adsabs/AstroCLIMB huggingface dataset:
Paper: The Breakthrough Listen Search for Intelligent Life: Detection and Characterization of Anomalous Transits in Kepler Lightcurves
Authors: Anna Zuckerman, James R. A. Davenport, Steve Croft, Andrew Siemion, Imke de Pater
Figure caption: Demonstration of the thresholds used for flagging fit transit parameters for an example planet (Kepler-696b). Each data point represents one transit.
Paper: The Breakthrough Listen Search for Intelligent Life: Detection and Characterization of Anomalous Transits in Kepler Lightcurves
Authors: Anna Zuckerman, James R. A. Davenport, Steve Croft, Andrew Siemion, Imke de Pater
Figure caption: Kepler-40b transit 201 is barely above the threshold for flagging, and consistent with contamination from stellar variability.
Paper: The Breakthrough Listen Search for Intelligent Life: Detection and Characterization of Anomalous Transits in Kepler Lightcurves
Authors: Anna Zuckerman, James R. A. Davenport, Steve Croft, Andrew Siemion, Imke de Pater
Figure caption: Kepler-40b transit 201 and Kepler-548b transit 132 are flagged for large TTVs and pass the visual inspection of the fit.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: Sky coverage vs. observation frequency for key SETI projects conducted to date (modified from Figure 5 of Ng et al. 2022). The color scale represents three levels of detectability for a 1013 W Arecibo-like transmitter emitting a 1 Hz wide technosignature. Blue represents low sensitivity, in which the transmitter must be within 5 pc from Earth; yellow represents medium sensitivity, corresponding to a transmitter 25 pc away; and red represents high sensitivity, enabling detection of a source at a distance of 75 pc.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: The anticipated rate of observation for sources over the duration of the COSMIC SETI program in comparison with current programs on MeerKAT, the Murriyang telescope, and the GBT. The VLA data consist of recorded information from the VLA Low Band Ionospheric and Transient Experiment (Clarke et al. 2016, 2018) and are used to simulate future observations, including commensal operation with VLASS.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: A high-level diagram of the data flow from the VLA antennas in the context of COSMIC. The signals from each antenna pass through the receivers, and in the 8 bit mode (the VLA can operate in both a 3 bit and an 8 bit mode), all received frequencies are shifted to the X band (8–10 GHz; upper sideband). COSMIC receives one copy of the digitized signals after they are amplified through an EDFA. The other copy is processed through the WIDAR correlator for standard VLA processing.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: The signal attenuators, amplifiers, and splitters installed for the COSMIC system in the VLA WIDAR correlator room. All of them are labeled with their corresponding antenna numbers.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: Histograms of pixel-wise bolometric luminosity surface density ﹩{{\rm{\Sigma }}}_{{L}_{\mathrm{bol}}}﹩ from the center (yellow), diffuse component (red), and H II regions (blue) for each of our targets. The median ﹩{{\rm{\Sigma }}}_{{L}_{\mathrm{bol}}}﹩ for H II regions (vertical blue line) remains roughly consistent between targets. The vertical dashed line shows the estimated Eddington luminosity surface density in star-forming regions, scaled from ﹩{{ \mathcal F }}_{{L}_{\mathrm{bol}}}﹩ to ﹩{{\rm{\Sigma }}}_{{L}_{\mathrm{bol}}}﹩ units for direct comparison.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: The PDFs of gas column density N(H) in diffuse regions (hatched red) derived from 7.7 μm intensities (Equations (13) and (14)) for each galaxy. Lognormal fits to each of the PDFs with the fit means are overlaid in black for comparison. The best-fit lognormal mean N(H) (μ  N ) and dispersion (σ  N ) are included, as in Table 2.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: NGC 1566 at 21 μm with all VLT/MUSE-identified H II regions outlined in blue (top), with the corresponding PDF (middle) and log-PDF in intensity (bottom). A few of the largest H II regions in NGC 1566 are highlighted in green. The overall pdf and log-PDF of intensities at 21 μm (black), from all H II regions (blue), and each of the highlighted individual H II regions (green) are shown for comparison.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: Stacked PDFs of emission from “diffuse” regions normalized by mean intensity and amplitude at 7.7 and 21 μm. The widths of the PDFs remain consistent across targets, with the exception of NGC 1300 with a broad PDF.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: Summarizing the fractional variation in diffuse column density PDF mean (μ  N ) and dispersion (σ  N ) and in diffuse F770W emission PDF mean (μ) and dispersion (σ).
