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: 2480912
    num_examples: 100
  download_size: 1006617
  dataset_size: 2480912
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-5

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-5/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-5/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 galactic-scale energy release mechanism that could create kiloparsec-sized shells and holes in the interstellar medium of spiral galaxies.",
            "role": "user"
        },
        {
            "content": "To design a galactic-scale energy release mechanism capable of creating kiloparsec-sized shells and holes in the interstellar medium (ISM) of spiral galaxies, I\u0027ll propose a scenario involving Gamma-Ray Bursts (GRBs) as the primary energy source.\n\n**Mechanism:**\n\n1. **GRB Explosion:** A GRB occurs in the disk of a spiral galaxy, releasing an enormous amount of energy (approximately 10^53 ergs) in a short duration ( milliseconds to seconds).\n2. **Initial Expansion:** The explosion creates a hot, high-pressure bubble that expands rapidly into the surrounding ISM. This initial expansion phase is characterized by a high velocity (approximately 10,000 km/s) and a large amount of energy deposited into the ISM.\n3. **Pressurized Expansion Phase:** As the bubble expands, it sweeps up and heats the surrounding ISM, creating a pressurized region. This phase is critical, as it allows the bubble to acquire a significant amount of momentum, which will later contribute to the formation of kiloparsec-sized shells and holes.\n4. **Disk Blowout:** The expanding bubble eventually breaks out of the galactic disk, releasing a significant amount of energy into the halo region. This disk blowout phase marks the beginning of the bubble\u0027s transition from a pressure-driven to a momentum-driven expansion.\n5. **Snowplow Phase:** The bubble, now driven by its acquired momentum, continues to expand and sweep up the surrounding ISM, creating a large, kiloparsec-sized shell or hole. The snowplow phase is characterized by a slower expansion velocity (approximately 100-500 km/s) and a more gradual release of energy into the ISM.\n\n**Key Factors:**\n\n* **Energy Release:** The GRB explosion must release a sufficient amount of energy (approximately 10^53 ergs) to create a large, kiloparsec-sized shell or hole.\n* **ISM Density:** The density of the ISM plays a crucial role in determining the expansion velocity and momentum acquisition during the pressurized expansion phase. A denser ISM will lead to a more efficient transfer of energy and momentum.\n* **Galactic Structure:** The structure of the spiral galaxy, including the presence of spiral arms and the central bulge, can influence the expansion of the bubble and the formation of kiloparsec-sized shells and holes.\n\n**Advantages:**\n\n* **Efficient Energy Transfer:** The GRB explosion and subsequent expansion phases allow for an efficient transfer of",
            "role": "assistant"
        },
        {
            "content": "Design a galactic-scale energy release mechanism that could create kiloparsec-sized shells and holes in the interstellar medium of spiral galaxies.",
            "role": "user"
        },
        {
            "content": "To design a galactic-scale energy release mechanism capable of creating kiloparsec-sized shells and holes in the interstellar medium (ISM) of spiral galaxies, I\u0027ll propose a scenario involving a combination of supernovae (SNe) and stellar winds from massive star clusters.\n\n**Mechanism:**\n\n1. **Massive Star Cluster Formation:** A massive star cluster (MSC) forms in the disk of a spiral galaxy, containing thousands of massive stars (M \u003e 8 M).\n2. **Stellar Winds and SNe:** The massive stars in the MSC undergo intense mass loss through stellar winds, injecting energy and momentum into the surrounding ISM. As these stars reach the end of their lives, they explode as SNe, releasing additional energy and momentum.\n3. **Bubble Formation:** The cumulative effect of the stellar winds and SNe creates a large, hot bubble of gas that expands into the surrounding ISM. This bubble is characterized by a high temperature (T \u003e 10^7 K) and a large amount of energy deposited into the ISM.\n4. **Superbubble Expansion:** The bubble expands rapidly, driven by the continuous injection of energy and momentum from the MSC. As it grows, it sweeps up and heats the surrounding ISM, creating a large, kiloparsec-sized shell or hole.\n5. **ISM Disruption:** The expanding superbubble disrupts the surrounding ISM, creating a region of low density and high temperature. This disruption can lead to the formation of new stars and the triggering of further star formation in the surrounding region.\n\n**Key Factors:**\n\n* **MSC Properties:** The properties of the MSC, such as its mass, size, and star formation rate, play a crucial role in determining the energy and momentum injection into the ISM.\n* **ISM Density:** The density of the ISM affects the expansion velocity and momentum acquisition of the superbubble. A denser ISM will lead to a more efficient transfer of energy and momentum.\n* **Galactic Structure:** The structure of the spiral galaxy, including the presence of spiral arms and the central bulge, can influence the expansion of the superbubble and the formation of kiloparsec-sized shells and holes.\n\n**Advantages:**\n\n* **Sustained Energy Release:** The combination of stellar winds and SNe provides a sustained energy release mechanism, allowing for the creation of large, kiloparsec-sized shells and holes.\n* **Efficient Momentum Transfer:** The superbubble expansion phase allows for an efficient transfer of momentum to the",
