# Homogeneous search for helium in the atmosphere of 11 gas giant exoplanets with SPIRou

R. Allart, P.-B. Lemée-Joliecoeur, A. Jaziri, D. Lafrenière, E. Artigau, N.

Cook, A. Darveau-Bernier, L. Dang, C. Cadieux, A. Boucher, et al.

► To cite this version:

R. Allart, P.-B. Lemée-Joliecoeur, A. Jaziri, D. Lafrenière, E. Artigau, et al. Homogeneous search for helium in the atmosphere of 11 gas giant exoplanets with SPIRou. Astronomy & Astrophysics - A&A, 2023, 677, pp.A164. 10.1051/0004-6361/202245832. hal-04252137

HAL Id: hal-04252137

https://hal.science/hal-04252137v1

Submitted on 26 Oct 2023

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# Homogeneous search for helium in the atmosphere of 11 gas giant exoplanets with SPIRou

R. Allart¹,*, P.-B. Lemée-Joliecoeur¹, A. Y. Jaziri², D. Lafrenière¹, E. Artigau¹, N. Cook¹,

A. Darveau-Bernier¹, L. Dang¹,**, C. Cadieux¹, A. Boucher¹, V. Bourrier², E. K. Deibert³, S. Pelletier¹,
M. Radica¹, B. Benneke¹, A. Carmona⁴, R. Cloutier⁵, N. B. Cowan⁶,⁷, X. Delfosse⁴, J.-F. Donati⁸,
R. Doyon¹, P. Figueira², T. Forveille⁴, P. Fouqué⁸, E. Gaidos⁹, P.-G. Gu¹⁰, G. Hébrard¹¹,¹², F. Kiefer¹³,
Á. Kóspál¹⁴,¹⁵,¹⁶,¹⁷, R. Jayawardhana¹⁸, E. Martioli¹⁹,¹¹, L. A. Dos Santos²⁰, H. Shang²¹,
J. D. Turner²²,****, and A. A. Vidotto²³

*(Affiliations can be found after the references)*

Received 31 December 2022 / Accepted 22 June 2023

## ABSTRACT

The metastable helium triplet in the near-infrared (10 833 Å) is among the most important probes of exoplanet atmospheres. It can trace their extended outer layers and constrain mass loss. We used the near-infrared high-resolution spectropolarimeter SPIRou on the CFHT to search for the spectrally resolved helium triplet in the atmospheres of eleven exoplanets, ranging from warm mini-Neptunes to hot Jupiters and orbiting G, K, and M dwarfs. Observations were obtained as part of the SPIRou Legacy Survey and complementary open-time programs. We applied a homogeneous data reduction to all datasets and set constraints on the presence of metastable helium, despite the presence of systematics in the data. We confirm published detections for HAT-P-11 b, HD 189733 b, and WASP-69 b and set upper limits for the other planets. We applied the p-winds open source code to set upper limits on the mass-loss rate for the nondetections and to constrain the thermosphere temperature, mass-loss rate, line-of-sight velocity, and the altitude of the thermosphere for the detections. We confirm that the presence of metastable helium correlates with the stellar mass and the extreme-ultraviolet flux received by the planets. We investigated the correlation between the mass-loss rate and the presence of metastable helium, but it remains difficult to draw definitive conclusions. Finally, some of our results are in contradiction with previous results in the literature, and therefore we stress the importance of repeatable, homogeneous, and larger-scale analyses of the helium triplet to obtain robust statistics, study temporal variability, and better understand how the helium triplet can be used to explore the evolution of exoplanets.

**Key words.** planets and satellites: atmospheres – planets and satellites: gaseous planets – infrared: planetary systems – instrumentation: spectrographs – techniques: spectroscopic – methods: observational

## 1. Introduction

Through their lifetime, exoplanets might undergo several physical processes that can alter their compositions, masses, and sizes. Being the outer envelope of exoplanets, atmospheres are excellent windows onto the exoplanets and particularly subject to their evolution (be it impinging radiation, mass loss, etc.). The atmospheres of close-in gas giant planets hydrodynamically expand under the absorption of stellar irradiation (e.g., Vidal-Madjar et al. 2003; Lammer et al. 2003) and, in extreme conditions, they can evaporate and be stripped away from the planet core (Bourrier et al. 2018; Owen & Lai 2018). Such atmospheric changes could happen in the early stage of the system (100 Myr-1 Gyr, Owen 2019; Johnstone et al. 2021; King & Wheatley 2021), in particular, once the gaseous protoplanetary disk has been dissipated and the planet is directly irradiated by the central star for planets that either formed in situ (Batygin et al. 2016; Matsumoto et al. 2021) or during their disk-driven inward migrations (e.g., Ida & Lin 2008). Under such intense irradiation, Neptune-sized

planets could be unable to retain their gaseous envelopes and could even become bare cores due to their lower initial mass. This is consistent with the observed lack of close-in hot Neptunes (Fig. 1), commonly called the Neptunian or the evaporation desert (e.g., Lecavelier Des Étangs 2007; Beaugé & Nesvorný 2013; Mazeh et al. 2016; Owen 2019). Another explanation for the lack of hot Neptunes can be found via the high-eccentricity migration scenario (e.g., Rasio & Ford 1996; Ford & Rasio 2008; Owen & Lai 2018). This scenario can bring some Neptunes to large orbital distances and delay their migration, and therefore it can protect them from evaporation. Alternatively, high-eccentricity migration can also bring some Neptunes closer to their host stars, and possibly disrupt them through stellar tides. Finally, the planets initially in the Neptune desert can migrate away through tidal and magnetic interactions with their host stars (Ahuir et al. 2021). Hence, one way to test these theories requires measuring the planet's stability against photoevaporation through mass-loss rate measurements for a large exoplanet population to derive statistical conclusions.

The ongoing evaporation of exoplanetary atmospheres was first observed through the hydrogen Lyman-α line at ultraviolet (UV) wavelengths for several hot Jupiters

<footnote>* Trottier Postdoctoral Fellow.</footnote>

<footnote>** Banting Postdoctoral Fellow.</footnote>

<footnote>*** NHFP Sagan Fellow.</footnote>
<figure><img src="image_2.png" /><figcaption>**Fig. 1.** Planetary mass-irradiation diagram of the exoplanet population with the studied SPIRou targets highlighted as black squares. The blues dots is the exoplanet population from the NASA exoplanet Archive (December 23rd 2022).</figcaption></figure>

(e.g., Vidal-Madjar et al. 2003; Lecavelier Des Étangs et al. 2012; Bourrier et al. 2013) and warm Neptunes (Ehrenreich et al. 2015; Bourrier et al. 2018; Ben-Jaffel et al. 2022). However, the interstellar medium (ISM), the geocoronal emission, and the lack of stellar continuum limit the use of the Ly-α line, only observable from space, to measure the exoplanet mass-loss rate.

The near-infrared helium triplet, predicted earlier on by Seager & Sasselov (2000; see also Oklopčić & Hirata 2018), has recently been discovered (Spake et al. 2018) and has since been used to study the upper layers of the exoplanet atmosphere from the thermosphere to the exosphere. The exosphere is the outermost atmospheric layer of an exoplanet and is no longer gravitationally bound to it. Ground-based near-infrared high-resolution spectrographs (e.g., CARMENES, GIANO, NIRPSEC, or SPIRou) have led to several unambiguous spec- trally and temporally resolved detections (e.g., Allart et al. 2018, 2019; Nortmann et al. 2018; Salz et al. 2018; Alonso-Floriano et al. 2019b; Kirk et al. 2020; Guilluy et al. 2020; Spake et al. 2021a; Zhang et al. 2022b,a; Czesla et al. 2022), highlighting the use of the helium triplet as a robust atmospheric tracer. In addition, low-resolution observations have confirmed and detected helium signatures (e.g., Spake et al. 2018; Mansfield et al. 2018; Vissapragada et al. 2020; Paragas et al. 2021; Fu et al. 2022). Most of these detections were obtained for planets orbiting K dwarfs, which favor the presence of helium particles in their metastable state in exoplanet atmospheres due to their higher extreme-ultraviolet (XUV) and lower mid-ultraviolet flux (Oklopčić 2019). This is also in agreement with several nonde- tections for planets orbiting around stars of other spectral types (e.g., Kasper et al. 2020; Casasayas-Barris et al. 2021; Fossati et al. 2022).

In addition to being a powerful atmospheric tracer, the helium triplet is weakly (or not) affected by the ISM absorption (Indriolo et al. 2009), the Rossiter-McLaughlin effect, the center-to-limb variation, or by stellar activity (Cauley et al. 2018). Therefore, measuring these transitions has yielded estimates of the mass-loss rate of tens of exoplanets orbiting K dwarfs. However, the disparateness in the instruments, data reduction pipelines, transmission spectrum extractions, data reproducibil- ity, and modeling framework have prevented homogeneous anal- yses thus far. Although, homogenous analyses have been carried out for a small number of exoplanets (e.g., Kasper et al. 2020;

Vissapragada et al. 2022b; Zhang et al. 2023), we provide the largest homogeneous analysis of the helium triplet in the atmosphere of eleven exoplanets observed with SPIRou.

We describe the instrument and the observations in Sect. 2, then detail the methods used in Sect. 3. Section 4 presents the helium analysis for each planet, while Sect. 6 discusses the gen- eral trends that can be drawn from this sample. We conclude in Sect. 7.

## 2. Observations

SPIRou (SPectromètre InfraROUge, Donati et al. 2020) is a fiber-fed near-infrared (0.98–2.51 µm) echelle spectro-polarimeter installed on the 3.6 m Canada France Hawaii Tele-scope in Maunakea (CFHT). It has a high spectral resolution of 70 000 with 1.9 pixels per resolution element and a pixel sam- pling of 2.3 km·s⁻¹. SPIRou is fed by three fibers: fibers A and B for science with orthogonal polarization and fiber C for ref- erence. SPIRou was already used for atmospheric studies (e.g., Boucher et al. 2021; Pelletier et al. 2021), which reported the presence of non white noise instrumental systematics that might be associated to modal noise for example (Oliva et al. 2019). Data reduction and analysis are described in Sect. 3.

Transit datasets of 13 exoplanets have been collected with SPIRou as part of the SPIRou Legacy Survey (SLS, PI: Donati) and various programs obtained through Canadian open time or collaborations (namely AU Mic b, GJ1214 b, GJ3470 b, HAT-P-11 b, HD1897333 b, K2-25 b, TOI-1728 b WASP-11 b, WASP-39 b, WASP-52 b, WASP-69 b, WASP-80 b, and WASP-127 b). The polarimetry mode was used for the datasets collected on 2019 June 17 for AU Mic b, 2019 February 18 for GJ 3470 b, and 2020 July 03, 2020 July 05, 2020 July 25, and 2021 July 24 for HD 189733 b. However, we used the extracted data in the AB mode such that we do not differentiate between polarization (see Sect. 3.1 and Cook et al. 2022). We discard K2-25b (19BP40, PI: Donati) due to the very low signal-to-noise ratio (S/N) obtained for each exposure and TOI-1728b (21BC14, PI: Allart) due to a mismatch of the transit window. Figure 1 highlights the targets observed with SPIRou in a planetary mass-irradiation diagram. The sample is mainly composed of hot to warm Jupiters (7) with some warm Neptunes (2), and mini-Neptunes (2) spanning a broad range of stellar ages and orbiting mainly K and M-type stars. We summarize the observational conditions (i.e., S/N, seeing, and airmass) during planetary transits in Table 1. We note that due to CFHT scheduling constraints for SPIRou and different program strategies, it was not possible to gather more than one transit for some targets, limiting the reproducibility of the results.

