distilabel-internal-testing/fine-preferences-test
收藏数据集卡片 for fine-preferences-test
数据集摘要
该数据集包含一个 pipeline.yaml 文件，可以使用 distilabel CLI 重现生成该数据集的管道：
console distilabel pipeline run --config "https://huggingface.co/datasets/distilabel-internal-testing/fine-preferences-test/raw/main/pipeline.yaml"
或者探索配置：
console distilabel pipeline info --config "https://huggingface.co/datasets/distilabel-internal-testing/fine-preferences-test/raw/main/pipeline.yaml"
数据集结构
示例按照以下结构配置：
<details><summary> 配置: default </summary><hr>
json { "context": "Previous abstract Next abstract Session 40 - The Interstellar Medium. Display session, Tuesday, June 09 Gamma 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. Program listing for Tuesday", "conversation": [ { "content": "What are Gamma Ray Bursts (GRBs) and how do they affect the interstellar medium?", "role": "User" }, { "content": "Gamma Ray Bursts are extremely powerful explosions that can occur in spiral galaxies, and they can create kiloparsec-size shells and holes in the interstellar medium (ISM). This happens when a significant amount of energy from the burst heats the local gas to extremely high temperatures, above 10^7 K.", "role": "Assistant" }, { "content": "Thatu0027s fascinating! How do these GRBs compare to the standard model of shell creation, which involves multiple supernovae?", "role": "User" }, { "content": "The GRB model differs from the standard model in that it can overcome some of the limitations of the supernovae model, such as radiative cooling, evaporative losses, and disk blow-out. The momentum acquired during the pressurized expansion phase of a GRB can be large enough to create a kpc-diameter bubble, even with disk blowout occurring.", "role": "Assistant" }, { "content": "You mentioned that some of these giant shells may be GRB remnants. Can you tell me more about that?", "role": "User" }, { "content": "Yes, some of these giant shells have energies of around 10^53 ergs, and they donu0027t appear to have any obvious central star clusters. Itu0027s possible that these are indeed GRB remnants, although itu0027s worth noting that older star clusters may be difficult to detect.", "role": "Assistant" }, { "content": "How common are GRBs in normal galaxies, and can they account for the number of giant shells we observe?", "role": "User" }, { "content": "According to our understanding, the expected frequency of GRBs in normal galaxies can indeed account for the number of giant shells we see. This suggests that GRBs may play a significant role in shaping the interstellar medium of spiral galaxies.", "role": "Assistant" } ], "distilabel_metadata": { "raw_output_generate_conv_with_context_0": "User: What are Gamma Ray Bursts (GRBs) and how do they affect the interstellar medium? Assistant: Gamma Ray Bursts are extremely powerful explosions that can occur in spiral galaxies, and they can create kiloparsec-size shells and holes in the interstellar medium (ISM). This happens when a significant amount of energy from the burst heats the local gas to extremely high temperatures, above 10^7 K. User: Thatu0027s fascinating! How do these GRBs compare to the standard model of shell creation, which involves multiple supernovae? Assistant: The GRB model differs from the standard model in that it can overcome some of the limitations of the supernovae model, such as radiative cooling, evaporative losses, and disk blow-out. The momentum acquired during the pressurized expansion phase of a GRB can be large enough to create a kpc-diameter bubble, even with disk blowout occurring. User: You mentioned that some of these giant shells may be GRB remnants. Can you tell me more about that? Assistant: Yes, some of these giant shells have energies of around 10^53 ergs, and they donu0027t appear to have any obvious central star clusters. Itu0027s possible that these are indeed GRB remnants, although itu0027s worth noting that older star clusters may be difficult to detect. User: How common are GRBs in normal galaxies, and can they account for the number of giant shells we observe? Assistant: According to our understanding, the expected frequency of GRBs in normal galaxies can indeed account for the number of giant shells we see. This suggests that GRBs may play a significant role in shaping the interstellar medium of spiral galaxies." }, "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-4e80-92b3-7ec88785cc9du003e", "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" }
该子集可以加载为：
python from datasets import load_dataset
ds = load_dataset("distilabel-internal-testing/fine-preferences-test", "default")
或者简单地加载，因为只有一个配置并且命名为 default：
python from datasets import load_dataset
ds = load_dataset("distilabel-internal-testing/fine-preferences-test")
</details>
