Is the target (Rp/Rs)^2, or delF/F? Equivalently, is there an assumed model of limb darkening implied by the simulated train and test data?
", "messages": [ { "id": 2964295, "postDate": "2024-08-19T17:29:28.363Z", "content": "That’s an excellent question!
\nThe target in our simulations is ΔF/F, or the relative flux change during a transit, which corresponds to the transit depth. This is directly related to (Rp/Rs)^2, the square of the planet-to-star radius ratio. However, this relationship is perturbed by the contribution from the planet’s atmosphere.
\nFor a simple reference, let’s start with the model presented in Sing (2018), eq. 15:
\n$$
\n\\Delta F/F = \\frac{\\pi R_p^2 + A}{\\pi R_s^2}
\n$$
where A represents the contribution of the planet’s atmosphere to the signal. This can be rewritten as:
\n$$
\n\\Delta F/F = \\frac{R_p^2}{R_s^2} + \\frac{A}{\\pi R_s^2}
\n$$
This highlights how the relationship between ΔF/F and Rp/Rs is perturbed by the planet’s atmosphere. This perturbation changes with wavelength due to the physical and chemical properties of the exoplanet’s atmosphere. I won't go into further details here, as there are already suggested references that explain the science behind this more thoroughly.
\nFor this particular exercise, we’ve chosen not to include a limb darkening model to avoid adding further complexity to the problem.
", "rawMarkdown": "That’s an excellent question!\n\nThe target in our simulations is ΔF/F, or the relative flux change during a transit, which corresponds to the transit depth. This is directly related to (Rp/Rs)^2, the square of the planet-to-star radius ratio. However, this relationship is perturbed by the contribution from the planet’s atmosphere.\n\nFor a simple reference, let’s start with the model presented in [Sing (2018)](https://arxiv.org/pdf/1804.07357), eq. 15:\n\n$$\n\\Delta F/F = \\frac{\\pi R_p^2 + A}{\\pi R_s^2}\n$$\n\nwhere A represents the contribution of the planet’s atmosphere to the signal. This can be rewritten as:\n\n$$\n\\Delta F/F = \\frac{R_p^2}{R_s^2} + \\frac{A}{\\pi R_s^2}\n$$\n\nThis highlights how the relationship between ΔF/F and Rp/Rs is perturbed by the planet’s atmosphere. This perturbation changes with wavelength due to the physical and chemical properties of the exoplanet’s atmosphere. I won't go into further details here, as there are already suggested [references](https://www.kaggle.com/competitions/ariel-data-challenge-2024/discussion/528233) that explain the science behind this more thoroughly.\n\nFor this particular exercise, we’ve chosen not to include a limb darkening model to avoid adding further complexity to the problem.\n", "votes": 10 }, { "id": 2961623, "postDate": "2024-08-16T18:42:26.263Z", "content": "Is the target (Rp/Rs)^2, or delF/F? Equivalently, is there an assumed model of limb darkening implied by the simulated train and test data?
", "rawMarkdown": "Is the target (Rp/Rs)^2, or delF/F? Equivalently, is there an assumed model of limb darkening implied by the simulated train and test data?", "votes": 6 } ], "comments": [ { "id": 2964295, "author_name": "Lorenzo Mugnai", "author_url": "", "post_date": "2024-08-19T17:29:28.363000", "content": "That’s an excellent question!
\nThe target in our simulations is ΔF/F, or the relative flux change during a transit, which corresponds to the transit depth. This is directly related to (Rp/Rs)^2, the square of the planet-to-star radius ratio. However, this relationship is perturbed by the contribution from the planet’s atmosphere.
\nFor a simple reference, let’s start with the model presented in Sing (2018), eq. 15:
\n$$
\n\\Delta F/F = \\frac{\\pi R_p^2 + A}{\\pi R_s^2}
\n$$
where A represents the contribution of the planet’s atmosphere to the signal. This can be rewritten as:
\n$$
\n\\Delta F/F = \\frac{R_p^2}{R_s^2} + \\frac{A}{\\pi R_s^2}
\n$$
This highlights how the relationship between ΔF/F and Rp/Rs is perturbed by the planet’s atmosphere. This perturbation changes with wavelength due to the physical and chemical properties of the exoplanet’s atmosphere. I won't go into further details here, as there are already suggested references that explain the science behind this more thoroughly.
\nFor this particular exercise, we’ve chosen not to include a limb darkening model to avoid adding further complexity to the problem.
", "votes": 10, "replies": [] } ], "raw_markdown_by_id": { "2964295": "That’s an excellent question!\n\nThe target in our simulations is ΔF/F, or the relative flux change during a transit, which corresponds to the transit depth. This is directly related to (Rp/Rs)^2, the square of the planet-to-star radius ratio. However, this relationship is perturbed by the contribution from the planet’s atmosphere.\n\nFor a simple reference, let’s start with the model presented in [Sing (2018)](https://arxiv.org/pdf/1804.07357), eq. 15:\n\n$$\n\\Delta F/F = \\frac{\\pi R_p^2 + A}{\\pi R_s^2}\n$$\n\nwhere A represents the contribution of the planet’s atmosphere to the signal. This can be rewritten as:\n\n$$\n\\Delta F/F = \\frac{R_p^2}{R_s^2} + \\frac{A}{\\pi R_s^2}\n$$\n\nThis highlights how the relationship between ΔF/F and Rp/Rs is perturbed by the planet’s atmosphere. This perturbation changes with wavelength due to the physical and chemical properties of the exoplanet’s atmosphere. I won't go into further details here, as there are already suggested [references](https://www.kaggle.com/competitions/ariel-data-challenge-2024/discussion/528233) that explain the science behind this more thoroughly.\n\nFor this particular exercise, we’ve chosen not to include a limb darkening model to avoid adding further complexity to the problem.\n", "2961623": "Is the target (Rp/Rs)^2, or delF/F? Equivalently, is there an assumed model of limb darkening implied by the simulated train and test data?" } }