adsabs/AstroCLIMB huggingface dataset:
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Broadening function of KIC09164694 showing at least two components.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Folded Kepler light curve of KIC09345838 and mean light curve.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Broadening function and model line profile of KIC11097678 showing two spectral components.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Histogram of best-fitting model contact binary parameters for contact plus ambiguous systems.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Light-curve morphology vs. orbital period for the probable contact binaries, detached binaries, and ambiguous cases, as denoted by symbol type.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Model light curves and velocity curves of KIC11097678 in comparison to the data with the data.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Histograms of the uncertainties on systems classified as a contact binary (C), detached (D), or ambiguous (A), characterized as one-half the difference between the 84th- and 16th-percentile values of each parameter. Vertical dotted lines mark the median of each C + A distribution.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Bayesian uncertainty vs. ﹩\cos i﹩ for probable contact binaries, detached binaries, and ambiguous cases.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Posterior probability distributions for combinations of four free parameters for KIC11097678 when irradiation effects are included in the PHOEBE models. The distributions are shifted markedly from those in Figure 55, particularly regarding third light, which is now l3 ≃ 0.24 instead of 0.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Posterior probability distributions for combinations of four parameters for KIC11097678.
Paper: A Bayesian Analysis of Physical Parameters for 783 Kepler Close Binaries: Extreme-mass-ratio Systems and a New Mass Ratio versus Period Lower Limit
Authors: Henry A. Kobulnicky, Lawrence A. Molnar, Evan M. Cook, Lauren E. Henderson
Figure caption: Best-fitting values of ﹩\cos i﹩, f, ﹩\mathrm{log}(q)﹩, l3, and T 2/T 1 for all 669 systems designated as contact binaries (blue squares) or ambiguous (gray points).
Paper: Monitoring AGNs with Hβ Asymmetry. III. Long-term Reverberation Mapping Results of 15 Palomar–Green Quasars
Authors: Dong-Wei Bao, Michael S. Brotherton, Pu Du, Jacob N. McLane, T. E. Zastrocky, Kianna A. Olson, Feng-Na Fang, Shuo Zhai, Zheng-Peng Huang, Kai Wang, Bi-Xuan Zhao, Sha-Sha Li, Sen Yang, Yong-Jie Chen, Jun-Rong Liu, Zhu-Heng Yao, Yue-Chang Peng, Wei-Jian Guo, Yu-Yang Songsheng, Yan-Rong Li, Bo-Wei Jiang, David H. Kasper, William T. Chick, My L. Nguyen, Jaya Maithil, H. A. Kobulnicky, D. A. Dale, Derek Hand, C. Adelman, Z. Carter, A. M. Murphree, M. Oeur, S. Schonsberg, T. Roth, Hartmut Winkler, Paola Marziani, Mauro D'Onofrio, Chen Hu, Ming Xiao, Suijian Xue, Bożena Czerny, Jesús Aceituno, Luis C. Ho, Jin-Ming Bai, Jian-Min Wang
Figure caption: Time-series analysis of PG 0007+106. Panels (a), (b), and (c) are the scaled continuum, combined continuum, and Hβ light curves. The units are 10−15 erg s−1 cm−2  Å−1 for panels (a) and (b) and 10−13 erg s−1 cm−2 for panel (c). The gray dotted lines separate different seasons. The gray shadow and gray dashed lines are the MICA reconstructions for the whole light curve and single seasons, respectively. Panels (d)–(m) are the mean (rms) spectra of the seasons and the entire light curve in the rest frames. The black dashed lines are the narrow-line-subtracted mean spectra. The gray and blue shades mark the integration and background windows for Hβ fluxes, and the two blue dotted lines mark the 5100 Å continuum window. The units in panels (d)–(m) are 10−15 erg s−1 cm−2  Å−1 (10−16 erg s−1 cm−2  Å−1). Panels (n)–(ab) are the MICA, ICCF, and χ 2 results for the corresponding seasons and the entire light curve (in observed frame). The gray histograms are the distributions of the centroid lags obtained from MICA (CCCDs from ICCF or lag distributions from χ 2 method) in panels (n)–(r), (s)–(w), or (x)–(ab). The blue dotted lines are the median of the distributions. The error bars shown in the light curves do not include the systematic uncertainties in Table 4 (they are used in the time-series analysis in Section 3.5; see also Section 3.2).
