pith. sign in

arxiv: 2605.16491 · v1 · pith:Q5IONUONnew · submitted 2026-05-15 · 🌌 astro-ph.EP

Spinning out of focus: The challenge of rotational line broadening in exoplanet reflection spectroscopy

T. O. Winterhalder , K. Molaverdikhani , D. Cont , F. Yan , E. Nagel , A. Kaminski , L. Nortmann , P. J. Amado
show 12 more authors
V. J. S. B\'ejar G. Bergond J. A. Caballero S. Czesla Th. Henning G. Morello D. Montes E. Palle A. Quirrenbach A. Reiners I. Ribas A. Schweitzer
This is my paper

Pith reviewed 2026-05-19 21:58 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords exoplanet reflection spectroscopyrotational line broadeninghigh-resolution spectroscopyspin-orbit misalignmentKELT-9CARMENESinjection-recovery test
0
0 comments X

The pith

Rotational broadening hides reflected exoplanet signals unless properly modeled in misaligned systems.

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

The paper examines why high-resolution searches for light reflected from exoplanet daysides have failed so far. It introduces a reflection spectroscopy metric to rate how suitable different star-planet systems are for such detections. The authors select the KELT-9 system, whose star spins rapidly and is strongly misaligned with the planet orbit, as a test case using CARMENES spectra. An injection-recovery experiment shows that the reflected spectrum is strongly broadened by the star's rotation, lowering the cross-correlation signal and explaining the non-detection. The work demonstrates that models must include both stellar rotation and spin-orbit misalignment to judge whether a reflection signal should be visible.

Core claim

In systems with rapidly rotating stars and large spin-orbit misalignments, the reflected planetary spectrum experiences significant rotational line broadening. This broadening reduces the contrast of the signal in cross-correlation analyses, making detection more difficult. The injection-recovery test on the KELT-9 CARMENES time series confirms that templates without this broadening overestimate detectability, while properly broadened templates show the signal is likely below the noise threshold. The non-detection in the real data aligns with these broadened expectations.

What carries the argument

The reflection spectroscopy metric that scores system favorability together with the rotational broadening kernel applied to the injected planetary reflection template in the injection-recovery test.

If this is right

  • Reflection spectroscopy favorability assessments must include stellar rotation rate and spin-orbit angle.
  • Rapidly rotating, misaligned systems like KELT-9 are less promising targets than their other properties suggest.
  • Previous non-detections may partly stem from unaccounted line broadening rather than absence of the signal.
  • Future template matching for reflection searches should convolve the planetary spectrum with the appropriate stellar rotation kernel.

Where Pith is reading between the lines

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

  • The metric could be used to rank other known hot Jupiters and identify better-suited targets with slower rotators and aligned orbits.
  • Incorporating broadening may change the estimated number of hours needed to reach a given detection significance in similar systems.
  • The approach might generalize to transmission spectroscopy where stellar rotation and misalignment also affect line profiles.

Load-bearing premise

The modeled rotational broadening kernel and the injected signal template accurately represent the true reflected spectrum shape and noise properties in the CARMENES KELT-9 time series.

What would settle it

A clear recovery of the injected reflected signal when the template includes the measured rotational broadening kernel, or a failure to recover it even after broadening is added, would test the claim.

Figures

Figures reproduced from arXiv: 2605.16491 by A. Kaminski, A. Quirrenbach, A. Reiners, A. Schweitzer, D. Cont, D. Montes, E. Nagel, E. Palle, F. Yan, G. Bergond, G. Morello, I. Ribas, J. A. Caballero, K. Molaverdikhani, L. Nortmann, P. J. Amado, S. Czesla, Th. Henning, T. O. Winterhalder, V. J. S. B\'ejar.

