Trigonometric Distances of Planetary Nebulae

Gutiérrez‐Moreno, A.; Anguita, C.; Loyola, P.; Moreno, H.

doi:10.1086/316427

Cited by 18 publications

(19 citation statements)

References 10 publications

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“…While this distance is a little on the low side, it is still within the error margins of the statistical distance calculated by Stanghellini et al (2008, of 890 pc) and the distance by trigonometric parallax of ∼780 pc (Gutiérrez-Moreno et al 1999). We recalculated the distance using the Stanghellini et al (2008) method, our extinction value, a radius of 32 and log F(Hβ) = −12.14 (Acker et al 1992).…”

Section: Lightcurvesupporting

confidence: 53%

The post-common-envelope, binary central star of the planetary nebula Hen 2-11

Jones

Boffin

Miszalski

et al. 2014

A&A

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We present a detailed photometric study of the central star system of the planetary nebula Hen 2-11, selected for study because of its low-ionisation filaments and bipolar morphology -traits which have been strongly linked with central star binarity. Photometric monitoring with NTT-EFOSC2 reveals a highly irradiated, double-eclipsing, post-common-envelope system with a period of 0.609 d. Modelling of the lightcurve indicates that the nebular progenitor is extremely hot, while the secondary in the system is probably a K-type main sequence star. The chemical composition of the nebula is analysed, showing Hen 2-11 to be a medium-excitation nonType i nebula. A simple photoionisation model is constructed determining abundance ratios of C/O and N/O which would be consistent with the common-envelope cutting short the AGB evolution of the nebular progenitor. The detection of a post-common-envelope binary system at the heart of Hen 2-11 further strengthens the link between binary progeny and the formation of axisymmetric planetary nebulae with patterns of low-ionisation filaments, clearly demonstrating their use as morphological indicators of central star binarity.

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Section: Lightcurvesupporting

confidence: 53%

The post-common-envelope, binary central star of the planetary nebula Hen 2-11

Jones

Boffin

Miszalski

et al. 2014

A&A

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“…(1) Acker (1978), (2) Acker et al (1998), (3) , (4) Bässgen et al (1995), (5) Christianto & Seaquist (1998), (6) Ciardullo et al (1999), (7) Costero et al (1986), (8) Gathier et al (1986a), (9) Gathier et al (1986b), (10) Gurzadyan (1970) (11) Gutiérrez- Moreno et al (1999), (12) Hajian et al (1993), (13) Hajian et al (1995), (14) Hajian et al (1997), (15) Harrington & Dahn (1980), (16) Harris et al (1997), (17) Huemer & Weinberger (1988), (18) Jacoby (1988), (19) Kaler & Lutz (1985), (20) , (21) Kohoutek (1995), (22) Lutz (1973), (23) Maciel (1996), (24) Maciel & Cazetta (1997), (25) Maciel & Pottasch (1980), (26) Martin (1994), (27) Masson (1986), (28) Masson (1989), (29) Meatheringham et al (1988), (30) Mendez & Niemela (1981), (31) …”

Section: Discussionmentioning

confidence: 99%

The distance scale of planetary nebulae

Bensby

Lundström

2001

A&A

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Abstract. By collecting distances from the literature, a set of 73 planetary nebulae with mean distances of high accuracy is derived. This sample is used for recalibration of the mass-radius relationship, used by many statistical distance methods. An attempt to correct for a statistical peculiarity, where errors in the distances influences the mass-radius relationship by increasing its slope, has been made for the first time. Distances to PNe in the Galactic Bulge, derived by this new method as well as other statistical methods from the last decade, are then used for the evaluation of these methods as distance indicators. In order of achieving a Bulge sample that is free from outliers we derive new criteria for Bulge membership. These criteria are much more stringent than those used hitherto, in the sense that they also discriminate against background objects. By splitting our Bulge sample in two, one with optically thick (small) PNe and one with optically thin (large) PNe, we find that our calibration is of higher accuracy than most other calibrations. Differences between the two subsamples, we believe, are due to the incompleteness of the Bulge sample, as well as the dominance of optical diameters in the "thin" sample and radio diameters in the "thick" sample. Our final conclusion is that statistical methods give distances that are at least as accurate as the ones obtained from many individual methods. Also, the "long" distance scale of Galactic PNe is confirmed.

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“…The ground-based US Naval Observatory (USNO) CCD parallaxes of Harris et al (2007) form an homogenous sample of accurate distances for several nearby PNe, and Smith (2015) has shown that they form a reliable, internally consistent dataset. Owing to uncertain systematics, we have not used the ground-based data from Gutiérrez-Moreno et al (1999). The Hipparcos parallaxes (van Leeuwen 2007) have also been shown to be problematic (e.g.…”

Section: Trigonometric Distancesmentioning

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

166

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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Trigonometric Distances of Planetary Nebulae

Cited by 18 publications

References 10 publications

The post-common-envelope, binary central star of the planetary nebula Hen 2-11

The post-common-envelope, binary central star of the planetary nebula Hen 2-11

The distance scale of planetary nebulae

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

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