V598 Puppis

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V598 Puppis
V598PupLightCurve.png
A light curve for V598 Puppis, plotted from data published by Hounsell et al. (2016) [1]
Observation data
Epoch J2000.0        Equinox J2000.0 (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 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]

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<span class="mw-page-title-main">OU Puppis</span> Star in the constellation Puppis

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<span class="mw-page-title-main">V392 Persei</span> Nova in the constellation Perseus

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<span class="mw-page-title-main">R Puppis</span> Variable star in the constellation Puppis

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References

  1. ↑ 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.
  2. 1 2 3 4 5 Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics . arXiv: 2208.00211 . doi: 10.1051/0004-6361/202243940 . Gaia DR3 record for this source at VizieR.
  3. 1 2 "V598 Pup". International Variable Star Index. AAVSO . Retrieved 2023-07-26.
  4. ↑ 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.
  5. ↑ 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 .
  6. 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.
  7. ↑ 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.
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