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
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  - name: language
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  - name: conversation
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    - name: role
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  - name: generations
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  - name: distilabel_metadata
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  splits:
  - name: train
    num_bytes: 2578965
    num_examples: 100
  download_size: 1148436
  dataset_size: 2578965
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-4

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-4/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-4/raw/main/pipeline.yaml"
```

## Dataset structure

The examples have the following structure per configuration:


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

```json
{
    "conversation": [
        {
            "content": "Critically evaluate the role of Gamma Ray Bursts (GRBs) in shaping the interstellar medium (ISM) of spiral galaxies.",
            "role": "user"
        },
        {
            "content": "The role of Gamma Ray Bursts (GRBs) in shaping the interstellar medium (ISM) of spiral galaxies is a complex and multifaceted phenomenon that warrants critical evaluation. On one hand, GRBs have the potential to create kiloparsec-size shells and holes in the ISM, which can significantly impact the galaxy\u0027s structure and evolution. On the other hand, the energy released by GRBs can also be lost through various mechanisms, such as disk blowout, radiative cooling, and evaporative losses, which can mitigate their overall impact.\n\nOne of the primary arguments in favor of GRBs playing a significant role in shaping the ISM is their ability to heat the local gas to extremely high temperatures, exceeding 10^7 K. This can lead to the formation of large bubbles that can snowplow through the ISM, creating cavities and shells. The momentum acquired during the pressurized expansion phase can be substantial, allowing the bubble to expand to kiloparsec scales. This process can be more efficient than the standard model of multiple supernovae explosions, which may struggle to overcome radiative cooling and disk blowout.\n\nHowever, it is essential to consider the limitations and uncertainties associated with GRBs as a primary driver of ISM shaping. For instance, the frequency of GRBs in normal galaxies is still a topic of debate, and it is unclear whether they can account for the observed number of giant shells. Additionally, the detection of GRB remnants can be challenging, especially if the central star clusters are old and faint.\n\nAnother critical aspect to evaluate is the potential impact of GRBs on the galaxy\u0027s overall evolution. While GRBs can create large cavities and shells, they may also disrupt the galaxy\u0027s disk and trigger the formation of new stars. This could lead to a complex interplay between GRBs, star formation, and galaxy evolution, which is not yet fully understood.\n\nIn conclusion, while GRBs have the potential to play a significant role in shaping the ISM of spiral galaxies, their impact is likely to be complex and multifaceted. Further research is needed to fully understand the mechanisms by which GRBs interact with the ISM, as well as their overall contribution to galaxy evolution. A critical evaluation of the available evidence suggests that GRBs are likely to be one of several factors that shape the ISM, rather than the sole driver of this process.",
            "role": "assistant"
        },
        {
            "content": "Compare the approach described with two alternative methodologies in the field for creating kiloparsec-size shells and holes in the interstellar medium of spiral galaxies.",
            "role": "user"
        },
        {
            "content": "The approach described, which involves Gamma Ray Bursts (GRBs) creating kiloparsec-size shells and holes in the interstellar medium (ISM) of spiral galaxies, can be compared to two alternative methodologies in the field: the multiple supernovae (SNe) explosion model and the galactic fountain model.\n\n**Multiple Supernovae (SNe) Explosion Model:**\n\nIn this approach, multiple SNe explosions are thought to create kiloparsec-size shells and holes in the ISM. The cumulative energy released by these explosions can heat and expel gas from the galaxy, creating cavities and shells. However, this model has some limitations. For instance, radiative cooling can reduce the effectiveness of SNe in creating large-scale structures, and disk blowout can lead to energy loss. Additionally, the required number of SNe explosions to create kiloparsec-size shells may be unrealistically high.\n\nIn comparison to the GRB approach, the multiple SNe explosion model is more gradual, with energy released over a longer period. This can lead to a more gentle shaping of the ISM, but may not be as effective in creating large-scale structures. The GRB approach, on the other hand, involves a more rapid and intense energy release, which can create larger cavities and shells.\n\n**Galactic Fountain Model:**\n\nThe galactic fountain model proposes that gas is expelled from the galaxy through a process of star formation and supernovae explosions, only to fall back onto the galaxy, creating a circulation of gas. This process can create kiloparsec-size shells and holes in the ISM, but it is a more gradual and continuous process compared to the GRB approach. The galactic fountain model is thought to be more effective in creating smaller-scale structures, such as HI holes and shells, rather than large kiloparsec-size cavities.\n\nIn comparison to the GRB approach, the galactic fountain model is a more gentle and continuous process, with gas being expelled and re-accreted over longer timescales. This can lead to a more subtle shaping of the ISM, with smaller-scale structures being created. The GRB approach, on the other hand, involves a more rapid and intense energy release, which can create larger cavities and shells.\n\n**Comparison Summary:**\n\n| Approach | Energy Release | Timescale | Structure Size | Limitations |\n| --- | --- | --- | --- | --- |\n| GRB | Rapid, intense | Short | Kiloparsec-size | Energy loss through disk",
