Astronomy:V598 Puppis
| Observation data Epoch J2000.0 Equinox (celestial coordinates) | |
|---|---|
| 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[2] mas |
| Distance | 6,000 ± 300 ly (1,900 ± 100 pc) |
| Other designations | |
| Database references | |
| SIMBAD | data |
V598 Puppis is the name given to a nova in the Milky Way Galaxy. USNO-A2.0 0450-03360039, a catalog number for the star, was discovered to be much brighter than normal in X-ray emissions on October 9, 2007, by the European Space Agency's XMM-Newton telescope. The star was confirmed to be over 10 magnitudes, or 10,000 times, brighter than normal by the Magellan-Clay telescope Magellan-Clay telescope at Las Campanas Observatory in Chile .[6] Pre-discovery images and identification of the progenitor would ultimately shows that the nova brightened from visual magnitude 16.6 to brighter than magnitude 4.[3]
The nova has been officially given the variable 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 professional astronomers alike until XMM-Newton spotted the unusual X-ray source while turning from one target to another. The All 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]
References
- ↑ Hounsell, R.; Darnley, M. J.; Bode, M. F.; Harman, D. J.; Surina, F.; Starrfield, S.; Holdsworth, D. L.; Bewsher, D. et al. (April 2016). "Nova Light Curves From The Solar Mass Ejection Imager (SMEI) - II. The extended catalog". The Astrophysical Journal 820 (2): 104. doi:10.3847/0004-637X/820/2/104. Bibcode: 2016ApJ...820..104H.
- ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 "V598 Pup". AAVSO. https://www.aavso.org/vsx/index.php?view=detail.top&oid=161061.
- ↑ Samus, N. N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1. Bibcode: 2009yCat....102025S.
- ↑ Feast, M. W.; Thackeray, A. D.; Wesselink, A. J. (1960). "The brightest stars in the Magellanic Clouds". Monthly Notices of the Royal Astronomical Society 121 (4): 337–385. doi:10.1093/mnras/121.4.337. Bibcode: 1960MNRAS.121..337F.
- ↑ 6.0 6.1 6.2 Read, A. M.; Saxton, R. D.; Torres, M. A. P.; Esquej, P.; Kuulkers, E.; Jonker, P. G.; Osborne, J. P.; Freyberg, M. J. et al. (2008). "XMM-Newton slew survey discovery of the nova XMMSL1 J070542.7-381442 (V598 Puppis)". Astronomy and Astrophysics 482 (2): L1–L4. doi:10.1051/0004-6361:200809456. Bibcode: 2008A&A...482L...1R.
- ↑ Schaefer, Bradley E. (2021). "Discovery of 13 New Orbital Periods for Classical Novae". Research Notes of the AAS 5 (6): 150. doi:10.3847/2515-5172/ac0d5b. Bibcode: 2021RNAAS...5..150S.
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