[ITAL]HUBBLE SPACE TELESCOPE[/ITAL][ITAL]Hubble Space Telescope[/ITAL] Observations of the Planetary Nebula K648 in the Globular Cluster M15

Alves, D. R.; Bond, Howard E.; Livio, Mario

doi:10.1086/301558

Cited by 54 publications

(74 citation statements)

References 66 publications

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“…Globular cluster PNe: Both Pease 1, also known as K 648 (Buell et al 1997;Alves, Bond & Livio 2000) and the peculiar H-deficient nebula GJJC 1 (Cohen & Gillett 1989;Borkowski & Harrington 1991) are bona fide members of their respective globular clusters, M 15 (NGC 7078) and M 22 (NGC 6656). Pease 1 has been imaged with HST and has good estimates of its angular size (Alves et al 2000) and integrated flux which qualify it to be a primary calibrator. Jacoby et al (1997) conducted an extensive search for PN candidates in Galactic globular clusters, finding two new examples, JaFu 1 in Palomar 6 and JaFu 2 in the luminous cluster NGC 6441.…”

Section: Bmp J1613-5406mentioning

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

172

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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Section: Bmp J1613-5406mentioning

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

172

127

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“…Another possible alternative could perhaps be a sufficiently wide initial-to-final mass relation, allowing lower initial masses to sometimes contribute high enough final masses. This idea is somewhat unpopular but has not been empirically rejected yet (Weidemann 2000;Alves et al 2000;Ferrario et al 2005). Metallicity could certainly play a role in widening the initial-to-final mass relation ( Meng et al 2007).…”

Section: Post-agb Ages and Massesmentioning

confidence: 99%

“…This central star is bright enough to permit a good non-LTE model atmosphere analysis of its absorption-line spectrum, which gives information about its effective temperature and surface gravity (e.g., McCarthy et al 1997). Together with the known distance to the cluster, this permits to obtain the luminosity and (again using the luminosityYcore mass relation) the mass of the central star, which turns out to be 0.6 M (Alves et al 2000).…”

Section: Post-agb Ages and Massesmentioning

confidence: 99%

Toward Better Simulations of Planetary Nebulae Luminosity Functions

Méndez

Teodorescu

Schönberner

et al. 2008

ApJ

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We describe a procedure for the numerical simulation of the planetary nebulae luminosity function ( PNLF), improving on previous work. Earlier PNLF simulations were based on an imitation of the observed distribution of the intensities of [O iii] k5007 relative to H , generated predominantly using random numbers. We are now able to replace this by a distribution derived from the predictions of hydrodynamical PN models (Schönberner et al. 2007), which are made to evolve as the central star moves across the HR diagram, using proper initial and boundary conditions. In this way we move one step closer to a physically consistent procedure for the generation of a PNLF. As an example of these new simulations, we have been able to reproduce the observed PNLF in the Small Magellanic Cloud.

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“…While this scenario, considered in some detail by Alves et al (2000) for K 648 (see also Jacoby et al 1997), is especially appealing for a PN in a globular cluster where the number density of stars is high, it offers a valuable explanation for the existence of Pop II PNe in general.…”

Section: Initial Mass Of the Progenitor Star?mentioning

confidence: 99%

“…This explanation is hampered by the discovery of many WDs with masses close to 0.51 M in the nearby globular cluster M 4 (Richer et al 1997;see, however, de Marchi et al 2004) and would probably not work for, e.g., K 648 (Alves et al 2000). Nonetheless, for extremely metal-deficient stars, including first-generation Population III stars (Pop III, Z ≤ 10 −10 ) and other "crypto-Population III" stars (Z ≤ 10 −5 ), this possibility appears quite conceivable (e.g., Willson et al 1996).…”

Section: Initial Mass Of the Progenitor Star?mentioning

confidence: 99%

Endogenous oxygen in the extremely metal-poor planetary nebula PN G135.9+55.9

Pequignot¹,

Tsamis²

2005

A&A

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Abstract. It is shown that, in contrast to recent claims, oxygen (and helium) may not be extraordinarily underabundant in the new galactic halo planetary nebula (GHPN) PN G135.9+55.9 (hereafter PN G135). Determining elemental abundances in hot, highly ionized objects such as PN G135 depends critically on a proper description of the collisional excitation of the hydrogen Balmer lines, the departure from Case B recombination of hydrogen, the underlying stellar absorption lines, the shape of the primary continuum and the ionization equilibrium of highly ionized species of both oxygen and neon. Conversely, PN G135provides unique checks of atomic data in unusual conditions: the H  collision strengths obtained by Aggarwal et al. (1991) for 1s − n transitions (3 ≤ n ≤ 5) are too large, while those obtained by Anderson et al. (2002) are acceptable. Empirical collision strengths are presented for n > 5. Photoionization models of PN G135 that fit all available optical data can be demonstrated only for oxygen abundances 12 + log (O/H) > 7.2 (>1/30 solar) and values 0.6 dex larger are possible, depending on the assumed C/O abundance ratio. Plausible variations in the geometry of the nebula, the primary stellar continuum and the atomic data do not alter this conclusion. The C/O ratio is less than 10 by number and Ne/O is at most solar. A satisfactory model for PN G135 can be obtained in which elemental abundances are nearly the same as those of a new detailed model for K 648, the prototypical GHPN in the old globular cluster M 15 (with 12 + log (O/H) = 7.58 ∼ 1/13 solar), although C/O may be smaller. Nonetheless, given the paucity of argon and iron in the nebula, PN G135 is likely to be a more extreme Population II object than K 648, reinforcing the idea of an endogenous origin for part of the oxygen in very metal-poor PNe. Assuming a standard H-burning post-Asymptotic Giant Branch evolution, timescale and spectroscopic considerations lead to an optimal solution, in which the distance to PN G135 is 8 kpc, the effective temperature of the nucleus slightly less than 1.3 × 10 5 K, its luminosity 1.4 × 10 37 erg s −1 , its mass 0.59 M , the age of the ionized shell 10 4 yrs, the ionized mass 0.05 M and the abundances by number (H:He:C:O:Ne) = (10 6 :81 500:90:30:4.5), with C/H being rather an upper limit and O/H and Ne/H uncertain by ±0.3 and ±0.1 dex respectively. Line intensities that could be used as diagnostics of the nebular elemental abundances are provided. Detailed imaging together with ultraviolet and very deep far-red spectra of PN G135 will be essential to definitely narrow the range of acceptable parameters and help us decide whether this exceptional PN is so oxygen-poor as to possibly influence current views on stellar evolution.

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[ITAL]HUBBLE SPACE TELESCOPE[/ITAL][ITAL]Hubble Space Telescope[/ITAL] Observations of the Planetary Nebula K648 in the Globular Cluster M15

Cited by 54 publications

References 66 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

Toward Better Simulations of Planetary Nebulae Luminosity Functions

Endogenous oxygen in the extremely metal-poor planetary nebula PN G135.9+55.9

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