adsabs/AstroCLIMB huggingface dataset:
Paper: First Frequency Phase Transfer from the 3 mm to the 1 mm Band on an Earth-sized Baseline
Authors: Sara Issaoun, Dominic W. Pesce, María J. Rioja, Richard Dodson, Lindy Blackburn, Garrett K. Keating, Sheperd S. Doeleman, Bong Won Sohn, Wu Jiang, 悟 江, Dan Hoak, Wei Yu, 威 于, Pablo Torne, Ramprasad Rao, Remo P. J. Tilanus, Iván Martí-Vidal, Taehyun Jung, Garret Fitzpatrick, Miguel Sánchez-Portal, Salvador Sánchez, Jonathan Weintroub, Mark Gurwell, Carsten Kramer, Carlos Durán, David John, Juan L. Santaren, Derek Kubo, Chih-Chiang Han, Helge Rottmann, Jason SooHoo, Vincent L. Fish, Guang-Yao Zhao, Juan Carlos Algaba, Ru-Sen Lu, 如森 路, Ilje Cho, Satoki Matsushita, Karl-Friedrich Schuster
Figure caption: Comparison between the visibility phases on an intra-SMA baseline (in blue) and the phase residual on the VLBI baseline (in red) after carrying out FPT. The VLBI phase residuals have been coherently averaged over 10 s to match the SMA cadence. The intra-SMA phases shown here correspond to the baseline between antennas 2 and 6, as indicated in Figure 1. The separation between the intra-SMA antennas is  ∼180 m, while the separation between the SMA reference antenna and the JCMT is  ∼160 m.
Paper: First Frequency Phase Transfer from the 3 mm to the 1 mm Band on an Earth-sized Baseline
Authors: Sara Issaoun, Dominic W. Pesce, María J. Rioja, Richard Dodson, Lindy Blackburn, Garrett K. Keating, Sheperd S. Doeleman, Bong Won Sohn, Wu Jiang, 悟 江, Dan Hoak, Wei Yu, 威 于, Pablo Torne, Ramprasad Rao, Remo P. J. Tilanus, Iván Martí-Vidal, Taehyun Jung, Garret Fitzpatrick, Miguel Sánchez-Portal, Salvador Sánchez, Jonathan Weintroub, Mark Gurwell, Carsten Kramer, Carlos Durán, David John, Juan L. Santaren, Derek Kubo, Chih-Chiang Han, Helge Rottmann, Jason SooHoo, Vincent L. Fish, Guang-Yao Zhao, Juan Carlos Algaba, Ru-Sen Lu, 如森 路, Ilje Cho, Satoki Matsushita, Karl-Friedrich Schuster
Figure caption: The array used for the observations presented in this paper, as seen from the source J0958+6533. The IRAM−JCMT baseline at 86 GHz is shown in red, the IRAM−SMA baseline at 215 GHz is shown in cyan. The inset on top shows the distribution of antennas on Maunakea, with the JCMT shown in red and the individual SMA antennas shown in cyan and enumerated. Antenna 6 was the SMA reference antenna for our observations.
Paper: First Frequency Phase Transfer from the 3 mm to the 1 mm Band on an Earth-sized Baseline
Authors: Sara Issaoun, Dominic W. Pesce, María J. Rioja, Richard Dodson, Lindy Blackburn, Garrett K. Keating, Sheperd S. Doeleman, Bong Won Sohn, Wu Jiang, 悟 江, Dan Hoak, Wei Yu, 威 于, Pablo Torne, Ramprasad Rao, Remo P. J. Tilanus, Iván Martí-Vidal, Taehyun Jung, Garret Fitzpatrick, Miguel Sánchez-Portal, Salvador Sánchez, Jonathan Weintroub, Mark Gurwell, Carsten Kramer, Carlos Durán, David John, Juan L. Santaren, Derek Kubo, Chih-Chiang Han, Helge Rottmann, Jason SooHoo, Vincent L. Fish, Guang-Yao Zhao, Juan Carlos Algaba, Ru-Sen Lu, 如森 路, Ilje Cho, Satoki Matsushita, Karl-Friedrich Schuster
Figure caption: Bandpass-calibrated and rate-removed visibility phases on the IRAM−JCMT baseline at 86 GHz after scaling by the frequency ratio (in red) and on the IRAM−SMA baseline at 215 GHz (in blue), with moving 10 s averages overlaid as solid curves. The phases are shown for Scan 03 on the source OJ 287 (left) and for Scan 05 on the source J0958+6533 (right). Time is indicated in UT hours on 2024 January 24.
