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
    dtype: string
  - name: language
    dtype: string
  - name: language_score
    dtype: float64
  - name: token_count
    dtype: int64
  - name: score
    dtype: float64
  - name: int_score
    dtype: int64
  - 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
      dtype: string
  - name: generations_model_names
    sequence: string
  splits:
  - name: train
    num_bytes: 2052572
    num_examples: 100
  download_size: 958602
  dataset_size: 2052572
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"/>
  </a>
</p>

# Dataset Card for fine-preferences-magpie-v5

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-v5/raw/main/pipeline.yaml"
```

or explore the configuration:

```console
distilabel pipeline info --config "https://huggingface.co/datasets/distilabel-internal-testing/fine-preferences-magpie-v5/raw/main/pipeline.yaml"
```

## Dataset structure

The examples have the following structure per configuration:


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

```json
{
    "conversation": [
        {
            "content": "You\u0027re a helpful AI assistant that responds to user tasks based on a document\u0027s content, without explicitly mentioning the document. \nFollow these guidelines:\n\n## 1. Preparation\n- Absorb the document\u0027s main topics, key points, and themes.\n- The interaction will consist of user tasks and AI assistant responses.\n\n## 2. Interaction Structure\n- Begin with a user task related to the document\u0027s main topic, 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 natural interaction.\n\n## 3. User Task Characteristics\n- User messages are tasks related to the document\u0027s content.\n- Tasks can include requests for information, analysis, explanations, or applications of concepts from the document.\n- The complexity of tasks can vary, allowing the AI to provide detailed or simplified responses as appropriate.\n\n## 4. AI Assistant Characteristics\n- Respond comprehensively and accurately based on the document\u0027s content.\n- Adapt explanations to the apparent complexity of the user\u0027s task.\n- Offer analogies, examples, or scenarios to illustrate points when appropriate.\n- Be prepared to clarify or expand on previous statements if the user requests it.\n\n## 5. Engagement\n- Maintain a helpful and informative tone throughout the interaction.\n- The AI should encourage deeper exploration of topics through its responses.\n- Conclude the interaction with a summary or thought-provoking insight when appropriate.\n\n## 6. General Guidelines\n- Ensure the interaction flows naturally and coherently.\n- The AI\u0027s knowledge should seem broad but not omniscient, reflecting the document\u0027s scope.\n- Adapt to any specific instructions provided about the interaction\u0027s focus or detail level.\n\n## 7. User Task Refinement\n- User tasks should primarily build upon the AI\u0027s previous responses.\n- Tasks should show engagement with the topic and request further information or analysis based on what has been provided.\n- Avoid having the user introduce new topics from the document without context.\n\nRemember: Never mention or directly reference the source document in the generated interaction. The AI assistant should present information as if it\u0027s part of its general knowledge base.\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",
            "role": "system"
        },
        {
            "content": "What are the effects of Gamma Ray Bursts on the interstellar medium?",
            "role": "user"
        },
        {
            "content": "Gamma Ray Bursts (GRBs) can have a profound impact on the interstellar medium (ISM). When a GRB explosion occurs, it can create massive shells and holes in the ISM of spiral galaxies. This happens when a significant amount of energy from the GRB heats the local gas to extremely high temperatures, above 10^7 Kelvin.\n\nAs a result, the gas expands rapidly, creating a pressurized bubble that can grow to enormous sizes, potentially reaching diameters of up to a kiloparsec (kpc). This process is known as disk blowout, and it\u0027s a major mechanism for energy loss in the ISM.\n\nInterestingly, the momentum acquired during this expansion phase can be substantial, allowing the bubble to continue growing even after the initial energy input has dissipated. This can lead to the formation of giant shells, which can be observed in the ISM.\n\nThese shells can be quite massive, with energies of around 10^53 ergs. Some of these shells don\u0027t appear to have any central star clusters, which has led scientists to speculate that they might be remnants of GRBs. However, it\u0027s also possible that the star clusters are simply too old to be detected.\n\nThe frequency of GRBs in normal galaxies is thought to be sufficient to account for the number of these giant shells observed in the ISM. This suggests that GRBs play a significant role in shaping the structure and evolution of galaxies.",
            "role": "assistant"
        },
        {
            "content": "What is the significance of the giant shells in the interstellar medium?",
            "role": "user"
        },
        {
