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: 1738104
    num_examples: 100
  download_size: 876872
  dataset_size: 1738104
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-v6-tasky

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

## Dataset structure

The examples have the following structure per configuration:


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

```json
{
    "conversation": [
        {
            "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. Here are some of the key consequences:\n\n1. **Gas Removal and Quenching of Star Formation**: GRBs can heat and expel gas from the galaxy, suppressing star formation and potentially quenching it altogether. This can have a significant impact on the galaxy\u0027s overall evolution, as star formation is a crucial process that shapes the galaxy\u0027s structure and composition.\n2. **Regulation of Supermassive Black Hole Growth**: GRBs are thought to be connected to the formation of supermassive black holes at the centers of galaxies. The energy released by GRBs can regulate the growth of these black holes, preventing them from becoming too massive and dominating the galaxy\u0027s evolution.\n3. **Chemical Evolution and Enrichment**: GRBs can create heavy elements through nucleosynthesis, enriching the interstellar medium and influencing the chemical evolution of the galaxy. This can have a profound impact on the formation of subsequent generations of stars and planets.\n4. **Galaxy Morphology and Structure**: The energy released by GRBs can shape the galaxy\u0027s morphology and structure, creating cavities and holes in the interstellar medium. This can lead to the formation of galaxy-scale outflows, which can affect the distribution of gas and stars within the galaxy.\n5. **Reionization of the Universe**: GRBs are thought to have played a significant role in the reionization of the universe, particularly during the early stages of galaxy evolution. The intense radiation and energy released by GRBs can ionize the surrounding intergalactic medium, contributing to the reionization process.\n6. **Feedback Mechanisms**: GRBs can provide a feedback mechanism, regulating the growth of galaxies and preventing them from becoming too massive. This feedback can occur through the heating and expulsion of gas, as well as the suppression of star formation.\n7. **Cosmic Rays and High-Energy Particles**: GRBs can accelerate high-energy particles, such as cosmic rays, which can propagate throughout the galaxy and affect the formation of stars and planets.\n8. **Galaxy Interactions and Mergers**: GRBs can occur during galaxy interactions and mergers, which can trigger the formation of new stars and affect the overall evolution of the merging galaxies.\n\nIn summary, GRBs can have a profound impact on a galaxy\u0027s evolution, influencing its structure, composition, and overall evolution. The effects of GRBs can be seen in the galaxy\u0027s morphology, star"
    },
    "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. The intense energy released during a GRB can create giant shells and holes in the interstellar medium (ISM), which can affect the distribution of gas and stars within the galaxy.\n\nThe energy input from GRBs can also have a profound impact on the star formation rate in the galaxy. The heating and ionization of the ISM can trigger or suppress star formation, depending on the local conditions. In some cases, the energy input from GRBs can create low-density channels in the ISM, allowing cold gas to flow into the galaxy\u0027s center and triggering a burst of star formation.\n\nAdditionally, the afterglow of a GRB can emit a significant amount of ultraviolet (UV) radiation. This radiation can ionize the ISM, creating a feedback loop that can regulate the star formation rate. The UV radiation can also affect the chemical evolution of the galaxy, by breaking up molecules and creating new elements.\n\nThe frequency and distribution of GRBs in a galaxy can also provide insights into the galaxy\u0027s history of star formation. GRBs are most commonly associated with the deaths of massive stars, so the rate of GRBs in a galaxy can be used to infer the rate of star formation in the past.\n\nFinally, the interaction between GRBs and the ISM can produce high-energy particles and radiation that can affect the galaxy\u0027s magnetic field and cosmic ray population. These particles and radiation can travel to the outer regions of the galaxy, affecting the galactic ecosystem and potentially triggering further star formation.\n\nIn summary, the implications of GRBs on the evolution of galaxies are far-reaching and multifaceted. By studying GRBs and their impact on the ISM, scientists can gain a deeper understanding of the complex and dynamic processes that shape the evolution of galaxies over billions of years.",
