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arxiv: 2606.30721 · v1 · pith:X5OUA2YFnew · submitted 2026-06-29 · 🌌 astro-ph.IM

SHARP -- A spectrograph proposal to fully exploit ELT capabilities and look beyond JWST

P. Saracco , P. Conconi , C. Arcidiacono , H. Mahmoodzadeh , I. Di Antonio , E. Portaluri , P. Franzetti , A. Gargiulo
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I. Arosio L. Barbalini G. Lops E. Molinari J. M. Alcala S. Bisogni R. Bonito E. Bortolas M. Cantiello A. Caratti o Garatti E. Cascone V. Cianniello E. M. Corsini F. Damiani F. D'Ammando F. D'Alessio E. Dalla Bonta M. DallOra V. De Caprio G. De Lucia B. Di Francesco G. Di Rico V. D'Orazi C. Eredia A. R. Gallazzi M. G. Guarcello L. Izzo F. La Barbera M. M. Lippi M. Longhetti A. Longobardo C. Mancini M. Mirabile E. Piconcelli A. Pizzella L. Podio L. Prisinzano C. Tortora G. Vietri F. Vitali H.-F. Wang S. Zibetti
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Pith reviewed 2026-07-01 01:52 UTC · model grok-4.3

classification 🌌 astro-ph.IM
keywords ELT spectrographnear-infraredmulti-object spectrographintegral field unitadaptive opticsinstrument conceptastrophysics instrumentation
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The pith

SHARP proposes a near-infrared spectrograph for the ELT that uses two specialized units to achieve observations sharper and deeper than JWST.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper presents a concept study for SHARP, a near-IR spectrograph designed to take full advantage of the ELT's large aperture and multi-conjugate adaptive optics system. It argues that the instrument must handle both the faintest distant sources and brighter nearby targets through two distinct units, NEXUS and VESPER, to address key questions spanning primordial galaxies to nearby star and planet formation. This dual approach provides the versatility needed to bridge local and distant universe observations in a single facility. A sympathetic reader would care because it outlines a concrete path to collect data that current telescopes cannot match across wide fields.

Core claim

The central claim is that the optical design solutions developed for NEXUS, a multi-object spectrograph optimized for the faintest sources, and VESPER, a multi-object integral field unit for brighter targets, will deliver the angular resolution and sensitivity required to tackle major astrophysics and cosmology questions with the ELT.

What carries the argument

SHARP instrument concept consisting of NEXUS (multi-object spectrograph for faint sources) and VESPER (multi-object integral field unit for brighter sources), both operating in the 0.95-2.45 micron range.

If this is right

  • Detection of the faintest high-redshift sources becomes possible across large fields with the multi-object mode.
  • Detailed spectroscopy of brighter nearby objects in dust-enshrouded regions is enabled by the integral field unit mode.
  • Observations can connect the formation of young stellar objects and planetary systems with the properties of distant galaxies.
  • The instrument meets the performance goals set by the ELT's collecting area and resolution capabilities.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The dual-unit split could serve as a template for optimizing spectrographs on other extremely large telescopes where source brightness varies widely.
  • Specific science cases such as measuring chemical abundances in primordial galaxies could be quantified more precisely once detailed throughput calculations are available.
  • Combining the two units might allow efficient survey strategies that alternate between deep MOS pointings and IFU follow-up on the same field.

Load-bearing premise

The optical designs for the two units will actually deliver the angular resolution and sensitivity needed when used with the ELT's adaptive optics system.

What would settle it

An end-to-end performance simulation or laboratory test of the NEXUS or VESPER optics that shows the achieved sensitivity or resolution falls below the threshold required to detect the faintest high-redshift galaxies targeted by the science case.

