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
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  - name: int_score
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  - name: system_prompt
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  - name: conversation
    list:
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      dtype: string
    - name: role
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  - name: gen_conv_model_name
    dtype: string
  - name: generations
    sequence: string
  - name: distilabel_metadata
    struct:
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  - name: generations_model_names
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  splits:
  - name: train
    num_bytes: 2495203
    num_examples: 100
  download_size: 1133248
  dataset_size: 2495203
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-7-2

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-7-2/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-7-2/raw/main/pipeline.yaml"
```

## Dataset structure

The examples have the following structure per configuration:


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

```json
{
    "conversation": [
        {
            "content": "Explain the role of Gamma Ray Bursts (GRBs) in shaping the interstellar medium (ISM) of spiral galaxies, and discuss the implications of this process on our understanding of galaxy evolution.",
            "role": "user"
        },
        {
            "content": "Gamma Ray Bursts (GRBs) play a significant role in shaping the interstellar medium (ISM) of spiral galaxies by creating kiloparsec-size shells and holes through their explosive energy release. When a GRB occurs, a substantial amount of energy is deposited into the local ISM, heating the gas to extremely high temperatures (above 10^7 K). This energy injection leads to a rapid expansion of the gas, resulting in the formation of large bubbles that can eventually blow out of the galactic disk.\n\nThe process of disk blowout is a crucial aspect of GRB-ISM interactions, as it allows the energy released by the GRB to escape the galaxy and affect the surrounding ISM. During the pressurized expansion phase, the bubble acquires significant momentum, which enables it to continue expanding even after the initial energy input has ceased. This momentum-driven expansion can lead to the formation of large, kpc-size shells and holes in the ISM.\n\nThe implications of GRB-ISM interactions on our understanding of galaxy evolution are multifaceted. Firstly, GRBs can contribute significantly to the formation of giant shells and holes in spiral galaxies, which were previously thought to be the result of multiple supernovae explosions. This challenges the standard model of shell formation and highlights the importance of considering alternative mechanisms.\n\nSecondly, the frequency of GRBs in normal galaxies can account for the observed number of giant shells, suggesting that GRBs may be a primary driver of ISM shaping in these galaxies. This, in turn, has implications for our understanding of galaxy evolution, as it suggests that GRBs play a more significant role in shaping the ISM than previously thought.\n\nThirdly, the energy released by GRBs can have a profound impact on the surrounding ISM, potentially affecting the formation of stars and planets. The creation of large bubbles and holes can lead to the dispersal of gas and dust, influencing the availability of raw materials for star formation. Additionally, the radiation and high-energy particles emitted by GRBs can ionize and heat the surrounding gas, further altering the conditions for star formation.\n\nLastly, the study of GRB-ISM interactions can provide valuable insights into the properties of GRBs themselves. By analyzing the effects of GRBs on the ISM, researchers can infer the energy release and explosion mechanisms of these enigmatic events, ultimately shedding light on the underlying physics of GRBs.\n\nIn conclusion, the role of GRBs in shaping the ISM of spiral galaxies is a complex and multifaceted process with significant implications for our",
            "role": "assistant"
        },
        {
            "content": "Can you elaborate on the potential consequences of GRB-ISM interactions on star formation and galaxy evolution?",
            "role": "user"
        },
        {
