{ "id": 524109, "title": "For better understanding Exoplanets & FSG1 Signal", "url": "/competitions/ariel-data-challenge-2024/discussion/524109", "author_name": "SeshuRaju šŸ§˜ā€ā™‚ļø", "post_date": "2024-08-04T16:09:26.767000", "votes": 29, "comment_count": 8, "views": 0, "content": "

Youtube Video - How to find a planet you canā€™t see

\n

\"\"
\nChatGPT used to make the sections for better understanding

\n

\"\"

\n
\n
    \n
  1. Discovery of Exoplanets
      \n
    • Time: 00:00:00 - 00:00:18
      \n NASA's recent announcements have revealed the discovery of numerous exoplanets, some of which hold the potential to have liquid water on their surfaces. These planets, found outside our solar system, are referred to as \"exoplanets.\" The excitement stems from the possibility that some of these planets might be rocky, similar to Earth, making them candidates for potential habitability. The discovery of these exoplanets opens up the possibility of finding new worlds that could support life, providing a significant milestone in our understanding of the universe.
    2. \n
\n
\n
\n
\n
    \n
  1. Challenges in Detecting Exoplanets
      \n
    • Time: 00:00:22 - 00:01:30
      \n Detecting exoplanets is an incredibly challenging task due to their proximity to their parent stars. These stars are immensely bright and often overshadow the planets orbiting around them. The light from these stars is so intense that it overwhelms the faint light reflected from the planets, making it almost impossible to see them directly. This is akin to trying to spot a tiny firefly next to a powerful stadium floodlight. The challenge is further compounded by the vast distances involved, as these planets are trillions of miles away from Earth. To overcome this, astronomers have developed innovative methods to indirectly detect these elusive worlds.
    2. \n
\n
\n
\n
\n
    \n
  1. The Wobble Method
      \n
    • Time: 00:01:33 - 00:04:31
      \n One of the primary methods used to detect exoplanets is known as the \"wobble method\" or radial velocity method. This technique is based on the fact that stars and their planets orbit a common center of mass, causing the star to wobble slightly due to the gravitational pull of the planets. Larger planets exert a stronger pull, resulting in a more noticeable wobble, while smaller planets cause a subtler effect. The first successful detection using this method was made in 1995 by Swiss astronomers, who observed a star in the Pegasus constellation exhibiting a periodic oscillation. This method has since been instrumental in discovering numerous exoplanets and measuring their distance from their parent stars.
    2. \n
\n
\n
\n
\n
    \n
  1. The Transit Method
      \n
    • Time: 00:04:37 - 00:06:12
      \n Another significant technique for finding exoplanets is the transit method. This method involves observing a planet as it passes in front of its star, causing a temporary dip in the starā€™s brightness. By carefully monitoring these tiny drops in brightness, astronomers can infer the presence of a planet. The transit method is particularly challenging because the decrease in brightness is minuscule and requires precise instruments and prolonged observation of many stars. The Kepler Space Telescope, launched in 2009, played a crucial role in this method, leading to the discovery of thousands of exoplanets by observing a single patch of sky for years.
    2. \n
\n
\n

\"\"

\n

Do we need to wait to track every exoplanet with respective its sun/suns planet i.e for earth => 365 days for other planets it vary ( solution below )

\n

Reason for @ambrosm notebook phase before, during, after => correlate with targets so well

\n

We are using 2 stars as per data shared in Kaggle ( is it 2 solar systems ? 1 solar system with 2 stars ? )