## 3. Methods

### 3.1. Data reduction, spectral extraction, and telluric correction

All data were reduced using A PipelinE to Reduce Observa-tions (APERO; version 0.7.179; Cook et al. 2022), the standard SPIRou data reduction software. APERO performs all calibra-tions and pre-processing to remove detector effects including dark, bad pixel, background, and performs detector nonlinear- ity corrections (Artigau et al. 2018), localization of the orders, geometric changes in the image plane, correction of the flat and blaze, hot pixel and cosmic ray correction, wavelength calibra-tion (using both a hollow-cathode UNe lamp and the Fabry-Pérot étalon; Hobson et al. 2021), and removal of diffuse light from the reference fiber leaking into the science channels (when a Fabry-Pérot is used simultaneously in the reference fiber). This
<table><caption>**Table 1.** Observations summary.</caption><thead><tr><th>Target</th><th>Program ID</th><th>PI</th><th>UT date</th><th>S/N</th><th>Seeing</th><th>Airmass</th><th>t<sub>exp</sub> (s)</th><th>N<sub>exp</sub></th><th>Partial transit</th></tr></thead><tbody><tr><td>AU Mic b</td><td>19AP42</td><td>Donati</td><td>2019-06-17</td><td>57-91-105</td><td>0.5-0.8-1.7</td><td>1.6-1.7-2.9</td><td>122.6</td><td>116</td><td>No</td></tr><tr><td>GJ1214 b</td><td>20AP40</td><td>Donati</td><td>2020-05-14</td><td>8-9-11</td><td>-</td><td>1.1-1.2-1.4</td><td>250.7</td><td>30</td><td>No</td></tr><tr><td>GJ3470 b</td><td>19AP40</td><td>Donati</td><td>2019-02-18</td><td>17-21-25</td><td>-</td><td>1.0-1.1-1.5</td><td>434.6</td><td>32</td><td>No</td></tr><tr><td></td><td>21BP40</td><td>Donati</td><td>2021-12-15</td><td>24-38-42</td><td>0.5-0.7-1.4</td><td>1.0-1.2-2.1</td><td>300.9</td><td>43</td><td>No</td></tr><tr><td>HAT-P-11 b</td><td>21BC09</td><td>Radica</td><td>2021-08-13</td><td>98-107-111</td><td>0.2-0.3-0.8</td><td>1.1-1.2-1.3</td><td>323.2</td><td>44</td><td>No</td></tr><tr><td></td><td>21BF19</td><td>Debras</td><td>2021-08-18</td><td>69-87-96</td><td>0.7-1.0-1.4</td><td>1.1-1.2-1.6</td><td>284.2</td><td>46</td><td>No</td></tr><tr><td>HD189733 b</td><td>21BC09</td><td>Donati</td><td>2018-09-22</td><td>112-120-126</td><td>0.4-0.5-0.6</td><td>1.0-1.1-1.3</td><td>250.7</td><td>36</td><td>No</td></tr><tr><td></td><td>19AP40</td><td>Donati</td><td>2019-06-15</td><td>84-114-125</td><td>0.4-0.7-0.9</td><td>1.0-1.0-1.1</td><td>250.7</td><td>50</td><td>No</td></tr><tr><td></td><td>20AC01</td><td>Deibert</td><td>2020-07-03</td><td>12-94-99</td><td>0.4-0.5-0.7</td><td>1.1-1.2-1.4</td><td>50.1</td><td>56</td><td>Yes</td></tr><tr><td></td><td>20AC01</td><td>Deibert</td><td>2020-07-05</td><td>41-63-83</td><td>-</td><td>1.0-1.0-1.1</td><td>94.7</td><td>52</td><td>Yes</td></tr><tr><td></td><td>20AC01</td><td>Deibert</td><td>2020-07-25</td><td>42-78-92</td><td>-</td><td>1.0-1.2-2.1</td><td>94.7</td><td>124</td><td>No</td></tr><tr><td></td><td>21BC16</td><td>Deibert</td><td>2021-08-24</td><td>77-104-118</td><td>0.5-0.7-1.0</td><td>1.0-1.0-1.3</td><td>94.7</td><td>108</td><td>No</td></tr><tr><td>WASP-11 b</td><td>19BC08</td><td>Boucher</td><td>2019-10-08</td><td>15-17-18</td><td>-</td><td>1.0-1.1-1.3</td><td>601.8</td><td>30</td><td>No</td></tr><tr><td>WASP-39 b</td><td>22AC30</td><td>Pelletier</td><td>2022-06-04</td><td>9-10-12</td><td>0.4-0.7-0.9</td><td>1.1-1.1-1.0</td><td>300.9</td><td>46</td><td>No</td></tr><tr><td></td><td>22AC30</td><td>Pelletier</td><td>2022-06-08</td><td>9-12-14</td><td>0.3-0.4-0.7</td><td>1.1-1.1-1.3</td><td>300.9</td><td>46</td><td>No</td></tr><tr><td>WASP-52 b</td><td>19BC07</td><td>Boucher</td><td>2019-10-15</td><td>7-9-12</td><td>-</td><td>1.0-1.0-1.2</td><td>685.3</td><td>18</td><td>No</td></tr><tr><td></td><td>19BC07</td><td>Boucher</td><td>2019-11-05</td><td>10-13-14</td><td>0.2-0.3-0.5</td><td>1.0-1.0-1.3</td><td>685.3</td><td>18</td><td>No</td></tr><tr><td>WASP-69 b</td><td>19BP40</td><td>Donati</td><td>2019-10-13</td><td>7-20-26</td><td>0.5-0.7-1.4</td><td>1.1-1.3-2.2</td><td>122.6</td><td>93</td><td>No</td></tr><tr><td>WASP-80 b</td><td>19BP40</td><td>Donati</td><td>2019-10-07</td><td>10-12-13</td><td>-</td><td>1.1-1.1-1.7</td><td>183.9</td><td>74</td><td>No</td></tr><tr><td>WASP-127 b</td><td>20AP42</td><td>Donati</td><td>2020-03-11</td><td>22-26-28</td><td>-</td><td>1.1-1.1-1.5</td><td>300.9</td><td>50</td><td>No</td></tr><tr><td></td><td>21AC02</td><td>Boucher</td><td>2021-03-22</td><td>32-51-56</td><td>-</td><td>1.1-1.2-1.8</td><td>373.3</td><td>28</td><td>Yes</td></tr><tr><td></td><td>21AC02</td><td>Boucher</td><td>2021-05-03</td><td>14-36-62</td><td>0.3-0.4-0.6</td><td>1.1-1.1-1.5</td><td>501.5</td><td>28</td><td>Yes</td></tr></tbody></table>

**Notes.** S/N, Seeing, and Airmass values are given as the minimum-median-maximum values of each night. The S/N values are for the echelle order 71, where the helium lines are. Some seeing values are missing due to the lack of measurements. Partial transits are defined as transit with more than a fourth is missing.

is done using a combination of daily calibrations and reference calibrations. The result is an optimally extracted spectrum of dimensions 4088 pixels (4096 minus 8 reference pixels) with 49 orders, referred to as extracted 2D spectra; E2DS. While the E2DS are produced for the two science fibers (A and B) and the combined flux in the science fibers (AB), we only used the AB extraction as this is the relevant data product for nonpolarimetric observations.

APER0 also provides telluric-corrected versions of the spectra (Artigau et al., in prep.) from both the absorption and emission of the Earth's atmosphere. The telluric absorption line correction done in APER0 is a two-step process and is briefly outlined here. First, the extracted spectra of both science targets and a large set of rapidly rotating hot stars are fitted with an Earth's transmittance model from TAPAS (Bertaux et al. 2014) that leaves percent-level residuals. Then, from the ensemble of hot star observations, APER0 derives a correction model for the residuals with three components for each pixel (optical depths for water, non-water absorbing components, and a constant). This residual model is adjusted to each science observation according to the optical depth of each component from the TAPAS fit. The resulting correction leaves residuals at the level of the PCA-based method of Artigau et al. (2014), but has the advantage of simplicity and that any spurious point in the data will result in a local error rather than affecting the transmission globally as for a PCA analysis. Finally, a reconstruction of the telluric spectrum is derived using the fitted TAPAS template and the residuals model, for each observed spectrum. The pipeline performs the telluric absorption correction for lines with a transmission down to ~10% (i.e., with relative depths of 90% with respect to the continuum), with deeper lines being masked out<fnref n="1" />. SPIRou does

not include a simultaneous sky fiber, so the sky emission correction is done through a high-signal-to-noise ration (S/N) sky library. A large library of sky spectra has been obtained through the life of the instrument and, from it, a PCA decomposition has been performed. The first 9 components of the sky spectra are fitted to the science data. To avoid subtracting the continuum of stars, this is done through a fit of the derivative of the flux rather than the flux. As sky emission lines are very narrow and have no correspondence in the stellar spectrum, this derivative-fitting is not biased systematically. However, the OH emission lines surrounding the metastable helium triplet are not well modeled and, therefore, not well corrected (residuals up to a few percent) in comparison to the other sky emission lines in the SPIRou spectral range. As described in Oliva et al. (2015) and Czesla et al. (2022), the OH lines around the He triplet are composed of two doublets: 10 834.3338 Å ([5-2]Q1e) with 10 832.412 Å ([5-2]Q2e) and 10 834.241 Å ([5-2]Q1f) with 10 832.103 Å ([5-2]Q2f). The Q1-branch transition lines are the strongest and cannot be distinguished from each other. We, therefore, model these lines as three Gaussians with fixed positions, an amplitude ratio between the Q1 and Q2 lines of 0.0482, a free amplitude and full width at half maximum (FWHM) for the strongest unresolved Q1 lines, and fixed FWHM for the Q2 lines at the element resolution. This model is fitted to the reconstructed sky emission spectra of APER0 and then a linear minimization of this best fit with a stellar template is applied for each stellar spectrum. The telluric correction can be seen in Fig. A.1.

## 3.2. Data analysis

We follow standard data analysis procedures for studies of exoplanet atmospheres at high resolution as described in detail for

<footnote n="1">¹ In the spectral order of interest, there are no such deep lines.</footnote>
example in Wyttenbach et al. (2015), Casasayas-Barris et al. (2017), Allart et al. (2018, 2019) or Seidel et al. (2020).

Once the stellar spectra are extracted and telluric corrected, we focus our analysis on echelle order 71 (10 639–10 976 Å), where the helium triplet falls at the top of the blaze function. The spectra are moved to the stellar rest frame using the systemic velocity measured by the line-by-line (LBL, Artigau et al. 2022) code, normalized using the median flux in two bands (10 823–10 826 Å and 10 839–10 842 Å), and remaining outliers (e.g., cosmic rays) are sigma replaced following Allart et al. (2017). Spectra obtained before and after transit, hereafter called out-of-transit spectra, are averaged to create a reference master-out spectrum. Figure A.1 displays the master out for each night of each star before and after applying the telluric correction.

### 3.2.1. Transmission spectrum

To remove stellar features and obtain a transmission spectroscopy map, we divide each spectrum of the time series by the master out. Figure B.1 displays the transmission spectroscopy map for each night of each planet in the stellar rest frame. They are then Doppler-shifted to the planet rest frame based on the parameters in Tables 2 and 3. Figure 2 shows the transmission spectroscopy map in the planet rest frame for each planet, but averaged over the multiple transits. Partial transits will contribute only to the phases where data were collected. The 1-dimensional transmission spectrum is computed for each night as the average of the transmission spectroscopy map weighted by a modeled white light curve (Allart et al. 2019; Mounzer et al. 2022). The batman (Kreidberg 2015) package was used to model the white light curve with the parameters from Tables 2 and 3, where the quadratic linear limb darkening coefficient have been estimated in the J-band with the EXOFAST (Eastman et al. 2013) code based on the tables of Claret & Bloemen (2011). This scaling is necessary to properly take into account the true contribution of the ingress and egress spectra into the transit average transmission spectrum. Finally, and for a given planet, the transmission spectrum of each night are weight averaged by their uncertainties to build the average transmission spectrum. Figure 3 displays the average transmission spectrum around the helium triplet for each planet.

We neglect the impact of the Rossiter McLaughlin effect (Rossiter 1924; McLaughlin 1924) and the center-to-limb variation (Pierce & Slaughter 1977; Neckel & Labs 1994) as it was shown to have little impact on the helium lines in several studies (e.g., Allart et al. 2018, 2019; Nortmann et al. 2018; Salz et al. 2018; Fossati et al. 2022), which include part of the targets studied here.

### 3.2.2. Light curve

We derive the helium light curve to study the temporal variability of the signal by measuring the excess absorption, assuming a symmetric signal, in a passband of 0.75 Å centered at 10 833.22 Å for each exposure of the transmission spectroscopy map in the planet rest frame. Figure 4 displays the measured helium light curve for each planet averaged over the multiple transits.

### 3.2.3. Detection significance

The excess absorption is estimated on the transmission spectrum for each transit and the average transmission spectrum by

measuring the average signal on a passband of 0.75 Å centered at 10 833.22 Å. To assess the uncertainty on the measured excess absorption we produced Allan plots (Fig. C.1) to estimate the contribution of red-noise to the data. We applied the technique described in Winn et al. (2007); Cowan et al. (2012); Cubillos et al. (2017) but instead of having a time-correlated noise source we have a spectrally correlated noise source. We first estimate the expected Allan curve if our transmission spectrum is solely affected by white noise. We compute the standard deviation of the transmission spectrum excluding the helium triplet (10 820–10 830 and 10 836–10 845 Å) and scale it for decreasing spectral resolution as $\sqrt{n}$, where *n* is the number of pixels in the bin. We then binned the transmission spectrum by *n*, compute the root mean square (rms), and repeat the process for a different *n* size. We then fit the rms in a log-log space to derive the general trend of the noise properties. We then scale our white noise value on the 0.75 Å bandpass to match the fitted rms. This technique provides a more rigorous estimation of the noise present in the data. We set the detection level as the measured excess absorption divided by the inflated $1-\sigma$ uncertainty, following the aforementioned noise estimation. In the case of nondetections (below $5-\sigma$), we report three times the $1-\sigma$ uncertainty to set the $3-\sigma$ upper limit. From there, we derive the equivalent opaque radius and the widely used $\delta R_p/H$ parameter. The latter corresponds to the number of scale heights probed by the equivalent opaque radius.

### 3.2.4. Bootstrap analysis

The last test that is performed to confirm the planetary origin of the helium absorption is a bootstrap analysis, also called Empirical Monte Carlo (EMC) simulations (e.g., Redfield et al. 2008; Wyttenbach et al. 2015). It consists of generating three transmission spectrum scenarios (out-out, in-in, and in-out) of 10 000 iterations each. The goal is to in produce fake time series' to estimate how likely the measured signal can be built by random noise. For each iteration, the in- and out-of-transit spectra are randomized among the pool of spectra considered in each scenario. Then, the transmission spectrum is built for each of these iterations and the excess absorption is measured as described in Sect. 3.2.3. The in-in and out-out distributions are expected to be centered at zero absorption while the in-out scenario should be close to the excess absorption measured. The results are shown in Fig. D.1.

