adsabs/AstroCLIMB huggingface dataset:
Paper: The Karl G. Jansky Very Large Array Local Group L-Band Survey (LGLBS)
Authors: Eric W. Koch, Adam K. Leroy, Erik W. Rosolowsky, Laura Chomiuk, Julianne J. Dalcanton, Nickolas M. Pingel, Sumit K. Sarbadhicary, Snežana Stanimirović, Fabian Walter, Haylee N. Archer, Alberto D. Bolatto, Michael P. Busch, Hongxing Chen, Ryan Chown, Harrisen Corbould, Serena A. Cronin, Jeremy Darling, Thomas Do, Jennifer Donovan Meyer, Cosima Eibensteiner, Deidre Hunter, Rémy Indebetouw, Preshanth Jagannathan, Amanda A. Kepley, Chang-Goo Kim, Shin-Jeong Kim, Timea O. Kovacs, Joshua Marvil, Eric J. Murphy, Claire E. Murray, Jürgen Ott, D.J. Pisano, Mary Putman, Daniel R. Rybarczyk, Julia Roman-Duval, Karin Sandstrom, Eva Schinnerer, Evan D. Skillman, Adam Smercina, Ioana Stelea, Jay Strader, Jiayi Sun, Devisree Tallapaneni, Elizabeth Tarantino, Vicente Villanueva, Daniel R. Weisz, Thomas G. Williams, Tony Wong
Figure caption: H I  line width maps of M31 and M33, as measured with the effective width, defined as ﹩\sigma ={I}_{{\rm{HI}}}/\sqrt{2\pi }\,{T}_{{\rm{peak}}}﹩. Each map is shown at a common physical resolution of 120 pc. Both M31 and M33 have regions of larger line widths relative to the dwarf galaxies (Figure 14), with the largest line widths in M31 likely resulting from multiple components along single sight lines from its high inclination angle (e.g., R. Braun et al. 2009; L. Chemin et al. 2009; E. W. Koch et al. 2021).
Paper: The Karl G. Jansky Very Large Array Local Group L-Band Survey (LGLBS)
Authors: Eric W. Koch, Adam K. Leroy, Erik W. Rosolowsky, Laura Chomiuk, Julianne J. Dalcanton, Nickolas M. Pingel, Sumit K. Sarbadhicary, Snežana Stanimirović, Fabian Walter, Haylee N. Archer, Alberto D. Bolatto, Michael P. Busch, Hongxing Chen, Ryan Chown, Harrisen Corbould, Serena A. Cronin, Jeremy Darling, Thomas Do, Jennifer Donovan Meyer, Cosima Eibensteiner, Deidre Hunter, Rémy Indebetouw, Preshanth Jagannathan, Amanda A. Kepley, Chang-Goo Kim, Shin-Jeong Kim, Timea O. Kovacs, Joshua Marvil, Eric J. Murphy, Claire E. Murray, Jürgen Ott, D.J. Pisano, Mary Putman, Daniel R. Rybarczyk, Julia Roman-Duval, Karin Sandstrom, Eva Schinnerer, Evan D. Skillman, Adam Smercina, Ioana Stelea, Jay Strader, Jiayi Sun, Devisree Tallapaneni, Elizabeth Tarantino, Vicente Villanueva, Daniel R. Weisz, Thomas G. Williams, Tony Wong
Figure caption: H I  integrated intensity maps of the four LGLBS dwarf galaxy targets at their native angular resolution. These maps show the wide-field extent combining CD configuration and GBT observations. The morphology of the H I varies between these four galaxies, and we highlight in WLM where we recover faint H I emission from the edge of the foreground Magellanic Stream (M. E. Putman et al. 2003).
Paper: The Karl G. Jansky Very Large Array Local Group L-Band Survey (LGLBS)
Authors: Eric W. Koch, Adam K. Leroy, Erik W. Rosolowsky, Laura Chomiuk, Julianne J. Dalcanton, Nickolas M. Pingel, Sumit K. Sarbadhicary, Snežana Stanimirović, Fabian Walter, Haylee N. Archer, Alberto D. Bolatto, Michael P. Busch, Hongxing Chen, Ryan Chown, Harrisen Corbould, Serena A. Cronin, Jeremy Darling, Thomas Do, Jennifer Donovan Meyer, Cosima Eibensteiner, Deidre Hunter, Rémy Indebetouw, Preshanth Jagannathan, Amanda A. Kepley, Chang-Goo Kim, Shin-Jeong Kim, Timea O. Kovacs, Joshua Marvil, Eric J. Murphy, Claire E. Murray, Jürgen Ott, D.J. Pisano, Mary Putman, Daniel R. Rybarczyk, Julia Roman-Duval, Karin Sandstrom, Eva Schinnerer, Evan D. Skillman, Adam Smercina, Ioana Stelea, Jay Strader, Jiayi Sun, Devisree Tallapaneni, Elizabeth Tarantino, Vicente Villanueva, Daniel R. Weisz, Thomas G. Williams, Tony Wong
Figure caption: H I  centroid velocity maps of M31 and M33 at a common physical resolution of 120 pc. The color maps are centered at the galaxy’s systemic velocity indicated by the vertical black line in each color bar and extend to ﹩\pm {V}_{{\rm{\max }}}﹩ (the maximum rotation velocity).
