adsabs/AstroCLIMB huggingface dataset:
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: Passbands for individual channels on the detector array (solid/scatter) and the single-pixel box (dashed–dotted) measured using the FLS and the FTS. The variable power of the FLS allows for a larger dynamic range in the out-of-band regions than is possible with the constrained signal-to-noise ratio of the FTS. Additionally, comparing the FLS and FTS passbands together helps to highlight out-of-band features in the FTS spectral response that are due to instrumental systematics. The single-pixel box is plotted for high frequencies where the detector array measurements are limited due to the NDF correction. These single-pixel box measurements highlight the powerful ability of the FLS to probe significantly smaller signal levels than the FTS.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: Left column: holography beam map measurements in the mid-frequency band. Middle column: all beam maps propagated at the secondary illumination of the large aperture telescope. The spilled power to 300 K is calculated by integrating power outside the boundary of the secondary (red line) with respect to the total integrated power of the map. Right column: using Fresnel diffraction, the LATR-Tester measurements are propagated through the large aperture telescope from the near-focal plane to the far field.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: Top: optical response of detectors to a thermal source chopped between 5 mHz and 200 Hz. The response is plotted in arbitrary units and fit to a single pole low-pass filter model to obtain an effective time constant, τ eff for each detector channel. Bottom: spread of the effective time-constant fit parameter measured across the full detector array.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: White noise curves taken over the span of 9 days in a noisy lab environment demonstrate the long-term stability of the readout system. Plotted channels include uncoupled readout resonators along with coupled superconducting and on-transition detectors. We note that the absolute noise levels shown here result from a suboptimal readout configuration and do not represent the expected field performance, which is anticipated to be about 2–3x lower in noise.
Paper: Kinematics of Young Stellar Objects under Various Stellar Feedback
Authors: Longhui Yang, Dejian Liu, Chaojie Hao, Zehao Lin, YingJie Li, Yiwei Dong, Zu-Jia Lu, En-Wei Liang, Y. Xu
Figure caption: Projected distributions of the Class I (green filled circles), Class II (red crosses), and Class III (blue hollow circles) YSOs in Orion A. The background is a false-color image of Orion A observed by Herschel’s Photodetector Array Camera and Spectrometer at 70 μm (blue) and 160 μm (red). The three cyan stars from left to right represent θ 1 Ori C, NU Ori, and 42 Orionis, respectively. The green circles from left to right represent the H II regions M42, M43, and NGC 1977, respectively. The contour represents the boundary of the cloud, which has a velocity range of [−2.6, 18.2] km s−1.
Paper: Kinematics of Young Stellar Objects under Various Stellar Feedback
Authors: Longhui Yang, Dejian Liu, Chaojie Hao, Zehao Lin, YingJie Li, Yiwei Dong, Zu-Jia Lu, En-Wei Liang, Y. Xu
Figure caption: Projected distribution of YSOs in Orion B. The yellow circle represents the H II region driven by IRS 2b. The cyan stars represent IRS 2b and the massive O-type star ζ Ori, from north to south. L1630N, from top to bottom, comprises NGC 2071 and NGC 2068. The contours represent the velocity channel of [−2.6, 18.2] km s−1. The other features are the same in Figure 1.
Paper: Kinematics of Young Stellar Objects under Various Stellar Feedback
Authors: Longhui Yang, Dejian Liu, Chaojie Hao, Zehao Lin, YingJie Li, Yiwei Dong, Zu-Jia Lu, En-Wei Liang, Y. Xu
Figure caption: Projected distribution of YSOs in Taurus. The background is a false-color image of Taurus (red: Planck at 353 GHz; green: IRAS at 100 μm). The contours represent the velocity channel of [−2.6,15.6] km s−1. The other features are the same as in Figure 1.
Paper: Kinematics of Young Stellar Objects under Various Stellar Feedback
Authors: Longhui Yang, Dejian Liu, Chaojie Hao, Zehao Lin, YingJie Li, Yiwei Dong, Zu-Jia Lu, En-Wei Liang, Y. Xu
Figure caption: Projected distribution of YSOs in Perseus. The background is a false-color image of Perseus observed by Herschel/SPIRE at 250 μm (blue), 350 μm (green), and 500 μm (red). The contours represent the velocity channel of [−5.2, 15.6] km s−1. The other features are the same as in Figure 1.
