Probing unexplored territories with MUSE: a second generation instrument for the VLT

Bacon, Roland; Bauer, Svend‐Marian; Boehm, Paul D.; Boudon, Didier; Brau-Nogué, Sylvie; Caillier, Patrick; Capoani, L.; Carollo, C. M.; Champavert, N.; Contini, T.; Daguisé, Eric; Dalle, Didier; Délabre, Bernard; Devriendt, Julien; Dubois, Jean‐Pierre; Dupieux, M.; Dupin, J. P.; Emsellem, Éric; Ferruit, Pierre; Franx, Marijn; Gallou, G.; Gerssen, J.; Guiderdoni, B.; Hahn, T.; Hofmann, D.; Jarno, Aurélien; Kelz, Andreas; Koehler, C.; Kollatschny, W.; Kosmalski, Johan; Laurent, Florence; Lilly, S. J.; Lizon, Jean-Louis; Loupias, M.; Lynn, Stuart; Manescau, A.; McDermid, Richard M.; Monstein, C.; Nicklas, H.; Parès, L.; Pasquini, L.; Pécontal-Rousset, Arlette; Pécontal, É.; Pelló, R.; Petit, C.; Picat, J. P.; Popow, Emil; Quirrenbach, A.; Reiss, Roland; Renault, Edgard; Roth, M. M.; Schaye, Joop; Soucail, G.; Steinmetz, Matthias; Stroebele, Stefan; Stuik, Remko; Weilbacher, Peter M.; Wozniak, H.; Zeeuw, P. T. de

doi:10.1117/12.669772

Cited by 27 publications

(16 citation statements)

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“…So far, IFUs such as SINFONI allowed us to probe galaxies within 20 kpc from the quasar LOS (at redshift around 1). With the new Very Large Telescope (VLT)/Multi Unit Spectroscopic Explorer (MUSE) instrument (Bacon et al 2006(Bacon et al , 2009, one can now detect galaxies further away (∼250 kpc away at z = 1) thanks to its field of view of 1×1 arcmin (compared to 8″ × 8″ for SINFONI). The large wavelength coverage of MUSE (4800-9300 Å) allows us to target quasar fields with multiple Mg II (λλ2796, 2802) absorption lines having redshifts from 0.4-1.4 for [O II](λλ3727, 3729) identification.…”

Section: Cmentioning

confidence: 99%

Muse Gas Flow and Wind (Megaflow). I. First Muse Results on Background Quasars*

Schroetter

Bouché

Wendt

et al. 2016

ApJ

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122

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The physical properties of galactic winds are one of the keys to understand galaxy formation and evolution. These properties can be constrained thanks to background quasar lines of sight (LOS) passing near star-forming galaxies (SFGs). We present the first results of the MusE GAs FLOw and Wind survey obtained from two quasar fields, which have eight Mg II absorbers of which three have rest equivalent width greater than 0.8 Å. With the new Multi Unit Spectroscopic Explorer (MUSE) spectrograph on the Very Large Telescope (VLT), we detect six (75%) Mg II host galaxy candidates within a radius of 30″ from the quasar LOS. Out of these six galaxy-quasar pairs, from geometrical argument, one is likely probing galactic outflows, where two are classified as "ambiguous," two are likely probing extended gaseous disks and one pair seems to be a merger. We focus on the wind-pair and constrain the outflow using a high-resolution quasar spectra from the Ultraviolet and Visual Echelle Spectrograph. Assuming the metal absorption to be due to ga;s flowing out of the detected galaxy through a cone along the minor axis, we find outflow velocities in the order of ≈150 -km s 1 (i.e., smaller than the escape velocity) with a loading factor, h = M SFR ouṫ , of ≈0.7. We see evidence for an open conical flow, with a low-density inner core. In the future, MUSE will provide us with about 80 multiple galaxy−quasar pairs in two dozen fields.

