Science requirements and trade-offs for the MOSAIC instrument for the European ELT

Evans, Christopher J.; Puech, M.; Rodrigues, M.; Barbuy, B.; Cuby, Jean-Gabriel; Dalton, Gavin; Fitzsimons, E.; Hammer, F.; Jagourel, Pascal; Kaper, L.; Morris, S. L.; Morris, Tim

doi:10.1117/12.2231675

Cited by 12 publications

(14 citation statements)

References 14 publications

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“…Recently, Krolewski et al (2018) presented 3D H i density field reconstruction at z ∼ 2 using wiener filtering technique (with an effective smoothing scales of 2.5 h −1 cMpc) applied to Lyα absorption detected in moderate resolution spectra of high-z star-forming galaxies. While we wait for the arrival of extremely large telescopes to probe IGM tomography over a large range of scales with better sensitivity (Skidmore et al 2015;Evans et al 2016), SDSS quasar catalog offers rare possibilities to make some important progress. Recently, Sien Tie et al (2019) has made a theoretical predication of three-point correlation in Lyα forest at large scales (10-30h −1 Mpc).…”

Section: Introductionmentioning

confidence: 99%

Three- and two-point spatial correlations of intergalactic medium at z ∼ 2 using projected quasar triplets

Maitra

Srianand

Petitjean

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present analysis of two-and three-point correlation functions of Lyα forest (at 2 ≤ z ≤ 2.5) using X-Shooter spectra of three background quasar triplets probing transverse separations of 0.5-1.6 pMpc. We present statistics based on transmitted flux and clouds identified using Voigt profile fitting. We show that the observed two-, three-point correlation functions and reduced three-point correlation (i.e Q) are well reproduced by our simulations. We assign probabilities for realising all the observed correlation properties simultaneously using our simulations. Our simulations suggest an increase in correlation amplitudes and Q with increasing N HI . We roughly see this trend in the observations too. We identify a concurrent gap of 17Å (i.e 14.2 h −1 cMpc, one of the longest reported) wide in one of the triplets. Such gap is realised only in 14.2% of our simulated sightlines and most of the time belongs to a void in the matter distribution. In the second triplet, we detect DLAs along all three sightlines (with spatial separations 0.64 to 1.6 pMpc) within a narrow redshift interval (i.e ∆z = 0.088). Detection of a foreground quasar (∼ 1 pMpc from the triplet sightlines) and excess partial Lyman Limit systems around these DLAs suggest that we may be probing a large over-dense region. We also report positive C iv-C iv correlations up to ∼ 500 kms −1 only in the longitudinal direction. Additionally, we conclude a positive C iv-Lyα correlations for higher N HI thresholds up to a scale of ∼ 1000 kms −1 both in transverse and longitudinal directions.

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Section: Introductionmentioning

confidence: 99%

Three- and two-point spatial correlations of intergalactic medium at z ∼ 2 using projected quasar triplets

Maitra

Srianand

Petitjean

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Nonetheless, after decades mostly spent exploring these potentialities, astrophotonics is already starting to become a favorite companion of advanced astronomical instrumentation. For example, photonic technologies will be part of the instrumentation for Extremely Large Telescopes (ELTs) already from the very beginning, as for instance laser guide stars for adaptive optics (Ciliegi et al 2018) and optical fibers as key components of multi-object and/or integral field spectrographs (Evans et al 2016).…”

Section: Astronomical Instrumentation and Sciencementioning

confidence: 99%

Astrophotonics: astronomy and modern optics

Minardi¹,

Harris

Labadie

2021

Astron Astrophys Rev

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Much of the progress in astronomy has been driven by instrumental developments, from the first telescopes to fiber fed spectrographs. In this review, we describe the field of astrophotonics, a combination of photonics and astronomical instrumentation that is gaining importance in the development of current and future instrumentation. We begin with the science cases that have been identified as possibly benefiting from astrophotonic devices. We then discuss devices, methods and developments in the field along with the advantages they provide. We conclude by describing possible future perspectives in the field and their influence on astronomy.

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“…Figure 2 shows that above 2 µm, the 39m telescope thermal background increasingly dominates, which rapidly reaches 1000 times the zodiacal light that limits JWST's performance in space. We are carrying out an analytic comparison of the MOSAIC HDM vs. the JWST/NIRSpec single IFU (see more details in [3]). These preliminary calculations reveal that for J-and H-band observations MOSAIC with 10 IFUs in the HDM mode will be a few times more efficient than assembling surveys of targets one at a time with NIRSpec.…”

Section: Trade-off Regarding Extension Of Mosaic To Include K-bandmentioning

confidence: 99%

“…The potential performance of MOSAIC at the blue end of the visible spectrum will be investigated (see also [3]). This is primarily motivated by a couple of the science cases (IGM tomography and Galaxy archaeology).…”

Section: Analysis Of Potential Blue-visible Performance Of Mosaicmentioning

confidence: 99%

The E-ELT multi-object spectrograph: latest news from MOSAIC

Hammer

Morris

Kaper³

et al. 2016

SPIE Proceedings

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There are 8000 galaxies, including 1600 at z≥ 1.6, which could be simultaneously observed in an E-ELT field of view of 40 arcmin 2 . A considerable fraction of astrophysical discoveries require large statistical samples, which can only be obtained with multi-object spectrographs (MOS). MOSAIC will provide a vast discovery space, enabled by a multiplex of 200 and spectral resolving powers of R=5000 and 20000. MOSAIC will also offer the unique capability of more than 10 `high-definition' (multi-object adaptive optics, MOAO) integral-field units, optimised to investigate the physics of the sources of reionization. The combination of these modes will make MOSAIC the world-leading MOS facility, contributing to all fields of contemporary astronomy, from extra-solar planets, to the study of the halo of the Milky Way and its satellites, and from resolved stellar populations in nearby galaxies out to observations of the earliest 'first-light' structures in the Universe. It will also study the distribution of the dark and ordinary matter at all scales and epochs of the Universe. Recent studies of critical technical issues such as sky-background subtraction and MOAO have demonstrated that such a MOS is feasible with state-of-the-art technology and techniques. Current studies of the MOSAIC team include further trade-offs on the wavelength coverage, a solution for compensating for the non-telecentric new design of the telescope, and tests of the saturation of skylines especially in the near-IR bands. In the 2020s the E-ELT will become the world's largest optical/IR telescope, and we argue that it has to be equipped as soon as possible with a MOS to provide the most efficient, and likely the best way to follow-up on James Webb Space Telescope (JWST) observations.

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Science requirements and trade-offs for the MOSAIC instrument for the European ELT

Cited by 12 publications

References 14 publications

Three- and two-point spatial correlations of intergalactic medium at z ∼ 2 using projected quasar triplets

Three- and two-point spatial correlations of intergalactic medium at z ∼ 2 using projected quasar triplets

Astrophotonics: astronomy and modern optics

The E-ELT multi-object spectrograph: latest news from MOSAIC

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