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Puckett, Ruby P.; Schmidt, Ronald H.; Rodrick, Gary E.

doi:10.1002/047172159x.ch27

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“…The nova was independently discovered by Haseda (2005). An accurate astrometric position was derived by Puckett (2005) as α = 18 38 42.93, δ = −12 16 15.6 (corresponding to galactic coordinates l = 20.57, b = −2.79). No field star is visible at this position on DSS1 and DSS2 survey plates, indicating an outburst amplitude ∆V ≥ 11 mag.…”

Section: Introductionmentioning

confidence: 99%

BVI photometry and the spectroscopy of Nova Scuti 2005 N.2

Munari

Siviero

Navasardyan

et al. 2006

A&A

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Our CCD photometry of Nova Scuti 2005 N.2 (=V477 Sct) shows it to be a very fast nova, which is characterized by t 2 = 3 and t 3 = 6 days, affected by a E B−V ≥ 1.3 mag reddening, and which peaked at V ∼ 9.8 mag on ∼Oct. 12.0 UT. The nova was probably entering a dust condensation episode or brightness oscillations during the transition phase when it became unobservable for the seasonal conjunction with the Sun. Absolute spectrophotometry shows it to belong to the He/N class. The emission line width at half intensity is 2600 km s −1 . At least five ripples are identified in the high resolution emission lines profiles at radial velocities ranging from −980 to +700 km s −1 . The nova erupted at a large distance from the Sun and at an appreciable height above the Galactic plane, suggesting an association with the Galactic bulge (unusual for a He/N nova). The progenitor was too faint to be recorded on DSS1/2 survey plates, when setting the outburst amplitude to ∆V ≥ 11 mag.

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Section: Introductionmentioning

confidence: 99%