The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos

Research output: Contribution to journal › Journal article › Research › peer-review

Standard

The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos. / Yamato, Yoshihide; Furuya, Kenji; Aikawa, Yuri; Persson, Magnus V.; Tobin, John J.; Jorgensen, Jes K.; Kama, Mihkel.

In: Astrophysical Journal, Vol. 941, No. 1, 75, 01.12.2022.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Yamato, Y, Furuya, K, Aikawa, Y, Persson, MV, Tobin, JJ, Jorgensen, JK & Kama, M 2022, 'The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos', Astrophysical Journal, vol. 941, no. 1, 75. https://doi.org/10.3847/1538-4357/ac9ea5

APA

Yamato, Y., Furuya, K., Aikawa, Y., Persson, M. V., Tobin, J. J., Jorgensen, J. K., & Kama, M. (2022). The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos. Astrophysical Journal, 941(1), [75]. https://doi.org/10.3847/1538-4357/ac9ea5

Vancouver

Yamato Y, Furuya K, Aikawa Y, Persson MV, Tobin JJ, Jorgensen JK et al. The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos. Astrophysical Journal. 2022 Dec 1;941(1). 75. https://doi.org/10.3847/1538-4357/ac9ea5

Author

Yamato, Yoshihide ; Furuya, Kenji ; Aikawa, Yuri ; Persson, Magnus V. ; Tobin, John J. ; Jorgensen, Jes K. ; Kama, Mihkel. / The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos. In: Astrophysical Journal. 2022 ; Vol. 941, No. 1.

Bibtex

@article{139f097c64844f95bb0a4ad21896e629,
title = "The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos",
abstract = "The chemical evolution of nitrogen during star and planet formation is still not fully understood. Ammonia (NH3) is a key specie in the understanding of the molecular evolution in star-forming clouds and nitrogen isotope fractionation. In this paper, we present high-spatial-resolution observations of multiple emission lines of NH3 toward the protobinary system NGC1333 IRAS4A with the Karl G. Jansky Very Large Array. We spatially resolved the binary (hereafter, 4A1 and 4A2) and detected compact emission of NH3 transitions with high excitation energies (greater than or similar to 100 K) from the vicinity of the protostars, indicating the NH3 ice has sublimated at the inner hot region. The NH3 column density is estimated to be similar to 10(17)-10(18) cm(-2). We also detected two NH2D transitions, allowing us to constrain the deuterium fractionation of ammonia. The NH2D/NH3 ratios are as high as similar to 0.3-1 in both 4A1 and 4A2. From comparisons with the astrochemical models in the literature, the high NH2D/NH3 ratios suggest that the formation of NH3 ices mainly started in the prestellar phase after the formation of bulk water ice finished, and that the primary nitrogen reservoir in the star-forming cloud could be atomic nitrogen (or N atoms) rather than nitrogen-bearing species such as N-2 and NH3. The implications on the physical properties of IRAS4A's cores are discussed as well.",
keywords = "DEUTERATED AMMONIA, HYPERFINE STRUCTURE, INTERSTELLAR ICES, DENSE CORES, SUBMILLIMETER, ABUNDANCE, ROTATION, NITROGEN, NH3, PARAMETERS",
author = "Yoshihide Yamato and Kenji Furuya and Yuri Aikawa and Persson, {Magnus V.} and Tobin, {John J.} and Jorgensen, {Jes K.} and Mihkel Kama",
year = "2022",
month = dec,
day = "1",
doi = "10.3847/1538-4357/ac9ea5",
language = "English",
volume = "941",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing, Inc",
number = "1",

}

RIS

TY - JOUR

T1 - The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos

AU - Yamato, Yoshihide

AU - Furuya, Kenji

AU - Aikawa, Yuri

AU - Persson, Magnus V.

AU - Tobin, John J.

AU - Jorgensen, Jes K.

AU - Kama, Mihkel

PY - 2022/12/1

Y1 - 2022/12/1

N2 - The chemical evolution of nitrogen during star and planet formation is still not fully understood. Ammonia (NH3) is a key specie in the understanding of the molecular evolution in star-forming clouds and nitrogen isotope fractionation. In this paper, we present high-spatial-resolution observations of multiple emission lines of NH3 toward the protobinary system NGC1333 IRAS4A with the Karl G. Jansky Very Large Array. We spatially resolved the binary (hereafter, 4A1 and 4A2) and detected compact emission of NH3 transitions with high excitation energies (greater than or similar to 100 K) from the vicinity of the protostars, indicating the NH3 ice has sublimated at the inner hot region. The NH3 column density is estimated to be similar to 10(17)-10(18) cm(-2). We also detected two NH2D transitions, allowing us to constrain the deuterium fractionation of ammonia. The NH2D/NH3 ratios are as high as similar to 0.3-1 in both 4A1 and 4A2. From comparisons with the astrochemical models in the literature, the high NH2D/NH3 ratios suggest that the formation of NH3 ices mainly started in the prestellar phase after the formation of bulk water ice finished, and that the primary nitrogen reservoir in the star-forming cloud could be atomic nitrogen (or N atoms) rather than nitrogen-bearing species such as N-2 and NH3. The implications on the physical properties of IRAS4A's cores are discussed as well.

AB - The chemical evolution of nitrogen during star and planet formation is still not fully understood. Ammonia (NH3) is a key specie in the understanding of the molecular evolution in star-forming clouds and nitrogen isotope fractionation. In this paper, we present high-spatial-resolution observations of multiple emission lines of NH3 toward the protobinary system NGC1333 IRAS4A with the Karl G. Jansky Very Large Array. We spatially resolved the binary (hereafter, 4A1 and 4A2) and detected compact emission of NH3 transitions with high excitation energies (greater than or similar to 100 K) from the vicinity of the protostars, indicating the NH3 ice has sublimated at the inner hot region. The NH3 column density is estimated to be similar to 10(17)-10(18) cm(-2). We also detected two NH2D transitions, allowing us to constrain the deuterium fractionation of ammonia. The NH2D/NH3 ratios are as high as similar to 0.3-1 in both 4A1 and 4A2. From comparisons with the astrochemical models in the literature, the high NH2D/NH3 ratios suggest that the formation of NH3 ices mainly started in the prestellar phase after the formation of bulk water ice finished, and that the primary nitrogen reservoir in the star-forming cloud could be atomic nitrogen (or N atoms) rather than nitrogen-bearing species such as N-2 and NH3. The implications on the physical properties of IRAS4A's cores are discussed as well.

KW - DEUTERATED AMMONIA

KW - HYPERFINE STRUCTURE

KW - INTERSTELLAR ICES

KW - DENSE CORES

KW - SUBMILLIMETER

KW - ABUNDANCE

KW - ROTATION

KW - NITROGEN

KW - NH3

KW - PARAMETERS

U2 - 10.3847/1538-4357/ac9ea5

DO - 10.3847/1538-4357/ac9ea5

M3 - Journal article

VL - 941

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 75

ER -

ID: 332118936