&lt;title&gt;Data flow system for the very large telescope interferometer&lt;/title&gt;

Ballester, P.; Chavan, A. M.; Cotton, Bill; Foresto, V. Coudé du; Glindemann, Andreas; Guirao, Carlos; Jaffe, W.; Kervella, P.; Longinotti, Antonio; Percheron, Isabelle; Peron, M.; Duc, Than Phan; Pirenne, B.; Quinn, Peter J.; Richichi, A.; Schoeller, Markus; Wicenec, A.; Wilhelm, Rainer; Wittkowski, M.; Zampieri, Stefano

doi:10.1117/12.447178

Cited by 7 publications

(2 citation statements)

References 4 publications

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“…We reduced the SDSS J1111+1437 spectra using the ESO Reflex workflow (Ballester et al 2011). The onedimensional spectra extracted were then coadded after manually performing cosmic-ray rejection on each spectrum.…”

Section: Observation and Data Reductionmentioning

confidence: 99%

A Mini-BAL Outflow at 900 pc from the Central Source: VLT/X-shooter Observations

Arav

Miller

et al. 2018

ApJ

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We determine the physical conditions and location of the outflow material seen in the mini-BAL quasar SDSS J1111+1437 (z = 2.138). These results are based on the analysis of a high S/N, mediumresolution VLT/X-shooter spectrum. The main outflow component spans the velocity range −1500 to −3000 km s −1 and has detected absorption troughs from both high-ionization species: C iv, N v, O vi, Si iv, P v, and S iv; and low-ionization species: H i, C ii, Mg ii, Al ii, Al iii, Si ii, and Si iii. Measurements of these troughs allow us to derive an accurate photoionization solution for this absorption component: a hydrogen column density, log(N H ) = 21.47 +0.21 −0.27 cm −2 and ionization parameter, log(U H ) = −1.23 +0.20 −0.25 . Troughs produced from the ground and excited states of S iv combined with the derived U H value allow us to determine an electron number density of log(n e ) = 3.62 +0.09 −0.11 cm −3 ; and to obtain the distance of the ionized gas from the central source: R = 880 +210 −260 pc.

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Section: Observation and Data Reductionmentioning

confidence: 99%

A Mini-BAL Outflow at 900 pc from the Central Source: VLT/X-shooter Observations

Arav

Miller

et al. 2018

ApJ

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“…1), and ranges from ∼50 to roughly 300 for the second one. All the spectra were reduced using the ESO UVES pipeline Reflex v2.1 (Ballester et al 2011).…”

Section: Spectroscopic Datamentioning

confidence: 99%

Neutron-capture elements across the Galactic thin disk using Cepheids

Silva

Lemasle

Bono

et al. 2016

A&A

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We present new accurate abundances for five neutron-capture elements (Y, La, Ce, Nd, Eu) in 73 classical Cepheids located across the Galactic thin disk. Individual abundances are based on high spectral resolution (R ∼ 38 000) and high signal-to-noise ratio (S /N ∼ 50−300) spectra collected with UVES at ESO VLT for the DIONYSOS project. Taking into account similar Cepheid abundances provided by our group (111 stars) and available in the literature, we end up with a sample of 435 Cepheids covering a broad range in iron abundances (−1.6 < [Fe/H] < 0.6). We found, via homogeneous individual distances and abundance scales, well-defined gradients for the above elements. However, the slope of the light s-process element (Y) is at least a factor of two steeper than the slopes of heavy s-(La, Ce, Nd) and r-(Eu) process elements. The s-to-r abundance ratio ([La/Eu]) of Cepheids shows a welldefined anticorrelation with both Eu and Fe. On the other hand, Galactic field stars attain an almost constant value and display a mild enhancement in La only when they approach solar iron abundance. The [Y/Eu] ratio shows slight evidence of a correlation with Eu and, in particular, with iron abundance for field Galactic stars. We also investigated the s-process index ([hs/ls]) and we found a well-defined anticorrelation, as expected, between [La/Y] and iron abundance. Moreover, we found a strong correlation between [La/Y] and [La/Fe] and, in particular, a clear separation between Galactic and Sagittarius red giants. Finally, the comparison between predictions for low-mass asymptotic giant branch stars and the observed [La/Y] ratio indicate a very good agreement over the entire metallicity range covered by Cepheids. However, the observed spread at fixed iron content is larger than predicted by current models.

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