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: The PDFs of I F770W across different resolutions from native F770W (0.″269) down to 8.″0 for each target. The PDFs are colored by the FWHM of the Gaussian PSF at each resolution. With lower resolution, the overall PDFs become narrower and shift to lower intensities.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: The PDFs of N(H) across different resolutions from native F770W (0.″269) down to 8.″0 for each target. The PDFs are colored by the FWHM of the Gaussian PSF at each resolution. With lower resolution, the overall PDFs become narrower and shift to lower column densities.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: Stellar metallicity with respect to planetary (minimum) mass (﹩{M}_{{\rm{p}}}\,\sin \,i\lt 13\,{M}_{\mathrm{Jup}}﹩). The red circles (both filled and empty circles) correspond to planet-hosting giant stars, and the gray dots correspond to dwarf stars. Giant stars with stellar radius below and above 8 R ☉ (see Figure 12) are indicated in red empty and filled circles, respectively, and their sizes are proportional to the stellar mass. It is worth noting that giants with radius >21 R ☉ are excluded in this figure because the planets around them might be masqueraded by stellar intrinsic variability (see next section). The top and right panels show histograms of planetary mass and stellar metallicity, respectively. An evident transition at ∼4 M Jup can be found within the histogram of giants in the top panel. The thick dashed line in gray denotes a possible limit for giant stars in the metallicity–mass plane.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: Comparison of the evolved stellar binaries with giant planets orbiting giant stars. Left panel: Eccentricity-period distribution. The light blue, green, and purple circles denote the evolved systems with the primary star settling on the RC, 2RC, and RGB phases, respectively. The vertical dashed line denotes the 1034 day baseline of Gaia DR3. The period of planets is restricted to 50 – 2000  days to match the period distribution of stellar binaries. Middle panel: Histogram of eccentricity distribution. Right panel: Cumulative distribution. The legend shows the p-values between planets and stellar binaries. The eccentricity distribution of planets orbiting giant stars is similar to RC. The data of evolved stellar binaries are compiled from Appendix B of Beck et al. (2023).
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: Stellar radius with respect to planetary semimajor axis. The circles represent currently known evolved systems. The size and color of the circles are scaled by planetary (minimum) mass and stellar metallicity, respectively. The oblique dashed lines indicate the ratios of the semimajor axis to the stellar radius. The horizontal and vertical cyan lines denote R ⋆ = 15 R ☉ and a = 2.5  au, respectively.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: The diagnostic plot of HD 112570 (left panel) and HD 154391 (right panel). (a) Collapsed échelle diagram. (b) Echelle diagram. (c) Power spectrum, selected as a range of 3Δν around ﹩{\nu }_{\max }﹩ after subtracting the background. (d) Autocorrelation function resulting from autocorrelation function (ACF) analysis of the power spectrum. In both (a) and (b), the green dashed line indicates the radial mode ridge. In (b) and (c), the green dashed line represents ﹩{\nu }_{\max }﹩. In (d), the two red dashed lines correspond to the positions of Δν and twice Δν, from left to right.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: Left panel: Eccentricity vs. semimajor axis (a < 10 au) for known giant planets (﹩{M}_{{\rm{p}}}\,\sin \,i\gt 0.1\,{M}_{\mathrm{Jup}}﹩) around dwarf and giant stars. Right panel: Planetary (minimum) mass vs. semimajor axis. HD 112570 b and HD 154391 b are marked by blue and green diamonds. The gray dots and red circles correspond to dwarf and giant hosts, respectively. We also show five substellar companions with orbits at the widest separation. HD 154391 b has one of the longest orbital periods among known planets orbiting evolved stars. All the data points are compiled from the exoplanet.eu (Schneider et al. 2011) and NASA exoplanet archive (Akeson et al. 2013). Data acquisitions on 2023 April 2.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: Light curves of HD 112570 (left panel) and HD 154391 (right panel) generated by the TESS SPOC pipeline. Each panel shows the raw (top) and corrected (bottom) 2 minute cadence light curves. Additionally, a smoothed version of the light curve, obtained using a 0.1 day boxcar filter, is depicted in each subpanel with a blue curve.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: BIS and S H against RVs and 1-Keplerian fittings (O − C). HIDES-S data are shown in red circles, HIDES-F1 data are shown in red triangles and HIDES-F2 data are shown in red squares. HRS data from Xinglong are shown in blue circles.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption:  RadVel results for HD 154391. The symbols are the same as in Figure 5.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: Generalized Lomb–Scargle (GLS) periodograms for HD 154391. The symbols are the same as in Figure 4.