## 3.3. Modeling

### 3.3.1. Stellar pseudo-signal

The typical shape of the helium profiles is too broad to spectrally differentiate between a planetary and stellar origin. The planet and star signatures overlap for most orbital configurations, though an exception is made if the planet is on an eccentric orbit, such as HAT-P-11b (Allart et al. 2018). Moreover, it is possible that the planet transits in front of an inhomogeneous stellar surface that can create pseudo signal either in absorption or emission and can partly contribute to the observed He signal (e.g., Rackham et al. 2017; Salz et al. 2018; Guilluy et al. 2020). We can consider the stellar disk as two distinct regions with bright and dark stellar patches. The helium absorption line is only produced in the dark region and the planet only transits one of those two regions. If the planet only transits the bright region, the pseudo-absorption signal is maximized. Conversely, if the planet only transits the dark region, the pseudo-emission
<table><caption>**Table 2.** System parameters of the first eight planets.</caption><thead><tr><th>Parameters</th><th>Symbol (unit)</th><th>AU</th><th>Mic b</th><th>GJ1214 b</th><th>GJ3470 b</th><th>HAT-P-11 b</th></tr></thead><tbody><tr><td colspan="7" style="text-align:center; font-weight:bold;">Star</td></tr><tr><td>Stellar mass</td><td>M<sub>★</sub> (M<sub>☉</sub>)</td><td>0.50 ± 0.03<sup>(1)</sup></td><td>0.178 ± 0.010<sup>(3)</sup></td><td>0.51 ± 0.06<sup>(4)</sup></td><td>0.802 ± 0.028<sup>(6)</sup></td><td></td></tr><tr><td>Stellar radius</td><td>R<sub>★</sub> (R<sub>☉</sub>)</td><td>0.86 ± 0.05<sup>(18)</sup></td><td>0.215 ± 0.008<sup>(3)</sup></td><td>0.48 ± 0.04<sup>(4)</sup></td><td>0.683 ± 0.009<sup>(6)</sup></td><td></td></tr><tr><td>Stellar age</td><td>(Gyr)</td><td>0.022 ± 0.003<sup>(1)</sup></td><td>3–10<sup>(14)</sup></td><td>1.65 ± 1.35<sup>(4)</sup></td><td>6.5<sup>+5.9</sup><sub>-4.1</sub><sup>(13)</sup></td><td></td></tr><tr><td>Limb darkening coefficient</td><td>u<sub>1</sub></td><td>0.2348</td><td>0.0775</td><td>0.0866</td><td>0.2673</td><td></td></tr><tr><td>Limb darkening coefficient</td><td>u<sub>2</sub></td><td>0.3750</td><td>0.3627</td><td>0.3499</td><td>0.2649</td><td></td></tr><tr><td>Stellar metallicity</td><td>Fe/H (dex)</td><td>—</td><td>0.29 ± 0.12<sup>(3)</sup></td><td>0.2 ± 0.1<sup>(4)</sup></td><td>0.31 ± 0.05<sup>(6)</sup></td><td></td></tr><tr><td>Stellar temperature</td><td>T<sub>eff</sub> (K)</td><td>3700 ± 100<sup>(1)</sup></td><td>3250 ± 100<sup>(3)</sup></td><td>3652 ± 50<sup>(4)</sup></td><td>4780 ± 50<sup>(6)</sup></td><td></td></tr><tr><td>Surface gravity</td><td>log(g) (cgs)</td><td>4.39 ± 0.03<sup>(1)</sup></td><td>5.026 ± 0.040<sup>(3)</sup></td><td>4.658 ± 0.035<sup>(4)</sup></td><td>4.59 ± 0.03<sup>(6)</sup></td><td></td></tr><tr><td>Spectral type</td><td></td><td>M1V</td><td>M4V</td><td>M1.5V</td><td>K4V</td><td></td></tr><tr><td colspan="7" style="text-align:center; font-weight:bold;">Planet</td></tr><tr><td>Planetary mass</td><td>M<sub>p</sub> (M<sub>☉</sub>)</td><td>11.7 ± 5<sup>(1)</sup></td><td>8.17 ± 0.43<sup>(3)</sup></td><td>13.9 ± 1.5<sup>(4)</sup></td><td>27.74 ± 3.11<sup>(6)</sup></td><td></td></tr><tr><td>Planetary radius</td><td>R<sub>p</sub> (R<sub>☉</sub>)</td><td>3.55 ± 0.13<sup>(19)</sup></td><td>2.742 ± 0.17<sup>(3)</sup></td><td>4.57 ± 0.18<sup>(4)</sup></td><td>4.36 ± 0.06<sup>(6)</sup></td><td></td></tr><tr><td>Density</td><td>ρ (cgs)</td><td>1.25 ± 0.75<sup>(19)</sup></td><td>2.20 ± 0.17<sup>(3)</sup></td><td>0.93 ± 0.56<sup>(4)</sup></td><td>1.84 ± 0.21</td><td></td></tr><tr><td>Equilibrium temperature</td><td>T<sub>eq</sub> (K)</td><td>593 ± 21<sup>(1)</sup></td><td>596 ± 19<sup>(3)</sup></td><td>615 ± 16<sup>(4)</sup></td><td>787 ± 11</td><td></td></tr><tr><td>Orbital period</td><td>P (days)</td><td>8.463000(2)<sup>(1)</sup></td><td>1.58040433(13)<sup>(3)</sup></td><td>3.3366413(6)<sup>(4)</sup></td><td>4.887802443(34)<sup>(6)</sup></td><td></td></tr><tr><td>Mid-transit time (–2 450 000)</td><td>T<sub>0</sub> (days)</td><td>8330.39051(15)<sup>(1)</sup></td><td>5701.413328(66)<sup>(3)</sup></td><td>6677.727712(22)<sup>(4)</sup></td><td>4957.8132067(53)<sup>(6)</sup></td><td></td></tr><tr><td>Transit duration</td><td>t<sub>14</sub> (h)</td><td>3.51 ± 0.1<sup>(19)</sup></td><td>0.8688 ± 0.0029<sup>(3)</sup></td><td>1.918 ± 0.024<sup>(4)</sup></td><td>2.3565 ± 0.0015<sup>(6)</sup></td><td></td></tr><tr><td>Semi-amplitude</td><td>K<sub>★</sub> (m s<sup>-1</sup>)</td><td>5.8 ± 2.5<sup>(1)</sup></td><td>14.36 ± 0.53<sup>(3)</sup></td><td>8.21 ± 0.47<sup>(4)</sup></td><td>12.01 ± 1.38<sup>(6)</sup></td><td></td></tr><tr><td>Semi-major axis</td><td>a (R<sub>★</sub>)</td><td>18.95 ± 0.35<sup>(19)</sup></td><td>14.85 ± 0.16<sup>(3)</sup></td><td>12.92 ± 0.72<sup>(4)</sup></td><td>16.50 ± 0.18<sup>(6)</sup></td><td></td></tr><tr><td>Inclination</td><td>i (deg)</td><td>89.5 ± 0.3<sup>(2)</sup></td><td>88.7 ± 0.1<sup>(3)</sup></td><td>88.88 ± 0.62<sup>(5)</sup></td><td>89.05 ± 0.15<sup>(6)</sup></td><td></td></tr><tr><td>Impact parameter</td><td>b (R<sub>☉</sub>)</td><td>0.17 ± 0.11<sup>(19)</sup></td><td>0.325 ± 0.025<sup>(3)</sup></td><td>0.29 ± 0.14<sup>(5)</sup></td><td>0.209 ± 0.032<sup>(15)</sup></td><td></td></tr><tr><td>Eccentricity</td><td>e</td><td>0</td><td>0</td><td>0.114 ± 0.052<sup>(4)</sup></td><td>0.2644 ± 0.0006<sup>(6)</sup></td><td></td></tr><tr><td>Periastron argument</td><td>ω</td><td>90</td><td>90</td><td>-82.5 ± 5.7<sup>(4)</sup></td><td>342.186 ± 0.179<sup>(6)</sup></td><td></td></tr><tr><td colspan="7" style="text-align:center; font-weight:bold;">WASP-11 b</td></tr><tr><td>Stellar mass</td><td>M<sub>★</sub> (M<sub>☉</sub>)</td><td>0.81 ± 0.04<sup>(7)</sup></td><td>0.913 ± 0.047<sup>(9)</sup></td><td>0.87 ± 0.03<sup>(10)</sup></td><td>0.826 ± 0.029<sup>(11)</sup></td><td></td></tr><tr><td>Stellar radius</td><td>R<sub>★</sub> (R<sub>☉</sub>)</td><td>0.772 ± 0.015<sup>(7)</sup></td><td>0.939 ± 0.022<sup>(9)</sup></td><td>0.79 ± 0.24<sup>(10)</sup></td><td>0.813 ± 0.028<sup>(11)</sup></td><td></td></tr><tr><td>Stellar age</td><td>(Gyr)</td><td>7.6<sup>+6.0</sup><sub>-3.5</sub><sup>(7)</sup></td><td>8.5<sup>+4.0</sup><sub>-3.4</sub><sup>(9)</sup></td><td>0.4<sup>+0.3</sup><sub>-0.2</sub><sup>(10)</sup></td><td>~2<sup>(12)</sup></td><td></td></tr><tr><td>Limb darkening coefficient</td><td>u<sub>1</sub></td><td>0.2465</td><td>0.1767</td><td>0.2321</td><td>0.2696</td><td></td></tr><tr><td>Limb darkening coefficient</td><td>u<sub>2</sub></td><td>0.2721</td><td>0.2942</td><td>0.2773</td><td>0.2617</td><td></td></tr><tr><td>Stellar metallicity</td><td>Fe/H (dex)</td><td>0.12 ± 0.09<sup>(7)</sup></td><td>0.01 ± 0.09<sup>(9)</sup></td><td>0.03 ± 0.12<sup>(10)</sup></td><td>0.144 ± 0.077<sup>(12)</sup></td><td></td></tr><tr><td>Stellar temperature</td><td>T<sub>eff</sub> (K)</td><td>4900 ± 65<sup>(7)</sup></td><td>5485 ± 50<sup>(9)</sup></td><td>5000 ± 100<sup>(10)</sup></td><td>4715 ± 50<sup>(12)</sup></td><td></td></tr><tr><td>Surface gravity</td><td>log(g) (cgs)</td><td>4.569 ± 0.018<sup>(7)</sup></td><td>4.453 ± 0.012<sup>(9)</sup></td><td>4.582 ± 0.014<sup>(10)</sup></td><td>4.535 ± 0.023<sup>(12)</sup></td><td></td></tr><tr><td>Spectral type</td><td></td><td>K3</td><td>G8</td><td>K2</td><td>K5</td><td></td></tr><tr><td colspan="7" style="text-align:center; font-weight:bold;">WASP-39 b</td></tr><tr><td>Planetary mass</td><td>M<sub>p</sub> (M<sub>☉</sub>)</td><td>156 ± 8<sup>(7)</sup></td><td>89.3 ± 10.2<sup>(9)</sup></td><td>146.2 ± 6.36<sup>(10)</sup></td><td>82.64 ± 5.88<sup>(11)</sup></td><td></td></tr><tr><td>Planetary radius</td><td>R<sub>p</sub> (R<sub>☉</sub>)</td><td>11.10 ± 0.25<sup>(7)</sup></td><td>14.34 ± 0.45<sup>(9)</sup></td><td>14.24 ± 0.34<sup>(10)</sup></td><td>11.85 ± 0.19<sup>(11)</sup></td><td></td></tr><tr><td>Density</td><td>ρ (cgs)</td><td>0.632 ± 0.035<sup>(7)</sup></td><td>0.167 ± 0.023<sup>(9)</sup></td><td>0.29 ± 0.03<sup>(10)</sup></td><td>0.262 ± 0.047<sup>(11)</sup></td><td></td></tr><tr><td>Equilibrium temperature</td><td>T<sub>eq</sub> (K)</td><td>992 ± 14<sup>(7)</sup></td><td>1166 ± 14<sup>(9)</sup></td><td>1315 ± 35<sup>(10)</sup></td><td>963 ± 18<sup>(11)</sup></td><td></td></tr><tr><td>Orbital period</td><td>P (days)</td><td>3.7224790(3)<sup>(8)</sup></td><td>4.0552941(34)<sup>(9)</sup></td><td>1.7497798(12)<sup>(10)</sup></td><td>3.8681390(6)<sup>(8)</sup></td><td></td></tr><tr><td>Mid-transit time (–2 450 000)</td><td>T<sub>0</sub> (days)</td><td>6200.28683(9)<sup>(8)</sup></td><td>5342.96913(63)<sup>(9)</sup></td><td>5793.68143(9)<sup>(10)</sup></td><td>7176.17789(17)<sup>(8)</sup></td><td></td></tr><tr><td>Transit duration</td><td>t<sub>14</sub> (h)</td><td>2.58 ± 0.91<sup>(7)</sup></td><td>2.80 ± 0.02<sup>(9)</sup></td><td>1.81 ± 0.012<sup>(10)</sup></td><td>2.23 ± 0.03<sup>(11)</sup></td><td></td></tr><tr><td>Semi-amplitude</td><td>K<sub>★</sub> (m s<sup>-1</sup>)</td><td>82.7 ± 4.2<sup>(7)</sup></td><td>37.9 ± 5.4<sup>(9)</sup></td><td>109.6 ± 4.4<sup>(10)</sup></td><td>38.1 ± 2.4<sup>(11)</sup></td><td></td></tr><tr><td>Semi-major axis</td><td>a (R<sub>★</sub>)</td><td>12.19 ± 0.21<sup>(7)</sup></td><td>11.37 ± 0.24<sup>(9)</sup></td><td>7.38 ± 0.11<sup>(10)</sup></td><td>12.00 ± 0.46<sup>(11)</sup></td><td></td></tr><tr><td>Inclination</td><td>i (deg)</td><td>89.03 ± 0.34<sup>(7)</sup></td><td>87.32 ± 0.17<sup>(9)</sup></td><td>85.35 ± 0.2<sup>(10)</sup></td><td>86.71 ± 0.20<sup>(11)</sup></td><td></td></tr><tr><td>Impact parameter</td><td>b (R<sub>☉</sub>)</td><td>0.054 ± 0.168<sup>(16)</sup></td><td>0.447 ± 0.055<sup>(17)</sup></td><td>0.60 ± 0.02<sup>(10)</sup></td><td>0.686 ± 0.023<sup>(11)</sup></td><td></td></tr><tr><td>Eccentricity</td><td>e</td><td>0</td><td>0</td><td>0</td><td>0</td><td></td></tr><tr><td>Periastron argument</td><td>ω</td><td>90</td><td>90</td><td>90</td><td>90</td><td></td></tr></tbody></table>

