adsabs/AstroCLIMB huggingface dataset:
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: Contours of Δχ 2 = (1, 2, 3, 4) for three different fits (as indicated by the colors in the legend), for each of four different geometries (labeled in the four panels). The contours are derived from the means and covariances matrices of the MCMCs from the 12 different models. In all four cases, the Spitzer-“only” (green) and unconstrained ground+Spitzer (blue) fits are in close agreement. After imposing the color constraint (red), the minimum of the inner solution is displaced by ∼1σ, while the minimum of the outer solution is displaced by ∼2σ. Note that the (+, + ) and (−, − ) solutions are approximately related by reflections in π E,N .
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: Data (color-coded by observatory) together with the predictions and residuals for two of the three models of OGLE-2017-BLG-1275 specified in Table 2, that is, an “inner”/”outer” pair that explain the “dip” near the peak by a minor-image pertubation. We do not show the third (“wide”) solution, which explains this dip by a major-image pertubation, to avoid clutter and because it is formally excluded by Δχ 2 = 35. The Spitzer data (cyan), which were taken from solar orbit, show a similar dip near the peak followed by a similar decline, which together imply that the source trajectory as seen by Spitzer was similar to one from the ground (right insets) and hence that the microlens parallax π E is small.
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: Data (color-coded by observatory) together with the model prediction for OGLE-2017-BLG-0640. The dip in the light curve at HJD﹩{}^{{\prime} }\sim 7895﹩ is caused by the source passing over a channel of depressed magnification that threads the two planetary caustics on the opposite side of the host relative to the planet, as illustrated in the inset.
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: Data (color-coded by observatory) together with the model prediction for OGLE-2017-BLG-1237. There is a low-amplitude bump at HJD﹩{}^{{\prime} }\sim 7936﹩ flanked by two U-shaped troughs. Together, these imply that the source has passed the central cusp of a resonant caustic and has intersected sections of this caustic before and after the passage. See inset.
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: Long-term linear trend in the OGLE-IV light curve of OGLE-2017-BLG-1777. The magnitudes are constructed by first doing difference-image photometry, then adding in the flux of the “baseline object,” and finally converting to magnitudes. The baseline object is unrelated to the microlensing event, but it accounts for the long-term trend seen here. The fit is a simple linear fit in magnitudes, with the region enclosed by red lines excluded from the fit. More detailed investigations are carried out in flux units. See Appendix A.
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: Empirical IHL color–color relation for giants (black) and dwarfs (red) determined from local stars by Bessell & Brett (1988). The green line segment shows the slope of the relation that we derived from bulge giants (whose range is represented by the length of the segment) from OGLE-III, UKIRT, and Spitzer (OUS) data, which has been transposed to the local relation, showing excellent agreement with the slope of the black curve. The magenta line is the extrapolation of the green relation to a bluer range. The inset shows the offset between the magenta and red curves. The (I − L) color of the dwarf (actually turnoff) source is determined by applying the extrapolated OUS relation and then correcting this using the inset relation at the color of the source (blue).
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: CMDs for all six events, indicated by, for example, OB171275 for OGLE-2017-BLG-1275. The red clump and the source position are shown in red and blue, respectively. Where relevant, the blended light is shown in green. For OB171237, the bright variable at 1.″4 is shown in magenta. When there are multiple solutions, we only show the source and blend for the lowest-χ 2 solution.
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: Distributions of β ≡ ∣KE/PE∣⊥, that is, the ratio of transverse kinetic to potential energy (Equation (7)) for the two solutions of OGLE-2017-BLG-1777. The orbital-motion determination is strongly influenced by the need to match a single, otherwise discrepant, point. See Figure 5. If this point were an artifact, one would expect the inferred β to be either unphysically high (β > 1) or improbably low (β ≲ 0.1). Instead, the distributions are peaked near values that are physically expected, thus increasing the plausibility of these solutions. The red vertical lines are the beta values of best-fit solution for each solution.
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: Envelope functions (line segments) based on MCMC data (points), giving Δχ 2(ρ) for OGLE-2017-BLG-1275 and OGLE-2017-BLG-0640. Note that at, for example, 2σ, ρ < 0.09 and ρ < 0.045, so that μ rel = θ ast/ρ t E is constrained to be μ rel ≳ 0.46 mas yr−1 and μ rel ≳ 2.80 mas yr−1, for OGLE-2017-BLG-1275 and OGLE-2017-BLG-0640, respectively. Thus, the ρ limit is completely unconstraining for the first case and mildly constraining for the second. See Equation (9).