Figures

Figures reproduced from arXiv: 2606.30721 by A. Caratti o Garatti, A. Gargiulo, A. Longobardo, A. Pizzella, A. R. Gallazzi, B. Di Francesco, C. Arcidiacono, C. Eredia, C. Mancini, C. Tortora, E. Bortolas, E. Cascone, E. Dalla Bonta, E. M. Corsini, E. Molinari, E. Piconcelli, E. Portaluri, F. D'Alessio, F. Damiani, F. D'Ammando, F. La Barbera, F. Vitali, G. De Lucia, G. Di Rico, G. Lops, G. Vietri, H.-F. Wang, H. Mahmoodzadeh, I. Arosio, I. Di Antonio, J. M. Alcala, L. Barbalini, L. Izzo, L. Podio, L. Prisinzano, M. Cantiello, M. DallOra, M. G. Guarcello, M. Longhetti, M. Mirabile, M. M. Lippi, P. Conconi, P. Franzetti, P. Saracco, R. Bonito, S. Bisogni, S. Zibetti, V. Cianniello, V. De Caprio, V. D'Orazi.

Figure 1
Figure 1. Figure 1: Linear size [pc] in subtended by a pixel of SHARP, 𝜃=0.035" (blue band), as a function of redshift. The green horizontal stripe represents the typical size of giant molecular gas clouds, 150-250 pc. For comparison, the red line is the linear size subtended by the pixel size (0.1"/pix) of NIRSpec at the JWST. Mass growth and hierarchical assembly - Indeed, mas￾sive, high-redshift (𝑧∼3-4) galaxies that host … view at source ↗
Figure 2
Figure 2. Figure 2: Observed wavelength of the main atomic emission (solid lines) and absorption lines (dotted lines) as a function of redshift. The blue horizontal line marks the limiting wavelength at 1.8 𝜇m of some of the next generation spectrograph as MOSAIC and ANDES at the ELT and MOONS at the VLT. In the left-hand panel, the atomic lines in the visible rest-frame (0.35-0.65 𝜇m), tracing stellar population properties a… view at source ↗
Figure 3
Figure 3. Figure 3: Linear size [pc] in logarithmic scale subtended by a pixel of SHARP, 𝜃=0.035" (blue curve), as a function of redshift. The orange line marks 1 kpc scale, the green stripe represents the typical size of giant molecular gas clouds, 150-250 pc, globular clusters and high-redshift clumps observed by JWST. The green stripe also indicates the hypothetical PopIII system at 𝑧 ∼ 10 discussed in Sections 2.2 and 3.4… view at source ↗
Figure 4
Figure 4. Figure 4: Schematic view of the components and of the optical path from the last mirror of the telescope (gray mirror on the left) to SHARP. SHARP needs a MCAO unit, an NGS unit and an Atmospheric Dispersion Corrector (ADC). Note that the NGS unit may be integrated with the MCAO system. 4.1. Instrument concept [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The Field of View (FoV) of NEXUS (blue square, 1.2’×1.2’) and the area probed by the 12 FSs of VESPER (see 4.4, red rectangle, ∼21"×40") are shown on the AO￾corrected area of the MCAO unit MORFEO (black circle, diameter D∼160"). The dark-red filled circles are the wavefront sensors for the 6 Laser Guide Stars used by MORFEO, while the yellow stars are those for the 3 Natural Guide Stars. We remind that, fo… view at source ↗
Figure 6
Figure 6. Figure 6: SHARP architecture. SHARP is enclosed in a cryogenic tank. Below the entrance window of SHARP there is the USS that manages the light between NEXUS and VESPER. NEXUS - Three dichroics split the beam into four wavelength ranges feeding 4 cameras, W1-W4. The whole wavelength range 0.95-2.45 𝜇m is thus simultaneously covered. VESPER - The image focused on the VESPER focal plane is divided into four equal stri… view at source ↗
Figure 7
Figure 7. Figure 7: Optical design from the focal plane of the MCAO unit to the detectors of NEXUS (left) and of one module of VESPER (right). In the center, the optical path from the SHARP entrance window to detectors. NEXUS - When the light is intercepted by the CSS, it passes through the slits to enters NEXUS. Three folding mirrors (FM) provide a compact design, while three dichroics (D1-D3) split the beam into four wavele… view at source ↗
Figure 9
Figure 9. Figure 9: Conceptual view of the configurable masking mechanism. Pairs of bars move toward each other to form a slit at the target position masking the outside regions [PITH_FULL_IMAGE:figures/full_fig_p012_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Optical design of a Pechan inversion prism (central panel). This prism is composed of two paired prisms. The light entering from above undergoes five reflections and comes out from below inverted. Rotating the prism by an angle 𝜃 the coming out image is rotated by a similar angle. As example, all the target galaxies (left-hand panel) are aligned along the slit according to their major axis (right-hand pan… view at source ↗
Figure 11
Figure 11. Figure 11: Fraction of Encircled Energy as a function of radial distance for VESPER at wavelength 𝜆=2.19 𝜇m. The two curves, as in [PITH_FULL_IMAGE:figures/full_fig_p014_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Schematic view of the Integral Field Selector (FSS) system feeding one channel of VESPER. Left - The 6 FSs are aligned along the 𝑥-direction and can move along the 𝑦-direction sampling an area of ≈10"×40". Center - Each FS is composed of a prism and a collimator (Co). They rigidly move by Δ𝑦. Their movement is compensated by the movement (Δ𝑦∕2) of the two 45-degree moving mirrors M1 and M2 to keep constan… view at source ↗
Figure 13
Figure 13. Figure 13: Slicer onto the focal plane of VESPER. The slicer consists of four sets of 72 micro mirrors each and the corresponding sets of pupil mirrors. Two set of micro mirrors (upper panel) and of pupil mirrors (lower panel) are shown as example. Each set samples a stripe of 0.375”×10” of the image provided by the 6 FSs. The pupil mirrors bring the light to the corresponding cameras. An MCAO unit like MORFEO at th… view at source ↗
Figure 14
Figure 14. Figure 14: Left - NIRCam image of the field centered on galaxy GLASS-180009 at 𝑧∼2.66, adapted from Bevacqua et al. (2026) ( [PITH_FULL_IMAGE:figures/full_fig_p017_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Left - Zoom in of the composite JWST image centered on GLASS-180009. The big red square is the area (∼ 1.7 ′′ × 1.5 ′′) of a single FS of VESPER. The thin red lines schematically represent the slicing at 0.031". Highlighted in green are the central spaxel with a corresponding simulated spectrum representing a SSP 1.75 Gyr old and the sum of four spaxel in the outer region with a corresponding SSP of 0.9 G… view at source ↗
read the original abstract

