adsabs/AstroCLIMB huggingface dataset:
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: The blue lines are the α (top), β (middle), and γ (bottom) lines of ion RRLs stacked from the spectra of Orion KL measured in the Ka band using the TMRT 65 m (left) and in the K band using the Effelsberg 100 m by Gong et al. (2015; right). The orange lines are the modeled spectra of ion RRLs. The orange lines in the right panels have been multiplied by a factor of 0.8. Only the unblended transitions are stacked. In particular, in the Ka band, we stacked X+ n α (n = 99, 97, 95, 92, 91), X+ n β (n = 123, 121, 119, 117, 115), and X+ n γ (n = 142, 137, 136, 134, 131). In K band, we stacked X+ n α (n = 112, 111, 110, 108, 107, 106, 105, 104, 103, 101, 100), X+ n β (n = 141, 137, 135, 131, 127) and X+ n γ (n = 162, 159, 158, 156, 153, 148, 147, 146, 145, 144).
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: Left: Spliced spectrum of CH3OH; same as the upper left panel of Figure 10, but with a different y-axis scale. The labeled transitions are ﹩{J}_{{K}_{a},{K}_{c}}={J}_{2,J-1}-{J}_{1,J-1}﹩. Right: Peak intensities (I peak) of CH3OH J 2,J−1 − J 1,J−1 detected in this survey (blue squares) and in the K-band survey of Gong et al. (2015; orange squares). The red solid, gray dashed, and gray solid lines show the predicted peak intensity distribution along J under LTE with a T ex of 100, 200, and 50 K, respectively. The cyan line shows the rest frequency (f 0) of the transitions with different J.
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: The blue lines are the spliced spectra of CH3OH and its isotopologues as well as these species in vibrationally excited states. The spectrum between two neighboring upper ticks are independent frequency segment. The red solid lines show the result of the model fitting of the corresponding species. The red dashed lines include the modeled emission of all species and RRLs. See Figure 17 for other molecular species detected in the Ka-band survey.
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption:  K-band α lines of ion RRLs (blue) from the archive data of Effelsberg (Gong et al. 2015). The orange lines are the modeled spectrum. The orange dashed line takes all species into account, and the orange solid line only considers the ion RRLs.
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: Spectra of CH3C3N (blue) in the Ka and Q bands. The y-axis in all panels has the same scale. Each rotational line is split into several transitions by the value of K, as marked in the upper left panel. The orange solid lines are the model fitting of CH3C3N, and the orange dashed lines have taken all species into account. All transitions of CH3C3N expected to be stronger than 5 mK have been shown here.
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: Spliced spectrum of C2H5CN v 13/v 21. The meaning of solid and dashed red lines are same as that of the upper left panel of Figure 10. The center frequencies of each segment are marked by the gray text labels.
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption:                       ﹩{\mathrm{log}}_{10}({f}_{{n}_{1},{n}_{2}}^{\dagger })﹩ (left) and ﹩{f}_{{n}_{1},{n}_{2}}^{\dagger }/{f}_{{n}_{1},{n}_{2}}^{\star }﹩ (right) for RRLs with different n and Δn.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The stellar population properties of the star particles of a sample NH2 galaxy (NH2 ID: 2). (a) The density map of all the star particles in terms of chemical properties. The cyan contours show the MW stellar data adopted from the APOGEE (Jönsson et al. 2020) and GALAH (Buder et al. 2021) projects. The dashed–dotted lines show the zero-points and the white box shows the region that panel (b) zooms in on. (b) The zoom-in map of the box in panel (a). This smoothed distribution appears to be bimodal, which is similar to what is found in the MW disk. One may divide the bimodal distribution at the valley marked by the horizontal dashed line at [α/Fe]=0.06, which in turn classifies the stars into thin-disk (below the line) and thick-disk (above the line) stars. (c) [α/Fe] vs. age for the star particles in panel (b). The bimodality in [α/Fe] is clearly associated with the age distribution and hence the star formation history. The coalescence time for the gas-rich minor merger at 6.2 Gyr of lookback time, discussed in the main text, is marked.