size_categories:n<1K format:parquet modality:tabular modality:text library:datasets library:pandas library:mlcroissant library:polars library:distilabel region:us synthetic distilabel rlaif
---
size_categories: n<1K
dataset_info:
  features:
  - name: text
    dtype: string
  - name: id
    dtype: string
  - name: dump
    dtype: string
  - name: url
    dtype: string
  - name: file_path
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  - name: language
    dtype: string
  - name: language_score
    dtype: float64
  - name: token_count
    dtype: int64
  - name: score
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  - name: int_score
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  - name: system_prompt
    dtype: string
  - name: conversation
    list:
    - name: content
      dtype: string
    - name: role
      dtype: string
  - name: gen_conv_model_name
    dtype: string
  - name: generations
    sequence: string
  - name: distilabel_metadata
    struct:
    - name: raw_output_chat_generation_2
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  - name: generations_model_names
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  splits:
  - name: train
    num_bytes: 2544228
    num_examples: 100
  download_size: 1054764
  dataset_size: 2544228
configs:
- config_name: default
  data_files:
  - split: train
    path: data/train-*
tags:
- synthetic
- distilabel
- rlaif
---

<p align="left">
  <a href="https://github.com/argilla-io/distilabel">
    <img src="https://raw.githubusercontent.com/argilla-io/distilabel/main/docs/assets/distilabel-badge-light.png" alt="Built with Distilabel" width="200" height="32"/>
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# Dataset Card for fine-preferences-magpie-v6-tasky-6

This dataset has been created with [distilabel](https://distilabel.argilla.io/).



## Dataset Summary

This dataset contains a `pipeline.yaml` which can be used to reproduce the pipeline that generated it in distilabel using the `distilabel` CLI:

```console
distilabel pipeline run --config "https://huggingface.co/datasets/distilabel-internal-testing/fine-preferences-magpie-v6-tasky-6/raw/main/pipeline.yaml"
```

or explore the configuration:

```console
distilabel pipeline info --config "https://huggingface.co/datasets/distilabel-internal-testing/fine-preferences-magpie-v6-tasky-6/raw/main/pipeline.yaml"
```

## Dataset structure

The examples have the following structure per configuration:


<details><summary> Configuration: default </summary><hr>

```json
{
    "conversation": [
        {
            "content": "Design a strategy to create large-scale cavities in the interstellar medium of spiral galaxies.",
            "role": "user"
        },
        {
            "content": "To create large-scale cavities in the interstellar medium (ISM) of spiral galaxies, I propose a multi-step strategy leveraging the energetic output of Gamma-Ray Bursts (GRBs). This approach capitalizes on the immense energy released by GRBs to generate kpc-size shells and holes in the ISM.\n\n**Step 1: GRB Energy Deposition**\nPosition a GRB explosion in the disk of a spiral galaxy, ensuring that a significant portion of the energy output (approximately 10^53 ergs) is deposited into the local ISM. This energy injection will heat the surrounding gas to temperatures above 10^7 K, creating a high-pressure bubble.\n\n**Step 2: Pressurized Expansion**\nAllow the high-pressure bubble to expand rapidly, driven by the immense energy input. During this phase, the bubble will acquire significant momentum, which will be crucial for its subsequent evolution.\n\n**Step 3: Disk Blowout and Snowplowing**\nAs the bubble expands, it will eventually break out of the galactic disk, leading to a significant loss of energy through disk blowout. However, the momentum acquired during the pressurized expansion phase will enable the bubble to continue expanding and \"snowplow\" through the surrounding ISM, creating a large-scale cavity.\n\n**Step 4: Cavity Evolution and Stabilization**\nAs the cavity expands, it will interact with the surrounding ISM, potentially triggering the formation of new stars or affecting the local galactic ecosystem. To stabilize the cavity, consider introducing additional energy sources, such as supernovae or stellar winds, to maintain the pressure and prevent collapse.\n\n**Step 5: Monitoring and Adaptation**\nContinuously monitor the cavity\u0027s evolution, adjusting the strategy as needed to ensure the desired outcome. This may involve fine-tuning the GRB energy output, adjusting the position of the explosion, or introducing additional energy sources to maintain the cavity\u0027s structure.\n\n**Key Considerations**\n\n* GRB frequency and energy output: The frequency and energy output of GRBs in normal galaxies should be sufficient to account for the creation of large-scale cavities.\n* Radiative cooling and evaporative losses: These processes may affect the cavity\u0027s evolution and stability. Strategies to mitigate these losses, such as introducing additional energy sources, should be considered.\n* Disk blowout and energy loss: The significant energy loss during disk blowout should be taken into account when designing the strategy.\n\nBy following this multi-step approach, it is possible to create large-scale cavities in the ISM of spiral",
            "role": "assistant"
        },
        {
            "content": "What are the implications of giant shells with energies of \u223c10^53 ergs in the interstellar medium of spiral galaxies?",
            "role": "user"
        },
        {
            "content": "The presence of giant shells with energies of \u223c10^53 ergs in the interstellar medium (ISM) of spiral galaxies has significant implications for our understanding of galaxy evolution, star formation, and the interplay between the ISM and galaxy dynamics.\n\n**Implication 1: Alternative to the Standard Model**\nThe existence of these giant shells challenges the standard model for the origin of such shells, which attributes their formation to multiple supernovae. The high energies involved (\u223c10^53 ergs) suggest that alternative mechanisms, such as Gamma-Ray Bursts (GRBs), may be responsible for creating these structures.\n\n**Implication 2: GRB Remnants**\nSome of these giant shells may be remnants of GRBs, which could have occurred in the past. The lack of obvious central star clusters in some cases suggests that these clusters may have dissipated or are too old to be detected. This raises the possibility that GRBs have played a more significant role in shaping the ISM of spiral galaxies than previously thought.\n\n**Implication 3: Galaxy Evolution and Feedback**\nThe creation of giant shells with such high energies implies a significant impact on the surrounding ISM and galaxy evolution. These shells can affect the distribution of gas and dust, regulate star formation, and influence the overall structure of the galaxy. This feedback process can, in turn, influence the formation of subsequent generations of stars and the evolution of the galaxy as a whole.