The Extremely Large Telescopes (ELTs), with their large apertures and cutting-edge Multi-Conjugate Adaptive Optics (MCAO) systems, promise to deliver data that is both sharper and deeper than even the James Webb Space Telescope (JWST) across large fields. SHARP is a concept study for a near-IR (0.95-2.45 $\mu$m) spectrograph specifically designed to fully exploit the collecting area and angular resolution capabilities of the upcoming ESO's ELT. The instrument concept is driven by the goal of tackling the most important questions in astrophysics and cosmology, from exploring primordial galaxies to studying the formation of young stellar object and planetary systems in the nearby dust-enshrouded regions, bridging the gap between the local and the distant Universe. This requires versatility to accommodate diverse observational needs. SHARP is composed of two main units: NEXUS, a Multi-Object Spectrograph (MOS) optimized for detecting the faintest sources, and VESPER, a multi-object Integral Field Unit (multi-IFU) designed for brighter ones. This article provides an overview of the scientific design drivers, the solutions developed to meet them, and the resulting optical design that achieves the required performance.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript presents the SHARP near-IR (0.95-2.45 μm) spectrograph concept for the ELT, driven by science cases spanning primordial galaxies to nearby star and planet formation. It describes a dual-unit architecture: NEXUS (MOS optimized for faintest sources) and VESPER (multi-IFU for brighter sources), with optical design solutions developed to exploit ELT MCAO angular resolution and sensitivity, claiming these achieve the required performance to bridge local and distant universe observations.