Figure 1
Figure 1. Figure 1: Declination of the 50 targets presenting the largest RSM′ values as a function of their respective score. The ten most favourable targets are annotated with their names. The areas of the data points scale with the planetary radii. For reference, an exemplary data point corresponding to 1 RJup is shown in the bottom right. The colour of a given data point indicates the respective planetary equilibrium tempe… view at source ↗
Figure 2
Figure 2. Figure 2: Orbital coverage of the CARMENES dataset used in this study. The spectra were taken on 30 August 2021 between orbital phases of 0.58 and 0.66, here indicated in orange. The secondary eclipse range around φ = 0.5 is indicated in grey. mated procedure was triggered during the exposure in question and contaminated the recorded science spectrum. We decided to discard the exposure, thereby incurring a loss of 2… view at source ↗
Figure 3
Figure 3. Figure 3: Reflection template of KELT-9 b. The inset in the lower right shows a close-up of the template compared to two rotationally broad￾ened versions of the model. the effects of rotational line broadening on the reflection spec￾trum of an exoplanet. Due to the varying stellar rotational velocity perceived by the planet, the foundation of a reflection template adequate for the KELT-9 system must lie in the an un… view at source ↗
Figure 5
Figure 5. Figure 5: Injection-recovery tests of KELT-9 b for different geometric albedo, Ag, and net rotational velocity, 3rot, values. The panels show S/N maps resulting from the cross-correlation of the reflection template with the CARMENES dataset, into which the respective artificial reflection signals were injected beforehand. The rotational velocity used to broaden the injected signal as well as the template increases t… view at source ↗
Figure 6
Figure 6. Figure 6: Sensitivity region of a reflection study applied to the CARMENES dataset. The blue colour map shows the corrected S/N as a function of the planet’s geometric albedo as well as the velocity used for the rotational line broadening of the artificial signal. The dashed white lines indicate different corrected S/N contours, with the S/Nc = 5 contour delineating the region where a robust detection based on the C… view at source ↗
read the original abstract

Detecting light reflected off the dayside of an exoplanet in high-resolution spectroscopic data has proved to be a notoriously difficult endeavour. Despite several attempts, the faint signal has yet to be detected. We present a new effort at finding reflection signatures and show how a strong rotational broadening of the reflected spectrum can complicate this objective. We introduce a new figure of merit that quantifies the favourability of different systems for a reflection study, the reflection spectroscopy metric. Applying this metric, we identify the KELT-9 system, which features a highly misaligned, rapidly rotating host star, as the target for a case study based on a spectroscopic time series obtained by CARMENES. We also perform an injection-recovery test to determine the detectability of the signal in our data and demonstrate its sensitivity to rotational line broadening. The search for a genuine reflection signal in our data resulted in a non-detection. The injection-recovery test puts this finding into context by revealing the critical importance of taking rotational broadening into account when dealing with systems featuring rapidly rotating stars and large spin-orbit misalignments. The case study presented here underscores the need to incorporate stellar rotation and spin-orbit misalignment into assessments of a given planet's favourability to reflection studies.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

1 major / 2 minor

Summary. The manuscript introduces a new 'reflection spectroscopy metric' to quantify the favorability of exoplanet systems for detecting reflected light in high-resolution spectra. Applying the metric, the authors identify the KELT-9 system (rapidly rotating host with large spin-orbit misalignment) as a case study, analyze a CARMENES time series, report a non-detection of the planetary reflection signal, and use an injection-recovery test to argue that rotational line broadening must be accounted for in such systems.

Significance. If the injection-recovery test is shown to be faithful to the data, the work identifies a previously under-emphasized observational obstacle—rotational broadening in misaligned, fast-rotating systems—that can dilute or obscure reflected-light signals. The new metric offers a concrete, parameter-based way to rank targets and could usefully inform future observing proposals with instruments such as CARMENES, ESPRESSO, or ANDES.

major comments (1)
  1. [Abstract / injection-recovery test] Abstract and injection-recovery section: the central claim that the test 'reveals the critical importance of taking rotational broadening into account' rests on an unverified match between the modeled broadening kernel (constructed from v sin i, spin-orbit angle, and line profiles) and the actual shape plus noise properties of the CARMENES KELT-9 reflected spectrum. No quantitative validation (e.g., cross-check against stellar spectra, residual analysis after injection, or comparison of recovered vs. injected line depths) is provided, leaving open the possibility that the reported sensitivity to broadening is an artifact of the template or noise model rather than a genuine observational limit.
minor comments (2)
  1. [Abstract] The abstract would benefit from a single sentence stating the numerical value of the reflection spectroscopy metric for KELT-9 and the detection threshold (e.g., S/N or significance) adopted in the injection test.
  2. [Methods / metric definition] Notation for the broadening kernel and the reflection spectroscopy metric should be defined explicitly the first time each appears, even if the definitions are standard in the field.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive feedback on our manuscript. We address the single major comment below and agree that additional validation will improve the presentation of the injection-recovery results.

