adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA/ACA CO Survey of the IC 1459 and NGC 4636 Groups: Environmental Effects on the Molecular Gas of Group Galaxies
Authors: Bumhyun Lee, Jing Wang, Aeree Chung, Luis C. Ho, Ran Wang, Tomonari Michiyama, Juan Molina, Yongjung Kim, Li Shao, Virginia Kilborn, Shun Wang, Xuchen Lin, Dawoon E. Kim, Barbara Catinella, Luca Cortese, Nathan Deg, Helga Denes, Ahmed Elagali, Bi-Qing For, Dane Kleiner, Bärbel S. Koribalski, Karen Lee-Waddell, Jonghwan Rhee, Kristine Spekkens, Tobias Westmeier, O. Ivy Wong, Frank Bigiel, Albert Bosma, Benne W. Holwerda, Jan M. van der Hulst, Sambit Roychowdhury, Lourdes Verdes-Montenegro, Martin A. Zwaan
Figure caption: IC 5270.
Paper: ALMA/ACA CO Survey of the IC 1459 and NGC 4636 Groups: Environmental Effects on the Molecular Gas of Group Galaxies
Authors: Bumhyun Lee, Jing Wang, Aeree Chung, Luis C. Ho, Ran Wang, Tomonari Michiyama, Juan Molina, Yongjung Kim, Li Shao, Virginia Kilborn, Shun Wang, Xuchen Lin, Dawoon E. Kim, Barbara Catinella, Luca Cortese, Nathan Deg, Helga Denes, Ahmed Elagali, Bi-Qing For, Dane Kleiner, Bärbel S. Koribalski, Karen Lee-Waddell, Jonghwan Rhee, Kristine Spekkens, Tobias Westmeier, O. Ivy Wong, Frank Bigiel, Albert Bosma, Benne W. Holwerda, Jan M. van der Hulst, Sambit Roychowdhury, Lourdes Verdes-Montenegro, Martin A. Zwaan
Figure caption: IC 5269B.
Paper: Simulating the Legacy Survey of Space and Time Stellar Content with TRILEGAL 
Authors: Piero Dal Tio, Giada Pastorelli, Alessandro Mazzi, Michele Trabucchi, Guglielmo Costa, Alice Jacques, Adriano Pieres, Léo Girardi, Yang Chen, Knut A. G. Olsen, Mario Juric, Željko Ivezić, Peter Yoachim, William I. Clarkson, Paola Marigo, Thaise S. Rodrigues, Simone Zaggia, Mauro Barbieri, Yazan Momany, Alessandro Bressan, Robert Nikutta, Luiz Nicolaci da Costa
Figure caption: Top panel: simulated stellar density for the stars with 17 < r < 20, for the Galactic plane and bulge areas. The squares are areas for which we are checking the star counts with DECaPS data (see Figures 10 and 11 below). Bottom panel: extinction A  V  derived from Planck maps. All regions with A  V  > 10 mag appear in dark red. See Section 4.2.
Paper: Simulating the Legacy Survey of Space and Time Stellar Content with TRILEGAL 
Authors: Piero Dal Tio, Giada Pastorelli, Alessandro Mazzi, Michele Trabucchi, Guglielmo Costa, Alice Jacques, Adriano Pieres, Léo Girardi, Yang Chen, Knut A. G. Olsen, Mario Juric, Željko Ivezić, Peter Yoachim, William I. Clarkson, Paola Marigo, Thaise S. Rodrigues, Simone Zaggia, Mauro Barbieri, Yazan Momany, Alessandro Bressan, Robert Nikutta, Luiz Nicolaci da Costa
Figure caption: Comparison between the star counts in the present catalog (TRILEGAL; orange lines) with the previous galfast catalog (dashed–dotted blue lines), and the real star counts from DECaPS (dashed green lines), for the low-b areas depicted in Figure 9 and for all grizy filters (from top to bottom). All panels cover a similar range in magnitude with the exception of VVV372 and baade, which are limited at the faint end where star counts start to decrease because of crowding. The number counts are computed in magnitude bins 0.1 mag wide. See Section 4.2.
