WFRF:(Persson Magnus V. 1983)
Sökning: WFRF:(Persson Magnus V. 1983) > (2022) > The First Interfero...
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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 03485naa a2200397 4500 | |
| 001 | oai:research.chalmers.se:fb0ae754-5fae-452a-ba3e-b33952a10058 | |
| 003 | SwePub | |
| 008 | 230101s2022 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://research.chalmers.se/publication/5339292 URI |
| 024 | 7 | a https://doi.org/10.3847/1538-4357/ac9ea52 DOI |
| 040 | a (SwePub)cth | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a art2 swepub-publicationtype |
| 072 | 7 | a ref2 swepub-contenttype |
| 100 | 1 | a Yamato, Yoshihideu University of Tokyo, Japan4 aut |
| 245 | 1 0 | a The First Interferometric Measurements of NH 2 D/NH 3 Ratio in Hot Corinos |
| 264 | c 2022-12-13 | |
| 264 | 1 | b American Astronomical Society,c 2022 |
| 338 | a electronic2 rdacarrier | |
| 520 | a 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 (≳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 ∼1017-1018 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 ∼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 N2 and NH3. The implications on the physical properties of IRAS4A’s cores are discussed as well. | |
| 650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
| 650 | 7 | a NATURVETENSKAPx Fysikx Atom- och molekylfysik och optik0 (SwePub)103022 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Atom and Molecular Physics and Optics0 (SwePub)103022 hsv//eng |
| 700 | 1 | a Furuya, Kenjiu National Astronomical Observatory of Japan4 aut |
| 700 | 1 | a Aikawa, Y.u University of Tokyo, Japan4 aut |
| 700 | 1 | a Persson, Magnus V.,d 1983u Chalmers tekniska högskola,Chalmers University of Technology4 aut0 (Swepub:cth)magnpe |
| 700 | 1 | a Tobin, J. J.u National Radio Astronomy Observatory4 aut |
| 700 | 1 | a Jorgensen, J. K.u Niels Bohr Institute4 aut |
| 700 | 1 | a Kama, M.u University College London (UCL),Tartu Ülikool,University of Tartu4 aut |
| 710 | 2 | a University of Tokyo, Japanb National Astronomical Observatory of Japan4 org |
| 773 | 0 | t Astrophysical Journald : American Astronomical Societyg 941:1q 941:1x 1538-4357x 0004-637X |
| 856 | 4 | u https://research.chalmers.se/publication/533929/file/533929_Fulltext.pdfx primaryx freey FULLTEXT |
| 856 | 4 8 | u https://research.chalmers.se/publication/533929 |
| 856 | 4 8 | u https://doi.org/10.3847/1538-4357/ac9ea5 |
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