Planetary nebula K1-9

Kondratyeva, L. N.; Denissyuk, E. K.

doi:10.1051/0004-6361:20031563

Cited by 3 publications

(2 citation statements)

References 10 publications

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“…All objects were cross-checked for duplication and identity, noting that the classifications of many nebulae have been fluid over time. An example is the Type I planetary K 1-9 (PK 219+01.1; Kondratyeva & Denissyuk 2003) as noted in the SIMBAD database.…”

Section: Input Cataloguementioning

confidence: 99%

“…For PNe without integrated values for R [N ii] , we adopted an average of the data presented in the Catalog of Relative Emission Line Intensities Observed in Planetary Nebulae (ELCAT) 8 compiled by Kaler, Shaw & Browning (1997), supplemented with data taken from more recent papers in the literature, including Kraan-Korteweg et al (1996), Pollacco & Bell (1997), , Kerber et al (1997Kerber et al ( , 1998Kerber et al ( , 2000, Perinotto & Corradi (1998), Condon, Kaplan & Terzian (1999), Ali (1999), Escudero & Costa (2001), Rodríguez, Corradi & Mampaso (2001), Milingo et al (2002, Kondratyeva & Denissyuk (2003), Kwitter, Henry & Milingo (2003), Costa, Uchida & Maciel (2004), Emprechtinger et al (2004), Exter, Barlow & Walton (2004, Costa, Uchida & Maciel (2004), Górny et al (2004Górny et al ( , 2009, Krabbe & Copetti (2006), Henry et al (2010, Miszalski et al (2012a,b), García-Rojas et al (2012) and Frew et al (2012). An average of measurements from several independent sources should be fairly representative of the integrated [N ii]/Hα ratio for each PN, and we estimate a typical uncertainties in R [N ii] of 10-30%.…”

Section: Spectrophotometric Datamentioning

confidence: 99%

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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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Section: Input Cataloguementioning

confidence: 99%

Section: Spectrophotometric Datamentioning

confidence: 99%

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

Frew,

Bojicic,

Parker

2012

Preprint

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Properties of central stars of planetary nebulae with distances in Gaia DR2

González-Santamaría

Manteiga

Manchado

et al. 2019

A&A

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Context. We have compiled a catalogue of central stars of planetary nebulae (CSPN) with reliable distances and positions obtained from Gaia Data Release 2 (DR2) astrometry. Distances derived from parallaxes allow us to analyse the galactic distribution and estimate other parameters such as sizes, kinematical ages, bolometric magnitudes, and luminosities. Aims. Our objective is to analyse the information regarding distances together with other available literature data about photometric properties, nebular kinematics, and stellar effective temperatures to throw new light on this rapid and rather unknown evolutionary phase. We seek to understand how Gaia distances compare with other indirect methods commonly used and, in particular, with those derived from non-local thermodynamic equilibrium (non-LTE) models; how many planetary nebulae (PNe) populate the Galaxy; and how are they spatially distributed. We also aim to comprehend their intrinsic luminosities, range of physical sizes of the nebulae; how to derive the values for their kinematical ages; and whether those ages are compatible with those derived from evolutionary models. Methods. We considered all PNe listed in catalogues from different authors and in Hong Kong/AAO/Strasbourg/H α (HASH) database. By X-matching their positions with Gaia DR2 astrometry we were able to identify 1571 objects in Gaia second archive, for which we assumed distances calculated upon a Bayesian statistical approach. From those objects, we selected a sample of PNe with good quality parallax measurements and distance derivations, we which refer to as our Golden Astrometry PNe sample (GAPN), and obtained literature values of their apparent sizes, radial and expansion velocities, visual magnitudes, interstellar reddening, and effective temperatures. Results. We found that the distances derived from DR2 parallaxes compare well with previous astrometric derivations of the United States Naval Observatory and Hubble Space Telescope, but that distances inferred from non-LTE model fitting are overestimated and need to be carefully reviewed. From literature apparent sizes, we calculated the physical radii for a subsample of nebulae that we used to derive the so-called kinematical ages, taking into account literature expansion velocities. Luminosities calculated with DR2 distances were combined with literature central stars T e f f values in a Hertzsprung-Russell (HR) diagram to infer information on the evolutionary status of the nebulae. We compared their positions with updated evolutionary tracks finding a rather consistent picture. Stars with the smallest associated nebular radii are located in the flat luminosity region of the HR diagram, while those with the largest radii correspond to objects in a later stage, getting dimmer on their way to become a white dwarf. Finally, we commented on the completeness of our catalogue and calculated an approximate value for the total number of PNe in the Galaxy.

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