Paper: First Frequency Phase Transfer from the 3 mm to the 1 mm Band on an Earth-sized Baseline
Authors: Sara Issaoun, Dominic W. Pesce, María J. Rioja, Richard Dodson, Lindy Blackburn, Garrett K. Keating, Sheperd S. Doeleman, Bong Won Sohn, Wu Jiang, 悟 江, Dan Hoak, Wei Yu, 威 于, Pablo Torne, Ramprasad Rao, Remo P. J. Tilanus, Iván Martí-Vidal, Taehyun Jung, Garret Fitzpatrick, Miguel Sánchez-Portal, Salvador Sánchez, Jonathan Weintroub, Mark Gurwell, Carsten Kramer, Carlos Durán, David John, Juan L. Santaren, Derek Kubo, Chih-Chiang Han, Helge Rottmann, Jason SooHoo, Vincent L. Fish, Guang-Yao Zhao, Juan Carlos Algaba, Ru-Sen Lu, 如森 路, Ilje Cho, Satoki Matsushita, Karl-Friedrich Schuster
Figure caption: Phase coherence (see Equation (1)) as a function of averaging time for the same two scans as shown in Figure 2. The blue curves indicate the 215 GHz coherence prior to transferring phase corrections from 86 GHz, and the red curves show the postcorrection coherence.
Paper: First Frequency Phase Transfer from the 3 mm to the 1 mm Band on an Earth-sized Baseline
Authors: Sara Issaoun, Dominic W. Pesce, María J. Rioja, Richard Dodson, Lindy Blackburn, Garrett K. Keating, Sheperd S. Doeleman, Bong Won Sohn, Wu Jiang, 悟 江, Dan Hoak, Wei Yu, 威 于, Pablo Torne, Ramprasad Rao, Remo P. J. Tilanus, Iván Martí-Vidal, Taehyun Jung, Garret Fitzpatrick, Miguel Sánchez-Portal, Salvador Sánchez, Jonathan Weintroub, Mark Gurwell, Carsten Kramer, Carlos Durán, David John, Juan L. Santaren, Derek Kubo, Chih-Chiang Han, Helge Rottmann, Jason SooHoo, Vincent L. Fish, Guang-Yao Zhao, Juan Carlos Algaba, Ru-Sen Lu, 如森 路, Ilje Cho, Satoki Matsushita, Karl-Friedrich Schuster
Figure caption: Correlation between 86 and 215 GHz visibility phases for OJ 287 (top) and J0958+6533 (bottom). The dashed red line in both panels has a slope equal to the frequency ratio of  ∼2.5.
Paper: Deep Optical Images of the Ejecta Nebula around the Wolf–Rayet Star WR 8 (HD 62910)
Authors: Robert A. Fesen, Daniel Patnaude, Wei-Hao Wang, You-Hua Chu, Jason Sun, Manuel C. Peitsch, Martin Pugh, Scott Garrod, Michael Selby, Alex Woronow
Figure caption: Two independent color composite Hα and [O III] images of WR 8’s nebula with and without stars.
Paper: Deep Optical Images of the Ejecta Nebula around the Wolf–Rayet Star WR 8 (HD 62910)
Authors: Robert A. Fesen, Daniel Patnaude, Wei-Hao Wang, You-Hua Chu, Jason Sun, Manuel C. Peitsch, Martin Pugh, Scott Garrod, Michael Selby, Alex Woronow
Figure caption: Color composites of WR 8’s nebula. Left panel: WISE 4.6 μm (blue), 12 μm (green), and 22 μm (red) images. Right panel: WISE 22 μm (red) and [O III] λ5007 (blue) images.
