Tetrahedral hydrocarbon nanoparticles in space: X-ray spectra

Bilalbegović, Goranka; Maksimović, Aleksandar; Valencic, Lynne

doi:10.1093/mnras/sty607

Cited by 8 publications

(7 citation statements)

References 98 publications

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“…Finally, under special condition of high pressure, for instance in a shocked environment, graphite and amorphous carbon can turn into nano-diamonds, which can constitute as much as 5% of the amount of C in the ISM (Tielens et al 1987), possibly with H and N inclusion (Van Kerckhoven et al 2002;Bilalbegović et al 2018). Diamonds of possible ISM origin have been found in meteorites (Lewis et al 1987).…”

Section: Elements In This Studymentioning

confidence: 99%

X-ray extinction from interstellar dust

Costantini

Zeegers

Rogantini

et al. 2019

A&A

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Aims. We present a study on the prospects of observing carbon, sulfur, and other lower abundance elements (namely Al, Ca, Ti, and Ni) present in the interstellar medium using future X-ray instruments. We focus in particular on the detection and characterization of interstellar dust along the lines of sight. Methods. We compared the simulated data with different sets of dust aggregates, either obtained from past literature or measured by us using the SOLEIL-LUCIA synchrotron beamline. Extinction by interstellar grains induces modulations of a given photolelectric edge, which can be in principle traced back to the chemistry of the absorbing grains. We simulated data of instruments with characteristics of resolution and sensitivity of the current Athena, XRISM, and Arcus concepts. Results. In the relatively near future, the depletion and abundances of the elements under study will be determined with confidence. In the case of carbon and sulfur, the characterization of the chemistry of the absorbing dust will be also determined, depending on the dominant compound. For aluminum and calcium, despite the large depletion in the interstellar medium and the prominent dust absorption, in many cases the edge feature may not be changing significantly with the change of chemistry in the Al- or Ca-bearing compounds. The exinction signature of large grains may be detected and modeled, allowing a test on different grain size distributions for these elements. The low cosmic abundance of Ti and Ni will not allow us a detailed study of the edge features.

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Section: Elements In This Studymentioning

confidence: 99%

X-ray extinction from interstellar dust

Costantini

Zeegers

Rogantini

et al. 2019

A&A

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show abstract

“…Finally, under special condition of high pressure, for instance in a shocked environment, graphite and amorphous carbon can turn into nano-diamonds, which can constitute as much as 5% of the amount of C in the ISM (Tielens et al 1987), possibly with H andN inclusion (Van Kerckhoven et al 2002;Bilalbegović et al 2018). Diamonds of possible ISM origin have been found in meteorites (Lewis et al 1987).…”

Section: The Elements In This Studymentioning

confidence: 99%

X-ray extinction from interstellar dust: Prospects of observing carbon, sulfur and other trace elements

Costantini,

Zeegers,

Rogantini

et al. 2019

Preprint

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Aims. We present a study on the prospects of observing carbon, sulfur, and other lower abundance elements (namely Al, Ca, Ti and Ni) present in the interstellar medium using future X-ray instruments. We focus in particular on the detection and characterization of interstellar dust along the lines of sight. Methods. We compare the simulated data with different sets of dust aggregates, either obtained from past literature or measured by us using the SOLEIL-LUCIA synchrotron beamline. Extinction by interstellar grains induces modulations of a given photolelectric edge, which can be in principle traced back to the chemistry of the absorbing grains. We simulated data of instruments with characteristics of resolution and sensitivity of the current Athena, XRISM and Arcus concepts. Results. In the relatively near future, the depletion and abundances of the elements under study will be determined with confidence. In the case of carbon and sulfur, the characterization of the chemistry of the absorbing dust will be also determined, depending on the dominant compound. For aluminum and calcium, despite the large depletion in the interstellar medium and the prominent dust absorption, in many cases the edge feature may not be changing significantly with the change of chemistry in the Al-or Ca-bearing compounds. The exinction signature of large grains may be detected and modeled, allowing a test on different grain size distributions for these elements. The low cosmic abundance of Ti and Ni will not allow us a detailed study of the edge features.

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“…Nowadays, accurate extinction cross-sections of several interstellar dust analogues are available. It is possible to characterise the XAFS for multiple photoelectric K-shells: in particular the K edges of carbon (Bilalbegović et al 2018;Costantini et al 2019), oxygen (Costantini et al 2012;Psaradaki et al;in prep. ), magnesium (Rogantini et al 2019), silicon (Zeegers et al 2017(Zeegers et al , 2019, iron (Lee & Ravel 2005;Rogantini et al 2018), aluminium, sulfur, and other low abundant elements (Costantini et al 2019), plus the L-edges of iron (Lee et al 2009;Westphal et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Magnesium and silicon in interstellar dust: X-ray overview

Rogantini

Costantini

Zeegers

et al. 2020

A&A

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Context. The dense Galactic environment is a large reservoir of interstellar dust. Therefore, this region represents a perfect laboratory to study the properties of cosmic dust grains. X-rays are the most direct way to detect the interaction of light with dust present in these dense environments. Aims. The interaction between the radiation and the interstellar matter imprints specific absorption features on the X-ray spectrum. We study them with the aim of defining the chemical composition, the crystallinity, and structure of the dust grains that populate the inner regions of the Galaxy. Methods. We investigated the magnesium and the silicon K-edges detected in the Chandra /HETG spectra of eight bright X-ray binaries, distributed in the neighbourhood of the Galactic centre. We modelled the two spectral features using accurate extinction cross-sections of silicates, which we measured at the synchrotron facility Soleil, France. Results. Near the Galactic centre, magnesium and silicon show abundances similar to the solar ones and they are highly depleted from the gas phase (δMg > 0.90 and δSi > 0.96). We find that amorphous olivine with a composition of MgFeSiO4 is the most representative compound along all lines of sight according to our fits. The contribution of Mg-rich silicates and quartz is low (less than 10%). On average we observe a percentage of crystalline dust equal to 11%. For the extragalactic source LMC X-1, we find a preference for forsterite, a magnesium-rich olivine. Along this line of sight we also observe an under-abundance of silicon ASi∕ALMC = 0.5 ± 0.2.

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Tetrahedral hydrocarbon nanoparticles in space: X-ray spectra

Cited by 8 publications

References 98 publications

X-ray extinction from interstellar dust

X-ray extinction from interstellar dust

X-ray extinction from interstellar dust: Prospects of observing carbon, sulfur and other trace elements

Magnesium and silicon in interstellar dust: X-ray overview

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