adsabs/AstroCLIMB huggingface dataset:
Paper: Machine-learning Inferences of the Interior Structure of Rocky Exoplanets from Bulk Observational Constraints
Authors: Yong Zhao, Dongdong Ni, Zibo Liu
Figure caption: Dependence of the NLL loss on the size of the training data set for all three MDNs: model A trained on the inputs of mass M, radius R, and bulk molar ratios Fe/Mg and Mg/Si; model B trained on the inputs of mass M, radius R, and tidal Love number k 2; and model C trained on the inputs of mass M, radius R, bulk molar ratios Fe/(Mg + Si), and tidal Love number k 2. Random seeds are varied for each training size to sample different sets of training data.
Paper: Machine-learning Inferences of the Interior Structure of Rocky Exoplanets from Bulk Observational Constraints
Authors: Yong Zhao, Dongdong Ni, Zibo Liu
Figure caption: Predicted distributions of six output variables from the MDN trained on the [M, R, Fe/(Mg + Si)] inputs vs. the actual values obtained from the interior models for the testing data set. The three panels in the upper half show the radial fractions of the water–ice layer, mantle, and core (denoted by WRF, MRF, and CRF), respectively. The three panels in the lower half show the CMF as well as pressure and temperature at the CMB, respectively. Blue dashed diagonal lines denote perfect performance of the MDN. The rightmost bar indicates the relation between color scale and local probability density (the color scale is dark at the maximum).
Paper: Machine-learning Inferences of the Interior Structure of Rocky Exoplanets from Bulk Observational Constraints
Authors: Yong Zhao, Dongdong Ni, Zibo Liu
Figure caption: Comparison of the MDN predictions with the results from the Monte Carlo sampling for the interior of Kepler-78 b: (a) the MDN predictions using the [M, R, Fe/(Mg + Si)] inputs and the Monte Carlo results confined by σ 1 ≤ 2%, and (b) the MDN predictions using the [M, R, Fe/(Mg + Si), k 2] inputs and the Monte Carlo results confined by σ 2 ≤ 2%. Based on the iron enrichment suggested by Adibekyan et al. (2021), the MDN predictions are shown by blue solid lines and the Monte Carlo results are indicated by green shaded areas. For comparison, the MDN predictions are also made using the stellar abundance ratios as proxies for the rocky planet compositions (red dotted lines).
Paper: Machine-learning Inferences of the Interior Structure of Rocky Exoplanets from Bulk Observational Constraints
Authors: Yong Zhao, Dongdong Ni, Zibo Liu
Figure caption: Comparison of the MDN predictions with the results from the Monte Carlo sampling for the interior of the Earth: (a) the MDN predictions using the [M, R, Fe/(Mg + Si)] inputs and the Monte Carlo sample confined by σ 1 ≤ 2% and (b) the MDN predictions using the [M, R, Fe/(Mg + Si), k 2] inputs and the Monte Carlo sampling confined by σ 2 ≤ 2%. Blue solid lines denote the MDN predictions and green shade areas denote the Monte Carlo results.
Paper: Machine-learning Inferences of the Interior Structure of Rocky Exoplanets from Bulk Observational Constraints
Authors: Yong Zhao, Dongdong Ni, Zibo Liu
Figure caption: Same as in Figure 5, but for the predicted distributions from the MDN trained on the [M, R, Fe/(Mg + Si), k 2] inputs.
Paper: Machine-learning Inferences of the Interior Structure of Rocky Exoplanets from Bulk Observational Constraints
Authors: Yong Zhao, Dongdong Ni, Zibo Liu
Figure caption: DNN model trained on inputs of mass M, radius R, and bulk molar ratios Fe/Mg, Mg/Si: (a) MSE loss of the DNN for both the training and validation data sets and (b) DNN predictions of the static Love numbers k 2 vs. the k 2 values obtained by solving the interior models.