Paper: Monitoring AGNs with Hβ Asymmetry. III. Long-term Reverberation Mapping Results of 15 Palomar–Green Quasars
Authors: Dong-Wei Bao, Michael S. Brotherton, Pu Du, Jacob N. McLane, T. E. Zastrocky, Kianna A. Olson, Feng-Na Fang, Shuo Zhai, Zheng-Peng Huang, Kai Wang, Bi-Xuan Zhao, Sha-Sha Li, Sen Yang, Yong-Jie Chen, Jun-Rong Liu, Zhu-Heng Yao, Yue-Chang Peng, Wei-Jian Guo, Yu-Yang Songsheng, Yan-Rong Li, Bo-Wei Jiang, David H. Kasper, William T. Chick, My L. Nguyen, Jaya Maithil, H. A. Kobulnicky, D. A. Dale, Derek Hand, C. Adelman, Z. Carter, A. M. Murphree, M. Oeur, S. Schonsberg, T. Roth, Hartmut Winkler, Paola Marziani, Mauro D'Onofrio, Chen Hu, Ming Xiao, Suijian Xue, Bożena Czerny, Jesús Aceituno, Luis C. Ho, Jin-Ming Bai, Jian-Min Wang
Figure caption: Time-series analysis of PG 0049+171. The gray and black dashed lines in panels (i)–(m) are the original and continuum-cleaned rms spectra (see more details in Section 3.1). The meanings of the other panels, lines, and histograms are the same as in Figure 2.
Paper: Monitoring AGNs with Hβ Asymmetry. III. Long-term Reverberation Mapping Results of 15 Palomar–Green Quasars
Authors: Dong-Wei Bao, Michael S. Brotherton, Pu Du, Jacob N. McLane, T. E. Zastrocky, Kianna A. Olson, Feng-Na Fang, Shuo Zhai, Zheng-Peng Huang, Kai Wang, Bi-Xuan Zhao, Sha-Sha Li, Sen Yang, Yong-Jie Chen, Jun-Rong Liu, Zhu-Heng Yao, Yue-Chang Peng, Wei-Jian Guo, Yu-Yang Songsheng, Yan-Rong Li, Bo-Wei Jiang, David H. Kasper, William T. Chick, My L. Nguyen, Jaya Maithil, H. A. Kobulnicky, D. A. Dale, Derek Hand, C. Adelman, Z. Carter, A. M. Murphree, M. Oeur, S. Schonsberg, T. Roth, Hartmut Winkler, Paola Marziani, Mauro D'Onofrio, Chen Hu, Ming Xiao, Suijian Xue, Bożena Czerny, Jesús Aceituno, Luis C. Ho, Jin-Ming Bai, Jian-Min Wang
Figure caption: Time-series analysis of PG 0947+396. The gray and black dashed lines in panels (i)–(m) are the original and continuum-cleaned rms spectra (see more details in Section 3.1). The meanings of the other panels, lines, and histograms are the same as in Figure 2.
Paper: Monitoring AGNs with Hβ Asymmetry. III. Long-term Reverberation Mapping Results of 15 Palomar–Green Quasars
Authors: Dong-Wei Bao, Michael S. Brotherton, Pu Du, Jacob N. McLane, T. E. Zastrocky, Kianna A. Olson, Feng-Na Fang, Shuo Zhai, Zheng-Peng Huang, Kai Wang, Bi-Xuan Zhao, Sha-Sha Li, Sen Yang, Yong-Jie Chen, Jun-Rong Liu, Zhu-Heng Yao, Yue-Chang Peng, Wei-Jian Guo, Yu-Yang Songsheng, Yan-Rong Li, Bo-Wei Jiang, David H. Kasper, William T. Chick, My L. Nguyen, Jaya Maithil, H. A. Kobulnicky, D. A. Dale, Derek Hand, C. Adelman, Z. Carter, A. M. Murphree, M. Oeur, S. Schonsberg, T. Roth, Hartmut Winkler, Paola Marziani, Mauro D'Onofrio, Chen Hu, Ming Xiao, Suijian Xue, Bożena Czerny, Jesús Aceituno, Luis C. Ho, Jin-Ming Bai, Jian-Min Wang
Figure caption: Mean spectra (observed flux density versus rest-frame wavelength) of the objects. Flux units are 10−15 erg s−1 cm−2  Å−1.
Paper: Monitoring AGNs with Hβ Asymmetry. III. Long-term Reverberation Mapping Results of 15 Palomar–Green Quasars
Authors: Dong-Wei Bao, Michael S. Brotherton, Pu Du, Jacob N. McLane, T. E. Zastrocky, Kianna A. Olson, Feng-Na Fang, Shuo Zhai, Zheng-Peng Huang, Kai Wang, Bi-Xuan Zhao, Sha-Sha Li, Sen Yang, Yong-Jie Chen, Jun-Rong Liu, Zhu-Heng Yao, Yue-Chang Peng, Wei-Jian Guo, Yu-Yang Songsheng, Yan-Rong Li, Bo-Wei Jiang, David H. Kasper, William T. Chick, My L. Nguyen, Jaya Maithil, H. A. Kobulnicky, D. A. Dale, Derek Hand, C. Adelman, Z. Carter, A. M. Murphree, M. Oeur, S. Schonsberg, T. Roth, Hartmut Winkler, Paola Marziani, Mauro D'Onofrio, Chen Hu, Ming Xiao, Suijian Xue, Bożena Czerny, Jesús Aceituno, Luis C. Ho, Jin-Ming Bai, Jian-Min Wang
Figure caption: Time-series analysis of PG 0923+129. The meanings of the panels, lines, and histograms are the same as in Figure 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: Maps of the crowding limit in the LSST simulation with f bin = 0, for the ugrizy bands (from the top-left to the bottom-right panels) and for a uniform seeing value of 0.″6 at all wavelengths. They are derived from the n side = 128 density maps. The color scale covers a maximum range of 7 mag, starting from the coadd limiting depth (gray level). We plot only the areas around the bulge and the Magellanic Clouds, as the remaining sky areas turn out to be above the crowding limit (although they have nonnegligible photometric errors due to crowding). The white horizontal line in the color scale signals the single-visit depth for every filter.
