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NIRPS joining HARPS at ESO 3.6 m. On-sky performance and science objectives

T0 review · 3 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read A near-infrared spectrograph reaches 77 cm/s radial-velocity precision on Proxima

desk verdict NIRPS first-light paper is a comprehensive and useful instrument characterization, but the 77 cm/s headline is a model-relative residual that overstates what is demonstrated. read the letter →

arxiv 2507.21767 v1 pith:Q5CKAI6C submitted 2025-07-29 astro-ph.IM astro-ph.EP

Francois Bouchy , Rene Doyon , Francesco Pepe , Claudio Melo , Etienne Artigau , Lison Malo , Francois Wildi , Frederique Baron
show 126 more authors
Xavier Delfosse Jose Renan De Medeiros Rafael Rebolo Nuno C. Santos Gregg Wade Romain Allart Khaled Al Moulla Nicolas Blind Charles Cadieux Bruno L. Canto Martins Neil J. Cook Xavier Dumusque Yolanda Frensch Frederic Genest Jonay I. Gonzalez Hernandez Nolan Grieves Gaspare Lo Curto Christophe Lovis Lucile Mignon Louise D. Nielsen Anne-Sophie Poulin-Girard Jose Luis Rasilla Vladimir Reshetov Danuta Sosnowska Michael Sordet Jonathan Saint-Antoine Alejandro Suarez Mascareno Simon Thibault Philippe Vallee Thomas Vandal Manuel Abreu Jose L. A. Aguiar Guillaume Allain Tomy Arial Hugues Auger Susana C. C. Barros Luc Bazinet Bjorn Benneke Xavier Bonfils Anne Boucher Vincent Bourrier Sebastien Bovay Christopher Broeg Denis Brousseau Vincent Bruniquel Marta Bryan Alexandre Cabral Andres Carmona Yann Carteret Zalpha Challita Bruno Chazelas Ryan Cloutier Joao Coelho Marion Cointepas Uriel Conod Nicolas B. Cowan Eduardo Cristo Joao Gomes da Silva Laurie Dauplaise Antoine Darveau-Bernier Roseane de Lima Gomes Daniel Brito de Freitas Elisa Delgado-Mena Jean-Baptiste Delisle David Ehrenreich Joao Faria Pedro Figueira Dasaev O. Fontinele Thierry Forveille Jonathan Gagne Ludovic Genolet Felix Gracia Temich Olivier Hernandez Melissa J. Hobson Jens Hoeijmakers Norbert Hubin Farbod Jahandar Ray Jayawardhana Hans-Ulrich Kauf Dan Kerley Johann Kolb Vigneshwaran Krishnamurthy David Lafreniere Pierrot Lamontagne Pierre Larue Henry Leath Alexandrine L Heureux Izan de Castro Leao Olivia Lim Allan M. Martins Jaymie Matthews Jean-Sebastien Mayer Yuri S. Messias Stan Metchev Leslie Moranta Christoph Mordasini Dany Mounzer Nicola Nari Ares Osborn Mathieu Ouellet Jon Otegi Lena Parc Luca Pasquini Vera M. Passegger Stefan Pelletier Celine Peroux Caroline Piaulet-Ghorayeb Mykhaylo Plotnykov Emanuela Pompei Jason Rowe Mirsad Sarajlic Alex Segovia Julia Seidel Damien Segransan Robin Schnell Ana Rita Costa Silva Avidaan Srivastava Valentina Vaulato Atanas K. Stefanov Marcio A. Teixeira Stephane Udry Joost P. Wardenier Bachar Wehbe Drew Weisserman Vincent Yariv Gerard Zins
This is my paper · ORCID
classification astro-ph.IMastro-ph.EP
keywords NIRPSnear-infraredspectrographradialvelocityprecisionMdwarfexoplanetsadaptiveopticsmodalnoiseHARPSsimultaneousobservationexoplanetatmospheres
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper presents the NIRPS near-infrared spectrograph, installed on the ESO 3.6-m telescope in 2023. It claims that an adaptive-optics-fed, cryogenic echelle has reached a radial-velocity precision of 77 cm/s on the bright M dwarf Proxima and a precision around 1 m/s over several weeks, matching optical spectrographs. Because NIRPS covers the Y, J, and H bands (972.4-1919.6 nm) and can observe simultaneously with HARPS, it offers continuous wavelength coverage from 378 to 1920 nm for M dwarf planet searches and atmospheric studies. If these performance numbers hold, the instrument pushes precise planet hunting into the near-infrared, where very red late-M and active stars are easier to measure.