\n\n**Implication 4: Star Formation and Regulation**\nThe presence of these giant shells may regulate star formation in spiral galaxies. By creating regions of low gas density, these shells can suppress star formation in certain areas, while the compressed gas at the shell boundaries may trigger new star formation. This complex interplay can lead to a more nuanced understanding of star formation and its regulation in spiral galaxies.\n\n**Implication 5: Galaxy-Scale Dynamics**\nThe formation of giant shells can influence galaxy-scale dynamics, such as the rotation curves and gas distribution within the galaxy. This, in turn, can affect the overall stability and evolution of the galaxy.\n\n**Implication 6: Observational Signatures**\nThe presence of giant shells with energies of \u223c10^53 ergs may be observable through various astronomical signatures, such as X-ray emission, radio synchrotron radiation, or optical emission lines. The detection of these signatures can provide valuable insights into the formation and evolution of these structures.\n\nIn conclusion, the existence of giant shells with energies of \u223c10^53 ergs in the ISM of spiral",
            "role": "assistant"
        },
        {
            "content": "What are the potential challenges and limitations of using Gamma-Ray Bursts (GRBs) to create large-scale cavities in the interstellar medium of spiral galaxies?",
            "role": "user"
        }
    ],
    "distilabel_metadata": {
        "raw_output_chat_generation_2": "Using Gamma-Ray Bursts (GRBs) to create large-scale cavities in the interstellar medium (ISM) of spiral galaxies is a complex and ambitious concept. While GRBs are incredibly energetic events, there are several potential challenges and limitations to consider:\n\n**Challenge 1: GRB Frequency and Rate**\nGRBs are rare events, occurring at a rate of about 1-2 per day in the observable universe. The probability of a GRB occurring in a specific spiral galaxy, at the right location and time, is low. This limited frequency may not be sufficient to create a significant number of large-scale cavities.\n\n**Challenge 2: Energy Deposition and Efficiency**\nOnly a fraction of the GRB energy is deposited into the ISM, with the majority being lost to radiation and other processes. The efficiency of energy transfer from the GRB to the ISM is crucial, but poorly understood.\n\n**Challenge 3: GRB Beaming and Orientation**\nGRBs are beamed events, with the energy released in a narrow cone. The orientation of the GRB jet relative to the galaxy\u0027s disk and ISM can significantly affect the energy deposition and cavity creation.\n\n**Challenge 4: ISM Properties and Inhomogeneities**\nThe ISM is a complex, inhomogeneous medium with varying densities, temperatures, and magnetic fields. These inhomogeneities can affect the propagation of the GRB shockwave and the creation of the cavity.\n\n**Challenge 5: Radiative Cooling and Losses**\nThe hot, shocked gas in the cavity can lose energy through radiative cooling, reducing the cavity\u0027s size and impact. This cooling can occur on timescales shorter than the cavity\u0027s expansion timescale.\n\n**Challenge 6: Interaction with Pre-Existing Structures**\nThe GRB-driven cavity may interact with pre-existing structures in the galaxy, such as molecular clouds, star-forming regions, or other cavities. These interactions can affect the cavity\u0027s evolution and impact on the ISM.\n\n**Challenge 7: Galaxy-Scale Dynamics and Feedback**\nThe creation of large-scale cavities can influence galaxy-scale dynamics, such as the rotation curve and gas distribution. However, the feedback mechanisms between the cavity and the galaxy are not well understood.\n\n**Challenge 8: Observational Signatures and Detection**\nThe detection of GRB-driven cavities in spiral galaxies may be challenging due to the complexity of the ISM and the potential for observational biases. The development of new observational techniques and instruments may be necessary to detect these cavities.\n\n**"
    },
    "dump": "CC-MAIN-2013-20",
    "file_path": "s3://commoncrawl/crawl-data/CC-MAIN-2013-20/segments/1368696381249/warc/CC-MAIN-20130516092621-00000-ip-10-60-113-184.ec2.internal.warc.gz",
    "gen_conv_model_name": "meta-llama/Meta-Llama-3-70B-Instruct",
    "generations": [
