Carbon Isotope Ratios in M10 Giants

Maas, Z. G.; Gerber, Jeffrey M.; Deibel, Alex; Pilachowski, Catherine A.

doi:10.3847/1538-4357/ab1eab

Cited by 9 publications

(11 citation statements)

References 91 publications

(142 reference statements)

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“…Note that the CN-w and the CN-s populations in our study correspond to the CN-Normal and the CN-Enhanced population byMaas et al (2019).…”

supporting

confidence: 51%

“…Recently, Maas et al (2019) reported carbon isotope ratios in giants stars in the globular cluster M10, finding that the decrement in the 12 C/ 13 C ratios both in the CN-w and the CN-s populations 3 in M10. They discuss further that to match their measurements of the surface carbon and carbon isotope ratios requires two different thermohaline mixing efficiencies.…”

Section: Synthetic Population Models and The Need For Extra Abundancementioning

confidence: 99%

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Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH Photometry. V. as a Surrogate cn_JWL Index and NGC 6723^∗ †

Lee

2019

ApJ

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We introduce new color indices cn ′ JWL (= Ca CTIO − Ca JWL ) and ch JWL [=(JW L43 − b) − (b − y)], accurate photometric measures of the CN band at λ3883 and the CH G band, respectively, in the study of the multiple populations (MPs) in globular clusters (GCs). Our photometric CN-CH relation for a large number of red-giant branch (RGB) in M5 shows that the evolutions of the CN and CH between the CN-w and CN-s populations are not continuous. Armed with our new color indices, we investigate the MPs of NGC 6723, finding the RGB populational number ratio of n(CN-w):n(CN-s) ≈ 35.5:64.5 (±2.8) with no radial gradient. Similar to other normal GCs with MPs, the helium abundance of the CN-s population inferred from the RGB bump magnitude is slightly enhanced by ∆Y = 0.012 ± 0.012. Our cn JWL and cn ′ JWL color-magnitude diagrams clearly show the discrete double AGB populations in NGC 6723, whose bright AGB populational number ratio is in marginally agreement with that of the RGB stars within the statistical errors. Finally, our synthetic cn JWL index is in good agreement with observations, except for the CN-w asymptotic giant branch (AGB). To mitigate the discrepancy in the CN-w AGB may require a mild nitrogen enhancement and/or a large decrement in the 12 C/ 13 C ratio with respect to the bright RGB.

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“…Note that the CN-w and the CN-s populations in our study correspond to the CN-Normal and the CN-Enhanced population byMaas et al (2019).…”

supporting

confidence: 51%

Section: Synthetic Population Models and The Need For Extra Abundancementioning

confidence: 99%

Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH Photometry. V. as a Surrogate cn_JWL Index and NGC 6723^∗ †

Lee

2019

ApJ

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“…The CNO surface abundances in evolved stars are modified by the nuclear burning together with internal mixing processes (Charbonnel 1994;Gratton et al 2000;Maas et al 2019). Therefore, dwarf stars are fundamentally indispensable to be observed in order to trace the CNO enrichment in the ISM.…”

mentioning

confidence: 99%

Carbon, isotopic ratio 12C/13C, and nitrogen in solar twins: constraints for the chemical evolution of the local disc

Botelho

Milone

Meléndez

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Abundances of light elements in dwarf stars of different ages are important constraints for stellar yields, Galactic chemical evolution and exoplanet chemical composition studies. We have measured C and N abundances and 12C/13C ratios for a sample of 63 solar twins spanning a wide range in age, based on spectral synthesis of a comprehensive list of CH A-X and CN B-X features using HARPS spectra. The analysis of 55 thin disc solar twins confirms the dependences of [C/Fe] and [N/Fe] on [Fe/H]. [N/Fe] is investigated as a function of [Fe/H] and age for the first time for these stars. Our derived correlation [C/Fe]-age agrees with works for solar-type stars and solar twins, but the [N/Fe]-age correlation does not. The relations [C,N/Fe]-[Fe/H] and [C,N/Fe]-age for the solar twins lay under-solar. 12C/13C is found correlated with [Fe/H] and seems to have decreased along the evolution of the local thin disc. Predictions from chemical evolution models for the solar vicinity corroborate the relations [C,N/Fe]-[Fe/H], 12C/13C-age and [N/O]-[O/H], but do not for the 12C/13C-[Fe/H] and [C/O]-[O/H] relations. The N/O ratio in the Sun is placed at the high end of the homogeneous distribution of solar twins, which suggests uniformity in the N-O budget for the formation of icy planetesimals, watery super-earths and giant planets. C and N had different nucleosynthetic origins along the thin disc evolution, as shown by the relations of [C/N], [C/O] and [N/O] against [O/H] and age. [C/N] and [C/O] are particularly observed increasing in time for solar twins younger than the Sun.