**References.** (1)Zicher et al. (2022). (2)Martioli et al. (2021). (3)Cloutier et al. (2021). (4)Kosiarek et al. (2019). (5)Biddle et al. (2014). (6)Allart et al. (2018). (7)Mancini et al. (2015). (8)Kokori et al. (2022). (9)Mancini et al. (2018). (10)Hébrard et al. (2013). (11)Casasayas-Barris et al. (2017). (12)Anderson et al. (2014). (13)Bakos et al. (2010). (14)Charbonneau et al. (2009). (15)Huber et al. (2017). (16)West et al. (2009). (17)Maciejewski et al. (2016). (18)Gallenne et al. (2022). (19)Szabó et al. (2022).
<table><caption>**Table 3.** Continuation of Table 2 for the three remaining targets.</caption><thead><tr><th>Parameters</th><th>Symbol [Unit]</th><th>WASP-80 b</th><th>WASP-127b</th><th>HD189733 b</th></tr></thead><tbody><tr><td colspan="5" style="text-align: center; font-weight: bold;">Star</td></tr><tr><td>Stellar mass</td><td>M<sub>★</sub> (M<sub>☉</sub>)</td><td>0.577 ± 0.054<sup>(2)</sup></td><td>0.960 ± 0.023<sup>(3)</sup></td><td>0.806 ± 0.048<sup>(5)</sup></td></tr><tr><td>Stellar radius</td><td>R<sub>★</sub> (R<sub>☉</sub>)</td><td>0.586 ± 0.018<sup>(2)</sup></td><td>1.303 ± 0.037<sup>(3)</sup></td><td>0.756 ± 0.018<sup>(5)</sup></td></tr><tr><td>Stellar age</td><td>(Gyr)</td><td>&lt;0.2<sup>(2)</sup></td><td>9.656 ± 1.002<sup>(3)</sup></td><td>6.8 ± 5.2<sup>(5)</sup></td></tr><tr><td>Limb darkening coefficient</td><td>u<sub>1</sub></td><td>0.2146</td><td>0.1365</td><td>0.2248</td></tr><tr><td>Limb darkening coefficient</td><td>u<sub>2</sub></td><td>0.2830</td><td>0.2990</td><td>0.2795</td></tr><tr><td>Stellar metallicity</td><td>Fe/H (dex)</td><td>-0.13 ± 0.17<sup>(2)</sup></td><td>-0.19 ± 0.01<sup>(3)</sup></td><td>-0.03 ± 0.08<sup>(5)</sup></td></tr><tr><td>Stellar temperature</td><td>T<sub>eff</sub> (K)</td><td>4143 ± 94<sup>(2)</sup></td><td>5842 ± 13<sup>(3)</sup></td><td>5040 ± 50<sup>(5)</sup></td></tr><tr><td>Surface gravity</td><td>log(g) (cgs)</td><td>4.663 ± 0.016<sup>(2)</sup></td><td>4.23 ± 0.02<sup>(3)</sup></td><td>4.587 ± 0.015<sup>(5)</sup></td></tr><tr><td>Spectral type</td><td></td><td>K7V</td><td>G5</td><td>K2V</td></tr><tr><td colspan="5" style="text-align: center; font-weight: bold;">Planet</td></tr><tr><td>Planetary mass</td><td>M<sub>p</sub> (M<sub>⊕</sub>)</td><td>171 ± 11<sup>(2)</sup></td><td>52.35 ± 6.8<sup>(4)</sup></td><td>363.582 ± 18.116<sup>(5)</sup></td></tr><tr><td>Planetary radius</td><td>R<sub>p</sub> (R<sub>⊕</sub>)</td><td>11.2 ± 0.335<sup>(2)</sup></td><td>14.69 ± 0.33<sup>(4)</sup></td><td>12.756 ± 0.303<sup>(5)</sup></td></tr><tr><td>Density</td><td>ρ (cgs)</td><td>0.717 ± 0.039<sup>(2)</sup></td><td>0.097 ± 0.013<sup>(4)</sup></td><td>0.963 ± 0.088<sup>(5)</sup></td></tr><tr><td>Equilibrium temperature</td><td>T<sub>eq</sub> (K)</td><td>825 ± 19<sup>(2)</sup></td><td>1400 ± 24<sup>(3)</sup></td><td>1201 ± 13<sup>(5)</sup></td></tr><tr><td>Orbital period</td><td>P (days)</td><td>3.06785271(19)<sup>(1)</sup></td><td>4.17806203(88)<sup>(4)</sup></td><td>2.21857519(14)<sup>(1)</sup></td></tr><tr><td>Mid-transit time (-2 450 000)</td><td>T<sub>0</sub> (days)</td><td>6671.49615(4)<sup>(1)</sup></td><td>6776.62124(28)<sup>(4)</sup></td><td>4403.677711(25)<sup>(1)</sup></td></tr><tr><td>Transit duration</td><td>t<sub>14</sub> (h)</td><td>2.131 ± 0.003<sup>(2)</sup></td><td>4.353 ± 0.014<sup>(4)</sup></td><td>1.8036 ± 0.0023<sup>(6)</sup></td></tr><tr><td>Semi-amplitude</td><td>K<sub>★</sub> (m s<sup>-1</sup>)</td><td>109.0 ± 4.4<sup>(2)</sup></td><td>22 ± 3<sup>(3)</sup></td><td>205 ± 6<sup>(5)</sup></td></tr><tr><td>Semi-major axis</td><td>a (R<sub>★</sub>)</td><td>12.63 ± 0.13<sup>(2)</sup></td><td>7.81 ± 0.11<sup>(4)</sup></td><td>8.81 ± 0.06<sup>(5)</sup></td></tr><tr><td>Inclination</td><td>i (deg)</td><td>89.02 ± 0.1<sup>(2)</sup></td><td>87.84 ± 0.36<sup>(4)</sup></td><td>85.58 ± 0.06<sup>(5)</sup></td></tr><tr><td>Impact parameter</td><td>b (R<sub>☉</sub>)</td><td>0.215 ± 0.022<sup>(2)</sup></td><td>0.29 ± 0.045<sup>(4)</sup></td><td>0.680 ± 0.005<sup>(5)</sup></td></tr><tr><td>Eccentricity</td><td>e</td><td>0</td><td>0</td><td>0</td></tr><tr><td>Periastron argument</td><td>ω</td><td>90</td><td>90</td><td>90</td></tr></tbody></table>

**References.** (1) Kokori et al. (2022). (2) Triaud et al. (2015). (3) Allart et al. (2020). (4) Seidel et al. (2020). (5) Torres et al. (2008). (6) Baluev et al. (2015).

signal is maximized. To better visualize this effect, we developed a simple toy model that describes these extreme cases and consists of two stellar spectra representing the bright ($F_B$) and dark ($F_D$) regions associated with the fraction of dark regions ($f$, also called filling factor). The observed normalized master out-of-transit spectrum ($F_{out,norm}$) can be expressed as

$$F_{out,norm} = (1 - f) \cdot F_B + f \cdot F_D. \qquad (1)$$

We note that $F_B$ and $F_D$ are fitted from 10 827 to 10 837 Å to the Si I line at 10 830.054 Å and to the He I lines of the $F_{out,norm}$. Following the prescription of Andretta et al. (2017) and used in Salz et al. (2018), two superposed Voigt profiles are fitted to the Si I at the same fixed wavelength, and two Gaussians are fitted to the He I lines with fixed wavelengths. We fixed the Si I line profile to be similar between $F_B$ and $F_D$ and we consider that the amplitude of the He I lines between $F_B$ and $F_D$ are proportional to a constant $\alpha$. The filling factor is estimated using the relation of Andretta et al. (2017; Fig. 11) with the equivalent width (EW) of the He I lines at 10 833 Å.

Assuming the planet only transits the bright region, the pseudo-signal can be written as

$$\frac{F_{in,norm}}{F_{out,norm}} = \frac{1}{1 - (R_p/R_\star)^2} \frac{(1 - (R_p/R_\star)^2) \cdot F_B + f \cdot (F_D - F_B)}{(1 - f) \cdot F_B + f \cdot F_D}, \qquad (2)$$

which is equivalent to Eq. (11) of Rackham et al. (2017) in the case of ground-based high-resolution normalized spectra.

We explored the impact of $\alpha$ and $f$ on the stellar spectrum and the strength of the pseudo-signal for all our targets. The stellar spectra are well reproduced except for low values of $\alpha$ and $f$, that is when the stellar helium absorption comes only from a small dark region. The maximum pseudo-signal is produced when all the stellar helium absorption comes from the dark region ($\alpha = 0$) independently of the filling factor value selected between ~0.4 and 1.

### 3.3.2. p-winds modeling

The p-winds code (Dos Santos et al. 2022) is used to calculate the thermospheric structure of the 11 targets and the resulting neutral helium triplet signature. This 1D model is largely based on the formulations of Oklopčić & Hirata (2018) and Lampón et al. (2020) and we assumed an atmospheric composition of 90% H and 10% He. The density and velocity profiles of the atmosphere are calculated according to the Parker wind approximation assuming an isothermal planetary outflow (Parker 1958). To do so, we input the X-EUV spectral energy distribution (over 0–1170 Å, Linsky et al. 2014) of the 11 targets used to calculate the photoionization of H and He, which we calculate in a mutually consistent manner using the formula from Linsky et al. (2014) that predicts the EUV luminosity. This depends
<figure><img src="image_3.png" /><figcaption>**Fig. 2.** Transmission spectroscopy maps in the planet rest frame for the eleven planets. Detections are visible for HAT-P-11 b, HD 189733 b and WASP-69 b as white clusters. The pink dashed horizontal lines are the contact lines from bottom to top: *t*₁, *t*₂, *t*₃, and *t*₄. The vertical orange dashed lines indicate the helium lines' positions.</figcaption></figure>
<figure><img src="image_4.png" /><figcaption>**Fig. 3.** Average transmission spectra in the planet rest frame for the eleven planets. The vertical blue dashed lines indicate the helium lines' positions. The horizontal gray dashed line represents null excess absorption. The orange curves are the best-fit model from p-winds obtained for the three detections: HAT-P-11 b, HD 189733 b, and WASP-69 b.</figcaption></figure>
<figure><img src="image_5.png" /><figcaption>**Fig. 4.** Average excess helium light curves for the eleven planets. The blue dashed vertical lines are the contact lines from left to right: *t*₁, *t*₂, *t*₃, and *t*₄. The gray horizontal dashed line is the continuum level.</figcaption></figure>

on the total X-EUV flux received by the planet which is calcu-
lated thanks to the stellar age and the formula from Sanz-Forcada
et al. (2011). The code calculates the density profiles of hydro-
gen in its neutral and ionized states, and of helium in its neutral,
excited, and singly ionized states. The excited helium level cor-
responds to the metastable transition at 10 830 Å, which is the
signature of interest for which the code calculates theoretical
absorption spectra. The absorption signature is compared to
the observation in order to estimate the characteristics of the

upper atmosphere, such as temperature and mass-loss rate. How-
ever, it remains an approximate characterization by considering
ideal theoretical spectra calculated at mid transit without taking
geometrical effects and inhomogeneities of the stellar surface
into account, while it is compared to the observed mean trans-
mission spectra.

We explore the input parameter space of the p-winds models
for each of the 11 planets, varying the isothermal tempera-
ture profile, *T*, and the total atmospheric escape rate, *im*, while
<table><caption>**Table 4.** Summary of the helium triplet measurements from this work.</caption><thead><tr><th>Target units</th><th>Excess absorption %</th><th>Eq. opaque radius R<sub>p</sub></th><th>H km</th><th>δR<sub>p</sub>/H</th><th>F<sub>5-504Å</sub> erg s<sup>-1</sup> cm<sup>-2</sup></th><th>Roche Lobe R<sub>p</sub></th><th>ṁ</th></tr></thead><tbody><tr><td>AU Mic b</td><td>&lt;0.26</td><td>&lt;1.67</td><td>399</td><td>&lt;38</td><td>158.50</td><td>7.7</td><td>&lt;1.51</td></tr><tr><td>GJ1214 b</td><td>&lt;2.92</td><td>&lt;1.77</td><td>339</td><td>&lt;40</td><td>1.97</td><td>3.2</td><td>—</td></tr><tr><td>GJ3470 b</td><td>&lt;0.64</td><td>&lt;1.36</td><td>666</td><td>&lt;16</td><td>2.97</td><td>3.1</td><td>&lt;1.41</td></tr><tr><td>HAT-P-11 b</td><td>0.76 ± 0.07</td><td>1.80 ± 0.05</td><td>352</td><td>63 ± 4</td><td>0.16</td><td>6.5</td><td>0.67<sup>+0.27</sup><sub>-0.24</sub></td></tr><tr><td>HD189733 b</td><td>0.69 ± 0.04</td><td>1.14 ± 0.01</td><td>331</td><td>33 ± 2</td><td>0.42</td><td>3.0</td><td>0.94<sup>+0.82</sup><sub>-0.61</sub></td></tr><tr><td>WASP-11 b</td><td>&lt;1.56</td><td>&lt;1.38</td><td>484</td><td>&lt;55</td><td>0.19</td><td>3.7</td><td>&lt;0.08</td></tr><tr><td>WASP-39 b</td><td>&lt;2.04</td><td>&lt;1.43</td><td>1635</td><td>&lt;24</td><td>0.12</td><td>2.6</td><td>&lt;1.50</td></tr><tr><td>WASP-52 b</td><td>&lt;1.69</td><td>&lt;1.27</td><td>1114</td><td>&lt;22</td><td>20.93</td><td>1.7</td><td>&lt;6.99</td></tr><tr><td>WASP-69 b</td><td>2.35 ± 0.46</td><td>1.50 ± 0.09</td><td>1001</td><td>38 ± 7</td><td>0.93</td><td>2.9</td><td>0.40<sup>+0.58</sup><sub>-0.25</sub></td></tr><tr><td>WASP-80 b</td><td>&lt;1.24</td><td>&lt;1.19</td><td>373</td><td>&lt;35</td><td>31.78</td><td>3.4</td><td>&lt;0.14</td></tr><tr><td>WASP-127 b</td><td>&lt;0.48</td><td>&lt;1.20</td><td>3762</td><td>&lt;5</td><td>0.12</td><td>2.0</td><td>—</td></tr></tbody></table>

**Notes.** Excess absorption, equivalent radius, and $\delta R_p/H$ are the 3-$\sigma$ upper limits unless a detection is reported. $F_{5-504\AA}$ is the integrated XUV flux from 5 to 504 Å and scaled to the semi-major axis of the planets. The Roche Lobe was estimated following Rappaport et al. (2013).

having a fixed line-of-sight bulk velocity, $v$, and radius value at the top of the model, $r$. The line-of-sight bulk velocity corresponds to an average helium particle motion due to winds in the probe area around the terminator. For the three planets with detected helium lines, we further explore these last two parameters, $v$ and $r$. Previous studies using the p-wind code or similar codes (e.g., Oklopčić & Hirata 2018; Lampón et al. 2020; Dos Santos et al. 2022; Kirk et al. 2022) seem to not have explored the role of the upper radius boundary used to calculate the thermospheric structure. Yet, this radius is critical for the calculation of the theoretical helium signature. Increasing the radius until the neutral triplet helium density no longer contributes significantly to the absorption signal is rarely consistent with the validity of the model beyond the Roche lobe. Above the Roche lobe, species are no longer gravitationally bound to the planet, which limits the validity of the model. We, therefore, decided to fit the model top radius for targets with neutral triplet helium detection but set an upper limit at the Roche lobe. This arbitrarily restricts the amount of neutral triplet helium in the atmosphere and impacts the relative depth between the two neutral triplet helium absorption lines due to the relative radius ratio or the altitude of the optical thickness of the atmosphere. Varying the model top radius cannot be done for nondetection, as it allows finding a model compatible with the data for any temperature and mass-loss rate by reducing the radius to decrease the absorption. We thus set the radius to the Roche lobe to constrain the maximum escape rate for nondetections.