Paper: Deep Optical Images of the Ejecta Nebula around the Wolf–Rayet Star WR 8 (HD 62910)
Authors: Robert A. Fesen, Daniel Patnaude, Wei-Hao Wang, You-Hua Chu, Jason Sun, Manuel C. Peitsch, Martin Pugh, Scott Garrod, Michael Selby, Alex Woronow
Figure caption: A stretched positive [O III] image showing extended emission around WR 8’s brighter inner nebula.
Paper: Deep Optical Images of the Ejecta Nebula around the Wolf–Rayet Star WR 8 (HD 62910)
Authors: Robert A. Fesen, Daniel Patnaude, Wei-Hao Wang, You-Hua Chu, Jason Sun, Manuel C. Peitsch, Martin Pugh, Scott Garrod, Michael Selby, Alex Woronow
Figure caption: Wide FOV color image of WR 8 composited of Hα (red), [O III] (blue) and broadband filter images.
Paper: Small and Close-in Planets are Uncommon Around A-type Stars
Authors: Steven Giacalone, Courtney D. Dressing
Figure caption: Pipeline sensitivity (top) and completeness (bottom) for different planet radii and orbital periods for our sample of 20,257 stars. The color of each cell corresponds to the value displayed within it. Uncertainties in sensitivity are Poisson errors associated with injected planets that were recovered in each cell. Uncertainties in completeness include both Poisson errors and an additional 20% systematic uncertainty to account for the precision of the stellar-mass and radius estimates. Nonmonotonicity near large Rp and low Porb is a product of the automated vetting tests described in Section 3.2. The overall completeness of the pipeline (i.e., integrated over the full Porb and Rp range) is 7.2%. The completenesses for planets with radii of 4–8 R⊕, 2–4 R⊕, and 1–2 R⊕ are 13.1%, 3.2%, and 0.2%, respectively.
Paper: Small and Close-in Planets are Uncommon Around A-type Stars
Authors: Steven Giacalone, Courtney D. Dressing
Figure caption: Periods and depths of TCEs detected by the automated pipeline described in Section 3.2. The points are divided into two categories: red circles, which were determined to be false alarms or false positives in the SPOC comparison vetting test (Section 3.3.1), and blue squares, which were determined to be false positives in the secondary eclipse test (Section 3.3.2), centroid offset test (Section 3.3.3), ExoFOP crossmatch (Section 3.3.4), or transit shape analysis (Section 3.3.5). The period distribution of TCEs is somewhat bimodal, with peaks between 0.5 and 1 day and between 6 and 9 days. Nearly all of the TCEs with longer periods were ruled out as false alarms in the SPOC comparison test, which suggests that they are artifacts associated with the orbit of the TESS spacecraft or its momentum dumps (e.g., M. Kunimoto et al. 2023). Most of the shorter-period TCEs are consistent with being false positives caused by eclipsing binary stars or stellar variability.
Paper: Small and Close-in Planets are Uncommon Around A-type Stars
Authors: Steven Giacalone, Courtney D. Dressing
Figure caption: Calculated 3σ upper limits on the occurrence rates of sub-Saturns (4 R⊕ < Rp < 8 R⊕; top), sub-Neptunes (2 R⊕ < Rp < 4 R⊕; middle), and super-Earths (1 R⊕ < Rp < 2 R⊕; bottom) with Porb < 10 days around A-type stars from TESS data (black). Error bars on the 3σ upper limits are shown as gray shading. Shown for comparison are the corresponding occurrence rates from C. D. Dressing & D. Charbonneau (2013, Porb = 0.68−10 days; red), C. D. Dressing & D. Charbonneau (2015, Porb = 0.5−10 days; red), G. D. Mulders et al. (2015a, Porb = 0.4−10 days; light green), and M. Kunimoto & J. M. Matthews (2020, Porb = 0.78​​​​​​−12.5 days; blue) for FGKM-type stars, which are calculated from Kepler data. Our results indicate a continual decrease in the occurrence rate of sub-Saturns and sub-Neptunes between G-type and A-type stars, and rules out the possibility of an M dwarf–like super-Earth occurrence rate around A-type stars at a high level of confidence. These findings suggest that small planets either cannot survive at, form at, or migrate to short separations around hot stars.