        "Gamma Ray Bursts (GRBs) can have significant implications for the evolution of galaxies. Some of these implications include:\n\n1. Energetic feedback: GRBs release enormous amounts of energy, which can have a profound impact on the interstellar medium (ISM) of galaxies. The energy released by a single GRB can heat the local gas to temperatures above 10^7 Kelvin, creating massive shells and holes in the ISM. This process, known as disk blowout, can affect the distribution of gas and stars within the galaxy and play a role in regulating star formation.\n\n2. Metal enrichment: GRBs can contribute to the metal enrichment of the ISM and the intergalactic medium (IGM). When a massive star explodes as a GRB, it ejects heavy elements into the surrounding environment. These elements can later be incorporated into new generations of stars and planets, affecting their composition and potentially influencing the development of life.\n\n3. Triggering star formation: The intense radiation and shockwaves produced by GRBs can trigger the formation of new stars in the surrounding gas. This process, known as \"positive feedback,\" can lead to the formation of dense star clusters and contribute to the overall star formation rate in the galaxy.\n\n4. Galaxy mergers and interactions: GRBs can be used as tracers of galaxy mergers and interactions. When galaxies collide, the resulting gravitational disturbances can increase the rate of star formation, leading to more frequent GRBs. By studying the distribution and properties of GRBs, astronomers can gain insights into the merger history of galaxies and the factors that drive their evolution.\n\n5. Cosmological implications: GRBs can be used as probes of the early universe. Since they are among the most luminous events in the cosmos, they can be detected at great distances and used to study the properties of the IGM and the expansion history of the universe. This information can help us understand the processes that shaped the universe since the Big Bang and the role of GRBs in galaxy evolution.\n\nIn summary, GRBs can have far-reaching implications for the evolution of galaxies, influencing the distribution of gas and stars, metal enrichment, star formation rates, and the overall history of the universe. By studying these events, astronomers can gain valuable insights into the complex processes",
        "The implications of Gamma Ray Bursts (GRBs) on a galaxy\u0027s evolution are far-reaching and multifaceted. Here are some of the key consequences:\n\n1. **Gas Removal and Quenching of Star Formation**: GRBs can heat and expel gas from the galaxy, suppressing star formation and potentially quenching it altogether. This can have a significant impact on the galaxy\u0027s overall evolution, as star formation is a crucial process that shapes the galaxy\u0027s structure and composition.\n2. **Regulation of Supermassive Black Hole Growth**: GRBs are thought to be connected to the formation of supermassive black holes at the centers of galaxies. The energy released by GRBs can regulate the growth of these black holes, preventing them from becoming too massive and dominating the galaxy\u0027s evolution.\n3. **Chemical Evolution and Enrichment**: GRBs can create heavy elements through nucleosynthesis, enriching the interstellar medium and influencing the chemical evolution of the galaxy. This can have a profound impact on the formation of subsequent generations of stars and planets.\n4. **Galaxy Morphology and Structure**: The energy released by GRBs can shape the galaxy\u0027s morphology and structure, creating cavities and holes in the interstellar medium. This can lead to the formation of galaxy-scale outflows, which can affect the distribution of gas and stars within the galaxy.\n5. **Reionization of the Universe**: GRBs are thought to have played a significant role in the reionization of the universe, particularly during the early stages of galaxy evolution. The intense radiation and energy released by GRBs can ionize the surrounding intergalactic medium, contributing to the reionization process.\n6. **Feedback Mechanisms**: GRBs can provide a feedback mechanism, regulating the growth of galaxies and preventing them from becoming too massive. This feedback can occur through the heating and expulsion of gas, as well as the suppression of star formation.\n7. **Cosmic Rays and High-Energy Particles**: GRBs can accelerate high-energy particles, such as cosmic rays, which can propagate throughout the galaxy and affect the formation of stars and planets.\n8. **Galaxy Interactions and Mergers**: GRBs can occur during galaxy interactions and mergers, which can trigger the formation of new stars and affect the overall evolution of the merging galaxies.\n\nIn summary, GRBs can have a profound impact on a galaxy\u0027s evolution, influencing its structure, composition, and overall evolution. The effects of GRBs can be seen in the galaxy\u0027s morphology, star"
    ],
    "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-v6-tasky", "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")
```


</details>