\n
\n
\n
    \n
  1. Mass and Density Calculation
      \n
    • Time: 00:06:14 - 00:06:45
      \n Determining the mass and size of an exoplanet is essential for calculating its density, which helps in distinguishing between different types of planets. For instance, gas giants like Jupiter are composed mostly of hydrogen and helium, whereas rocky planets like Earth are made of denser materials. By understanding the density, scientists can infer the composition and potential habitability of the planet. This information is critical in identifying planets that are similar to Earth and could potentially support life.
    2. \n
\n
\n
\n
\n
    \n
  1. Atmosphere Detection
      \n
    • Time: 00:06:47 - 00:08:23
      \n Detecting the atmospheres of exoplanets is another crucial step in understanding their potential to support life. Scientists look for biosignature gases, such as oxygen, which on Earth is produced by plants and photosynthetic bacteria. When an exoplanet passes in front of its star, some of the starlight filters through its atmosphere. By analyzing the light that reaches Earth, scientists can identify the specific gases present in the atmosphere. This technique, however, is incredibly challenging, especially for Earth-sized planets around sun-like stars, due to the tiny signals involved.
    2. \n
\n
\n

Do wavelengths provide information about the climate on exoplanets? ? =>

\n

\"\"

\n

\"\"

\n
\n
\n
    \n
  1. Direct Imaging
      \n
    • Time: 00:08:25 - 00:09:09
      \n Direct imaging of exoplanets involves capturing pictures of the planets themselves by blocking out the overwhelming light from their parent stars. This method has become possible with the use of devices like coronagraphs, which can effectively mask the starā€™s glare. Direct imaging works best for large planets that are far from their stars and emit their own infrared light. This technique holds promise for future advancements, enabling astronomers to capture images of smaller and cooler planets.
    2. \n
\n
\n

So, interesting concepts involved in the Ariel data challenge

\n

Anyone know similar source for \"CH0 Sensor\" ?

", "messages": [ { "id": 2946743, "postDate": "2024-08-04T16:09:26.767Z", "content": "

Youtube Video - How to find a planet you canā€™t see

\n

\"\"
\nChatGPT used to make the sections for better understanding

\n

\"\"

\n
\n
    \n
  1. Discovery of Exoplanets
      \n
    • Time: 00:00:00 - 00:00:18
      \n NASA's recent announcements have revealed the discovery of numerous exoplanets, some of which hold the potential to have liquid water on their surfaces. These planets, found outside our solar system, are referred to as \"exoplanets.\" The excitement stems from the possibility that some of these planets might be rocky, similar to Earth, making them candidates for potential habitability. The discovery of these exoplanets opens up the possibility of finding new worlds that could support life, providing a significant milestone in our understanding of the universe.
    2. \n
\n
\n
\n
\n
    \n
  1. Challenges in Detecting Exoplanets
      \n
    • Time: 00:00:22 - 00:01:30
      \n Detecting exoplanets is an incredibly challenging task due to their proximity to their parent stars. These stars are immensely bright and often overshadow the planets orbiting around them. The light from these stars is so intense that it overwhelms the faint light reflected from the planets, making it almost impossible to see them directly. This is akin to trying to spot a tiny firefly next to a powerful stadium floodlight. The challenge is further compounded by the vast distances involved, as these planets are trillions of miles away from Earth. To overcome this, astronomers have developed innovative methods to indirectly detect these elusive worlds.
    2. \n
\n
\n
\n
\n
    \n
  1. The Wobble Method
      \n
    • Time: 00:01:33 - 00:04:31
      \n One of the primary methods used to detect exoplanets is known as the \"wobble method\" or radial velocity method. This technique is based on the fact that stars and their planets orbit a common center of mass, causing the star to wobble slightly due to the gravitational pull of the planets. Larger planets exert a stronger pull, resulting in a more noticeable wobble, while smaller planets cause a subtler effect. The first successful detection using this method was made in 1995 by Swiss astronomers, who observed a star in the Pegasus constellation exhibiting a periodic oscillation. This method has since been instrumental in discovering numerous exoplanets and measuring their distance from their parent stars.
    2. \n
\n
\n
\n
\n
    \n
  1. The Transit Method
      \n
    • Time: 00:04:37 - 00:06:12
      \n Another significant technique for finding exoplanets is the transit method. This method involves observing a planet as it passes in front of its star, causing a temporary dip in the starā€™s brightness. By carefully monitoring these tiny drops in brightness, astronomers can infer the presence of a planet. The transit method is particularly challenging because the decrease in brightness is minuscule and requires precise instruments and prolonged observation of many stars. The Kepler Space Telescope, launched in 2009, played a crucial role in this method, leading to the discovery of thousands of exoplanets by observing a single patch of sky for years.
    2. \n
\n
\n