Paper: Small and Close-in Planets are Uncommon Around A-type Stars
Authors: Steven Giacalone, Courtney D. Dressing
Figure caption: Visualization of the centroid offset test for TIC 177120452, which was found to have 2.5 day signal by the TCE detection pipeline. Left: the difference image of the TESS Sector 7 data of the star, which show a clear offset 3 pixels (approximately ﹩1^{\prime} \rm{}\,\rm{}\,﹩) to the east. TIC 177120452 is indicated by a white star and bright nearby stars are indicated by cyan circles, where size corresponds to relative brightness. Center: the time-averaged TESS Sector 7 image of the target. The red square corresponds to the pixel with the peak residual flux in the difference image. Right: the light curve extracted from the highlighted pixel, phase folded to the ephemeris detected by the TCE pipeline. The red dashed line shows the signal predicted by the TCE pipeline for photometry extracted from TIC 177120452. The true source if the detected signal appears to be a pair of eclipsing binary stars originating from TIC 177014166 (ΔT = 4.71, separation = 6″).
Paper: Small and Close-in Planets are Uncommon Around A-type Stars
Authors: Steven Giacalone, Courtney D. Dressing
Figure caption: Phase-folded light curves of the four signals discussed in Section 3.3.5, binned to 2 minute intervals for clarity. Best-fit transit models with 1σ uncertainties are shown in blue. After fitting the signal around TIC 120155231 with a transit model, we determined the planet candidate to be larger than 8 R⊕. We determined the remaining signals to be false positives based on analyses with TRICERATOPS.
Paper: Small and Close-in Planets are Uncommon Around A-type Stars
Authors: Steven Giacalone, Courtney D. Dressing
Figure caption: Occurrence rates for super-Earths, sub-Neptunes, sub-Saturns, and hot Jupiters for G-type (left), F-type (center), and A-type (left) stars. Blue data are from M. Kunimoto & J. M. Matthews (2020), green data are from M. Beleznay & M. Kunimoto (2022), and black data are the 3σ upper limits calculated in this paper. The limits calculated from each of these papers suggest that the radius cliff may become less steep with increasing host star Teff, based on the ratio of sub-Neptune occurrence rate to hot Jupiter occurrence rate (﹩{f}_{{\rm{SN}}}/{f}_{{\rm{HJ}}}﹩). In other words, the frequency of close-in sub-Neptunes may decrease more rapidly than that of hot Jupiters around progressively hotter stars.
Paper: Small and Close-in Planets are Uncommon Around A-type Stars
Authors: Steven Giacalone, Courtney D. Dressing
Figure caption: Visualization of the event symmetry test described in Section 3.2. The left-side panels show the phase-folded events detected by the BLS periodogram. The right-side panels compare the binned premidpoint (blue circles) and postmidpoint (red squares) data. The top two panels show the results for a symmetric event detected around TIC 25590886, which returns ﹩{\chi }_{{\rm{red}}}^{2}=0.75﹩. The bottom two panels show the results for an asymmetric event detected around TIC 337442870, which returns ﹩{\chi }_{{\rm{red}}}^{2}=19.34﹩. With our threshold of ﹩{\chi }_{{\rm{red}}}^{2}=2﹩, the former passes the symmetry test and the latter fails.
