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: 1627504
    num_examples: 100
  download_size: 793055
  dataset_size: 1627504
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-3

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-3/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-3/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 main factors that contribute to the formation of kpc-size shells and holes in the interstellar medium of spiral galaxies?",
            "role": "user"
        },
        {
            "content": "The formation of kpc-size shells and holes in the interstellar medium (ISM) of spiral galaxies is primarily attributed to the explosive energy released by Gamma Ray Bursts (GRBs). When a significant amount of this energy heats the local gas to temperatures above 10^7 K, it can create large-scale structures in the ISM.\n\nIn particular, the pressurized expansion phase of a GRB can impart a substantial amount of momentum to the surrounding gas, causing it to expand and create a bubble that can grow to sizes of up to a kiloparsec (kpc) in diameter. This process, known as \"snowplowing,\" can overcome the energy losses associated with disk blowout, which is a major mechanism for energy dissipation in these systems.\n\nIt\u0027s worth noting that this mechanism differs from the traditional model, which suggests that multiple supernovae are responsible for creating such large-scale structures in the ISM. The GRB-driven model can potentially overcome some of the limitations of the supernova-driven model, such as radiative cooling, evaporative losses, and disk blowout.",
            "role": "assistant"
        },
        {
            "content": "What are the implications of GRBs being the primary cause of kpc-size shells and holes in the interstellar medium of spiral galaxies?",
            "role": "user"
        },
        {
            "content": "If GRBs are indeed the primary cause of kpc-size shells and holes in the interstellar medium of spiral galaxies, it would have significant implications for our understanding of galaxy evolution and the interstellar medium.\n\nFirstly, it would suggest that GRBs play a more important role in shaping the structure and evolution of galaxies than previously thought. GRBs are extremely powerful events that can release enormous amounts of energy, and if they are capable of creating large-scale structures in the ISM, it would imply that they have a profound impact on the galaxy\u0027s overall morphology and dynamics.\n\nSecondly, it would provide an alternative explanation for the origin of these large-scale structures, which are often attributed to multiple supernovae explosions. This would challenge our current understanding of the role of supernovae in shaping the ISM and galaxy evolution.\n\nThirdly, it would imply that GRBs are more frequent in normal galaxies than previously thought, as the expected frequency of GRBs can account for the number of observed kpc-size shells and holes. This would have significant implications for our understanding of GRB rates and their role in galaxy evolution.\n\nFinally, it would also raise interesting questions about the potential connection between GRBs and the formation of star clusters. If some of these kpc-size shells and holes are indeed GRB remnants, it would suggest that GRBs may be responsible for triggering the formation of star clusters, or that they are somehow related to the same physical processes that give rise to star cluster formation.\n\nOverall, the implications of GRBs being the primary cause of kpc-size shells and holes in the interstellar medium of spiral galaxies would be far-reaching and would require a significant re-evaluation of our current understanding of galaxy evolution and the interstellar medium.",
            "role": "assistant"
        },
        {
            "content": "What are the potential challenges or limitations of the GRB-driven model for the formation of kpc-size shells and holes in the interstellar medium of spiral galaxies?",
            "role": "user"
        }
    ],
    "distilabel_metadata": {
        "raw_output_chat_generation_2": "While the GRB-driven model for the formation of kpc-size shells and holes in the interstellar medium of spiral galaxies is an intriguing idea, there are several potential challenges and limitations to consider:\n\n1. **GRB frequency and rate**: The frequency and rate of GRBs in normal galaxies are still not well constrained. If GRBs are not frequent enough, they may not be able to account for the observed number of kpc-size shells and holes.\n2. **Energy deposition and coupling**: The energy released by a GRB must be efficiently deposited into the ISM to create a kpc-size shell or hole. However, the coupling between the GRB energy and the ISM is not well understood, and it\u0027s unclear how much energy is actually transferred to the ISM.\n3. **ISM density and structure**: The density and structure of the ISM can affect the formation and evolution of kpc-size shells and holes. If the ISM is too dense or has a complex structure, it may be difficult for a GRB to create a large-scale cavity.\n4. **Cooling and radiative losses**: The hot gas created by a GRB can cool rapidly, leading to radiative losses that reduce the energy available to create a kpc-size shell or hole.