            "role": "assistant"
        },
        {
            "content": "Based on the trends discussed, forecast potential developments in this area over the next 5-10 years.",
            "role": "user"
        }
    ],
    "distilabel_metadata": {
        "raw_output_chat_generation_2": "Based on the trends discussed, here are some potential developments in the area of Gamma Ray Bursts (GRBs) and their role in shaping the interstellar medium (ISM) of spiral galaxies over the next 5-10 years:\n\n**Short-term developments (2023-2025):**\n\n1. **Improved GRB detection and localization:** The next generation of gamma-ray telescopes, such as the Gamma-Ray Burst Monitor (GBM) on the Fermi Gamma-Ray Space Telescope and the Burst Alert Telescope (BAT) on the Swift Gamma-Ray Burst Mission, will continue to detect and localize GRBs with increasing accuracy. This will provide more precise information on GRB properties and their environments.\n2. **Enhanced simulations and modeling:** Advances in computational power and numerical methods will enable more sophisticated simulations of GRB-ISM interactions, allowing for a better understanding of the complex processes involved.\n3. **Increased focus on multi-messenger astronomy:** The detection of gravitational waves (GWs) by LIGO and VIRGO will continue to provide new insights into the progenitors of GRBs. The combination of GW and electromagnetic observations will help to better understand the role of GRBs in shaping the ISM.\n\n**Mid-term developments (2025-2028):**\n\n1. **Next-generation surveys and telescopes:** The Square Kilometre Array (SKA) and other next-generation radio telescopes will begin to survey the sky, providing unprecedented sensitivity and resolution to study the ISM and GRB-ISM interactions.\n2. **Increased emphasis on GRB-induced star formation:** Researchers will investigate the role of GRBs in triggering star formation, exploring the connection between GRBs and the formation of new stars and stellar clusters.\n3. **Development of new diagnostic tools:** Astronomers will develop and refine new diagnostic tools, such as spectroscopy and imaging, to study the ISM and GRB-ISM interactions in greater detail.\n\n**Long-term developments (2028-2033):**\n\n1. **The rise of multi-messenger astronomy:** The combination of electromagnetic and GW observations will become increasingly important for understanding GRBs and their role in shaping the ISM. The development of new detectors, such as LISA, will enable the detection of GWs from GRBs and other sources.\n2. **Simulations of galaxy evolution:** Researchers will develop more sophisticated simulations of galaxy evolution, incorporating GRBs as a key component of galaxy formation and evolution. These simulations will help to better understand the role of GRBs in shaping the ISM and galaxy structure.\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": [
        " Based on the trends discussed, the following potential developments in the area of creating kiloparsec-size shells and holes in the interstellar medium (ISM) of spiral galaxies can be forecasted over the next 5-10 years:\n\n**GRB Approach:**\n\n* Improved modeling techniques: With the continued development of computational models and simulations, the impact of GRBs on the ISM can be more accurately modeled, taking into account the various mechanisms that can affect their effectiveness, such as energy loss through disk blowout and radiative cooling.\n* Increased observational evidence: With the advent of more sensitive telescopes and detectors, it is likely that more GRB remnants will be detected, providing stronger evidence for their role in shaping the ISM.\n* New insights into GRB properties: With the ongoing study of GRBs, new insights into their properties and behavior can be gained, leading to a better understanding of their impact on the ISM.\n\n**Multiple Supernovae (SNe) Explosion Model:**\n\n* Improved modeling techniques: With the continued development of computational models and simulations, the impact of multiple SNe explosions on the ISM can be more accurately modeled, taking into account the various mechanisms that can affect their effectiveness, such as radiative cooling and disk blowout.\n* New insights into SNe properties: With the ongoing study of SNe, new insights into their properties and behavior can be gained, leading to a better understanding of their impact on the ISM.\n\n**Galactic Fountain Model:**\n\n* Improved modeling techniques: With the continued development of computational models and simulations, the impact of the galactic fountain on the ISM can be more accurately modeled, taking into account the various mechanisms that can affect its effectiveness, such as the rate of gas acceleration and re-accretion.\n* New insights into the galactic fountain process: With the ongoing study of the galactic fountain, new insights into its properties and behavior can be gained, leading to a better understanding of its impact on the ISM.\n\n**Cross-cutting Developments:**\n\n* Comparative studies: Comparative studies between the GRB, multiple SNe explosion, and galactic fountain models can be conducted to better understand the relative contributions of each process in shaping the ISM.\n",
