Diverse Nuclear Star-forming Activities in the Heart of NGC 253 Resolved with 10-pc-scale ALMA Images

We present an 8 pc × 5 pc resolution view of the central ∼200 pc region of the nearby starburst galaxy NGC 253, based on ALMA Band 7 ( or GHz) observations covering 11 GHz. We resolve the nuclear starburst of NGC 253 into eight dusty star-forming clumps, 10 pc in scale, for the first time. These clu...

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Bibliographic Details
Published in:The Astrophysical journal 2017-11, Vol.849 (2), p.81
Main Authors: Ando, Ryo, Nakanishi, Kouichiro, Kohno, Kotaro, Izumi, Takuma, Martín, Sergio, Harada, Nanase, Takano, Shuro, Kuno, Nario, Nakai, Naomasa, Sugai, Hajime, Sorai, Kazuo, Tosaki, Tomoka, Matsubayashi, Kazuya, Nakajima, Taku, Nishimura, Yuri, Tamura, Yoichi
Format: Article
Language:English
Subjects:
Astrophysics
Clumps
Dust
Emission lines
Emission spectra
Galaxies
galaxies: individual (NGC 253)
galaxies: ISM
galaxies: star formation
galaxies: starburst
Hydrogen
Hydrogen recombinations
Line spectra
Molecular gases
Organic chemistry
Star formation
Starburst galaxies
Stars & galaxies
submillimeter: galaxies
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Summary:We present an 8 pc × 5 pc resolution view of the central ∼200 pc region of the nearby starburst galaxy NGC 253, based on ALMA Band 7 ( or GHz) observations covering 11 GHz. We resolve the nuclear starburst of NGC 253 into eight dusty star-forming clumps, 10 pc in scale, for the first time. These clumps, each of which contains (4-10) of dust (assuming that the dust temperature is 25 K) and up to massive (O5V) stars, appear to be aligned in two parallel ridges, while they have been blended in previous studies. Despite the similarities in sizes and dust masses of these clumps, their line spectra vary drastically from clump to clump, although they are separated by only ∼10 pc. Specifically, one of the clumps, Clump 1, exhibits line-confusion-limited spectra with at least 36 emission lines from 19 molecules (including CH3OH, HNCO, H2CO, CH3CCH, H2CS, and H3O+) and a hydrogen recombination line (H26 ), while far fewer kinds of molecular lines are detected in some other clumps where fragile species, such as complex organic molecules and HNCO, completely disappear from their spectra. We demonstrate the existence of hot molecular gas ( K) in the former clump, which suggests that the hot and chemically rich environments are localized within a 10-pc-scale star-forming clump.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aa8fd4