We used $\chi^2$ minimization to identify the best-fitting models and their uncertainties. As we found best fits to yield reduced $\chi^2$ larger than unity, likely because of systematic noise in the data, we chose the conservative approach of scaling the error bars of the data by the square root of the reduced $\chi^2$ from the best fit (see, Hébrard et al. 2002; Lemoine et al. 2002).

For planets with detected signals, we provide uncertainties on the best-fit properties at $1-\sigma$, while for nondetection we provide upper limits at $3-\sigma$.

We limit the parameter space in temperature using the model Salz et al. (2016; see also Caldiroli et al. 2021, 2022) as a function of the gravitational potential of the planet. Below $\log(-\Phi_G) = \log GM_{pl}/R_{pl} = 13.0$ in erg g$^{-1}$ they predict temperatures below 10 000 K, while above this limit they predict temperatures below 20 000 K. We limit the parameter space

in mass-loss rate using the maximum mass-loss efficiency for a photoionization-driven isothermal Parker wind (e.g., Vissapragada et al. 2022a).

# 4. SPIRou survey

Tables 2 and 3 summarize the stellar and planetary parameters used for the eleven systems that we observed. In the following subsections, for each exoplanet, we provide a short background history before describing the analysis of the helium triplet and then present our modeling of the transmission spectra. Table 4 summarizes these parameters for each planet.

## 4.1. AU Mic b

### 4.1.1. Background

AU Mic b is the inner planet of a two Neptune-sized system orbiting a young M dwarf discovered with TESS and monitored by several radial velocity (RV) spectrographs (Plavchan et al. 2020; Klein et al. 2021; Martioli et al. 2021; Zicher et al. 2022). With an age of $22 \pm 3$ Myr, this system still hosts an edge-on debris disk (Kalas et al. 2004; Boccaletti et al. 2015; Vizgan et al. 2022) and has an intense magnetic activity cycle. It was shown (e.g., Martioli et al. 2020; Palle et al. 2020; Addison et al. 2021) that the planet b has an aligned orbit, and thus, might have formed and migrated within the disk. Therefore, it is thought that AU Mic b, and c are progenitors of the super-Earth/mini-Neptune population and key targets for in-depth characterization. Such a young planetary system is of particular importance to understand how planets and their atmospheres evolve. No detections of atomic or molecular species have been reported in the literature, but attempts in the visible have been made with ESPRESSO (Palle et al. 2020). In addition, Hirano et al. (2020) used IRD and NIRSPEC data to study the presence of metastable helium and set an upper limit on the equivalent width of 3.7 mÅ at 99%. The lack of atmospheric detections observed could be linked to the stellar wind confining the planet's atmosphere outflow Carolan et al. (2020).

### 4.1.2. Helium triplet

The only transit of AU Mic b observed with SPIRou has no baseline before transit and is missing data until after ingress, due to
high airmass during constraints. The telluric lines are redshifted from the helium triplet (Fig. A.1). A variable excess absorption feature is visible at the position of the helium triplet, but the width and intensity evolve across the transit with a maximum of absorption before mid-transit (Figs. 2, 3 and 4). The measured excess absorption on the transmission spectrum is 0.37 ± 0.09% (4.3 σ) assuming the noise properties derived from the Allan plot (Fig. C.1). Indeed, similar structures are visible at different wavelengths (Fig. 3). These structures are not caused by telluric contamination (see Fig. A.1). However, it can be expected that young active stars have variable stellar features and it is, therefore, not possible to claim any robust detection of helium for AU Mic b with only one transit. We set the 3-σ upper limit on the presence of helium at a conservative <0.26% following the procedure of Sect. 3.2.3, which is in agreement with Hirano et al. (2020). It is also possible that due to the high stellar activity of AU Mic, the master out spectrum is not representative enough of the stellar features over the transit duration. We, therefore, call for more observations of the system to confirm the signature and average out the stellar activity.

## 4.2. GJ 1214 b

### 4.2.1. Background

GJ 1214 b is a warm mini-Neptune orbiting a nearby M dwarf (Charbonneau et al. 2009). Its density is in good agreement with a water-rich composition and a hydrogen-helium envelope, which encouraged in-depth analysis of its atmosphere. However, Kreidberg et al. (2014) revealed a featureless near-infrared spectrum obtained with the Hubble Space Telescope (HST), even with exquisite precision. The authors ruled out numerous compositions and concluded that the lower atmosphere of GJ1214 b is dominated by clouds. Nonetheless, recent attempts have been performed to detect the thermosphere and exosphere of the planet (layers well above the cloud deck) through the helium triplet. Crossfield et al. (2019), Petit dit de la Roche et al. (2020) and Kasper et al. (2020) reported only upper limits on the presence of He, while Orell-Miquel et al. (2022) reported a tentative detection at 4.6σ. It is interesting to compare the two last results as they have been obtained at high resolution with Keck/NIRSPEC (Kasper et al. 2020) and CARMENES (Orell-Miquel et al. 2022). The upper limit set with NIRSPEC is ~0.13% at the 90% confidence interval obtained for one transit, while the detection obtained with CARMENES is of 2.1 ± 0.5% and was also obtained for one transit. Orell-Miquel et al. (2022) proposed that the discrepancy might be caused by the telluric contamination of the nearby OH and H₂O lines and their poor correction. The authors scheduled their CARMENES transits to avoid such contamination, and showed that the H₂O line is superposed to the helium triplet in the NIRSPEC data. However, Spake et al. (2022) reported an upper limit of ~1.22% at the 95% confidence interval by observing one transit of GJ 1214 b with NIRSPEC at a time of the year where there is no telluric contamination. Their results are in clear contradiction with Orell-Miquel et al. (2022) and could be explained by instrumental or reduction systematics (Radica et al. 2022), or by strong variability from the star or in the planet's atmosphere.

### 4.2.2. Helium triplet

The time series of GJ 1214 b observed with SPIRou spans the full transit with a baseline before and after. The telluric lines are shifted to the red from the helium triplet and do not overlap

with the planetary track (Fig. A.1). The transmission spectrum (Fig. 3) is impacted by some systematics and the helium light curve (Fig. 4) has some variability before and during transit, but the bootstrap analysis (Fig. D.1) reveals similar distribution with no significant excess absorption for any of the three scenarios. The measured excess absorption on the transmission spectrum is of 1.59 ± 0.97%, and the 3-σ upper limit on the presence of helium of <2.92%, which is not constraining enough to settle the difference between the detection of Orell-Miquel et al. (2022) and the nondetections of Kasper et al. (2020) and Spake et al. (2022). Despite having similar instrument and telescope, our results are less sensitive than Orell-Miquel et al. (2022) but are due to the lower S/N of the SPIRou data.

## 4.3. GJ3470 b

### 4.3.1. Background

GJ3470 b is a warm Neptune orbiting a nearby M dwarf (Bonfils et al. 2012) on an eccentric polar orbit (Stefansson et al. 2022). Benneke et al. (2019) revealed a low-metallicity, hydrogen-dominated atmosphere with the detection of water, but depleted in methane. One possibility proposed by the authors is the presence of an unknown planet that could have caused tidal heating and pushed the atmosphere to be CO-dominated. The eccentric polar orbit of GJ3470 b could be an additional consequence of an unknown companion at long period (Stefansson et al. 2022). In addition, Bourrier et al. (2018) revealed through the detection of neutral hydrogen that the upper atmosphere extends beyond the Roche lobe, is elongated in the direction of the planet's motion, and strongly escapes into space. This could indicate that GJ3470 b may have lost 4 to 35% of its current mass over its lifetime (~2Gyr). Metastable helium has also been detected in the upper atmosphere of this planet (Ninan et al. 2020; Palle et al. 2020). The latter reported detection of 1.5 ± 0.3% maximum excess absorption with CARMENES and derived a mass-loss rate of the same magnitude as Bourrier et al. (2018).

### 4.3.2. Helium triplet

The two time series observed with SPIRou span the full transit with baselines before and after transit. Telluric lines of OH and water overlap with the helium triplet for the first night but are redshifted for the second night (Fig. A.1). In addition, the second time series was observed under better weather conditions. The transmission spectra and helium light curves of both nights are in very good agreement with each other. From the transmission spectroscopic map (Fig. 2), we can see an overall increase of excess absorption on a broad wavelength range from after ingress until the end of the time series, independently of the transit. This effect is visible in the helium light curve (Fig. 4). However, the averaged transmission spectrum (Fig. 3) does not have significant excess absorption, which is in agreement with the bootstrap analysis (Fig. D.1) of the two time series. The measured excess absorption on the transmission spectrum is 0.55 ± 0.21% (2.6σ). We put the 3-σ upper limit on the presence of helium at <0.63% as it is difficult to differentiate the observed broad feature between a planetary origin or noise structure. Our result is in disagreement with the detections reported by Ninan et al. (2020) and Palle et al. (2020), even once they are integrated over the same 0.75 Å bandpass (~1.2% for Palle et al. 2020). We also performed an injection-recovery test by adding to our transmission spectrum a Gaussian of amplitude
1.5% and FWHM of 1 Å following the result of Palle et al. (2020). The measured excess absorption on these injected data is $1.62 \pm 0.21\%$ ($7.7\sigma$), which confirm the tension with the literature. More data are needed to mitigate nonwhite noise source and confirm or infirm the presence of metastable helium in the atmosphere of GJ3470 b.

## 4.4. HAT-P-11 b

### 4.4.1. Background

HAT-P-11 b is the inner planet, a warm Neptune (Bakos et al. 2010), in a two-planet system (Yee et al. 2018) around a K dwarf star on an eccentric misaligned orbit (Winn et al. 2010), with properties similar to GJ3470 b. Fraine et al. (2014) and Chachan et al. (2019) reported the detection of water and methane in its lower atmosphere with high-altitude clouds and a low metallicity, which is in contradiction to the metallicity-mass trend known for the Solar system planets. It is even more striking that the star has a super-solar metallicity. A possible scenario is that metals stopped being accreted before the envelope formed (Thorngren & Fortney 2018). This was further supported by Ben-Jaffel et al. (2022) who reported a low metallicity atmosphere through a panchromatic UV approach. In addition, the authors measured the escape of neutral hydrogen and the presence of a cometary-like tail. Allart et al. (2018) and Mansfield et al. (2018) detected the presence of metastable helium at near-infrared wavelengths with CARMENES and HST. Due to the high resolution of CARMENES, Allart et al. (2018) resolved the helium lines and measured an excess absorption of $1.08 \pm 0.05\%$ on a $0.75$ Å passband with some variability between their two transits ($0.82 \pm 0.09\%$ and $1.21 \pm 0.06\%$). They also constrained the presence of helium to the thermosphere at high temperatures (or low mean molecular weight) with the presence of strong day-to-night side winds and without a strong mass-loss rate.

### 4.4.2. Helium triplet

The two transits of HAT-P-11 b are well observed with a baseline before and after transit. Due to the high systemic velocity of the system, there is no overlap with telluric lines (Fig. A.1). A clear repeatable signature is visible during the transit and is slightly blue-shifted from the expected position of the helium triplet in the planetary rest frame, which cannot be mistaken with the stellar rest frame due to the planet eccentricity (Figs. 2, 3 and 4). The helium light curve does not significantly extend beyond the transit duration in agreement with Allart et al. (2018). In addition, the two transits show similar helium line shapes and light curve with no significant temporal variation. The measured excess absorption on the transmission spectrum is $0.76 \pm 0.07\%$ ($11\sigma$) with a maximum of excess absorption at ~1.3%. The excess absorption is significantly below the reported average excess absorption measured by Allart et al. (2018), but in agreement with the value reported for their first transit of $0.82 \pm 0.09\%$.

## 4.5. HD189733 b

### 4.5.1. Background

HD189733 b is a hot Jupiter orbiting a relatively active K dwarf (Bouchy et al. 2005). Due to its host star brightness, it is one of the most studied exoplanets from its lower atmosphere to its exosphere. Multiple detections of molecules (such as H$_2$O and CO) have been reported both at low and high resolution (e.g.,

<table><caption>**Table 5.** Summary of the helium triplet excess absorption for each transit of HD 189733 b.</caption><thead><tr><th rowspan="2">Night</th><th rowspan="2">1-pixel<br>dispersion [%]</th><th colspan="2">Excess absorption [%], bandpass:</th></tr><tr><th>0.75 Å</th><th>1.44 Å (40 km s<sup>-1</sup>)</th></tr></thead><tbody><tr><td>2018-09-22</td><td>0.23</td><td>0.85 ± 0.10</td><td>0.45 ± 0.08</td></tr><tr><td>2019-06-15</td><td>0.19</td><td>0.52 ± 0.09</td><td>0.37 ± 0.07</td></tr><tr><td>2020-07-03</td><td>0.28</td><td>0.61 ± 0.14</td><td>0.29 ± 0.10</td></tr><tr><td>2020-07-05</td><td>0.32</td><td>0.58 ± 0.15</td><td>0.57 ± 0.11</td></tr><tr><td>2020-07-25</td><td>0.22</td><td>0.90 ± 0.07</td><td>0.75 ± 0.04</td></tr><tr><td>2021-08-24</td><td>0.15</td><td>0.68 ± 0.07</td><td>0.61 ± 0.05</td></tr><tr><td>Average</td><td>0.09</td><td>0.69 ± 0.04</td><td>0.51 ± 0.03</td></tr></tbody></table>

Birkby et al. 2013; de Kok et al. 2013; McCullough et al. 2014; Sing et al. 2016; Brogi et al. 2016, 2018; Alonso-Floriano et al. 2019a; Cabot et al. 2019; Boucher et al. 2021). Detection of atomic species probing the higher atmospheric layers have also been reported, including Na (e.g., Redfield et al. 2008; Wyttenbach et al. 2015), K (e.g., Keles et al. 2019), H (through H-$\alpha$, e.g., Cauley et al. 2015, 2016, 2017 and Lyman-$\alpha$, e.g., Lecavelier Des Étangs et al. 2010, 2012; Bourrier et al. 2013) or He (Salz et al. 2018; Guilluy et al. 2020; Zhang et al. 2022a). The helium triplet has been observed from 2016 to 2020 with three different high-resolution spectrographs (CARMENES, GIANO, and Keck/NIRSPEC) for a total of nine transits. The three studies all report a compact metastable helium atmosphere probing similar atmospheric layers (~$1.2 R_p$) and dynamic (blueshift of ~3–4 km s$^{-1}$) than the Sodium doublet. However, it was put in evidence in Zhang et al. (2022a) that the excess absorption varies between epochs and instruments: $0.617 \pm 0.017\%$ for CARMENES (Salz et al. 2018), $0.508 \pm 0.015\%$ for GIANO (Guilluy et al. 2020) and $0.420 \pm 0.013\%$ for NIRPSEC (Zhang et al. 2022a). These variations are unlikely due to starspot occultation but could be caused by instrumental systematics, unocculted stellar active regions, the planet's atmospheric outflow, shear instability, or stellar flares increasing the star's XUV flux (Wang & Dai 2021b,a; Hazra et al. 2022).

