Atlas of Galactic Center Diffuse X-ray features (see Ponti et al. 2015)

Please find below few tables of diffuse Galactic Center X-ray features (see Ponti et al. 2015).
To try to make these tables as complete as possible, these tables will be routinely updated.
Please, notify the authors, would any feature be missing from these tables.


OnlineTables

Table 1: Atlas of diffuse X-ray emitting features. The first two columns in the table indicate the name primarily used in this work to refer to the feature as well as the other names used in the previous literature. The third and fourth columns show the coordinates of each feature as well as its approximate projected size. Finally, the fifth column provides references to selected works discussing the feature. For convenience, we report in Tab. 1 all the references ordered according to the numbering used in this table. The other names column shows the different designations used in previous literature. In the case of bubbles, these features are not necessarily referring to the same structure but to features forming the bubble candidate. (c) The low X-ray absorption towards these star clusters indicate that they are located in front of the GC region. (d) Most probably a foreground feature. (e) This feature appears to be part of the superbubble G359.77-0.09. (f) New extended X-ray feature, possibly part of the superbubble G359.77-0.09. (g) Possibly due to a thermal filament. (h) This feature appears to be part of the Arc bubble. (i) Possibly connected to G0.61+0.01. (l) X-ray emission primarily non-thermal, therefore it appears also in the next table. (n) Because of the low X-ray absorption column density, this is most probably a foreground source (Bamba et al. 2000; 2009). (o) The Chimney is most probably either part of a large scale structure (see section 8.7 of Ponti et al. 2015) or an outflow from G359.4-0.12 (Tsuru et al. 2009), therefore most probably it is not a separate SNR.
ATLAS OF DIFFUSE X-RAY EMITTING FEATURES
Name Other name or Coordinates Size References
associated features (l, b) arcmin
STAR CLUSTERS:
Central cluster 359.9442, -0.046 0.33 45,116,117,118
Quintuplet 0.1604, -0.0591 0.5 1,63,11
Arches G0.12+0.02 0.1217, 0.0188 0.7 1,2,3,4,5,6,7,8,9,39,40,11
Sh2-10(c) DB-6 0.3072,-0.2000 1.92 10,11,12,63,11
Sh2-17(c) DB-58 0.0013, 0.1588 1.65 13,63,11
DB-05(c) G0.33-0.18 0.31 -0.19 0.4 22,63,11
SNR and Super-bubbles candidates:
G359.0-0.9(n) G358.5-0.9 - G359.1-0.9 359.03,-0.96 26×20 X-R 48,51,75,76,81,119,120
G359.07-0.02(n) G359.0-0.0 359.07,-0.02 22×10 R 14,48,51,66
G359.12-0.05 359.12,-0.05 24×16 X 66
G359.10-0.5 359.10,-0.51 22×22 X-R 37,48,51,56,74,75,81,120,121
G359.41-0.12 359.41,-0.12 3.5×5.0 X 14
Chimney(o) 359.46,+0.04 6.8×2.3 X 14
G359.73-0.35(d) 359.73,-0.35 4 X 58
G359.77-0.09  Superbubble 359.77,-0.09 20×16 X 15,16,17,58
G359.9-0.125 359.84,-0.14 15×3 X 15,16,17,58
G359.79-0.26(e) 359.79,-0.26 8×5.2 X 15,16,17,58
G0.0-0.16(f) 0.00,-0.16 X This work
20 pc lobes 359.94, -0.04 5.88 X-R 32,33,34,17
G359.92-0.09(g) Parachute - G359.93-0.07 359.93,-0.09 1 R 35,38,43,47,58,60,61
Sgr A East G0.0+0.0 359.963, -0.053 3.2×2.5 X-R 5,18,19,20,48,75,81
G0.1-0.1 Arc Bubble 0.109,-0.108 13.6×11 X This work
G0.13,-0.11(h) 0.13,-0.12 3×3 X 17
G0.224-0.032 0.224,-0.032 2.3×4.6 X This work
G0.30+0.04 G0.3+0.0 0.34,+0.045 14×8.8 R 21,48,51,81,82
G0.34+0.05
G0.33+0.04
G0.42-0.04 Suzaku J1746.4-2835.4 0.40,-0.02 4.7×7.4 X 22
G0.40-0.02
G0.52-0.046 0.519,-0.046(i) 2.4×5.1 This work
G0.57-0.001 0.57,-0.001 1.5×2.9 This work
G0.57-0.018(g) CXO J174702.6-282733 0.570,-0.018 0.2 X 23,24,58,59,68,80
G0.61+0.01(g) Suzaku J1747.0-2824.5 0.61,+0.01 2.2×4.8 X 22,65,79
G0.9+01(l) SNR 0.9+0.1 0.867,+0.073 7.6×7.2 R 25,26,27,28,29,48,75,81,82
DS1 G1.2-0.0 1.17,+0.00 3.4×6.9 X 31
Sgr D SNR G1.02-0.18 1.02,-0.17 10×8.0 R 30,31,48,51,75,77,81,82
G1.05-0.15
G1.05-0.1
G1.0-0.1
G1.4-0.1 1.4,-0.10 10×10 R 73,81,82
Table 2: Atlas of diffuse X-ray emitting features. This table has the same structure as Tab. 2. Because of possible misplacements between the peak emission of the radio and X-ray counterparts of filaments, SNR, PWN and other diffuse structures (generally related to the different ages of the population of electrons traced at radio and X-ray bands), when available we give the best X-ray position (following the preference: Chandra, XMM-Newton, Suzaku), otherwise we state the radio position. We cite the literature results separating thes between the X-ray (X) from the radio (R) detections. (m) Possibly part of a young supernova remnant. For convenience, we report in Tab. 1 all the references ordered according to the numbering used in this table.