Paper: Small and Close-in Planets are Uncommon Around A-type Stars
Authors: Steven Giacalone, Courtney D. Dressing
Figure caption: Visualization of signals that fail the manual secondary eclipse search. The left-side panel shows the signal detected in the light curve of TIC 126449150, which has a convincing secondary eclipse. The phase-folded light curve is shifted by half of the detected period so that the secondary eclipse appears at the center of the plot. The right-side panel shows the phase-folded odd-numbered events (blue circles) and even-numbered events (red squares) of the signal detected in the light curve of TIC 355453890, which exhibit significantly different depths.
Paper: Photometric and Spectroscopic Investigations of Three Large Amplitude Contact Binaries
Authors: Xin Xu, Kai Li, Fei Liu, Qian-Xue Yan, Yi-Fan Wang, Xin-Yu Cui, Jing-Yi Wang, Xing Gao, Guo-You Sun, Cheng-Yu Wu, Mu-Zi-Mei Li
Figure caption: The left is energy transfer parameter–bolometric luminosity ratio diagram and the right is the corrected transfer parameter–bolometric luminosity diagram. The dashed lines correspond to different α values. The non-H systems are collected by K. Li et al. (2021b), which are depicted as open circles and triangles for A and W subtype. The filled circles and triangles depict the H/A and H/W contact binaries we collected. The filled squares and diamonds depict the H/A and H/W systems collected by S. Csizmadia & P. Klagyivik (2004).
Paper: Photometric and Spectroscopic Investigations of Three Large Amplitude Contact Binaries
Authors: Xin Xu, Kai Li, Fei Liu, Qian-Xue Yan, Yi-Fan Wang, Xin-Yu Cui, Jing-Yi Wang, Xing Gao, Guo-You Sun, Cheng-Yu Wu, Mu-Zi-Mei Li
Figure caption: The logJo-logMtotal diagram. The black crosses represent the detached binaries collected by Z. Eker et al. (2006). The black solid circles represent the contact binaries collected by K. Li et al. (2021b). The solid red circles are our three targets. This diagram also incorporates a borderline depicted as a dashed line.
Paper: Photometric and Spectroscopic Investigations of Three Large Amplitude Contact Binaries
Authors: Xin Xu, Kai Li, Fei Liu, Qian-Xue Yan, Yi-Fan Wang, Xin-Yu Cui, Jing-Yi Wang, Xing Gao, Guo-You Sun, Cheng-Yu Wu, Mu-Zi-Mei Li
Figure caption: The mass–luminosity and mass–radius diagrams, the left is M–L diagram and the right is M-R diagram. The black solid and open circles represent primary and secondary of collected H-subtype targets and the red solid and open circles represent primary and secondary of our targets.
Paper: Photometric and Spectroscopic Investigations of Three Large Amplitude Contact Binaries
Authors: Xin Xu, Kai Li, Fei Liu, Qian-Xue Yan, Yi-Fan Wang, Xin-Yu Cui, Jing-Yi Wang, Xing Gao, Guo-You Sun, Cheng-Yu Wu, Mu-Zi-Mei Li
Figure caption: The left is energy transfer parameter–contact degree diagram and the right is the corrected transfer parameter–contact degree diagram.
Paper: Photometric and Spectroscopic Investigations of Three Large Amplitude Contact Binaries
Authors: Xin Xu, Kai Li, Fei Liu, Qian-Xue Yan, Yi-Fan Wang, Xin-Yu Cui, Jing-Yi Wang, Xing Gao, Guo-You Sun, Cheng-Yu Wu, Mu-Zi-Mei Li
Figure caption: The spectroscopic investigations for the three targets, including one for J034828, two for J073802, and three for J084000.
Paper: Photometric and Spectroscopic Investigations of Three Large Amplitude Contact Binaries
Authors: Xin Xu, Kai Li, Fei Liu, Qian-Xue Yan, Yi-Fan Wang, Xin-Yu Cui, Jing-Yi Wang, Xing Gao, Guo-You Sun, Cheng-Yu Wu, Mu-Zi-Mei Li
Figure caption: The relationship between mean residuals and mass ratio of light curves from D. P. Kjurkchieva et al. (2017b).