\"\"

\n

Do we need to wait to track every exoplanet with respective its sun/suns planet i.e for earth => 365 days for other planets it vary ( solution below )

\n

Reason for @ambrosm notebook phase before, during, after => correlate with targets so well

\n

We are using 2 stars as per data shared in Kaggle ( is it 2 solar systems ? 1 solar system with 2 stars ? )

\n
\n
\n
    \n
  1. Mass and Density Calculation
      \n
    • Time: 00:06:14 - 00:06:45
      \n Determining the mass and size of an exoplanet is essential for calculating its density, which helps in distinguishing between different types of planets. For instance, gas giants like Jupiter are composed mostly of hydrogen and helium, whereas rocky planets like Earth are made of denser materials. By understanding the density, scientists can infer the composition and potential habitability of the planet. This information is critical in identifying planets that are similar to Earth and could potentially support life.
    2. \n
\n
\n
\n
\n
    \n
  1. Atmosphere Detection
      \n
    • Time: 00:06:47 - 00:08:23
      \n Detecting the atmospheres of exoplanets is another crucial step in understanding their potential to support life. Scientists look for biosignature gases, such as oxygen, which on Earth is produced by plants and photosynthetic bacteria. When an exoplanet passes in front of its star, some of the starlight filters through its atmosphere. By analyzing the light that reaches Earth, scientists can identify the specific gases present in the atmosphere. This technique, however, is incredibly challenging, especially for Earth-sized planets around sun-like stars, due to the tiny signals involved.
    2. \n
\n
\n

Do wavelengths provide information about the climate on exoplanets? ? =>

\n

\"\"

\n

\"\"

\n
\n
\n
    \n
  1. Direct Imaging
      \n
    • Time: 00:08:25 - 00:09:09
      \n Direct imaging of exoplanets involves capturing pictures of the planets themselves by blocking out the overwhelming light from their parent stars. This method has become possible with the use of devices like coronagraphs, which can effectively mask the starā€™s glare. Direct imaging works best for large planets that are far from their stars and emit their own infrared light. This technique holds promise for future advancements, enabling astronomers to capture images of smaller and cooler planets.
    2. \n
\n
\n

So, interesting concepts involved in the Ariel data challenge

\n

Anyone know similar source for \"CH0 Sensor\" ?