Paper: Machine-learning Inferences of the Interior Structure of Rocky Exoplanets from Bulk Observational Constraints
Authors: Yong Zhao, Dongdong Ni, Zibo Liu
Figure caption: Learning curves of the three MDN models: (a) MDN (A) model trained on the inputs of mass M, radius R, and bulk molar ratio Fe/(Mg + Si); (b) MDN (B) model trained on the inputs of mass M, radius R, and tidal Love number k 2; and (c) MDN (C) model trained on the inputs of mass M, radius R, bulk molar ratio Fe/(Mg + Si), and tidal Love number k 2.
Paper: Machine-learning Inferences of the Interior Structure of Rocky Exoplanets from Bulk Observational Constraints
Authors: Yong Zhao, Dongdong Ni, Zibo Liu
Figure caption: Same as in Figure 5, but for the predicted distributions from the MDN trained on the [M, R, k 2] inputs.
Paper: Machine-learning Inferences of the Interior Structure of Rocky Exoplanets from Bulk Observational Constraints
Authors: Yong Zhao, Dongdong Ni, Zibo Liu
Figure caption: Same as in Figure 9, but for the interior of HD 3167 b.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Example exposure map and science image (0.3–10 keV) of a DGPS mosaic. The mosaic is centered at l, b = 333.°87, 0.°026. White circles represent the locations of sources detected in this image. The bright source to the right of the image is MAXI J1651-501, a Type-I X-ray burster uncovered through DGPS observations (Gorgone et al. 2019). A weak stray light pattern (concentric bands) is visible on the left end of the mosaic. The images have been rebinned (7.″07 pix−1) and smoothed with a Gaussian kernel (with FWHM of 3 pixels) for display purposes.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: LogN − ﹩\mathrm{log}S﹩ plot for the full Swift DGPS (0.3–10 keV) catalog. The best-fit line is displayed in red corresponding to N( > S) ∝ S −0.78. The green solid line displays the ﹩\mathrm{log}N﹩ − ﹩\mathrm{log}S﹩ for non-LSXPS sources. The dotted and dashed lines correspond to the 50% and 90% completeness flux of the DGPS, respectively. The blue dotted line is an estimate of the extragalactic source population (Ueda et al. 1999).
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Top: histogram of the 90% X-ray position error for sources in the DGPS catalog. Bottom: radial separation R divided by the 68% error of the DGPS sources and the 68% error of other X-ray source error added in quadrature. The radial separation is from the DGPS source to the X-ray counterpart centroid from 4XMM, 2CSC, and 1SWXRT. The dashed red line shows the expected Rayleigh distribution with σ = 1.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Histogram of average flux values for DGPS sources (gray), the non-LSXPS sources (blue), and known classified sources (purple), including IP CVs, LMXBs, HMXBs, and magnetars. The dotted and dashed lines correspond to the 50% and 90% completeness flux of the DGPS, respectively (see Section 5.1).
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Breakdown of the source type for the 73 classified sources in the full DGPS catalog.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: The ratio of the peak-to-mean X-ray flux R flux vs. the ratio of the mean X-ray flux F  X  and the X-ray flux error ﹩{\sigma }_{{F}_{X}}﹩. The points are colored by the log of the 0.3–10 keV X-ray flux in erg cm−2 s−1. The black dashed line indicates a region of parameter space where sources are likely flaring or highly variable.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Examples of variable sources identified in DGPS observations: IGR J18219-1347 is a BeXRB (O’Connor et al. 2022), XTE J1810-197 is a magnetar candidate (Markwardt et al. 2003; Israel et al. 2004), OAO 1657-41 is an HMXB (Polidan et al. 1978; Chakrabarty et al. 1993), and AX J165420-43337 (also known as 1RXS J165424.6-433758) is a polar CV (O’Connor et al. 2023a).
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Cumulative distribution of the Pearson’s χ 2 variability test for all DGPS sources. The dashed line represents a threshold of ﹩{P}_{\chi ,\mathrm{const}}=0.05﹩, below which a source is considered variable. Approximately 50% of sources lie below this threshold.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Breakdown of the 928 X-ray sources (802 LSXPS + 126 non-LSXPS) in the full DGPS source catalog.