            "content": "The interactions between Gamma Ray Bursts (GRBs) and the interstellar medium (ISM) can have far-reaching consequences for star formation and galaxy evolution. Here are some potential implications:\n\n1. **Disruption of Star-Forming Regions**: The explosive energy released by GRBs can disperse and destroy star-forming regions, such as molecular clouds and dense gas clumps. This can lead to a temporary suppression of star formation in the affected areas, as the gas is dispersed and becomes unavailable for star formation.\n\n2. **Regulation of Star Formation Rates**: GRBs can regulate star formation rates by controlling the availability of gas and dust in the ISM. By dispersing gas and dust, GRBs can limit the fuel available for star formation, thereby reducing the star formation rate. Conversely, the compression of gas and dust by GRB-driven shocks can trigger the formation of new stars.\n\n3. **Induced Starbursts**: The radiation and high-energy particles emitted by GRBs can compress and shock the surrounding ISM, triggering the formation of new stars. This can lead to induced starbursts, where the GRB acts as a catalyst for star formation.\n\n4. **Galaxy-Scale Outflows**: The energy released by GRBs can drive galaxy-scale outflows, expelling gas and metals from the galaxy. This can affect the chemical evolution of the galaxy, as metals are removed from the system, and can also impact the formation of subsequent generations of stars.\n\n5. **Galaxy Morphology and Structure**: Repeated GRB-ISM interactions can shape the morphology and structure of galaxies. The creation of large bubbles and holes can lead to the formation of galactic fountains, where gas is expelled from the galaxy and then re-accreted, influencing the galaxy\u0027s overall structure and evolution.\n\n6. **Feedback Mechanisms**: GRBs can provide a feedback mechanism, regulating the growth of supermassive black holes at the centers of galaxies. By expelling gas and reducing the fuel available for star formation, GRBs can limit the growth of these black holes.\n\n7. **Cosmic Ray and High-Energy Particle Production**: GRBs can produce copious amounts of cosmic rays and high-energy particles, which can permeate the ISM and affect the formation of stars and planets. These particles can ionize and heat the surrounding gas, influencing the conditions for star formation.\n\n8. **Galaxy Evolution and the Build-Up of the ISM**: The cumulative effect of GRB-ISM interactions over cosmic time can influence the build-up",
            "role": "assistant"
        },
        {
            "content": "Can you provide some examples of how GRBs can affect the formation of stars and planets in the surrounding interstellar medium?",
            "role": "user"
        }
    ],
    "distilabel_metadata": {
        "raw_output_chat_generation_2": "Gamma Ray Bursts (GRBs) can impact the formation of stars and planets in the surrounding interstellar medium (ISM) in several ways:\n\n1. **Ionization and Dissociation**: GRBs can ionize and dissociate the surrounding gas, altering the chemical composition of the ISM. This can affect the formation of molecules, such as CO, HCN, and H2, which are essential for star formation.\n\n2. **Heating and Cooling**: GRBs can heat the ISM, increasing the kinetic energy of the gas and altering its thermal balance. This can affect the cooling rates of the gas, influencing the formation of dense regions and the subsequent collapse of gas into stars.\n\n3. **Turbulence and Fragmentation**: GRBs can inject turbulence into the ISM, leading to the formation of density fluctuations and altering the fragmentation of the gas. This can influence the mass distribution of forming stars and the efficiency of star formation.\n\n4. **Magnetic Field Amplification**: GRBs can amplify magnetic fields in the ISM, which can affect the collapse of gas into stars. Stronger magnetic fields can suppress star formation by inhibiting the collapse of gas, while weaker fields can facilitate star formation.\n\n5. **Dust Destruction**: GRBs can destroy dust grains in the ISM, reducing the amount of dust available for planet formation. This can impact the formation of terrestrial planets, which rely on dust grains to form their cores.\n\n6. **Gas Removal and Stripping**: GRBs can remove gas from the ISM, reducing the fuel available for star formation. This can lead to a decrease in the star formation rate and affect the overall evolution of the galaxy.\n\n7. **Triggering Star Formation**: GRBs can trigger star formation by compressing gas and inducing the collapse of dense regions. This can lead to the formation of new stars and star clusters.\n\n8. **Impact on Planet-Disk Systems**: GRBs can affect the formation and evolution of planet-disk systems by ionizing and heating the disk, altering the chemistry and dynamics of the system. This can impact the formation of planets and the delivery of volatile compounds to planetary surfaces.\n\n9. **Influence on the Initial Mass Function**: GRBs can influence the initial mass function (IMF) of stars, affecting the distribution of stellar masses in the galaxy. This can have implications for the overall evolution of the galaxy and the formation of subsequent generations of stars.\n\n10. **Cosmic Ray and High-Energy Particle Effects**: GRBs can produce copious amounts 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": [
