The MUSE second-generation VLT instrument

Bacon, Roland; Accardo, M.; Adjali, L.; Anwand, H.; Bauer, Svend M.; Biswas, I.; Blaizot, Jérémy; Boudon, Didier; Brau-Nogué, Sylvie; Brinchmann, Jarle; Caillier, Patrick; Capoani, L.; Carollo, C. M.; Contini, T.; Couderc, Paul; Daguisé, Eric; Deiries, S.; Délabre, Bernard; Dreizler, S.; Dubois, Jean‐Pierre; Dupieux, M.; Dupuy, Christophe; Emsellem, Éric; Fechner, Thomas; Fleischmann, Andreas; François, M.; Gallou, G.; Gharsa, T.; Glindemann, Andreas; Gojak, D.; Guiderdoni, B.; Hansali, G.; Hahn, T.; Jarno, Aurélien; Kelz, Andreas; Koehler, C.; Kosmalski, Johan; Laurent, Florence; Floc’h, M. Le; Lilly, S. J.; Lizon, Jean-Louis; Loupias, M.; Manescau, A.; Monstein, C.; Nicklas, H.; Olaya, Jean-Christophe; Parès, L.; Pasquini, L.; Pécontal-Rousset, Arlette; Pelló, R.; Petit, C.; Popow, Emil; Reiss, Roland; Remillieux, A.; Renault, Edgard; Roth, M. M.; Rupprecht, G.; Serre, Denis; Schaye, Joop; Soucail, G.; Steinmetz, Matthias; Streicher, O.; Stuik, Remko; Valentin, Hervé; Vernet, J.; Weilbacher, P.; Wisotzki, L.; Yerle, N.

doi:10.1117/12.856027

Cited by 679 publications

(224 citation statements)

References 4 publications

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“…Similar results have been reported very recently for six galaxies by van Dokkum et al (2016). Other studies, however, have argued that while steep gradients in some spectral features are indeed present, the pattern of trends (especially the weakness or absence of gradient in the Fe H Wing-Ford band) is more consistent with abundance variation than with IMF trends (McConnell, Lu & Mann 2016;Alton, Smith & Lucey 2017). For the Abell 1201 BCG itself, the classic IMF indicators (e.g.…”

Section: Discussionsupporting

confidence: 71%

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A counter-image to the gravitational arc in Abell 1201:Evidence for IMF variations, or a 10 ¹⁰ M _⊙ black hole?

Smith¹,

Lucey²,

Edge³

2017

Mon. Not. R. Astron. Soc.

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Section: Discussionsupporting

confidence: 71%

“…We observed Abell 1201 with the Multi-Unit Spectroscopic Explorer (MUSE) (Bacon et al 2010) on the 8.2m Yepun (Unit Telescope 4) of European Southern Observatory's Very Large Telescope. The data used in this paper were obtained on the nights of March 31 and April 2, 2016, under good seeing conditions.…”

Section: Muse Observationsmentioning

confidence: 99%

A counter-image to the gravitational arc in Abell 1201:Evidence for IMF variations, or a 10 ¹⁰ M _⊙ black hole?

Smith¹,

Lucey²,

Edge³

2017

Mon. Not. R. Astron. Soc.

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“…Furthermore, the simulations allow us to probe the effect of spiral arm pitch angle, spiral arm number and solar position with respect to the spiral arm on the resulting power spectrum, which may provide constraints on spiral arm parameters. We take further advantage of the simulations by computing the power spectra of both stars and gas over the whole disc (not just the solar neighbourhood region), which serve as observational predictions of the spiral-bar induced kinematics for external galaxies that may be tested by integral field spectroscopy (IFU) surveys such as MUSE (Bacon et al 2010) and CALIFA (Sánchez et al 2012).…”

mentioning

confidence: 99%

Spiral- and bar-driven peculiar velocities in Milky Way-sized galaxy simulations

Grand

Bovy

Kawata

et al. 2015

Mon. Not. R. Astron. Soc.

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We investigate the kinematic signatures induced by spiral and bar structure in a set of simulations of Milky Way-sized spiral disc galaxies. The set includes test particle simulations that follow a quasi-stationary density wave-like scenario with rigidly rotating spiral arms, and N -body simulations that host a bar and transient, co-rotating spiral arms. From a location similar to that of the Sun, we calculate the radial, tangential and line-of-sight peculiar velocity fields of a patch of the disc and quantify the fluctuations by computing the power spectrum from a two-dimensional Fourier transform. We find that the peculiar velocity power spectrum of the simulation with a bar and transient, co-rotating spiral arms fits very well to that of APOGEE red clump star data, while the quasi-stationary density wave spiral model without a bar does not. We determine that the power spectrum is sensitive to the number of spiral arms, spiral arm pitch angle and position with respect to the spiral arm. However, it is necessary to go beyond the line of sight velocity field in order to distinguish fully between the various spiral models with this method. We compute the power spectrum for different regions of the spiral discs, and discuss the application of this analysis technique to external galaxies.