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: Data (color-coded by observatory) together with the model predictions for OGLE-2017-BLG-0543. The bump at HJD﹩{}^{{\prime} }\sim 7873.7﹩ can be fit either by a weak cusp approach due to a planet (upper two inset panels) or a companion of the source passing the primary lens. Because these, respectively, 2L1S and 1L2S models cannot be distinguished from the data, the nature of the lens system remains undetermined.
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: Data (color-coded by observatory) together with model predictions for OGLE-2017-BLG-1694. Although the light-curve distortion is unambiguously detected, it can be fit by numerous, widely differing models. Hence, no definite conclusions can be drawn about the lens system.
Paper: Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-field Planets
Authors: Yoon-Hyun Ryu, Andrzej Udalski, Jennifer C. Yee, Weicheng Zang, Yossi Shvartzvald, Cheongho Han, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Hanyue Wang, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Charles Beichman, Geoffry Bryden, Sean Carey, Calen B. Henderson, Sebastiano Calchi Novati, Wei Zhu, Savannah Jacklin, Matthew T. Penny
Figure caption: Histograms of the host mass (left) and lens distance (right) for the three unambiguously planetary events, plus one very likely candidate (OB171777), as derived from the Bayesian analyses. Disk (blue) and bulge (red) distributions are shown separately, with their total shown in black.
Paper: Gas-phase Molecules in Protoplanetary Nebulae with the 21 μm Emission Feature
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jun-ichi Nakashima, Jiang-Shui Zhang, Fei Li, Deng-Rong Lu, Xin-Di Tang, Xiao-Ling Yu, Lan-Wei Jia
Figure caption: The lines of CO, 13CO, HCN, HNC, and CN in IRAS 06530-0213. The curves represent the stellar-shell fitting, except for the CO J = 1 → 0 transition that is fitted with two Gaussian profiles. The vertical lines mark the positions and intrinsic relative intensities of hyperfine components. The velocity resolutions are listed in Tables 2–7. For the CN N = 2 → 1 transition, panel (a) shows the unresolved hyperfine structures of J  F  = 3/21/2 → 1/23/2, 3/23/2 → 1/23/2, 3/25/2 → 1/23/2, 3/21/2 → 1/21/2, and 3/23/2 → 1/21/2 in the frequency range 226.6–226.7 GHz, and panel (b) shows the unresolved hyperfine structures of J  F  = 5/25/2 → 3/23/2, 5/27/2 → 3/25/2, 5/23/2 → 3/21/2, 5/23/2 → 3/23/2, 5/25/2 → 3/25/2, and 5/23/2 → 3/2, 5/2 in the frequency range 226.8–226.9 GHz.
Paper: Gas-phase Molecules in Protoplanetary Nebulae with the 21 μm Emission Feature
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jun-ichi Nakashima, Jiang-Shui Zhang, Fei Li, Deng-Rong Lu, Xin-Di Tang, Xiao-Ling Yu, Lan-Wei Jia
Figure caption: Spectra of the 21 μm sources obtained with the PMO 13.7 m telescope. The dotted vertical lines mark the strong lines in the spectrum of CRL 2688. To bring out the lines against the noise, 36 adjacent channels have been binned, resulting in a frequency resolution of about 2 MHz. To avoid smearing, we cut off part of the spectra of IRAS Z0229+6208, and the zoom-out spectra are shown in the insets.
Paper: Gas-phase Molecules in Protoplanetary Nebulae with the 21 μm Emission Feature
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jun-ichi Nakashima, Jiang-Shui Zhang, Fei Li, Deng-Rong Lu, Xin-Di Tang, Xiao-Ling Yu, Lan-Wei Jia
Figure caption: Spectra of the 21 μm sources obtained with the SMT 10 m telescope. The dotted vertical lines mark the strong lines in the spectrum of CRL 2688. To bring out the lines against the noise, three adjacent channels have been binned, resulting in a frequency resolutions of about 3 MHz.
Paper: Gas-phase Molecules in Protoplanetary Nebulae with the 21 μm Emission Feature
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jun-ichi Nakashima, Jiang-Shui Zhang, Fei Li, Deng-Rong Lu, Xin-Di Tang, Xiao-Ling Yu, Lan-Wei Jia
Figure caption: Same as Figure 3, but for CO, 13CO, HCN, and CN in IRAS 07134+1005.
