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/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAITA/8DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /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 simulated galaxy? | 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/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAGZAlADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /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 the current study? | 1.1 million years | 2.9 million years | 289,548 years | 211,078 years | C |
5 | 2,405.15844 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJWBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /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 image? | 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/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAIMA7oDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /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/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAKDBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /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, indicating a strong magnetic field? | Mg II 15210 Å | Si II 16911 Å | Ca II 16654 Å | Ce III 16133 Å | D |
8 | 2,403.07395 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCALfA/8DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /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/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAFeBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /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 image? | 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/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJzBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /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 |
11 | 2,402.04343 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAEJA7UDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2402.04343_figALMAmaps.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which molecular transition is represented by the cyan contours in the center-left panel of the image? | CO (2-1) | SO (6-5) | CN peak emission | H2 S(7) | C |
12 | 2,403.06575 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAOUBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.06575_figcomp.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following studies does not show a turnover in the star-forming main sequence (MS) relation? | Speagle et al. (2014) | Tomczak et al. (2016) | Popesso et al. (2023) | This work | A |
13 | 2,401.11221 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAFOBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2401.11221_theoreticallineratio.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which line ratio is most resistant to change by the external stellar radiation field? | Si-IV/C-IV | N-V/O-VI | C-II/C-IV | None of the above | B |
14 | 2,407.1209 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQAA/kDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.12090_figSFR.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which model shows a more bursty nature of star formation, as indicated by the higher peaks in the star formation rate (SFR) and intrinsic UV magnitude ($M_{\rm 1500}$) in the image? | Gravo-thermo-turbulent model | Sink particle algorithm | Both models show similar burstiness | Neither model shows bursty star formation | B |
15 | 2,405.19135 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAMuA/8DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2405.19135_figcrowding.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What does the magenta line in the image represent? | The distribution of stars in the NGC 3377 field | The relationship between the local crowding level and the galactocentric radius | The surface brightness profile of the galaxy | The background sky brightness | B |
16 | 2,407.16757 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCANSBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.16757_figphotdistrib.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What is the primary purpose of the simulated photon counts distribution shown in the image? | To measure the quantum efficiency of the silicon drift detector (SDD) | To determine the uniformity of the photon distribution across the detector chamber door | To estimate the incident flux on the chamber door | To calculate the vorticity of the photon distribution | B |
17 | 2,407.1374 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQAA0EDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.13740_figmultipanelgridsB.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following is a common feature in the parallax contours of the microlensing events shown in the image? | Highly elongated contours in all panels | Consistent central peaks across all modeling approaches | Exclusion of central regions in the π_EN-π_EE space | Uniform color coding across all panels | D |
18 | 2,311.137 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAHqBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2311.13700_figsampleage.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following features is most strongly associated with the presence of a classical bulge in the galaxies shown in the image? | A strong positive radial gradient in the thin disk | A strong negative radial gradient in the thick disk | A region enclosed by vertical dashed black lines | A region with the youngest stars concentrated in an inner region | C |