### 4.5.2. Helium triplet

A total of six transit time series of HD 189733 were observed with SPIRou from 2018 to 2021. Two of them observed on 2020-07-13 (night 3) and 2020-07-05 (night 4) are partial transits with respectively only egress and before mid-transit spectra. The transit of 2021-08-24 (night 6) has no after-transit baseline. The remaining transits are well covered with before and after baseline. The telluric contamination is negligible for all nights as either the strong OH component is very shallow or is far away from the helium line. A clear excess absorption feature is detected (Figs. 2, 3 and 4) during the transit of HD 189733 b at the expected position of the helium lines, but cannot be disentangled between the stellar and planetary rest frame. The signature is slightly blue-shifted in the planetary rest frame and the two components of the helium doublet are visible with a contrast ratio of ~2. Despite some large variability in the helium light curve before the transit, the excess absorption is well contained to the transit duration. The measured excess absorption on the transmission spectrum is $0.69 \pm 0.04\%$ ($17\sigma$) with a maximum at ~0.9%. We report in Table 5 the excess absorption measured for each night for the bandpass of $0.75$ Å but also for a $40$ km s$^{-1}$ ($1.44$ Å) bandpass to allow comparison with the
<figure><img src="image_6.png" /><figcaption>**Fig. 5.** Transmission spectra of HD 189733 b for the nights where the full transit was observed, respectively 2018-09-22 (blue), 2019-06-15 (green), 2020-07-25 (pink), and 2021-08-24 (orange).</figcaption></figure>

previous results of Zhang et al. (2022a). The measured excess absorption over this bandpass on the average transmission spectrum differs from the results of NIRSPEC at 3-σ, GIANO at 0.1-σ, and CARMENES at 3.6-σ. The variability in the signal strength is not due to reduction artifact, or Earth's atmosphere residuals as significant variations are measured for different transits obtained with the same instrument (GIANO and SPIRou) and the same data reduction. To further explore this variation in the signal strength, we compare in Fig. 5 the transmission spectra obtained for the nights where the complete transit was observed (2018-09-22, 2019-06-15, 2020-07-25 and 2021-08-24). We note that for the transit of 2018-09-22 (blue), the weak component of the helium triplet has no excess absorption while the strong component has more excess absorption than the other nights. The transmission spectrum of 2019-06-15 (green) has less excess absorption in the main component and a clear lack of absorption between the two components. The transmission spectrum of 2020-07-25 (pink) has larger noise structures and there are no clear distinctions between the two components of the helium triplet. These variations of the helium line shape can have different origins such as instrumental systematics, the optical thickness of the outflow or the presence of strong blueshifted helium gas. It is beyond the scope of this paper to investigate the causes of these variations.

## 4.6. WASP-11 b

### 4.6.1. Background

WASP-11b, also known as HAT-P-10b, is a hot Jupiter orbiting an inactive K dwarf (West et al. 2009; Bakos et al. 2009). It has an aligned orbit, as is the case for many hot Jupiters (Albrecht et al. 2022). No studies have been reported on its atmosphere.

### 4.6.2. Helium triplet

The time series of WASP-11 b observed with SPIRou spans the full transit with a baseline before and after. We removed the two first exposures due to high variability in the stellar spectrum. The telluric lines are redshifted relative to the helium triplet

(Fig. A.1). The transmission spectrum (Fig. 3) exhibits a slightly decreasing slope from 10 830 to 10 833 Å which is likely due to the Si I stellar line at 10 830 Å. It also has some excess absorption features around 10 833.7 Å (redward of the helium triplet), which seems to be associated with a few of exposures before mid-transit (Fig. 2). However, the helium light curve (Fig. 4) is stable across the time series and the bootstrap analysis (Fig. D.1) reveals similar distribution with no excess absorption for the out- out, in-in, and in-out scenarios. The measured excess absorption on the transmission spectrum is -0.09 ± 0.52%, consistent with no absorption. The 3-σ upper limit on the presence of helium is set at <1.56% due to the observed systematics. At the difference of the our other datasets, the noise structures disappear and tend toward white noise for larger bin (Fig. C.1).

## 4.7. WASP-39 b

### 4.7.1. Background

WASP-39 b is an inflated warm Neptune orbiting a late G-type star (Faedi et al. 2011). It is one of the archetype exoplanets for atmospheric characterization and comparison due to its cloud-free high metallicity atmosphere (Wakeford et al. 2018; Sing et al. 2016). Detections of water, carbon monoxide, carbon dioxide, and hydrogen sulfide have been reported with HST, Spitzer, and the newly launched JWST (Wakeford et al. 2018; JWST Transiting Exoplanet Community Early Release Science Team 2023; Rustamkulov et al. 2023; Feinstein et al. 2023; Alderson et al. 2023; Ahrer et al. 2023; Tsai et al. 2023). However, no studies have been reported for its upper atmosphere.

### 4.7.2. Helium triplet

The two time series (2022-06-04 and 2022-06-08) respectively cover the full transit with baseline and the transit until the start of egress with baseline only before transit. The weakest components of the OH doublets overlap with the red wing of the stellar helium triplet but are well corrected (Fig. A.1). Some features are visible in the transmission spectrum and the helium light curve (Figs. 3 and 4) at different wavelengths and phases. We attribute these features to instrumental systematics rather than the presence of helium in the exoplanet atmosphere. To reinforce this point, the bootstrap analysis (Fig. D.1) shows distributions with no excess absorption for the out-out and in-in scenarios while the in-out scenario mean value varies between the two nights from positive to negative excess absorption value, but is still compatible with no excess absorption. The measured excess absorption on the transmission spectrum is 0.47 ± 0.68%, but the 3-σ upper limit on the presence of helium is set at <2.05%.

## 4.8. WASP-52 b

### 4.8.1. Background

WASP-52 b is a hot Jupiter orbiting around an active K dwarf (Hébrard et al. 2013). While detection of water and clouds in its lower atmosphere have been reported (Alam et al. 2018; Tsiaras et al. 2018; Bruno et al. 2020), WASP-52 b was intensively more studied for its upper atmosphere. Detections of the sodium and potassium doublets and the H-α line in the visible with ESPRESSO (Chen et al. 2020) indicate an extended thermosphere above the cloud deck up to ~1.2 $R_p$, still below the Roche lobe radius (1.75 $R_p$). These detections are a bit surprising with respect to the equilibrium temperature of ~1200 K, but
could be explained by hot upper layers due to the strong stellar XUV flux correlated to stellar activity. More recently, metastable helium was detected at high resolution by Kirk et al. (2022) but only an upper limit was set at low resolution (Vissapragada et al. 2020). Kirk et al. (2022), one of the strongest, excess absorption of $3.44 \pm 0.31\%$ with NIRSPEC, such that helium almost fill the Roche lobe. They, further, applied p-winds (Dos Santos et al. 2022) to estimate that the planet loses 0.5% of its mass per Gyr.

### 4.8.2. Helium triplet

The two time series cover the full transit with a baseline before and after transit. The strong component of the telluric OH line overlaps partially and completely with the helium triplet for the two nights (Fig. A.1). We note that the telluric-corrected master-out of each night is not perfectly identical. This is likely due to the low S/N of the datasets. This also impacts the shape of the stellar helium line where it is shallower and broader for the first night. Nonetheless, the transmission spectra and helium light curves of both nights are in good agreement with each other. From the transmission spectroscopic map (Fig. 2), we can see that the before-transit and in-transit spectra have features in excess absorption across the spectral range. This is also captured by the helium light curve (Fig. 4). In the averaged transmission spectrum (Fig. 3), noise structures are also visible, but no significant excess absorption is detected at the helium line position and it is concurred by the bootstrap analysis (Fig. D.1) of the two time series. The measured excess absorption on the transmission spectrum is $1.36 \pm 0.56\%$, and the $3-\sigma$ upper limit on the presence of helium is set at <1.69%. From the Allan plot (Fig. C.1), the WASP-52b data best follow the white noise estimations even if features have large amplitudes up to 4% they are below the $3-\sigma$ upper limit once integrated over the 0.75 Å passband. This is in strong disagreement with the results reported by Kirk et al. (2022) and Vissapragada et al. (2022b). We note that the value reported by Kirk et al. (2022) is the maximum absorption of their signature, but once integrated over a 0.75% passband their absorption is ~2.7%, which is still in strong disagreement with our observations. We also performed an injection-recovery test by adding to our transmission spectrum a Gaussian of amplitude 3.44% and FWHM of 1 Å following the result of Kirk et al. (2022). The measured excess absorption on these injected data is $3.93 \pm 0.56\%$ ($7\sigma$), which confirm the tension with the literature. Here again, we need more data to settle the debate on the presence of metastable helium.

## 4.9. WASP-69b

### 4.9.1. Background

WASP-69b is a warm Neptune orbiting an active K dwarf (Anderson et al. 2014). It is one of the best targets for atmospheric characterization due to its large-scale height and was, therefore, well studied at high spectral resolution and combined with data at low resolution. Guilluy et al. (2022) reported the presence in the lower atmosphere of five molecules at more than $3\sigma$ with the near-infrared high-resolution spectrograph GIANO, but with variability for some molecules between transits. Nonetheless, water was independently confirmed with HST (Tsiaras et al. 2018; Estrela et al. 2021) alongside aerosols. The detection of the sodium doublet in the thermosphere was also reported at high spectral resolution (Casasayas-Barris et al. 2017; Khalafinejad et al. 2021), but with a strong amplitude ratio between the two lines, which is likely due to the presence of

hazes. WASP-69b is also one of the two first exoplanets (with HAT-P-11 b, Allart et al. 2018) with a measured excess absorption of helium obtained at high resolution with CARMENES (Nortmann et al. 2018). The authors measured a blueshifted line profile with a clear excess absorption of $3.59 \pm 0.19\%$ with a slight excess after the opaque transit. This is in agreement with an extended thermosphere up to $2.2 R_p$. This signature was also confirmed at low resolution by Vissapragada et al. (2020).

### 4.9.2. Helium triplet

The time series of WASP-69b covers the full transit with a baseline before and after. The strong component of the OH lines overlaps with the redwing of the helium triplet (Fig. A.1). A clear signature is visible during the transit slightly blue-shifted to the expected position of the helium triplet, but can still be associated with both the stellar and planetary rest frame (Figs. 2, 3 and 4). From the helium light curve, it is not possible to confirm the presence of post-transit absorption as discussed in Nortmann et al. (2018). Moreover, we see that there is some variability along the transit duration with a maximum of excess absorption before mid-transit. The measured excess absorption on the transmission spectrum is $2.21 \pm 0.46\%$ ($4.8 \sigma$) with a maximum excess absorption of ~3.1%. This is significantly below the reported maximum excess absorption measured by Nortmann et al. (2018) but the integrated signal over a 0.75 Å bandpass is in agreement with an absorption of ~2% as their line profile is quite narrow. The difference at the maximum of excess absorption is too large to be explained by data reduction effects but could be caused by some instrumental or systematic effects as well as some astrophysical variability linked either to the star or the planet.

## 4.10. WASP-80b

### 4.10.1. Background

WASP-80b is a hot Jupiter orbiting a K7 dwarf (Triaud et al. 2013). Broadband absorption features of water and carbon dioxide partly muted by clouds and aerosols reveal an enhanced atmospheric metallicity (Wong et al. 2022). No detection of metastable helium has been reported either at low resolution by Vissapragada et al. (2022b) nor at high resolution by Fossati et al. (2022). The latter set an upper limit of 0.7% was set with GIANO with three transits. The authors estimated that the helium-to-hydrogen abundance ratio of WASP-80b has to be lower than solar to match their data.

### 4.10.2. Helium triplet

The time series of WASP-80b observed with SPIRou spans the full transit with a baseline before and after. The telluric line positions overlap with the helium triplet with the strong component of the OH doublet on the bluewing and the water telluric line on the redwing (Fig. A.1). The telluric (absorption and emission) lines seem to be well corrected and should not impact the potential presence of planetary helium. Systematics are present in the transmission spectrum and the helium light curve (Figs. 3 and 4), but are not related to the presence of helium in the exoplanet atmosphere. The bootstrap analysis (Fig. D.1) shows distributions with no excess absorption for the out-out, in-in, and in-out scenarios. The measured excess absorption on the transmission spectrum is $0.03 \pm 0.41\%$. The $3-\sigma$ upper limit on the presence of helium was set at <1.24%, which is less stringent than the upper
limit set by Fossati et al. (2022) even if scaled to three transits and with the same upper limit metric.

