The Origin of the Galaxy and Local Group

Bland‐Hawthorn, J.; Freeman, K. C.; Matteuccí, F.

doi:10.1007/978-3-642-41720-7

Cited by 10 publications

(10 citation statements)

References 276 publications

(426 reference statements)

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“…CMFs with a higher mass cutoff produce more clumpiness in chemical space. Although not shown, a flatter CMF also entails a larger number of massive clusters and hence a clumpier chemical space, echoing the results of Bland-Hawthorn et al (2010a), Bland-Hawthorn & Freeman (2014). The effect of the CMF on the distribution of deviations could potentially be exploited to reconstruct the CMF (and the physical processes that the CMF depends on, such as the SFH) from observational samples.…”

Section: Finding and Counting Groups In Chemical Spacesupporting

confidence: 57%

Prospects for Chemically Tagging Stars in the Galaxy

Ting

Conroy

Goodman

2015

ApJ

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It is now well-established that the elemental abundance patterns of stars hold key clues not only to their formation, but also to the assembly histories of galaxies. One of the most exciting possibilities is the use of stellar abundance patterns as "chemical tags" to identify stars that were born in the same molecular cloud. In this paper, we assess the prospects of chemical tagging as a function of several key underlying parameters. We show that in the fiducial case of 10 4 distinct cells in chemical space and 10 10 5 6 stars in the survey, one can expect to detect 10 10 2 3 groups that are 5s ⩾ overdensities in the chemical space. However, we find that even very large overdensities in chemical space do not guarantee that the overdensity is due to a single set of stars from a common birth cloud. In fact, for our fiducial model parameters, the typical 5s overdensity is comprised of stars from a wide range of clusters with the most dominant cluster contributing only 25% of the stars. The most important factors limiting the identification of disrupted clusters via chemical tagging are the number of chemical cells in the chemical space and the survey sampling rate of the underlying stellar population. Both of these factors can be improved through strategic observational plans. While recovering individual clusters through chemical tagging may prove challenging, we show, in agreement with previous work, that different CMFs imprint different degrees of clumpiness in chemical space. These differences provide the opportunity to statistically reconstruct the slope and high-mass cutoff of CMF and its evolution through cosmic time.

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Section: Finding and Counting Groups In Chemical Spacesupporting

confidence: 57%

Prospects for Chemically Tagging Stars in the Galaxy

Ting

Conroy

Goodman

2015

ApJ

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“…The key questions are what caused the specific change in isotopic composition of the infalling molecular cloud material and over what time period could these changes occur? It was thought that molecular clouds in star forming regions were chemically homoge-neous because star clusters (which formed from large molecular clouds) are homogeneous (e.g., Klessen 2011;Bland-Hawthorn and Freeman 2014). It has also been proposed, how-ever, that chemical heterogeneities (e.g., carbon monoxide and water) may persist between the pre-stellar core, the protostar, and circumstellar disk (Visser et al 2009).…”

Section: Implications Of the Nc-cc Dichotomy On Disk Evolution Modelsmentioning

confidence: 99%

The NC-CC Isotope Dichotomy: Implications for the Chemical and Isotopic Evolution of the Early Solar System

et al. 2020

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Understanding the formation of our planetary system requires identification of the materials from which it originated and the accretion processes that produced the planets. The compositional evolution of the solar system can be constrained by synthesizing astronomical datasets and numerical models with elemental and isotopic compositions from objects that directly sampled the disk: meteorites and their constituents (chondrules, refractory inclusions, and matrix). This contribution reviews constraints on early solar system evolution provided by the so-called non-carbonaceous (NC) and carbonaceous chondrite (CC) groups and their relationship to the volatile element characteristics of chondritic meteorites. In previous work, the NC or CC character of a parent body was used to infer its accretion location in the protoplanetary disk. The NC groups purportedly originated in the inner disk, and the CC groups were derived from the outer disk, where the NC and CC regions of the disk may have been separated early on by proto-Jupiter, a pressure maximum, or a dust trap in the disk. The tenet that all CC parent bodies accreted in the outer disk is, in part, based on evidence that a handful of CC meteorites are enriched in volatile species compared to NC meteorites. Here, it is reviewed if and how the volatile element and nucleosynthetic isotope compositions of meteorites can be linked to accretion locations within the disk. The nucleosynthetic isotope compositions of whole rock meteorite samples contrast the trends found for their major volatile element compositions (i.e., C, N, and O). Although there may be an increase in volatile abundances when comparing some stony NC and CC meteorites and their inferred accretion locations within the disk, this is not necessarily a general rule. The difficulties with inferring parent body accretion locations are discussed. It is found that it cannot always be assumed that parent bodies which formed in the CC reservoir are "volatile-rich" relative to those that formed in the NC reservoir which are "volatilepoor". Consequently, tracing the origin of terrestrial volatiles using the NC-CC isotope dichotomy remains challenging.

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“…Numerous dating methods have been developed based on different physical processes and models. Nuclear cosmochronology (Hoyle & Fowler 1960;Bland-Hawthorn & Freeman 2014), isochrone fitting (first discovered by Schaltenbrand 1974;Luri et al 1992;Valls-Gabaud 2014), asteroseismology techniques (Pesnell 1987;Guzik et al 2000), and more indirect chemical proxies of stellar age have been used and applied to very different samples of stars. In particular, for Galactic Archaeology studies, dating techniques applicable to large numbers of objects are crucial.…”

Section: Introductionmentioning

confidence: 99%

The AMBRE Project: [Y/Mg] stellar dating calibration with Gaia

Titarenko

Recio–Blanco

Laverny

et al. 2019

A&A

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Chemical abundance dating methods open new paths for temporal evolution studies of the Milky Way stellar populations. In this paper, we use a high spectral resolution database of turn-off stars in the solar neighbourhood to study the age dependence of the [Y/Mg] chemical abundance ratio. Our analysis reveals a clear correlation between [Y/Mg] and age for thin disc stars of different metallicities, in synergy with previous studies of solar-type stars. In addition, no metallicity dependence with stellar age is detected, allowing us to use the [Y/Mg] ratio as a reliable age proxy. Finally, the [Y/Mg]–age relation presents a discontinuity between thin and thick disc stars around 9–10 Gyr. For thick disc stars, the correlation has a different zero point and probably a steeper trend with age, reflecting the different chemical evolution histories of the two disc components.

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The Origin of the Galaxy and Local Group

Cited by 10 publications

References 276 publications

Prospects for Chemically Tagging Stars in the Galaxy

Prospects for Chemically Tagging Stars in the Galaxy

The NC-CC Isotope Dichotomy: Implications for the Chemical and Isotopic Evolution of the Early Solar System

The AMBRE Project: [Y/Mg] stellar dating calibration with Gaia

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