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Section: Cmentioning

confidence: 99%

Muse Gas Flow and Wind (Megaflow). I. First Muse Results on Background Quasars*

Schroetter

Bouché

Wendt

et al. 2016

ApJ

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122

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“…These include the DEIMOS 5 and VIMOS 6 imaging spectrographs with two and four copies of each, respectively, within single structures. The MUSE 7 instrument for ESO VLT will field-slice a 1 arcmin. square field into 24 duplicated spectrographs.…”

Section: Introductionmentioning

confidence: 99%

Design, construction, and performance of VIRUS-P: the prototype of a highly replicated integral-field spectrograph for HET

et al. 2008

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We describe the design, construction, and performance of VIRUS-P (Visible Integral-field Replicable Unit Spectrograph -Prototype), the prototype for 150+ identical fiber-fed integral field spectrographs for the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX ‡ ). VIRUS-P was commissioned in 2007, is in regular service on the McDonald Observatory 2.7 m Smith telescope, and offers the largest field of any integral field spectrograph. The 246-fiber IFU uses a densepak-type fiber bundle with a 1/3 fill factor. It is fed at f/3.65 through a telecentric, two-group dioptric focal reducer. The spectrograph's double-Schmidt optical design uses a volume phase holographic grating at the pupil between the articulating f/3.32 folded collimator and the f/1.33 cryogenic prime focus camera. High on-sky throughput is achieved with this catadioptric system by the use of high reflectivity dielectric coatings, which set the 340-670 nm bandwidth. VIRUS-P is gimbal-mounted on the telescope to allow short fibers for high UV throughput, while maintaining high mechanical stability. The instrument software and the 18 square arcmin field, fixed-offset guider provide rapid acquisition, guiding, and precision dithering to fill in the IFU field. Custom software yields Poisson noise limited, sky subtracted spectra. The design characteristics are described that achieved uniformly high image quality with low scattered light and fiber-to-fiber cross talk. System throughput exceeds requirements and peaks at 40%. The observing procedures are described, and example observations are given.

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“…One example is the MUSE project [3] with 24 simple identical spectrometers-cum-image slicers making up for a survey-type integral field system, giving in a single exposure 9 × 10 4 spectra, 1 octave long, over a 1 × 1 field on an 8-m ESO Unit Telescope. An even more ambitious project features 145 small replicated VIRUS spectrometers [15] at the HobbyEberly Telescope.…”

Section: Multiple Small Instrumentsmentioning

confidence: 99%

Astronomical spectroscopy in the last four decades: survival of the fittest

Monnet

2009

Exp Astron

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Spectroscopic astronomical instrumentation has much evolved in the last 40 years. Long-slit grating spectrographs with a photographic plate as the detector working in the 0.3-1 µm range were prevalent up to the early 1970s. The replacement of photographic plates by two-dimensional digital detectors provided gains in sensitivity of two orders of magnitude and much better photometric and radial velocity precision, and opened the 1 to 25 µm infrared domain. Another gain in speed by up to two orders of magnitude was then obtained through the development of various spectroscopic systems, each optimized for a subset of astronomical objects. This development was underpinned by a number of technological advances, in particular the development of automatic data reduction pipelines using sophisticated algorithms. With ever larger and more complex instrument systems for the present 8-10 m diameter telescopes-and soon even more for the next generation of Extremely Large Telescopes, the development of an instrument is now a big enterprise, ranging all the way from long-term enabling technology efforts to management of large teams for construction and deployment over typically 7-8 years.

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Probing unexplored territories with MUSE: a second generation instrument for the VLT

Cited by 27 publications

References 0 publications

Muse Gas Flow and Wind (Megaflow). I. First Muse Results on Background Quasars*

Muse Gas Flow and Wind (Megaflow). I. First Muse Results on Background Quasars*

Design, construction, and performance of VIRUS-P: the prototype of a highly replicated integral-field spectrograph for HET

Astronomical spectroscopy in the last four decades: survival of the fittest

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