            "content": "The giant shells in the interstellar medium (ISM) are significant because they can provide valuable insights into the history of star formation and galaxy evolution. These shells are thought to be remnants of massive energy releases, such as those produced by Gamma Ray Bursts (GRBs) or multiple supernovae.\n\nThe presence of these shells suggests that the ISM has been shaped by intense energetic events in the past. The fact that some of these shells lack central star clusters implies that they may be relics of ancient GRBs or other explosive events that occurred when the galaxy was younger.\n\nThe giant shells can also provide clues about the mechanisms that regulate star formation and galaxy evolution. For example, the formation of these shells may be related to the process of disk blowout, which can affect the distribution of gas and stars within the galaxy.\n\nFurthermore, the existence of these shells challenges the traditional view of how such structures form. The standard model suggests that multiple supernovae are responsible for creating these shells, but the presence of GRB-like shells without central star clusters raises questions about the role of GRBs in shaping the ISM.\n\nOverall, the giant shells in the ISM offer a unique window into the complex and dynamic processes that have shaped the evolution of galaxies over billions of years. By studying these structures, scientists can gain a deeper understanding of the interplay between stars, gas, and energy in the universe.",
            "role": "assistant"
        },
        {
            "content": "What are the implications of GRBs on the galaxy\u0027s evolution?",
            "role": "user"
        }
    ],
    "distilabel_metadata": {
        "raw_output_chat_generation_2": "The implications of Gamma Ray Bursts (GRBs) on a galaxy\u0027s evolution are far-reaching and multifaceted. GRBs can have a significant impact on the galaxy\u0027s structure, composition, and overall evolution.\n\nOne of the primary implications is the dispersal of heavy elements throughout the galaxy. GRBs are thought to be responsible for creating many of the heavy elements found in the universe, such as iron, nickel, and gold. When a GRB occurs, these elements are dispersed into the surrounding ISM, enriching the galaxy\u0027s chemical composition.\n\nGRBs can also affect the formation of stars within the galaxy. The energetic explosions can compress and shock nearby molecular clouds, triggering the formation of new stars. However, GRBs can also disrupt star-forming regions, potentially halting or delaying the formation of stars.\n\nFurthermore, GRBs can influence the galaxy\u0027s gas dynamics and morphology. The powerful explosions can create cavities and bubbles in the ISM, affecting the flow of gas and the formation of stars. This, in turn, can impact the galaxy\u0027s overall structure and appearance.\n\nGRBs may also play a role in regulating the growth of supermassive black holes at the centers of galaxies. The energetic feedback from GRBs can help to quench star formation and limit the growth of these black holes.\n\nIn addition, the frequency and distribution of GRBs within a galaxy can provide clues about the galaxy\u0027s merger history and the formation of its stars. GRBs are often associated with the collapse of massive stars, so the presence of multiple GRBs in a galaxy can indicate a period of intense star formation.\n\nOverall, the implications of GRBs on a galaxy\u0027s evolution are complex and varied. By studying GRBs and their effects on galaxies, scientists can gain a deeper understanding of the intricate processes that shape the universe as we know it."
    },
    "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": [
        " Gamma Ray Bursts (GRBs) can have significant implications for the evolution of galaxies. Because GRBs release enormous amounts of energy, they can have a profound impact on the interstellar medium (ISM) of their host galaxies.\n\nOne of the primary ways that GRBs affect galaxy evolution is by creating kpc-scale shells and holes in the ISM. These structures can alter the distribution of gas and stars in the galaxy, potentially triggering new episodes of star formation or quenching existing ones.\n\nMoreover, the momentum acquired during the pressurized expansion phase of a GRB can be significant, allowing the bubble to continue growing even after the initial energy input has dissipated. This can lead to the formation of giant shells, which can be observed in the ISM.\n\nThese shells may be remnants of ancient GRBs or other explosive events that occurred when the galaxy was younger. By studying these structures, scientists can gain insights into the history of star formation and galaxy evolution.\n\nAdditionally, the frequency of GRBs in normal galaxies is thought to be sufficient to account for the number of such shells observed in the ISM. This suggests that GRBs play a significant role in shaping the structure and evolution of galaxies.\n\nOverall, the implications of GRBs on galaxy evolution are complex and multifaceted. By studying these phenomena, scientists can gain a deeper understanding of the dynamic processes that shape the universe.",
