distilabel-internal-testing/fine-preferences-test-2

---
size_categories: n<1K
tags:
- synthetic
- distilabel
- rlaif
---

<p align="left">
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# Dataset Card for fine-preferences-test-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-test-2/raw/main/pipeline.yaml"
```

or explore the configuration:

```console
distilabel pipeline info --config "https://huggingface.co/datasets/distilabel-internal-testing/fine-preferences-test-2/raw/main/pipeline.yaml"
```

## Dataset structure

The examples have the following structure per configuration:

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

```json
{
"context": "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",
"conversation": [
{
"content": "I\u0027m trying to understand the impact of Gamma Ray Bursts (GRBs) on the interstellar medium (ISM). Can you explain how they create kpc-size shells and holes in spiral galaxies?",
"role": "User"
},
{
"content": "GRBs can heat the local gas to above 10^7 K, causing a pressurized expansion that creates large bubbles. These bubbles can snowplow to a kpc diameter, even with disk blowout, which is a major energy loss mechanism.",
"role": "Assistant"
},
{
"content": "That\u0027s fascinating! How does this process differ from the standard model of shell formation through multiple supernovae?",
"role": "User"
},
{
"content": "The standard model has issues with radiative cooling, evaporative losses, and disk blow-out, whereas GRBs can create large shells without these limitations. The momentum acquired during the expansion phase is sufficient to overcome these losses.",
"role": "Assistant"
},
{
"content": "I see. Are there any observations that support the idea that GRBs can create these giant shells?",
"role": "User"
},
{
"content": "Yes, there\u0027s evidence for giant shells with energies of around 10^53 ergs. Some of these shells don\u0027t have obvious central star clusters, which could indicate that they\u0027re GRB remnants. However, it\u0027s possible that older star clusters might be hard to detect.",
"role": "Assistant"
},
{
"content": "That\u0027s really interesting. Can you tell me more about the expected frequency of GRBs in normal galaxies and how it relates to the number of observed shells?",
"role": "User"
},
{
"content": "The expected frequency of GRBs in normal galaxies can actually account for the number of observed shells. This suggests that GRBs might be a significant contributor to the formation of these large structures.",
"role": "Assistant"
},
{
"content": "I\u0027d love to learn more about the program listing for Tuesday. Are there any sessions or talks that focus specifically on GRBs and their impact on the ISM?",
"role": "User"
}
],
"distilabel_metadata": {
"raw_output_generate_conv_with_context_0": "User: I\u0027m trying to understand the impact of Gamma Ray Bursts (GRBs) on the interstellar medium (ISM). Can you explain how they create kpc-size shells and holes in spiral galaxies?\nAssistant: GRBs can heat the local gas to above 10^7 K, causing a pressurized expansion that creates large bubbles. These bubbles can snowplow to a kpc diameter, even with disk blowout, which is a major energy loss mechanism.\nUser: That\u0027s fascinating! How does this process differ from the standard model of shell formation through multiple supernovae?\nAssistant: The standard model has issues with radiative cooling, evaporative losses, and disk blow-out, whereas GRBs can create large shells without these limitations. The momentum acquired during the expansion phase is sufficient to overcome these losses.\nUser: I see. Are there any observations that support the idea that GRBs can create these giant shells?\nAssistant: Yes, there\u0027s evidence for giant shells with energies of around 10^53 ergs. Some of these shells don\u0027t have obvious central star clusters, which could indicate that they\u0027re GRB remnants. However, it\u0027s possible that older star clusters might be hard to detect.\nUser: That\u0027s really interesting. Can you tell me more about the expected frequency of GRBs in normal galaxies and how it relates to the number of observed shells?\nAssistant: The expected frequency of GRBs in normal galaxies can actually account for the number of observed shells. This suggests that GRBs might be a significant contributor to the formation of these large structures.\nUser: I\u0027d love to learn more about the program listing for Tuesday. Are there any sessions or talks that focus specifically on GRBs and their impact on the ISM?"
},
"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",
"id": "\u003curn:uuid:e2300ad5-01dd-4e80-92b3-7ec88785cc9d\u003e",
"int_score": 3,
"language": "en",
"language_score": 0.9126408100128174,
"model_name": "meta-llama/Meta-Llama-3-70B-Instruct",
"score": 2.765625,
"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-test-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-test-2")
```

</details>

原始信息汇总

数据集概述

数据集名称

• 名称: fine-preferences-test-2

数据集创建工具

• 工具: distilabel

数据集大小

• 大小: n<1K

数据集标签

• 标签:
  • synthetic
  • distilabel
  • rlaif

数据集结构

• 结构: 数据集包含一个pipeline.yaml文件，用于在distilabel中重现生成数据集的流程。

数据集示例结构

• 示例结构: 每个示例包含以下信息：
  • 上下文（context）
  • 对话（conversation）
  • distilabel元数据（distilabel_metadata）
  • 转储信息（dump）
  • 文件路径（file_path）
  • ID（id）
  • 内部评分（int_score）
  • 语言（language）
  • 语言评分（language_score）
  • 模型名称（model_name）
  • 评分（score）
  • 令牌计数（token_count）
  • URL（url）

数据集加载方式

• 加载方式:
  • 通过Python代码加载数据集，可以使用以下命令： python from datasets import load_dataset ds = load_dataset("distilabel-internal-testing/fine-preferences-test-2")