19 | 2,406.14101 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAERAbYDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.14101_figvelocityscatternoM.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | Which method shows a better correlation between the predicted and true velocity magnitudes in the scatter plot? | FFT | Unet | Both methods show equal correlation | Neither method shows a significant correlation | B |
20 | 2,403.1691 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAP/A2UDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.16910_figexample.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which solar wind type is characterized by the most uniform presence of large-amplitude fluctuations, indicative of anti-sunward propagating Alfvén waves? | Magnetic Cloud | Sheath | Fast Wind | Slow Solar Wind | C |
21 | 2,311.16991 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAI0A8wDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2311.16991_figlikelihoodvsOmega.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the primary conclusion drawn from the plot of the log of the likelihood function against the rotation rates $v/v_\mathrm{crit}$ for the young open cluster NGC 2516? | The majority of stars in the cluster rotate at rates greater than 50% of their critical value. | The likelihood function is independent of the rotation rates. | The cluster's CMD is best reproduced by isochrones with $v/v_\mathrm{crit} \leq 0.4$. | The cluster's CMD is best reproduced by isochrones with $v/v_\mathrm{crit} \geq 0.5$. | C |
22 | 2,404.02211 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAMkBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.02211_figdlyamuv.jpg | Astrophysics of Galaxies (astro-ph.GA) | What is the primary characteristic of the galaxy population with the strongest Ly$\alpha$ emission ($D_{\rm Ly\alpha} < -100\,\AA$) as indicated by the scatter plot? | High UV brightness ($M_{\rm UV} < -16$\,mag) | Low UV brightness ($M_{\rm UV} > -19$\,mag) | High redshift ($z < 5.5$) | High HI gas overdensities | B |
23 | 2,406.01716 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAFKAssDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.01716_figRTSjumps.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What is the primary cause of the observed variations in the hot pixel's dark current as shown in the image? | Thermal fluctuations in the detector | Quantum fluctuations in the pixel's charge carriers | External cosmic rays impacting the detector | Software artifacts during data processing | B |
24 | 2,405.14238 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQABAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2405.14238_figinstancecore.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | Which celestial object is most likely represented by the green mask with a confidence level of 0.999? | A distant galaxy | A bright star | A planet within the Milky Way | A satellite or artificial object | B |
25 | 2,404.08728 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAGKA2wDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.08728_figmeasstdevs.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What is the primary reason for the larger uncertainties in the inner ring of segments as shown in the right panel of the image? | Higher segment piston measurements in the inner ring | Partial blockage caused by the central obscuration of the telescope top end | Increased atmospheric distortion in the inner ring | Higher density of segments in the inner ring | B |
26 | 2,404.18658 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAF2BAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.18658_figAgedependencekineamtics.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which kinematic parameter shows the most significant variation for clusters in the age range of 100-200 Myr? | Inclination (i) | Position angle of the line of nodes ($\Theta$) | Scale radius ($R_0$) | None of the above | A |
27 | 2,404.16201 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAKMBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.16201_figspectrumjd2.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which emission line in the spectrum of MACS0647-JD shows the most significant detection? | [OII] | [OIII] | [HeI] | [NeII] | A |
28 | 2,407.10079 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAFHBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.10079_figalignmentdiskphisp.jpg | Astrophysics of Galaxies (astro-ph.GA) | What is the primary effect of increasing the volume filling factor of iron clusters inside dust grains ($\phi_{\rm sp}$) on the distribution of dust grain sizes within 400 au of the disk midplane? | Decreased magnetic alignment of very large grains (VLGs) | Increased internal alignment of dust grains | Enhanced Magnetic Alignment by Radiative Torques (MRAT) alignment for micron-sized grains | Reduced polarization degree within the disk scale | C |
29 | 2,407.04113 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAESAZMDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.04113_figbarlength.jpg | Astrophysics of Galaxies (astro-ph.GA) | What is the primary cause of the two distinct buckling events observed in the plot of the bar semi-major axis? | Galactic mergers | Gravitational interactions with satellite galaxies | Internal dynamical instabilities | External tidal forces | C |
30 | 2,404.17622 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQAAfgDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.17622_figfigure2.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What is the primary periodic signal frequency detected in the synthetic time series datasets 'Signal x(t)' and 'Signal y(t)'? | 1Hz | 2Hz | 3Hz | 4Hz | B |