Paper: The Karl G. Jansky Very Large Array Local Group L-Band Survey (LGLBS)
Authors: Eric W. Koch, Adam K. Leroy, Erik W. Rosolowsky, Laura Chomiuk, Julianne J. Dalcanton, Nickolas M. Pingel, Sumit K. Sarbadhicary, Snežana Stanimirović, Fabian Walter, Haylee N. Archer, Alberto D. Bolatto, Michael P. Busch, Hongxing Chen, Ryan Chown, Harrisen Corbould, Serena A. Cronin, Jeremy Darling, Thomas Do, Jennifer Donovan Meyer, Cosima Eibensteiner, Deidre Hunter, Rémy Indebetouw, Preshanth Jagannathan, Amanda A. Kepley, Chang-Goo Kim, Shin-Jeong Kim, Timea O. Kovacs, Joshua Marvil, Eric J. Murphy, Claire E. Murray, Jürgen Ott, D.J. Pisano, Mary Putman, Daniel R. Rybarczyk, Julia Roman-Duval, Karin Sandstrom, Eva Schinnerer, Evan D. Skillman, Adam Smercina, Ioana Stelea, Jay Strader, Jiayi Sun, Devisree Tallapaneni, Elizabeth Tarantino, Vicente Villanueva, Daniel R. Weisz, Thomas G. Williams, Tony Wong
Figure caption: H I  centroid velocity maps of the four LGLBS dwarf galaxies at a common physical resolution of 120 pc. The color maps are centered at the galaxy’s systemic velocity indicated by the vertical black line in each color bar and extend to ﹩\pm {V}_{{\rm{\max }}}﹩ (the maximum rotation velocity). For IC 10, we show the velocity extent to ﹩\pm 1.5{V}_{{\rm{\max }}}﹩ to better include the velocity ranges of the H I tidal tails.
Paper: The Karl G. Jansky Very Large Array Local Group L-Band Survey (LGLBS)
Authors: Eric W. Koch, Adam K. Leroy, Erik W. Rosolowsky, Laura Chomiuk, Julianne J. Dalcanton, Nickolas M. Pingel, Sumit K. Sarbadhicary, Snežana Stanimirović, Fabian Walter, Haylee N. Archer, Alberto D. Bolatto, Michael P. Busch, Hongxing Chen, Ryan Chown, Harrisen Corbould, Serena A. Cronin, Jeremy Darling, Thomas Do, Jennifer Donovan Meyer, Cosima Eibensteiner, Deidre Hunter, Rémy Indebetouw, Preshanth Jagannathan, Amanda A. Kepley, Chang-Goo Kim, Shin-Jeong Kim, Timea O. Kovacs, Joshua Marvil, Eric J. Murphy, Claire E. Murray, Jürgen Ott, D.J. Pisano, Mary Putman, Daniel R. Rybarczyk, Julia Roman-Duval, Karin Sandstrom, Eva Schinnerer, Evan D. Skillman, Adam Smercina, Ioana Stelea, Jay Strader, Jiayi Sun, Devisree Tallapaneni, Elizabeth Tarantino, Vicente Villanueva, Daniel R. Weisz, Thomas G. Williams, Tony Wong
Figure caption: Foreground Galactic H I separation in NGC 6822 using CloudClean.jl  (A. K. Saydjari & D. P. Finkbeiner 2022). We show the original GBT cube (left column), the Galactic H I–only model produced with CloudClean.jl (center column), and the NGC 6822–only cube from subtracting the Galactic model from the original (right column). The rows show a single channel at recession velocity 0 km s−1 (top row), integrated intensity (moment 0; middle row), and peak temperature (bottom row). LPI shows excellent results for separating Galactic H I foreground from NGC 6822 emission where both overlap in velocity.
Paper: Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
Authors: Jianzhao Zhou, 建召 周, Shaolan Bi, 少兰 毕, Yaguang Li, 亚光 李, Jie Yu, Tanda Li, 坦达 李, Xianfei Zhang, Lifei Ye, Mengjie Li, Liu Long, Tiancheng Sun, Yuqin Chen
Figure caption: Background fit for the representative stars. The gray line shows the observed power spectrum, while the black line represents the spectrum smoothed using a boxcar filter with a width of 3 μHz. The solid blue line indicates the result of the Markov Chain Monte Carlo fit. The red dashed line shows the fitted Gaussian envelope, the green dashed curve represents the sum of the three Harvey-like components, and the brown straight line corresponds to the white noise level.