Paper: Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 with FAST and Arecibo
Authors: Lei Zhang, Paulo C. C. Freire, Alessandro Ridolfi, Zhichen Pan, Jiaqi Zhao, Craig O. Heinke, Jianxing Chen, Mario Cadelano, Cristina Pallanca, Xian Hou, Xiaoting Fu, Shi Dai, Erbil Gügercinoğlu, Meng Guo, Jason Hessels, Jiale Hu, Guodong Li, Mengmeng Ni, Jingshan Pan, Scott M. Ransom, Qitong Ruan, Ingrid Stairs, Chao-Wei Tsai, Pei Wang, Long Wang, Na Wang, Qingdong Wu, Jianping Yuan, Jie Zhang, Weiwei Zhu, Yongkun Zhang, Di Li
Figure caption: Left panel: CMD of M5 in a combination of the F275W and F336W filters. The red square, circle, and pentagon are the positions of the counterparts to M5D, M5E, and M5F, respectively. The solid and dashed black curves are a 12.5 Gyr stellar population isochrone and a 0.55 M ⊙ WD cooling track, respectively. Blue curves are cooling tracks of He WDs with masses of 0.17, 0.19, 0.21, 0.25, and 0.30 M ⊙, with increasing masses from left to right. Right panel: same as the left panel, but with a combination of F275W and F435W filters.
Paper: Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 with FAST and Arecibo
Authors: Lei Zhang, Paulo C. C. Freire, Alessandro Ridolfi, Zhichen Pan, Jiaqi Zhao, Craig O. Heinke, Jianxing Chen, Mario Cadelano, Cristina Pallanca, Xian Hou, Xiaoting Fu, Shi Dai, Erbil Gügercinoğlu, Meng Guo, Jason Hessels, Jiale Hu, Guodong Li, Mengmeng Ni, Jingshan Pan, Scott M. Ransom, Qitong Ruan, Ingrid Stairs, Chao-Wei Tsai, Pei Wang, Long Wang, Na Wang, Qingdong Wu, Jianping Yuan, Jie Zhang, Weiwei Zhu, Yongkun Zhang, Di Li
Figure caption: The mass of the NS as a function of companion mass for M5D, M5E, and M5F. The derived mass of the companion star is marked with a horizontal solid line, and the corresponding uncertainty is limited by two horizontal dashed lines in shallow areas. The colored curves represent the relationship between the companion masses and the NS masses at different inclinations, and the black region is excluded by the pulsar mass function.
Paper: Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]
Authors: Yiwei Dong, Yan Sun, Ye Xu, Zehao Lin, Shuaibo Bian, Chaojie Hao, Dejian Liu, Yingjie Li, Ji Yang, Yang Su, Xin Zhou, Shaobo Zhang, Qing-Zeng Yan, Zhiwei Chen
Figure caption: Physical properties of the 12CO (blue), 13CO (green), and C18O (red) structures as a function of Galactocentric radius. The histograms and triangles indicate the mean and median values of the physical properties in the R GC bins of 1 kpc width, respectively, and the vertical lines correspond to the standard deviations around the mean values. From top to bottom: velocity dispersion, effective radius, mass, mass surface density, and virial parameter. Note that the y-axis is logarithmically scaled for the physical properties whose mean or median values span more than ∼2 orders of magnitude along R GC.
Paper: Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]
Authors: Yiwei Dong, Yan Sun, Ye Xu, Zehao Lin, Shuaibo Bian, Chaojie Hao, Dejian Liu, Yingjie Li, Ji Yang, Yang Su, Xin Zhou, Shaobo Zhang, Qing-Zeng Yan, Zhiwei Chen
Figure caption: Longitude–velocity map of the “uncleaned” 12CO emission, integrated over a Galactic latitude range from −5.°25 to 5.°25. The three MCs in red circles are contaminated by the bad channels.
