EELT-HIRES the high-resolution spectrograph for the E-ELT

Marconi, A.; Marcantonio, P. Di; D’Odorico, V.; Cristiani, S.; Maiolino, R.; Oliva, E.; Origlia, L.; Riva, M.; Valenziano, L.; Zerbi, F. M.; Abreu, Manuel; Adibekyan, V.; Prieto, C. Allende; Amado, P. J.; Benz, W.; Boisse, I.; Bonfils, X.; Bouchy, F.; Buchhave, Lars A.; Buscher, David F.; Cabral, Alexandre; Martins, B. L. Canto; Chiavassa, A.; Coelho, João M. P.; Christensen, L.; Delgado-Mena, E.; Medeiros, J. R. De; Varano, I. Di; Figueira, P.; Fisher, Martin; Fynbo, J. P. U.; Glasse, Alistair; Haehnelt, Martin G.; Haniff, C.; Hansen, C. J.; Hatzes, A. P.; Huke, P.; Korn, A. J.; Leão, I. C.; Liske, J.; Lovis, C.; Masłowski, Piotr; Matute, I.; McCracken, Richard A.; Martins, C. J. A. P.; Monteiro, M. J. P. F. G.; Morris, S. L.; Morris, Tim; Nicklas, H.; Niedzielski, A.; Nunes, Nelson J.; Πάλλη, Ε.; Parr-Burman, Phil; Parro, Vanderlei Cunha; Parry, Ian; Pepe, F.; Piskunov, Nikolai; Queloz, D.; Quirrenbach, A.; Rebolo, R.; Reiners, A.; Reid, Derryck T.; Santos, N. C.; Seifert, W.; Sousa, S. G.; Stempels, H. C.; Strassmeier, K. G.; Sun, Xiaowei; Udry, S.; Vanzi, L.; Vestergaard, M.; Weber, M.; Zackrisson, Erik

doi:10.1117/12.2231653

Cited by 42 publications

(14 citation statements)

References 1 publication

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“…Turning this around, however, the presence of a vast population of metal absorbers that are too weak to be observed given the detection limits of current surveys is a robust prediction. Future surveys with next-generation telescopes and instruments, for example the GMT-Consortium Large Earth Finder on the Giant Magellan Telescope (G-CLEF on GMT) (Ben-Ami et al 2016) and the High Resolution Spectrograph on the Extremely Large Telescope (HIRES on ELT) (Marconi et al 2016), that probe to lower column densities will detect some of these weak absorbers, facilitating more comprehensive comparisons with the bulk of the model populations. This could lead to a greater divergence between the different models' predictions, increasing the constraining power of observations.…”

Section: Discussionmentioning

confidence: 99%

Aligned metal absorbers and the ultraviolet background at the end of reionization

Doughty

Finlator

Oppenheimer³

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We use observations of spatially-aligned C ii, C iv, Si ii, Si iv, and O i absorbers to probe the slope and intensity of the ultraviolet background (UVB) at z ∼ 6. We accomplish this by comparing observations with predictions from a cosmological hydrodynamic simulation using three trial UVBs applied in post-processing: a spectrally soft, fluctuating UVB calculated using multi-frequency radiative transfer; a soft, spatiallyuniform UVB; and a hard, spatially-uniform "quasars-only" model. When considering our paired high-ionization absorbers (Civ/Siiv), the observed statistics strongly prefer the hard, spatially-uniform UVB. This echoes recent findings that cosmological simulations generically underproduce strong C iv absorbers at z > 5. A single low/high ionization pair (Si ii/Si iv), by contrast, shows a preference for the HM12 UVB, while two more (C ii/C iv and O i/C iv) show no preference for any of the three UVBs. Despite this, future observations of specific absorbers, particularly Si iv/C iv, with next-generation telescopes probing to lower column densities should yield tighter constraints on the UVB.