Paper: Gas-phase Molecules in Protoplanetary Nebulae with the 21 μm Emission Feature
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jun-ichi Nakashima, Jiang-Shui Zhang, Fei Li, Deng-Rong Lu, Xin-Di Tang, Xiao-Ling Yu, Lan-Wei Jia
Figure caption: Same as Figure 3, but for CO, 13CO, HCN, HNC, and CN in IRAS 19500-1709.
Paper: Gas-phase Molecules in Protoplanetary Nebulae with the 21 μm Emission Feature
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jun-ichi Nakashima, Jiang-Shui Zhang, Fei Li, Deng-Rong Lu, Xin-Di Tang, Xiao-Ling Yu, Lan-Wei Jia
Figure caption: Same as Figure 3, but for CO in IRAS 22272+5435.
Paper: Gas-phase Molecules in Protoplanetary Nebulae with the 21 μm Emission Feature
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jun-ichi Nakashima, Jiang-Shui Zhang, Fei Li, Deng-Rong Lu, Xin-Di Tang, Xiao-Ling Yu, Lan-Wei Jia
Figure caption: Abundance ratios and densities vs. intensities of the 21 μm feature with respect to total IR emission. The dotted lines are the best linear fits. The correlation coefficient is marked at the top of each panel. The numbers 02, 06, 07, 19, 22, and 23 on the plot are for IRAS Z02229+6208, IRAS 06530-0213, IRAS 07134+1005, IRAS 19500-1709, IRAS 22272+5435, and IRAS 23304+6147, respectively.
Paper: Gas-phase Molecules in Protoplanetary Nebulae with the 21 μm Emission Feature
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jun-ichi Nakashima, Jiang-Shui Zhang, Fei Li, Deng-Rong Lu, Xin-Di Tang, Xiao-Ling Yu, Lan-Wei Jia
Figure caption: Same as Figure 3, but for CO, 13CO, HCN, H13CN, HNC, HC3N, and CN in IRAS Z02229+6208.
Paper: Gas-phase Molecules in Protoplanetary Nebulae with the 21 μm Emission Feature
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jun-ichi Nakashima, Jiang-Shui Zhang, Fei Li, Deng-Rong Lu, Xin-Di Tang, Xiao-Ling Yu, Lan-Wei Jia
Figure caption: Same as Figure 3, but for CO, 13CO, HCN, H13CN, HNC, and CN in IRAS 23304+6147.
Paper: Gas-phase Molecules in Protoplanetary Nebulae with the 21 μm Emission Feature
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jun-ichi Nakashima, Jiang-Shui Zhang, Fei Li, Deng-Rong Lu, Xin-Di Tang, Xiao-Ling Yu, Lan-Wei Jia
Figure caption: Rotational diagram of HC3N in IRAS Z02229+6208.
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: Color–color diagrams are shown for all human-selected Class 1 + 2 cluster candidates. U − B vs. V − I is shown on the left and B − V vs. V − I on the right. The predicted color evolution from the BC03 stellar population models are shown for solar metallicity (red) and 1/50 × solar metallicity (blue). The light blue oval at the upper left shows the “young cluster locus,” the green oval shows the “middle-aged plume,” and the red oval shows the “old GC clump.” Dashed lines indicate the color cuts we use to select our initial list of GC candidates, B – V ≥ 0.5 and V – I ≥ 0.73. Only those candidates with significant U-band measurements are plotted in the left panel. The arrows represent the direction and amount of reddening for A  V  = 1.
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: Diagnostic plots for a reddened young cluster. In the middle panels the source occupies a similar region in color–color space as a GC, but it is in a somewhat crowded region, appears lumpy, and has a nonuniform color in the BVI image (left). In the right panel (B − Hα − I) there is a partial bubble of Hα emission encircling the cluster. These are strong indications that the source is young and reddened rather than ancient. The color–color diagrams are in the same format as Figure 3.
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: Diagnostic plots for an ancient GC. The source appears symmetric, round, and has a uniform color in a BVI image (left). The right panel, a B − V – CO image, shows there is no CO emission associated with the cluster. In the color–color diagrams shown in the center panel, the cluster (blue circle) lies close to predictions from the 1/50 × solar metallicity single stellar population (SSP) model. Black star symbols mark ages of 1 Myr, 10 Myr, 100 Myr, 1 Gyr, and 10 Gyr on the solar metallicity track. A cyan star marks the predicted position for 10 Gyr in the 1/50 solar model.
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: Color BVI images of the 17 PHANGS-HST galaxies studied in this work. The sample includes nearby face-on, massive spiral galaxies that cover a broad range of morphology, dust content, and spiral arm type.