index int64 1 592 | paper_ids float64 2.31k 2.41k | image stringlengths 10.5k 401k | image_path stringlengths 42 76 | category stringclasses 6
values | question stringlengths 40 253 | A stringlengths 1 167 | B stringlengths 1 128 | C stringlengths 1 138 | D stringlengths 1 165 | answer stringclasses 4
values |
|---|---|---|---|---|---|---|---|---|---|---|
1 | 2,404.17538 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAInAsEDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.17538_figM17fixed1.jpg | Astrophysics of Galaxies (astro-ph.GA) | What is the primary reason for the significant residuals in the observed data fit shown in the image? | Insufficient data points | Incorrect background model | Fixed foreground parameters | Instrumental error | C |
2 | 2,406.04204 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAFqA9EDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.04204_figlcfit.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the primary feature observed in the light curve of the EBLM J0608-59 system? | A single transit event | A double eclipse event | A single eclipse event | A continuous out-of-eclipse variation | B |
3 | 2,402.0606 | "/9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDA(...TRUNCATED) | /root/benchmark/data/2024/2402.06060_fshearbar.jpg | Astrophysics of Galaxies (astro-ph.GA) | "What is the primary cause of the quadrupolar signature observed in the radial velocity map of the s(...TRUNCATED) | Gravitational interactions with a satellite galaxy | Bar-driven flows | Radial shear flow | Tidal forces from a nearby galaxy cluster | C |
4 | 2,405.05127 | "/9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDA(...TRUNCATED) | /root/benchmark/data/2024/2405.05127_figspinchangelinear.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | "What is the characteristic timescale (\\tau) for the spin period of CC Sculptoris as determined by (...TRUNCATED) | 1.1 million years | 2.9 million years | 289,548 years | 211,078 years | C |
5 | 2,405.15844 | "/9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDA(...TRUNCATED) | /root/benchmark/data/2024/2405.15844_figradial.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | "What is the primary characteristic of the region highlighted in purple across all panels in the ima(...TRUNCATED) | A region of high magnetic field intensity | A region of high plasma β | A region of sub-Alfvénic flow | A region of high proton number density | C |
6 | 2,404.15575 | "/9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDA(...TRUNCATED) | /root/benchmark/data/2024/2404.15575_figexportedvibe.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What is the primary reason for shifting the data from the spare cryocooler by +4 Hz in the graph? | To account for the difference in the operating frequency of the two cryocoolers | To enhance the clarity of the graph by separating overlapping data points | To compensate for the phase difference between the two cryocoolers | To adjust for the difference in the measurement time of the two cryocoolers | B |
7 | 2,405.11594 | "/9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDA(...TRUNCATED) | /root/benchmark/data/2024/2405.11594_figapvar.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | "Which spectral line in the upper panel of the image shows a quasi-triplet Zeeman pattern, indicatin(...TRUNCATED) | Mg II 15210 Å | Si II 16911 Å | Ca II 16654 Å | Ce III 16133 Å | D |
8 | 2,403.07395 | "/9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDA(...TRUNCATED) | /root/benchmark/data/2024/2403.07395_figf5.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which model predicts an asymptotically large transport rate as the Prandtl number approaches 1? | The Quasilinear (QL) model | The Closure model | Both models predict this behavior | Neither model predicts this behavior | B |
9 | 2,403.12233 | "/9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDA(...TRUNCATED) | /root/benchmark/data/2024/2403.12233_figrbr.jpg | Astrophysics of Galaxies (astro-ph.GA) | "What is the primary factor that determines the growth rate of edge modes in the left panel of the i(...TRUNCATED) | The multiplicity of the edge modes | The break strength of the galaxy disc | The break radius of the galaxy disc | The type of galaxy disc profile | C |
10 | 2,406.19013 | "/9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDA(...TRUNCATED) | /root/benchmark/data/2024/2406.19013_figspectrum.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | Which feed exhibits the highest relative amplitude at approximately 720 MHz? | A1Y | A10X | B3Y | C12X | A |
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