Significance. If the designs deliver the stated resolution and sensitivity, SHARP would provide a versatile facility instrument enabling key ELT science beyond JWST reach across large fields. The separation into faint-source MOS and brighter-source multi-IFU units is a pragmatic response to diverse observational needs. However, the manuscript supplies no quantitative performance predictions, error budgets, or verification data, so the significance remains prospective rather than demonstrated.

major comments (2)
  1. [Abstract and instrument concept paragraph] Abstract, final sentence, and instrument-concept paragraph: the assertion that the optical design 'achieves the required performance' is load-bearing for the central claim yet is unsupported by any error budgets, throughput calculations, Strehl predictions, or sensitivity simulations. The reader's weakest assumption (that NEXUS/VESPER solutions will deliver the needed resolution and sensitivity with the MCAO system) therefore rests on unshown engineering work.
  2. [Scientific design drivers] Scientific design drivers section (implied by abstract): no quantitative comparison to JWST or existing ELT instruments is given to substantiate how the dual-unit architecture meets the stated goals of detecting faintest sources while handling brighter ones across the 0.95-2.45 μm range.
minor comments (2)
  1. The manuscript would benefit from explicit tables or figures showing the optical layouts, resolving power, and field coverage for NEXUS and VESPER separately.
  2. Clarify whether the two units share a common fore-optics path or operate independently, and state the assumed MCAO performance parameters used in the design.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive review of our manuscript on the SHARP spectrograph concept. We address the major comments point by point below, noting where revisions will be made to improve clarity and support for the claims.

read point-by-point responses

  1. Referee: [Abstract and instrument concept paragraph] Abstract, final sentence, and instrument-concept paragraph: the assertion that the optical design 'achieves the required performance' is load-bearing for the central claim yet is unsupported by any error budgets, throughput calculations, Strehl predictions, or sensitivity simulations. The reader's weakest assumption (that NEXUS/VESPER solutions will deliver the needed resolution and sensitivity with the MCAO system) therefore rests on unshown engineering work.

    Authors: We agree that the current text asserts performance achievement without presenting supporting quantitative analyses such as error budgets or simulations, which is a valid observation for a concept overview paper. The optical designs were developed to meet the stated requirements based on preliminary engineering considerations, but these details are not included in the manuscript. We will revise the wording in the abstract and instrument-concept section to indicate that the designs are intended to achieve the required performance, and we will add a short summary of high-level performance expectations (e.g., resolution and sensitivity targets) to better substantiate the claims. revision: yes

  2. Referee: [Scientific design drivers] Scientific design drivers section (implied by abstract): no quantitative comparison to JWST or existing ELT instruments is given to substantiate how the dual-unit architecture meets the stated goals of detecting faintest sources while handling brighter ones across the 0.95-2.45 μm range.

    Authors: The manuscript prioritizes the science drivers and the rationale for the dual-unit (NEXUS MOS and VESPER multi-IFU) architecture to address the range of source brightnesses and the ELT MCAO capabilities. However, we acknowledge that explicit quantitative comparisons would strengthen the justification. We will incorporate a concise comparison table or paragraph in the scientific design drivers section, highlighting advantages in sensitivity, field coverage, and wavelength range relative to JWST and instruments such as HARMONI. revision: yes

Circularity Check

0 steps flagged

No significant circularity; instrument concept paper with no derivations or self-referential claims

full rationale

The paper is a forward-looking instrument concept study describing the SHARP spectrograph design (NEXUS MOS and VESPER multi-IFU units) to meet ELT MCAO goals for specified science cases. No equations, fitted parameters, predictions, or derivation chains are present that could reduce to inputs by construction. No self-citations are invoked as load-bearing uniqueness theorems or ansatzes. The central claims are design choices framed as solutions developed to address requirements, with performance presented as the outcome of the design process rather than an internal tautology. This is self-contained against external benchmarks (ELT capabilities, JWST comparison) with no internal circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The proposal rests on the unverified premise that the described optical solutions will meet ELT performance targets; no free parameters, axioms, or invented entities are introduced because no quantitative model is presented.

pith-pipeline@v0.9.1-grok · 6026 in / 1133 out tokens · 22250 ms · 2026-07-01T01:52:43.115042+00:00 · methodology

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