An ISO and IUE study of planetary nebula NGC 2440

Salas, JB; Pottasch, S. R.; Feibelman, W. A.; Wesselius, P. R.

doi:10.1051/0004-6361:20020351

Cited by 27 publications

(7 citation statements)

References 29 publications

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“…NGC 2440 has been observed by many authors, including Bernard-Salas et al (2002) who combined ISO IR data with IUE UV data and previously-published optical data; and Tsamis et al (2003), who observed the entire nebula and combined their optical data with IUE data; and Krabbe & Copetti (2006) observed in the optical only. Our ion-summed C abundance is 82% of what Tsamis et al (2003) reports, and only 28% of values reported by Kwitter et al (2003) and Bernard-Salas et al (2002). Our ion-summed N abundance is ∼50% of Kwitter et al (2003) Tsamis et al (2003).…”

Section: Ngc 2440contrasting

confidence: 45%

CO-SPATIAL LONG-SLIT UV/OPTIC AL SPECTRA OF 10 GALACTIC PLANETARY NEBULAE WITHHST/STIS. I. DESCRIPTION OF THE OBSERVATIONS, GLOBAL EMISSION-LINE MEASUREMENTS, AND CNO ABUNDANCES

Dufour

Kwitter

Shaw

et al. 2015

ApJ

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We present observations and initial analysis from an HST Cycle 19 program using STIS to obtain the first co-spatial, UV-optical spectra of ten Galactic planetary nebulae (PNe). Our primary objective was to measure the critical emission lines of carbon and nitrogen with unprecedented S/N and spatial resolution over the wavelength range 1150-10270Å, with the ultimate goal of quantifying the production of these elements in low-and intermediate-mass stars. Our sample was selected from PNe with a near-solar metallicity, but spanning a broad range in N/O based on published ground-based and IUE spectra. This study, the first of a series, concentrates on the observations and emission-line measurements obtained by integrating along the entire spatial extent of the slit. We derived ionic and total elemental abundances for the seven PNe with the strongest UV line detections (IC 2165, IC 3568, NGC 2440, NGC 3242, NGC 5315, NGC 5882, and NGC 7662). We compare these new results with other recent studies of the nebulae, and discuss the relative merits of deriving the total elemental abundances of C, N, and O using ionization correction factors (ICFs) versus summed abundances. For the seven PNe with the best UV line detections, we conclude that summed abundances from direct diagnostics of ions with measurable UV lines gives the most accurate values for the total elemental abundances of C and N (although ICF abundances often produced good results for C). In some cases where significant discrepancies exist between our abundances and those from other studies, we show that the differences can often be attributed to their use of fluxes that are not co-spatial. Finally, we examined C/O and N/O versus O/H and He/H in well-observed Galactic, LMC, and SMC PNe, and found that highly accurate abundances are essential for properly inferring elemental yields from their progenitor stars. Future papers will discuss photoionization modeling of our observations, both of the integrated spectra and spatial variations of the UV vs. optical lines along the STIS slit lengths, which are unique to our observations.

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Section: Ngc 2440contrasting

confidence: 45%

CO-SPATIAL LONG-SLIT UV/OPTIC AL SPECTRA OF 10 GALACTIC PLANETARY NEBULAE WITHHST/STIS. I. DESCRIPTION OF THE OBSERVATIONS, GLOBAL EMISSION-LINE MEASUREMENTS, AND CNO ABUNDANCES

Dufour

Kwitter

Shaw

et al. 2015

ApJ

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“…Lowering T e from 19,000 K to 15,000 K would double the Ne iii abundance derived from the 3869 8 line. It is known that in some PNs the temperature obtained from the Ne iii ion is lower than that from the O iii (Bernard-Salas et al 2002). Another possible explanation is that there are some regions with dust obscuring the optical emission lines.…”

Section: Neon and Sulfur Abundancesmentioning

confidence: 98%

Dust in the Extremely Metal‐Poor Blue Compact Dwarf Galaxy I Zw 18: TheSpitzerMid‐infrared View