read point-by-point responses

  1. Referee: [Abstract / injection-recovery test] Abstract and injection-recovery section: the central claim that the test 'reveals the critical importance of taking rotational broadening into account' rests on an unverified match between the modeled broadening kernel (constructed from v sin i, spin-orbit angle, and line profiles) and the actual shape plus noise properties of the CARMENES KELT-9 reflected spectrum. No quantitative validation (e.g., cross-check against stellar spectra, residual analysis after injection, or comparison of recovered vs. injected line depths) is provided, leaving open the possibility that the reported sensitivity to broadening is an artifact of the template or noise model rather than a genuine observational limit.

    Authors: We acknowledge that the submitted manuscript does not present explicit quantitative checks such as direct comparisons of the modeled kernel to independent stellar spectra or detailed residual maps after injection. The injection-recovery procedure does, however, embed the full modeled kernel (derived from the literature values of v sin i and the spin-orbit angle together with a line profile taken from the CARMENES data themselves) directly into the real observed time series; this ensures that the noise properties, instrumental systematics, and data-reduction steps are identical to those affecting any putative planetary signal. The sensitivity to broadening is shown by the difference in recovery statistics between runs performed with and without the kernel applied. To meet the referee’s request for stronger validation, we will add a dedicated subsection and accompanying figure in the revised manuscript that (i) overlays the modeled kernel on the average observed stellar line profile, (ii) reports the residuals after kernel subtraction, and (iii) tabulates the recovered versus injected line depths for both broadened and unbroadened cases. revision: yes

Circularity Check

0 steps flagged

No significant circularity: new metric and injection test are independent of fitted inputs

full rationale

The paper defines a new reflection spectroscopy metric from independently measured stellar and orbital parameters (v sin i, spin-orbit angle, etc.) and applies it to select KELT-9. The injection-recovery test then injects a modeled template into real CARMENES data to assess detectability under rotational broadening; this is an external simulation check rather than a quantity defined by the paper's own fit or self-citation chain. No step reduces by construction to its inputs, no load-bearing self-citation is invoked for a uniqueness theorem, and the non-detection result stands separate from the test. The derivation chain is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The paper rests on standard assumptions of high-resolution spectroscopy and introduces one new composite metric; no new physical entities or free parameters are described in the abstract.

axioms (1)
  • domain assumption Rotational line broadening due to stellar rotation and spin-orbit misalignment is the dominant factor limiting reflected-light detectability in the KELT-9 system.
    This premise is invoked to explain both the non-detection and the injection-recovery results.

pith-pipeline@v0.9.0 · 5855 in / 1334 out tokens · 63833 ms · 2026-05-19T21:58:58.955292+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

129 extracted references · 129 canonical work pages · 34 internal anchors

  1. [1]

    Clouds in the atmospheres of extrasolar planets. II. Thermal emission spectra of Earth-like planets influenced by low and high-level clouds. , keywords =. doi:10.1051/0004-6361/201014343 , archivePrefix =. 1105.3568 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201014343

  2. [2]

    Albedo and Reflection Spectra of Extrasolar Giant Planets

    Albedo and Reflection Spectra of Extrasolar Giant Planets. , keywords =. doi:10.1086/309160 , archivePrefix =. astro-ph/9910504 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/309160

  3. [3]

    The Albedos of Kepler's Close-in super-Earths

    The Albedos of Kepler's Close-in Super-Earths. , keywords =. doi:10.1088/2041-8205/789/1/L20 , archivePrefix =. 1405.3798 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/789/1/l20 2041

  4. [4]

    , keywords =

    Reflected Spectroscopy of Small Exoplanets II: Characterization of Terrestrial Exoplanets. , keywords =. doi:10.3847/1538-3881/ac6b97 , archivePrefix =. 2204.13816 , primaryClass =

    work page doi:10.3847/1538-3881/ac6b97

  5. [5]

    , keywords =

    EXOREL \ \ \ \^\ \ \ R\ \ \ : A Bayesian Inverse Retrieval Framework for Exoplanetary Reflected Light Spectra. , keywords =. doi:10.3847/1538-3881/ab79a5 , archivePrefix =. 2003.01814 , primaryClass =

    work page doi:10.3847/1538-3881/ab79a5 2003

  6. [6]