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The positions of the spatially thin and thick disk stars of all the 27 NH galaxies when they are observed (final snapshot) and at their birth. The abscissa shows the mean radial position of the stars from the galactic center in units of the disk scale length in the final snapshot. The ordinate shows the mean position of the stars in vertical distance from the galaxy disk’s midplane in units of the thin-disk scale height in the final snapshot. The three spatially separated groups of stars in the final snapshot (circles) were barely distinguishable in terms of birth position (star symbols). The median positions of the thin (∣z∣/z thick < 0.5;  blue), thick (1.5 < ∣z∣/z thick < 2.5;  green), and thicker (5 < ∣z∣/z thick < 6;  red) components are shown with the first and third quantiles, where z thick is roughly 0.8 kpc.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The kinematic properties of all the star particles of a sample NH galaxy. This GMM exercise identified the five components in order of mass fraction based on three properties (﹩e/| {e}_{\max }| ﹩, J z/J circ(e), and J p/J circ(e)). The dashed ellipses show the thin-disk (Component 1, marked in blue), thick-disk (Components 2 and 4, marked in green), and spheroid (Components 3 and 5, marked in red) components. The projected histograms associated with the three groups (blue, green, and red curves) along with the total (black) are also presented.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The face-on and edge-on images of sample galaxies from NH (panels (a) and (c); also in the Appendix in Figure A1 as NH ID: 8) and from NH2 (panels (b) and (d); also in the Appendix in Figure A2 as NH2 ID: 2). The red, green, and blue colors correspond to the SDSS i-, r-, and g-band fluxes, respectively.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The color images of the thin-disk (top row) and thick-disk (bottom row) stars classified by [α/Fe] as illustrated in Figure 5(b) (NH2 ID: 2). Seemingly, the [α/Fe] = 0.06 cut is effective as a thin–thick disk classifier.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The two-component fit to the profiles of the galaxy shown in Figure 1 (NH ID: 8). The plus symbols show the actual profiles and the continuous lines show the fits. (a) The radial profile of the galaxy (face-on) is well reproduced by a combination of two components: an exponential disk and a spheroid with a Sérsic index 4. (b) The vertical luminosity profile at (2.0 ± 0.1)R d and ∣z∣ ≤ 3 kpc is well reproduced by a two-component model. (c) The vertical mass profile appears slightly different from the mass profile, but is still closely reproduced by a two-component model.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The measured properties of the thin and thick disks of the NH galaxies in the r band compared with the observational data. The circles denote the NH galaxies. (a) The ratios in the vertical scale height between thick and thin disks. (b) The luminosity fraction of the thick disks. The dashed lines and shades with matching colors show the median and first–third quantiles of the three data sets.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The face-on and edge-on images of the components in Figure 7. The mass fraction of each component is shown in each panel.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The chemical and kinematic properties of the star particles of two NH2 galaxies. (a) The same galaxy as shown in Figures 5 and 6. The [α/Fe] bimodality shown in Figure 5 is also visible here. The horizontal dashed line shows the arbitrary cut that separates the low- and high-[α/Fe] stars from the bimodality. The vertical line at ϵ = 0.5 divides rotation-dominant (ϵ ≥ 0.5) and dispersion-dominant (ϵ < 0.5) stars. The other vertical line at ϵ = 0.75 divides kinematically thin and thick disk components. The percentage of stars in each section is also given. (b) The same information, but for a different galaxy. This galaxy has more than three main [α/Fe] components in the disk, instead of two.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The correspondence between different sampling results based on the NH2 galaxy shown in Figure 9(a) (NH2 ID: 2). (a) The circularity distribution of the three components by GMM. This galaxy has one thin-disk component and one thick-disk component detected by GMM. (b) The [α/Fe] distribution of the thin- and thick-disk stars sampled as shown in (a). The two vertical lines show the mean values of the two disk components. As shown in Figure 9, contamination is severe in the case of the thick disk. (c) The same as panel (b), but for [Fe/H]. (d) The same as panel (b), but for age. (e) The vertical distribution of the thin- and thick-disk stars sampled in (a). (f) The vertical r-band luminosity profile fitted by a two-component model as described in Section 3.2.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The comparison between the circularity at birth and the circularity today for all the stars of one NH galaxy. A one-to-one correlation is shown by the diagonal line. The black curves show the 0.5σ, 1.0σ, and 1.5σ contours. The distribution is heavily biased. Most stars are born with a large value of circularity on a thin rotating disk and are gradually heated to show a much wider distribution in the end.