        "Over the next 5-10 years, several potential developments can be expected in the field of understanding the role of Gamma Ray Bursts (GRBs) in shaping the interstellar medium (ISM) of spiral galaxies:\n\n1. **Improved detection capabilities:** With advancements in telescope technology and observational techniques, it is likely that more GRB remnants will be detected, allowing for a better understanding of their frequency and distribution in galaxies. This will help researchers refine models of how GRBs interact with the ISM and their overall contribution to the shaping of the ISM.\n\n2. **Multi-wavelength observations:** The next decade will likely see increased multi-wavelength observations of GRB afterglows, allowing researchers to study the interaction between GRBs and the ISM in more detail. This will provide valuable information on the energy transfer processes at play and help refine models of how GRBs shape the ISM.\n\n3. **Advanced simulations:** As computational power continues to increase, researchers will be able to develop more sophisticated and detailed simulations of the interaction between GRBs and the ISM. These simulations will help to better understand the physical processes involved and provide more accurate predictions of the impact of GRBs on the ISM.\n\n4. **Interdisciplinary research:** The study of how GRBs shape the ISM is inherently interdisciplinary, involving expertise in astrophysics, high-energy physics, and computational modeling. Over the next 5-10 years, it is likely that there will be increased collaboration between researchers in these different fields, leading to a more comprehensive understanding of the role of GRBs in shaping the ISM.\n\n5. **Integration with other models:** As our understanding of how GRBs shape the ISM improves, it is likely that researchers will begin to integrate this knowledge with other models of galaxy evolution. This will help to create a more complete picture of how the ISM interacts with other components of the galaxy, such as stars, dark matter, and magnetic fields.\n\nIn summary, over the next 5-10 years, we can expect significant advances in our understanding of how GRBs shape the ISM of spiral galaxies, driven by improvements in detection capabilities, multi-wavelength observations, advanced simulations, interdisciplinary research, and the integration of GRB models",
        "Based on the trends discussed, here are some potential developments in the area of Gamma Ray Bursts (GRBs) and their role in shaping the interstellar medium (ISM) of spiral galaxies over the next 5-10 years:\n\n**Short-term developments (2023-2025):**\n\n1. **Improved GRB detection and localization:** The next generation of gamma-ray telescopes, such as the Gamma-Ray Burst Monitor (GBM) on the Fermi Gamma-Ray Space Telescope and the Burst Alert Telescope (BAT) on the Swift Gamma-Ray Burst Mission, will continue to detect and localize GRBs with increasing accuracy. This will provide more precise information on GRB properties and their environments.\n2. **Enhanced simulations and modeling:** Advances in computational power and numerical methods will enable more sophisticated simulations of GRB-ISM interactions, allowing for a better understanding of the complex processes involved.\n3. **Increased focus on multi-messenger astronomy:** The detection of gravitational waves (GWs) by LIGO and VIRGO will continue to provide new insights into the progenitors of GRBs. The combination of GW and electromagnetic observations will help to better understand the role of GRBs in shaping the ISM.\n\n**Mid-term developments (2025-2028):**\n\n1. **Next-generation surveys and telescopes:** The Square Kilometre Array (SKA) and other next-generation radio telescopes will begin to survey the sky, providing unprecedented sensitivity and resolution to study the ISM and GRB-ISM interactions.\n2. **Increased emphasis on GRB-induced star formation:** Researchers will investigate the role of GRBs in triggering star formation, exploring the connection between GRBs and the formation of new stars and stellar clusters.\n3. **Development of new diagnostic tools:** Astronomers will develop and refine new diagnostic tools, such as spectroscopy and imaging, to study the ISM and GRB-ISM interactions in greater detail.\n\n**Long-term developments (2028-2033):**\n\n1. **The rise of multi-messenger astronomy:** The combination of electromagnetic and GW observations will become increasingly important for understanding GRBs and their role in shaping the ISM. The development of new detectors, such as LISA, will enable the detection of GWs from GRBs and other sources.\n2. **Simulations of galaxy evolution:** Researchers will develop more sophisticated simulations of galaxy evolution, incorporating GRBs as a key component of galaxy formation and evolution. These simulations will help to better understand the role of GRBs in shaping the ISM and galaxy structure.\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- User messages should represent a diverse range of complex tasks that require in-depth engagement with the document\u0027s content. \n- These may include analysis, synthesis, evaluation, application, prediction, problem-solving, and creative exercises. \n- Tasks should challenge different cognitive skills and perspectives.\n- Tasks should be specific and challenging, often requiring multiple steps or considerations to complete.\n- Examples of complex tasks include:\n  * \"Critically evaluate the assumptions underlying the main argument in the document.\"\n  * \"Compare the approach described with two alternative methodologies in the field.\"\n  * \"Based on the trends discussed, forecast potential developments in this area over the next 5-10 years.\"\n  * \"Identify three major challenges not addressed and propose solutions based on the principles outlined.\"\n  * \"Design an innovative product or service that applies the key concepts presented in a novel way.\"\n  * \"Argue both for and against the main thesis presented, using evidence from the document and potential counterarguments.\"\n  * \"Develop a strategy to implement the key recommendations, considering potential obstacles and how to overcome them.\"\n  * \"Analyze the methodology used and propose three ways it could be improved or expanded for future research.\"\n- Avoid simple questions like \"What is X?\" or \"Why is Y important?\" Instead, frame tasks that require deeper engagement with the material.\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. Ensuring Task Diversity\n- Maintain a balance of task types throughout the interaction. \n- Avoid repeating similar task structures and instead aim for a mix that explores different aspects of critical thinking and application.\n- Tailor the types of tasks to the nature of the document. For technical papers, include more analytical and methodological tasks. For policy documents, focus more on implementation and impact analysis. For theoretical works, emphasize conceptual analysis and application to diverse scenarios.\n\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-4", "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-4")
```


</details>
