Table 4
X-ray spectral classifications of symbiotic stars.
| Object | Type | Reference |
|
|
||
| StHα 32 | α | 1, this work |
| SMC 3 | α | 2 |
| Ln 358 | α | 2 |
| AG Dra | α | 2 |
| Draco C-1 | α | 2 |
| RR Tel | α | 2 |
| CD-43 14304 | α | 2 |
| BI Crua | β/δ | this work |
| SWIFT J171951.7-300206 | β | this work |
| RX Pup | β | 2, 3 |
| Z And | β | 2, 4 |
| V1329 Cyg | β | 5 |
| Mira AB | β | 6 |
| EG And | β | 2 |
| HM Sge | β | 2 |
| V1016 Cyg | β | 2 |
| PU Vul | β | 2 |
| AG Peg | β | 2 |
| Hen 2-104 | β | 21 |
| Hen 3-1341 | β | 22 |
| NQ Gem | β/δ | this work |
| UV Aur | β/δ | this work |
| ZZ CMi | β/δ | this work |
| V347 Nor | β/δ | this work |
| R Aqr | β/δ | 2, 7 |
| CH Cyg | β/δ | 2, 8 |
| MWC 560 | β/δ | 20 |
| ER Del | δ | this work |
| Hen 3-461 | δ | this work |
| CD -283719 | δ | this work |
| RT Cru | δ | 9, 10 |
| T CrB | δ | 11 |
| V648 Car | δ | 12, 13 |
| GX 1+4 | γ | 2 |
| Hen 3-1591b | γ | 2 |
| V934 Her | γ | 14 |
| 4U 1954+31 | γ | 15 |
| Sct X-1 | γ | 16 |
| IGR J16194-2810 | γ | 17 |
| IGR J16358-4726c | γ | 19 |
| IGR J16393-4643 | γ | 18 |
| CGCS 5926 | γ | 19 |
Notes.
Questionable classification due to short exposure time. There are hints of the presence of a second soft spectral component, but it needs confirmation.
Questionable classification. Hen 3-1591 has been observed only with ROSAT, therefore no information is available about its hard X-ray emission, and the nature of the accreting object is not firm enough to secure its classification.
Questionable classification. Chaty et al. (2008) suggest that IGR J16358-4726 is a high-mass X-ray binary, however Nespoli et al. (2010) suggest a symbiotic nature.
Reference. (1) Orio et al. (2007); (2) Muerset et al. (1997); (3) Luna et al. (2006); (4) Sokoloski et al. (2006a); (5) Stute et al. (2011); (6) Sokoloski & Bildsten (2010); (7) Nichols et al. (2007); (8) Mukai et al. (2007); (9) Luna & Sokoloski (2007); (10) Kennea et al. (2009); (11) Luna et al. (2008); (12) Eze et al. (2010); (13) Smith et al. (2008); (14) Masetti et al. (2002); (15) Masetti et al. (2006); (16) Kaplan et al. (2007); (17) Masetti et al. (2007a); (18) Thompson et al. (2006); (19) Masetti et al. (2011); (20) Stute & Sahai (2009); (21) Montez et al. (2006); (22) Stute et al. (2013).
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