31 | 2,406.04166 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJXArsDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.04166_Figbayesiancbdpost.jpg | Astrophysics of Galaxies (astro-ph.GA) | What does the concentration of red points around the center of the Colour-Brightness Diagram (CBD) indicate about the stellar population in this region? | A higher density of early-type stars | A higher density of late-type stars | A higher density of intermediate-type stars | A higher density of white dwarfs | B |
32 | 2,406.06174 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQAAu0DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.06174_figExample.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What does the lower panel of the image represent? | The raw flux measurements of the star | The difference between PDCSAP and SAP fluxes | The cleaned light curve of the star in magnitudes | The standard deviation of the flux measurements | C |
33 | 2,401.02876 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCALzBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2401.02876_Figmapsc201.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following best describes the relationship between the H$\alpha$ and NUV emissions in CIG 201? | The H$\alpha$ emission is more extended than the NUV emission. | The NUV emission is more extended than the H$\alpha$ emission. | The H$\alpha$ and NUV emissions have similar extents. | The H$\alpha$ and NUV emissions are anti-correlated. | C |
34 | 2,404.09791 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQAA1YDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.09791_figGRBARSFRnorm.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following is a common underlying physical process governing the formation of the central gas reservoir and the triggering of star formation in the simulated galaxies? | Galactic rotation | Supernova feedback | Bar strength evolution | Dark matter halo formation | C |
35 | 2,406.13146 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAMeBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.13146_figPq1.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which of the following binary systems is predicted to be in the stable mass transfer phase according to the figure? | NGC 247 ULX-1 | V445 Pup | HD 49798 | Max-RMS | C |
36 | 2,402.13806 | /9j/4AAQSkZJRgABAQAAAQABAAD//gAfTEVBRCBUZWNobm9sb2dpZXMgSW5jLiBWMS4wMQD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAMWA/8DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcI... | /root/benchmark/data/2024/2402.13806_Fig3.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What does the strong negative correlation (r = -0.99) between the imbalance of radial velocity fluxes and the unsigned magnetic flux suggest about the behavior of solar material? | The solar material is moving outward at higher magnetic fluxes | The solar material is moving downward at higher magnetic fluxes | The solar material is moving outward at lower magnetic fluxes | The solar material is moving downward at lower magnetic fluxes | B |
37 | 2,406.19229 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAMUBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.19229_figNewDIBsJK.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following statements best describes the relationship between the equivalent width (EW) of the DIBs at $\lambda$14795 Å and the $E(J-K)$ index for the CygOB2 association? | The EW of the DIBs increases linearly with the $E(J-K)$ index. | The EW of the DIBs remains nearly constant despite varying $E(J-K)$ index. | The EW of the DIBs decreases as the $E(J-K)$ index increases. | The EW of the DIBs shows a random distribution with no clear trend. | B |
38 | 2,403.00247 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJwBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.00247_figmapawpropermotionsnew.jpg | Astrophysics of Galaxies (astro-ph.GA) | What is the primary kinematic feature observed in the Lagoon Nebula Cluster (LNC) as depicted in the image? | Contraction of the stellar groups | Rotation of the stellar groups around a common center | Expansion of the stellar groups | Random motion of individual stars | C |
39 | 2,405.1812 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJqBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2405.18120_figdynamicalparams.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which dynamical property of stars in the Galactic disk shows a notable positive correlation with the absolute metallicity excess ($\left| \delta \text{[Fe/H]} \right|$) according to the image? | Angular momentum (J$_z$) | Vertical action (J$_z$) | Radial action (J$_r$) | Total energy | C |
40 | 2,406.0228 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJtBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.02280_emmapssh1.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which temperature range is associated with the 'warm rain' in the coronal rain event depicted in the image? | log T = 5.1 - 6.2 | log T = 5.5 - 6.2 | log T = 5.7 - 6.4 | log T = 5.9 - 6.6 | B |
41 | 2,401.12728 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAESA/8DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2401.12728_fighist.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the prevailing orientation of the local gravity in the high-mass star-forming region NGC 2264? | Approximately 30° | Approximately 40° to 50° | Approximately 150° | Approximately 144° | B |