    , keywords =

    Information in the Reflected-light Spectra of Widely Separated Giant Exoplanets. , keywords =. doi:10.3847/1538-4357/ab58c7 , archivePrefix =. 1911.06274 , primaryClass =

    work page doi:10.3847/1538-4357/ab58c7 1911

  7. [7]

    A giant planet undergoing extreme ultraviolet irradiation by its hot massive-star host

    A giant planet undergoing extreme-ultraviolet irradiation by its hot massive-star host. , keywords =. doi:10.1038/nature22392 , archivePrefix =. 1706.06723 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature22392

  8. [8]

    , keywords =

    Nodal Precession and Tidal Evolution of Two Hot Jupiters: WASP-33 b and KELT-9 b. , keywords =. doi:10.3847/1538-4357/ac6b9a , archivePrefix =. 2203.02546 , primaryClass =

    work page doi:10.3847/1538-4357/ac6b9a

  9. [9]

    Theoretical Transmission Spectra During Extrasolar Giant Planet Transits

    Theoretical Transmission Spectra during Extrasolar Giant Planet Transits. , keywords =. doi:10.1086/309088 , archivePrefix =. astro-ph/9912241 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/309088

  10. [10]

    Thermal structure of an exoplanet atmosphere from phase-resolved emission spectroscopy

    Thermal structure of an exoplanet atmosphere from phase-resolved emission spectroscopy. Science , keywords =. doi:10.1126/science.1256758 , archivePrefix =. 1410.2241 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1256758

  11. [11]

    An Upper Limit on the Reflected Light from the Planet Orbiting the Star tau Bootis

    An Upper Limit on the Reflected Light from the Planet Orbiting the Star Bootis. , keywords =. doi:10.1086/312234 , archivePrefix =. astro-ph/9907195 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/312234

  12. [12]

    Probable detection of starlight reflected from the giant exoplanet orbiting tau Bootis

    Probable detection of starlight reflected from the giant planet orbiting Bo \"o tis. , keywords =. doi:10.1038/45451 , archivePrefix =. astro-ph/9911314 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/45451

  13. [13]

    tau Boo b: Not so bright, but just as heavy

    tau Boo b: Not so bright, but just as heavy. arXiv e-prints , keywords =. doi:10.48550/arXiv.astro-ph/0012186 , archivePrefix =. astro-ph/0012186 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0012186

  14. [14]

    , keywords =

    A new upper limit on the reflected starlight from Bootis b. , keywords =. doi:10.1046/j.1365-8711.2003.06901.x , archivePrefix =. astro-ph/0308413 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06901.x 2003

  15. [15]

    Tau Boo b: Hunting for reflected starlight

    Bo \"o tis b: Hunting for reflected starlight. , keywords =. doi:10.1051/0004-6361/200913627 , archivePrefix =. 1002.1638 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200913627

  16. [16]

    The Exoplanet Handbook

    work page

  17. [17]

    Handbook of Exoplanets , year = 2018, editor =

    Exoplanet Atmosphere Measurements from Transmission Spectroscopy and Other Planet Star Combined Light Observations. Handbook of Exoplanets , year = 2018, editor =. doi:10.1007/978-3-319-55333-7_100 , adsurl =

    work page doi:10.1007/978-3-319-55333-7_100 2018

  18. [18]

    , keywords =

    A search for starlight reflected from And's innermost planet. , keywords =. doi:10.1046/j.1365-8711.2002.05084.x , archivePrefix =. astro-ph/0110577 , primaryClass =

    work page doi:10.1046/j.1365-8711.2002.05084.x 2002

  19. [19]

    A map of the day-night contrast of the extrasolar planet HD 189733b

    A map of the day-night contrast of the extrasolar planet HD 189733b. , keywords =. doi:10.1038/nature05782 , archivePrefix =. 0705.0993 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature05782

  20. [20]

    Exoplanet Classification and Yield Estimates for Direct Imaging Missions

    Exoplanet Classification and Yield Estimates for Direct Imaging Missions. , keywords =. doi:10.3847/1538-4357/aab205 , archivePrefix =. 1802.09602 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aab205

  21. [21]

    Searching for reflected light from $\tau$ Bootis b with high-resolution ground-based spectroscopy: Approaching the $10^{-5}$ contrast barrier