ATLAS OF DIFFUSE X-RAY EMITTING FEATURES
Name Other name or Coordinates Size References
associate features (l, b) arcsec
Radio and X-ray filaments and PWN candidates:
Snake G359.15-0.2 359.15,-0.17 312×54 R 48
G539.40-0.08 359.40,-0.08 27.5×5.1 X 41
G359.43-0.14 359.43,-0.14 21.4×3.9 X 41
Sgr C Thread 359.45,-0.01 500×42 R 48,51
Ripple filament G359.54+0.18 359.548,+0.177 320×55 R 43,44,48,51
G359.55+0.16 X-ray thread 359.55,+0.16 56.1×8.0 X 13,41,42,43,79
Suzaku J174400-2913
Crescent G359.79+0.17 359.791,+0.16 300×74 R 63,50,51
Curved filament
Pelican G359.85+0.47 359.859,+0.426 300×54 R 48,50,51
Cane G359.87+0.44 359.87,+0.44 420×50 R 48
G359.85+0.39
Sgr A-E G359.889-0.081- wisp 359.889,-0.081 20×5 R X 5,35,41,42,43,44,50,55
XMM J174540-2904.5
G359.89-0.08
G359.897-0.023 359.897,-0.023 6.4×4 X 55
G359.899-0.065 Sgr A-F 359.899,-0.065 6.5×2.5 X 42,44,55
G359.90-0.06
G359.904-0.047 359.904,-0.047 6.5×3 X 55
G359.915-0.061 359.915,-0.061 7×2 X 55
G359.91-1.03 359.919,-1.033 138×36 R 48
G359.921-0.030 F7 359.921,-0.030 7.5×3 X 42,55
G359.921-0.052 359.921,-0.052 5.5×2 X 55
The Mouse G359.23-0.82 359.30-0.82 156×108 PWN F 37,48,57,123
G359.925-0.051 359.925,-0.051 8×2.2 X 55
G359.933-0.037 F2 359.934,-0.0372 12×3 X 41,42,55
G359.933-0.039 F1 359.933,-0.039 5×2 X 42,55
G359.941-0.029 359.941,-0.029 6×2 X 41,55 Stellar wind
G359.942-0.045 359.942,-0.045 5×3 X 55
G359.944-0.052 359.944,-0.052 9×1.5 X 41,55
G359.945-0.044 359.945,-0.044 6×2.5 X 41,1,42,55 PWN
G359.95-0.04 359.950,-0.043 10×4 X 55,70 PWN
G359.956-0.052 359.956,-0.052 4×2.5 X 55
G359.959-0.027 F5 359.959,-0.027 9×3 X 41,42,55
Southern thread G359.96+0.09 359.96,+0.11 500×40 R 48,50,51
359.96+0.09
G359.962-0.062 359.962,-0.062 5.5×3.5 X 55
G359.964-0.053 F3 359.964,-0.053 16×3.5 X 41,42,45,55 PWN
G359.965-0.056 F4 359.965,-0.056 9×3 X 42,55
G359.969-0.033 359.969,-0.033 5×2 X 55
G359.970-0.009 F8 359.970,-0.009 10×2.5 X 41,42,55 PWN
G359.971-0.038 F6 359.971,-0.038 16×8 X 41,42,55 PWN
G359.974-0.000 F9 359.974,-0.000 7×2 X 42
G359.977-0.076 359.977,-0.076 6×4 X 55
Cannonball J174545.5-285829 359.983,-0.0459 30×15 X-R PWN 36,122
G359.983-0.040 359.983,-0.040 6.5×4.5 X 42,55
G359.98-0.11 359.979,-0.110 Streak R 50
G0.007-0.014 G0.008-0.015 0.008,-0.015 11×3.5 X 41,55
G0.014-0.054 0.014,-0.054 18×14 X 55
G0.017-0.044 MC2 0.017,-0.044 15×4 X 41,42 FeKa
G0.02+0.04 0.0219,+0.044 Streak R 50
G0.021-0.051 0.021,-0.051 15×12 X 55
G0.029-0.08 0.029,-0.08 29×18 X 55
G0.032-0.056 G0.029-0.06 - F10 0.0324,-0.0554 35×6 FeKa 41,42,55 PWN
G0.03-0.06
G0.039-0.077 0.039,-0.077 22×15 X 55
G0.062+0.010 G0.06+0.06 0.062,+0.010 40×25 R 50,55
