adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA-IMF. XIV. Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
Authors: Roberto Galván-Madrid, Daniel J. Díaz-González, Frédérique Motte, Adam Ginsburg, Nichol Cunningham, Karl M. Menten, Mélanie Armante, Mélisse Bonfand, Jonathan Braine, Timea Csengeri, Pierre Dell'Ova, Fabien Louvet, Thomas Nony, Rudy Rivera-Soto, Patricio Sanhueza, Amelia M. Stutz, Friedrich Wyrowski, Rodrigo H. Álvarez-Gutiérrez, Tapas Baug, Sylvain Bontemps, Leonardo Bronfman, Manuel Fernández-López, Antoine Gusdorf, Atanu Koley, Hong-Li Liu, Javiera Salinas, Allison P. M. Towner, Anthony P. Whitworth
Figure caption: Validation of the procedure to estimate the free–free emission in the ALMA-IMF maps via the H41α line. The plots show a pixel-by-pixel comparison between the free–free intensity at 3 mm derived from H41α vs. that derived from the 2 cm continuum, assuming a spectral index of −0.1. We used the W51-IRS2 and W51-E protoclusters, for which there are also high-quality VLA data at a similar angular resolution (Ginsburg et al. 2016). The left panel shows all the 145,862 pixels with an intensity above 5σ in both maps. 96.8% of those pixels fall within ±3σ of the one-to-one relation. The middle panel shows the 0.2% of the pixels that are defined as bright outliers; their location is analyzed in Figure 4. The right panel shows the faint outliers (3% of the pixels), which are mostly in the periphery of H II regions and have a lower signal-to-noise ratio. The colored points and bars in the middle and right panels have the same color as their error bars in the left panel.
Paper: ALMA-IMF. XIV. Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
Authors: Roberto Galván-Madrid, Daniel J. Díaz-González, Frédérique Motte, Adam Ginsburg, Nichol Cunningham, Karl M. Menten, Mélanie Armante, Mélisse Bonfand, Jonathan Braine, Timea Csengeri, Pierre Dell'Ova, Fabien Louvet, Thomas Nony, Rudy Rivera-Soto, Patricio Sanhueza, Amelia M. Stutz, Friedrich Wyrowski, Rodrigo H. Álvarez-Gutiérrez, Tapas Baug, Sylvain Bontemps, Leonardo Bronfman, Manuel Fernández-López, Antoine Gusdorf, Atanu Koley, Hong-Li Liu, Javiera Salinas, Allison P. M. Towner, Anthony P. Whitworth
Figure caption: A detailed look at the areas labeled as “bright outliers” (red points) in Figure 3. The top left panel shows the outliers at the position of the well-known HC H II region W51 e2. The CH3CN line is seen in absorption at this location due to the high brightness temperature of the partially optically thick H II emission. The bottom left panel shows the location of the outliers at the position of the UC H II region W51 d2, which is not as bright in the millimeter continuum; therefore CH3CN is not seen in absorption. The right panels plot the corresponding H41α and He41α spectra inside the red contours, showing that molecular-line contamination is not significant. Therefore, the most likely origin of the bright outliers is an underestimation of the free–free extrapolation from centimeter wavelengths.
Paper: ALMA-IMF. XIV. Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
Authors: Roberto Galván-Madrid, Daniel J. Díaz-González, Frédérique Motte, Adam Ginsburg, Nichol Cunningham, Karl M. Menten, Mélanie Armante, Mélisse Bonfand, Jonathan Braine, Timea Csengeri, Pierre Dell'Ova, Fabien Louvet, Thomas Nony, Rudy Rivera-Soto, Patricio Sanhueza, Amelia M. Stutz, Friedrich Wyrowski, Rodrigo H. Álvarez-Gutiérrez, Tapas Baug, Sylvain Bontemps, Leonardo Bronfman, Manuel Fernández-López, Antoine Gusdorf, Atanu Koley, Hong-Li Liu, Javiera Salinas, Allison P. M. Towner, Anthony P. Whitworth
Figure caption: Flowchart of the procedure to create two types of output in each of the observed ALMA continuum bands: free–free maps with their associated errors, and estimation maps of dust-only emission. The primary-beam-corrected versions of the previous two are calculated at the end of the procedure.