Wu¹,

Charmandaris²,

Hunt³

et al. 2007

ApJ

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I Zw 18, a blue compact dwarf (BCD) galaxy with the second lowest metallicity measured in a star-forming object, has been observed with all three instruments on board the Spitzer Space Telescope. We present the deepest 5Y36 m mid-infrared (mid-IR) spectrum of this galaxy as yet obtained, as well as 3.6Y70 m imaging results. As with SBS 0335À052E, another BCD with similar metallicity, I Zw 18 shows no detectable emission from polycyclic aromatic hydrocarbons (PAHs). However, the continuum emission, from 15 to 70 m, of I Zw 18 has a much steeper slope, more characteristic of a typical starburst galaxy of solar abundance. The neon abundance as measured from the infrared finestructure lines is $1/23 Z , and the sulfur abundance is $1/35 Z , generally consistent with the nebular oxygen abundance of 1/30 Z derived from optical lines. This suggests that the extinction to the infrared-emitting regions of this galaxy is low, also in agreement with the optical Balmer line ratios.

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“…Finally, we shall be presenting an Infrared Space Observatory (ISO) 1 pipeline spectrum for NGC 2440. Sections of these data have previously been presented by Bernard Salas et al (2002), and used to determine electron densities, temperatures and elemental abundances within the source. The basic characteristics of these observations can be summarized as follows.…”

Section: Observationsmentioning

confidence: 99%

“…This is not, however, the only possible explanation, or even the most likely. The ISO spectrum of the source has been analysed by Bernard Salas et al (2002), and we show a segment of these data in Fig. 5.…”

Section: Mid‐infrared Observations Of Planetary Nebulaementioning

confidence: 99%

The haloes of planetary nebulae in the mid-infrared: evidence for interaction with the interstellar medium

Ramos-Larios¹,

Phillips²

2009

Monthly Notices of the Royal Astronomical Society

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The motion of planetary nebulae through the interstellar medium (ISM) is thought to lead to a variety of observational consequences, including the formation of bright rims, deformation and fragmentation of the shells, and a shift of the central stars away from the geometric centres of the envelopes. These and other characteristics have been noted through imaging in the visual wavelength regime. We report further observations of such shells taken in the mid-infrared (MIR), acquired through programmes of Infrared Array Camera imaging undertaken using the Spitzer Space Telescope. NGC 2440 and NGC 6629 are shown to possess likely interacting haloes, together with ram-pressure-stripped material to one side of their shells. Similarly, the outer haloes of NGC 3242 and NGC 6772 appear to have been fragmented through Rayleigh-Taylor (RT) instabilities, leading to a possible flow of ISM material towards the inner portions of their envelopes. If this interpretation is correct, then it would suggest that NGC 3242 is moving towards the NE, a suggestion which is also supported through the presence of a 60 μm tail extending in the opposite direction, and curved bands of Hα emission in the direction of motion -components which may arise through RT instabilities in the magnetized ISM.NGC 2438 possesses strong scalloping at the outer limits of its asymptotic giant branch (AGB) halo, probably reflecting RT instabilities at the nebular/ISM interface We also note that the interior structure of the source has been interpreted in terms of a recombining shell, a hypothesis which may not be consistent with the central star luminosities.Finally, we point out that two of the rims (and likely shock interfaces) appear to have a distinct signature in the MIR, whereby relative levels of 8.0 μm emission are reduced. This may imply that the grain emission agents are depleted in the post-shock AGB regimes.

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An ISO and IUE study of planetary nebula NGC 2440

Cited by 27 publications

References 29 publications

CO-SPATIAL LONG-SLIT UV/OPTIC AL SPECTRA OF 10 GALACTIC PLANETARY NEBULAE WITHHST/STIS. I. DESCRIPTION OF THE OBSERVATIONS, GLOBAL EMISSION-LINE MEASUREMENTS, AND CNO ABUNDANCES

CO-SPATIAL LONG-SLIT UV/OPTIC AL SPECTRA OF 10 GALACTIC PLANETARY NEBULAE WITHHST/STIS. I. DESCRIPTION OF THE OBSERVATIONS, GLOBAL EMISSION-LINE MEASUREMENTS, AND CNO ABUNDANCES

Dust in the Extremely Metal‐Poor Blue Compact Dwarf Galaxy I Zw 18: TheSpitzerMid‐infrared View

The haloes of planetary nebulae in the mid-infrared: evidence for interaction with the interstellar medium

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