); (4) Dall’Ora et al. (2006); (5) Walsh et al. (2007); (6) Grcevich & Putman (2009); (7) Walsh et al. (2008); (8) Grillmair (2009); (9) Carlin et al. (2009); (10) Correnti et al. (2009); (11) Zucker et al. (2006); (12) Belokurov et al. (2007); (13) Okamoto et al. (2012); (14) Kraan-Korteweg & Tammann (1979); (15) Mateo et al. (1998); (16) Martin et al. (2004); (17) Martin et al. (2005); (18) Musella et al. (2009); (19) Cotton et al. (1999); (20) Falco et al. (1999); (21) Tyler (2002); (22) Koposov et al. (2015a); (23) The DES Collaboration et al. (2015); (24) Piatek et al. (2007); (25) Poretti et al. (2008); (26) Musella et al. (2012); (27) Koposov et al. (2015b); (28) Whiting et al. (2007); (29) Young (2000); (30) Caputo et al. (1999); (31) Coleman et al. (2007); (32) Gullieuszik et al. (2008); (33) Irwin et al. (2007); (34) Clementini et al. (2012); (35) Belokurov et al. (2008); (36) de Jong et al. (2010); (37) Richter et al. (1987); (38) Feast & Walker (1987); (39) Belokurov et al. (2010); (40) Kirby et al. (2015); (41) Sand et al. (2012); (42) Simon et al. (2015); (43) Walker et al. (2015); (44) Majewski et al. (2003); (45) Ibata et al. (1994); (46) Monaco et al. (2004); (47) Quelozet al. (1995); (48) Belokurov et al. (2009); (49) Irwin et al. (1990); (50) Battaglia et al. (2011); (51) Lee et al. (2003); (52) Matsunaga et al. (2011); (53) Bekki & Stanimirović (2009); (54) Willman et al. (2005b); (55) Kleyna et al. (2005); (56) Okamoto et al. (2008); (57) Peñarrubia et al. (2006); (58) Fellhauer et al. (2007); (59) Dall’Ora et al. (2012); (60) Norris et al. (2010); (61) de Jong et al. (2008); (62) Martin et al. (2008); (63) Simon et al. (2011); (64) Willman et al. (2005a); (65) Willman et al. (2011); (66) Cote et al. (1997); (67) Zaggia et al. (2011); (68) Gallart et al. (2001); (69) Mateo (1998); (70) Koribalski et al. (2004); (71) Rogstad et al. (1967); (72) Veljanoski et al. (2015).
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