\n5. **Multiple supernovae and other feedback mechanisms**: Supernovae, stellar winds, and other feedback mechanisms can also create cavities and bubbles in the ISM. It\u0027s possible that these mechanisms may dominate the creation of kpc-size shells and holes, rather than GRBs.\n6. **Galaxy evolution and morphology**: The GRB-driven model may not be applicable to all types of galaxies or at all epochs of galaxy evolution. For example, galaxies with high star formation rates or those in the early universe may have different ISM properties that affect the formation of kpc-size shells and holes.\n7. **Observational signatures**: The observational signatures of GRB-driven kpc-size shells and holes may not be unique or distinguishable from those created by other mechanisms.\n8. **Simulations and modeling**: Current simulations and models of GRB-driven kpc-size shells and holes may not accurately capture the complex physics involved, leading to uncertainties in the results.\n9. **Lack of direct observational evidence**: There is currently no direct observational evidence linking GRBs to the formation of kpc-size shells and holes in spiral galaxies.\n10. **Alternative explanations**: Other mechanisms, such as galaxy interactions, AGN feedback, or magnetic fields, may also be able to"
    },
    "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": [
        " While the GRB-driven model is a promising mechanism for the formation of kpc-size shells and holes in the interstellar medium of spiral galaxies, it also faces several challenges and limitations.\n\nFirstly, the GRB-driven model requires a high rate of GRBs in normal galaxies to account for the observed number of kpc-size shells and holes. However, current estimates of GRB rates suggest that they are relatively rare events, occurring at a rate of only a few per million years in a typical galaxy. Therefore, additional mechanisms may be necessary to explain the observed frequency of these large-scale structures.\n\nSecondly, the GRB-driven model requires that a significant fraction of the GRB energy is deposited into the surrounding medium. However, recent simulations suggest that most of the energy from a GRB may be carried away by the relativistic jet, leaving little energy available for driving the expansion of the surrounding medium.\n\nThirdly, the GRB-driven model assumes that the surrounding medium is composed of a uniform density, which is unlikely to be the case in most galaxies. In a clumpy medium, the GRB-driven expansion may be subject to significant variations in density, leading to complex structures that may not resemble the idealized kpc-size shells and holes.\n\nFinally, the GRB-driven model is still a relatively new idea, and there are many uncertainties associated with the details of the physical processes involved. Further theoretical and observational studies are needed to better understand the role of GRBs in shaping the interstellar medium and to test the predictions of the GRB-driven model.\n\nIn summary, while the GRB-driven model offers a promising mechanism for the formation of kpc-size shells and holes in the interstellar medium of spiral galaxies, it faces several challenges and limitations. Further studies are needed to better understand the physical processes involved and to test the predictions of the model.",
        "There are several potential challenges and limitations to the GRB-driven model for the formation of kpc-size shells and holes in the interstellar medium of spiral galaxies:\n\n1. Detection of GRBs: GRBs are rare events, with a typical rate of one per galaxy per million years. Detecting a GRB that occurred in the past and is responsible for a specific kpc-size shell or hole would be extremely challenging, as the evidence would be faint and difficult to disentangle from other sources of energy input in the ISM.\n\n2. Energy input from other sources: There are many other sources of energy input in the ISM, such as supernovae, stellar winds, and active galactic nuclei. These sources can also produce large-scale structures in the ISM, and it may be difficult to disentangle the effects of GRBs from those of other sources.\n\n3. Radiative cooling: The GRB-driven model assumes that the heated gas expands and cools adiabatically, but in reality, radiative cooling can be a significant factor in the evolution of the gas. This could limit the size and longevity of the kpc-scale structures created by GRBs.\n\n4. Spatial distribution: The spatial distribution of kpc-size shells and holes in spiral galaxies is not uniform, and it is not clear how the GRB-driven model can account for this variability. GRBs are expected to occur randomly throughout the galaxy, but the observed distribution of shells and holes suggests that there may be other factors at play.\n\n5. Injection of metals: GRBs are known to produce large amounts of heavy elements, which can be injected into the ISM. However, the observed metallicity of the ISM in spiral galaxies is relatively low, suggesting that other sources of metal enrichment, such as supernovae, are more dominant. This could limit the role of GRBs in shaping the ISM.\n\nOverall, while the GRB-driven model offers an intriguing alternative to the traditional supernova-driven model for the formation of kpc-size shells and holes in the interstellar medium of spiral galaxies, there are several challenges and limitations that need to be addressed. Further observational and theoretical work will be required to determine the true role of GRBs in shaping",