", "rawMarkdown": "# [Youtube Video - How to find a planet you canā€™t see](https://www.youtube.com/watch?v=STsI6IbPbGQ&ab_channel=Vox) \n\n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F761268%2F3e5901506193e42ae2ec1ac77d9fa77a%2FScreenshot%202024-08-04%20at%209.41.09PM.png?generation=1722787887443942&alt=media)\n**ChatGPT used to make the sections for better understanding**\n\n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F761268%2F449ed3cb8bc43f498fcd917733a33064%2FScreenshot%202024-08-04%20at%209.24.19PM.png?generation=1722786886542329&alt=media)\n\n> 1. **Discovery of Exoplanets**\n - **Time: 00:00:00 - 00:00:18**\n NASA's recent announcements have revealed the discovery of numerous exoplanets, some of which hold the potential to have liquid water on their surfaces. These planets, found outside our solar system, are referred to as \"exoplanets.\" The excitement stems from the possibility that some of these planets might be rocky, similar to Earth, making them candidates for potential habitability. The discovery of these exoplanets opens up the possibility of finding new worlds that could support life, providing a significant milestone in our understanding of the universe.\n\n---\n\n> 2. **Challenges in Detecting Exoplanets**\n - **Time: 00:00:22 - 00:01:30**\n Detecting exoplanets is an incredibly challenging task due to their proximity to their parent stars. These stars are immensely bright and often overshadow the planets orbiting around them. The light from these stars is so intense that it overwhelms the faint light reflected from the planets, making it almost impossible to see them directly. This is akin to trying to spot a tiny firefly next to a powerful stadium floodlight. The challenge is further compounded by the vast distances involved, as these planets are trillions of miles away from Earth. To overcome this, astronomers have developed innovative methods to indirectly detect these elusive worlds.\n\n---\n\n> 3. **The Wobble Method**\n - **Time: 00:01:33 - 00:04:31**\n One of the primary methods used to detect exoplanets is known as the \"wobble method\" or radial velocity method. This technique is based on the fact that stars and their planets orbit a common center of mass, causing the star to wobble slightly due to the gravitational pull of the planets. Larger planets exert a stronger pull, resulting in a more noticeable wobble, while smaller planets cause a subtler effect. The first successful detection using this method was made in 1995 by Swiss astronomers, who observed a star in the Pegasus constellation exhibiting a periodic oscillation. This method has since been instrumental in discovering numerous exoplanets and measuring their distance from their parent stars.\n\n---\n\n> 4. **The Transit Method**\n - **Time: 00:04:37 - 00:06:12**\n Another significant technique for finding exoplanets is the transit method. This method involves observing a planet as it passes in front of its star, causing a temporary dip in the starā€™s brightness. By carefully monitoring these tiny drops in brightness, astronomers can infer the presence of a planet. The transit method is particularly challenging because the decrease in brightness is minuscule and requires precise instruments and prolonged observation of many stars. The Kepler Space Telescope, launched in 2009, played a crucial role in this method, leading to the discovery of thousands of exoplanets by observing a single patch of sky for years.\n\n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F761268%2Fc0142b8449002ad2e05f0e3c4994a3d5%2FScreenshot%202024-08-04%20at%209.18.34PM.png?generation=1722786540051858&alt=media) \n\n\n## Do we need to wait to track every exoplanet with respective its sun/suns planet i.e for earth => 365 days for other planets it vary ( solution below )\n## Reason for @ambrosm notebook phase before, during, after => correlate with targets so well\n\n## We are using 2 stars as per data shared in Kaggle ( is it 2 solar systems ? 1 solar system with 2 stars ? )\n\n---\n\n> 5. **Mass and Density Calculation**\n - **Time: 00:06:14 - 00:06:45**\n Determining the mass and size of an exoplanet is essential for calculating its density, which helps in distinguishing between different types of planets. For instance, gas giants like Jupiter are composed mostly of hydrogen and helium, whereas rocky planets like Earth are made of denser materials. By understanding the density, scientists can infer the composition and potential habitability of the planet. This information is critical in identifying planets that are similar to Earth and could potentially support life.\n\n---\n\n> 6. **Atmosphere Detection**\n - **Time: 00:06:47 - 00:08:23**\n Detecting the atmospheres of exoplanets is another crucial step in understanding their potential to support life. Scientists look for biosignature gases, such as oxygen, which on Earth is produced by plants and photosynthetic bacteria. When an exoplanet passes in front of its star, some of the starlight filters through its atmosphere. By analyzing the light that reaches Earth, scientists can identify the specific gases present in the atmosphere. This technique, however, is incredibly challenging, especially for Earth-sized planets around sun-like stars, due to the tiny signals involved.\n\n# Do wavelengths provide information about the climate on exoplanets? ? => \n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F761268%2F84b0b31fc2cf8b755fc8a03bfada44da%2FScreenshot%202024-08-04%20at%209.31.46PM.png?generation=1722787320090497&alt=media)\n\n\n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F761268%2F186c458add98021896fc54271002bfcf%2FScreenshot%202024-08-07%20at%2021.45.25.png?generation=1723047619090456&alt=media)\n\n---\n\n> 7. **Direct Imaging**\n - **Time: 00:08:25 - 00:09:09**\n Direct imaging of exoplanets involves capturing pictures of the planets themselves by blocking out the overwhelming light from their parent stars. This method has become possible with the use of devices like coronagraphs, which can effectively mask the starā€™s glare. Direct imaging works best for large planets that are far from their stars and emit their own infrared light. This technique holds promise for future advancements, enabling astronomers to capture images of smaller and cooler planets.\n\n# So, interesting concepts involved in the Ariel data challenge\n\n# Anyone know similar source for \"CH0 Sensor\" ? ", "votes": 28 }, { "id": 2947655, "postDate": "2024-08-05T11:07:51.377Z", "content": "

