The data processing pipeline for the MUSE instrument

Weilbacher, Peter M.; Palsa, Ralf; Streicher, O.; Bacon, Roland; Urrutia, T.; Wisotzki, L.; Conseil, Simon; Husemann, B.; Jarno, Aurélien; Kelz, Andreas; Pécontal-Rousset, Arlette; Richard, Johan; Roth, Martin; Selman, F.; Vernet, J.

doi:10.1051/0004-6361/202037855

Cited by 314 publications

(250 citation statements)

References 71 publications

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“…For the UDG candidate MATLAS-2019 we requested 12 observation blocks (OBs) with the Multi-unit spectroscopic explorer (MUSE) mounted at the Very Large Telescope at Cerro Paranal, of which 3 were taken in Period 103 (PI: Francine Marleau) under program 0103.B-0635. The data were reduced via the MUSE pipeline (Weilbacher et al 2020) wrapped within the pymusepipe python package pymusepipe 1 (Emsellem et al 2019), which was previously used to reduce MUSE data taken for the UDG NGC 1052-DF2. This pipeline takes all raw data available in the European Southern Observatory science archive and produces a combined and calibrated (i.e., bias and flat-field…”

Section: Observations Data Reduction and Spectroscopymentioning

confidence: 99%

Spectroscopic study of MATLAS-2019 with MUSE: An ultra-diffuse galaxy with an excess of old globular clusters

Müller

Marleau

Duc

et al. 2020

A&A

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The MATLAS deep imaging survey has uncovered a plethora of dwarf galaxies in the low density environment it has mapped. A fraction of them are unusually extended and have low surface brightness. Among these so-called ultra-diffuse galaxies, a few seem to host an excess of globular clusters (GCs). With the integral field unit spectrograph MUSE we have observed one of these galaxies – MATLAS J15052031+0148447 (MATLAS-2019) – located toward the nearby group NGC 5846 and measured its systemic velocity, age, and metallicity, and that of its GC candidates. For the stellar body of MATLAS-2019 we derive a metallicity of −1.33−0.01+0.19 dex and an age of 11.2−0.8+1.8 Gyr. For some of the individual GCs and the stacked GC population, we derive consistent ages and metallicities. From the 11 confirmed GCs and using a Markov Chain Monte Carlo approach we derived a dynamical mass-to-light ratio of 4.2−3.4+8.6 M⊙/L⊙. This is at the lower end of the luminosity-mass scaling relation defined by the Local Group dwarf galaxies. Furthermore, we could not confirm or reject the possibility of a rotational component in the GC system. If present, this would further modify the inferred mass. Follow-up observations of the GC population and of the stellar body of the galaxy are needed to assess whether this galaxy lacks dark matter, as was suggested for the pair of dwarf galaxies in the field of NGC 1052, or if this is a misinterpretation arising from systematic uncertainties of the method commonly used for these systems and the large uncertainties of the individual GC velocities.

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Section: Observations Data Reduction and Spectroscopymentioning

confidence: 99%

Spectroscopic study of MATLAS-2019 with MUSE: An ultra-diffuse galaxy with an excess of old globular clusters

Müller

Marleau

Duc

et al. 2020

A&A

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“…Data reduction was performed using the MUSE pipeline (version 1.6.2, Weilbacher et al 2012Weilbacher et al , 2016 under the ES-OREFLEX environment (Freudling et al 2013). In summary, the data reduction involved bias and overscan subtraction, flat fielding, wavelength calibration, determination of the line spread function, illumination correction with twilight flats (to account for large-scale variation of the illumination of the detectors) and similar with lamp flats (to correct for edge effects between the integral-field units).…”

Section: Fcc Common Namementioning

confidence: 99%

AlFoCS + Fornax3D: resolved star formation in the Fornax cluster with ALMA and MUSE

Zabel

Davis

Sarzi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We combine data from ALMA and MUSE to study the resolved (∼300 pc scale) star formation relation (star formation rate, SFR, versus molecular gas surface density) in cluster galaxies. Our sample consists of nine Fornax cluster galaxies, including spirals, ellipticals, and dwarfs, covering a stellar mass range of ∼108.8–1011 M⊙. CO(1-0) and extinction corrected Hα were used as tracers for the molecular gas mass and SFR, respectively. We compare our results with Kennicutt and Bigiel et al. Furthermore, we create depletion time maps to reveal small-scale variations in individual galaxies. We explore these further in FCC290, using the ‘uncertainty principle for star formation’ (Kruijssen & Longmore) to estimate molecular cloud lifetimes, which we find to be short (<10 Myr) in this galaxy. Galaxy-averaged depletion times are compared with other parameters such as stellar mass and cluster-centric distance. We find that the star formation relation in the Fornax cluster is close to those from Kennicutt and Bigiel et al., but overlaps mostly with the shortest depletion times predicted by Bigiel et al. This slight decrease in depletion time is mostly driven by dwarf galaxies with disturbed molecular gas reservoirs close to the virial radius. In FCC90, a dwarf galaxy with a molecular gas tail, we find that depletion times are a factor ≳10 higher in its tail than in its stellar body.

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“…During the observing runs the average seeing was nearly constant with a FWHM of about 1.6 . The reduction of the data and the construction of the final calibrated data cubes were carried out within the ESO REFLEX environment (Freudling et al 2013) using the standard MUSE Data Reduction Software (version 2.4.2) (Weilbacher et al 2012(Weilbacher et al , 2016. Sky residuals were removed from the final data cube by using MUSE-ZAP (v.2.2) (Soto et al 2016).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

On the accretion of a new group of galaxies on to Virgo: I. Internal kinematics of nine in-falling dEs

Bidaran

Pasquali

Lisker

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Galaxy environment has been shown to play an important role in transforming late-type, star-forming galaxies to quiescent spheroids. This transformation is expected to be more severe for low-mass galaxies (M < 1010M⊙) in dense galaxy groups and clusters, mostly due to the influence of their past host halos (also known as pre-processing) and their present-day environments. For the first time, in this study, we investigate a sample of nine early-type dwarf galaxies (dEs) that were accreted as a likely bound group onto the Virgo galaxy cluster about 2-3 Gyr ago. Considering this special condition, these nine dEs may provide a test bed for distinguishing between the influence of the Virgo galaxy cluster and the effects of the previous host halo on their current properties. Specifically, we use VLT/MUSE integral-field unit spectra to derive their kinematics and specific angular momentum (λR) profiles. We observe a spread in the λR profiles of our sample dEs, finding that the λR profiles of half of them are as high as those of low-mass field galaxies. The remaining dEs exhibit λR profiles as low as those of Virgo dEs that were likely accreted longer ago. Moreover, we detect nebular emission in one dE with a gas velocity offset suggesting ongoing gas stripping in Virgo. We suggest that the low-λR dEs in our sample were processed by their previous host halo, prior to their infall to Virgo, and that the high-λR dEs may be experiencing ram pressure stripping in Virgo.

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The data processing pipeline for the MUSE instrument

Cited by 314 publications

References 71 publications

Spectroscopic study of MATLAS-2019 with MUSE: An ultra-diffuse galaxy with an excess of old globular clusters

Spectroscopic study of MATLAS-2019 with MUSE: An ultra-diffuse galaxy with an excess of old globular clusters

AlFoCS + Fornax3D: resolved star formation in the Fornax cluster with ALMA and MUSE

On the accretion of a new group of galaxies on to Virgo: I. Internal kinematics of nine in-falling dEs

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