Paper: Kinematics of Young Stellar Objects under Various Stellar Feedback
Authors: Longhui Yang, Dejian Liu, Chaojie Hao, Zehao Lin, YingJie Li, Yiwei Dong, Zu-Jia Lu, En-Wei Liang, Y. Xu
Figure caption: PV diagram for the Class II (red crosses) and Class III (blue circles) YSOs in Orion A. The average velocity per region for all YSOs, as well as for the Class II and III YSOs individually are shown with black squares, red crosses, and blue circles, respectively, with the error bars representing the velocity dispersion per region.
Paper: Kinematics of Young Stellar Objects under Various Stellar Feedback
Authors: Longhui Yang, Dejian Liu, Chaojie Hao, Zehao Lin, YingJie Li, Yiwei Dong, Zu-Jia Lu, En-Wei Liang, Y. Xu
Figure caption: Distribution of the proper motions of the YSOs in the subregions of Orion A, where the crosses and circles represent Class II and III YSOs, respectively.
Paper: Kinematics of Young Stellar Objects under Various Stellar Feedback
Authors: Longhui Yang, Dejian Liu, Chaojie Hao, Zehao Lin, YingJie Li, Yiwei Dong, Zu-Jia Lu, En-Wei Liang, Y. Xu
Figure caption: Proper-motion distribution of YSOs in Perseus, where the crosses represent Class II YSOs and the circles represent Class III YSOs.
Paper: Kinematics of Young Stellar Objects under Various Stellar Feedback
Authors: Longhui Yang, Dejian Liu, Chaojie Hao, Zehao Lin, YingJie Li, Yiwei Dong, Zu-Jia Lu, En-Wei Liang, Y. Xu
Figure caption: Proper-motion distribution of YSOs in Orion B, where the crosses represent Class II YSOs and the circles represent Class III YSOs.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Gallery of continuum images (top row) and RRL integrated-intensity maps (bottom row) for the SMA sample. Color scale shows the 230 GHz continuum and gray contours show the 345 GHz continuum. The synthesized beam and a scale bar indicating 5000 au is shown in the lower-left and lower-right corner, respectively, of each panel.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: SMA spectra from ≈209 to 233 GHz of our sample extracted within one beam at the continuum peak of each source. There are small gaps in spectral coverage at the edges of each sideband. Sources are ordered by evolutionary stage from top (most evolved) to bottom (youngest). A few selected lines are labeled.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: SMA spectra from ≈333 to 357 GHz of our sample. Otherwise, as in Figure 2.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Peak positions for different molecular families (columns) are shown for each source (rows). Individual points are the median line peak positions for all detected molecules and the contours show the kernel density estimation. The 1.3 mm continuum is shown in the color scale. Continuum peaks are shown as gray triangles in all panels. In G28, the positions of HMC1 and HMC2 are denoted by white squares. In G35, the left-hand triangle corresponds to G35-East and the right-hand triangle marks G35-West. Only a few molecules peak far outside the continuum and are not shown here (but see Appendix C for a full gallery of zeroth-moment maps for each species).