    Searching for reflected light from Bootis b with high-resolution ground-based spectroscopy: Approaching the 10 ^ -5 contrast barrier. , keywords =. doi:10.1051/0004-6361/201731192 , archivePrefix =. 1711.05334 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201731192

  22. [22]

    Spectral Atlas for Amateur Astronomers: A Guide to the Spectra of Astronomical Objects and Terrestrial Light Sources , Chapter=

    Walker, Richard , year=. Spectral Atlas for Amateur Astronomers: A Guide to the Spectra of Astronomical Objects and Terrestrial Light Sources , Chapter=

    work page

  23. [23]

    Large Interferometer For Exoplanets (LIFE). I. Improved exoplanet detection yield estimates for a large mid-infrared space-interferometer mission. , keywords =. doi:10.1051/0004-6361/202140366 , archivePrefix =. 2101.07500 , primaryClass =

    work page doi:10.1051/0004-6361/202140366

  24. [24]

    The NASA Exoplanet Archive: Data and Tools for Exoplanet Research

    The NASA Exoplanet Archive: Data and Tools for Exoplanet Research. , keywords =. doi:10.1086/672273 , archivePrefix =. 1307.2944 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/672273

  25. [25]

    , keywords =

    Three New ``51 Pegasi-Type'' Planets. , keywords =. doi:10.1086/310444 , adsurl =

    work page doi:10.1086/310444

  26. [26]

    Near-IR Direct Detection of Water Vapor in Tau Boo b

    Near-IR Direct Detection of Water Vapor in Tau Bo \"o tis b. , keywords =. doi:10.1088/2041-8205/783/2/L29 , archivePrefix =. 1402.0846 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/783/2/l29 2041

  27. [27]

    A Framework for Prioritizing the TESS Planetary Candidates Most Amenable to Atmospheric Characterization

    A Framework for Prioritizing the TESS Planetary Candidates Most Amenable to Atmospheric Characterization. , keywords =. doi:10.1088/1538-3873/aadf6f , archivePrefix =. 1805.03671 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1538-3873/aadf6f

  28. [28]

    Ground-based and Airborne Instrumentation for Astronomy V , year = 2014, editor =

    CARMENES instrument overview. Ground-based and Airborne Instrumentation for Astronomy V , year = 2014, editor =. doi:10.1117/12.2056453 , adsurl =

    work page doi:10.1117/12.2056453 2014

  29. [29]

    Ground-based and Airborne Instrumentation for Astronomy VI , year = 2016, editor =

    CARMENES: an overview six months after first light. Ground-based and Airborne Instrumentation for Astronomy VI , year = 2016, editor =. doi:10.1117/12.2231880 , adsurl =

    work page doi:10.1117/12.2231880 2016

  30. [30]

    Ground-based and Airborne Instrumentation for Astronomy V , year = 2014, editor =

    CRIRES+: a cross-dispersed high-resolution infrared spectrograph for the ESO VLT. Ground-based and Airborne Instrumentation for Astronomy V , year = 2014, editor =. doi:10.1117/12.2054197 , adsurl =

    work page doi:10.1117/12.2054197 2014

  31. [31]

    , keywords =

    Line-profile tomography of exoplanet transits - II. A gas-giant planet transiting a rapidly rotating A5 star. , keywords =. doi:10.1111/j.1365-2966.2010.16922.x , archivePrefix =. 1004.4551 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.16922.x 2010

  32. [32]

    , author Padovani, P

    Thermal emission from WASP-33b, the hottest known planet. , keywords =. doi:10.1111/j.1365-2966.2011.19187.x , archivePrefix =. 1101.2432 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.19187.x 2011

  33. [33]

    A ground-based NUV secondary eclipse observation of KELT-9b

    A Ground-based Near-ultraviolet Secondary Eclipse Observation of KELT-9b. , keywords =. doi:10.3847/2041-8213/aaf6a9 , archivePrefix =. 1812.02773 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aaf6a9 2041

  34. [34]

    petitRADTRANS: a Python radiative transfer package for exoplanet characterization and retrieval

    petitRADTRANS. A Python radiative transfer package for exoplanet characterization and retrieval. , keywords =. doi:10.1051/0004-6361/201935470 , archivePrefix =. 1904.11504 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201935470 1904