Paper: ALMA-IMF. XIV. Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
Authors: Roberto Galván-Madrid, Daniel J. Díaz-González, Frédérique Motte, Adam Ginsburg, Nichol Cunningham, Karl M. Menten, Mélanie Armante, Mélisse Bonfand, Jonathan Braine, Timea Csengeri, Pierre Dell'Ova, Fabien Louvet, Thomas Nony, Rudy Rivera-Soto, Patricio Sanhueza, Amelia M. Stutz, Friedrich Wyrowski, Rodrigo H. Álvarez-Gutiérrez, Tapas Baug, Sylvain Bontemps, Leonardo Bronfman, Manuel Fernández-López, Antoine Gusdorf, Atanu Koley, Hong-Li Liu, Javiera Salinas, Allison P. M. Towner, Anthony P. Whitworth
Figure caption: Detailed view of areas of the free–free oversubtraction issue, or negative “potholes” in G010.62. Top panels: 3 mm continuum minus free–free estimation (left) and corresponding error of the free–free estimation (right). Dashed contours are at −10 × σ mad_std = −8.2 mJy beam−1. Bottom panels: B6 continuum minus free–free estimation (left) and corresponding error of the free–free estimation (right). Dashed contours are at −10 × σ mad_std = −12.6 mJy beam−1. “Potholes” in the central UC H II region are present in both the 3 mm and 1 mm subtractions, but the negative peak is still consistent with zero when the error map of the free–free estimation is considered.
Paper: ALMA-IMF. XIV. Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
Authors: Roberto Galván-Madrid, Daniel J. Díaz-González, Frédérique Motte, Adam Ginsburg, Nichol Cunningham, Karl M. Menten, Mélanie Armante, Mélisse Bonfand, Jonathan Braine, Timea Csengeri, Pierre Dell'Ova, Fabien Louvet, Thomas Nony, Rudy Rivera-Soto, Patricio Sanhueza, Amelia M. Stutz, Friedrich Wyrowski, Rodrigo H. Álvarez-Gutiérrez, Tapas Baug, Sylvain Bontemps, Leonardo Bronfman, Manuel Fernández-López, Antoine Gusdorf, Atanu Koley, Hong-Li Liu, Javiera Salinas, Allison P. M. Towner, Anthony P. Whitworth
Figure caption: Number abundance of helium with respect to hydrogen N He/N H for the H II regions in the 11 ALMA-IMF protoclusters with detection H41α and He41α. The shaded area within dashed lines marks the expected range for the Milky Way ISM, 0.08 to 0.1.
Paper: Statistics and Habitability of F-type Star–Planet Systems
Authors: Shaan D. Patel, Manfred Cuntz, Nevin N. Weinberg
Figure caption: Theoretical curves relating stellar temperatures and stellar radii for the MS F-type stars. The main curve depicts the main relationship. We also give upper and lower curves representing 10% and 20% higher and lower radii, respectively. The actual data points from the table are overlaid.
Paper: Statistics and Habitability of F-type Star–Planet Systems
Authors: Shaan D. Patel, Manfred Cuntz, Nevin N. Weinberg
Figure caption: Theoretical tracks of stellar radii vs. temperatures for stars on the MS from MESA models of different masses (1.0–2.0 M ⊙, as shown in the color bar). The actual data points from the table are overlaid along with their error bars.
Paper: Statistics and Habitability of F-type Star–Planet Systems
Authors: Shaan D. Patel, Manfred Cuntz, Nevin N. Weinberg
Figure caption: Distance from the planet’s semimajor axis to the inner or outer limit of the HZ (whichever is closer); see the Appendix for index information. HD 26161 is not shown due to its outlying distance of 17.82 au.
