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arxiv: 2601.16268 · v3 · pith:T3M7XPK5new · submitted 2026-01-22 · 🌌 astro-ph.IM · astro-ph.EP· astro-ph.HE· astro-ph.SR

proto-Lightspeed: a high-speed, ultra-low read noise imager on the Magellan Clay Telescope

Christopher Layden , Kevin Burdge , Gabor Furesz , Juliana Garcia-Mejia , Jack Dinsmore , Geoffrey Mo , David Osip , John J. Piotrowski
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Roger W. Romani August Berne Deepto Chakrabarty Emma Chickles
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classification 🌌 astro-ph.IM astro-ph.EPastro-ph.HEastro-ph.SR
keywords high-speed imaginglow read noiseastronomical instrumentationMagellan telescopeoptical photometrytime-domain astronomyexoplanet transitspulsars
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The pith

proto-Lightspeed enables 6600 Hz imaging with sub-electron read noise on Magellan Clay Telescope

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

The paper presents proto-Lightspeed, a new instrument commissioned on the Nasmyth East port of the Magellan Clay Telescope for high-speed optical imaging. It achieves frame rates up to 200 Hz full frame or 6600 Hz in windowed mode using commercial re-imaging lenses and the ORCA-Quest 2 camera. The system provides seeing-limited performance in the g', r', and i' bands with adjustable pixel scales from 0.017 to 0.050 arcseconds. This setup targets observations of fast-varying sources such as compact binary systems, exoplanet transits, and pulsar emissions. The authors also outline plans for an upgraded facility instrument called Lightspeed with simultaneous multicolor imaging over a larger field.

Core claim

Proto-Lightspeed demonstrates that a high-speed imager built with off-the-shelf components can deliver deep sub-electron read noise and seeing-limited image quality at frame rates up to 6600 Hz when mounted on the Nasmyth port of the Magellan Clay Telescope, as verified through commissioning observations.

What carries the argument

The ORCA-Quest 2 camera combined with re-imaging optics that provide adjustable magnification for pixel scales between 0.017 and 0.050 arcseconds while preserving low read noise.

Load-bearing premise

The commercial re-imaging lenses and ORCA-Quest 2 camera maintain their specified performance without unexpected optical or mechanical degradation from the Nasmyth East port environment.

What would settle it

Commissioning data showing read noise above one electron or image quality significantly worse than seeing-limited would falsify the performance claims.

Figures

Figures reproduced from arXiv: 2601.16268 by August Berne, Christopher Layden, David Osip, Deepto Chakrabarty, Emma Chickles, Gabor Furesz, Geoffrey Mo, Jack Dinsmore, John J. Piotrowski, Juliana Garcia-Mejia, Kevin Burdge, Roger W. Romani.

Figure 1
Figure 1. Figure 1: Computer-aided design model of the optical components of proto-Lightspeed. Reflected light from the telescope’s tertiary mirror enters the instrument from the right. The length of each breadboard is 36 in. 2.1. Re-imaging Components We do not present a detailed optical prescription for proto-Lightspeed’s re-imaging system, as the COTS optics have proprietary designs. However, the fundamental optical princi… view at source ↗
Figure 2
Figure 2. Figure 2: a) Transmission curves for filters available in proto-Lightspeed (dashed lines), the quantum efficiency of the ORCA￾Quest 2 camera (crosses and solid line), and atmospheric transmission at unit airmass (dotted line). b) Total throughput for each bandpass. This includes the filter transmission, sensor quantum efficiency, losses due to the re-imaging optics, and atmospheric transmission at unit airmass. It d… view at source ↗
Figure 3
Figure 3. Figure 3 [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Nonlinearity and internal QE of the ORCA-Quest 2 camera. a) Top panel: The raw sensor response to increasing exposure times from a stable uniform light source, averaged across the sensor (blue points), shows significant nonlinearity at low signal levels. Individual pixels (gray points) all have slightly different response. The red dashed line shows a linear fit to the linear regime. The blue dash-dotted li… view at source ↗
Figure 5
Figure 5. Figure 5: a) Photon transfer curve (PTC) for images that have been corrected for linearity. Here the contributions from read noise and from Poissonian shot noise have been scaled to appropriately account for the effect of the linearity calibration. b) PTC for raw frames at increasing levels of exposure, with contributions from read noise and from Poissonian shot noise. The bumps around 2500 ADU in a) and b) results … view at source ↗
Figure 6
Figure 6. Figure 6: a): Flat fields taken before and after a translation caused by the lack of image stabilization in the RF lens. b): A flat field demonstrating vignetting caused by the COTS re-imaging optics. The asymmetry is likely caused by misalignment, again from the lack of image stabilization. Contours show the illumination relative to the geometric center of the field, with a maximum value of 1.15 reached slightly to… view at source ↗
Figure 7
Figure 7. Figure 7: Quadruply lensed quasar DES J0420-4037 and its lensing galaxy. a) The system observed with a single 10 s proto￾Lightspeed exposure in white light. b) A stack of the best 7% of 600 frames with exposure time 200 ms improves the PSF FWHM from 0.51′′ to 0.37′′ . c) For comparison, the system observed by the Hubble Space Telescope. lensing galaxy and better image localization. Thus, proto-Lightspeed can benefit… view at source ↗
Figure 8
Figure 8. Figure 8: Optical light curve of the Crab pulsar obtained with proto-Lightspeed over a total integration time of 300 s, sampled at 9259 Hz and phase-folded on the Crab’s rotational ephemeris. The red dotted line marks the expected phase of the optical main pulse, computed using the December 2025 radio ephemeris from the Jodrell Bank Observatory (Lyne et al. 1993) and applying the known ≈ 255 µs optical–radio pulse o… view at source ↗
Figure 9
Figure 9. Figure 9: Noise-to-signal ratio (NSR) measured for sources identified in globular cluster M30 (black points), compared to theoretical predictions from the ETC (solid red curve). M30 was observed in r ′ for 15 min at an exposure time of 30 ms. The total theoretical noise is the quadrature sum of source shot noise (green dashed), read noise (magenta dashed), scintillation noise (blue dashed), sky background noise (neg… view at source ↗
Figure 10
Figure 10. Figure 10: a) Phase-folded light curve of PSR B0540−69. Red represents the highest quality existing light curve, collected with Iqueye, while the black lines represent proto-Lightspeed’s result with 1% of the exposure time. The solid black line additionally employs an electron counting technique to reduce noise, which is enabled by proto-Lightspeed’s deep sub-electron read noise. b) Light curve of BH XRB GX 339−4, s… view at source ↗
Figure 11
Figure 11. Figure 11: Left: Optical design of the full Lightspeed instrument, allowing for either five-channel u ′ , g′ , r′ , i′ , z′ simultaneous imaging (with the potential for an additional infrared arm) or a single white light channel with polarimetric capabilities. Right: Designed image quality of Lightspeed’s five optical channels. proto-Lightspeed’s speckle interferometry capabilities and develop a data reduction pipel… view at source ↗
read the original abstract