Hi @seshurajup , thank you for the resources. For this challenge you will probably find Transit method and atmosphere detection most useful to this challenge! Of course, having relevant knowledge of the exoplanets will help too!

", "rawMarkdown": "Hi @seshurajup , thank you for the resources. For this challenge you will probably find Transit method and atmosphere detection most useful to this challenge! Of course, having relevant knowledge of the exoplanets will help too!", "votes": 7, "replies": [ { "id": 2950885, "postDate": "2024-08-08T03:15:32.310Z", "content": "

Hi @gordonyip!
\nMay I ask what's the x and y axis meaning of AIRS-CH0_signal which has a shape of 356x32?

", "rawMarkdown": "Hi @gordonyip!\nMay I ask what's the x and y axis meaning of AIRS-CH0_signal which has a shape of 356x32?", "votes": 4, "replies": [ { "id": 2953775, "postDate": "2024-08-09T04:10:48.737Z", "content": "

My understanding is that this is wavelength x spatial domain

\n

Take a look at the axis_info parquet file, which provides the wavelength for each channel in the \"AIRS-CH0-axis2-um\" column

\n

I do find it interesting that they provide simulated data outside the sensors wavelength sensitivity though (1.95 -> 3.90 Āµm); it looks like Gordon is correcting for it in the notebook.
\n(https://www.kaggle.com/code/gordonyip/calibrating-and-time-binning-astronomical-data?scriptVersionId=191665579)

\n

I struggled to visualize it until I looked at the AIRS optical chain diagram in the ARIEL red book, which shows light entering via a slit then being partitioned by wavelength using a Prism

\n

\"\"

", "rawMarkdown": "My understanding is that this is wavelength x spatial domain\n\nTake a look at the axis_info parquet file, which provides the wavelength for each channel in the \"AIRS-CH0-axis2-um\" column\n\nI do find it interesting that they provide simulated data outside the sensors wavelength sensitivity though (1.95 -> 3.90 Āµm); it looks like Gordon is correcting for it in the notebook.\n(https://www.kaggle.com/code/gordonyip/calibrating-and-time-binning-astronomical-data?scriptVersionId=191665579)\n\nI struggled to visualize it until I looked at the AIRS optical chain diagram in the ARIEL red book, which shows light entering via a slit then being partitioned by wavelength using a Prism\n\n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F21697054%2F77035a62e8833b58416f9aeb2d00b98b%2FScreenshot%202024-08-09%20at%2012.06.20AM.png?generation=1723176501340282&alt=media)", "votes": 3 }, { "id": 2953854, "postDate": "2024-08-09T06:17:59.407Z", "content": "

Thanks for your reply! I agree with you that x is wavelength domain, but how to understand that y is spatial domain, why is it only one dimension?
\nFor a give x (wavelength), we have a high flux when y has a middle value, what's the meaning of this?
\n\"\"

", "rawMarkdown": "Thanks for your reply! I agree with you that x is wavelength domain, but how to understand that y is spatial domain, why is it only one dimension?\nFor a give x (wavelength), we have a high flux when y has a middle value, what's the meaning of this?\n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F1565062%2Fdad17badf348e50f57cd40310b88a354%2F2024-08-09%2014.15.11.png?generation=1723184275055524&alt=media)", "votes": 1 }, { "id": 2953868, "postDate": "2024-08-09T06:44:04.480Z", "content": "
\n