        " Gamma Ray Bursts (GRBs) can significantly affect the formation of stars and planets in the surrounding interstellar medium (ISM) in various ways. Here are some examples:\n\n1. **Disruption of Protoplanetary Disks**: GRBs can emit intense radiation and high-energy particles that can penetrate protoplanetary disks around young stars. This radiation can ionize and heat the disk, potentially disrupting the formation of planets. For instance, a nearby GRB could strip away the outer layers of the protoplanetary disk, leaving the inner regions unprotected from further ionizing radiation.\n\n2. **Photoevaporation**: The intense radiation from a GRB can cause photoevaporation of the protoplanetary disk, leading to the loss of gas and dust. This can affect the formation of planets, as the availability of raw materials for planet formation is reduced.\n\n3. **Generation of Magnetic Fields**: GRBs can generate strong magnetic fields in the ISM, which can influence the formation of stars and planets. Magnetic fields can regulate the accretion of gas and dust onto protostars, impacting the conditions for planet formation. Additionally, magnetic fields can affect the dynamics of protoplanetary disks, influencing the migration and formation of planets.\n\n4. **Triggering of Second-Generation Star Formation**: GRBs can trigger the formation of second-generation stars by compressing and shocking the surrounding ISM, leading to the collapse of molecular clouds and the formation of new stars. These second-generation stars may have different chemical compositions and properties than the first generation of stars, affecting their ability to form planets.\n\n5. **Ionizing Radiation-Induced Chemistry**: The ionizing radiation from GRBs can induce chemical reactions in the ISM, creating molecules and ions that can affect the formation of stars and planets. For instance, the radiation can create molecules that promote or inhibit star formation, depending on the local conditions in the ISM.\n\n6. **Alteration of the ISM Physical Conditions**: GRBs can alter the physical conditions of the ISM, such as temperature, density, and ionization state, affecting the formation of stars and planets. By ionizing and heating the ISM, GRBs can affect the ability of gas and dust to collapse and form stars.\n",
        "Gamma Ray Bursts (GRBs) can affect the formation of stars and planets in the surrounding interstellar medium (ISM) through various mechanisms, including the following examples:\n\n1. **Disruption of Protoplanetary Disks**: GRBs can release a significant amount of high-energy radiation and particles, which can penetrate and disrupt protoplanetary disks around newly formed stars. This can lead to the dispersal of dust and gas, potentially affecting the formation of planets within these disks.\n\n2. **Photoevaporation of Molecular Clouds**: The intense radiation from GRBs can ionize and heat the surrounding ISM, leading to the photoevaporation of molecular clouds. This process can disperse the gas and dust, making it unavailable for star and planet formation.\n\n3. **Triggering Star Formation**: The compression of gas and dust by GRB-driven shocks can trigger the formation of new stars. As the shock wave passes through the ISM, it can compress the gas and dust, leading to the gravitational collapse of dense regions and the formation of new stars. These newly formed stars can then host their own planetary systems.\n\n4. **Stimulating Planetesimal Formation**: The high-energy radiation and particles from GRBs can interact with the dust grains in protoplanetary disks, potentially stimulating the formation of planetesimals. These planetesimals can then grow through collisions and accretion, eventually forming planets.\n\n5. **Altering the Composition of Planetary Atmospheres**: The high-energy particles and radiation from GRBs can interact with the atmospheres of planets, potentially altering their composition. This can have implications for the habitability of these planets and the conditions necessary for life to arise.\n\n6. **Influencing the Formation of Giant Planets**: GRB-driven shocks can compress the gas and dust in protoplanetary disks, potentially affecting the formation of giant planets. The increased density in the disk can lead to the rapid accretion of gas, resulting in the formation of gas giants.\n\n7. **Affecting the Formation of Terrestrial Planets**: The dispersal of gas and dust by GRBs can affect the formation of terrestrial planets. In systems where GRBs are common, the reduced availability",