Paper: Simulating the Legacy Survey of Space and Time Stellar Content with TRILEGAL 
Authors: Piero Dal Tio, Giada Pastorelli, Alessandro Mazzi, Michele Trabucchi, Guglielmo Costa, Alice Jacques, Adriano Pieres, Léo Girardi, Yang Chen, Knut A. G. Olsen, Mario Juric, Željko Ivezić, Peter Yoachim, William I. Clarkson, Paola Marigo, Thaise S. Rodrigues, Simone Zaggia, Mauro Barbieri, Yazan Momany, Alessandro Bressan, Robert Nikutta, Luiz Nicolaci da Costa
Figure caption: Ratio between star counts (in the sense S = (simulated/observed) as a function of the Galactic longitude l (top panel) and mean extinction A  V  (bottom panel). Circles show the ratio TRILEGAL/DECaPS while triangles show TRILEGAL/VVV. Filters are indicated in the legend. Note that the two clouds of points with (simulated/observed) ≳ 0.8 are identified with the outlier fields at longitude ∣l∣ > 90°. See Section 4.2.
Paper: Simulating the Legacy Survey of Space and Time Stellar Content with TRILEGAL 
Authors: Piero Dal Tio, Giada Pastorelli, Alessandro Mazzi, Michele Trabucchi, Guglielmo Costa, Alice Jacques, Adriano Pieres, Léo Girardi, Yang Chen, Knut A. G. Olsen, Mario Juric, Željko Ivezić, Peter Yoachim, William I. Clarkson, Paola Marigo, Thaise S. Rodrigues, Simone Zaggia, Mauro Barbieri, Yazan Momany, Alessandro Bressan, Robert Nikutta, Luiz Nicolaci da Costa
Figure caption: Comparison between TRILEGAL and VVV CMDs (or Hess diagrams), for the two areas in Figure 9 covered by the VVV survey. See Section 4.2. It is worth noting that the same main features appear in both the model and in the observed CMDs, although not exactly at the same colors and magnitudes. Much of these differences might be associated to the imperfect treatment of extinction in the models (see text).
Paper: Simulating the Legacy Survey of Space and Time Stellar Content with TRILEGAL 
Authors: Piero Dal Tio, Giada Pastorelli, Alessandro Mazzi, Michele Trabucchi, Guglielmo Costa, Alice Jacques, Adriano Pieres, Léo Girardi, Yang Chen, Knut A. G. Olsen, Mario Juric, Željko Ivezić, Peter Yoachim, William I. Clarkson, Paola Marigo, Thaise S. Rodrigues, Simone Zaggia, Mauro Barbieri, Yazan Momany, Alessandro Bressan, Robert Nikutta, Luiz Nicolaci da Costa
Figure caption: Comparison between the star counts in the present catalog (TRILEGAL, orange lines) with the real star counts from VVV (green lines), for the VVV372 and baade fields, and for all ZYJHK s filters. The range in magnitude is limited at the faint end at the point where star counts start to decrease because of crowding. The number counts are computed in magnitude bins 0.1 mag wide. See Section 4.2.
Paper: Simulating the Legacy Survey of Space and Time Stellar Content with TRILEGAL 
Authors: Piero Dal Tio, Giada Pastorelli, Alessandro Mazzi, Michele Trabucchi, Guglielmo Costa, Alice Jacques, Adriano Pieres, Léo Girardi, Yang Chen, Knut A. G. Olsen, Mario Juric, Željko Ivezić, Peter Yoachim, William I. Clarkson, Paola Marigo, Thaise S. Rodrigues, Simone Zaggia, Mauro Barbieri, Yazan Momany, Alessandro Bressan, Robert Nikutta, Luiz Nicolaci da Costa
Figure caption: Comparison between TRILEGAL and DECaPS CMDs (or Hess diagrams), for two of the areas drawn in Figure 9, namely, baade (which corresponds to Baade’s Window; left panels) and disk7 (right panels). Additional plots are presented in Appendix C. See Section 4.2.
