Trigonometric Parallaxes of Central Stars of Planetary Nebulae

Harris, Hugh C.; Dahn, C. C.; Canzian, B.; Guetter, H. H.; Leggett, S. K.; Levine, S. E.; Luginbuhl, C. B.; Monet, A. K. B.; Monet, D. G.; Pier, Jeffrey R.; Stone, R. C.; Tilleman, T.; Vrba, F. J.; Walker, Richard L.

doi:10.1086/510348

Cited by 91 publications

(127 citation statements)

References 31 publications

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“…In addition, the spectral energy distribution derived from available optical and 2MASS data (Arp & Scargle 1967;Wesemael et al 1992;Allard et al 1994;Cutri et al 2003;Harris et al 2007) is consistent with no near-IR excess from a cool companion.…”

Section: Non-binary Status Of Phl 932mentioning

confidence: 54%

“…The revised Hipparcos catalog gives a distance of 113(+114, −38) pc (van Leeuwen 2007), however this value, as with the original Hipparcos parallax leads to an non-physical stellar mass for PHL 932 of <0.1 M . An improved parallax of 3.36 ± 0.62 mas (Harris et al 2007) has shown that the Hipparcos value is in error. We adopt the new parallax distance of 298(+67, −47) pc hereafter.…”

Section: Spectral Analysis and Distancementioning

confidence: 98%

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PHL 932: When Is a Planetary Nebula Not a Planetary Nebula?

Frew

Madsen

O'Toole

et al. 2010

Publ. – Astron. Soc. Aust

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Abstract:The emission nebula around the subdwarf B (sdB) star PHL 932 is currently classified as a planetary nebula (PN) in the literature. Based on a large body of multi-wavelength data, both new and previously published, we show here that this low-excitation nebula is in fact a small Strömgren sphere (Hii region) in the interstellar medium around this star. We summarise the properties of the nebula and its ionizing star, and discuss its evolutionary status. We find no compelling evidence for close binarity, arguing that PHL 932 is an ordinary sdB star. We also find that the emission nebulae around the hot DO stars PG 0108 + 101 and PG 0109 + 111 are also Strömgren spheres in the ISM, and along with PHL 932, are probably associated with the same extensive region of high-latitude molecular gas in Pisces-Pegasus.

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Section: Non-binary Status Of Phl 932mentioning

confidence: 54%

Section: Spectral Analysis and Distancementioning

confidence: 98%

PHL 932: When Is a Planetary Nebula Not a Planetary Nebula?

Frew

Madsen

O'Toole

et al. 2010

Publ. – Astron. Soc. Aust

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“…The added incentive here is that the absolute magnitudes obtained from parallaxes are completely model independent. We have 92 DA white dwarfs in our sample with available parallax measurements from either the Yale Parallax Catalogue (van Altena et al 1995), or Hipparcos (Perryman & ESA 1997) and 9 central stars of planetary nebulae with parallaxes taken from Harris et al (2007). We present in Figure 29 the comparison between the M V values from parallax measurements and those obtained through our spectroscopic analysis.…”

Section: Comparison With Parallax Measurementsmentioning

confidence: 99%

A Spectroscopic Survey and Analysis of Bright, Hydrogen-Rich White Dwarfs

Gianninas¹,

Bergeron²,

Ruíz³

2011

ApJ

351

477

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We have conducted a spectroscopic survey of over 1300 bright (V ≤ 17.5), hydrogen-rich white dwarfs based largely on the last published version of the McCook & Sion catalog. The complete results from our survey, including the spectroscopic analysis of over 1100 DA white dwarfs, are presented. High signal-to-noise ratio optical spectra were obtained for each star and were subsequently analyzed using our standard spectroscopic technique where the observed Balmer line profiles are compared to synthetic spectra computed from the latest generation of model atmospheres appropriate for these stars. First, we present the spectroscopic content of our sample, which includes many misclassifications as well as several DAB, DAZ, and magnetic white dwarfs. Next, we look at how the new Stark broadening profiles affect the determination of the atmospheric parameters. When necessary, specific models and analysis techniques are used to derive the most accurate atmospheric parameters possible. In particular, we employ M dwarf templates to obtain better estimates of the atmospheric parameters for those white dwarfs that are in DA+dM binary systems. Certain unique white dwarfs and doubledegenerate binary systems are also analyzed in greater detail. We then examine the global properties of our sample including the mass distribution and their distribution as a function of temperature. We then proceed to test the accuracy and robustness of our method by comparing our results to those of other surveys such as SPY and Sloan Digital Sky Survey. Finally, we revisit the ZZ Ceti instability strip and examine how the determination of its empirical boundaries is affected by the latest line profile calculations.

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“…For the remaining 3 PNe, NGC 6826, NGC 2392 and IC 418 our individual distances are about 45% smaller than those given by Mendez et al (1992). For the single PN for which an optical parallax is available, NGC 7293, Harris et al (2007) measure a distance of 219 pc while Mendez et al (1992) give the higher value of 300 pc. We regard the values of Mendez et al as rather high and do not give tham much weight.…”

Section: Referencesmentioning

confidence: 99%

Planetary nebulae abundances and stellar evolution II

Pottasch

Bernard─Salas

2010

A&A

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Context. In recent years mid-and far infrared spectra of planetary nebulae have been analysed and lead to more accurate abundances. It may be expected that these better abundances lead to a better understanding of the evolution of these objects. Aims. The observed abundances in planetary nebulae are compared to those predicted by the models of Karakas (2003, Thesis, Monash Univ. Melbourne) in order to predict the progenitor masses of the various PNe used. The morphology of the PNe is included in the comparison. Since the central stars play an important role in the evolution, it is expected that this comparison will yield additional information about them. Methods. First the nitrogen/oxygen ratio is discussed with relation to the helium/hydrogen ratio. The progenitor mass for each PNe can be found by a comparison with the models of Karakas. Then the present luminosity of the central stars is determined in two ways: first by computing the central star effective temperature and radius, and second by computing the nebular luminosity from the hydrogen and helium lines. This luminosity is also a function of the initial mass so that these two values of initial mass can be compared. Results. Six of the seven bipolar nebulae can be identified as descendants of high mass stars (4−6 M ) while the seventh is ambiguous. Most of the elliptical PNe have central stars which descend from low initial mass stars, although there are a few caveats which are discussed. There is no observational evidence for a higher mass for central stars which have a high carbon/oxygen ratio. The evidence provided by the abundance comparison with the models of Karakas is consistent with the HR diagram to which it is compared. In the course of this discussion it is shown how "optically thin" nebulae can be separated from those which are "optically thick".

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Trigonometric Parallaxes of Central Stars of Planetary Nebulae

Cited by 91 publications

References 31 publications

PHL 932: When Is a Planetary Nebula Not a Planetary Nebula?

PHL 932: When Is a Planetary Nebula Not a Planetary Nebula?

A Spectroscopic Survey and Analysis of Bright, Hydrogen-Rich White Dwarfs

Planetary nebulae abundances and stellar evolution II

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