        "Gamma Ray Bursts (GRBs) can impact the formation of stars and planets in the surrounding interstellar medium (ISM) in several ways:\n\n1. **Ionization and Dissociation**: GRBs can ionize and dissociate the surrounding gas, altering the chemical composition of the ISM. This can affect the formation of molecules, such as CO, HCN, and H2, which are essential for star formation.\n\n2. **Heating and Cooling**: GRBs can heat the ISM, increasing the kinetic energy of the gas and altering its thermal balance. This can affect the cooling rates of the gas, influencing the formation of dense regions and the subsequent collapse of gas into stars.\n\n3. **Turbulence and Fragmentation**: GRBs can inject turbulence into the ISM, leading to the formation of density fluctuations and altering the fragmentation of the gas. This can influence the mass distribution of forming stars and the efficiency of star formation.\n\n4. **Magnetic Field Amplification**: GRBs can amplify magnetic fields in the ISM, which can affect the collapse of gas into stars. Stronger magnetic fields can suppress star formation by inhibiting the collapse of gas, while weaker fields can facilitate star formation.\n\n5. **Dust Destruction**: GRBs can destroy dust grains in the ISM, reducing the amount of dust available for planet formation. This can impact the formation of terrestrial planets, which rely on dust grains to form their cores.\n\n6. **Gas Removal and Stripping**: GRBs can remove gas from the ISM, reducing the fuel available for star formation. This can lead to a decrease in the star formation rate and affect the overall evolution of the galaxy.\n\n7. **Triggering Star Formation**: GRBs can trigger star formation by compressing gas and inducing the collapse of dense regions. This can lead to the formation of new stars and star clusters.\n\n8. **Impact on Planet-Disk Systems**: GRBs can affect the formation and evolution of planet-disk systems by ionizing and heating the disk, altering the chemistry and dynamics of the system. This can impact the formation of planets and the delivery of volatile compounds to planetary surfaces.\n\n9. **Influence on the Initial Mass Function**: GRBs can influence the initial mass function (IMF) of stars, affecting the distribution of stellar masses in the galaxy. This can have implications for the overall evolution of the galaxy and the formation of subsequent generations of stars.\n\n10. **Cosmic Ray and High-Energy Particle Effects**: GRBs can produce copious amounts 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 complex user tasks, follow-up questions, and detailed AI assistant responses.\n\n## 2. Interaction Structure and Roles\n\nThis interaction involves two roles: the User and the AI Assistant. The conversation will follow this structure:\n\n1. User: Provides complex tasks and follow-up questions.\n   First message format: \u003ctask_description\u003e\n   Subsequent messages:\n   a) \u003cquestion_or_comment\u003e\n   b) \u003cnew_task_description\u003e\n\n2. AI Assistant: Responds to tasks and follow-up questions using information from the document.\n\nThe conversation will follow this pattern:\n[TASK] -\u003e AI Response -\u003e [FOLLOW-UP] -\u003e AI Response -\u003e [FOLLOW-UP] -\u003e AI Response -\u003e [NEXT TASK] -\u003e AI Response -\u003e (repeat)\n\nUser Guidelines:\n- The first message MUST be a complex task related to the document\u0027s content.\n- For [FOLLOW-UP], ask for clarification, request examples, challenge the AI\u0027s response, or propose alternatives.\n- Use [NEXT TASK] to introduce a new complex task exploring a different aspect of the document.\n\nAI Assistant Guidelines:\n- Provide detailed responses to tasks and thoughtful engagement with follow-ups.\n- Never mention or reference the source document directly.\n\n## 3. User Task Characteristics\n\nComplex 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\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-7-2", "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-7-2")
```


</details>