Paper: Simulating the Legacy Survey of Space and Time Stellar Content with TRILEGAL 
Authors: Piero Dal Tio, Giada Pastorelli, Alessandro Mazzi, Michele Trabucchi, Guglielmo Costa, Alice Jacques, Adriano Pieres, Léo Girardi, Yang Chen, Knut A. G. Olsen, Mario Juric, Željko Ivezić, Peter Yoachim, William I. Clarkson, Paola Marigo, Thaise S. Rodrigues, Simone Zaggia, Mauro Barbieri, Yazan Momany, Alessandro Bressan, Robert Nikutta, Luiz Nicolaci da Costa
Figure caption: CCD for all simulated single stars in the n side = 64 pixels whose centers lie within 5° of the South Galactic Pole (SGP). Stars are color coded as in Figure 5.
Paper: Simulating the Legacy Survey of Space and Time Stellar Content with TRILEGAL 
Authors: Piero Dal Tio, Giada Pastorelli, Alessandro Mazzi, Michele Trabucchi, Guglielmo Costa, Alice Jacques, Adriano Pieres, Léo Girardi, Yang Chen, Knut A. G. Olsen, Mario Juric, Željko Ivezić, Peter Yoachim, William I. Clarkson, Paola Marigo, Thaise S. Rodrigues, Simone Zaggia, Mauro Barbieri, Yazan Momany, Alessandro Bressan, Robert Nikutta, Luiz Nicolaci da Costa
Figure caption: CMD for all simulated binaries in the n side = 64 pixels whose centers lie within 5° of the South Galactic Pole (SGP). Their distributions of galactic components, distances, and metallicities are similar to those in Figure 5.
Paper: Simulating the Legacy Survey of Space and Time Stellar Content with TRILEGAL 
Authors: Piero Dal Tio, Giada Pastorelli, Alessandro Mazzi, Michele Trabucchi, Guglielmo Costa, Alice Jacques, Adriano Pieres, Léo Girardi, Yang Chen, Knut A. G. Olsen, Mario Juric, Željko Ivezić, Peter Yoachim, William I. Clarkson, Paola Marigo, Thaise S. Rodrigues, Simone Zaggia, Mauro Barbieri, Yazan Momany, Alessandro Bressan, Robert Nikutta, Luiz Nicolaci da Costa
Figure caption: CCD for all simulated binary stars in the n side = 64 pixels whose centers lie within 5° of the South Galactic Pole (SGP).
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: A neuron of the ANN.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: An example of a mixture model.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: Left: Mean Lyα luminosity 〈L  α (M UV)〉 within the 2″ aperture of the REW > 0 Å population as a function of the UV magnitude M UV, as presented in Equation (B8). The gray dotted lines denote the turning points of a 1 as expressed in Equation (B3). The green dashed line denotes the expected Lyα luminosity for the SFR associated with the UV luminosity. Right: UV LF of the REW < 0 Å population ﹩{{\rm{\Phi }}}_{\mathrm{UV}}^{a}﹩, the REW > 0 Å population ﹩{{\rm{\Phi }}}_{\mathrm{UV}}^{e}﹩, and the entire population Φ UV as a function of M UV, as presented in Equations (B6) and (B7). We take the Reddy & Steidel (2009) UV LF as an example. The gray dotted line denotes one of the turning points of a 1 (Equation (B3)), where a 1 = 0 and the REW remains larger than 0 as M UV increases. That is, we assume that there is no REW < 0 Å population over this M UV range, which will lead to an underestimation of the total Lyα luminosity.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: Modified monopole, quadrupole, and hexadecapole of the Lyα forest–Lyα emission cross-correlation as a function of the Lyα forest–Lyα emission pixel pair separation. The data points are the measurements, and the solid curves are the predictions using parameters in literature to describe the Lyα forest and parameters 〈μ  α 〉 and β  α  derived from fits to the quasar–Lyα emission cross-correlation under the galaxy-dominated scenario. The various solid curves are the predicted modified multipoles from randomly drawing 〈μ  α 〉 and β  α  from their posterior probability distribution, with the thickest ones from adopting the best-fit parameters.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: A test for the robustness of our fiducial sample selection, by performing joint fits to the multipoles and SB profiles of quasar–Lyα emission cross-correlation after different sample selections. The model parameters are the same as those in Figure 7. Fiber Cut 5 refers to the sample where any LRG fiber with Δfiber < 5 from a quasar fiber is excluded, which is the fiducial sample for our measurements; Fiber Cut 8 and Fiber Cut 10 refer to Δfiber < 8 and Δfiber < 10, respectively. Pair Cut 5 refers to the sample in which a quasar–LRG spectrum pixel pair is excluded if it satisfies Δfiber < 5, i.e., the method adopted in Croft et al. (2018).