Paper: Statistics and Habitability of F-type Star–Planet Systems
Authors: Shaan D. Patel, Manfred Cuntz, Nevin N. Weinberg
Figure caption: Metallicities vs. stellar temperatures (left panel) and metallicities vs. stellar radii (right panel) for all systems.
Paper: Statistics and Habitability of F-type Star–Planet Systems
Authors: Shaan D. Patel, Manfred Cuntz, Nevin N. Weinberg
Figure caption: Histogram of the stellar temperatures for all systems considered.
Paper: Statistics and Habitability of F-type Star–Planet Systems
Authors: Shaan D. Patel, Manfred Cuntz, Nevin N. Weinberg
Figure caption: Histogram of the stellar metallicities for all systems considered.
Paper: Statistics and Habitability of F-type Star–Planet Systems
Authors: Shaan D. Patel, Manfred Cuntz, Nevin N. Weinberg
Figure caption: Planetary distances (circular approximation) from the HZs in relation to the planetary eccentricities. The eccentricity is either the assumed value, an upper limit, or the actual eccentricity. The left panel conveys the full data set, whereas the right panel conveys a zoomed-in portion. Error bars for the nonzero eccentricities are given as well. HD 26161 is not included due to its outlying distance of 17.82 au.
Paper: Statistics and Habitability of F-type Star–Planet Systems
Authors: Shaan D. Patel, Manfred Cuntz, Nevin N. Weinberg
Figure caption: Depiction of all 18 systems that spend at least part of their time within their respective HZs. Empty markers in panel (c) represent actual planetary mass values as opposed to ﹩{M}_{{\rm{p}}}\sin i﹩ minimum mass values, which are represented by filled in markers.
Paper: Statistics and Habitability of F-type Star–Planet Systems
Authors: Shaan D. Patel, Manfred Cuntz, Nevin N. Weinberg
Figure caption: Histogram showing the number of systems as a function of the planet’s distance from the HZ. HD 26161 is not included due to its outlying distance of 17.82 au.
Paper: Statistics and Habitability of F-type Star–Planet Systems
Authors: Shaan D. Patel, Manfred Cuntz, Nevin N. Weinberg
Figure caption: Classification of planetary orbits relative to the stellar HZ, including the cushion; see text for details.
Paper: A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys
Authors: Shaohua Zhang, 少华 张, Zhijian Luo, 智坚 罗, Xiheng Shi, 习珩 史, Chenggang Shu, 成钢 束, Hubing Xiao, 胡兵 肖, Hongyan Zhou, 宏岩 周
Figure caption: Infrared luminosity and color diagrams for the ULIRGs. The open circles represent sources with flux upper limits, while high and moderate flux qualities are shown with open circles with arrows and filled circles, respectively. Top-left panel: the dotted line represents the boundary between galaxies and stars (Kim & Sanders 1998). Top-right panel: for sources with flux upper limits, we use the WISE W4 magnitudes (centered at 22 μm) to replace the upper limits at 25 μm; the green filled circles represent the color of W4/f60. The dotted lines represent the boundaries between normal galaxies, Type II Seyferts, and quasars (Neff & Hutchings 1992). Bottom-left panel: the dotted line represents the selection criteria (﹩\mathrm{log}\,f60/f100\gt -0.3﹩) of the 1 Jy sample of ULIRGs (Kim & Sanders 1998). The squares are at the mean color and the central luminosity of ULIRGs in the three luminosity bins. The vertical error bars define the limiting luminosities of the bins, and the horizontal error bars represent the standard deviation of ﹩\mathrm{log}\,f60/f100﹩ colors in each bin. Bottom-right panel: WISE color–color diagram for the ULIRGs. The red, blue, and green filled circles symbolize galaxies (not included in the Million Quasars (Milliquas) catalog) as well as Type I and II objects (distinguished by the presence or absence of broad emission lines as per Paliya et al. 2024; Wu & Shen 2022; see details in Section 4), respectively. The plotted isodensity contours refer to WISE thermal sources, and the locations of various source classes are also highlighted. The contour data are adopted from Massaro et al. (2011).