proto-Lightspeed is a new instrument that has been commissioned on the Nasmyth East port of the Magellan Clay Telescope at Las Campanas Observatory to deliver high-speed optical imaging with deep sub-electron read noise. Making use of commercial re-imaging lenses and the ORCA-Quest 2 camera from Hamamatsu, proto-Lightspeed images a field $1'$ in diameter at up to $200$ Hz or windowed fields at higher rates, up to 6600 Hz for a $1.6''\times 1'$ field of view. proto-Lightspeed delivers seeing-limited image quality in the $g'$, $r'$, and $i'$ bands and adjustable magnification for pixel scales between $0.017''-0.050''$. proto-Lightspeed is well suited to studying compact binary systems, exoplanet transits, rapid flaring associated with accretion, periodic optical emission from pulsars, occultations of background stars by small trans-Neptunian Objects, and any other rapidly variable source. proto-Lightspeed will be a P.I. instrument beginning in 2026B, available for use by members of the Magellan Consortium. In this paper, we discuss the design and performance of the instrument, results from its two commissioning runs, and plans for a facility instrument, Lightspeed, to support simultaneous multicolor imaging across a $7'\times4'$ field.

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

0 major / 2 minor

Summary. The manuscript describes the design, commissioning on the Nasmyth East port of the Magellan Clay Telescope, and on-sky performance of proto-Lightspeed, a high-speed imager built from commercial re-imaging lenses and the Hamamatsu ORCA-Quest 2 camera. It reports concrete measured capabilities including full-frame rates up to 200 Hz (or 6600 Hz for a 1.6'' × 1' window), adjustable pixel scales of 0.017''–0.050'', sub-electron read noise, and seeing-limited image quality in the g', r', and i' bands. Results are drawn from two commissioning runs; the paper also outlines plans for a future facility-class Lightspeed instrument enabling simultaneous multicolor imaging over a 7' × 4' field. The instrument is positioned for studies of compact binaries, exoplanet transits, accretion flares, pulsars, and TNO occultations, and will become available as a PI instrument in 2026B.

Significance. If the reported on-sky metrics hold, proto-Lightspeed supplies a practical high-cadence, low-noise optical capability on a 6.5 m telescope that is currently underserved. The empirical validation from actual telescope runs (rather than datasheet extrapolations) directly supports its utility for time-domain programs, and the explicit roadmap to a wider-field multicolor facility instrument adds long-term value to the Magellan user community.

minor comments (2)
  1. [Commissioning results section] Commissioning results section: the summarized performance numbers (frame rates, read noise, image quality) would be more verifiable if accompanied by a table listing measured values with uncertainties from the two runs together with direct side-by-side comparison to the ORCA-Quest 2 laboratory specifications.
  2. [Design and performance sections] Design and performance sections: the mechanism for achieving the quoted range of magnifications and pixel scales is described at a high level; a short optical layout diagram or ray-trace summary would clarify any vignetting or image-quality trade-offs across the range.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive and accurate summary of our manuscript on proto-Lightspeed, including its design, on-sky commissioning results, and future plans. We appreciate the recognition of the instrument's practical value for time-domain observations on Magellan and the recommendation for minor revision. We will incorporate any minor suggestions into the revised manuscript. No specific major comments were listed in the report, so we provide no point-by-point responses below.

Circularity Check

0 steps flagged

No significant circularity identified

full rationale

The paper is a commissioning report for the proto-Lightspeed instrument that presents measured on-sky performance data from two runs, comparisons to manufacturer specifications for the ORCA-Quest 2 camera and commercial re-imaging lenses, and design details for pixel scales, frame rates, and sub-electron read noise. No equations or first-principles derivations are present that reduce claimed quantities to quantities fitted from the same data; the central performance assertions rest on direct empirical measurements against external benchmarks rather than any self-referential loop or self-citation chain.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

This is an instrument commissioning paper with no theoretical derivation; the central claims rest on standard assumptions about commercial detector specifications and telescope optics rather than new axioms or fitted parameters.

axioms (1)
  • domain assumption Commercial camera and lens specifications remain valid after integration and mounting on the telescope.
    The performance numbers are presented as achieved on-sky, implicitly assuming the lab specs transfer without degradation.

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