Northern thread G0.09+0.17 0.09,+0.17 714×48 R 48,49,50,51
G0.08+0.15
G0.097-0.131 0.097,-0.131 70×50 X 55
Radio Arc GCRA 0.167,-0.07 1690×145 R 38,48,49,50,51
G0.16-0.15
G0.116-0.111 0.116,-0.111 50×40 X 55
G0.13-0.11 0.13,-0.11 55×12 71,17,41,42 PWN
G0.15-0.07 Steep spectrum of Radio Arc 0.138,-0.077 R 50
XMM J0.173-0.413 G0.17-0.42 0.173,-0.413 180×18 X This work
S5 0.17,-0.42 912×100 R 82
G0.223-0.012 0.223,-0.012 50×20 X 41
G0.57-0.018(m) CXO J174702.6-282733 0.57,-0.0180 0.33 X 23,24,58,59,68,79,80
G0.61+0.01(m) 0.61,+0.01 132×288 X 22,65,79
G0.9+0.1 0.9,+0.1 PWN
Table 3: List of bright and transient point sources during the 2012 XMM-Newton scan as well as bright point sources observed in all scans of the region. To avoid exessive crowding around Sgr A*, CXOCG J174540.0-290005 and SGR J1745-2900 are not shown. (b) Fluxes are given in units of 10-12 erg cm-2 s-1 and correspond to the mean flux observed during the 2012 XMM-Newton scan of the CMZ. (a) Coordinates are in Galactic format.
BRIGHT AND TRANSIENT POINT SOURCES
Source name Coordinates(a) Flux(b) References
within the 2012 CMZ scan
1E 1743.1-2843 0.2608,-0.0287 110 90,92,93
XMMU J174505.3-291445 359.6756,-0.0634 14 94
XMMU J174457-2850.3 0.0076,-0.1743 0.3 90,95
GRS 1741.9-2853 359.9528,+0.1202 ≤0.02 90,59,97
AX J1745.6-2901 359.9203,-0.0420 ≤0.1 59,90,91,124
CXOGC J174540.0-290031 359.9435,-0.0465 ≤5 98,99
SGR J1745-2900 359.9441,-0.0468 ≤5 101,102,103,104
XMMU J174554.4-285456 0.0506,-0.0429 ≤0.2 98
SAX J1747.7-2853 0.2073,-0.2385 ≤0.2 90,105,106,107
CXOCG J174540.0-290005 359.9497,-0.04269 ≤5 100
within the total GC scan
1E 1740.7-2942 359.1160,-0.1057 111,112,113
1A 1742-294 359.5590,-0.3882 90,108,109
IGR J17497-2821 0.9532,-0.4528 90,114,115
GRO J1744-28 0.0445,+0.3015 90
XMMU J174654.1-291542 359.8675,-0.4086 90
XMMU J174554.4-285456 359.1268,-0.3143 84,85,86
SLX 1744-299 359.2961,-0.8892 37,59,87,88,89
SLX 1744-300 359.2565,-0.9111 37,59,87,88,89

References: (1) Wang et al. 2006a; (2) Yusef-Zadeh et al. 2002; (3) Capelli et al. 2011; (4) Tatischeff et al. 2012; (5) Sakano et al. 2003; (6) Habibi et al. 2013; (7) Habibi et al. 2014; (8) Krivonos et al. 2014; (9) Clavel et al. 2014; (10) Dutra et al. 2003; (11) Law et al. 2004; (12) Fukuoka et al. 2009; (13) Wang et al. 2002a; (14) Tsuru et al. 2009; (15) Mori et al. 2008; (16) Mori et al. 2009; (17) Heard & Warwick 2013a; (18) Maeda et al. 2002; (19) Park et al. 2005; (20) Koyama et al. 2007a; (21) Kassim & Frail 1996; (22) Nobukawa et al. 2008; (23) Senda et al. 2002; (24) Renaud et al. 2006; (25) Mereghetti et al. 1998; (26) Gaensler