High-Resolution Spectroscopy of the Planetary Nebulae PM 1–242, PM 1–318 and PM 1–322

Miranda, L. F.; Vázquez, R.; Guerrero, M. A.; Pereira, C. B.; Iñiguez-Garín, E.

doi:10.1071/as09029

Cited by 6 publications

(2 citation statements)

References 17 publications

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“…We expect most if not all of our detected PNe to be relatively young, as highly evolved PNe have often lost their radio emission Cohen et al (2011), We also expect them to have more massive central stars exhibiting high stellar temperatures as is usually the case for Type I PNe (Tylenda 1989;Cohen et al 2007a). Their compact nature, bright IR emission and the measured relatively high electron densities of FBP2, FBP3 and FBP4 further support their early evolutionary stage (see Zhang & Kwok 1991;Miranda et al 2010).…”

Section: Discussionmentioning

confidence: 65%

New Galactic Planetary nebulae selected by radio and multiwavelength characteristics

Fragkou

Parker

Bojičić

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We have used the Cornish radio catalogue combined with the use of multiwavelength data to identify 62 new Planetary Nebula (PN) candidates close to the Galactic mid-plane. Of this sample 11 have weak optical counterparts in deep narrow band Hα imaging that allows their spectroscopic follow-up. We have observed eight of these candidates spectroscopically, leading to the confirmation of 7 out of 8 as PNe. All but one of our sample of newly detected PNe appear to be of Type I chemistry with very large [NII]/Hα ratios. This indicates that our selection method heavily favours detection of this kind of PN. Cornish is a low Galactic latitude survey where young objects and Type I PNe (thought to derive from higher mass progenitors) are more plentiful, but where optical extinction is large. The very high success rate in correctly identifying PNe in this zone proves the efficacy of our radio and multiple multi-wavelength diagnostic tools used to successfully predict and then confirm their PN nature, at least in the cases where an optical counterpart is found and has been observed. The study reinforces the effective use of a combination of multi-wavelength and optical data in the identification of new Galactic PNe and especially those of Type I chemistries whose dusty environments often prevents their easy detection in the optical regime alone.

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Section: Discussionmentioning

confidence: 65%

New Galactic Planetary nebulae selected by radio and multiwavelength characteristics

Fragkou

Parker

Bojičić

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…To supplement these catalogues, we also added a sample of ∼320 true and candidate PNe from the recent literature, primarily discovered (or confirmed) optically. These were taken from Zanin et al (1997), Weinberger et al (1999), Beer & Vaughan (1999), Kerber et al (2000), Cappellaro et al (2001), Eracleous et al (2002, Whiting, Hau & Irwin (2002), Bond, Pollacco & Webbink (2003), Boumis et al (2003Boumis et al ( , 2006, Lanning & Meakes (2004), Jacoby & Van de Steene ( 2004), Suárez et al (2006), Frew, Madsen & Parker (2006, Whiting et al (2007), Miszalski et al (2009), Fesen & Milisavljevic (2010, Jacoby et al (2010), Miranda et al (2010), Acker et al (2012), Parker et al (2012b), Parthasarathy et al (2012), andKronberger et al (2012).…”

Section: Input Cataloguementioning

confidence: 99%

A catalogue of integrated H-alpha fluxes for 1,258 Galactic planetary nebulae

Frew,

Bojicic,

Parker

2012

Preprint

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We present a catalogue of new integrated Hα fluxes for 1258 Galactic planetary nebulae (PNe), with the majority, totalling 1234, measured from the Southern Hα Sky Survey Atlas (SHASSA) and/or the Virginia Tech Spectral-line Survey (VTSS). Aperture photometry on the continuum-subtracted digital images was performed to extract Hα+[N ii] fluxes in the case of SHASSA, and Hα fluxes from VTSS. The [N ii] contribution was then deconvolved from the SHASSA flux using spectrophotometric data taken from the literature or derived by us. Comparison with previous work shows that the flux scale presented here has no significant zero-point error. Our catalogue is the largest compilation of homogeneously derived PN fluxes in any waveband yet measured, and will be an important legacy and fresh benchmark for the community. Amongst its many applications, it can be used to determine statistical distances for these PNe, determine new absolute magnitudes for delineating the faint end of the PN luminosity function, provide baseline data for photoionization and hydrodynamical modelling, and allow better estimates of Zanstra temperatures for PN central stars with accurate optical photometry. We also provide total Hα fluxes for another 76 objects which were formerly classified as PNe, as well as independent reddening determinations for ∼270 PNe, derived from a comparison of our Hα data with the best literature Hβ fluxes. In an appendix, we list corrected Hα fluxes for 49 PNe taken from the literature, including 24 PNe not detected on SHASSA or VTSS, re-calibrated to a common zero-point.

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Catalogue of the central stars of planetary nebulae

Weidmann

Mari

Schmidt

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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High-Resolution Spectroscopy of the Planetary Nebulae PM 1–242, PM 1–318 and PM 1–322

Cited by 6 publications

References 17 publications

New Galactic Planetary nebulae selected by radio and multiwavelength characteristics

New Galactic Planetary nebulae selected by radio and multiwavelength characteristics

A catalogue of integrated H-alpha fluxes for 1,258 Galactic planetary nebulae

Catalogue of the central stars of planetary nebulae

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