42 | 2,406.10394 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAFmBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.10394_figPrelimDesign.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What is the primary design consideration that led to the selection of a Gregorian reflector system for the Black Hole Explorer (BHEX) spaceborne antenna? | Maximizing the aperture size to increase light collection | Minimizing the focal length to diameter ratio (F/D_m) for a more compact design | Optimizing the edge taper angle (\theta_e) for better illumination efficiency | Reducing the subreflector to main reflector diameter ratio (D_s/D_m) to minimize blockage | C |
43 | 2,406.13022 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJcBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.13022_figdata.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the primary feature highlighted by the dark orange region in the top panel of the image? | A solar flare | A magnetic cloud interval | A coronal mass ejection (CME) leading edge | A region of high plasma beta | B |
44 | 2,401.13737 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAIHBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2401.13737_figelzsun.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following best describes the distribution of in-situ stars in the $E-L_z$ space for the simulation with an initial vertical metallicity gradient only? | A uniform distribution of metallicity across all energy levels | A concentration of metal-rich stars at high energies and low angular momenta | A concentration of metal-poor stars at high energies and low angular momenta | A bimodal distribution with both metal-rich and metal-poor stars at high energies | C |
45 | 2,407.0036 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQABAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.00360_figfigure5.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the current evolutionary stage of SZ Lyn as indicated by its position on the Hertzsprung-Russell diagram? | Pre-main sequence | Main sequence | Post-main sequence | Red giant | C |
46 | 2,310.16026 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQAA94DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2310.16026_f3.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which of the following parameters is most strongly correlated with the HD fluxes at both 112 $\mu$m and 56 $\mu$m wavelengths, as indicated by the color coding in the scatter plot? | Disk gas mass | Central star luminosity | Chemical age of the disk | Distance to the disk | B |
47 | 2,407.14421 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAKGBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.14421_figincomega.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the primary reason for the observed trend in the distribution of arguments of periastron ($\omega$) for doubly-eclipsing binary systems, as shown in the image? | The gravitational influence of a third body | The orientation of the orbits favoring double eclipses | The presence of a circumstellar disk | The effect of general relativistic precession | B |
48 | 2,405.0427 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAHHA/8DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2405.04270_fig1.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following dual-AGN systems shows a significant increase in SNR with the reduction of long baseline weight, followed by a decrease? | J2206+0003A | J2232+0012A | J0051+0020B | J2300-0005A | C |
49 | 2,407.07229 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAHsBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.07229_figgalaxyfittingloss.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | Which model generates galaxies with a galaxy fitting loss closer to that of real galaxies across all redshift bins? | DDPM | CVAE | Real | Both DDPM and CVAE | A |
50 | 2,407.03709 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAPxBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.03709_figexamplefiltering.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the primary effect of applying a 60-day high-pass filter to the light curve LC1, as shown in the image? | Enhancement of long-period signals | Removal of short-period signals | Suppression of long-period variability | Amplification of noise | C |
51 | 2,407.09684 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJtA/8DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.09684_figfootpointexpansion.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which parameter shows the highest median value for non-CH SASW compared to other wind streams? | Photospheric footpoint field strength (B0) | AIA 193Å intensity | Expansion factor (f_ss) | Electron temperature | C |
52 | 2,407.08046 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJYAxQDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.08046_figorangelineplot.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | Which system exhibits a more consistent performance across different azimuthal coordinates? | TCS system | Both systems equally | Neural Network (NN) system | Neither system | C |
53 | 2,406.09144 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAFOBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.09144_figfastVSslowstd.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | Which algorithm provides a lower relative uncertainty in regions of high surface brightness? | Resolve algorithm | Fast-resolve algorithm | Both algorithms provide the same relative uncertainty | Neither algorithm provides a lower relative uncertainty | B |