Not sure it is correlation or theory, but => wavelength as 283 is what famous from previous papers. @jiazhuang => cross check once is the 283 or not from your wavelenght

\n
", "rawMarkdown": "> Not sure it is correlation or theory, but => wavelength as 283 is what famous from previous papers. @jiazhuang => cross check once is the 283 or not from your wavelenght" }, { "id": 2954425, "postDate": "2024-08-09T17:07:38.410Z", "content": "

Originally, scientists only have irradiated pixels, with the only unit being pixels. To simplify the process of linking these pixels to the wavelength of the light, we simulated the detector so that the light always aligns with the pixel window and is dispersed in one direction, the x-axis. And this is why we provide the wavelength of the light hitting each pixel.

\n

Also, the signal is strongest at the center of the y-axis because we've aligned the signal to be dispersed horizontally, and the light from a point source is spread by the telescope optics, and typically it peaks at the center.

", "rawMarkdown": "Originally, scientists only have irradiated pixels, with the only unit being pixels. To simplify the process of linking these pixels to the wavelength of the light, we simulated the detector so that the light always aligns with the pixel window and is dispersed in one direction, the x-axis. And this is why we provide the wavelength of the light hitting each pixel. \n\nAlso, the signal is strongest at the center of the y-axis because we've aligned the signal to be dispersed horizontally, and the light from a point source is spread by the telescope optics, and typically it peaks at the center.\n", "votes": 7 }, { "id": 2954682, "postDate": "2024-08-10T03:41:56.383Z", "content": "

Thanks for the explanation, it helps a lot!

", "rawMarkdown": "Thanks for the explanation, it helps a lot!", "votes": 2 } ] } ] }, { "id": 2978378, "postDate": "2024-09-03T20:23:15.873Z", "content": "

Out of curiosity, when you mention 'ChatGPT used to make the sections for better understanding', what prompts did you use to improve it?

", "rawMarkdown": "Out of curiosity, when you mention 'ChatGPT used to make the sections for better understanding', what prompts did you use to improve it?" } ], "comments": [ { "id": 2947655, "author_name": "Gordon Yip", "author_url": "", "post_date": "2024-08-05T11:07:51.377000", "content": "

Hi @seshurajup , thank you for the resources. For this challenge you will probably find Transit method and atmosphere detection most useful to this challenge! Of course, having relevant knowledge of the exoplanets will help too!

", "votes": 7, "replies": [ { "id": 2950885, "author_name": "Zhuang Jia", "author_url": "", "post_date": "2024-08-08T03:15:32.310000", "content": "

Hi @gordonyip!
\nMay I ask what's the x and y axis meaning of AIRS-CH0_signal which has a shape of 356x32?

", "votes": 4, "replies": [ { "id": 2953775, "author_name": "Jay", "author_url": "", "post_date": "2024-08-09T04:10:48.737000", "content": "

My understanding is that this is wavelength x spatial domain

\n

Take a look at the axis_info parquet file, which provides the wavelength for each channel in the \"AIRS-CH0-axis2-um\" column

\n

I do find it interesting that they provide simulated data outside the sensors wavelength sensitivity though (1.95 -> 3.90 Āµm); it looks like Gordon is correcting for it in the notebook.
\n(https://www.kaggle.com/code/gordonyip/calibrating-and-time-binning-astronomical-data?scriptVersionId=191665579)

\n

I struggled to visualize it until I looked at the AIRS optical chain diagram in the ARIEL red book, which shows light entering via a slit then being partitioned by wavelength using a Prism

\n

\"\"

", "votes": 3, "replies": [] }, { "id": 2953854, "author_name": "Zhuang Jia", "author_url": "", "post_date": "2024-08-09T06:17:59.407000", "content": "

Thanks for your reply! I agree with you that x is wavelength domain, but how to understand that y is spatial domain, why is it only one dimension?
\nFor a give x (wavelength), we have a high flux when y has a middle value, what's the meaning of this?
\n\"\"