et al. 2001; (27) Porquet et al. 2003a; (28) Aharonian et al. 2005; (29) Dubner et al. 2008; (30) Nobukawa et al. 2009; (31) Sawada et al. 2009; (32) Morris et al. 2003; (33) Morris et al. 2004; (34) Markoff et al. 2010; (35) Zhang et al. 2014; (36) Nynka et al. 2013; (37) Gaensler et al. 2004; (38) Pedlar et al. 1989; (39) Cotera et al. 1996; (40) Figer et al. 1999; (41) Johnson et al. 2009; (42) Lu et al. 2008; (43) Lu et al. 2003; (44) Yusef-Zadeh et al. 2005; (45) Baganoff et al. 2003; (46) Ho et al. 1985; (47) Bamba et al. 2002; (48) LaRosa et al. 2000; (49) Morris & Yusef-Zadeh 1985; (50) Lang et al. 1999; (51) Anantharamaiah et al. 1991; (52) Yusef-Zadeh & Morris 1987a; (53) Yusef-Zadeh & Morris 1987b; (54) Yusef-Zadeh & Morris 1987c; (55) Muno et al. 2008; (56) Uchida et al. 1992; (57) Predehl & Kulkarni 1995; (58) Senda et al. 2003; (59) Sakano et al. 2002; (60) Coil et al. 2000; (61) Murakami 2002; (62) Yusef-Zadeh et al. 2007; (63) Dutra & Bica 2000; (64) Zoglauer et al. 2014; (65) Koyama et al. 2007b; (66) Nakashima et al. 2010; (67) Downes & Maxwell 1966; (68) Tanaka et al. 2009; (69) Tanaka et al. 2007; (70) Wang et al. 2006b; (71) Wang et al. 2002b; (72) Phillips & Marquez-Lugo 2010; (73) Hewitt et al. 2008; (74) Reich & Fuerst 1984; (75) Gray 1994; (76) Roy & Bhatnagar 2006; (77) Marquez-Lugo & Phillips 2010; (78) Borkowski et al. 2013; (79) Yamauchi et al. 2014; (80) Inui et al. 2009; (81) Green 2014; (82) Yusef-Zadeh et al. 2004; (83) Nord et al. 2004; (84) Uchiyama et al. 2011; (85) Heinke et al. 2009; (86) Muno et al. 2006; (87) Mori et al. 2005; (88) Skinner et al. 1990; (89) Pavlinski et al. 1994; (90) Degenaar et al. 2012; (91) Ponti et al. 2014; (92) Porquet et al. 2003b; (93) Del Santo et al. 2006; (94) Soldi et al. 2014; (95) Sakano et al. 2005; (97) Trap et al. 2009; (98) Porquet et al. 2005a; (99) Muno et al. 2005b; (100) Kock et al. 2014; (101) Degenaar et al. 2013; (102) Dwelly & Ponti 2013; (103) Rea et al. 2013; (104) Kaspi et al. 2014; (105) Wijnands et al. 2002; (106) Natalucci et at al. 2004; (107) Werner et al. 2004; (108) Belanger et al. 2006; (109) Kuulkers et al. 2007; (110) Piraino et al. 2012; (111) Castro et al. 2013; (112) Reynolds & Miller 2010; (113) Natalucci et al. 2014; (114) Soldi et al. 2006; (115) Paizis et al. 2009 (116) Lu et al. 2013; (117) Do et al. 2013; (118) Yelda et al. 2014; (119) Bamba et al. 2000; (120) Bamba et al. 2009; (121) Ohnishi et al. 2011; (122) Zhao et al. 2013; (123) Hales et al. 2009; (124) Ponti et al. 2015.


Gabriele Ponti 2015-05-19
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