What carries the argument

The load-bearing components are the adaptive-optics front end and an AO-assisted fibre link that feeds either a 0.4-arcsecond 'high-accuracy' fibre (HA) or a 0.9-arcsecond 'high-efficiency' fibre (HE) with a pupil slicer. The HA fibre is a 29-micron octagonal fibre, while the HE fibre is a 66-micron octagonal fibre feeding a rectangular 33 by 132 micron output; at H-band wavelengths only about 30 modes propagate, so modal noise dominates the precision budget. Fibre stretchers stretching a 20-m section by 6-8 mm at 0.3 Hz plus an AO tip-tilt scanning mode reduce the modal-noise-induced continuum dispersion to about 0.5-0.7 percent, at the cost of a floor of roughly 1.4 m/s and 0.9 m/s in HA and HE modes. A cryogenic white-pupil echelle spectrograph with a 4096 by 4096 H4RG detector and better than 1 mK thermal stability supplies the long-term drift control, while a Fabry-Perot etalon calibrated with uranium-neon lines yields about 17,800 wavelength references across the Y, J, and H bands.

What would settle it

Observe a bright exoplanet-hosting M dwarf with NIRPS alone for several weeks and fit the RVs without imposing an external model; if the residuals remain below about 1 m/s and planet amplitudes match literature values, the precision claim is instrument-level. If residuals are larger or amplitudes differ, the 77 cm/s value is model-dependent. A companion check is a simultaneous HARPS-NIRPS series on one star, looking for an optical-to-NIR RV offset that drifts with telescope position or time.

Watch

Extended reading notes

Core claim

The paper's central claim is that the instrument meets its top-level requirement of 1 m/s radial-velocity precision in the near-infrared: the measured residual RMS against a published Keplerian-plus-activity model of Proxima is 0.77 m/s, the signature of Proxima b is recovered with a semi-amplitude near 1.24 m/s, and the spectrograph's intrinsic drift is only a few cm/s per day with a dispersion of 72 cm/s over five months. The paper also shows that the empirical radial-velocity content of M dwarfs in the Y, J, and H bands is about 1.7 to 2.5 times better than model-based estimates, implying a photon-noise floor near 1.7 m/s at signal-to-noise 100 in H. Additional claims include a peak throughput of 13 percent, successful telluric and OH-line removal, a water detection in a single transit of the hot Saturn WASP-127 b, and the first clear detection of solar p-mode oscillations with a near-infrared spectrograph using the solar feed HELIOS.

Load-bearing premise

The headline 77 cm/s precision assumes that the published ESPRESSO model of Proxima's planets and activity is correct and that NIRPS's wavelength scale and zero point match that model, because only a radial-velocity offset is fitted; if either assumption fails, the residual RMS is not purely NIRPS precision.