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“…MUSE is an integral-field optical spectrograph (4750 to 9350 Å in nominal mode) with a field of view of 1 ×1 arcmin 2 (Bacon et al 2010). The field of view is divided into 24 sub-fields (channels) and each of them is sliced into 48 which are dispersed by a grating and projected on to the detector (one per channel).…”

Section: U S E O B S E Rvat I O N S a N D Data R E D U C T I O Nmentioning

confidence: 99%

A young star-forming galaxy at z = 3.5 with an extended Lyman α halo seen with MUSE

Patrício¹,

Richard²,

Verhamme

2015

Proc. IAU

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Spatially resolved studies of high-redshift galaxies, an essential insight into galaxy formation processes, have been mostly limited to stacking or unusually bright objects. We present here the study of a typical (L * , M = 6 × 10 9 M ) young lensed galaxy at z = 3.5, observed with Multi Unit Spectroscopic Explorer (MUSE), for which we obtain 2D resolved spatial information of Lyα and, for the first time, of C III] emission. The exceptional signal-to-noise ratio of the data reveals UV emission and absorption lines rarely seen at these redshifts, allowing us to derive important physical properties (T e ∼ 15600 K, n e ∼ 300 cm −3 , covering fraction f c ∼ 0.4) using multiple diagnostics. Inferred stellar and gas-phase metallicities point towards a low-metallicity object (Z stellar = ∼0.07 Z and Z ISM < 0.16 Z ). The Lyα emission extends over ∼10 kpc across the galaxy and presents a very uniform spectral profile, showing only a small velocity shift which is unrelated to the intrinsic kinematics of the nebular emission. The Lyα extension is approximately four times larger than the continuum emission, and makes this object comparable to low-mass LAEs at low redshift, and more compact than the Lyman-break galaxies and Lyα emitters usually studied at high redshift. We model the Lyα line and surface brightness profile using a radiative transfer code in an expanding gas shell, finding that this model provides a good description of both observables.Key words: techniques: imaging spectroscopy -galaxies: abundances -galaxies: highredshift -galaxies: individual: SMACSJ2031.8-4036. I N T RO D U C T I O NDuring the past few decades, our understanding of galaxy formation and evolution has made significant progress thanks to the hundreds of high-redshift (z > 3) galaxies which have been detected in dedicated observing campaigns (e.g. Shapley et al. 2003;Vanzella et al. 2009;Stark et al. 2013). The main spectral feature used to confirm the distances of these galaxies is the Lyα emission, since it E-mail: vera.patricio@univ-lyon1.fr (VP); johan.richard@univ-lyon1.fr (JR) is the brightest emission line we can observe in distant sources. Unfortunately, many of these objects are too faint to show any other emission line at rest-frame UV wavelengths or, even less likely, continuum and absorption lines, offering a limited picture of the characteristics of high-redshift galaxies. The complexity of the Lyα resonant process, which depends not only on the gas dynamics but also on gas density and dust content, also requires the observation of non-resonant lines in order to robustly probe the physical properties of such galaxies.Stacking techniques, which combine spectra or images of dozens or even hundreds of objects in order to increase signal-to-noise ratio (e.g.

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The MUSE second-generation VLT instrument

Cited by 679 publications

References 4 publications

A counter-image to the gravitational arc in Abell 1201:Evidence for IMF variations, or a 10 ¹⁰ M _⊙ black hole?

A counter-image to the gravitational arc in Abell 1201:Evidence for IMF variations, or a 10 ¹⁰ M _⊙ black hole?

Spiral- and bar-driven peculiar velocities in Milky Way-sized galaxy simulations

A young star-forming galaxy at z = 3.5 with an extended Lyman α halo seen with MUSE

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The MUSE second-generation VLT instrument

Cited by 679 publications

References 4 publications

A counter-image to the gravitational arc in Abell 1201:Evidence for IMF variations, or a 10 10 M ⊙ black hole?

A counter-image to the gravitational arc in Abell 1201:Evidence for IMF variations, or a 10 10 M ⊙ black hole?

Spiral- and bar-driven peculiar velocities in Milky Way-sized galaxy simulations

A young star-forming galaxy at z = 3.5 with an extended Lyman α halo seen with MUSE

Contact Info

Product

Resources

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A counter-image to the gravitational arc in Abell 1201:Evidence for IMF variations, or a 10 ¹⁰ M _⊙ black hole?

A counter-image to the gravitational arc in Abell 1201:Evidence for IMF variations, or a 10 ¹⁰ M _⊙ black hole?