            "role": "assistant"
        },
        {
            "content": "Design a galactic-scale energy release mechanism that could create kiloparsec-sized shells and holes in the interstellar medium of spiral galaxies.",
            "role": "user"
        }
    ],
    "distilabel_metadata": {
        "raw_output_chat_generation_2": "Here\u0027s a design for a galactic-scale energy release mechanism that could create kiloparsec-sized shells and holes in the interstellar medium (ISM) of spiral galaxies:\n\n**Mechanism:**\n\n**Galactic Center Magnetic Reconnection Event (GCMRE)**\n\nThe GCMRE is a catastrophic event that occurs when the magnetic fields of the galactic center, fueled by the supermassive black hole (SMBH) and the surrounding starburst region, build up and suddenly reconnect. This event releases an enormous amount of energy, which propagates outward from the galactic center, shaping the ISM and creating kiloparsec-sized shells and holes.\n\n**Energy Release:**\n\n1. **Magnetic Field Build-up:** The SMBH and the surrounding starburst region generate strong magnetic fields, which build up over time. These fields are fueled by the SMBH\u0027s spin-down, accretion of material, and the intense star formation activity in the starburst region.\n2. **Magnetic Reconnection:** When the magnetic fields reach a critical threshold, they suddenly reconnect, releasing an enormous amount of energy (\u2248 10^55 ergs). This energy is comparable to the total energy released by a million supernovae.\n3. **Energy Propagation:** The released energy propagates outward from the galactic center as a powerful shockwave, accelerating particles and heating the ISM. This shockwave expands at a velocity of \u2248 10,000 km/s, sweeping up and shaping the surrounding ISM.\n\n**ISM Shaping:**\n\n1. **Shell Formation:** As the shockwave expands, it compresses and heats the ISM, creating a large, kiloparsec-sized shell of dense, hot gas. This shell can be tens of parsecs thick and contains a significant fraction of the galaxy\u0027s gas mass.\n2. **Hole Creation:** The shockwave can also create kiloparsec-sized holes in the ISM by expelling gas from the galaxy\u0027s disk. These holes can be filled with hot, ionized gas that is visible in X-rays and other wavelengths.\n3. **ISM Turbulence:** The GCMRE event injects a large amount of turbulence into the ISM, driving the formation of molecular clouds and star-forming regions. This turbulence can also regulate the galaxy\u0027s star formation rate and chemical evolution.\n\n**Key Factors:**\n\n* **SMBH Mass and Spin:** The mass and spin of the SMBH play a crucial role in determining the strength and build-up of"
    },
    "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": [
        " To design a galactic-scale energy release mechanism capable of creating kiloparsec-sized shells and holes in the interstellar medium (ISM) of spiral galaxies, I\u0027ll propose a scenario involving the collision of high-velocity clouds (HVCs) with the disk of a spiral galaxy.\n\n**Mechanism:**\n\n1. **HVC Formation:** HVCs form through various mechanisms, such as the cooling of hot gas in the galactic halo, tidal interactions with nearby galaxies, or the expansion of supernova remnants in the halo.\n2. **HVC Collision:** An HVC with a mass of approximately 10^6 M and a velocity of several hundred km/s collides with the disk of a spiral galaxy.\n3. **Shock Wave Formation:** The collision between the HVC and the disk of the spiral galaxy generates a shock wave that propagates into the ISM. This shock wave compresses and heats the ISM, creating a large, hot bubble of gas.\n4. **Shell Formation:** The expanding shock wave sweeps up and heats the surrounding ISM, creating a large, kiloparsec-sized shell or hole. The shell is characterized by a high temperature (T \u003e 10^6 K) and a large amount of energy deposited into the ISM.\n5. **ISM Disruption and Feedback:** The expanding shell disrupts the surrounding ISM, creating a region of low density and high temperature. This disruption can lead to the triggering of star formation and the injection of energy into the ISM through feedback processes, such as supernova explosions and stellar winds.\n\n**Key Factors:**\n\n* **HVC Properties:** The properties of the HVC, such as its mass, size, and velocity, play a crucial role in determining the energy and momentum injection into the ISM.\n* **ISM Density:** The density of the ISM affects the expansion velocity and momentum acquisition of the shell. A denser ISM will lead to a more efficient transfer of energy and momentum.\n* **Galactic Structure:** The structure of the spiral galaxy, including the presence of spiral arms and the central bulge, can influence the expansion of the shell and the formation of kiloparsec-sized shells and holes.\n\n**",