54 | 2,405.19388 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAOEAy0DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2405.19388_fighrd.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the primary factor that correlates with the distribution of $\delta$ Scuti variables in the Hertzsprung-Russell diagram? | Stellar mass | Stellar age | Stellar rotation velocity | Stellar metallicity | C |
55 | 2,404.0349 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCALoA3sDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.03490_figlambdadistrib.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | Which physical parameter does the latent parameter $\theta_3$ most strongly correlate with in the Interpolatory Auto-Encoder (IAE) model? | Redshift (z) | Temperature (kT) | Both equally | Neither | A |
56 | 2,401.17553 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAHTAioDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2401.17553_figmasssize.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following simulations predicts a larger effective radius (Re) for a given stellar mass (M*) compared to the other? | EAGLE | TNG-100 | Both predict similar Re for a given M* | Neither, as both underestimate Re for a given M* | A |
57 | 2,402.14954 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAKqBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2402.14954_figvalidated.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which classifier has a higher true positive rate for identifying rotation periods? | Classifier #1 | Classifier #2 | Both have the same true positive rate | Cannot be determined from the image | B |
58 | 2,407.09427 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCANNBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.09427_figasfgridclumpcomparison.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the primary reason for the systematic discrepancy between the CNF$_{\mathrm{asfgrid}}$ and Yu et al. (2018) mass and radius estimates? | Use of different input data | Use of different model grids | Use of different asteroseismic scaling relations | Use of different computational methods | D |
59 | 2,407.14873 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQAA5oDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.14873_figM87realresolveCLEAN.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | Which of the following is a characteristic feature of the Bayesian self-calibration image (top panel) compared to the CLEAN image (bottom panel) in the provided image? | Higher noise level | More pronounced negative flux | Clearer counter-jet structure | Less extended jet emission | C |
60 | 2,403.16867 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJSBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.16867_figcompdfgwffgwf1.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which scenario in the image shows a distinct bump of systems around a few mHz, contributing to a slight increase in confusion noise in that frequency band? | Low spins, weak tides | Low spins, strong tides | GWs only | Accreting systems | B |
61 | 2,406.17123 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCANkBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.17123_figIC1553lines.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which line ratio shows the most significant variation with height above the galactic plane in the IC1553 galaxy? | [NII]/Hα | [SII]/Hα | [OIII]/Hβ | [OI]/Hα | D |
62 | 2,401.11869 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCALuAV4DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2401.11869_figLC.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which convection parameter set (A, B, C, or D) shows the least variation in the bolometric light curve? | A | B | C | D | A |
63 | 2,404.16926 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAPwBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.16926_figfcovIC.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following statements is true about the HI covering fraction in the intracluster region of Fornax-like galaxy clusters as depicted in the image? | The HI covering fraction increases with increasing radius. | The HI covering fraction remains constant across different radii. | The HI covering fraction decreases with increasing radius. | The HI covering fraction is highest at the virial radius. | C |
64 | 2,312.15196 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAEXBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2312.15196_figsobwithsignalfit.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What does the peak in the time pdf (EM) curve at approximately 57000 MJD indicate? | A background event | A neutrino flare | A solar flare | A supernova event | B |
65 | 2,402.05991 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQAAtEDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2402.05991_figstackedtransit.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which telescope and filter combination observed the primary transit with the highest normalized flux? | MEarth UT 2009-05-13 (I) | FLWO UT 2009-05-29 (V) | MEarth UT 2009-06-01 (I) | JWST UT 2022-07-21 (MIRILRS) | A |
66 | 2,403.0859 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQAAy8DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.08590_figzdievol.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which star exhibits a progressive increase in the poloidal component, a decrease in field strength, and a reduction in the complexity of the poloidal component, becoming predominantly dipolar? | AD Leo | EV Lac | CN Leo | DS Leo | D |