### 4.11. WASP-127 b

#### 4.11.1. Background

WASP-127 b is a bloated hot Neptune on a misaligned circular orbit around an old (~10 Gyr) G-type star (Lam et al. 2017; Allart et al. 2020). With its large scale height, WASP-127 b is one of the most amenable planets for atmospheric characterization. Spake et al. (2021b) indeed revealed with HST and Spitzer a feature-rich atmosphere with the strongest amplitude known (~800 ppm) for the water band at 1.4 µm. In addition, they constrained the presence of clouds, aerosols, and of carbon-bearing species without the possibility to distinguish between a CO-rich high C/O ratio atmosphere or a CO₂-rich low C/O ratio atmosphere. High-resolution observations with SPIRou Boucher et al. (2023) reported the detection of water and a possible hint of OH, but did not detect the presence of CO. By combining their data with the data of Spake et al. (2021b), their model tends to favor the low C/O atmosphere. Although the presence of many species in the thermosphere could have been expected, only sodium was detected with ESPRESSO (Allart et al. 2020), which extends over 7 scale heights only and strong upper limits were set for the potassium doublet and H-α. Similarly, dos Santos et al. (2020) reported an upper limit of 0.87% on the presence of metastable helium with one transit with Gemini/Phoenix, which is probably due to the relatively mild high-energy environment around the star.

#### 4.11.2. Helium triplet

Due to the long transit duration of WASP-127b, the three time series do not cover the full transit and have a little baseline before or after. Only for the last time series (2021-05-03), there is an overlap between the strong component of the OH doublet with the redwing of the stellar helium position (Fig. A.1). We note that the stellar helium line is broad and shallow. The transmission spectroscopy map (Figs. 2 and B.1) exhibits noise structures in the observer or stellar rest frame during the transit, which impacts the transmission spectrum (Fig. 3). They might be caused by instrumental systematics not caught by APER0 or caused by small telluric residuals from the weak component of the OH lines. The average transmission spectrum has a broad-band slope that we detrend with a polynomial of order 2. The helium light curve (Fig. 4) does not show any excess absorption during transit, which is confirmed by the bootstrap analysis of the in-out scenario (Fig. D.1). We note the unusual trimodal distribution of the out-out scenario for the first and last night (2020-03-11 and 2021-05-03), which is likely caused by the lack of out-of-transit spectra. The measured excess absorption on the transmission spectrum is 0.05 ± 0.16 %. We put a 3-σ upper limit on the presence of helium at <0.48%, which improves the previous constraint set by dos Santos et al. (2020).

# 5. Interpretation

## 5.1. Stellar pseudo-signal

During a transit, the planet occults different stellar regions where metastable helium can be present or not. This can imprint the transmission spectrum with an absorption or emission spectral

<table><caption>**Table 6.** Strength of the maximum pseudo-absorption signal producible.</caption><thead><tr><td>Target</td><td>Pseudo-signal excess absorption [%]</td></tr></thead><tbody><tr><td>AU Mic b</td><td>~0.03</td></tr><tr><td>GJ 1214 b</td><td>~0.05</td></tr><tr><td>GJ 3470 b</td><td>~0.21</td></tr><tr><td>HAT-P-11 b</td><td>~0.02</td></tr><tr><td>HD 189733 b</td><td>~0.75</td></tr><tr><td>WASP-52 b</td><td>~0.95</td></tr><tr><td>WASP-69 b</td><td>~0.53</td></tr></tbody></table>

feature mimicking planetary signals. We studied the impact of a stellar pseudo-signal with the model described in Sect. 3.3.1 for the following planets: AU Mic b, GJ 1214 b, GJ 3470 b, HAT-P-11 b, HD 189733 b, WASP-52 b, and WASP-69 b, which are the planets where a stellar pseudo-signal could play a role on the presence of helium or its variability. For all the systems, we explored the impact of the filling factor, *f*, with values between 0.2 and 1 on the strength of the stellar pseudo-absorption signal but no significant variations were measured. Table 6 reports the maximum integrated pseudo-signal excess absorption for the different planets assuming the planets only transit bright regions and all the stellar helium absorption comes from dark regions ($α = 0$). For AU Mic b, GJ 1214 b, GJ 3470 b, and HAT-P-11 b, the impact of stellar pseudo-signal is negligible due to their small $R_p/R_★$ and cannot explain the measured excess absorptions or their variability. However, we note that in the case of GJ 3470 b, a pseudo-emission signal could reduce the helium signature amplitude by ~0.6% if the planet was only transiting dark regions ($f = 0.75$ based on Andretta et al. (2017) and a helium EW of ~270 mÅ) during our observations, and could partly explain the observed discrepancy with Palle et al. (2020). In the case of the larger planets, namely HD 189733 b, WASP-52 b, and WASP-69 b, the maximum pseudo-absorption signal from the star can contribute to the variability observed between different transits but cannot be the single cause of the He absorption seen and other processes are required. We describe in the following two subsections the extreme case of HD 189733 b where the pseudo-signal can have a similar excess absorption than the observed one and the case of HAT-P-11b as the best target to study planetary variability.

### 5.1.1. HD 189733 b: Impact of stellar variability

The measured helium EW is ~295 mÅ which is very close to the value measured by Salz et al. (2018), and sets the filling factor value to 80% (Andretta et al. 2017). As it was discussed in Salz et al. (2018) and Guilluy et al. (2020), the impact of a stellar pseudo-signal is significant for HD 189733 b (Fig. 6) due to its large $R_p/R_★$ with a value of ~0.75%, which is equivalent to the measured excess absorption on the transmission spectrum. However, it is important to note that the line shape of the pseudo-signal does not match our measured helium line shape. On the latter, there is a clear additional blueshifted signal that cannot be reproduced by pseudo-signal. In addition, the strength of the pseudo-signal slightly overestimates the observed one and requires the production of helium in the bright region as well to decrease it. Therefore, it is not possible that all the detected signal is of stellar origin, such that a significant fraction must come
<figure><img src="image_7.png" /></figure>

**Fig. 6.** Impact of stellar pseudo-signal on the transmission spectrum of HD 189733 b. Top: stellar master spectrum (black dots) with the modeled stellar spectra of bright (orange) and dark (blue) regions and both combined (dashed gray) for a filling factor of 0.8. Bottom: observed transmission spectrum in black. Average transmission spectrum caused by stellar pseudo-absorption (blue) signal. The dashed-dotted brown line is at the position of the Si I line and the dashed-dotted purple lines are at the position of the He I lines in the star (top) and planet (bottom) rest frame.

from the planet's atmosphere. However, the observed variability between transits (and instruments) might come from stellar variability.

### 5.1.2. HAT-P-11b: The advantage of its eccentric orbit

Based on Andretta et al. (2017) and an EW of the stellar helium line of ~240 mÅ, we estimate a filling factor of ~0.7. As shown in Fig. 7, the modeled stellar pseudo signal contributes ~0.02% to the absorption measured at the positions of the helium lines in the planet rest frame. This is less than the 1σ uncertainty and is due to the eccentric orbit of HAT-P-11 b, which decorrelates the planetary track from the stellar one. This strengthens the planetary origin scenario for the slight variability of the helium triplet between transits. Interestingly, the impact of stellar pseudo-signal could explain the feature visible on the red wing of

<figure><img src="image_8.png" /></figure>

**Fig. 7.** Same as Fig. 6, but for a filling factor of 0.7. Bottom: average transmission spectra caused by stellar pseudo-absorption (blue) and pseudo-emission (orange) signals.

the helium triplet in Allart et al. (2018) in absorption and here in emission depending on the occultation of bright or dark regions.

## 5.2. Atmospheric modeling

Figure 8 shows the $\Delta\chi^2$ of the atmospheric best fit model as a function of mass-loss rate and temperature of the thermosphere as derived from the *p-winds* models (Dos Santos et al. 2022). Regions of the parameter space in red are in agreement with the data, while models in blue cannot reproduce the observed transmission spectra. Some simulations did not converge properly at each altitudes due to numerical issues in *p-winds* related to high variation of the different contributions. It is consequently better to exclude them and they are represented as white regions. The hatched region of the parameter space is physically excluded based on the gravitational potential for temperature and on the energy limited for the mass-loss rate (see Sect. 3.3.2).

For the nondetections, we are able to identify regions of the parameter space that are in disagreement with the data but with a clear correlation between temperature and mass-loss rate. However, these regions are split between models with low and high mass-loss rate that both are within the data error bars. This contradiction can be explained by our choice of homogeneous
<figure><img src="image_9.png" /><figcaption>**Fig. 8.** $\Delta\chi^2$ maps of mass-loss rate and temperature for the eleven planets. Regions of the parameter space in red are in agreement with the data, while models in blue cannot reproduce the observed transmission spectra. The hatched region of the parameter space is physically excluded.</figcaption></figure>

analysis and fixed thermosphere radius to the Roche lobe. The metastable helium profiles for the models at high mass-loss rates have a large fraction of helium particles at altitudes higher than the Roche Lobe. Consequently, the quantity of metastable helium below this radius is sufficient to reproduce the nondetections observed. As described before, we do not consider these models as realistic and therefore used the 3-$\sigma$ contour of the regions of the parameter space at a low mass-loss rate to set its upper limit (Table 4). However, it was not possible to derive upper limits for GJ 1214 b, and WASP-127 b as there is always one

model at a given temperature that fit the data independently of the mass-loss rate. We note that the upper limit on the mass-loss rate of GJ 3470 b is similar to the one derived by Palle et al. (2020) of $3\times10^{10}$ g s$^{-1}$. However, we constrained less well the mass-loss rate of WASP-52 b compared to Kirk et al. (2022).

For the detections, the thermospheric radius, where the p-winds simulation is stopped, was set as a free parameter with an upper limit at the Roche Lobe along a free line-of-sight bulk velocity. We allow the thermospheric radius to be below the Roche Lobe radius in case of a compact thermosphere probed
by the helium triplet. The p-winds best-fit models are displayed in Fig. 3 for the three detections: HAT-P-11 b, HD 189733 b, and WASP-69 b, while the $\Delta\chi^2$ map of mass-loss rate and temperature is shown in Fig. 8.

The best-fit model for HAT-P-11 b is obtained for $\dot{m} = 0.67_{-0.24}^{+0.27} \cdot 10^{11} \text{ g s}^{-1}$, $T = 8726_{-557}^{+158} \text{ K}$, $v = -5.3 \pm 0.8 \text{ km s}^{-1}$ and $r = 6.5_{-1.5}^{+0} R_p$. We confirm the blueshifted nature of the helium triplet reported by Allart et al. (2018) ($v \sim -3 \text{ km s}^{-1}$), which is marginally at $2-3 \sigma$. Our results can be compared to Dos Santos et al. (2022), where the authors benchmarked the use of p-winds on the HAT-P-11 b data of Allart et al. (2018) obtained with CARMENES. The only caveat is that we let the radius free, but it cannot be higher than the limit set at the Roche Lobe, indicative of an exospheric contribution. Nonetheless, we find a good agreement with Dos Santos et al. (2022) for both the temperature and the mass-loss rate. The comparison with the results of Allart et al. (2018) is less straightforward as the authors used the 3D code EVE that simulates both the thermosphere and exosphere, which is more complex than a Parker wind model. For example, we derive a lower temperature but a higher mass-loss rate. This shows that the derivation of the physical parameters of the thermosphere highly depends on the models used and their assumptions.

The best-fit model for HD 189733 b is obtained for $\dot{m} = 0.94_{-0.60}^{+0.82} \cdot 10^{11} \text{ g s}^{-1}$, $T = 16\,690_{-2182}^{+1966} \text{ K}$, $v = -4.2 \pm 0.8 \text{ km s}^{-1}$ and $r = 1.41_{-0.03}^{+0.20} R_p$. Due to limitations of the p-winds code<fnref n="2" />, it was not possible to compute models for temperatures lower than 11 320 K, which reduced the explored parameter space. The measured blueshift is in agreement at $1-\sigma$ with the values of Salz et al. (2018) and Guilluy et al. (2020). We confirm that the region of HD 189733 b atmosphere with helium in the triplet state is hot, compact, and sizes to only ~0.2 $R_p$ (Salz et al. 2018; Guilluy et al. 2020; Lampón et al. 2021). The derived mass-loss rate is similar to Lampón et al. (2021) but they assumed an almost fully ionized atmosphere with a very low mean molecular weight of H/He = 99.2/0.8, which was necessary to fit their data.

The best-fit model for WASP-69 b is obtained for $\dot{m} = 0.40_{-0.25}^{+0.58} \cdot 10^{11} \text{ g s}^{-1}$, $T = 6987_{-1604}^{+1617} \text{ K}$, $v = -5.4 \pm 1.2 \text{ km s}^{-1}$ and $r = 2.9_{-0.9}^{+0} R_p$. We confirm the blueshifted nature of the helium triplet reported by Nortmann et al. (2018); $v = -3.58 \pm 0.23 \text{ km s}^{-1}$ compatible at $2-\sigma$ and higher velocity. The derived mass-loss rate is also consistent with 3D hydrodynamics and self-consistent photochemistry models of Wang & Dai (2021b). The best-fit model uncertainty on the radius indicates that a radius larger than the Roche Lobe could be preferred but it requires the use of more complex models to describe the exosphere (e.g., Bourrier et al. 2013; Allart et al. 2018, 2019; Allan & Vidotto 2019; Wang & Dai 2021b).

# 6. Discussion

From the upper limits and detections measured in Sect. 4, we estimated the equivalent opaque radius, which can be normalized by the planet scale height to produce the quantity $\delta R_p/H$ proposed in Nortmann et al. (2018). This quantity expresses the number of scale heights that is probed by the helium triplet in the exoplanet atmosphere. We assumed here the equilibrium temperature and a mean molecular weight of 1.3 to estimate the scale height. We explored how $\delta R_p/H$ correlates with various

system parameters: stellar mass, stellar radius, effective temperature, age, planetary mass, planetary radius, planetary density, and equilibrium temperature. We also extended the search for possible correlations with the stellar XUV flux scaled to the semi-major axis of the planets measured between 5 and 504 Å which is the part of the XUV flux responsible for the creation of metastable helium in exoplanet atmospheres (Sanz-Forcada & Dupree 2008). However, these flux values are model-dependent and are subject to various assumptions such as the age of the system (see Sect. 3.3.2). We limited the search for correlation to the sample studied here because the data were obtained with the same instrument and reduced in a homogeneous way including the report of detections and upper limits, which differs in the literature from one paper to another. We note that a trend is noticeable with stellar age (not shown), but due to the lack of precision on the stellar age and the small number of targets in our sample, it is not possible to draw more conclusions.