Editorial extensions

If this is right

  • M dwarf radial-velocity surveys can now be conducted in the near-infrared at the same precision as optical surveys, which is decisive for very red, faint, or active late-M stars.
  • Because HARPS and NIRPS observe simultaneously, each epoch can deliver radial velocities from 378 to 1920 nm, letting stellar activity be distinguished from planetary signals by its wavelength dependence.
  • The empirical radial-velocity content measurements imply that a 30-minute NIRPS exposure on a slow-rotating M4 dwarf reaches about 1 m/s photon noise at H magnitude 8.2, making small-planet detection around nearby M dwarfs efficient.
  • The single-transit water detection on WASP-127 b shows that NIRPS can perform high-resolution atmospheric spectroscopy competitively with longer-established near-infrared instruments.
  • The instrument's intrinsic drift is low enough that simultaneous Fabry-Perot reference observations are unnecessary, and OBJ-SKY mode is recommended instead.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the 77 cm/s Proxima residual survives a fully independent radial-velocity fit, NIRPS would be the first 3.6-m-class near-infrared spectrograph with sub-m/s precision, erasing the practical precision gap between optical and near-infrared work for late M dwarfs.
  • The installed but not yet routine laser frequency comb could push the wavelength solution below the current 55 cm/s in HE mode, making the modal-noise floor near S/N 230 the next testable limit on NIRPS radial velocities.
  • A direct testable extension is a simultaneous HARPS-plus-NIRPS campaign on a bright RV standard: if the optical-to-near-infrared RV difference drifts with telescope position or time, zero-point systematics are larger than the quoted single-instrument precision.
  • The empirical RV content relations for M dwarfs, if adopted by survey planners, would let exposure time be allocated from measured H-band S/N targets rather than model predictions, improving the completeness of small-planet searches.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. This paper presents the design, commissioning, and on-sky performance of NIRPS, the AO-assisted near-infrared spectrograph installed at the ESO 3.6-m telescope and operated simultaneously with HARPS. The authors report full YJH coverage from 972.4 to 1919.6 nm, resolving powers of about 90,000 (HA) and 75,000 (HE), a peak throughput of 13%, thermal stability at the millikelvin level, and an RV residual RMS of 0.77 m/s on Proxima relative to the ESPRESSO Keplerian-plus-GP model of Faria et al. (2022). They also characterize modal noise and its mitigation, empirically calibrate the RV photon-noise content of M dwarfs, demonstrate telluric and OH-line corrections, show solar p-mode detection with HELIOS, and present a single-transit water detection in WASP-127b. The paper concludes with the GTO programme and a set of community recommendations for observing modes.

Significance. If the reported performance is confirmed, NIRPS is a rare facility: it is the first AO-assisted, high-resolution, high-stability NIR spectrograph on a 3.6-m-class telescope with sub-m/s-class RV precision, and its simultaneous operation with HARPS provides continuous spectroscopic coverage from 378 nm to 1920 nm. The paper's strengths are its extensive multi-epoch calibration dataset, the explicit benchmarking against the independent ESPRESSO model, the use of two independent pipelines (NIRPS-DRS and APERO) with the LBL algorithm, the empirical RV-content analysis based on on-sky templates, and the HELIOS solar validation that clearly detects solar p-modes in the NIR. These elements make the instrument characterization unusually transparent and reproducible. The main caveat is that the headline 0.77 m/s number is a model-relative residual, not a raw instrument scatter, and its wording in the abstract should be tightened.