Paper: Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]
Authors: Yiwei Dong, Yan Sun, Ye Xu, Zehao Lin, Shuaibo Bian, Chaojie Hao, Dejian Liu, Yingjie Li, Ji Yang, Yang Su, Xin Zhou, Shaobo Zhang, Qing-Zeng Yan, Zhiwei Chen
Figure caption: Relations between physical properties of the molecular structures traced by different CO isotopologues. Top row: most 12CO structures are plotted as small dots; those containing 13CO structures are plotted as bigger dots in darker colors; and those further containing C18O structures are enclosed in black squares. Middle row: similar to the top panels, but for 13CO structures. Bottom row: for C18O structures. Left column: mass vs. effective radius diagram. The yellow shadings, ﹩M(r)\leqslant 870\,{M}_{\odot }{\left(R/\mathrm{pc}\right)}^{1.33}﹩ , highlight the regions where the clouds fail to form high-mass stars (Kauffmann et al. 2010a, 2010b, 2013; Kauffmann & Pillai 2010). The solid red lines are the empirical lower limit of the surface density required for massive star formation (Σ = 0.05 g cm−2; Urquhart et al. 2013a, 2013b). Middle column: velocity dispersion vs. effective radius plot. The first Larson relation revealed by the data from Solomon et al. (1987) is also drawn with the cyan line for comparison. Right column: virial parameter as a function of mass. The pink shadings indicate the regions of α vir < 2. The black solid, black dashed, and green solid lines delineate the log–log linear least-squares fitting relations between the physical properties of the 12CO, 13CO, and C18O structures, respectively. The fitting results are also annotated in each graph, with the Pearson correlation coefficients marked in parentheses.
Paper: Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]
Authors: Yiwei Dong, Yan Sun, Ye Xu, Zehao Lin, Shuaibo Bian, Chaojie Hao, Dejian Liu, Yingjie Li, Ji Yang, Yang Su, Xin Zhou, Shaobo Zhang, Qing-Zeng Yan, Zhiwei Chen
Figure caption: Integrated intensity maps and spectra of the MCs MWISP G220.634−1.916, G221.775−3.007, G224.440−1.069, G223.736−2.027, and G221.921−2.121. The 12CO, 13CO, and C18O lines are drawn in blue, green, and red, respectively. The integrated intensity maps are shown in a square-root scale to clearly visualize the faint parts of the MCs, and the color bars represent integrated intensity in units of K km s−1. The spectra shown in each plot, with the y-axis on the T MB scale, are averaged over a 90″ × 90″ (3 × 3 pixels) region selected around the brightest pixel of each MC. The magenta crosses denote the 22 GHz H2O masers detected toward the star formation regions (Han et al. 1998; Valdettaro et al. 2001; Sunada et al. 2007; Urquhart et al. 2011). The H II regions from Blitz et al. (1982) and the WISE catalog (Anderson et al. 2014) are marked as green and yellow circles, respectively.
Paper: Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]
Authors: Yiwei Dong, Yan Sun, Ye Xu, Zehao Lin, Shuaibo Bian, Chaojie Hao, Dejian Liu, Yingjie Li, Ji Yang, Yang Su, Xin Zhou, Shaobo Zhang, Qing-Zeng Yan, Zhiwei Chen
Figure caption: Left: locations of the MCs projected on the Galactic plane. The plan view of the Milky Way (Reid et al. 2019) is overlaid. The straight dashed lines denote the directions of Galactic longitude l = 180°, 210°, 240°, and 270°. The Sun (red Sun symbol) is at (0, 8.15) kpc. The solid gray, orange, and blue curved lines trace the centers (and the dotted curved lines indicate the widths enclosing 90% of the high-mass star-forming regions of Reid et al. 2019) of the Local, Perseus, and Outer arms, respectively. Right: distribution of the z-scale height vs. the Galactocentric radius R GC. The Galactic plane (z = 0) is drawn with the dashed line. The Sun (red Sun symbol) is at (8.15 kpc, 5.5 pc). The red crosses indicate the centers of R GC and z of the three arms, whose values are also marked. The red bars denote the thicknesses of the arms, with their values noted on the side. In both panels, the lightest, medium, and darkest filled circles represent the 12CO, 13CO, and C18O structures, respectively. The symbol size is proportional to ﹩\mathrm{log}\left(M\right)﹩. The proportions of the three CO isotopologues are different for the convenience of presentation.