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“…While La is marginally enhanced, Ce and Nd are found to be marginally under-abundant. (Spite et al 2006;Aoki et al 2007;Maas et al 2019). The dashed line at 12 C/ 13 C = 10 separates the groups "Mixed" and "Unmixed".…”

Section: Discussionmentioning

confidence: 99%

LAMOST J045019.27+394758.7, with peculiar abundances of N, Na, V, Zn, is possibly a Sculptor dwarf galaxy escapee

Purandardas,

Goswami,

Shejeelammal

et al. 2022

Preprint

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We present the results of the high-resolution (R∼60,000) spectroscopic analysis of the star LAMOSTJ045019.27+394758.7 (hereafter J045) from the list of carbon stars of LAMOST DR2. From our analysis, we find that J045 does not exhibit the spectral characteristics of carbon stars. It is found to be a metal-poor ( [Fe/H] = −1.05) giant that shows very unusual elemental abundances, particularly for N, Na, V, and Zn. J045 shows -elements (Mg, Si, Ca) with near-solar values (<[ /Fe]> = 0.09) in contrast to Galactic stars that show [ /Fe] in the range 0.2 to 0.3 dex. In J045, Sc and Ti are under abundant with [X/Fe] ≤ −0.25. Vanadium gives [V/Fe] = 0.51 and zinc is under-abundant with [Zn/Fe] = −0.62. The object exhibits near-solar abundances for Sr, Y, Ba, Pr, and Sm. The La is marginally enhanced, and Ce and Nd are marginally under-abundant in J045. With [Ba/Eu] = −0.38, the object falls into the category of neutron-capture rich r-I stars. The estimated abundances of various elements show that the observed abundance pattern is not compatible with the abundances characteristic of Galactic metal-poor stars but matches quite closely with the abundance pattern of Sculptor Dwarf galaxy stars of similar metallicity. Based on the above observational evidences, we suggest that the object is a possible Sculptor Dwarf Galaxy escapee.

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Carbon Isotope Ratios in M10 Giants

Cited by 9 publications

References 91 publications

Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH Photometry. V. as a Surrogate cn_JWL Index and NGC 6723^∗ †

Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH Photometry. V. as a Surrogate cn_JWL Index and NGC 6723^∗ †

Carbon, isotopic ratio 12C/13C, and nitrogen in solar twins: constraints for the chemical evolution of the local disc

LAMOST J045019.27+394758.7, with peculiar abundances of N, Na, V, Zn, is possibly a Sculptor dwarf galaxy escapee

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Carbon Isotope Ratios in M10 Giants

Cited by 9 publications

References 91 publications

Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH Photometry. V. as a Surrogate cnJWL Index and NGC 6723∗ †

Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH Photometry. V. as a Surrogate cnJWL Index and NGC 6723∗ †

Carbon, isotopic ratio 12C/13C, and nitrogen in solar twins: constraints for the chemical evolution of the local disc

LAMOST J045019.27+394758.7, with peculiar abundances of N, Na, V, Zn, is possibly a Sculptor dwarf galaxy escapee

Contact Info

Product

Resources

About

Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH Photometry. V. as a Surrogate cn_JWL Index and NGC 6723^∗ †

Multiple Stellar Populations of Globular Clusters from Homogeneous Ca–CN–CH Photometry. V. as a Surrogate cn_JWL Index and NGC 6723^∗ †