ATLASGAL-selected massive clumps in the inner Galaxy

Navarete, Felipe; Leurini, S.; Giannetti, A.; Wyrowski, F.; Urquhart, J. S.; König, C.; Csengeri, T.; Güsten, R.; Damineli, A.; Menten, K. M.

doi:10.1051/0004-6361/201629777

Cited by 9 publications

(8 citation statements)

References 50 publications

(68 reference statements)

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“…We follow an analogous procedure to that described in Fernández-López et al (2020) for G5.89-0.39, and we consider local thermodynamic equilibrium and an optically thin CO emission. To derive the column density of the CO(3-2) transition, we use the communication; see also Navarete et al 2019), which are appropriate for many massive clumps in the Milky Way. We estimate the mass in each velocity channel as…”

Section: Outflow Energeticsmentioning

confidence: 99%

Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA

Ccolque

Fernández-López

Zapata

et al. 2022

ApJ

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We present 0.9 mm continuum and CO(3–2) line emission observations retrieved from the Atacama Large Millimeter/submillimeter Array archive toward the high-mass star formation region IRAS 16076-5134. We identify 14 dense cores with masses between 0.3 and 22 M ☉. We find an ensemble of filament-like CO(3–2) ejections from −62 to +83 km s−1 that appear to arise radially from a common central position, close to the dense core MM8. The ensemble of filaments has a quasi-isotropic distribution in the plane of the sky. The radial velocities of several filaments follow a linear velocity gradient, increasing from a common origin. Considering the whole ensemble of filaments, we estimate the total mass to be 138 and 216 M ☉, from its CO emission, for 70 K and 140 K, respectively. Also, assuming a constant velocity expansion for the filaments (of 83 km s−1), we estimate the dynamical age of the outflowing material (3500 yr), its momentum (∼104 M ☉ km s−1), and its kinetic energy (∼1048–49 erg). The morphology and kinematics presented by the filaments suggest the presence of a dispersal outflow with explosive characteristics in IRAS 16076-5134. In addition, we make a raw estimate of the lower limit of the frequency rate of the explosive dispersal outflows in the galaxy (one every 110 yr), considering a constant star formation rate and efficiency, with respect to the galactocentric radius of the galaxy. This may imply a comparable rate between dispersal outflows and supernovae (approximately one every 50 yr), which may be important for the energy budget of the and the link between dispersal outflows and high-mass star formation.

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Section: Outflow Energeticsmentioning

confidence: 99%

Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA

Ccolque

Fernández-López

Zapata

et al. 2022

ApJ

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“…The ATLASGAL CSC has therefore been the focus of an intensive campaign to characterise the properties and evolutionary state of the clumps. These have included dedicated molecular-line studies to produce the kinematics, temperatures, chemistry and determine kinematic distances (Wienen et al 2012;Giannetti et al 2014;Wienen et al 2015;Csengeri et al 2016;Kim et al 2017Kim et al , 2018Wienen et al 2018;Tang et al 2018;Navarete et al 2019;Urquhart et al 2019) and detailed analysis of clumps associated with star-formation tracers such as HII regions (Urquhart et al 2013b), methanol masers (Urquhart et al 2013a(Urquhart et al , 2015Billington et al 2019Billington et al , 2020, massive young stellar objects (MYSO; Urquhart et al 2014b;König et al 2017;Urquhart et al 2018) and filamentary structures (Li et al 2016;Mattern et al 2018;Lin et al 2019). This programme of follow-up observations and use of complementary multi-wavelength studies has resulted in the ATLASGAL sample being the most well characterised sample of high-mass star-forming clumps currently available.…”

Section: Introductionmentioning

confidence: 99%

ATLASGAL – evolutionary trends in high-mass star formation

Urquhart

Wells

Pillai

et al. 2021

Monthly Notices of the Royal Astronomical Society

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ATLASGAL is a 870-μm dust survey of 420 square degrees of the inner Galactic plane and has been used to identify ∼10 000 dense molecular clumps. Dedicated follow-up observations and complementary surveys are used to characterise the physical properties of these clumps, map their Galactic distribution and investigate the evolutionary sequence for high-mass star formation. The analysis of the ATLASGAL data is ongoing: we present an up-to-date version of the catalogue. We have classified 5007 clumps into four evolutionary stages (quiescent, protostellar, young stellar objects and H ii regions) and find similar numbers of clumps in each stage, suggesting a similar lifetime. The luminosity-to-mass (Lbol/Mfwhm) ratio curve shows a smooth distribution with no significant kinks or discontinuities when compared to the mean values for evolutionary stages indicating that the star-formation process is continuous and that the observational stages do not represent fundamentally different stages or changes in the physical mechanisms involved. We compare the evolutionary sample with other star-formation tracers (methanol and water masers, extended green objects and molecular outflows) and find that the association rates with these increases as a function of evolutionary stage, confirming that our clasfication is reliable. This also reveals a high association rate between quiescent sources and molecular outflows, revealing that outflows are the earliest indication that star formation has begun and that star formation is already ongoing in many of the clumps that are dark even at 70 μm.

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“…Several sources were identified with high angular resolution continuum mappings with SMA (Immer et al 2014). Among those sources, the northern fainter one AGAL012.804-00.199, was suggested to drive an outflow from CO observations (Navarete et al 2019). With the same central velocity of CO, the outflows seen in HNCO (4-3) and HCO + (1-0) in this observation could also be originated from AGAL012.804-00.199.…”

Section: Comments On Individual Sourcesmentioning

confidence: 55%

Imaging Molecular Outflow in Massive Star-forming Regions with HNCO Lines

Xie

Wang²,

Liu

et al. 2023

ApJ

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Protostellar outflows are considered a signpost of star formation. These outflows can cause shocks in the molecular gas and are typically traced by the line wings of certain molecules. HNCO (4–3) has been regarded as a shock tracer because of the high abundance in shocked regions. Here we present the first imaging results of HNCO (4–3) line wings toward nine sources in a sample of 23 massive star-forming regions using the Instituto de Radioastronomía Milimétrica 30 m Telescope. We adopt the velocity range of the full width of HC3N (10–9) and H13CO+ (1–0) emissions as the central emission values, beyond which the emission from HNCO (4–3) is considered to be from line wings. The spatial distributions of the red and/or blue lobes of HNCO (4–3) emission nicely associate with those lobes of HCO+ (1–0) in most of the sources. High-intensity ratios of HNCO (4–3) to HCO+ (1–0) are obtained in the line wings. The derived column density ratios of HNCO to HCO+ are consistent with those previously observed toward massive star-forming regions. These results provide direct evidence that HNCO could trace outflow in massive star-forming regions. This work also implies that the formation of some HNCO molecules is related to shock, either on the grain surface or within the shocked gas.

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ATLASGAL-selected massive clumps in the inner Galaxy

Cited by 9 publications

References 50 publications

Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA

Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA

ATLASGAL – evolutionary trends in high-mass star formation

Imaging Molecular Outflow in Massive Star-forming Regions with HNCO Lines

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