V598 Puppis
| Observation data Epoch J2000.0 Equinox 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 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 2 and 5, 2007, peaking in brightness on June 5.[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
[edit]- ↑ Hounsell, R.; Darnley, M. J.; Bode, M. F.; Harman, D. J.; Surina, F.; Starrfield, S.; Holdsworth, D. L.; Bewsher, D.; Hick, P. P.; Jackson, B. V.; Buffington, A.; Clover, J. M.; Shafter, A. W. (April 2016). "Nova Light Curves From The Solar Mass Ejection Imager (SMEI) - II. The extended catalog". The Astrophysical Journal. 820 (2): 104. arXiv:1512.03321. Bibcode:2016ApJ...820..104H. doi:10.3847/0004-637X/820/2/104. S2CID 53577268.
- 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- 1 2 "V598 Pup". International Variable Star Index. AAVSO. Retrieved 2023-07-26.
- ↑ Samus, N. N.; Durlevich, O. V.; 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. Bibcode:1960MNRAS.121..337F. doi:10.1093/mnras/121.4.337.
- 1 2 3 Read, A. M.; Saxton, R. D.; Torres, M. A. P.; Esquej, P.; Kuulkers, E.; Jonker, P. G.; Osborne, J. P.; Freyberg, M. J.; Challis, P. (2008). "XMM-Newton slew survey discovery of the nova XMMSL1 J070542.7-381442 (V598 Puppis)". Astronomy and Astrophysics. 482 (2): L1–L4. arXiv:0803.0419. Bibcode:2008A&A...482L...1R. doi:10.1051/0004-6361:200809456. S2CID 17579620.
- ↑ Schaefer, Bradley E. (2021). "Discovery of 13 New Orbital Periods for Classical Novae". Research Notes of the AAS. 5 (6): 150. arXiv:2106.13907. Bibcode:2021RNAAS...5..150S. doi:10.3847/2515-5172/ac0d5b. S2CID 235632263.