  35. [35]

    Atomic iron and titanium in the atmosphere of the exoplanet KELT-9b

    Atomic iron and titanium in the atmosphere of the exoplanet KELT-9b. , keywords =. doi:10.1038/s41586-018-0401-y , archivePrefix =. 1808.05653 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41586-018-0401-y

  36. [36]

    , keywords =

    Neutral Iron Emission Lines from the Dayside of KELT-9b: The GAPS Program with HARPS-N at TNG XX. , keywords =. doi:10.3847/2041-8213/ab8c44 , archivePrefix =. 2004.11335 , primaryClass =

    work page doi:10.3847/2041-8213/ab8c44 2041

  37. [37]

    Carbon monoxide and water vapor in the atmosphere of the non-transiting exoplanet HD 179949 b

    Carbon monoxide and water vapor in the atmosphere of the non-transiting exoplanet HD 179949 b. , keywords =. doi:10.1051/0004-6361/201423537 , archivePrefix =. 1404.3769 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201423537

  38. [38]

    The Influence of Host Star Spectral Type on Ultra-Hot Jupiter Atmospheres

    The Influence of Host Star Spectral Type on Ultra-hot Jupiter Atmospheres. , keywords =. doi:10.3847/1538-4357/ab1485 , archivePrefix =. 1903.12183 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab1485 1903

  39. [39]

    A new extensive library of PHOENIX stellar atmospheres and synthetic spectra

    A new extensive library of PHOENIX stellar atmospheres and synthetic spectra. , keywords =. doi:10.1051/0004-6361/201219058 , archivePrefix =. 1303.5632 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201219058

  40. [40]

    Molecfit: A general tool for telluric absorption correction. I. Method and application to ESO instruments. , keywords =. doi:10.1051/0004-6361/201423932 , archivePrefix =. 1501.07239 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201423932

  41. [41]

    Molecfit: A general tool for telluric absorption correction. II. Quantitative evaluation on ESO-VLT/X-Shooterspectra. , keywords =. doi:10.1051/0004-6361/201423909 , archivePrefix =. 1501.07265 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201423909

  42. [42]

    The orbital motion, absolute mass, and high-altitude winds of exoplanet HD209458b

    The orbital motion, absolute mass and high-altitude winds of exoplanet HD209458b. , keywords =. doi:10.1038/nature09111 , archivePrefix =. 1006.4364 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature09111

  43. [43]

    The signature of orbital motion from the dayside of the planet tau Bootis b

    The signature of orbital motion from the dayside of the planet Bo \"o tis b. , keywords =. doi:10.1038/nature11161 , archivePrefix =. 1206.6109 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature11161

  44. [44]

    Weighing The Non-Transiting Hot Jupiter Tau BOO b

    Weighing the Non-transiting Hot Jupiter Boo b. , keywords =. doi:10.1088/2041-8205/753/1/L25 , archivePrefix =. 1206.6197 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/753/1/l25 2041

  45. [45]

    The GAPS Programme at TNG. XLI. The climate of KELT-9b revealed with a new approach to high-spectral-resolution phase curves. , keywords =. doi:10.1051/0004-6361/202244593 , archivePrefix =. 2209.11735 , primaryClass =

    work page doi:10.1051/0004-6361/202244593

  46. [46]

    , keywords =

    Confirmation of Iron Emission Lines and Nondetection of TiO on the Dayside of KELT-9b with MAROON-X. , keywords =. doi:10.3847/2041-8213/ac30e1 , archivePrefix =. 2108.08389 , primaryClass =

    work page doi:10.3847/2041-8213/ac30e1 2041

  47. [47]

    , keywords =

    Silicon in the dayside atmospheres of two ultra-hot Jupiters. , keywords =. doi:10.1051/0004-6361/202142776 , archivePrefix =. 2112.10461 , primaryClass =

    work page doi:10.1051/0004-6361/202142776

  48. [48]

    Detection of Ti and V emission lines and retrieval of a broadened line profile

    Atmospheric characterization of the ultra-hot Jupiter WASP-33b. Detection of Ti and V emission lines and retrieval of a broadened line profile. , keywords =. doi:10.1051/0004-6361/202244277 , archivePrefix =. 2209.10618 , primaryClass =

    work page doi:10.1051/0004-6361/202244277

  49. [49]