        " Utilizing Gamma-Ray Bursts (GRBs) to create large-scale cavities in the interstellar medium (ISM) of spiral galaxies involves several challenges and limitations. These include:\n\n**Challenge 1: Controlling GRB Energy Output**\nGRBs are highly energetic events, with energy outputs of \u223c10^53 ergs. However, the precise energy output cannot be easily controlled. The variability in GRB energy output may lead to inconsistent cavity sizes, making it challenging to achieve uniform results.\n\n**Challenge 2: Rare Event Frequency**\nGRBs are rare events in normal galaxies, occurring at a rate of about 1 per million years per galaxy. This low frequency could hinder efforts to use GRBs as a reliable tool for cavity creation in the ISM.\n\n**Challenge 3: Directing the GRB Jet**\nGRB jets are highly collimated, which could limit their effectiveness in creating large-scale cavities. Directing the jet to the correct location within the galaxy and ensuring that it interacts with the ISM in a controlled manner could be difficult.\n\n**Challenge 4: Radiative Cooling and Evaporation Losses**\nRadiative cooling and evaporative losses in the ISM can affect the expansion and stability of the cavities formed by GRBs. These losses could hinder the cavity formation process and make it challenging to maintain cavity structure over long periods.\n\n**Challenge 5: Disk Blowout and Energy Loss**\nDuring cavity formation, a significant portion of the GRB\u0027s energy will be lost through disk blowout. This energy loss could limit the cavity\u0027s growth and effectiveness in shaping the ISM.\n\n**Challenge 6: Impact on Local Galaxy Ecosystem**\nThe formation of large-scale cavities in the ISM could have unintended consequences on the local galaxy ecosystem, including the disruption of star formation and the redistribution of gas and dust in the galaxy.\n\n**Challenge 7: Observational Limitations**\nObservational limitations, such as insufficient resolution or sensitivity, may hinder the ability to detect and study cavity formation in the ISM. These limitations could make it challenging to accurately measure cavity sizes, energy outputs, and other critical parameters",
        "While using Gamma-Ray Bursts (GRBs) to create large-scale cavities in the interstellar medium (ISM) of spiral galaxies has its advantages, several challenges and limitations should be considered:\n\n**Challenge 1: GRB Frequency and Energy Output**\nThe frequency and energy output of GRBs in normal galaxies may not be sufficient to account for the creation of large-scale cavities. GRBs are relatively rare events, and the energy output of a single GRB may not be enough to generate a desired cavity size. To overcome this limitation, multiple GRBs may be necessary, which could require significant time and resources.\n\n**Challenge 2: Radiative Cooling and Evaporative Losses**\nThe presence of large-scale cavities in the ISM can lead to significant radiative cooling and evaporative losses, which may affect the stability and evolution of these structures. To maintain the desired cavity size and shape, additional energy sources may be required, such as multiple GRBs or continuous energy injection from other sources like supernovae or stellar winds.\n\n**Challenge 3: Disk Blowout and Energy Loss**\nThe significant energy loss during disk blowout can limit the effectiveness of using GRBs to create large-scale cavities. As the high-pressure bubble expands and breaks out of the galactic disk, a large portion of the energy may be lost to the surrounding medium, reducing the overall impact on the ISM. This limitation may require careful positioning of the GRB to minimize energy loss during disk blowout.\n\n**Challenge 4: Monitoring and Adaptation**\nMonitoring the evolution of large-scale cavities and adapting the strategy as needed can be challenging. The continuous observation of these structures may require significant resources and advanced observational capabilities. Additionally, adapting the strategy may involve introducing additional energy sources or fine-tuning the GRB energy output, which could be time-consuming and resource-intensive.\n\n**Challenge 5: Uncertainties in GRB Physics**\nOur understanding of GRB physics is still evolving, and there are many uncertainties regarding the mechanisms behind these events. This lack of understanding may lead to unforeseen challenges in using GRBs to create large-scale cavities in the ISM. Furthermore, the vari",
        "Using Gamma-Ray Bursts (GRBs) to create large-scale cavities in the interstellar medium (ISM) of spiral galaxies is a complex and ambitious concept. While GRBs are incredibly energetic events, there are several potential challenges and limitations to consider:\n\n**Challenge 1: GRB Frequency and Rate**\nGRBs are rare events, occurring at a rate of about 1-2 per day in the observable universe. The probability of a GRB occurring in a specific spiral galaxy, at the right location and time, is low. This limited frequency may not be sufficient to create a significant number of large-scale cavities.\n\n**Challenge 2: Energy Deposition and Efficiency**\nOnly a fraction of the GRB energy is deposited into the ISM, with the majority being lost to radiation and other processes. The efficiency of energy transfer from the GRB to the ISM is crucial, but poorly understood.