ORCID Profile
0000-0002-5809-4834
Current Organisation
University of Helsinki
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Publisher: EDP Sciences
Date: 02-2013
Publisher: Oxford University Press (OUP)
Date: 06-06-2020
Abstract: The ATOMS, standing for ALMA Three-millimeter Observations of Massive Star-forming regions, survey has observed 146 active star-forming regions with ALMA band 3, aiming to systematically investigate the spatial distribution of various dense gas tracers in a large s le of Galactic massive clumps, to study the roles of stellar feedback in star formation, and to characterize filamentary structures inside massive clumps. In this work, the observations, data analysis, and ex le science of the ATOMS survey are presented, using a case study for the G9.62+0.19 complex. Toward this source, some transitions, commonly assumed to trace dense gas, including CS J = 2−1, HCO+J = 1−0, and HCN J = 1−0, are found to show extended gas emission in low-density regions within the clump less than 25 per cent of their emission is from dense cores. SO, CH3OH, H13CN, and HC3N show similar morphologies in their spatial distributions and reveal well the dense cores. Widespread narrow SiO emission is present (over ∼1 pc), which may be caused by slow shocks from large–scale colliding flows or H ii regions. Stellar feedback from an expanding H ii region has greatly reshaped the natal clump, significantly changed the spatial distribution of gas, and may also account for the sequential high-mass star formation in the G9.62+0.19 complex. The ATOMS survey data can be jointly analysed with other survey data, e.g. MALT90, Orion B, EMPIRE, ALMA_IMF, and ALMAGAL, to deepen our understandings of ‘dense gas’ star formation scaling relations and massive protocluster formation.
Publisher: EDP Sciences
Date: 06-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: American Astronomical Society
Date: 14-01-2016
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: American Astronomical Society
Date: 19-01-2021
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: Oxford University Press (OUP)
Date: 06-06-2020
Abstract: We report studies of the relationships between the total bolometric luminosity (Lbol or LTIR) and the molecular line luminosities of J = 1 − 0 transitions of H13CN, H13CO+, HCN, and HCO+ with data obtained from ACA observations in the ‘ATOMS’ survey of 146 active Galactic star-forming regions. The correlations between Lbol and molecular line luminosities $L^{\\prime }_{\\rm mol}$ of the four transitions all appear to be approximately linear. Line emission of isotopologues shows as large scatters in Lbol–$L^{\\prime }_{\\rm mol}$ relations as their main line emission. The log(Lbol/$L^{\\prime }_{\\rm mol}$) for different molecular line tracers have similar distributions. The Lbol-to-$L^{\\prime }_{\\rm mol}$ ratios do not change with galactocentric distances (RGC) and clump masses (Mclump). The molecular line luminosity ratios (HCN-to-HCO+, H13CN-to-H13CO+, HCN-to-H13CN, and HCO+-to-H13CO+) all appear constant against Lbol, dust temperature (Td), Mclump, and RGC. Our studies suggest that both the main lines and isotopologue lines are good tracers of the total masses of dense gas in Galactic molecular clumps. The large optical depths of main lines do not affect the interpretation of the slopes in star formation relations. We find that the mean star formation efficiency (SFE) of massive Galactic clumps in the ‘ATOMS’ survey is reasonably consistent with other measures of the SFE for dense gas, even those using very different tracers or examining very different spatial scales.
Publisher: American Astronomical Society
Date: 22-09-2016
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 30-09-2015
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 28-08-2013
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 04-2015
Publisher: EDP Sciences
Date: 11-2201
Publisher: EDP Sciences
Date: 04-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 29-10-2014
Publisher: EDP Sciences
Date: 04-2015
Publisher: American Astronomical Society
Date: 06-02-2017
No related grants have been discovered for Mika Juvela.