    , keywords =

    CRIRES ^ + detection of CO emissions lines and temperature inversions on the dayside of WASP-18b and WASP-76b. , keywords =. doi:10.1051/0004-6361/202245371 , archivePrefix =. 2302.08736 , primaryClass =

    work page doi:10.1051/0004-6361/202245371

  50. [50]

    Flat-relative optimal extraction. A quick and efficient algorithm for stabilised spectrographs

    Flat-relative optimal extraction. A quick and efficient algorithm for stabilised spectrographs. , keywords =. doi:10.1051/0004-6361/201322746 , archivePrefix =. 1311.5263 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322746

  51. [51]

    Observatory Operations: Strategies, Processes, and Systems VI , year = 2016, series =

    CARMENES: data flow. Observatory Operations: Strategies, Processes, and Systems VI , year = 2016, series =. doi:10.1117/12.2233574 , adsurl =

    work page doi:10.1117/12.2233574 2016

  52. [52]

    , keywords =

    Correcting systematic effects in a large set of photometric light curves. , keywords =. doi:10.1111/j.1365-2966.2004.08585.x , archivePrefix =. astro-ph/0502056 , primaryClass =

    work page doi:10.1111/j.1365-2966.2004.08585.x 2004

  53. [53]

    The PEPSI Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy. , keywords =. doi:10.3847/1538-3881/acb7e2 , archivePrefix =. 2205.12162 , primaryClass =

    work page doi:10.3847/1538-3881/acb7e2

  54. [54]

    Workshop on Astrophysical Opacities , year = 2018, series =

    Including All the Lines: Data Releases for Spectra and Opacities through 2017. Workshop on Astrophysical Opacities , year = 2018, series =

    work page 2017

  55. [55]

    Exoplanet Atmospheres at High Spectral Resolution

    Exoplanet Atmospheres at High Spectral Resolution. arXiv e-prints , keywords =. doi:10.48550/arXiv.1806.04617 , archivePrefix =. 1806.04617 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1806.04617

  56. [56]

    An extended hydrogen envelope of the extremely hot giant exoplanet KELT-9b

    An extended hydrogen envelope of the extremely hot giant exoplanet KELT-9b. Nature Astronomy , keywords =. doi:10.1038/s41550-018-0503-3 , archivePrefix =. 1807.00869 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-018-0503-3

  57. [57]

    , keywords =

    Black Mirror: The impact of rotational broadening on the search for reflected light from 51 Pegasi b with high resolution spectroscopy. , keywords =. doi:10.1051/0004-6361/202142314 , archivePrefix =. 2201.03600 , primaryClass =

    work page doi:10.1051/0004-6361/202142314

  58. [58]

    , keywords =

    Detection of Fe and evidence for TiO in the dayside emission spectrum of WASP-33b. , keywords =. doi:10.1051/0004-6361/202140732 , archivePrefix =. 2105.10230 , primaryClass =

    work page doi:10.1051/0004-6361/202140732

  59. [59]

    Analytic models for albedos, phase curves and polarization of reflected light from exoplanets

    Analytic Models for Albedos, Phase Curves, and Polarization of Reflected Light from Exoplanets. , keywords =. doi:10.1088/0004-637X/747/1/25 , archivePrefix =. 1112.4476 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/747/1/25

  60. [60]

    and Cristiani, S

    ESPRESSO at VLT. On-sky performance and first results. , keywords =. doi:10.1051/0004-6361/202038306 , archivePrefix =. 2010.00316 , primaryClass =

    work page doi:10.1051/0004-6361/202038306 2010

  61. [61]

    , keywords =

    Where Is the Water? Jupiter-like C/H Ratio but Strong H _ 2 O Depletion Found on Bo \"o tis b Using SPIRou. , keywords =. doi:10.3847/1538-3881/ac0428 , archivePrefix =. 2105.10513 , primaryClass =

    work page doi:10.3847/1538-3881/ac0428

  62. [62]

    , keywords =

    Water observed in the atmosphere of Bo \"o tis Ab with CARMENES/CAHA. , keywords =. doi:10.1093/mnras/stac1512 , archivePrefix =. 2205.14975 , primaryClass =

    work page doi:10.1093/mnras/stac1512

  63. [63]