major comments (3)
  1. [Abstract and Section 5.4, Fig. 22] The 0.77 m/s value is the RMS of NIRPS-HE RVs about the ESPRESSO Keplerian-plus-GP model of Faria et al. (2022), with only a constant offset fitted, and the paper itself notes that the residuals are 'not a fit.' This makes 0.77 m/s an upper limit on the intrinsic NIRPS precision rather than a direct measurement: the residual includes the external model's errors, possible differences between optical and NIR activity tracers, and potential NIRPS-ESPRESSO zero-point or wavelength-scale systematics. The abstract's wording 'The RV precision ... is 77 cm/s' therefore overstates what is demonstrated. I recommend rewording to something like 'the residual RMS of NIRPS RVs around the independent ESPRESSO model is 0.77 m/s, consistent with photon noise,' and adding an in-situ validation of sub-m/s precision (for example, a short-timescale repeatability sequence on the HE fibre or an explicit statement that the 55 cm/s wavelength-solution floor is the relevant calibration limit). The figure caption should also state whether the quoted RMS is computed on individual exposures or on nightly binned points.
  2. [Section 5.1.4 vs. Section 5.4, Fig. 22] There is an internal tension between the modal-noise budget and the Proxima residual. Section 5.1.4 states that the residual modal noise should limit HE-mode RV precision to about 0.9 m/s (and HA to about 1.4 m/s) at the S/N reached for H~8-9 dwarfs in 30 minutes, while Fig. 22 reports a 0.77 m/s residual RMS for Proxima in HE mode. These two numbers cannot both be simple statements of the same precision limit. The paper should explicitly reconcile them, for example by explaining that the Proxima sequence has a different S/N or spectral content, or by stating that the 0.77 m/s value is partly set by the fixed external model rather than by NIRPS noise. This matters because both numbers are used to support the sub-m/s precision claim.
  3. [Sections 5.1.2 and 7] The current wavelength-solution precision is quoted as 55 cm/s in HE mode and 69 cm/s in HA mode, and Section 7 notes that the laser frequency comb is not yet operational. Since this calibration floor is comparable to both the 0.77 m/s Proxima residual and the 0.9 m/s modal-noise estimate, the paper should state clearly that the demonstrated on-sky precision is at present bounded by the wavelength-solution floor and the modal-noise budget, and should not present 0.77 m/s as the instrument's intrinsic, ultimate precision. This clarification is needed not only in the abstract but also in the conclusions, where 'close to 1 m/s' is the more defensible summary.
minor comments (5)
  1. [Abstract and Section 5.1.1] The abstract says the spectral range 'continuously covers' 972.4 to 1919.6 nm, but Section 5.1.1 and Table 2 show that echelle orders 104 and 105 (1376.5 to 1397.3 nm) are missing because of OH-doped absorption in the fibre train; please change 'continuously covers' to 'covers' or explicitly note the gap.
  2. [Section 5.3] The comparison of the empirical RV photon-noise floor with literature predictions should be made apples-to-apples; the quoted factors of 1.7-2.5 mix different S/N conventions, wavelength coverages, telluric masks, and stellar parameters (vsini, metallicity), so the reader cannot tell how much of the improvement is intrinsic to NIRPS and how much follows from different assumptions. A short table listing the assumptions would remove the ambiguity.
  3. [Section 5.1.2 vs. Section 7] The long-term drift is reported as 4.1 cm/s/day (HA) and 3.4 cm/s/day (HE) in Section 5.1.2, but Section 7 quotes a 'typical drift of 0.1 m/s/day'; this is a factor of 2.5-3 larger and should be harmonized.
  4. [Section 5.6] The WASP-127b water detection is from a single transit and the reported 4-5 sigma is obtained after optimizing the PCA and telluric-masking parameters; the text already notes the sensitivity to parameters, but the conclusions should state more explicitly that this is a demonstration of capability rather than a confirmed detection.
  5. [References] Several references still use bracketed placeholders or 'submitted' status (e.g., Allart et al. 2025, Suárez Mascareño et al. 2025, Vaulato et al. 2025, Bazinet et al. 2025); these should be updated to the final journal citations before publication.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the headline precision claim is an external benchmark residual, not a fitted prediction.

full rationale

The paper's central quantitative claims are direct measurements benchmarked against external references. The abstract's 77 cm/s RV precision is the RMS residual of NIRPS-HE Proxima RVs about the Faria et al. (2022) ESPRESSO Keplerian-plus-GP model, with only a constant RV offset fit (Sec. 5.4, Fig. 22: 'the residuals of the ESPRESSO model (not a fit) are below the 1 m s−1'). The model parameters are constrained by ESPRESSO data, not by NIRPS RVs, so the residual is not a quantity defined by the paper's own inputs. The throughput measurement (Sec. 5.1.3) divides HR1544 spectra by a CRIRES/CTIO standard-star model, again an external reference. The empirical RV-content curves (Sec. 5.3) are compared with published theoretical predictions (Artigau et al. 2018a, Figueira et al. 2016, Reiners & Zechmeister 2020) rather than being used to generate those predictions. No step derives a 'predicted' quantity from a parameter fitted to that same quantity, and no load-bearing uniqueness theorem is imported from the authors' prior work. Internal citations to design papers (Wildi et al. 2022; Blind et al. 2022; Frensch et al. 2022) document engineering heritage and are not the evidential basis for the measured on-sky performance. The only minor self-referential element is that the Faria et al. (2022) Proxima model has overlapping authorship with the NIRPS consortium, but that does not make the benchmark circular because the model is an independent ESPRESSO-based product and only the offset is adjusted for NIRPS. The 0.77 m/s figure is therefore a legitimate consistency check, though its interpretation as the instrument's intrinsic precision is a correctness consideration, not a circularity one.