67 | 2,404.11656 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCALrBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.11656_figpanel2.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which galaxy in the image exhibits the most pronounced anti-correlation track in the bar-hosting region, indicating a significant depletion of gas reservoirs? | NGC~4579 | NGC~4725 | NGC~5236 | None of the above | A |
68 | 2,401.13252 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAK0BAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2401.13252_figcoalescgalaxiesMS.jpg | Astrophysics of Galaxies (astro-ph.GA) | What is the primary characteristic of the coalesced compact group of dwarf galaxies (CGDs) descendants in the stellar mass versus specific star formation rate (sSFR) diagram at $z=0$? | They are predominantly low-mass galaxies with high sSFR. | They are mostly high-mass galaxies with low sSFR. | They are normally star-forming galaxies in the mass range $8 \lesssim \log(M_\ast / \rm M_\odot) \lesssim 10$. | They are mostly quiescent galaxies with very low sSFR. | C |
69 | 2,407.158 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQAA0gDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.15800_figirs13evo.jpg | Astrophysics of Galaxies (astro-ph.GA) | What is the primary reason for the rapid migration of the IRS 13 cluster towards the inner parsec as shown in the simulations? | Gravitational interactions with the Circum Nuclear Disk (CND) | Stellar evolution and mass loss within the cluster | Loss of orbital angular momentum due to interactions with soft binaries | Galactic tidal forces | C |
70 | 2,402.06953 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAPOBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2402.06953_figSFHsAll.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which galaxy in the image shows a significant increase in its star formation rate (SFR) in recent times? | NGC 147 | NGC 185 | NGC 6822 | IC 1613 | C |
71 | 2,404.11523 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJVBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.11523_figCCF.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the primary reason for the strong peak in the cross-correlation function (CCF) between the KPIC data and the BT-Settl model for HD 984 B? | The presence of a strong stellar wind | The high rotational velocity of the companion | The high signal-to-noise ratio of the companion's spectrum | The presence of a strong magnetic field | C |
72 | 2,405.01384 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAO6AxgDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2405.01384_figtimeint.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which of the following heating events, marked in the image, exhibits the highest Doppler shift? | Event (a) | Event (b) | Event (c) | Event (d) | B |
73 | 2,406.18207 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAH8AtwDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.18207_figsedagncomponent.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following best describes the primary contribution of the AGN component to Virgil's spectral energy distribution (SED) as shown in the image? | Contribution at the shortest wavelengths | Contribution at the longest MIRI wavelengths | Contribution at the mid-infrared wavelengths | Contribution at the ultraviolet wavelengths | B |
74 | 2,403.03065 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAOkBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.03065_figcmdralikeeffect.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which of the following is a characteristic feature of the eclipsing binary EBLM J0659-61, as indicated by the sinusoid fit analysis in the image? | A consistent orbital phase across all sectors | A period of $1/2P_{\rm bin}$ with a standard deviation of 0.033 | A significant variation in the normalized flux | A standard deviation of 0.11 in the $1/2P_{\rm bin}$ period | B |
75 | 2,407.09915 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAMwBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.09915_fig5.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | Which of the following statements is true regarding the convergence of the proposal distributions in the parallel tempering chains shown in the image? | The proposal distributions converge after the same number of batches in all chains. | The proposal distributions for all chains stabilize at the same acceptance rate. | The proposal distributions for the chain with β = 1.0 stabilize at an acceptance rate of approximately 0.2. | The proposal distributions for all chains stabilize at the same β value. | C |
76 | 2,402.13913 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAGDBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2402.13913_3panelmm2.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which molecule shows the most uniform distribution in the MM2 region, as indicated by the column density maps? | 13-Methyl Formate | Glycolaldehyde | Acetic Acid | Formic Acid | A |
77 | 2,402.02604 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAMrA/8DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2402.02604_figdscthads.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which type of variable star is characterized by a rapid rise followed by a slow decline in its light curve? | Delta Scuti stars (DSCT) | High-Amplitude Delta Scuti stars (HADS) | RR Lyrae stars | Cepheid stars | B |
