The SEDIGISM survey: The influence of spiral arms on the molecular gas distribution of the inner Milky Way

Colombo, D.; Duarte-Cabral, A.; Pettitt, Alex R.; Urquhart, J. S.; Wyrowski, F.; Csengeri, T.; Neralwar, K. R.; Schüller, F.; Menten, K. M.; Barnes, Peter J.; Beuther, H.; Bronfman, L.; Eden, David; Ginsburg, Adam; Henning, Th.; König, C.; Lee, M.-Y.; Mattern, M.; Medina, S.; Ragan, S. E.; Rigby, Andrew; Sánchez-Monge, Á.; Traficante, A.; Yang, A. Y.; Wienen, M.

doi:10.1051/0004-6361/202141287

Cited by 13 publications

(2 citation statements)

References 130 publications

(158 reference statements)

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“…Pillai et al 2011;Sanhueza et al 2013). Additionally, several surveys like SEDIGISM (Schuller et al 2017;Yu et al 2019;Yang et al 2021;Colombo et al 2022), GLOSTAR (Nguyen et al 2021) are also aimed towards addressing various aspects of the formation mechanism and early evolutionary phases of high-mass stars.…”

Section: Introductionmentioning

confidence: 99%

ATOMS: ALMA three-millimeter observations of massive star-forming regions – XII: Fragmentation and multiscale gas kinematics in protoclusters G12.42+0.50 and G19.88−0.53

Saha

Tej

Liu

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present new continuum and molecular line data from the ALMA Three-millimeter Observations of Massive Star-forming regions (ATOMS) survey for the two protoclusters, G12.42+0.50 and G19.88-0.53. The 3 mm continuum maps reveal seven cores in each of the two globally contracting protoclusters. These cores satisfy the radius-mass relation and the surface mass density criteria for high-mass star formation. Similar to their natal clumps, the virial analysis of the cores suggests that they are undergoing gravitational collapse ($\rm \alpha _{vir} << 2$). The clump to core scale fragmentation is investigated and the derived core masses and separations are found to be consistent with thermal Jeans fragmentation. We detect large-scale filamentary structures with velocity gradients and multiple outflows in both regions. Dendrogram analysis of the H13CO+ map identifies several branch and leaf structures with sizes ∼ 0.1 and 0.03 pc, respectively. The supersonic gas motion displayed by the branch structures is in agreement with the Larson power-law indicating that the gas kinematics at this spatial scale is driven by turbulence. The transition to transonic/subsonic gas motion is seen to occur at spatial scales of ∼0.1 pc indicating the dissipation of turbulence. In agreement with this, the leaf structures reveal gas motions that deviate from the slope of Larson’s law. From the large-scale converging filaments to the collapsing cores, the gas dynamics in G12.42+0.50 and G19.88-0.53 show scale-dependent dominance of turbulence and gravity and the combination of these two driving mechanisms needs to be invoked to explain massive star formation in the protoclusters.

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Section: Introductionmentioning

confidence: 99%

ATOMS: ALMA three-millimeter observations of massive star-forming regions – XII: Fragmentation and multiscale gas kinematics in protoclusters G12.42+0.50 and G19.88−0.53

Saha

Tej

Liu

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…Recently, Querejeta et al (2021) show that spiral arms accumulate gas and star formation, without systematically increasing the SFE. Unlike the case of M51 (Colombo et al 2014), the GMC properties change slightly but not significantly between arms and inter-arms in non-interacting galaxies (Rosolowsky et al 2021;Colombo et al 2022). Although the spiral arms of our Galaxy seems have little or no effect on the enhancement of SFE (Eden et al 2015;Ragan et al 2016;Urquhart et al 2021), the evidence supporting the arms influencing the dense gas distribution or kinematics have been reported (Sakai et al 2015;Urquhart et al 2021).…”

Section: Spiral-driven Gas Inflowmentioning

confidence: 66%

The EDGE-CALIFA survey: The role of spiral arms and bars in driving central molecular gas concentrations