Paper: A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys
Authors: Shaohua Zhang, 少华 张, Zhijian Luo, 智坚 罗, Xiheng Shi, 习珩 史, Chenggang Shu, 成钢 束, Hubing Xiao, 胡兵 肖, Hongyan Zhou, 宏岩 周
Figure caption: Distribution of the 1.4 GHz radio luminosities (left panel) and q values (right panel) of the ULIRGs plotted as a function of 60 μm FIR luminosity. The sources in our ULIRG sample with detections in FIRST and NVSS are represented by black and green filled circles, respectively, and the IRAS 2 Jy sample galaxies are overplotted by gray crosses for contrast. In the left panel, the dashed line means the best-fitting line for an all-sky sample of infrared-detected galaxies from IRAS (Yun et al. 2001). In the right panel, the dashed line is at q = 2.34, which is the mean value obtained by Yun et al. (2001), while the above and below dotted lines are limits for 5× FIR excess and radio excess from the mean, respectively.
Paper: A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys
Authors: Shaohua Zhang, 少华 张, Zhijian Luo, 智坚 罗, Xiheng Shi, 习珩 史, Chenggang Shu, 成钢 束, Hubing Xiao, 胡兵 肖, Hongyan Zhou, 宏岩 周
Figure caption: Comparisons of various optical spectroscopic parameters measured/derived for Type I ULIRGs (red) as well as NLS1 (green) and BLS1 (blue) sources. All measurements are obtained from Paliya et al. (2024).
Paper: A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys
Authors: Shaohua Zhang, 少华 张, Zhijian Luo, 智坚 罗, Xiheng Shi, 习珩 史, Chenggang Shu, 成钢 束, Hubing Xiao, 胡兵 肖, Hongyan Zhou, 宏岩 周
Figure caption: SDSS spectra in the rest frame of three ULIRGs with Mg II BAL features. The main emission lines are represented by dashed lines, and the gray shaded regions illustrate the Mg II BAL troughs.
Paper: Automatic Parallel Tempering Markov Chain Monte Carlo with Nii-C
Authors: Sheng Jin, Wenxin Jiang, Dong-Hong Wu
Figure caption: The sampling outcomes of a five-dimensional Rastrigin function using Nii-C with different configurations. The top left panel gives the theoretical distribution of a two-dimensitional Rastrigin function. The top right panel displays the corner plots resulting from the implementation of standard parallel tempering MCMC configuration, whereby the early tuning of the parallel tempering ladders and proposal distributions have been disabled. The bottom left panel displays the results obtained in the case where only the early tuning of proposal distributions proposal is enabled, while the tuning of parallel tempering ladders is disabled. The bottom right panel shows the case in which both the parallel tempering ladders and proposal distributions proposal are activated in the initial tuning stage.
Paper: Automatic Parallel Tempering Markov Chain Monte Carlo with Nii-C
Authors: Sheng Jin, Wenxin Jiang, Dong-Hong Wu
Figure caption: A multimodal two-dimensional Gaussian distribution, left panel, and the results of an APT-MCMC sampling using Nii-C, right panel. The standard deviations of the two peaks of this multimodal Gaussian distribution are both equal to 1 on each axis. The centers of the two peaks are located at (10,10) and (–10,–10), respectively.
Paper: Identification of Carbon Stars in LAMOST DR9 Based on Deep Learning
Authors: YiMing He, Zhong Cao, Hui Deng, Feng Wang, Ying Mei, Lei Tan
Figure caption: Sample spectra of four subtypes of carbon stars from LAMOST. The spectrum in the top-left corner represents a C–H star, with prominent G-band absorption lines and a red area corresponding to the P-branch band. The spectrum in the top-right corner depicts a C–R star, with red lines indicating Ca I spectral lines. The bottom-left corner displays the spectrum of a C–N star. The bottom-right corner exhibits the spectrum of a barium star, with red lines representing Ba II and Sr II spectral lines.