Paper: A Measurement of the Water Abundance in the Atmosphere of the Hot Jupiter WASP-43b with High-resolution Cross-correlation Spectroscopy
Authors: Dare Bartelt, Megan Weiner Mansfield, Michael R. Line, Vivien Parmentier, Luis Welbanks, Elspeth K. H. Lee, Jorge Sanchez, Arjun B. Savel, Peter C. B. Smith, Emily Rauscher, Joost P. Wardenier
Figure caption: Posterior distributions from the retrieval on the atmospheric composition of WASP-43b. Off-diagonal plots show 2D posterior probabilities for pairs of parameters, with 1σ, 2σ, and 3σ intervals shaded in dark, medium, and light blue, respectively. On-diagonal plots show marginalized posterior probability distributions for each parameter. We find a constrained water abundance of ﹩{\mathrm{log}}_{10}({\rm{H}\,}_{2}\,\rm{O})=-2.2{4}_{-0.48}^{+0.57}﹩, an unconstrained CO abundance, and place 2σ upper limits on the abundances of CO2 and CH4 of ﹩{\mathrm{log}}_{10}({\,\rm{CO}\,}_{2})\lt -2.78﹩ and ﹩{\mathrm{log}}_{10}({\,\rm{CH}\,}_{4})\lt -5.89﹩.
Paper: A Measurement of the Water Abundance in the Atmosphere of the Hot Jupiter WASP-43b with High-resolution Cross-correlation Spectroscopy
Authors: Dare Bartelt, Megan Weiner Mansfield, Michael R. Line, Vivien Parmentier, Luis Welbanks, Elspeth K. H. Lee, Jorge Sanchez, Arjun B. Savel, Peter C. B. Smith, Emily Rauscher, Joost P. Wardenier
Figure caption: Cross-correlation SNRs as a function of systemic velocity (Vsys) and Keplerian velocity (Kp) for H2O, CH4, CO2, and CO from the four nights combined. We detect H2O at an SNR of 3.51 but do not detect any carbon-bearing species, although CO may be a tentative detection. The white dashed lines represent the Vsys and Kp values of WASP-43b from the literature (A. S. Bonomo et al. 2017; Gaia Collaboration et al. 2018). The red x's indicate the maximum signal from the cross-correlation.
Paper: A Measurement of the Water Abundance in the Atmosphere of the Hot Jupiter WASP-43b with High-resolution Cross-correlation Spectroscopy
Authors: Dare Bartelt, Megan Weiner Mansfield, Michael R. Line, Vivien Parmentier, Luis Welbanks, Elspeth K. H. Lee, Jorge Sanchez, Arjun B. Savel, Peter C. B. Smith, Emily Rauscher, Joost P. Wardenier
Figure caption: The humidities during each transit phase during night 1 (blue), night 2 (orange), night 3 (green), night 4 (red), and night 5 (purple). The higher humidity on night 4 resulted in a weaker detection of H2O. Therefore, we excluded it from the analysis.
Paper: A Measurement of the Water Abundance in the Atmosphere of the Hot Jupiter WASP-43b with High-resolution Cross-correlation Spectroscopy
Authors: Dare Bartelt, Megan Weiner Mansfield, Michael R. Line, Vivien Parmentier, Luis Welbanks, Elspeth K. H. Lee, Jorge Sanchez, Arjun B. Savel, Peter C. B. Smith, Emily Rauscher, Joost P. Wardenier
Figure caption: Progressive subtraction of SVs from the spectra obtained on night 5. Five components were removed by SVD, the optimal value for night 5. In the first panel, tellurics, stellar features, and the shape of the instrument throughput dominate the data. As components are progressively subtracted, the nonplanetary signals are removed, and the planet's signal is hidden in the remaining noise.
