| Observation data EpochJ2000.0 EquinoxJ2000.0 (ICRS) | |
|---|---|
| Constellation | Puppis |
| Right ascension | 07h 05m 42.500s[2] |
| Declination | −38° 14′ 39.44″[2] |
| Apparent magnitude (V) | ~3.6 - 16.6[3] |
| Characteristics | |
| Variable type | Nova[4] |
| Astrometry | |
| Radial velocity (Rv) | +292[5] km/s |
| Proper motion (μ) | RA: +0.927[2]mas/yr Dec.: +7.149[2]mas/yr |
| Parallax (π) | 0.5403±0.0306 mas[2] |
| Distance | 6,000 ± 300 ly (1,900 ± 100 pc) |
| Other designations | |
| Nova Puppis 2007b,V598 Pup,2MASS J07054250-3814394,USNO-A2.0 0450-03360039 | |
| Database references | |
| SIMBAD | data |
V598 Puppis is the name given to anova in theMilky Way Galaxy.USNO-A2.0 0450-03360039, a catalog number for the star, was discovered to be much brighter than normal inX-ray emissions on October 9, 2007, by theEuropean Space Agency'sXMM-Newtontelescope. The star was confirmed to be over 10 magnitudes, or 10,000 times, brighter than normal by the Magellan-Clay telescopeMagellan-Clay telescope atLas Campanas Observatory inChile.[6] Pre-discovery images and identification of the progenitor would ultimately shows that the nova brightened fromvisual magnitude 16.6 to brighter than magnitude 4.[3]
The nova has been officially given thevariable star designation V598 Puppis and is one of the brightest in the last decade.[6] Despite its brightness, the nova was apparently missed by amateur and professionalastronomers alike until XMM-Newton spotted the unusual X-ray source while turning from one target to another. TheAll Sky Automated Survey determined that the nova had occurred between June 2nd and 5th, 2007, peaking in brightness on June 5th.[6]
The orbital period of the two stars in V598 Puppis is 0.1628714 days, or 3 hours, 54 minutes, and 32 seconds.[7]