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The mean change of circularity of the star particles between their birth and now (Δϵ = ϵ now − ϵ birth). Panels (a), (b), and (c) are for three sample galaxies, and panel (d) shows the mean values for the whole sample of the 27 NH galaxies. The demarcation lines for the thin- and thick-disk components are marked by vertical dashed lines. The slanted line shows the criterion above which the star in the bin becomes kinematically thin. Considering that most of the stars are born with a high value of circularity, most of the disk stars become kinematically hotter compared to their birth.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The key properties of thick disks of NH galaxies compared between the photometric vertical profile fit and the kinematic decomposition at 2 R d. (a) The ratio of the vertical scale heights between the thin and thick disks. (b) The r-band luminosity contribution of the thick disks to the total disk luminosity.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The BIC-selected vertical fitting result, measured at 1 ± 0.1 R d for the same NH galaxies in Figure A1. The data points (gray plus symbols), thin disks (blue lines), thick disks (green lines), extra components (red lines), and total fits (magenta lines) are presented.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The face-on and edge-on images of the 16 most massive disk galaxies in the NH simulation. The blue, green, and red components in the mock images correspond to the SDSS g, r, and i bands.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The same as Figure A3, but for the measurement performed at 2 ± 0.1 R d for reference.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The same as Figure A1, but for the sample of 10 NH2 galaxies.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: Same as Figure 7 in the main text, but for additional NH galaxies for reference.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The same as Figure A7, but for different galaxies.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The same as Figure 9 in the main text, but for the rest of the NH2 sample.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: Similar to Figure 5(b) in the main text, but for the rest of the NH2 sample.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: Similar to Figure 5(c) in the main text, but for the rest of the NH2 sample.
Paper: On the Significance of the Thick Disks of Disk Galaxies
Authors: Sukyoung K. Yi, J. K. Jang, Julien Devriendt, Yohan Dubois, San Han, Taysun Kimm, Katarina Kraljic, Minjung Park, Sebastien Peirani, Christophe Pichon, Jinsu Rhee
Figure caption: The same as Figure 12 in the main text, but for the 16 most massive NH galaxies.
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: Mutual correlations between molecular gas surface density (Σmol), star formation rate surface density (based on extinction-corrected Hα emission, ΣSFR), and stellar surface density (Σ*) for the full set of square grid downsampled pixels. The three panels correspond to the Kennicutt–Schmidt, molecular gas main-sequence, and star-forming main-sequence diagrams respectively. Points in each panel are color coded and binned by the value of the third parameter. A horizontal line in the middle panel denotes the approximate sensitivity limit for the CARMA CO data.
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: CO rotation curves derived from the 3D-Barolo package (blue circles) compared to those previously published by Leung et al. (2018), Levy et al. (2018), for the sample of 54 galaxies studied by Leung et al. (2018). Circular velocities have been multiplied by a ﹩\sin i﹩ factor to compensate for different adopted inclinations; the plotted curves should thus approximate the observed velocity widths. Differences are most apparent in the central rings, where varying treatment of beam smearing and velocity dispersion can have significant effects.
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: Inclination-corrected radial CO profiles for the sample of 54 galaxies studied by Leung et al. (2018). The dashed curve in each panel represents a 3σ detection limit adopting a default velocity width of 200 km s−1 but using the actual mask width where it exceeds 200 km s−1 in width. Gray points denote radii where the azimuthal average is measured (i.e., there are >10% unmasked CO pixels at these radii) but falls below the detection limit and is thus unreliable.
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: Comparison of the three sampling methods in the edge_pydb, using the Hα image of NGC 3687 as an example. Counts of unblanked pixels are given in parentheses.