C/O ratios in planetary nebulae with dual-dust chemistry from faint optical recombination lines

García‐Rojas, J.; Delgado-Inglada, G.; García–Hernández, D. A.; Dell’Agli, F.; Lugaro, Maria; Karakas, Amanda I.; Rodríguez, Mónica

doi:10.1093/mnras/stx2519

Cited by 24 publications

(22 citation statements)

References 124 publications

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“…Also, for their intermediate O ++ /H + estimate of 5.61 × 10 −4 ,Liu et al (2000) state that the contamination from recombination excitation is roughly the same for the [Oii]λλ3726, 3729 nebular lines and the [Oii]λλ7320, 7330 auroral lines, so that their ratio is relatively unaffected. Similarly,García-Rojas et al (2018) studied nine planetary nebula with n e > 3500 cm −3 and found T e (Oii) was over-estimated by only a few hundred Kelvin due to recombination excitation. We therefore expect our lower-density Hii regions to be even less affected.…”

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confidence: 99%

Present-day mass-metallicity relation for galaxies using a new electron temperature method

Yates

Schady

Chen

et al. 2020

A&A

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Aims. We investigate electron temperature (T e ) and gas-phase oxygen abundance (Z Te ) measurements for galaxies in the local Universe (z < 0.25). Our sample comprises spectra from a total of 264 emission-line systems, ranging from individual Hii regions to whole galaxies, including 23 composite Hii regions from 'star-forming main sequence' galaxies in the MaNGA survey. Methods. We utilise 130 of these systems with directly measurable T e (Oii) to calibrate a new metallicity-dependent T e (Oiii) -T e (Oii) relation that provides a better representation of our varied dataset than existing relations from the literature. We also provide an alternative T e (Oiii) -T e (Nii) calibration. This new T e method is then used to obtain accurate Z Te estimates and form the mass -metallicity relation (MZR) for a sample of 118 local galaxies.Results. We find that all the T e (Oiii) -T e (Oii) relations considered here systematically under-estimate Z Te for low-ionisation systems by up to 0.6 dex. We determine that this is due to such systems having an intrinsically higher O + abundance than O ++ abundance, rendering Z Te estimates based only on [Oiii] lines inaccurate. We therefore provide an empirical correction based on strong emission lines to account for this bias when using our new T e (Oiii) -T e (Oii) and T e (Oiii) -T e (Nii) relations. This allows for accurate metallicities (1σ = 0.08 dex) to be derived for any low-redshift system with an [Oiii]λ4363 detection, regardless of its physical size or ionisation state. The MZR formed from our dataset is in very good agreement with those formed from direct measurements of metal recombination lines and blue supergiant absorption lines, in contrast to most other T e -based and strong-line-based MZRs. Our new T e method therefore provides an accurate and precise way of obtaining Z Te for a large and diverse range of star-forming systems in the local Universe.

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confidence: 99%

Present-day mass-metallicity relation for galaxies using a new electron temperature method

Yates

Schady

Chen

et al. 2020

A&A

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“…A good fit was achieved adopting three broad WR features from C , C and He and five narrow nebular lines corresponding to He , C , N and [Ar ]. We have relied on García-Rojas et al (2018) and the NIST Atomic Spectra Database Lines 5 to identify these emission lines. Two of the nebular lines listed in Table 1, those at 𝜆 obs 4644.1 and 4652.0 Å present in the BB, corresponds to blends.…”

Section: The Cspn Of M 2-31mentioning

confidence: 99%

Planetary nebulae with Wolf-Rayet-type central stars -- II. Dissecting the compact planetary nebula M2-31 with GTC MEGARA

Rechy-García,

Toalá,

Cazzoli

et al. 2021

Preprint

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We present a comprehensive analysis of the compact planetary nebula M 2-31 investigating its spectral properties, spatiokinematical structure and chemical composition using GTC MEGARA integral field spectroscopic observations and NOT ALFOSC medium-resolution spectra and narrow-band images. The GTC MEGARA high-dispersion observations have remarkable tomographic capabilities, producing an unprecedented view of the morphology and kinematics of M 2-31 that discloses a fast spectroscopic bipolar outflow along position angles 50 • and 230 • , an extended shell and a toroidal structure or waist surrounding the central star perpendicularly aligned with the fast outflows. These observations also show that the C emission is confined in the central region and enclosed by the [N ] emission. This is the first time that the spatial segregation revealed by a 2D map of the C line implies the presence of multiple plasma components. The deep NOT ALFOSC observations allowed us to detect broad WR features from the central star of M 2-31, including previously undetected broad O lines that suggest a reclassification as a [WO4]-type star.

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“…The colorbar located on the right side of both panels runs from low to high values of O ++ /(O + +O ++ ). Henry 2001; Hyung et al 2001;Pottasch et al 2003a;Tsamis et al 2003;Wesson & Liu 2004;Pottasch et al 2009;García-Rojas et al 2009, 2012Bohigas et al 2013;García-Rojas et al 2015;García-Rojas et al 2018;Wesson et al 2018).…”

Section: Potassiummentioning

confidence: 99%

Ionization correction factors for sodium, potassium, and calcium in planetary nebulae

Amayo

Delgado-Inglada

García‐Rojas

2019

Monthly Notices of the Royal Astronomical Society

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We use a large grid of photoionization models that are representative of observed planetary nebulae (PNe) to derive ionization correction factors (ICFs) for sodium, potassium, and calcium. In addition to the analytical expressions of the ICFs, we provide the range of validity where the ICFs can be safely used and an estimate of the typical uncertainties associated with the ICFs. We improved the previous ICFs for calcium and potassium in the literature and suggest for the first time an ICF for sodium. We tested our ICFs with a sample of 39 PNe with emission lines of some ion of these elements. No obvious trend is found between the derived abundances and the degree of ionization, suggesting that our ICFs do not seem to be introducing an artificial bias in the results. The abundances found in the studied PNe range from −2.88 +0.21 −0.22 to −2.09 ± 0.21 in log(Na/O), from −4.20 +0.31 −0.45 to −3.05 +0.26 −0.47 in log(K/O), and from −3.71 +0.41 −0.34 to −1.57 +0.33 −0.47 in log(Ca/O). These numbers imply that some of the studied PNe have up to ∼65%, 75%, or 95% of their Na, K, and/or Ca atoms condensed into dust grains, respectively. As expected, the highest depletions are found for calcium which is the element with the highest condensation temperature.

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C/O ratios in planetary nebulae with dual-dust chemistry from faint optical recombination lines

Cited by 24 publications

References 124 publications

Present-day mass-metallicity relation for galaxies using a new electron temperature method

Present-day mass-metallicity relation for galaxies using a new electron temperature method

Planetary nebulae with Wolf-Rayet-type central stars -- II. Dissecting the compact planetary nebula M2-31 with GTC MEGARA

Ionization correction factors for sodium, potassium, and calcium in planetary nebulae

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