The top panels of Fig. 9 show the correlations for $\delta R_p/H$ with the stellar mass and the XUV flux, the two parameters showing the strongest trends. We note that the upper limit set for WASP-11 b is not constraining enough to be useful. However, more observations of this planet might reveal the presence of metastable helium as the system is quite similar to the reported detections. The correlation with the stellar mass is well identified where the presence of metastable helium around exoplanet is favored for planets orbiting stars with masses between ~0.6 and ~0.85 $M_\odot$, which corresponds to K dwarfs as predicted by Oklopčić (2019). This range of stellar mass also agrees with previous detections and nondetections published in Kasper et al. (2020); Casasayas-Barris et al. (2021); Zhang et al. (2022b, 2023) for example. However, it is in contradiction with the detection of helium obtained for HD 209458 b by Alonso-Floriano et al. (2019b) or for HAT-P-32b by Czesla et al. (2022) for which the stellar masses are ~1.2 $M_\odot$. We can also identify a range of XUV flux received by the planets that seems to favor the presence of metastable helium between 1 400 and 17 800 erg s$^{-1}$·cm$^{-2}$. Nethertheless, as discussed above, these XUV values are model-dependent and linked to the stellar ages, which is usually not well constrained. We see that on the one hand WASP-39 b and WASP-127 b receive less XUV flux while orbiting G-type stars, and are the oldest planets studied here. On the other hand AU Mic b, WASP-52 b, and WASP-80 b are the youngest planets and receive the highest amount of XUV flux. It is also interesting to note that WASP-52 b, for which we have a contradictory result with Kirk et al. (2022), is well above the favored range of XUV flux range even with a well-constrained age, which is in contrast with its proximity to the acceptable range of stellar mass that seems to favor the presence of metastable helium.

The bottom panels of Fig. 9 show the correlations for $\dot{m}$ with the stellar mass and the XUV flux. The use of $\dot{m}$ should be preferred to the $\delta R_p/H$ as it is a more physical quantity to describe the thermosphere probed by the helium triplet. Indeed, the $\delta R_p/H$ quantity assumes H and He particles in their neutral state only and at the equilibrium temperature of the planet, which is much lower than the thermospheric temperature. However, the correlations between $\dot{m}$ with stellar mass and XUV flux are not well defined as upper limits on $\dot{m}$ are in agreement with some of the derived $\dot{m}$ for detections. This can be linked to the correlation reported in Sect. 5 between $\dot{m}$ and $T$. We note that the best upper limits on $\dot{m}$ are for WASP-11b and WASP-80b, while they have poorly constrained $\delta R_p/H$ as opposed to AU Mic b, GJ 3470 b, WASP-39 b and WASP-52 b. This is surprising for WASP-11 b as all the planets within the same stellar mass and XUV flux range

<footnote n="2">² Some differential equations cannot be solved depending of the initial parameters.</footnote>
<figure><img src="image_10.png" /><figcaption>**Fig. 9.** Correlation plots for the eleven planets studied in this paper. Detections are shown as blue points and upper limits as orange points. We pinpointed with a gray area the parameter space that seems to favor the detection of metastable helium in exoplanet atmospheres. Top left: $\delta R_p/H$ as a function of the stellar mass. Top right: $\delta R_p/H$ as a function of XUV flux received from 5 to 504 Å. Bottom left: mass-loss rate derived from the p-winds simulations as a function of the stellar mass. Bottom right: mass-loss rate derived from the p-winds simulations as a function of XUV flux received from 5 to 504 Å.</figcaption></figure>

have clear detections and higher $\dot{m}$. Interestingly, based on their gravitational potential all the planets studied here are expected to fall in the strong hydrodynamic wind regime (intermediate regime for HD 189733 b) and thus undergo strong evaporation (Salz et al. 2016). However, we do not observe signatures of the helium triplet for most of our targets. This discrepancy already reported by Fossati et al. (2022) or Vissapragada et al. (2022b) could be the result of more complex mechanisms not integrated in 1D hydrodynamical codes. Although, a simpler explanation can be found in the population of the metastable helium triplet. The strength of those helium lines does not depend on the evaporation rate but on the mid-UV flux ionizing the metastable helium particles and on the EUV flux populating the triplet state through recombination. Based on the metastable helium population mechanisms, Oklopčić (2019) suggested that planets orbiting K type stars and receiving the right balance of mid-UV and EUV flux are the most amenable to probe the evaporation through the helium triplet. To summarize, even if for the planets with non detection of the helium triplet strong evaporation can happen, but this process is not traced by the helium triplet as most of the helium particles are in the ground state.

## 7. Summary and conclusion

This paper presents the first homogeneous analysis of the metastable helium triplet for eleven exoplanets observed with a single high-resolution near-infrared spectrograph, SPIRou. We confirmed detection of He triplets in the atmosphere of HAT-P-11 b, HD 189733 b, and WASP-69 b. We obtained upper limits for GJ 3470 b and WASP-52 b, that disagree with previously published papers. We set new or confirm upper limits for AU Mic b, WASP-11 b, WASP-39 b, WASP-80 b, and WASP-127 b. We finally obtained an upper limit for GJ 1214 b, which is not constraining enough to settle the debate on the presence of helium.

We note that the SPIRou transmission spectra are affected by various systematics that are difficult to understand and to properly remove. We mitigated them by scaling our uncertainties but more robust approaches could be considered by combining Gaussian processes with model fitting algorithm (out of the scope of this paper). They can be caused by the low data quality (e.g., close to readout regime), instrumental effects, reduction pipeline errors, or stellar variability like in the case of AU Mic b. Nonetheless, we set $3-\sigma$ upper limits which are as representatives
as possible of these systematics and assuming a given helium line width.

We estimated the impact of stellar-pseudo signal on the observed helium features with a simple toy model. We concluded that none of the detections could solely be explained by such an effect, but that could contribute to some of the variability observed between transits and instruments. A more complex model would be needed to take into account the complexity of stellar surfaces and their occultation by planets combined with the intrinsic variability of the stellar flux in various wavelength domains. To better understand the impact of stellar variability on the presence of metastable helium in exoplanet atmospheres, applying homogeneous analysis of multiple stellar and planetary tracers (e.g., Na, H-α, He) as presented in Guilluy et al. (2020); Czesla et al. (2022) will be necessary for the future. Instruments like CARMENES, GIANO simultaneously to HARPS-N, SPIRou simultaneously to ESPaDOnS (in a near future), and NIRPS simultaneously to HARPS will have an edge to disentangle multisource effects. Among the three detections, HD 189733 b is probably the one most impacted by stellar variability and requires specific analysis to properly extract the true planetary signature. However, HAT-P-11 b emerges as the best candidate to search for temporal planetary variability signature as it is completely free of stellar contamination, and variability in the CARMENES data (Allart et al. 2018) still have to be explained.

The transmission spectra of the 11 planets were modeled with p-winds (Dos Santos et al. 2022). We excluded models at high temperatures and mass-loss rates to stay in a physical thermosphere assumption based on the gravitational potential of the planet and the maximum mass-loss efficiency for a photoionization-driven isothermal Parker wind (Vissapragada et al. 2022a). We also fixed the radius of the thermosphere to the Roche Lobe for the nondetections to derive reasonable constraints. However, we note that discussions on the criteria to set the radius are missing in the literature. Upper limits on the mass-loss rate were derived for all the nondetections with the exception of GJ 1214 b and WASP-127 b. In the case of the detections, we found a constant day-to-night side zonal wind for the three planets with hot thermospheres but a relatively low mass-loss rate, which is consistent with previous findings. While HD 189733 b is confirmed to have a shallow metastable helium atmosphere, HAT-P-11 b, and WASP-69 b tend to have a more extended thermosphere with possibly a small exosphere.

The correlation between $\delta R_p$/H and $M_★$ confirms that planets around K dwarfs are favored to have metastable helium in their atmosphere as proposed in Oklopčić (2019). The correlation between $\delta R_p$/H and XUV flux proposed and described in several studies also seems to remain a good indicator, but is much more model-dependent that with the stellar mass, and thus requires caution when comparing studies. We also point out that the EUV emission is linked to the coronal heavy element abundance and thus to the stellar metallicity (Poppenhaeger 2022). The use of the *in* instead of $\delta R_p$/H should be utilized more as it is physically more representative of exoplanet thermospheres, although it remains ambiguous to draw a strong conclusion at the population level for now. This could be improved by gathering higher quality datasets even for nondetections. Future studies and proposals could use as guidelines the $\delta R_p$/H versus $M_★$ correlation to build robust science cases as it is the less model-dependent correlation but one should not forget that studying planets outside this soft spot can turn out to be as important.

Finally, we want to draw attention to the necessity of building reproducible observations from the proposal phase taking

into account weather losses to get robust results. This lack of reproducibility for helium studies is frequent and calls for more than one transit observation per target. In this context, the NIRPS consortium will observe over 5 yr more than 75 gas-dominated planets with at least two transits for each of them as part of its Guaranteed Time Observations (GTO) program. It will, therefore, provide an extended sample to study exoplanet atmospheres as a population, unlocking constraints on the origin of the Neptunian desert and planet evolution.

**Acknowledgements.** Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated from the summit of Maunakea by the National Research Council of Canada, the Institut National des Sciences de l'Université du Centre National de la Recherche Scientifique of France, and the University of Hawaii. The observations at the Canada-France-Hawaii Telescope were performed with care and respect from the summit of Maunakea which is a significant cultural and historic site. We thank the anonymous referee for their comments that improved the overall quality of this work. R.A. is a Trottier Post-doctoral Fellow and acknowledges support from the Trottier Family Foundation. This work was supported in part through a grant from the Fonds de Recherche du Québec - Nature et Technologies (FRQNT). This work was funded by the Institut Trottier de Recherche sur les Exoplanètes (iREx). D.L., R.D. and M.R. would like to acknowledge funding from the National Sciences and Research Council of Canada (NSERC). This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (project SPICE DUNE, grant agreement No 947634; grant agreement no. 730890, project SACCRED, grant agreement No 716155, project ASTROFLOW, grant agreement no. 817540). J.D.T. was supported for this work by NASA through the NASA Hubble Fellowship grant #HST-HF2-51495.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. J.F.D. acknowledges funding from the European Research Council (ERC) under the H2020 research & innovation programme (grant agreement #740651 NewWorlds). We acknowledge funding from the French ANR under contract number ANR18CE310019 (SPiLaSH). A.C. and X.D. acknowledge funding from the Investissements d'Avenir program (ANR-15-IDEX-02), through the funding of the "Origin of Life" project of the Grenoble-Alpes University.

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¹ Département de Physique, Institut Trottier de Recherche sur les Exoplanètes, Université de Montréal, Montréal, Québec H3T 1J4, Canada
e-mail: romain.allart@umontreal.ca

² Observatoire astronomique de l'Université de Genève, Université de Genève, chemin Pegasi 51, 1290 Versoix, Switzerland

³ Gemini Observatory, NSF's NOIRLab, Casilla 603, La Serena, Chile

⁴ Université Grenoble Alpes, CNRS, IPAG. 38000 Grenoble, France

⁵ Dept. of Physics & Astronomy, McMaster University, 1280 Main St West, Hamilton, ON L8S 4L8, Canada

⁶ Department of Physics, McGill University, 3600 rue University, Montréal, QC H3A 2T8, Canada

⁷ Department of Earth & Planetary Sciences, McGill University, 3450 rue University, Montréal, QC H3A 0E8, Canada

⁸ Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, 14 avenue Édouard Belin, 31400, Toulouse, France

⁹ Department of Earth Sciences, University of Hawai'i at Manoa, Honolulu, HI 96822, USA

¹⁰ Institute of Astronomy and Astrophysics, Academia Sinica, Taipei 10617, Taiwan

¹¹ Institut d'Astrophysique de Paris, CNRS, UMR 7095, Sorbonne Université, 98 bis bd Arago, 75014 Paris, France

¹² Observatoire de Haute-Provence, 1912 Route de l'Observatoire, 04870 St Michel l'Observatoire, France

¹³ LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Cité, 5 place Jules Janssen, 92195 Meudon, France

¹⁴ Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network (ELKH), Konkoly-Thege Miklós út 15–17, 1121 Budapest, Hungary

¹⁵ CSFK, MTA Centre of Excellence, Konkoly-Thege Miklós út 15–17, 1121 Budapest, Hungary

¹⁶ ELTE Eötvös Loránd University, Institute of Physics, Pázmány Péter sétány 1/A, 1117 Budapest, Hungary

¹⁷ Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany

¹⁸ Department of Astronomy, Cornell University, Ithaca, NY 14853, USA

¹⁹ Laboratório Nacional de Astrofísica, Rua Estados Unidos 154, Itajubá, MG 37504364, Brazil

²⁰ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA

²¹ Institute of Astronomy and Astrophysics, Academia Sinica, Taipei 10617, Taiwan

²² Department of Astronomy and Carl Sagan Institute, Cornell University, 122 Sciences Drive, Ithaca, NY 14853, USA

²³ Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
Appendix A: Master out spectra

<figure><img src="image_11.png" /><figcaption>Fig. A.1: Master out spectra before (gray) and after (black) telluric correction for each time series of the eleven planets. The vertical blue dashed lines indicate the helium lines' positions.</figcaption></figure>
Appendix B: Transmission spectroscopy map

<figure><img src="image_12.png" /><figcaption>Fig. B.1: Transmission spectroscopy maps in the star rest frame for each transit of the eleven planets. The dark dashed horizontal lines are the contact lines from bottom to top: *t*₁, *t*₂, *t*₃, and *t*₄. The orange dashed lines indicate the helium lines' positions in the planet rest frame. The vertical pink dashed lines indicate the helium lines' positions in the star rest frame.</figcaption></figure>
Appendix C: Red noise contribution

<figure><img src="image_13.png" /><figcaption>Fig. C.1: Allan plot estimated on the average transmission spectra of the eleven planets. The dark dotted lines correspond to the white noise as function of the bin size. The white noise on 1 original pixel is estimated as the standard deviation of the transmission spectrum. The red dotted curves are the standard deviation of the transmission spectrum after various binning size. The dashed blue lines are the best fit applied of the reds curves.</figcaption></figure>
Appendix D: Bootstrap simulation

<figure><img src="image_14.png" /><figcaption>Fig. D.1: Bootstrap analysis for each transit of the eleven planets in the star rest frame. The red, blue, and black distributions correspond to the out-out, in-in, and in-out random scenarios with 10000 iterations.</figcaption></figure>