", "votes": 1, "replies": [] }, { "id": 2953868, "author_name": "SeshuRaju šŸ§˜ā€ā™‚ļø", "author_url": "", "post_date": "2024-08-09T06:44:04.480000", "content": "
\n

Not sure it is correlation or theory, but => wavelength as 283 is what famous from previous papers. @jiazhuang => cross check once is the 283 or not from your wavelenght

\n
", "votes": 0, "replies": [] }, { "id": 2954425, "author_name": "Lorenzo Mugnai", "author_url": "", "post_date": "2024-08-09T17:07:38.410000", "content": "

Originally, scientists only have irradiated pixels, with the only unit being pixels. To simplify the process of linking these pixels to the wavelength of the light, we simulated the detector so that the light always aligns with the pixel window and is dispersed in one direction, the x-axis. And this is why we provide the wavelength of the light hitting each pixel.

\n

Also, the signal is strongest at the center of the y-axis because we've aligned the signal to be dispersed horizontally, and the light from a point source is spread by the telescope optics, and typically it peaks at the center.

", "votes": 7, "replies": [] }, { "id": 2954682, "author_name": "Zhuang Jia", "author_url": "", "post_date": "2024-08-10T03:41:56.383000", "content": "

Thanks for the explanation, it helps a lot!

", "votes": 2, "replies": [] } ] } ] }, { "id": 2978378, "author_name": "Tony Lee", "author_url": "", "post_date": "2024-09-03T20:23:15.873000", "content": "

Out of curiosity, when you mention 'ChatGPT used to make the sections for better understanding', what prompts did you use to improve it?

