Resolving stellar populations with integral field spectroscopy

Roth, Martin; Weilbacher, Peter M.; Castro, N.

doi:10.1002/asna.201913751

Cited by 2 publications

(1 citation statement)

References 49 publications

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“…Although conceptually designed as a cosmology machine, the Multi-Unit Spectroscopic Explorer (MUSE; Bacon et al 2014) on the Very Large Telescope (VLT) presents exciting capabilities for the spectroscopy of stellar populations (see the review by Roth et al 2019) and a leap forward from pioneering studies based on 3D spectroscopy (e.g., Kamann et al 2013). This unique integral field spectrograph with a large field-of-view (1 × 1 ), excellent image quality, and high efficiency enables a novel approach to studying populations of massive stars, somewhere in between traditional photometric and multi-object spectroscopic surveys.…”

Section: Introductionmentioning

confidence: 99%

Mapping the core of the Tarantula Nebula with VLT-MUSE

Castro

Crowther

Evans

et al. 2021

A&A

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We present the spectroscopic analysis of 333 OB-type stars extracted from VLT-MUSE observations of the central 30 × 30 pc of NGC 2070 in the Tarantula Nebula on the Large Magellanic Cloud, the majority of which are analysed for the first time. The distribution of stars in the spectroscopic Hertzsprung-Russell diagram (sHRD) shows 281 stars in the main sequence. We find two groups in the main sequence, with estimated ages of 2.1 ± 0.8 and 6.2 ± 2 Myr. A subgroup of 52 stars is apparently beyond the main sequence phase, which we consider to be due to emission-type objects and/or significant nebular contamination affecting the analysis. As in previous studies, stellar masses derived from the sHRD are systematically larger than those obtained from the conventional HRD, with the differences being largest for the most massive stars. Additionally, we do not find any trend between the estimated projected rotational velocity and evolution in the sHRD. The projected rotational velocity distribution presents a tail of fast rotators that resembles findings in the wider population of 30 Doradus. We use published spectral types to calibrate the He Iλ4921/He IIλ5411 equivalent-width ratio as a classification diagnostic for early-type main sequence stars when the classical blue-visible region is not observed. Our model-atmosphere analyses demonstrate that the resulting calibration is well correlated with effective temperature.

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Section: Introductionmentioning

confidence: 99%

Mapping the core of the Tarantula Nebula with VLT-MUSE

Castro

Crowther

Evans

et al. 2021

A&A

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Reliable stellar abundances of individual stars with the MUSE integral-field spectrograph

Wang

Hayden

Sharma

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present a novel approach to deriving stellar labels for stars observed in MUSE fields making use of data-driven machine learning methods. Taking advantage of the comparable spectral properties (resolution, wavelength coverage) of the LAMOST and MUSE instruments, we adopt the Data-Driven Payne (DD-Payne) model used on LAMOST observations and apply it to stars observed in MUSE fields. Remarkably, in spite of instrumental differences, according to the cross-validation of 27 LAMOST-MUSE common stars, we are able to determine stellar labels with precision better than 75K in Teff, 0.15 dex in log g, and 0.1 dex in abundances of [Fe/H], [Mg/Fe], [Si/Fe], [Ti/Fe], [C/Fe], [Ni/Fe] and [Cr/Fe] for current MUSE observations over a parameter range of 3800 < Teff < 7000 K, −1.5 < [Fe/H] < 0.5 dex. To date, MUSE has been used to target 13,000 fields across the southern sky since it was first commissioned six years ago and it is unique in its ability to study dense star fields such as globular clusters or the Milky Way bulge. Our method will enable the automated determination of stellar parameters for all stars in these fields. Additionally, it opens the door for applications to data collected by other spectrographs having resolution similar to LAMOST. With the upcoming BlueMUSE and MAVIS, we will gain access to a whole new range of chemical abundances with higher precision, especially critical s-process elements such as [Y/Fe] and [Ba/Fe] that provide key age diagnostics for stellar targets.

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Resolving stellar populations with integral field spectroscopy

Cited by 2 publications

References 49 publications

Mapping the core of the Tarantula Nebula with VLT-MUSE

Mapping the core of the Tarantula Nebula with VLT-MUSE

Reliable stellar abundances of individual stars with the MUSE integral-field spectrograph

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