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: Left panel: counts of eclipsing binaries per square degree in the MW simulation for LSST with f bin = 1. Counts have been scaled up by taking into account that we simulated one-tenth of the expected binaries. Right panel: histogram of their maximum r-magnitude variations, ﹩{\rm{\Delta }}{r}_{\max }﹩. The red, yellow, and green areas divide eclipses into three groups separated at ﹩{\rm{\Delta }}{r}_{\max }﹩ of 0.01 and 0.1 mag. Total counts for each group are also indicated.
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: Histograms of LPVs periods in the LSST MW simulation with f bin = 0. The histograms are color coded according to the dominant mode, going from the fundamental to the third overtone.
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: Histograms of classical Cepheids periods in the LSST MW simulation with f bin = 0. The two histograms are color coded according to the dominant mode: blue if fundamental mode, green if first overtone.
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: Star-to-galaxy ratio for a single visit (i < 24 mag, left panel) and for a coadd (i < 26.8 mag, right panel).
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: Same as Figure 18 but now presenting the crowding limit in the r band at two different values of seeing.
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 areas drawn in Figure 9.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: One-dimensional distributions of w, Ωm, and μ  c  constrained from Pantheon SN-Ia.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: The same as Figure 12, but now w is manually set to −0.5.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: One-dimensional distributions of Ωm constrained from Pantheon SN-Ia, where the blue solid line is based on the MDN method with three Gaussian components and the red solid line is based on the MDN method with one beta component. Here w is set to −1.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: Examples of beta probability density function with different shape parameters calculated using the beta function in Equation (36).
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: Comparisons of global properties between our group galaxies and the xCOLD GASS galaxies. (a) SFR, (b) H I gas fraction (M H I/M ⋆), (c) H2 gas fraction (M H2/M ⋆), (d) the ratio of molecular to atomic gas (M H2/M H I), (e) H I gas depletion time (τ dep,H I), (f) H2 gas depletion time (τ dep,H2) as a function of the stellar mass (M ⋆). The red and blue filled circles indicate our sample galaxies with CO detection in the I1495G and the N4636G, respectively. The upper limit for nondetection of CO is shown as the open circles. Group samples with their names, which show asymmetric H I and/or CO distributions, are marked by yellow crosses. The xCOLD GASS sample is shown as gray filled circles (H I or CO detections) and open gray circles (nondetection in H I or nondetection in CO, respectively). In panel (a), the star-forming main sequence, which is determined by Saintonge et al. (2016), is indicated by a solid line, and the 0.3 dex scatter is shown in dashed lines. Filled circles indicate CO detections, while nondetections in CO are shown in open circles. In panels (b)–(f), the median trends (solid lines) and the 1σ standard deviations (dashed lines) are derived from the xCOLD GASS sample. In panel (d), the upper limit (i.e., nondetection in CO) and the lower limit (i.e., nondetection in H I) are represented by small magenta and cyan arrows, respectively. We limited our group sample to relatively massive galaxies (log (M ⋆/M ⊙) > 9) because all group samples with CO detection have their stellar mass of log (M ⋆/M ⊙) > 9.
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: H I (contours) and CO distributions (color scale) of 15 group galaxies (the first two rows: six galaxies in the I1459G, and the second three rows: nine galaxies in the N4636G) are overlaid on their optical images (DSS2 blue). In each CO map, while a cyan color indicates a low-intensity value, a magenta color shows a relatively high-intensity value. Contour levels of the H I gas are shown at the bottom of each panel. These H I images are from the ASKAP BETA data (Serra et al. 2015a) for the I1459G, the WALLABY pilot data (Koribalski et al. 2020) for the N4636G, and the VIVA data (Chung et al. 2009) for NGC 4536 and NGC 4772 in the N4636G. The green cross indicates the stellar disk center. The bar in the bottom-left corner represents the physical scale of 2 kpc. The synthesized beams of CO (blue ellipse) and H I (black open ellipse) observations are shown in the bottom-right corner.
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: Comparisons of global properties between our group galaxies and the xCOLD GASS galaxies. The H2 gas mass is calculated with the constant CO-to-H2 conversion factor (α CO = 4.35 M ⊙ pc−2 (K km s−1)−1 Strong & Mattox 1996; Bolatto et al. 2013). (a) H2 gas fraction (M H2/M ⋆), (b) the ratio of molecular to atomic gas (M H2/M H I), and (c) H2 gas depletion time (τ dep,H2) as a function of the stellar mass (M ⋆). All symbols are the same as the symbols in Figure 6.
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 5264.
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 5273.
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: CO-detected members in the I1459G.
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: CO-detected members in the N4636G.