        "While the GRB-driven model for the formation of kpc-size shells and holes in the interstellar medium of spiral galaxies is an intriguing idea, there are several potential challenges and limitations to consider:\n\n1. **GRB frequency and rate**: The frequency and rate of GRBs in normal galaxies are still not well constrained. If GRBs are not frequent enough, they may not be able to account for the observed number of kpc-size shells and holes.\n2. **Energy deposition and coupling**: The energy released by a GRB must be efficiently deposited into the ISM to create a kpc-size shell or hole. However, the coupling between the GRB energy and the ISM is not well understood, and it\u0027s unclear how much energy is actually transferred to the ISM.\n3. **ISM density and structure**: The density and structure of the ISM can affect the formation and evolution of kpc-size shells and holes. If the ISM is too dense or has a complex structure, it may be difficult for a GRB to create a large-scale cavity.\n4. **Cooling and radiative losses**: The hot gas created by a GRB can cool rapidly, leading to radiative losses that reduce the energy available to create a kpc-size shell or hole.\n5. **Multiple supernovae and other feedback mechanisms**: Supernovae, stellar winds, and other feedback mechanisms can also create cavities and bubbles in the ISM. It\u0027s possible that these mechanisms may dominate the creation of kpc-size shells and holes, rather than GRBs.\n6. **Galaxy evolution and morphology**: The GRB-driven model may not be applicable to all types of galaxies or at all epochs of galaxy evolution. For example, galaxies with high star formation rates or those in the early universe may have different ISM properties that affect the formation of kpc-size shells and holes.\n7. **Observational signatures**: The observational signatures of GRB-driven kpc-size shells and holes may not be unique or distinguishable from those created by other mechanisms.\n8. **Simulations and modeling**: Current simulations and models of GRB-driven kpc-size shells and holes may not accurately capture the complex physics involved, leading to uncertainties in the results.\n9. **Lack of direct observational evidence**: There is currently no direct observational evidence linking GRBs to the formation of kpc-size shells and holes in spiral galaxies.\n10. **Alternative explanations**: Other mechanisms, such as galaxy interactions, AGN feedback, or magnetic fields, may also be able to"
    ],
    "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 a variety of user tasks and questions 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 a mix of user tasks/questions and AI assistant responses.\n\n## 2. Interaction Structure\n- Begin with a user task or question 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 inputs and AI responses.\n- Cover main points from the document through this varied interaction.\n\n## 3. User Input Characteristics\n- User messages should include a mix of:\n  a) Complex tasks requiring in-depth analysis or application\n  b) Moderate difficulty questions or requests\n  c) Simple, straightforward questions\n- Examples of varied user inputs:\n  * Complex: \"Develop a strategy to implement the key recommendations outlined in sections 3 and 4, considering potential obstacles and how to overcome them.\"\n  * Moderate: \"Explain the relationship between factors X and Y discussed in the document, and provide an example of how they interact.\"\n  * Simple: \"What are the three main points made in the introduction?\"\n  * Clarification: \"Could you elaborate on the concept of Z that you just mentioned?\"\n  * Opinion-based: \"Do you think the approach described would be effective in a small business setting? Why or why not?\"\n- Aim for a natural progression of topics, with follow-up questions or tasks building on previous responses.\n\n## 4. AI Assistant Characteristics\n- Adapt your response style and depth to match the complexity of the user\u0027s input.\n- For complex tasks, provide comprehensive, well-structured responses.\n- For simpler questions, offer clear and concise answers.\n- Be prepared to clarify concepts or provide additional examples when asked.\n\n## 5. Engagement\n- Maintain a helpful and informative tone throughout the interaction.\n- For complex tasks, encourage critical thinking by highlighting potential challenges or alternative viewpoints.\n- For simpler questions, use the opportunity to add interesting related facts or context when appropriate.\n\n## 6. General Guidelines\n- Ensure the interaction flows naturally, with a mix of task complexities that might occur in a real conversation.\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 user\u0027s apparent level of understanding.\n\n## 7. Interaction Progression\n- Vary the complexity and type of user inputs throughout the conversation.\n- Allow for natural topic transitions and occasional shifts in focus, as long as they relate to the document\u0027s content.\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-3", "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-3")
```


</details>