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Zeroth-moment maps of representative lines demonstrating the multiple emission components that comprise G28. Salient emission features are labeled with arrows. The upper state energy of each transition is labeled in the upper right. The continuum peak is shown as a pink triangle and the synthesized beam is shown in the lower left of each panel. The boxed regions in the continuum image show zoom ins with corresponding scale bars denoting 20,000 au, 8000 au, or 4000 au depending on the spatial scale, respectively, in each panel. The outflow direction, as traced by SiO emission (P. Gorai et al. 2024), is marked in the continuum image.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Zeroth-moment maps of representative lines in G35. The outflow direction, as traced by high-velocity 12CO emission (C.-P. Zhang et al. 2014), is marked in the continuum image. Otherwise, as in Figure 6.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Gallery of molecular and RRL detections in the SMA sample which indicate if the species is detected in emission (solid box) or in both emission and absorption (diagonal lines). No molecules were detected only in absorption. Molecules are divided and colored as O-bearing (green), S-bearing (orange), N-bearing (blue), and hydrocarbons (gray). The detected RRLs are colored in pink. All listed transitions are in the v = 0 state, unless otherwise noted. Transitions with v = 1, 2, etc., are shown immediately to the right of the molecule name.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Violin plot of detected transitions as a function of Eu for G28, G20, G35, and W33. The width of each violin shows a kernel density estimation of the underlying Eu distribution for that molecule. Line detections are compiled from beam-averaged spectra at the continuum peaks of all sources, except for W33, where they represent the set of unique detections at both the molecule-rich and RRL emission-peak regions (see Appendix B). Molecules are colored as in Figure 4. The detected HCN v2 = 1 line, which has an Eu = 1067 K, is shown as an upward-facing arrow for visual clarity.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Derived rotational temperatures of O-bearing (green) and N-bearing (blue) species in our sample. Molecules containing both N and O, i.e., HNCO and NH2CHO, are excluded.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Zeroth-moment maps of representative lines in G20. The outflow direction, as traced by SiO emission (J.-L. Xu & J.-J. Wang 2013), is marked in the continuum image. Otherwise, as in Figure 6.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Derived molecular column densities for selected positions in G28 (left), G20 (middle), and G35 (right). Molecules are colored as in Figure 4 and labels for the vibrational states correspond to the molecule listed immediately above. Due to the wide range in Ncol shown, markers are larger than the uncertainties in most cases.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Column density ratios of select molecules (columns). Shaded bands correspond to the typical 1σ range of abundance ratios observed in star-forming regions for O-, N-, and S-bearing species (rows). Ratios from P. Nazari et al. (2022) and Y. Chen et al. (2023) include a sample of both high- and low-mass protostars, while J. Li et al. (2015) and A. Coletta et al. (2020) were derived from only high-mass sources. The CS column densities are computed from 13CS, assuming the relevant isotopic elemental ratios (Y. T. Yan et al. 2023). The ratios marked by a † symbol indicate those derived using likely optically thick SO. Bolometric luminosity uncertainties are on the order of ≈30%–50% (D. O. S. Wood & E. Churchwell 1989; Y. Liu et al. 2019b; C.-Y. Law et al. 2022). Molecules are colored as in Figure 4.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Zeroth-moment maps of representative lines of the spatially extended molecules in G28. The upper state energy of each transition is labeled in the upper right. The synthesized beam and a scale bar indicating 10,000 au are shown in the lower-left and lower-right corner, respectively, of each panel. The outflow direction, as traced by SiO emission (P. Gorai et al. 2024), is marked in the continuum image.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: 230 GHz continuum image and gallery of peak line intensity maps of W33 in an extended field of view. The location of the cores (W33 Main-Central, W33 Main-North, W33 Main-West, W33 Main-South) initially identified in K. Immer et al. (2014) are labeled in the top-left panel.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Schematic of expected gas-phase C/O ratios (top) and projected radial distance of molecular line peaks measured in G35 (bottom). Molecules containing oxygen are shown in green and those without are colored in gray.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Zeroth-moment maps of representative lines of the spatially compact molecules in G28. The synthesized beam and a scale bar indicating 4000 au are shown in the lower-left and lower-right corner, respectively, of each panel.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Gallery of spatially extended lines in G35. The outflow direction, as traced by high-velocity 12CO emission (C.-P. Zhang et al. 2014), is marked in the continuum image. Otherwise, as in Figure 16.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Gallery of spatially extended lines in G20. The outflow direction, as traced by SiO emission (J.-L. Xu & J.-J. Wang 2013), is marked in the continuum image. Otherwise, as in Figure 16.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Gallery of spatially compact lines in G20. Otherwise, as in Figure 17.
Paper: A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Charles J. Law, Qizhou Zhang, Arielle C. Frommer, Karin I. Öberg, Roberto Galván-Madrid, Eric Keto, Hauyu Baobab Liu, Paul T. P. Ho, Andrés F. Izquierdo, L. Ilsedore Cleeves
Figure caption: Gallery of spatially compact lines in G35. Otherwise, as in Figure 17.
Paper: Mass, Luminosity, and Stellar Age of Early-type Stars from the LAMOST Survey
Authors: Qida Li, Jianping Xiong, Jiao Li, Yanjun Guo, Zhanwen Han, Xuefei Chen, Chao Liu
Figure caption: Comparison with the literature. The x-axis represents the literature values, and the y-axis represents the predictions of our model. The left panel shows the M comparison with W. Sun et al. (2021), while the middle and right panels show the t and M i comparisons, respectively, with G. Kordopatis et al. (2023). The median relative error is marked on the top left of each panel.