Design, construction, and performance of UVES, the echelle spectrograph for the UT2 Kueyen Telescope at the ESO Paranal Observatory

By H. Dekker, S. D’odorico, A. Kaufer, B. Delabre, H. Kotzlowski. Astronomical Telescopes and Instrumentation, 2000

685 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d55e4427f8ed06b38e5903374f23866cee21df33

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In Astronomy and Astrophysics

1. Timothy C. Beers
2. M. Pettini
3. C. Steidel
4. A. Shapley
5. Naveen A. Reddy
6. C. Sneden
7. C. Conroy
8. D. Erb

In Atomic and Molecular Physics, and Optics

1. C. Steidel
2. Naveen A. Reddy
3. M. Pettini
4. A. Shapley
5. D. Erb
6. Martin Asplund
7. V. Hill
8. S. Desidera

In Instrumentation

1. C. Steidel
2. M. Pettini
3. A. Shapley
4. Naveen A. Reddy
5. D. Erb
6. Timothy C. Beers
7. E. Carretta
8. C. Sneden

Citations in the corpus

• A double stellar generation in the globular cluster NGC 6656 (M 22): Two stellar groups with different iron and s-process element abundances (2009, methodology): “The observations were obtained using UVES (Dekker et al. 2000) and FLAMES@UVES (Pasquini et al. 2002).”
• Galaxies and Intergalactic Matter at Redshift z ~ 3: Overview (2002, background): “Our results relied in part on public data released from UVES Commissioning observations at the VLT Kueyen telescope.”
• Probing the Interstellar Medium near Star-forming Regions with Gamma-Ray Burst Afterglow Spectroscopy: Gas, Metals, and Dust (2007, methodology): “…observations of quasars acquired with the HIRES (Vogt et al. 1994) and ESI (Sheinis et al. 2000) spectrometers at the Keck Observatory and the UVES (Dekker et al. 2000) spectrometer at the VLT Observatory; and (ii) the low-resolution QSO-DLA surveys of the Sloan Digital Sky Survey (SDSS; Prochaska…”
• The two metallicity groups of the globular cluster M 22: a chemical perspective (2011, neutral): “…50 75 5 Wang et al. (2003) MCD-2DC 60,000 4200−9000 70 120 6 Tull et al. (1995) LICK-HAM 50,000 4800−8800 50 90 9 Vogt et al. (1987) Valenti et al. (1995) VLT-UVES 45,000 3300−4500 100 120 16 Dekker et al. (2000) 4800−6800 Marino et al. (2009) (a) Short-hand notation adopted in this paper.”
• An Abundance Analysis of Bright Giants in the Globular Cluster NGC 1851 (2007, neutral): “The observations were obtained using UVES (Dekker et al. 2000).”
• First stars VII - Lithium in extremely metal poor dwarfs (2006, methodology): “We used the VLT-Kuyen 8.2 m telescope and the UVES spectrograph (Dekker et al. 2000) in two non-standard settings, both with dichroic # 1: 396+573, 396+850; the numbers are the central wavelength in nm in the blue and red arms, respectively.”
• The Evolution of the C/O Ratio in Metal-poor Halo Stars (2003, background): “We address this topic in the present paper with new observations of 34 halo stars obtained with the Ultraviolet and Visual Echelle Spectrograph (UVES; Dekker et al. 2000) on the European Southern Observatory Very Large Telescope (VLT).”
• The lithium content of the globular cluster NGC 6397 (2002, methodology): “Our spectra were collected at ESO-Paranal with the UVES spectrograph (Dekker et al. 2000) at the Kueyen 8.2m telescope between June 15th 2000 and June 22nd 2000, and have already been described in Gratton et al. (2001); the log of the observations is given in Table 1, the DIMM seeing was noted,…”
• FIES: The high-resolution Fiber-fed Echelle Spectrograph at the Nordic Optical Telescope (2014, background): “2; Baranne et al. 1972; Dekker et al. 2000) with two off-axis collimators, the first of which is double pass.”
