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Duerbeck, H. W.; Hazen, Martha L.; Misch, A.; Seitter, W. C.

doi:10.1023/a:1014685031286

Cited by 16 publications

(22 citation statements)

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“…MV = M Bol ). The peak visual brightness for V605 Aql (Abell 58), FG Sge (Hen 1-5), and V4334 Sgr (Sakurai's object = DPV 1) has been taken from Duerbeck et al (2002), van Genderen & Gautschy (1995, and Duerbeck et al (2000), respectively. An independent distance to FG Sge based on pulsation theory has been obtained by Mayor & Acker (1980).…”

Section: Miscellaneous Distance Methodsmentioning

confidence: 99%

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

Frew¹,

Parker²,

Bojičić³

2015

Monthly Notices of the Royal Astronomical Society

173

127

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Measuring the distances to Galactic planetary nebulae (PNe) has been an intractable problem for many decades. We have now established a robust optical statistical distance indicator, the Hα surface brightness -radius or S Hα -r relation, which addresses this problem. We developed this relation from a critically evaluated sample of primary calibrating PNe. The robust nature of the method results from our revised calibrating distances with significantly reduced systematic uncertainties, and the recent availability of high-quality data, including updated nebular diameters and integrated Hα fluxes. The S Hα -r technique is simple in its application, requiring only an angular size, an integrated Hα flux, and the reddening to the PN. From these quantities, an intrinsic radius is calculated, which when combined with the angular size, yields the distance directly. Furthermore, we have found that optically thick PNe tend to populate the upper bound of the trend, while optically-thin PNe fall along the lower boundary in the S Hα -r plane. This enables sub-trends to be developed which offer even better precision in the determination of distances, as good as 18 per cent in the case of optically-thin, high-excitation PNe. This is significantly better than any previous statistical indicator. We use this technique to create a catalogue of statistical distances for over 1100 Galactic PNe, the largest such compilation in the literature to date. Finally, in an appendix, we investigate both a set of transitional PNe and a range of PN mimics in the S Hα -r plane, to demonstrate its use as a diagnostic tool. Interestingly, stellar ejecta around massive stars plot on a tight locus in S Hα -r space with the potential to act as a separate distance indicator for these objects.

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Section: Miscellaneous Distance Methodsmentioning

confidence: 99%

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

Frew¹,

Parker²,

Bojičić³

2015

Monthly Notices of the Royal Astronomical Society

173

127

View full text Add to dashboard Cite

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“…Because of its brightness, RR Pic is one of the most studied novae (see Jones 1931;Warner 1986;Schmidtobreick et al 2003;Ribeiro & Diaz 2006;Schmidtobreick et al 2008, and references therein). An extended shell with a complex shape around RR Pic has been known and has been well documented for long time (Williams & Gallagher 1979;Duerbeck & Seitter 1979;Gill & O'Brien 1998;Downes & Duerbeck 2000). Some authors (Haefner & Metz 1982;Warner 1986) have suggested that the nova is an eclipsing binary with P = 3.…”

Section: Rr Picmentioning

confidence: 96%

“…More details on the previous and the last outbursts of T Pyx can be found in Schaefer (2010a), Schaefer et al (2013), Shore et al (2011), Shore et al (2013), De Gennaro Aquino et al (2014, Surina et al (2014), and references therein. An extended shell, different from the other nova shells and composed of many small knots, was discovered by Duerbeck & Seitter (1979). A recent study by Schaefer et al (2010) sheds new light on the complex shell of T Pyx.…”

Section: T Pyxmentioning

confidence: 98%

SALT observations of southern post-novae

Tomov

Swierczynski

Mikołajewski

et al. 2015

A&A

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Aims. We report on recent optical observations of the stellar and the nebular remnants of 22 southern post-novae. Methods. In this study, for each of our targets, we obtained and analysed long-slit spectra in the spectral range 3500-6600 Å and inResults. The changes in the emission lines' equivalent widths with the time since the outburst agree with earlier published results of other authors. We estimated an average value α = 2.37 for the exponent of the power law fitted to the post-novae continua. Our observations clearly show the two-component structure of the V842 Cen expanding nebulae, owing to the different velocities of the ejected matter. We discovered an expanding shell around V382 Vel with an outer diameter of about 12 .

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“…Already in 1979 ground-based imaging by Duerbeck & Seitter (1979) detected a shell of ejected matter, a few arcsec across, that surrounded the system. Subsequent observations by Seitter (1986) and Duerbeck (1987) revealed the presence of structures in the shell, while Shara et al (1989) discovered the additional presence of a fainter extended shell with a radius of about 10 arcsec.…”

Section: Introductionmentioning

confidence: 99%

The secrets of T Pyxidis

Gilmozzi¹,

Selvelli²

2006

A&A

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Aims. We study the UV spectral behavior of the recurrent nova T Pyx during 16 years of IUE observations. Methods. We examined both the IUE line-by-line images and the extracted spectra in order to understand the reality and the origin of the observed spectral variations. We compare different extraction methods and their influence on the spectrum of an extended object. Results. The UV continuum of T Pyx has remained nearly constant in slope and intensity over this time interval, without any indication of long-term trends. The reddening determined from the UV data is E B−V = 0.25 ± 0.02. The best single-curve fit to the dereddened UV continuum is a power-law distribution ∝λ −2.33 . The tail of this curve agrees well with the B, V, and J magnitudes of T Pyx, indicating that the contribution of the secondary star is negligible. One peculiar aspect of T Pyx is that most emission lines (the strongest ones being those of CIV 1550 and HeII 1640) show substantial changes both in intensity and detectability, in contrast to the near constancy of the continuum. Several individual spectra display emission features that are difficult to identify, suggesting a composite spectroscopic system. We tentatively ascribe the origin of these transient emission features either to loops and jets from the irradiated secondary or to moving knots of the surrounding nebula that are (temporarily) projected in front of the system. The inspection of all IUE line-by-line images has led to the detection of emission spikes outside the central strip of the spectrum, which in some cases seem associated to known emission features in the (main) spectrum. A comparison with other ex-novae reveals a surprising similarity to the spectrum of the very-slow nova HR Del, whose white dwarf primary has a mass that is allegedly about one half that of T Pyx.

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Cited by 16 publications

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The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

SALT observations of southern post-novae

The secrets of T Pyxidis

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