Paper: A Measurement of the Water Abundance in the Atmosphere of the Hot Jupiter WASP-43b with High-resolution Cross-correlation Spectroscopy
Authors: Dare Bartelt, Megan Weiner Mansfield, Michael R. Line, Vivien Parmentier, Luis Welbanks, Elspeth K. H. Lee, Jorge Sanchez, Arjun B. Savel, Peter C. B. Smith, Emily Rauscher, Joost P. Wardenier
Figure caption: Cross-correlation SNRs as a function of systemic velocity (Vsys) and Keplerian velocity (Kp) for water, for nights 1, 2, 3, and 5. The white dashed lines represent the Vsys and Kp values of WASP-43b from the literature (A. S. Bonomo et al. 2017; Gaia Collaboration et al. 2018). The red x's indicate the maximum signal from the cross-correlation.
Paper: A Measurement of the Water Abundance in the Atmosphere of the Hot Jupiter WASP-43b with High-resolution Cross-correlation Spectroscopy
Authors: Dare Bartelt, Megan Weiner Mansfield, Michael R. Line, Vivien Parmentier, Luis Welbanks, Elspeth K. H. Lee, Jorge Sanchez, Arjun B. Savel, Peter C. B. Smith, Emily Rauscher, Joost P. Wardenier
Figure caption: Water volume mixing ratios for WASP-43b, measured through direct observations. The circular points indicate that the measurement was from a transmission spectrum, whereas the square points indicate that the measurement was from emission spectra. References are listed in the legend in the bottom left corner and in Table 2.
Paper: The Stellar Disk Structure Revealed by the Mono-age Populations of the LAMOST Red Clump Star Sample
Authors: Zheng Yu, Bingqiu Chen, Jianhui Lian, Chun Wang, Xiaowei Liu
Figure caption: Radial surface density profiles Σ(R) for the five mono-age populations. Different populations are offset vertically for clarity. The top panel highlights Component 1, while the bottom panel focuses on Component 2. Each point represents the natural logarithm of surface densities across different radial segments. The fitting results are shown as solid lines in the figure.
Paper: The Stellar Disk Structure Revealed by the Mono-age Populations of the LAMOST Red Clump Star Sample
Authors: Zheng Yu, Bingqiu Chen, Jianhui Lian, Chun Wang, Xiaowei Liu
Figure caption: Vertical scale height profiles for various mono-age populations. Error bars indicate 1σ uncertainty. The top and bottom panels show the radial dependencies of hZ1 and hZ2, respectively, for different age groups, as indicated.
Paper: The Stellar Disk Structure Revealed by the Mono-age Populations of the LAMOST Red Clump Star Sample
Authors: Zheng Yu, Bingqiu Chen, Jianhui Lian, Chun Wang, Xiaowei Liu
Figure caption: The resulting age-hZ trend from the set of mock density distributions for a double exponential model. The left panel shows Component 1 (hZ1), while the right panel shows Component 2 (hZ2). The input density models had both hZ1 and hZ2 increasing monotonically with age in five bins (0–3, 3–5, 5–7, 7–9, and >9 Gyr), with hZ1 ranging from 0.2 to 0.6 kpc and hZ2 from 1.0 to 1.4 kpc (shown by the dashed lines). We applied random errors of 30% to the mock ages, and measured the structural parameters using our density fitting method. The fitted values with error bars are shown as points. This demonstrates the method's ability to recover the general trends of both disk components, despite the introduced age uncertainties.
Paper: The Stellar Disk Structure Revealed by the Mono-age Populations of the LAMOST Red Clump Star Sample
Authors: Zheng Yu, Bingqiu Chen, Jianhui Lian, Chun Wang, Xiaowei Liu
Figure caption: Top panel: the number density distribution of the RC star sample in the R−Z plane. The density map uses a bin size of 0.03 × 0.025 kpc. The Sun is located at (R, Z) = (8, 0.025) kpc. Bottom panel: sky maps of the selection function for our RC star sample, illustrating variations in detection probability across different Galactic coordinates. The scatter plot displays data points spanning Galactic latitudes from −60° to 80°. The accompanying color bar indicates the detection probability, scaled from 0.0 (dark purple) to 1.0 (bright green).