The Young Massive Star Cluster Westerlund 2 Observed with MUSE. II. MUSEpack—A Python Package to Analyze the Kinematics of Young Star Clusters

Zeidler, Peter; Nota, A.; Sabbi, E.; Luljak, Peter; McLeod, Anna F.; Grebel, Eva K.; Pasquali, A.; Tosi, M.

doi:10.3847/1538-3881/ab44bb

Cited by 10 publications

(11 citation statements)

References 46 publications

(59 reference statements)

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“…As described in M20, we proceed in reducing the data with the MUSE pipeline (Weilbacher et al 2012) in the environment with the standard static calibration files. For each specific observing block we use the available calibration files from the ESO archive, and subtract the sky lines according to Zeidler et al (2019) (for brevity we do not describe sky subtraction details here and refer the interested reader to M20). The flux calibration (also performed with the MUSE pipeline) is done for each observing block using the matched nightly standard star observations.…”

Section: Observationsmentioning

confidence: 99%

The impact of pre-supernova feedback and its dependence on environment

McLeod

Ali

Chevance

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Integral field units enable resolved studies of a large number of star-forming regions across entire nearby galaxies, providing insight on the conversion of gas into stars and the feedback from the emerging stellar populations over unprecedented dynamic ranges in terms of spatial scale, star-forming region properties, and environments. We use the VLT/MUSE legacy data set covering the central 35 arcmin2 (∼12 kpc2) of the nearby galaxy NGC 300 to quantify the effect of stellar feedback as a function of the local galactic environment. We extract spectra from emission line regions identified within dendrograms, combine emission line ratios and line widths to distinguish between ${\rm H\, \small {II}}$ regions, planetary nebulae, and supernova remnants, and compute their ionised gas properties, gas-phase oxygen abundances, and feedback-related pressure terms. For the ${\rm H\, \small {II}}$ regions, we find that the direct radiation pressure (Pdir) and the pressure of the ionised gas ($P_{{\rm H\, \small {II}}}$) weakly increase towards larger galactocentric radii, i.e. along the galaxy’s (negative) abundance and (positive) extinction gradients. While the increase of $P_{{\rm H\, \small {II}}}$ with galactocentric radius is likely due to higher photon fluxes from lower-metallicity stellar populations, we find that the increase of Pdir is likely driven by the combination of higher photon fluxes and enhanced dust content at larger galactocentric radii. In light of the above, we investigate the effect of increased pre-supernova feedback at larger galactocentric distances (lower metallicities and increased dust mass surface density) on the ISM, finding that supernovae at lower metallicities expand into lower-density environments, thereby enhancing the impact of supernova feedback.

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Section: Observationsmentioning

confidence: 99%

The impact of pre-supernova feedback and its dependence on environment

McLeod

Ali

Chevance

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…The optical IFU with the largest FOV to date (1 arcmin 2 ) is the Multi Unit Spectroscopic Explorer (MUSE, Bacon et al 2010) mounted at UT4 of the Very Large Telescope (VLT), which allows us to survey larger regions similar to photometric studies. MUSE has been proven to be an excellent instrument to spectroscopically map nearby star-forming regions to study the kinematics of their stars and the gas simultaneously (e.g., McLeod et al 2015McLeod et al , 2020Zeidler et al 2018Zeidler et al , 2019, for the latter two, hereafter Paper 1 and Paper 2). In Paper 1 we showed that it is indeed possible to measure stellar RVs in YSCs to an accuracy of ∼ 2 km s −1 using MUSEpack, despite the lack of pre-main sequence (PMS) stellar spectral libraries and the variable and high local background.…”

Section: Introductionmentioning

confidence: 99%

The Young Massive Star Cluster Westerlund 2 Observed with MUSE. III. A Cluster in Motion—The Complex Internal Dynamics

Zeidler

Sabbi

Nota

et al. 2021

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Analyzing the dynamical state of nearby young massive star clusters is essential for understanding star cluster formation and evolution during their earliest stages. In this work we analyze the stellar and gas kinematics of the young massive star cluster Westerlund 2 (Wd2) using data from the integral field unit Multi Unit Spectroscopic Explorer (MUSE) and complement them with proper motions from the Gaia DR2. The mean gas radial velocity of 15.9 km s−1 agrees with the assumption that Wd2 is the result of a cloud–cloud collision. The gas motions show the expansion of the H ii region, driven by the radiation from the many OB stars in the cluster center. The velocity profile of the cluster member stars reveals an increasing velocity dispersion with decreasing stellar mass and that the low-mass stars show five distinct velocity groups. Based on their spatial correlation with the cluster’s two clumps, we concluded that this is the imprint of the initial cloud collapse that formed Wd2. A thorough analysis of the dynamical state of Wd2, which determines a dynamical mass range of M dyn,Wd2 = (7.5 ± 1.9) × 104 − (4.4 ± 1.1) × 105 M ⊙ and exceeds the photometric mass by at least a factor of two, leads to the conclusion that Wd2 is not massive enough to remain gravitationally bound. Additionally we also identify 22 runaway candidates with peculiar velocities between 30 and 546 km s−1.

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Section: Observationsmentioning

confidence: 99%

The impact of pre-supernova feedback and its dependence on environment

Mcleod,

Ali,

Chevance

et al. 2021

Preprint

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Integral field units enable resolved studies of a large number of star-forming regions across entire nearby galaxies, providing insight on the conversion of gas into stars and the feedback from the emerging stellar populations over unprecedented dynamic ranges in terms of spatial scale, star-forming region properties, and environments. We use the VLT/MUSE legacy data set covering the central 35 arcmin 2 (∼12 kpc 2 ) of the nearby galaxy NGC 300 to quantify the effect of stellar feedback as a function of the local galactic environment. We extract spectra from emission line regions identified within dendrograms, combine emission line ratios and line widths to distinguish between H II regions, planetary nebulae, and supernova remnants, and compute their ionised gas properties, gas-phase oxygen abundances, and feedback-related pressure terms. For the H II regions, we find that the direct radiation pressure (𝑃 dir ) and the pressure of the ionised gas (𝑃 H II ) weakly increase towards larger galactocentric radii, i.e. along the galaxy's (negative) abundance and (positive) extinction gradients. While the increase of 𝑃 H II with galactocentric radius is likely due to higher photon fluxes from lower-metallicity stellar populations, we find that the increase of 𝑃 dir is likely driven by the combination of higher photon fluxes and enhanced dust content at larger galactocentric radii. In light of the above, we investigate the effect of increased pre-supernova feedback at larger galactocentric distances (lower metallicities and increased dust mass surface density) on the ISM, finding that supernovae at lower metallicities expand into lower-density environments, thereby enhancing the impact of supernova feedback.

show abstract

The Young Massive Star Cluster Westerlund 2 Observed with MUSE. II. MUSEpack—A Python Package to Analyze the Kinematics of Young Star Clusters

Cited by 10 publications

References 46 publications

The impact of pre-supernova feedback and its dependence on environment

The impact of pre-supernova feedback and its dependence on environment

The Young Massive Star Cluster Westerlund 2 Observed with MUSE. III. A Cluster in Motion—The Complex Internal Dynamics

The impact of pre-supernova feedback and its dependence on environment

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