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: The probability distribution of L  q,α  and β  α  from the joint fit to the multipoles and SB profiles from the measured quasar–Lyα emission cross-correlation. The mean quasar Lyα luminosity L  q,α  is in units of ergs per second. Note that there are actually three parameters, L  q,α , β  α , and SB0, in the model, but here we focus on the constraints on L  q,α  and β  α . See the text for details.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: Lyα forest–Lyα emission pixel–pixel correlation as a function of observed wavelength separations Δλ obs and transverse separations at a redshift of 2.41. Different-half-plate pairs refers to the sample in which the selected pixel pairs reside on different half-plates; Same-half-plate pairs refers to the sample in which all pairs are on the same half-plates. All pairs refers to the sample without preference for the plates/fibers. The bottom panels show the correlations averaged within 2 Å at Δλ obs ∼ 0.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: Lyα luminosity density computed in our model by integrating different observed UV LFs. Different colors denote the inner and outer Lyα parts, as described in Table 2 in detail. The model Lyα luminosity densities are compared with that inferred from our quasar–Lyα emission cross-correlation measurements, 6.6 × 1040 erg s−1 cMpc−3 (solid) with 1σ error bars (dashed) of ±3.2 × 1040 erg s−1 cMpc−3.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G000.31−00.20. Plotted are position offsets for three maser spots at V LSR = 15.5 (red), 16.6 (green), and 18.4 (blue) calibrated relative to the background sources J1748−2907 and J1752−3001. Left panel:  Positions on the sky with the first and last epochs labeled. Expected positions from the parallax and proper-motion fit are indicated (crosses).  Middle panel:  east (solid line) and north (dashed line) position offsets and best-fit parallax and proper motions vs. time. Right panel:  same as the middle panel but with the best-fit proper motions removed to display only the parallax sinusoids.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G010.32−00.15. Plotted are position offsets for four maser spot at V LSR = 4.1 (red triangles), 4.5 (green triangles), 5.5 (blue triangles), 6.3 (cyan triangles), 6.6 (yellow triangles), 9.5 (magenta triangles), 9.8 (red squares), 10.2 (green squares), 10.5 (blue squares), 12.7(cyan squares), 13.1 (yellow squares), and 13.4 (magenta squares) km s−1 calibrated relative to the background sources J1808−1822, J1821−2110, and J1751−1950, respectively. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G010.34−00.14. Plotted are position offsets for four maser spot at V LSR = 4.9 (red), 10.3 (green), 10.6 (blue), 12.8 (cyan), and 16.0 (yellow) km s−1 calibrated relative to the background sources J1808−1822, J1819−2036, and J1821−2110, respectively. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G009.21−00.20. Plotted are position offsets for four maser spots at V LSR = 40.5 (red), 41.8 (green), 45.5 (blue), and 45.7 (cyan) km s−1 calibrated relative to the background sources J1755−2232, J1808−1822, and J1819−2036. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G011.10−00.11. Plotted are position offsets for three maser spot at V LSR = 29.8 (red), 30.2 (green), and 32.0 (blue) km s−1 calibrated relative to the background sources J1751−1950 and J1821−2110, respectively. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G030.19−00.16. Plotted are position offsets for three maser spots at V LSR = 104.8 (red), 108.4 (green), and 110.2 (magenta) km s−1, and three other maser spots (blue, cyan, and yellow) at 109.4 km s−1 calibrated relative to the background sources J1834−0301, J1846−0003, J1853−0048, and J1857−0048. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G028.39+00.08 with water masers. Plotted are position offsets for three maser spots at V LSR = 77.5 (red), 77.6 (green), and 78.7 (blue) km s−1 calibrated relative to the background sources J1833−0323 (triangles), J1834−0301 (squares), and J1846−0651 (pentagons). A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G028.30−00.38. Plotted are position offsets for five maser spots at V LSR = 81.3 (red), 82.0 (green), 82.4 (blue), 92.4 (cyan), and 93.9 (yellow) km s−1 calibrated relative to the background sources J1833−0323, J1834−0301, and J1846−0651. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G028.39+00.08 with methanol masers. Plotted are position offsets for three maser spots at V LSR = 69.1 (red), 71.3 (green), and 81.7 (blue) km s−1 calibrated relative to the background sources J1833−0323, J1834−0301, and J1846−0651. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G028.83−00.25. Plotted are position offsets for two maser spots at V LSR = 90.8 (red) and 81.1 (green) km s−1 calibrated relative to the background sources J1833−0323, J1834−0301, J1846−0651, and J1853−0048. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G022.03+00.22. Plotted are position offsets for four maser spots at V LSR = 49.5 (red), 51.7 (green), 53.3 (blue), and 54.4 (cyan) km s−1 calibrated relative to the background source J1825−0737. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G024.63−00.32. Plotted are position offsets for two maser spots at V LSR = 35.7 (red) and 48.1 (green) km s−1 calibrated relative to the background sources J1825−0737 and J1846−0651. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G019.36−00.03. Plotted are position offsets for three maser spots at V LSR = 25.4 (red), 27.2 (green), and 28.6 (blue) km s−1 calibrated relative to the background source J1821−1224. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G018.87+00.05. Plotted are position offsets for one maser spot at V LSR = 38.3 (red) km s−1 calibrated relative to the background source J1821−1224. A description of the three panels is given in the caption for Figure 1.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Peculiar (noncircular) motions of massive young stars in the Milky Way, updated from Figure 6 of Reid et al. (2019). The Galactic center (red asterisk) is at (0,0) and the Sun (red Sun symbol) is at (0,8.15) kpc. A schematic “long” bar from Wegg et al. (2015) is indicated by the shaded ellipse. Filled and open circles indicate sources with peculiar motion uncertainties less than 25 and 50 km s−1, and sources with larger uncertainties are not plotted. Sources in the Scutum–Centaurus arm are indicated by blue symbols; other arms shown are the Norma arm (red), Sagittarius–Carina arm (magenta), Local Arm (cyan), and Perseus arm (black). White symbols are either interarm or unassigned sources. As noted by Immer et al. (2019) there are large peculiar motions toward the Galactic center for many sources in the Scutum–Centaurus arm, as well as a smaller number in the Norma and Sagittarius–Carina arms, near the end of the Galactic bar.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Histograms binned in Galactocentric azimuth of components of the peculiar motions in the Galactic plane for sources in the Scutum–Centaurus arm. Variance-weighted values in each bin are plotted against Galactocentric azimuth. Bins are 10° wide and only bins containing two or more points are plotted. Left panel:  U-component of peculiar motion (positive toward the Galactic center). Right panel:  V-component of peculiar motion (positive in the direction of Galactic rotation). Note that the large positive 〈U〉 values are confined to azimuths between 15° and 35° and are not evident throughout the arm, whereas the magnitudes of the 〈V〉 values are considerably smaller between those azimuths.
Paper: Accurate Distances of Massive Young Stars in the Scutum Spiral Arm
Authors: J. J. Li, K. Immer, M. J. Reid, A. Sanna, K. L. J. Rygl, Y. Xu, B. Zhang, A. Brunthaler, K. M. Menten
Figure caption: Parallax and proper-motion data and fits for G033.39+00.00. Plotted are position offsets for three maser spots at V LSR = 98.2 (red), 105.4 (green), and 106.1 (blue) km s−1 calibrated relative to the background sources J1846−0003, J1848+0138, and J1853−0048. A description of the three panels is given in the caption for Figure 1.