Paper: Chemical Homogeneity of Wide Binary Systems: An Approach from Near-Infrared Spectroscopy
Authors: Dongwook Lim, Andreas J. Koch-Hansen, Seungsoo Hong, Sang-Hyun Chun, Young-Wook Lee
Figure caption: Observed stars in the Gaia (top) and 2MASS (bottom) CMDs, together with comoving pair candidates of Jiménez-Esteban et al. (2019, gray dots). The observed stars are connected with dashed lines for each pair. The SWB 111893 pair is apart from the others because this target was selected from the catalog of Hartman & Lépine (2020, see Section 2.1). Open symbols indicate the stars for which chemical abundance measurements were not feasible. In the case of the SVO 2357 pair, spectral analysis was only available for the SVO 2357a star. The vertical magenta dotted line in each panel represents the approximate limit for the detailed chemical abundance measurements from the NIR spectroscopy (BP − RP = 0.65 and J − K  s  = 0.3).
Paper: Chemical Homogeneity of Wide Binary Systems: An Approach from Near-Infrared Spectroscopy
Authors: Dongwook Lim, Andreas J. Koch-Hansen, Seungsoo Hong, Sang-Hyun Chun, Young-Wook Lee
Figure caption: Target stars on a Kiel diagram, together with wide binaries of Hawkins et al. (2020, magenta squares). Our sample pairs share similar T eff and ﹩\mathrm{log}g﹩ parameters between the component stars, which are comparable to the samples of Hawkins et al. (2020). In particular, the two stars of the SVO 3206 pair, which is the only subgiant pair among our samples, are located in almost the same region in this diagram.
Paper: Chemical Homogeneity of Wide Binary Systems: An Approach from Near-Infrared Spectroscopy
Authors: Dongwook Lim, Andreas J. Koch-Hansen, Seungsoo Hong, Sang-Hyun Chun, Young-Wook Lee
Figure caption: Absolute differences in [Fe/H] as a function of separation between wide binary component stars. Our samples are indicated by filled circles with vertical ±1σ error bars estimated as the squared sum of [Fe/H] measurement error for each component star. Open symbols represent the data obtained from Ramírez et al. (2019), Hawkins et al. (2020), Nelson et al. (2021), and Liu et al. (2021).
Paper: Chemical Homogeneity of Wide Binary Systems: An Approach from Near-Infrared Spectroscopy
Authors: Dongwook Lim, Andreas J. Koch-Hansen, Seungsoo Hong, Sang-Hyun Chun, Young-Wook Lee
Figure caption: Average absolute differences in three abundance groups, which are classified according to the solar abundance. Four of our samples are indicated by colored symbols, except SVO 2759, and open symbols are literature data listed in Figure 7. Solid and dashed lines are the least-squares-fitted lines for each group. These lines appear to be located above the data points because the x-axis is plotted on a log scale.
Paper: Chemical Homogeneity of Wide Binary Systems: An Approach from Near-Infrared Spectroscopy
Authors: Dongwook Lim, Andreas J. Koch-Hansen, Seungsoo Hong, Sang-Hyun Chun, Young-Wook Lee
Figure caption:  E(B − V) values for the stars of the SVO 2759 pair obtained from Schlafly & Finkbeiner (2011), Bayestar 17 (Green et al. 2018), Bayestar 19 (Green et al. 2019), and Stilism (Lallement et al. 2018). Vertical dotted lines indicate the location of each star, estimated from Gaia DR3 parallaxes. Reddening values from different sources are significantly but differently increased in front of or behind the target stars, while Schlafly & Finkbeiner (2011) do not provide 3D reddening values.
Paper: Chemical Homogeneity of Wide Binary Systems: An Approach from Near-Infrared Spectroscopy
Authors: Dongwook Lim, Andreas J. Koch-Hansen, Seungsoo Hong, Sang-Hyun Chun, Young-Wook Lee
Figure caption: [X/H] abundance ratios and their measurement error (±1σ) for each wide binary system and their differences between component stars (Δ[X/H]). The chemical abundances of 10 elements are plotted for four wide binary pairs, while 13 elements, including C, N, and O, are indicated for the SVO 3206 pair. The dotted lines in the Δ[X/H] plot indicate the value of 0.0 dex.
Paper: Chemical Homogeneity of Wide Binary Systems: An Approach from Near-Infrared Spectroscopy
Authors: Dongwook Lim, Andreas J. Koch-Hansen, Seungsoo Hong, Sang-Hyun Chun, Young-Wook Lee
Figure caption: The comparison of continuum-normalized spectra for each wide binary pair in the H- and K-band regions, including several Fe, Si, and Ni lines. Two spectra of each pair demonstrate almost identical spectral features and strength of absorption lines.