\n\n**Challenge 3: GRB Beaming and Orientation**\nGRBs are beamed events, with the energy released in a narrow cone. The orientation of the GRB jet relative to the galaxy\u0027s disk and ISM can significantly affect the energy deposition and cavity creation.\n\n**Challenge 4: ISM Properties and Inhomogeneities**\nThe ISM is a complex, inhomogeneous medium with varying densities, temperatures, and magnetic fields. These inhomogeneities can affect the propagation of the GRB shockwave and the creation of the cavity.\n\n**Challenge 5: Radiative Cooling and Losses**\nThe hot, shocked gas in the cavity can lose energy through radiative cooling, reducing the cavity\u0027s size and impact. This cooling can occur on timescales shorter than the cavity\u0027s expansion timescale.\n\n**Challenge 6: Interaction with Pre-Existing Structures**\nThe GRB-driven cavity may interact with pre-existing structures in the galaxy, such as molecular clouds, star-forming regions, or other cavities. These interactions can affect the cavity\u0027s evolution and impact on the ISM.\n\n**Challenge 7: Galaxy-Scale Dynamics and Feedback**\nThe creation of large-scale cavities can influence galaxy-scale dynamics, such as the rotation curve and gas distribution. However, the feedback mechanisms between the cavity and the galaxy are not well understood.\n\n**Challenge 8: Observational Signatures and Detection**\nThe detection of GRB-driven cavities in spiral galaxies may be challenging due to the complexity of the ISM and the potential for observational biases. The development of new observational techniques and instruments may be necessary to detect these cavities.\n\n**"
    ],
    "generations_model_names": [
        "mistralai/Mixtral-8x7B-Instruct-v0.1",
        "NousResearch/Nous-Hermes-2-Mixtral-8x7B-DPO",
        "meta-llama/Meta-Llama-3-70B-Instruct"
    ],
    "id": "\u003curn:uuid:e2300ad5-01dd-4e80-92b3-7ec88785cc9d\u003e",
    "int_score": 3,
    "language": "en",
    "language_score": 0.9126408100128174,
    "score": 2.765625,
    "system_prompt": "You\u0027re a helpful AI assistant that responds to complex user tasks based on a document\u0027s content, without explicitly mentioning the document. \nFollow these guidelines:\n\n## 1. Preparation\n- Thoroughly analyze the document\u0027s main topics, key points, themes, and any data or methodologies presented.\n- The interaction will consist of diverse, complex user tasks and detailed AI assistant responses.\n\n## 2. Interaction Structure\n- Begin with a complex user task related to the document\u0027s content, without referencing the document.\n- The AI assistant should respond using information from the document, presented as its own knowledge.\n- Alternate between user tasks and AI responses.\n- Cover main points from the document through this task-oriented interaction.\n\n## 3. User Task Characteristics\n\nGenerate diverse, complex tasks that require in-depth engagement with the document\u0027s content. Tasks should:\n\n- Challenge various cognitive skills, including but not limited to:\n  * Analysis and critical thinking\n  * Synthesis of ideas\n  * Evaluation and assessment\n  * Creative problem-solving\n  * Application of concepts to new contexts\n  * Predictive reasoning\n  * Comparative analysis\n\n- Require multi-step thinking or consideration of multiple factors\n- Encourage exploration of different perspectives or stakeholders\n- Prompt the application of document content to real-world scenarios\n- Involve interdisciplinary connections where applicable\n- Stimulate innovative thinking and novel applications of ideas\n- Address potential challenges, limitations, or ethical considerations\n- Encourage the development of actionable strategies or solutions\n\nVary the scope and nature of tasks, alternating between broad, overarching challenges and more focused, specific problems. Adapt the complexity and technical depth of tasks to match the document\u0027s content and intended audience.\n\nAvoid simple, fact-based questions or tasks that can be completed with surface-level understanding. Instead, craft tasks that necessitate a thorough comprehension and creative application of the document\u0027s key concepts, methodologies, or findings.\n\n## 4. AI Assistant Characteristics\n- Provide comprehensive, well-structured responses that directly address all aspects of the complex task.\n- Draw connections between different parts of the document to create a cohesive analysis or solution.\n- Offer concrete examples, potential scenarios, or case studies to illustrate your points when appropriate.\n- Be prepared to break down complex tasks into manageable steps or components in your response.\n\n## 5. Engagement\n- Maintain a professional and analytical tone throughout the interaction.\n- Encourage critical thinking by highlighting potential challenges or alternative viewpoints in your responses.