Paper: Identification of Carbon Stars in LAMOST DR9 Based on Deep Learning
Authors: YiMing He, Zhong Cao, Hui Deng, Feng Wang, Ying Mei, Lei Tan
Figure caption: The LAMOST spectrum of a typical carbon star sample. The features of CH molecular band at λ4300, C2 molecular bands at λ4737, λ5165, and λ5635, and CN molecular bands at λ4215, λ7065 and λ7820 are annotated in the figure.
Paper: Identification of Carbon Stars in LAMOST DR9 Based on Deep Learning
Authors: YiMing He, Zhong Cao, Hui Deng, Feng Wang, Ying Mei, Lei Tan
Figure caption: The LAMOST spectra of the four carbon stars classified as UNKNOWN. The prominent carbon features in these stars are indicated by red dashed lines.
Paper: Identification of Carbon Stars in LAMOST DR9 Based on Deep Learning
Authors: YiMing He, Zhong Cao, Hui Deng, Feng Wang, Ying Mei, Lei Tan
Figure caption: The structure of the model.
Paper: Identification of Carbon Stars in LAMOST DR9 Based on Deep Learning
Authors: YiMing He, Zhong Cao, Hui Deng, Feng Wang, Ying Mei, Lei Tan
Figure caption: The confusion matrix of the model.
Paper: Identification of Carbon Stars in LAMOST DR9 Based on Deep Learning
Authors: YiMing He, Zhong Cao, Hui Deng, Feng Wang, Ying Mei, Lei Tan
Figure caption: Examples of carbon stars that were unidentified.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: A maximum relative difference with respect to the reference evolutionary model for log age, effective temperature, and luminosity at TAMS, tRGB, mCHeB, eCHeB, and mIS (see Table 4) as a function of mass. Metal content changes accordingly with shape of the marker. The color of the symbol indicates the model set that gives rise to the maximum relative difference for a given M and Z.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Similar to Figure 3, but for models with convective core overshooting during the main-sequence phase. At the tRGB, the 2 M ⊙, solar-metallicity model is an outlier, with the value of ﹩\delta \,\mathrm{log}\,L﹩ noted next to the arrow.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: The Kippenhahn diagrams for 10 M ⊙, Z = 0.014 models with convective boundaries computed using PM (top) and CPM schemes (bottom panel). The left panels illustrate full evolution, from ZAMS until AGB ascent, while the right panels show zoomed-in views illustrating the development of thin convective shells at the end of main-sequence evolution. Convective regions are marked with green hatched areas. Blue shaded areas indicate regions of strong nuclear burning, with efficiency color coded (scale on the right side).
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Left panel: the H-R diagram with evolutionary tracks for the 10 M ⊙, Z = 0.014 model computed under various assumptions as given in the key. Right panel: zoomed in around the Henyey hook, with circles marking the appearance of the first thin convective shell.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks with different numerical resolution controls for 5 and 11 M ⊙ and solar metallicity. Labels are defined in Table 2.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Evolutionary tracks of the reference models without convective core overshooting (blue) and with convective core overshooting during the main-sequence phase (orange). Mass and metal contents change in rows and columns, respectively.
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Evolutionary tracks for 2, 5, and 8 M ⊙ and metal contents Z = 0.014, 0.004, and 0.0014. Reference tracks are shown in blue and all other ones in gray.
Paper: A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys
Authors: Shaohua Zhang, 少华 张, Zhijian Luo, 智坚 罗, Xiheng Shi, 习珩 史, Chenggang Shu, 成钢 束, Hubing Xiao, 胡兵 肖, Hongyan Zhou, 宏岩 周
Figure caption: The 1 × 1 arcmin2 finding chart of F08449+2332 extracted from the SDSS gri composite image. The IRAS object names are presented in the bottom left-hand corner. The finding chart centered on the IRAS source position. North is up, and the east is to the left-hand side. The ellipses represent 1, 2, and 3σ positional uncertainties, and the red cross denotes the WISE counterpart. Two SDSS counterparts (SDSS J084750.17+232108.6 and SDSS J084750.26+232110.9) in the SDSS are marked by the squares, who positional separation is only 2.″5, less than the angular resolution of WISE.