Kalinova

Colombo

et al. 2022

A&A

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Shocks and torques produced by non-axisymmetric structures such as spiral arms and bars may transport gas to galaxy central regions. We test this hypothesis by studying the dependence of concentration of CO luminosity (C CO ), molecular gas (C mol ), and star formation rate (C SFR ) in central ∼ 2 kpc on the strength of non-axisymmetric disk structure using a sample of 57 disk galaxies selected from the EDGE-CALIFA survey. C mol is calculated using a CO-to-H 2 conversion factor that decreases with higher metallicity and higher stellar surface density. We find that C mol is systematically 0.22 dex lower than C CO . We confirm that high C mol and strong non-axisymmetric disk structure are more common in barred galaxies than in unbarred galaxies. However, we find that spiral arms also increase C mol . We show that there is a good correlation between C mol and the strength of non-axisymmetric structure (which can be due to a bar, spiral arms, or both). This suggests that the stronger the bars and spirals, the more efficient the galaxy is at transporting cold gas to its center. Despite the small subsample size, C mol of the four Seyferts are not significantly reduced compared to inactive galaxies of similar disk structure, implying that the AGN feedback in Seyferts may not notably affect the molecular gas distribution in the central ∼ 2 kpc. We find that C SFR tightly correlates with C mol in both unbarred and barred galaxies. Likewise, elevated C SFR is found in galaxies with strong disk structure. Our results suggest that the disk structure, either spirals or bars, can transport gas to the central regions, with higher inflow rates corresponding to stronger structure, and consequently boost central star formation. Both spirals and bars play, therefore, an essential role in the secular evolution of disk galaxies.

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The SEDIGISM survey: A search for molecular outflows

Yang

Urquhart

Wyrowski

et al. 2022

A&A

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Context. The formation processes of massive stars are still unclear but a picture is emerging involving accretion disks and molecular outflows in what appears to be a scaled-up version of low-mass star formation. A census of outflow activity towards high-mass star-forming clumps in various evolutionary stages has the potential to shed light on high-mass star formation. Aims. We conducted an outflow survey towards ATLASGAL (APEX Telescope Large Area Survey of the Galaxy) clumps, using SEDIGISM (structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium) data and aimed to obtain a large sample of clumps exhibiting outflow activity in different evolutionary stages. Methods. We identify the high-velocity wings of the 13 CO lines, indicating outflow activity, toward ATLASGAL clumps by (1) extracting the simultaneously observed 13 CO (2 -1) and C 18 O (2 -1) spectra from SEDIGISM, and (2) subtracting Gaussian fits to the scaled C 18 O (core emission) from the 13 CO line after considering opacity broadening. Results. We have detected high-velocity gas towards 1192 clumps out of a total sample of 2052 corresponding to an overall detection rate of 58%. Outflow activity has been detected in the earliest (apparently) quiescent clumps (i.e., 70µm weak), to the most evolved H ii region stages i.e., 8µm bright with tracers of massive star formation. The detection rate increases as a function of evolution (quiescent=51%, protostellar=47%, YSO = 57%, UC H ii regions = 76%). Conclusions. Our sample is the largest outflow sample identified so far. The high-detection rate from this large sample is consistent with the results of similar studies reported in the literature and supports the scenario that outflows are a ubiquitous feature of highmass star formation. The lower detection rate in early evolutionary stages may be due to the fact that outflows in the early stages are weak and difficult to detect. We obtain a statistically significant sample of outflow clumps for every evolutionary stage, especially for outflow clumps in the earliest stage (i.e., 70 µm dark). The detections of outflows in the 70 µm-dark clumps suggest that the absence of 70 µm emission is not a robust indicator of starless/pre-stellar cores.

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The SEDIGISM survey: The influence of spiral arms on the molecular gas distribution of the inner Milky Way

Abstract: The version in the Kent Academic Repository may differ from the final published version. Users are advised to check http://kar.kent.ac.uk for the status of the paper. Users should always cite the published version of record.

Cited by 13 publications

References 130 publications

ATOMS: ALMA three-millimeter observations of massive star-forming regions – XII: Fragmentation and multiscale gas kinematics in protoclusters G12.42+0.50 and G19.88−0.53

ATOMS: ALMA three-millimeter observations of massive star-forming regions – XII: Fragmentation and multiscale gas kinematics in protoclusters G12.42+0.50 and G19.88−0.53

The EDGE-CALIFA survey: The role of spiral arms and bars in driving central molecular gas concentrations

The SEDIGISM survey: A search for molecular outflows

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