Assumptions & free parameters 3 free parameters · 3 assumptions · 0 invented entities

The paper's central performance claims are empirical measurements; the ledger captures the external references (ESPRESSO model, CRIRES model) and hand-tuned settings (AO scan amplitude, telluric masking, PCA removal) that the quoted numbers rely on. No invented entities or new physical constants are introduced.

free parameters (3)
  • AO scanning amplitude = 0.1 arcsec (HA), 0.2 arcsec (HE)
    Hand-tuned in Section 5.1.4 to compromise between modal noise reduction and flux loss; affects the modal noise residuals and thus the effective S/N limits quoted.
  • WASP-127b telluric masking and PCA parameters = Telluric mask 70% transmission, wings to 90%; 4 PCs removed
    Optimized in Section 5.6 to maximize the water CCF detection; the paper notes the detection is robust across a wide range, but the headline 4-5 sigma is conditioned on these choices.
  • Empirical RV photon-noise calibration (Fig. 20) = 1.7 m/s at S/N=100 in H (YJH); 1 m/s at S/N~170 for slow M4; 1 m/s in 30 min for H=8.2
    Fit to NIRPS commissioning data in Section 5.3; used to state achievable RV precision as a function of magnitude, so the quoted capabilities depend on this empirical fit.
assumptions (3)
  • domain assumption The ESPRESSO Keplerian plus activity model of Proxima (Faria et al. 2022) accurately describes Proxima's RVs; residuals of NIRPS RVs relative to it measure NIRPS precision.
    Load-bearing for the 77 cm/s claim in Section 5.4; if the model is biased, the quoted precision is not established.
  • domain assumption The CRIRES/CTIO spectrophotometric model for HR1544 provides accurate absolute flux calibration for the on-sky throughput measurement.
    Load-bearing for the 13% peak throughput claim in Section 5.1.3.
  • standard math Poisson statistics and the cross-correlation/line-by-line RV frameworks (Bouchy et al. 2001; Artigau et al. 2022) correctly convert S/N to RV precision for M dwarfs.
    Used throughout Section 5.3 to define RV photon-noise floors; a standard, well-tested assumption.

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Cite this review

Pith. "Pith review of NIRPS joining HARPS at ESO 3.6 m. On-sky performance and science objectives." pith.science (2026). https://pith.science/paper/Q5CKAI6C

@misc{pith2026250721767,
  author       = {Pith},
  title        = {Pith review of: NIRPS joining HARPS at ESO 3.6 m. On-sky performance and science objectives},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/Q5CKAI6C}},
  note         = {Machine review of arXiv:2507.21767}
}
read the original abstract

The Near-InfraRed Planet Searcher (NIRPS) is a high-resolution, high-stability near-infrared (NIR) spectrograph equipped with an AO system. Installed on the ESO 3.6-m telescope, it was developed to enable radial velocity (RV) measurements of low-mass exoplanets around M dwarfs and to characterise exoplanet atmospheres in the NIR. This paper provides a comprehensive design overview and characterisation of the NIRPS instrument, reporting on its on-sky performance, and presenting its GTO programme. The instrument started its operations on 1 Apr 2023 after intensive on-sky testing phases. The spectral range continuously covers the Y, J, and H bands from 972.4 to 1919.6 nm. The thermal control system maintains 1 mK stability over several months. The NIRPS AO-assisted fibre link improves coupling efficiency and offers a unique high-angular resolution capability with a fibre acceptance of only 0.4 arcsec. A high spectral resolving power of 90 000 and 75 000 is provided in HA and HE modes, respectively. The overall throughput from the top of the atmosphere to the detector peaks at 13 percent. The RV precision, measured on the bright star Proxima with a known exoplanetary system, is 77 cm/s. NIRPS and HARPS can be used simultaneously, offering unprecedented spectral coverage for spectroscopic characterisation and stellar activity mitigation. Modal noise can be aptly mitigated by the implementation of fibre stretchers and AO scanning mode. Initial results confirm that NIRPS opens new possibilities for RV measurements, stellar characterisation, and exoplanet atmosphere studies with high precision and high spectral fidelity. NIRPS demonstrated stable RV precision at the level of 1 m/s over several weeks. The instrument high throughput offers a notable improvement over previous spectrographs, enhancing our ability to detect small exoplanets.