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Section: Discussionmentioning

confidence: 99%

Aligned metal absorbers and the ultraviolet background at the end of reionization

Doughty

Finlator

Oppenheimer³

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Fainter stars are not accessible with current telescopes and high-resolution spectrographs, which severely limits the detailed exploration of dwarf galaxies. The highresolution spectrograph for the Extremely Large Telescope (ELT-HIRES, Marconi et al 2016) will make many fainter stars accessible for such observations and may thus be ideally suited for finding surviving Pop III stars. Accordingly, we determine the fraction of Pop III survivor stars that are expected to be in the red giant branch and also in the horizontal branch phase of their evolution.…”

Section: Expected Number Of Stars On the Red Giant Branchmentioning

confidence: 99%

Predicting the locations of possible long-lived low-mass first stars: importance of satellite dwarf galaxies

Magg

Hartwig

Agarwal

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The search for metal-free stars has so far been unsuccessful, proving that if there are surviving stars from the first generation, they are rare, they have been polluted, or we have been looking in the wrong place. To predict the likely location of Population III (Pop III) survivors, we semi-analytically model early star formation in progenitors of Milky Way-like galaxies and their environments. We base our model on merger trees from the high-resolution dark matter only simulation suite Caterpillar. Radiative and chemical feedback are taken into account self-consistently, based on the spatial distribution of the haloes. Our results are consistent with the non-detection of Pop III survivors in the Milky Way today. We find that possible surviving Population III stars are more common in Milky Way satellites than in the main Galaxy. In particular, low mass Milky Way satellites contain a much larger fraction of Pop III stars than the Milky Way. Such nearby, low mass Milky Way satellites are promising targets for future attempts to find Pop III survivors, especially for high-resolution, high signalto-noise spectroscopic observations. We provide the probabilities of finding a Pop III survivor in the red giant branch phase for all known Milky Way satellites to guide future observations.

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“…Instruments intended to perform these experiments are therefore designed to have wavelength calibration precision around 1 cm s −1 and accuracy of order 1 metre per second (m s −1 ) over a period of a decade (e.g. Liske 2014; Marconi et al 2016). The success of these projects thus critically relies on the precision and accuracy of the wavelength calibration reaching these levels.…”

Section: Introductionmentioning

confidence: 99%

Precision and consistency of astrocombs

Milaković

Pasquini

Webb

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Astrocombs are ideal spectrograph calibrators whose limiting precision can be derived using a second, independent, astrocomb system. We therefore analyse data from two astrocombs (one 18 GHz and one 25 GHz) used simultaneously on the HARPS spectrograph at the European Southern Observatory. The first aim of this paper is to quantify the wavelength repeatability achieved by a particular astrocomb. The second aim is to measure wavelength calibration consistency between independent astrocombs, that is to place limits or measure any possible zero-point offsets. We present three main findings, each with important implications for exoplanet detection, varying fundamental constant and redshift drift measurements. Firstly, wavelength calibration procedures are important: using multiple segmented polynomials within one echelle order results in significantly better wavelength calibration compared to using a single higher-order polynomial. Segmented polynomials should be used in all applications aimed at precise spectral line position measurements. Secondly, we found that changing astrocombs causes significant zero-point offsets (≈ 60 cm s −1 in our raw data) which were removed. Thirdly, astrocombs achieve a precision of 4 cm s −1 in a single exposure (≈ 10% above the measured photon-limited precision) and 1 cm s −1 when time-averaged over a few hours, confirming previous results. Astrocombs therefore provide the technological requirements necessary for detecting Earth-Sun analogues, measuring variations of fundamental constants and the redshift drift.

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EELT-HIRES the high-resolution spectrograph for the E-ELT

Cited by 42 publications

References 1 publication

Aligned metal absorbers and the ultraviolet background at the end of reionization

Aligned metal absorbers and the ultraviolet background at the end of reionization

Predicting the locations of possible long-lived low-mass first stars: importance of satellite dwarf galaxies

Precision and consistency of astrocombs

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