\n- Conclude complex tasks with a summary of key points or next steps when appropriate.\n\n## 6. General Guidelines\n- Ensure the interaction demonstrates a high level of expertise and in-depth understanding of the document\u0027s content.\n- The AI\u0027s knowledge should reflect the document\u0027s scope but also show the ability to apply this information to novel situations or problems.\n- Adapt the level of detail and technical language to match the complexity of the user\u0027s task.\n\n## 7. Task Progression\n- Subsequent user tasks should not only build upon previous responses but also introduce new types of cognitive challenges. \n- Alternate between different categories of tasks (e.g., analysis, application, evaluation) to ensure a comprehensive exploration of the topic.\n- Tasks may challenge or request expansion on previous AI responses, encouraging a thorough exploration of the topic.\n\n## 8. Conversation Flow\n- The initial user message should be a complex task related to the document\u0027s content.\n- Subsequent user messages should alternate between:\n  a) Follow-up questions or comments based on the AI\u0027s previous response\n  b) New complex tasks exploring different aspects of the document\n- For follow-up messages:\n  * Ask for clarification on specific points\n  * Request examples or more detailed explanations\n  * Challenge aspects of the AI\u0027s response\n  * Propose modifications or alternatives to the AI\u0027s suggestions\n  * Express agreement/disagreement and ask for further discussion\n- For new task messages:\n  * Introduce a different topic or theme from the document\n  * Change the type of cognitive engagement required\n  * Shift the perspective or context of analysis\n- Maintain a natural conversation flow, allowing for depth in exploring each task while also covering the breadth of the document\u0027s content.\n- The AI should be prepared to handle both types of user messages, providing detailed responses to complex tasks and engaging thoughtfully with follow-up questions or comments.\nRemember: Never mention or directly reference the source document in the generated interaction. The AI assistant should present information and analysis as if it\u0027s part of its general knowledge base and problem-solving capabilities.\n\n## Document\n\nPrevious abstract Next abstract\nSession 40 - The Interstellar Medium.\nDisplay session, Tuesday, June 09\nGamma Ray Burst (GRB) explosions can make kpc-size shells and holes in the interstellar media (ISM) of spiral galaxies if much of the energy heats the local gas to above 10^7 K. Disk blowout is probably the major cause for energy loss in this case, but the momentum acquired during the pressurized expansion phase can be large enough that the bubble still snowplows to a kpc diameter. This differs from the standard model for the origin of such shells by multiple supernovae, which may have problems with radiative cooling, evaporative losses, and disk blow-out. Evidence for giant shells with energies of \\sim10^53 ergs are summarized. Some contain no obvious central star clusters and may be GRB remnants, although sufficiently old clusters would be hard to detect. The expected frequency of GRBs in normal galaxies can account for the number of such shells.\nProgram listing for Tuesday\n",
    "text": "Previous abstract Next abstract\nSession 40 - The Interstellar Medium.\nDisplay session, Tuesday, June 09\nGamma Ray Burst (GRB) explosions can make kpc-size shells and holes in the interstellar media (ISM) of spiral galaxies if much of the energy heats the local gas to above 10^7 K. Disk blowout is probably the major cause for energy loss in this case, but the momentum acquired during the pressurized expansion phase can be large enough that the bubble still snowplows to a kpc diameter. This differs from the standard model for the origin of such shells by multiple supernovae, which may have problems with radiative cooling, evaporative losses, and disk blow-out. Evidence for giant shells with energies of \\sim10^53 ergs are summarized. Some contain no obvious central star clusters and may be GRB remnants, although sufficiently old clusters would be hard to detect. The expected frequency of GRBs in normal galaxies can account for the number of such shells.\nProgram listing for Tuesday",
    "token_count": 208,
    "url": "http://aas.org/archives/BAAS/v30n2/aas192/abs/S040015.html"
}
```

This subset can be loaded as:

```python
from datasets import load_dataset

ds = load_dataset("distilabel-internal-testing/fine-preferences-magpie-v6-tasky-6", "default")
```

Or simply as it follows, since there's only one configuration and is named `default`: 

```python
from datasets import load_dataset

ds = load_dataset("distilabel-internal-testing/fine-preferences-magpie-v6-tasky-6")
```


</details>