Figures

Figures reproduced from arXiv: 2507.21767 by the authors.

Figure 1
Figure 1. Schematic view of optical design and layout of the NIRPS front end and its components NIRPS is specifically a conjugate AO-assisted instrument, allowing for the main fibre (so-called high-accuracy fibres, HA) to be only 0.4′′ in diameter on the sky and for the spectrograph to be much more compact than seeing-limited instruments. A larger fibre (high-efficiency fibre, HE) with a field of view (FoV) of Article number,… view at source ↗
Figure 2
Figure 2. [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. NIRPS adaptive optics performance measured during commis￾sioning #4. Top: Encircled energy for 0.5′′ and 0.9′′ and Strehl versus Imag. Dot size is proportional to Fried parameter, r0, corresponding to seeing ranging from 2.2′′ to 0.7′′˙(Bottom) Encircled energy for 0.5′′ and 0.9′′ and Strehl versus seeing from the AOP telemetry. Dot symbol size is proportional to the I mag. The guiding camera uses a NIR InGaAs camer… view at source ↗
Figures from the paper (23 more)
Figure 4
Figure 4. Figure 4: Schematic view of the optical design and layout of the NIRPS spectrograph and its components. The initial echelle grating manufactured by Bach (76◦ blaze angle, with 13.333 lines/mm and efficiency >55%.) used up to Commissioning #5 was a traditional grating ruled in a …
Figure 5
Figure 5. Figure 5: Raw frame of NIRPS with HE_A fibre illuminated by the Tung￾sten lamp showing the spectral format with the location of the 71 de￾tected spectral orders. Spectral orders are numbered with their locali￾sation order (from 1 to 71), physical diffraction order (from 148 to 7…
Figure 6
Figure 6. Figure 6: Top panel: Full extracted and wavelength calibrated spectrum with NIRPS-DRS of Proxima observed in HE mode. (4 Bottom panels) Zoom in on four different spectral domains. Blue curves and orange curves correspond to telluric uncorrected and telluric corrected spectra, re…
Figure 9
Figure 9. Figure 9: shows the intrinsic drift of the instrument mea￾sured on the UrNe lines over five months. The typical drift is of 4.1 cm s−1 /day and 3.4 cm s−1 /day in HA and HE mode, re￾spectively. The dispersion after removing the long-term linear drift is 72 cm s−1 and 64 cm s−1 f…
Figure 10
Figure 10. Figure 10: Relative temperature changes of the grating and prism mounts from April 2023 to Sept 2023. The mean temperature value is 75.16 K and 75.37 K for the grating and prism, respectively. The outliers and jumps are due to short power cuts. tively. With such high intrinsic s…
Figure 8
Figure 8. Figure 8 [PITH_FULL_IMAGE:figures/full_fig_p012_8.png]
Figure 11
Figure 11. Figure 11: Relative flat-field stability over one month as a function of spec￾tral orders for the four NIRPS fibres. scale with wavelength. The slight increase of dispersion around 1.38 µm (orders 42-43-44) and above 1.81 µm (above order 67) is due to water absorption lines visi…
Figure 13
Figure 13. Figure 13: shows the RV drift measured on the FP-FP sequence overtendays using HE mode. The first exposure on 2023 June 12 is taken as reference and RV drifts are measured relative to this reference. On fibre HE_A the overall measured drift presents modulation at the level of ±3…
Figure 14
Figure 14. Figure 14: Expected overall throughput of NIRPS instruments for HA mode and different I magnitude for a 0.9′′ seeing. The dark blue, green, and orange curves correspond to the overall throughput for I of 10, 11 and 12, respectively. The dashed curve represents the atmospheric ab…
Figure 16
Figure 16. Figure 16: shows the S/N results obtained at 1611 nm (H band) in an extracted-pixel bin of 5.4 nm (1.00 km s−1 ) as a function of target magnitude after renormalisation to an exposure time of five min for bright stars (H < 9) and 15 min for fainter stars. S/N was measured during…
Figure 17
