MISCLASSIFIED
MILKY WAY
|
| V1017 Sgr | IRAS - | GSC2.4.2 S9VC026532 | AAVSO 000-BCC-576 |
| SIMBAD V* V1017 Sgr | Pan-STARRS 72732780186636075 | SAO - | VSX 28717 |
| GAIA DR3 4048251562703375488 | SkyMapper 183204.48-292312.6 | WRAY - | GCVS V1017 Sgr |
| 2MASS J18320447-2923125 | HIP - | Hen - | BD - |
| WISE - | TYC - | ESO - | HD - |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | V1017 Sgr (Misc.) |
| Gaposchkin (1957) | - | Kenyon (1986) | V1017 Sgr (Conf.) | Akras et al. (2019) | - |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | V1017 Sgr (Conf.) |
| Right ascension (°) | 278.0187Ref | Parallax (mas) | 0.817±0.023Ref | Reddening E(B-V) (mag) | 0.23±0.0Ref, Note |
| Declination (°) | -29.3869Ref | Distance (kpc) | 1.17Ref, Note, 1.17Ref, Note | ||
| Galactic longitude (°) | 4.4908Ref | Proper motion in α (mas/yr) | 5.23±0.03Ref | ||
| Galactic latitude (°) | -9.1090Ref | Proper motion in δ (mas/yr) | -10.37±0.02Ref |
Considered as a symbiotic binary in some articles, possibly after inclusion in Kenyon (1986), the object was later deleted from the list of symbiotic stars by Belczyński et al. (2000). Known as a classical nova, Nova Sagitarii 1919, it has also exhibited dwarf nova outbursts in the last century (Sekiguchi, 1992). The study by Sekiguchi (1992) determined an orbital period of 5.7 days, with the secondary component being more evolved, resembling a G5 III star.