        "To design a galactic-scale energy release mechanism capable of creating kiloparsec-sized shells and holes in the interstellar medium (ISM) of spiral galaxies, I\u0027ll propose a scenario involving the interaction of active galactic nuclei (AGN) jets with the surrounding ISM.\n\n**Mechanism:**\n\n1. **AGN Activation:** A supermassive black hole (SMBH) at the center of a spiral galaxy becomes active, launching jets of relativistic particles and energy in opposite directions.\n2. **Jet Expansion:** The AGN jets expand into the surrounding ISM, creating a large, hot bubble of gas. The expansion is driven by the continuous injection of energy and momentum from the AGN.\n3. **Shock Waves:** The jets interact with the ISM, creating a series of shock waves that heat and compress the surrounding gas. These shock waves can propagate through the ISM, creating large-scale structures such as shells and holes.\n4. **Cocoon Expansion:** The shocked gas, now forming a \"cocoon\" around the AGN jets, expands into the ISM, sweeping up and heating the surrounding material. This expansion can create kiloparsec-sized shells and holes in the ISM.\n5. **ISM Disruption:** The expanding cocoon disrupts the surrounding ISM, creating a region of low density and high temperature. This disruption can lead to the formation of new stars and the triggering of further star formation in the surrounding region.\n\n**Key Factors:**\n\n* **AGN Properties:** The properties of the AGN, such as its luminosity, jet orientation, and jet power, play a crucial role in determining the energy and momentum injection into the ISM.\n* **ISM Density:** The density of the ISM affects the expansion velocity and momentum acquisition of the AGN jets. A denser ISM will lead to a more efficient transfer of energy and momentum.\n* **Galactic Structure:** The structure of the spiral galaxy, including the presence of spiral arms and the central bulge, can influence the expansion of the AGN jets and the formation of kiloparsec-sized shells and holes.\n\n**Advantages:**\n\n* **High Energy Release:** The AGN jets provide a",
        "Here\u0027s a design for a galactic-scale energy release mechanism that could create kiloparsec-sized shells and holes in the interstellar medium (ISM) of spiral galaxies:\n\n**Mechanism:**\n\n**Galactic Center Magnetic Reconnection Event (GCMRE)**\n\nThe GCMRE is a catastrophic event that occurs when the magnetic fields of the galactic center, fueled by the supermassive black hole (SMBH) and the surrounding starburst region, build up and suddenly reconnect. This event releases an enormous amount of energy, which propagates outward from the galactic center, shaping the ISM and creating kiloparsec-sized shells and holes.\n\n**Energy Release:**\n\n1. **Magnetic Field Build-up:** The SMBH and the surrounding starburst region generate strong magnetic fields, which build up over time. These fields are fueled by the SMBH\u0027s spin-down, accretion of material, and the intense star formation activity in the starburst region.\n2. **Magnetic Reconnection:** When the magnetic fields reach a critical threshold, they suddenly reconnect, releasing an enormous amount of energy (\u2248 10^55 ergs). This energy is comparable to the total energy released by a million supernovae.\n3. **Energy Propagation:** The released energy propagates outward from the galactic center as a powerful shockwave, accelerating particles and heating the ISM. This shockwave expands at a velocity of \u2248 10,000 km/s, sweeping up and shaping the surrounding ISM.\n\n**ISM Shaping:**\n\n1. **Shell Formation:** As the shockwave expands, it compresses and heats the ISM, creating a large, kiloparsec-sized shell of dense, hot gas. This shell can be tens of parsecs thick and contains a significant fraction of the galaxy\u0027s gas mass.\n2. **Hole Creation:** The shockwave can also create kiloparsec-sized holes in the ISM by expelling gas from the galaxy\u0027s disk. These holes can be filled with hot, ionized gas that is visible in X-rays and other wavelengths.\n3. **ISM Turbulence:** The GCMRE event injects a large amount of turbulence into the ISM, driving the formation of molecular clouds and star-forming regions. This turbulence can also regulate the galaxy\u0027s star formation rate and chemical evolution.\n\n**Key Factors:**\n\n* **SMBH Mass and Spin:** The mass and spin of the SMBH play a crucial role in determining the strength and build-up of"
    ],
    "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. 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-5", "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-5")
```


</details>