Figure 17. Figure 17: Near-field images of the 29-µm octagonal HA fibre (left) and the 33×132 µm rectangular HE fibre (right) illuminated with a 1.55 µm laser and the diffraction limited PSF of the front end. No fibre stretch￾ing nor AO scanning are applied. The pixel size on these images …
Figure 19
Figure 19. Figure 19: RV accuracy as function of effective temperature achievable with an S/N of 100 in Y, J and H bands for M dwarfs having high-S/N empirical spectral templates from NIRPS HE observations. The RV accuracy obtained by combining all three bands is expressed for an S/N=100 i…
Figure 20
Figure 20. Figure 20: Estimated RV photon-noise rescaled to a 30 min exposure for M dwarfs observed during the commissioning and the first year of op￾eration as a function of H magnitude. Black and red lines correspond to empirical relationships for the RV uncertainty obtained with NIRPS-H…
Figure 22
Figure 22. Figure 22: Proxima b Keplerian motion observed with NIRPS during com￾missioning with stellar activity and Proxima d signals removed. The residuals of the ESPRESSO model (not a fit) are below 1 m s−1 . The ex￾posure time is 3×200 s. The estimated photon-noise is 0.8 m s−1 . White…
Figure 21
Figure 21. Figure 21: Proxima sequence with NIRPS (HE) over two commissioning phases (#8 and #9) separated by about 40 days. The Keplerian compo￾nents (Proxima b and d) and activity GP model are taken from Faria et al. (2022) derived from ESPRESSO/VLT measurements. White dots correspond to…
Figure 25
Figure 25. Figure 25: RVs obtained for TOI-406 phase-folded to the 13.176 days of the sub-Neptunes TOI-406 b. The dispersion of the residuals is 3.4 m s−1 and 5.1 m s−1 for NIRPS and HARPS, respectively. telescope focuses the disk-integrated Sun’s light onto an inte￾grating sphere and feed…
Figure 24
Figure 24. Figure 24: RV sequence of α Cen B obtained on 12 March 2023 on lasting 68 min. The dispersion is 0.85 m s−1 with a binning of three minutes. the residuals is 3.4 m s−1 and 5.1 m s−1 for NIRPS and HARPS, respectively. The detection of the inner 1.3 R⊕ super-Earth is not significa…
Figure 27
Figure 27. Figure 27: shows the power spectral density of the HELIOS RV se￾quence. The dashed vertical line shows the central frequency of the oscillation bump at 3.16 mHz, as obtained from HARPS￾HELIOS RVs analysed in Al Moulla et al. (2023). NIRPS-HELIOS commissioning data were also used…
Figure 26
Figure 26. Figure 26: Top: one-hour sequence of simultaneous NIRPS, HARPS (both taken with HELIOS) and BISON RVs of the disk-integrated Sun’s light showing the 5-mn acoustic oscillations, shown from top to bottom. The data were taken on January the 26th 2023. Bottom: Power spectral den￾sit…
Figure 28
Figure 28. Figure 28: Full additional reduction steps and transmission spectra com￾putation from STARSHIPS for telluric lines below 70% transmission masked up to 90% transmission in their wings and four PCs removed for the echelle spectral order 86 with the NIRPS-DRS data products. Top: Si…
Figure 29
Figure 29. Figure 29: 2D CCF detection maps (top) for water absorption in the atmosphere of WASP-127 b, along with a 1D CCF curve (bottom) corresponding to a slice of the map at the known planetary Kp (horizontal line in the top panels). Left: APERO DRS reduction. Right: NIRPS DRS reductio…
Figure 30
Figure 30. Figure 30: Effective temperature as a function of the distance of the SP1 selected sample colour-coded as a function of their H magnitude. Grey dots correspond to known exoplanets around cool stars (< 4500 K). ical evolution. Once again, the ability to filter out the effects of …
Figure 32
Figure 32. Figure 32: Exoplanet population in a mass-irradiation diagram. SP3 targets are highlighted with a colour code linked to the different sub-programmes. COMPASS investigates the frequency of mutually￾misaligned small planets and has overlaps with other sub-programmes. gap between o…

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