Self-consistent grain depletions and abundances I: the Orion Nebula as a test case

Chamani M. Gunasekera; Xihan Ji; Marios Chatzikos; Renbin Yan; Gary Ferland

doi:10.1093/mnras/stac022

Self-consistent grain depletions and abundances I: the Orion Nebula as a test case

Chamani M. Gunasekera
, Xihan Ji
, Marios Chatzikos
, Renbin Yan
, Gary Ferland

Research output: Contribution to journal › Article › peer-review

9 Scopus citations

Abstract

Atomic species in the interstellar medium transition out of their gas phase mainly by depletion on to dust. In this study, we examine if there is any change to the spectral-line ratio predictions from a photoionization model of the Orion H ii region when the degree of dust depletions is altered according to the most recently published model. We use equations and parameters published by previous works, in order to streamline the calculation of depleted abundances within cloudy. Our aim is for cloudy users to be able to vary the level of depletion using a single parameter in the input file. This makes it possible to explore predictions for a large range of depletions more efficiently. Finally, we discuss the results obtained for a model of the Orion Nebula when the degree of depletions are manipulated in this way. We found that the intensity of line ratios are significantly affected by depletions on to dust grains. Further, we found that adjusting dust abundances along with depletion affects the structure and the overall temperature of the H+ layer across the H ii region.

Original language	English
Pages (from-to)	2310-2317
Number of pages	8
Journal	Monthly Notices of the Royal Astronomical Society
Volume	512
Issue number	2
DOIs	https://doi.org/10.1093/mnras/stac022
State	Published - May 1 2022

Bibliographical note

Publisher Copyright:
© 2022 The Author(s).

Funding

We thank all the people that have made this paper possible. This includes but not limited to the published work of Hensley & Draine ( 2021 ). CMG was supported by Space Telescope Science Institute (STScI, HST-AR-15018 and HST-GO-16196.003-A). MC acknowledges support by National Science Foundation (NSF, 1910687), National Aeronautics and Space Administration (NASA, 19-ATP19-0188), and STScI (HST-AR-14556.001-A). GF acknowledges support by NSF (1816537, 1910687), NASA (A TP 17-A TP17-0141, 19-ATP19-0188), and STScI (HST-AR-15018 and HST-GO-16196.003-A).

Funders	Funder number
National Aeronautics and Space Administration	1816537, HST-AR-14556.001-A, A TP 17-A TP17-0141, 19-ATP19-0188
Space Telescope Science Institute	HST-AR-15018, HST-GO-16196.003-A
U.S. Department of Energy Chinese Academy of Sciences Guangzhou Municipal Science and Technology Project Oak Ridge National Laboratory Extreme Science and Engineering Discovery Environment National Science Foundation National Energy Research Scientific Computing Center National Natural Science Foundation of China	1910687

Keywords

H ii regions
ISM: abundances
ISM: atoms
dust, extinction
ultraviolet: ISM

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/mnras/stac022

Cite this

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title = "Self-consistent grain depletions and abundances I: the Orion Nebula as a test case",

abstract = "Atomic species in the interstellar medium transition out of their gas phase mainly by depletion on to dust. In this study, we examine if there is any change to the spectral-line ratio predictions from a photoionization model of the Orion H ii region when the degree of dust depletions is altered according to the most recently published model. We use equations and parameters published by previous works, in order to streamline the calculation of depleted abundances within cloudy. Our aim is for cloudy users to be able to vary the level of depletion using a single parameter in the input file. This makes it possible to explore predictions for a large range of depletions more efficiently. Finally, we discuss the results obtained for a model of the Orion Nebula when the degree of depletions are manipulated in this way. We found that the intensity of line ratios are significantly affected by depletions on to dust grains. Further, we found that adjusting dust abundances along with depletion affects the structure and the overall temperature of the H+ layer across the H ii region.",

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author = "Gunasekera, \{Chamani M.\} and Xihan Ji and Marios Chatzikos and Renbin Yan and Gary Ferland",

note = "Publisher Copyright: {\textcopyright} 2022 The Author(s).",

year = "2022",

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T1 - Self-consistent grain depletions and abundances I

T2 - the Orion Nebula as a test case

AU - Gunasekera, Chamani M.

AU - Ji, Xihan

AU - Chatzikos, Marios

AU - Yan, Renbin

AU - Ferland, Gary

PY - 2022/5/1

Y1 - 2022/5/1

N2 - Atomic species in the interstellar medium transition out of their gas phase mainly by depletion on to dust. In this study, we examine if there is any change to the spectral-line ratio predictions from a photoionization model of the Orion H ii region when the degree of dust depletions is altered according to the most recently published model. We use equations and parameters published by previous works, in order to streamline the calculation of depleted abundances within cloudy. Our aim is for cloudy users to be able to vary the level of depletion using a single parameter in the input file. This makes it possible to explore predictions for a large range of depletions more efficiently. Finally, we discuss the results obtained for a model of the Orion Nebula when the degree of depletions are manipulated in this way. We found that the intensity of line ratios are significantly affected by depletions on to dust grains. Further, we found that adjusting dust abundances along with depletion affects the structure and the overall temperature of the H+ layer across the H ii region.

AB - Atomic species in the interstellar medium transition out of their gas phase mainly by depletion on to dust. In this study, we examine if there is any change to the spectral-line ratio predictions from a photoionization model of the Orion H ii region when the degree of dust depletions is altered according to the most recently published model. We use equations and parameters published by previous works, in order to streamline the calculation of depleted abundances within cloudy. Our aim is for cloudy users to be able to vary the level of depletion using a single parameter in the input file. This makes it possible to explore predictions for a large range of depletions more efficiently. Finally, we discuss the results obtained for a model of the Orion Nebula when the degree of depletions are manipulated in this way. We found that the intensity of line ratios are significantly affected by depletions on to dust grains. Further, we found that adjusting dust abundances along with depletion affects the structure and the overall temperature of the H+ layer across the H ii region.

KW - H ii regions

KW - ISM: abundances

KW - ISM: atoms

KW - dust, extinction

KW - ultraviolet: ISM

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JF - Monthly Notices of the Royal Astronomical Society

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Self-consistent grain depletions and abundances I: the Orion Nebula as a test case

Abstract

Bibliographical note

Funding

Keywords

ASJC Scopus subject areas

Access to Document

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