Paper: Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]
Authors: Yiwei Dong, Yan Sun, Ye Xu, Zehao Lin, Shuaibo Bian, Chaojie Hao, Dejian Liu, Yingjie Li, Ji Yang, Yang Su, Xin Zhou, Shaobo Zhang, Qing-Zeng Yan, Zhiwei Chen
Figure caption: Histograms of the derived physical properties of the 12CO (left), 13CO (center), and C18O (right) structures. Distributions for the structures in the whole G220 region and the Local, Perseus, and Outer arms are shown in black, gray, orange, and blue histograms, respectively. Top to bottom: histograms of the velocity dispersion, effective radius, mass, mass surface density, and virial parameter. The median values are labeled in each panel. The total numbers of molecular structures included in the statistics are marked in the top panels. The vertical dashed lines in the bottom panels denote the loci of α vir = 2.
Paper: Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]
Authors: Yiwei Dong, Yan Sun, Ye Xu, Zehao Lin, Shuaibo Bian, Chaojie Hao, Dejian Liu, Yingjie Li, Ji Yang, Yang Su, Xin Zhou, Shaobo Zhang, Qing-Zeng Yan, Zhiwei Chen
Figure caption: Histograms of ﹩{{\boldsymbol{A}}}_{12}^{13}﹩ (top left), ﹩{{\boldsymbol{A}}}_{12}^{18}﹩ (top right), ﹩{{\boldsymbol{M}}}_{12}^{13}﹩ (bottom left), and ﹩{{\boldsymbol{M}}}_{12}^{18}﹩ (bottom right) of MCs in the whole G220 region (black) and the Local (gray), Perseus (orange), and Outer (blue) arms. Please refer to Section 3.3.3 for the definitions of the area and mass ratios. The total numbers of structures included in the statistics and the median values for the ratios are marked.
Paper: Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]
Authors: Yiwei Dong, Yan Sun, Ye Xu, Zehao Lin, Shuaibo Bian, Chaojie Hao, Dejian Liu, Yingjie Li, Ji Yang, Yang Su, Xin Zhou, Shaobo Zhang, Qing-Zeng Yan, Zhiwei Chen
Figure caption: Mask regions of the entire G220 region (top left) and the Local (top right), Perseus (bottom left), and Outer (bottom right) arms. The definitions of the mask “B,” “G,” and “R” regions are the same as in Figure 2. The red circles and rectangles mark the structures that are contaminated by bad channels and touch the borders of the G220 region, respectively. These structures will be ignored in the statistical analysis.
Paper: Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]
Authors: Yiwei Dong, Yan Sun, Ye Xu, Zehao Lin, Shuaibo Bian, Chaojie Hao, Dejian Liu, Yingjie Li, Ji Yang, Yang Su, Xin Zhou, Shaobo Zhang, Qing-Zeng Yan, Zhiwei Chen
Figure caption: The velocity distribution of 12CO in the Local arm. The dashed lines indicate the boundaries of the six regions where different distances were adopted. The cold clumps (empty circles) of the Planck Collaboration et al. (2016) and the 13CO clouds (filled circles) of Kim et al. (2004) are used as references for determining the distances in the six regions.
Paper: Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]
Authors: Yiwei Dong, Yan Sun, Ye Xu, Zehao Lin, Shuaibo Bian, Chaojie Hao, Dejian Liu, Yingjie Li, Ji Yang, Yang Su, Xin Zhou, Shaobo Zhang, Qing-Zeng Yan, Zhiwei Chen
Figure caption: Molecular gas distributions along the Galactic longitude (upper panels) and the Galactic latitude (lower panels), integrated over a Galactic latitude range from −5.°25 to 5.°25 and a Galactic longitude range from 219.°75 to 229.°75, respectively. The mass distributions of the whole G220 region and the Local, Perseus, and Outer arms are shown in black, gray, orange, and blue histograms, respectively. And the mass distributions traced by 12CO, 13CO, and C18O are exhibited in the left, middle, and right panels, respectively.