    Journal of Geophysical Research (Planets) , keywords =

    Hazy Blue Worlds: A Holistic Aerosol Model for Uranus and Neptune, Including Dark Spots. Journal of Geophysical Research (Planets) , keywords =. doi:10.1029/2022JE007189 , archivePrefix =. 2201.04516 , primaryClass =

    work page doi:10.1029/2022je007189

  64. [64]

    The GAPS Programme at TNG. XXIX. No detection of reflected light from 51 Peg b using optical high-resolution spectroscopy. , keywords =. doi:10.1051/0004-6361/202039271 , archivePrefix =. 2012.10435 , primaryClass =

    work page doi:10.1051/0004-6361/202039271 2012

  65. [65]

    , keywords =

    No TiO detected in the hot-Neptune-desert planet LTT-9779 b in reflected light at high spectral resolution. , keywords =. doi:10.1051/0004-6361/202557240 , archivePrefix =. 2511.08691 , primaryClass =

    work page doi:10.1051/0004-6361/202557240

  66. [66]

    Astronomische Nachrichten , keywords =

    The return of the mummy: Evidence for starlight reflected from the massive hot Jupiter Boo b?. Astronomische Nachrichten , keywords =. doi:10.1002/asna.201211744 , adsurl =

    work page doi:10.1002/asna.201211744

  67. [67]

    Evidence for a spectroscopic direct detection of reflected light from 51 Peg b

    Evidence for a spectroscopic direct detection of reflected light from <ASTROBJ>51 Pegasi b</ASTROBJ>. , keywords =. doi:10.1051/0004-6361/201425298 , archivePrefix =. 1504.05962 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201425298

  68. [68]

    HD 75289Ab revisited - Searching for starlight reflected from a hot Jupiter

    HD 75289Ab revisited. Searching for starlight reflected from a hot Jupiter. , keywords =. doi:10.1051/0004-6361:20079175 , archivePrefix =. 0804.4609 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20079175

  69. [69]

    Astrobiology , keywords =

    Exoplanet Biosignatures: Understanding Oxygen as a Biosignature in the Context of Its Environment. Astrobiology , keywords =. doi:10.1089/ast.2017.1727 , archivePrefix =. 1705.07560 , primaryClass =

    work page doi:10.1089/ast.2017.1727 2017

  70. [70]

    , keywords =

    Into the red: an M-band study of the chemistry and rotation of Pictoris b at high spectral resolution. , keywords =. doi:10.1093/mnras/stae1277 , archivePrefix =. 2405.08867 , primaryClass =

    work page doi:10.1093/mnras/stae1277

  71. [71]

    L., Chen , X., Ciardi , D., et al

    Akeson , R. L., Chen , X., Ciardi , D., et al. 2013, , 125, 989

    work page 2013

  72. [72]

    Birkby , J. L. 2018, arXiv e-prints, arXiv:1806.04617

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  73. [73]

    Brogi , M., Snellen , I. A. G., de Kok , R. J., et al. 2012, , 486, 502

    work page 2012

  74. [74]

    A., Gu \`a rdia , J., L \'o pez del Fresno , M., et al

    Caballero , J. A., Gu \`a rdia , J., L \'o pez del Fresno , M., et al. 2016, in , Vol. 9910, Observatory Operations: Strategies, Processes, and Systems VI, 99100E

    work page 2016

  75. [75]

    W., Korzennik , S

    Charbonneau , D., Noyes , R. W., Korzennik , S. G., et al. 1999, , 522, L145

    work page 1999

  76. [76]

    2010, , 407, 507

    Collier Cameron , A., Guenther , E., Smalley , B., et al. 2010, , 407, 507

    work page 2010

  77. [77]

    2000, arXiv e-prints, astro

    Collier Cameron , A., Horne , K., James , D., Penny , A., & Semel , M. 2000, arXiv e-prints, astro

    work page 2000

  78. [78]

    1999, , 402, 751

    Collier Cameron , A., Horne , K., Penny , A., & James , D. 1999, , 402, 751

    work page 1999

  79. [79]

    2002, , 330, 187

    Collier Cameron , A., Horne , K., Penny , A., & Leigh , C. 2002, , 330, 187

    work page 2002

  80. [80]

    2021, , 651, A33

    Cont , D., Yan , F., Reiners , A., et al. 2021, , 651, A33

    work page 2021

Showing first 80 references.