Paper: A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys
Authors: Shaohua Zhang, 少华 张, Zhijian Luo, 智坚 罗, Xiheng Shi, 习珩 史, Chenggang Shu, 成钢 束, Hubing Xiao, 胡兵 肖, Hongyan Zhou, 宏岩 周
Figure caption: Finding charts of the 285 ULIRGs. The 2.5 × 2.5 arcmin2 finding charts extracted from the SDSS gri composite images are centered on the IRAS sources’ positions. Other features are the same as in Figure 5, where north is up, east is to the left-hand side, and the ellipses represent 1, 2, and 3σ positional uncertainties. The square and red crosses represent the SDSS counterpart and the WISE sources within the 3σ error ellipse, respectively. For F111388+0108, the scale of the image is ﹩5\times 5\,{\mathrm{arcmin}}^{2}﹩.
Paper: A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys
Authors: Shaohua Zhang, 少华 张, Zhijian Luo, 智坚 罗, Xiheng Shi, 习珩 史, Chenggang Shu, 成钢 束, Hubing Xiao, 胡兵 肖, Hongyan Zhou, 宏岩 周
Figure caption: The infrared luminosities of the primary ULIRG candidates vs. redshift. The primary candidates’ redshift and infrared luminosity distributions are shown in the upper and right-hand panels, respectively. As the SDSS-III/IV depth increases, many SDSS sources at high redshift are matched, and the estimated infrared luminosity also tends to be higher.
Paper: A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys
Authors: Shaohua Zhang, 少华 张, Zhijian Luo, 智坚 罗, Xiheng Shi, 习珩 史, Chenggang Shu, 成钢 束, Hubing Xiao, 胡兵 肖, Hongyan Zhou, 宏岩 周
Figure caption: Distributions of redshift (top panel), infrared luminosity (middle panel), and flux ratio (bottom panel) of the reliable ULIRG candidates. The gray regions are the distributions of the final ULIRGs with a flux ratio larger than 50%.
Paper: A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys
Authors: Shaohua Zhang, 少华 张, Zhijian Luo, 智坚 罗, Xiheng Shi, 习珩 史, Chenggang Shu, 成钢 束, Hubing Xiao, 胡兵 肖, Hongyan Zhou, 宏岩 周
Figure caption: The distribution of the angular separation between the brightest WISE sources in the W4 band and the SDSS counterpart for each primary ULIRG candidate. The size of each bin of the histogram is 2″.
Paper: A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys
Authors: Shaohua Zhang, 少华 张, Zhijian Luo, 智坚 罗, Xiheng Shi, 习珩 史, Chenggang Shu, 成钢 束, Hubing Xiao, 胡兵 肖, Hongyan Zhou, 宏岩 周
Figure caption: The number distribution of WISE counterparts for each primary ULIRG candidate. These primary candidates have eight WISE counterparts within 3σ error ellipse on average.
Paper: A Comparative Study of Ultraluminous Infrared Galaxies in the IRAS and SDSS Surveys
Authors: Shaohua Zhang, 少华 张, Zhijian Luo, 智坚 罗, Xiheng Shi, 习珩 史, Chenggang Shu, 成钢 束, Hubing Xiao, 胡兵 肖, Hongyan Zhou, 宏岩 周
Figure caption: Distribution of the primary ULIRG candidates in equatorial coordinates (map centered at R.A. = 8 hr).
Paper: Toward a Comprehensive Grid of Cepheid Models with MESA. I. Uncertainties of the Evolutionary Tracks of Intermediate-mass Stars
Authors: O. Ziółkowska, R. Smolec, A. Thoul, E. Farrell, R. Singh Rathour, V. Hocdé
Figure caption: Tracks for 2–8 M ⊙ (rows) and Z = 0.014, 0.004, and 0.0014 (columns) and different resolution settings (line style and color) as in Table 2.