78 | 2,403.02457 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAI0BAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.02457_impgoesrecrate.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which of the following best describes the relationship between the impulsiveness index and the peak GOES 1-8 Å soft X-ray flux? | A strong linear correlation | A moderate linear correlation | A weak linear correlation with a moderate monotonic, non-linear relationship | No correlation | C |
79 | 2,405.19388 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAHYBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2405.19388_figTP.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the primary characteristic that distinguishes the δ Scuti pulsators from contaminants in the right panel of the image? | Color index | Log-pulsation period | Absolute G magnitude | Period-luminosity relation | D |
80 | 2,406.1574 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCALaA1YDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.15740_figbeamforming.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What is the primary purpose of the beamforming process illustrated in the image? | To increase the signal-to-noise ratio of individual array elements | To form multiple beams for detecting Fast Radio Bursts (FRBs) | To reduce the computational load of the digital backend | To enhance the spatial resolution of the array | B |
81 | 2,404.09825 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAIiAjwDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.09825_figcontrast.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following is the most likely cause of the density contrast observed in the Pisces overdensity region? | Gravitational influence of the Andromeda Galaxy | Gravitational influence of the Large Magellanic Cloud (LMC) | Gravitational influence of the Sagittarius Dwarf Galaxy | Gravitational influence of the Milky Way's central bulge | B |
82 | 2,403.03743 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAMEAwIDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.03743_figHenucrate.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which network shows the most pronounced and narrow maximum in the nuclear energy generation rate at approximately 0.012 seconds? | \netalpha{} network | \net{} network | \netWN{} network | Both \net{} and \netWN{} networks | C |
83 | 2,401.01043 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCALmBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2401.01043_figLpahvsSFR.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which of the following studies found a similar correlation between PAH luminosity and star formation rate (SFR) as indicated by the blue solid line in the image? | Shipley et al. (2016) | Kovacs et al. (2019) | Our work | AKARI galaxies z<0.5 Kovacs et al. (2019) | B |
84 | 2,403.15118 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAGaAicDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.15118_plotrocTNG.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which method has the highest area under the curve (AUC) in the ROC plot, indicating the best performance in galaxy merger detection? | Method-1 (RF) | Method-2 (Swin) | Method-3 (Zoobot) | Method-4 (CNN1) | C |
85 | 2,404.1231 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAG6AkcDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2404.12310_figperiodvsflarerates.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which of the following statements is true regarding the relationship between the rotation period of stars and their flare rates as depicted in the image? | The flare rate increases with the rotation period for both NUV and optical flares. | The flare rate decreases with the rotation period for both NUV and optical flares. | The flare rate is independent of the rotation period for both NUV and optical flares. | The flare rate is higher for optical flares compared to NUV flares across all rotation periods. | C |
86 | 2,406.13801 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAITBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.13801_figrmsdistribution.jpg | Astrophysics of Galaxies (astro-ph.GA) | What is the primary purpose of the blue outline in the image? | To indicate the rms noise levels | To show the footprint of the Hubble Space Telescope (HST)/Wide Field Camera 3 (WFC3) F160W imaging | To highlight the regions of highest radio frequency emission | To delineate the boundaries of the GOODS-N field | B |
87 | 2,310.17196 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAKtBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2310.17196_XYZRageGBDT.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the primary feature indicated by the blue regions in the lower right panel of the image? | A region of high stellar density | A region of low stellar density | A region of high stellar age | A region of low stellar age | D |
88 | 2,402.12516 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAKGBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2402.12516_figLEDstep.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What phenomenon is illustrated by the sharp increase in pixel value after the 18th measurement in the image? | Photon detection | Charge accumulation | Pixel saturation | Background noise | B |
