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Detection of a spectroscopic transit by the planet orbiting the star HD209458
Astrophysics · Submitted 15 Jun 2000
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We report the first detection of a planetary transit by spectroscopic measurements.
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The abstract, sentence by sentence
We report the first detection of a planetary transit by spectroscopic measurements. We have detected the distortion of the stellar line profiles during a planetary transit. With the ELODIE spectrograph we took a sequence of high precision radial velocities of the star HD209458 at time of a transit of its planet. We detected an anomaly in the residuals of the orbit. The shape and the amplitude of the anomaly are modeled as a change of the mean stellar line profile resulting from the planet crossing the disk of the rotating star. The planetary orbit is in the same direction as the stellar rotation. Using the photometric transit to constrain the timing and the impact parameters of the transit, we measure an angle alpha=3.9d between the orbital plane and the apparent equatorial plane as well as a vsini=3.75(+-)1.25 kms-1. With additional constrains on the inclination of the star and on the statistics of the line of sight distribution, we can set an upper limit of 30d to the angle between the orbital plane and the stellar equatorial plane.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We report the first detection of a planetary transit by spectroscopic measurements. | contribution 0.59 | 0.96 | 0.87 | asserted 1.00 |
| s1 | We have detected the distortion of the stellar line profiles during a planetary transit. | result 0.91 | 0.97 | 0.32 | asserted 1.00 |
| s2 | With the ELODIE spectrograph we took a sequence of high precision radial velocities of the star HD209458 at time of a transit of its planet. | method 1.00 | 0.97 | 0.05 | asserted 1.00 |
| s3 | We detected an anomaly in the residuals of the orbit. | result 1.00 | 0.97 | 0.08 | asserted 1.00 |
| s4 | The shape and the amplitude of the anomaly are modeled as a change of the mean stellar line profile resulting from the planet crossing the disk of the rotating star. | interpretation 0.79 | 0.86 | 0.25 | asserted 0.87 |
| s5 | The planetary orbit is in the same direction as the stellar rotation. | result 0.95 | 0.78 | 0.10 | asserted 1.00 |
| s6 | Using the photometric transit to constrain the timing and the impact parameters of the transit, we measure an angle alpha=3.9d between the orbital plane and the apparent equatorial plane as well as a vsini=3.75(+-)1.25 kms-1. | result 0.99 | 0.96 | 0.13 | asserted 1.00 |
| s7 | With additional constrains on the inclination of the star and on the statistics of the line of sight distribution, we can set an upper limit of 30d to the angle between the orbital plane and the stellar equatorial plane. | result 0.97 | 0.91 | 0.13 | asserted 0.76 |
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The paper
Original abstract
We report the first detection of a planetary transit by spectroscopic measurements. We have detected the distortion of the stellar line profiles during a planetary transit. With the ELODIE spectrograph we took a sequence of high precision radial velocities of the star HD209458 at time of a transit of its planet. We detected an anomaly in the residuals of the orbit. The shape and the amplitude of the anomaly are modeled as a change of the mean stellar line profile resulting from the planet crossing the disk of the rotating star. The planetary orbit is in the same direction as the stellar rotation. Using the photometric transit to constrain the timing and the impact parameters of the transit, we measure an angle alpha=3.9d between the orbital plane and the apparent equatorial plane as well as a vsini=3.75(+-)1.25 kms-1. With additional constrains on the inclination of the star and on the statistics of the line of sight distribution, we can set an upper limit of 30d to the angle between the orbital plane and the stellar equatorial plane.
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References
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2 arXiv papers cite this in 2 sentences
Papers citing it
Uses its method or tool 1 paper
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This can be measured using the Rossiter-McLaughlin (RM) effect [ref] .
The EBLM Project XVIII. 3D Obliquities of Five Low-Mass Eclipsing Binaries · Introduction · 0.90
Cites it as background 1 paper
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However, a potential caveat of this method relates to the Rossiter-McLaughlin (R-M) effect [ref] .
Feasibility of High-Resolution Transmission Spectroscopy for Low-Velocity Exoplanets · Constraining transit duration in the low-velocity regime · 0.98
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