On the crucial cluster Andrews-Lindsay 1 and a 4% distance solution for its planetary nebula

Majaess, D.; Carraro, G.; Bidin, C. Moni; Bonatto, Charles Jose; Turner, D. G.; Moyano, Maximiliano; Бердников, Л. Н.; Giorgi, E. E.

doi:10.1051/0004-6361/201423673

“…Majaess et al (2014) refined the distance to the cluster to 10.0 ± 0.4 kpc, which we have adopted herein.…”

Section: Cluster 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

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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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“…PHR J1315-6555: Parker et al (2011 undertook a detailed study of the physical association between this bipolar PN and the intermediate-age open cluster ESO 96-SC04 (AL 1). Majaess et al (2014) refined the distance to the cluster to 10.0 ± 0.4 kpc, which we have adopted herein.…”

Section: Cluster Distancesmentioning

confidence: 99%

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

Frew,

Parker,

Bojicic

2015

Preprint

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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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“…Catalogues are an important tool in astrophysics, helping researchers in their pursuit of discoveries. For example, Majaess et al (2007) looked for a link between planetary nebulae (PNe) an open cluster, which led in part to the discovery of PN PHR 1315−6555 in the cluster Andrews-Lindsay 1 and a 4% distance solution (Majaess et al 2014). Miszalski et al (2009a) discovered 21 periodic binaries at the center of planetary nebulae by cross-matching PNe and OGLE microlensing survey catalogues.…”

Section: Introductionmentioning

confidence: 99%

Catalogue of the central stars of planetary nebulae

Weidmann

¹

,

Mari

²

,

Schmidt

³

et al. 2020

A&A

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Planetary nebulae represent a potential late stage of stellar evolution, however, their central stars (CSPNe) are relatively faint and, therefore, pertinent information is available for merely < 20% of the Galactic sample. Consequently, the literature was surveyed to construct a new catalogue of 620 CSPNe featuring important spectral classifications and information. The catalogue supersedes the existing iteration by 25% and includes physical parameters such as luminosity, surface gravity, temperature, magnitude estimates, and references for published spectra. The marked statistical improvement enabled the following pertinent conclusions to be determined: the H-rich/H-poor ratio is 2:1, there is a deficiency of CSPNe with types [WC 5-6], and nearly 80% of binary central stars belong to the H-rich group. The last finding suggests that evolutionary scenarios leading to the formation of binary central stars interfere with the conditions required for the formation of H-poor CSPN. Approximately 50% of the sample with derived values of log L⋆, log Teff, and log g, exhibit masses and ages consistent with single stellar evolutionary models. The implication is that single stars are indeed able to form planetary nebulae. Moreover, it is shown that H-poor CSPNe are formed by higher mass progenitors. The catalogue is available through the Vizier database.

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On the crucial cluster Andrews-Lindsay 1 and a 4% distance solution for its planetary nebula

Cited by 11 publications

References 53 publications

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

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

Catalogue of the central stars of planetary nebulae

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