• The most metal-poor damped Lyα systems: insights into chemical evolution in the very metal-poor regime★ (2011, methodology): “Most of our candidates were observed with the UVES spectrograph (Dekker et al. 2000), which is mounted on UT2 at the Very Large Telescope facility.”
• A new, precise measurement of the primordial abundance of deuterium (2012, methodology): “The spectrum was recorded with the Ultraviolet and Visual Echelle Spectrograph (UVES; Dekker et al. 2000) mounted on UT 2 of the Very Large Telescope facility.”
• The VLT-UVES survey for molecular hydrogen in high-redshift damped Lyman α systems: physical conditions in the neutral gas (2005, methodology): “UVES (Dekker et al. 2000), installed at the European Southern Observatory Very Large Telescope (ESO VLT) 8.2-m telescope unit, Kueyen, on Mount Paranal in Chile was used to search for H2 in a large sample of DLAs.”
• CARBON-ENHANCED METAL-POOR STARS IN SDSS/SEGUE. I. CARBON ABUNDANCE ESTIMATION AND FREQUENCY OF CEMP STARS (2013, methodology): “The spectra for the three stars from Spite et al. (2013) were collected with VLT/UVES (Dekker et al. 2000) at a resolving power ofR ∼ 39,000.”
• The Extremely Metal-poor, Neutron Capture-rich Star CS 22892-052: A Comprehensive Abundance Analysis (2003, methodology): “Single-line EW matches were employed for most transitions, but full spectrum syntheses were done for transitions of Sc i, Sc ii, Mn i, Mn ii, 16 Data release of 2000March, discussed in http://www.eso.org/science/uves_comm/UVES_comm_stars.html.”
• HE 0107–5240, a Chemically Ancient Star. I. A Detailed Abundance Analysis (2003, methodology): “Spectroscopy HE 0107 5240 was observed during the nights of 2001 December 19 and 20 at the European Southern Observatory, Paranal, Chile, with the Ultraviolet-Visual Echelle Spectrograph (UVES; Dekker et al. 2000) mounted on the 8 m Unit Telescope 2 (Kueyen) of the Very Large Telescope (VLT).”
• VLT/UVES Abundances in Four Nearby Dwarf Spheroidal Galaxies. I. Nucleosynthesis and Abundance Ratios (2002, methodology): “Spectra of red giants in four dSph’s were obtained at the Very Large Telescope Kueyen at Paranal, Chile, in 2000 August and 2001 January using the Ultraviolet-Visual Echelle Spectrograph (UVES, Dekker et al. 2000) in visitor mode (see Table 1).”
• OXYGEN ABUNDANCES IN NEARBY FGK STARS AND THE GALACTIC CHEMICAL EVOLUTION OF THE LOCAL DISK AND HALO (2013, neutral): “…Tull et al. 1995), HRS/HET (High Resolution Spec- trograph, 9.2m Hobby-Eberly Telescope; Tull 1998), UVES/VLT (UV-Visual Echelle Spectrograph, 8m Very Large Telescope; Dekker et al. 2000), and FEROS/ESO (Fiber-feb Extended Range Optical Spectrograph, ESO 1.52-m Telescope; Kaufer & Pasquini 1998).”
• THE GASEOUS ENVIRONMENT OF HIGH-z GALAXIES: PRECISION MEASUREMENTS OF NEUTRAL HYDROGEN IN THE CIRCUMGALACTIC MEDIUM OF z ∼ 2–3 GALAXIES IN THE KECK BARYONIC STRUCTURE SURVEY (2012, methodology): “All available archival data for these 15 QSOs have been incorporated, including data taken with UVES (Dekker et al. 2000) on the VLT for Q2206-199 and Q2343+125.”
• Discovery of HE 1523–0901, a Strongly r-Process-enhanced Metal-poor Star with Detected Uranium (2007, methodology): “OBSERVATIONS To confirm the tentative U detection in HE 1523−0901, new observations were obtained with the UltravioletVisual Echelle Spectrograph (UVES; Dekker et al. 2000) at the ESO Very Large Telescope.”