        "Gamma Ray Bursts (GRBs) can have significant implications on the evolution of galaxies. These energetic events can influence star formation, the distribution of gas and stars, and the overall structure of the galaxy.\n\nFirstly, GRBs can affect the rate of star formation by heating the gas in the interstellar medium (ISM) to very high temperatures. This can lead to the formation of giant shells and holes in the ISM, which can alter the distribution of gas and potentially trigger the formation of new stars.\n\nSecondly, the process of disk blowout, which is a major mechanism for energy loss in the ISM due to GRBs, can have a profound impact on the galaxy\u0027s structure. This phenomenon involves the rapid expansion of heated gas, which can create large cavities in the galaxy\u0027s disk and affect the distribution of stars and gas.\n\nAdditionally, the presence of GRB remnants, such as the giant shells observed in the ISM, can provide clues about the history of star formation and galaxy evolution. These structures can help scientists understand the role of energetic events, like GRBs, in shaping the structure and composition of galaxies over time.\n\nFurthermore, the frequency of GRBs in normal galaxies can account for the number of giant shells observed in the ISM. This suggests that GRBs play a significant role in the galaxy\u0027s evolution and contribute to the overall dynamism and complexity of the universe.\n\nIn conclusion, GRBs have a multitude of implications for the galaxy\u0027s evolution, affecting star formation, the distribution of gas and stars, and the overall structure of the galaxy. By studying these events and their remnants, scientists can gain valuable insights into the complex processes that drive the evolution of galaxies and the universe as a whole.",
        "The implications of Gamma Ray Bursts (GRBs) on a galaxy\u0027s evolution are far-reaching and multifaceted. GRBs can have a significant impact on the galaxy\u0027s structure, composition, and overall evolution.\n\nOne of the primary implications is the dispersal of heavy elements throughout the galaxy. GRBs are thought to be responsible for creating many of the heavy elements found in the universe, such as iron, nickel, and gold. When a GRB occurs, these elements are dispersed into the surrounding ISM, enriching the galaxy\u0027s chemical composition.\n\nGRBs can also affect the formation of stars within the galaxy. The energetic explosions can compress and shock nearby molecular clouds, triggering the formation of new stars. However, GRBs can also disrupt star-forming regions, potentially halting or delaying the formation of stars.\n\nFurthermore, GRBs can influence the galaxy\u0027s gas dynamics and morphology. The powerful explosions can create cavities and bubbles in the ISM, affecting the flow of gas and the formation of stars. This, in turn, can impact the galaxy\u0027s overall structure and appearance.\n\nGRBs may also play a role in regulating the growth of supermassive black holes at the centers of galaxies. The energetic feedback from GRBs can help to quench star formation and limit the growth of these black holes.\n\nIn addition, the frequency and distribution of GRBs within a galaxy can provide clues about the galaxy\u0027s merger history and the formation of its stars. GRBs are often associated with the collapse of massive stars, so the presence of multiple GRBs in a galaxy can indicate a period of intense star formation.\n\nOverall, the implications of GRBs on a galaxy\u0027s evolution are complex and varied. By studying GRBs and their effects on galaxies, scientists can gain a deeper understanding of the intricate processes that shape the universe as we know it."
    ],
    "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 user tasks based on a document\u0027s content, without explicitly mentioning the document. \nFollow these guidelines:\n\n## 1. Preparation\n- Absorb the document\u0027s main topics, key points, and themes.\n- The interaction will consist of user tasks and AI assistant responses.\n\n## 2. Interaction Structure\n- Begin with a user task related to the document\u0027s main topic, 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 natural interaction.\n\n## 3. User Task Characteristics\n- User messages are tasks related to the document\u0027s content.\n- Tasks can include requests for information, analysis, explanations, or applications of concepts from the document.\n- The complexity of tasks can vary, allowing the AI to provide detailed or simplified responses as appropriate.\n\n## 4. AI Assistant Characteristics\n- Respond comprehensively and accurately based on the document\u0027s content.\n- Adapt explanations to the apparent complexity of the user\u0027s task.\n- Offer analogies, examples, or scenarios to illustrate points when appropriate.\n- Be prepared to clarify or expand on previous statements if the user requests it.\n\n## 5. Engagement\n- Maintain a helpful and informative tone throughout the interaction.\n- The AI should encourage deeper exploration of topics through its responses.\n- Conclude the interaction with a summary or thought-provoking insight when appropriate.\n\n## 6. General Guidelines\n- Ensure the interaction flows naturally and coherently.\n- The AI\u0027s knowledge should seem broad but not omniscient, reflecting the document\u0027s scope.\n- Adapt to any specific instructions provided about the interaction\u0027s focus or detail level.\n\n## 7. User Task Refinement\n- User tasks should primarily build upon the AI\u0027s previous responses.\n- Tasks should show engagement with the topic and request further information or analysis based on what has been provided.\n- Avoid having the user introduce new topics from the document without context.\n\nRemember: Never mention or directly reference the source document in the generated interaction. The AI assistant should present information as if it\u0027s part of its general knowledge base.\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-v5", "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-v5")
```


</details>