89 | 2,406.07798 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAOHBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.07798_fig1.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | What is the primary function of the M1 model in the pipeline for detecting large-scale flux ropes (FRs) and their geoeffectiveness? | To derive geoeffective properties from the input data | To perform thresholding on the auto-detected FRs | To classify the input hodograms into FR and NFR categories | To generate the final list of FR boundaries and geoeffectiveness categories | C |
90 | 2,401.17171 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJgBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2401.17171_figlwvsangle.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which molecular line in the Flame Nebula shows a higher ratio of line width to the square root of the circular standard deviation of the magnetic field angle? | CN | HCO+ | CO | CH3OH | B |
91 | 2,403.18608 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJEAloDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.18608_m500planck.jpg | Astrophysics of Galaxies (astro-ph.GA) | What is the primary method used to estimate the masses of the galaxy clusters in the scatter plot? | Optical spectroscopy | X-ray luminosity | Gravitational lensing | Radio observations | B |
92 | 2,401.01091 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJqBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2401.01091_Fig2.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which parameter has the highest feature importance across all three machine learning models? | log(g) | T | Mbol | P | A |
93 | 2,401.03718 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJSAxwDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2401.03718_figfaceons4g.jpg | Astrophysics of Galaxies (astro-ph.GA) | What is the primary purpose of the histogram in the image? | To compare the scale length of the Milky Way with other galaxies | To determine the frequency of galaxies with specific scale lengths | To illustrate the distribution of galaxy types in the sample | To show the relationship between scale length and galaxy mass | A |
94 | 2,406.03553 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAJKBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2406.03553_figmetallicity.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which ion shows the most significant deviation in its ion fraction at higher metallicities (Z = 1.0) compared to the nominal metallicity (Z = 0.3) in the shaded density range? | \CII\ | \CIV\ | \SiIII\ | \SiIV\ | C |
95 | 2,402.10523 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAQABAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2402.10523_figsptcomparison.jpg | Solar and Stellar Astrophysics (astro-ph.SR) | Which star-forming region shows the most significant deviation from the 1:1 relationship in spectral type measurements? | Cha-I | Upper Scorpius | Ophiuchus | None of the above | C |
96 | 2,403.13419 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAIOAisDASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.13419_figrpsimpact.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which galaxy projection experiences the least amount of gas stripping at a low impact parameter ($b_{\rm min}/R_{\rm 200} = 0.04$) according to the graph? | Face-on projection | Edge-on projection | Velocity projection | Equal gas stripping for all projections | B |
97 | 2,402.05925 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAOXBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2402.05925_figsdc1trainingsample.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What is the primary purpose of including the two orange boxes, representing empty training areas, in the image? | To increase the overall number of sources in the training data | To improve the detector's ability to identify sources in low-density regions | To enhance the detector's performance by understanding noise-only regions | To reduce the computational load by focusing on high-density areas only | C |
98 | 2,407.06273 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAP9BAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2407.06273_figdglsingle.jpg | Astrophysics of Galaxies (astro-ph.GA) | Which FIR band exhibits the tightest linear relationship with the DGL + NCOB intensity, as indicated by the smallest scatter in the plots? | 100 μm | 350 μm | 550 μm | 849 μm | C |
99 | 2,405.18899 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCALFA/8DASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2405.18899_figdetperf.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | What is the primary purpose of the orange box in the dark noise map of the NIGHT instrument? | To highlight the region with the highest dark noise | To indicate the area designated for capturing stellar spectra | To show the region with the lowest dark noise | To demarcate the area for sky spectrum transmission | B |
100 | 2,403.00112 | /9j/4AAQSkZJRgABAQAAAQABAAD/2wBDAAgGBgcGBQgHBwcJCQgKDBQNDAsLDBkSEw8UHRofHh0aHBwgJC4nICIsIxwcKDcpLDAxNDQ0Hyc5PTgyPC4zNDL/2wBDAQkJCQwLDBgNDRgyIRwhMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjIyMjL/wAARCAIxBAADASIAAhEBAxEB/8QAHwAAAQUBAQEBAQEAAAAAAAAAAAECAwQFBgcICQoL/8QAtRAAAgEDAwIEAwUFBAQAAAF9AQIDAAQRBRIh... | /root/benchmark/data/2024/2403.00112_curves.jpg | Instrumentation and Methods for Astrophysics (astro-ph.IM) | Which filter in the image has the highest sensitivity to the emission peak of the LED 4000K lamp? | SQM filter | V filter | HPS emission | LED 3000K emission | A |
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