", "votes": 0, "replies": [] } ], "raw_markdown_by_id": { "2946743": "# [Youtube Video - How to find a planet you canā€™t see](https://www.youtube.com/watch?v=STsI6IbPbGQ&ab_channel=Vox) \n\n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F761268%2F3e5901506193e42ae2ec1ac77d9fa77a%2FScreenshot%202024-08-04%20at%209.41.09PM.png?generation=1722787887443942&alt=media)\n**ChatGPT used to make the sections for better understanding**\n\n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F761268%2F449ed3cb8bc43f498fcd917733a33064%2FScreenshot%202024-08-04%20at%209.24.19PM.png?generation=1722786886542329&alt=media)\n\n> 1. **Discovery of Exoplanets**\n - **Time: 00:00:00 - 00:00:18**\n NASA's recent announcements have revealed the discovery of numerous exoplanets, some of which hold the potential to have liquid water on their surfaces. These planets, found outside our solar system, are referred to as \"exoplanets.\" The excitement stems from the possibility that some of these planets might be rocky, similar to Earth, making them candidates for potential habitability. The discovery of these exoplanets opens up the possibility of finding new worlds that could support life, providing a significant milestone in our understanding of the universe.\n\n---\n\n> 2. **Challenges in Detecting Exoplanets**\n - **Time: 00:00:22 - 00:01:30**\n Detecting exoplanets is an incredibly challenging task due to their proximity to their parent stars. These stars are immensely bright and often overshadow the planets orbiting around them. The light from these stars is so intense that it overwhelms the faint light reflected from the planets, making it almost impossible to see them directly. This is akin to trying to spot a tiny firefly next to a powerful stadium floodlight. The challenge is further compounded by the vast distances involved, as these planets are trillions of miles away from Earth. To overcome this, astronomers have developed innovative methods to indirectly detect these elusive worlds.\n\n---\n\n> 3. **The Wobble Method**\n - **Time: 00:01:33 - 00:04:31**\n One of the primary methods used to detect exoplanets is known as the \"wobble method\" or radial velocity method. This technique is based on the fact that stars and their planets orbit a common center of mass, causing the star to wobble slightly due to the gravitational pull of the planets. Larger planets exert a stronger pull, resulting in a more noticeable wobble, while smaller planets cause a subtler effect. The first successful detection using this method was made in 1995 by Swiss astronomers, who observed a star in the Pegasus constellation exhibiting a periodic oscillation. This method has since been instrumental in discovering numerous exoplanets and measuring their distance from their parent stars.\n\n---\n\n> 4. **The Transit Method**\n - **Time: 00:04:37 - 00:06:12**\n Another significant technique for finding exoplanets is the transit method. This method involves observing a planet as it passes in front of its star, causing a temporary dip in the starā€™s brightness. By carefully monitoring these tiny drops in brightness, astronomers can infer the presence of a planet. The transit method is particularly challenging because the decrease in brightness is minuscule and requires precise instruments and prolonged observation of many stars. The Kepler Space Telescope, launched in 2009, played a crucial role in this method, leading to the discovery of thousands of exoplanets by observing a single patch of sky for years.\n\n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F761268%2Fc0142b8449002ad2e05f0e3c4994a3d5%2FScreenshot%202024-08-04%20at%209.18.34PM.png?generation=1722786540051858&alt=media) \n\n\n## Do we need to wait to track every exoplanet with respective its sun/suns planet i.e for earth => 365 days for other planets it vary ( solution below )\n## Reason for @ambrosm notebook phase before, during, after => correlate with targets so well\n\n## We are using 2 stars as per data shared in Kaggle ( is it 2 solar systems ? 1 solar system with 2 stars ? )\n\n---\n\n> 5. **Mass and Density Calculation**\n - **Time: 00:06:14 - 00:06:45**\n Determining the mass and size of an exoplanet is essential for calculating its density, which helps in distinguishing between different types of planets. For instance, gas giants like Jupiter are composed mostly of hydrogen and helium, whereas rocky planets like Earth are made of denser materials. By understanding the density, scientists can infer the composition and potential habitability of the planet. This information is critical in identifying planets that are similar to Earth and could potentially support life.\n\n---\n\n> 6. **Atmosphere Detection**\n - **Time: 00:06:47 - 00:08:23**\n Detecting the atmospheres of exoplanets is another crucial step in understanding their potential to support life. Scientists look for biosignature gases, such as oxygen, which on Earth is produced by plants and photosynthetic bacteria. When an exoplanet passes in front of its star, some of the starlight filters through its atmosphere. By analyzing the light that reaches Earth, scientists can identify the specific gases present in the atmosphere. This technique, however, is incredibly challenging, especially for Earth-sized planets around sun-like stars, due to the tiny signals involved.\n\n# Do wavelengths provide information about the climate on exoplanets? ? => \n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F761268%2F84b0b31fc2cf8b755fc8a03bfada44da%2FScreenshot%202024-08-04%20at%209.31.46PM.png?generation=1722787320090497&alt=media)\n\n\n![](https://www.googleapis.com/download/storage/v1/b/kaggle-forum-message-attachments/o/inbox%2F761268%2F186c458add98021896fc54271002bfcf%2FScreenshot%202024-08-07%20at%2021.45.25.png?generation=1723047619090456&alt=media)\n\n---\n\n> 7. **Direct Imaging**\n - **Time: 00:08:25 - 00:09:09**\n Direct imaging of exoplanets involves capturing pictures of the planets themselves by blocking out the overwhelming light from their parent stars. This method has become possible with the use of devices like coronagraphs, which can effectively mask the starā€™s glare. Direct imaging works best for large planets that are far from their stars and emit their own infrared light. This technique holds promise for future advancements, enabling astronomers to capture images of smaller and cooler planets.\n\n# So, interesting concepts involved in the Ariel data challenge\n\n# Anyone know similar source for \"CH0 Sensor\" ? ", "2947655": "Hi @seshurajup , thank you for the resources. For this challenge you will probably find Transit method and atmosphere detection most useful to this challenge! Of course, having relevant knowledge of the exoplanets will help too!", "2978378": "Out of curiosity, when you mention 'ChatGPT used to make the sections for better understanding', what prompts did you use to improve it?" } }