Paper: Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
Authors: Jianzhao Zhou, 建召 周, Shaolan Bi, 少兰 毕, Yaguang Li, 亚光 李, Jie Yu, Tanda Li, 坦达 李, Xianfei Zhang, Lifei Ye, Mengjie Li, Liu Long, Tiancheng Sun, Yuqin Chen
Figure caption: Echelle diagram of TIC 141280255. The blue and green regions correspond to the intervals of l = 0 and l = 2, respectively. Blue, green, and red points represent l = 0, l = 2, and l = 1 modes. The collapsed power spectrum is normalized by dividing it by the maximum value. The two black dashed lines indicate the positions of ϵp − δν02 and ϵp, with the distance corresponding to the initial estimate of δν02.
Paper: Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
Authors: Jianzhao Zhou, 建召 周, Shaolan Bi, 少兰 毕, Yaguang Li, 亚光 李, Jie Yu, Tanda Li, 坦达 李, Xianfei Zhang, Lifei Ye, Mengjie Li, Liu Long, Tiancheng Sun, Yuqin Chen
Figure caption: Asteroseismic Hertzsprung–Russell diagram. The gray squares, triangles, and points represent dwarfs, subgiants, and red giants, respectively, from M. N. Lund et al. (2017), Y. Li et al. (2020), and M. Vrard et al. (2018). The gray crosses are from M. Li et al. (2025, in preparation). The red points represent our sample.
Paper: Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
Authors: Jianzhao Zhou, 建召 周, Shaolan Bi, 少兰 毕, Yaguang Li, 亚光 李, Jie Yu, Tanda Li, 坦达 李, Xianfei Zhang, Lifei Ye, Mengjie Li, Liu Long, Tiancheng Sun, Yuqin Chen
Figure caption: (a) ϵp vs. Δν diagram: the gray dashed line shows the model calculations, and the solid line shows the results with surface effect corrections. (b) ϵc vs. Δν diagram. The red points are our sample, while the other points are the result from M. Vrard et al. (2025). The black dashed line corresponds to the relation from T. Kallinger et al. (2012).
Paper: Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
Authors: Jianzhao Zhou, 建召 周, Shaolan Bi, 少兰 毕, Yaguang Li, 亚光 李, Jie Yu, Tanda Li, 坦达 李, Xianfei Zhang, Lifei Ye, Mengjie Li, Liu Long, Tiancheng Sun, Yuqin Chen
Figure caption: C–D diagram: the ratio δν02 vs. Δν. The purple points are MS stars (M. N. Lund et al. 2017), the green points are subgiants (Y. Li et al. 2020), the gray points are giants (T. Kallinger et al. 2012), and the red points are our sample from TESS. The gray dashed lines are the evolutionary tracks for stars with solar metallicity in the mass range of 0.8–2.2 M⊙, computed using MESA and GYRE.
Paper: Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
Authors: Jianzhao Zhou, 建召 周, Shaolan Bi, 少兰 毕, Yaguang Li, 亚光 李, Jie Yu, Tanda Li, 坦达 李, Xianfei Zhang, Lifei Ye, Mengjie Li, Liu Long, Tiancheng Sun, Yuqin Chen
Figure caption: Modified C–D diagram: the ratio δν02/Δν vs. Δν. The purple points are MS stars (M. N. Lund et al. 2017), the green points are subgiants (Y. Li et al. 2020), the light blue and gray points are RC and RGB stars (T. Kallinger et al. 2012), respectively, and the red points are our sample from TESS.
Paper: Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
Authors: Jianzhao Zhou, 建召 周, Shaolan Bi, 少兰 毕, Yaguang Li, 亚光 李, Jie Yu, Tanda Li, 坦达 李, Xianfei Zhang, Lifei Ye, Mengjie Li, Liu Long, Tiancheng Sun, Yuqin Chen
Figure caption: Power spectrum of TIC 141280255. The dark gray line represents the original power spectrum, while the blue, green, and red lines correspond to the fitted results for l = 0, l = 2, and l = 1, respectively.
Paper: Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
Authors: Jianzhao Zhou, 建召 周, Shaolan Bi, 少兰 毕, Yaguang Li, 亚光 李, Jie Yu, Tanda Li, 坦达 李, Xianfei Zhang, Lifei Ye, Mengjie Li, Liu Long, Tiancheng Sun, Yuqin Chen
Figure caption: Parameters ΔΠ, q, and δν01 vs. Δν. (a) The dipolar g-mode period spacing ΔΠ vs. the large separation Δν. (b) The coupling factor q vs. Δν. (c) The small frequency separation δν01 vs. Δν.
Paper: Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
Authors: Jianzhao Zhou, 建召 周, Shaolan Bi, 少兰 毕, Yaguang Li, 亚光 李, Jie Yu, Tanda Li, 坦达 李, Xianfei Zhang, Lifei Ye, Mengjie Li, Liu Long, Tiancheng Sun, Yuqin Chen
Figure caption: The ϵc vs. Δν diagram. (a) The evolutionary stages based on the empirical boundary from T. Kallinger et al. (2012). (b) The evolutionary stages based on ΔΠ1 from this work.
Paper: Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
Authors: Jianzhao Zhou, 建召 周, Shaolan Bi, 少兰 毕, Yaguang Li, 亚光 李, Jie Yu, Tanda Li, 坦达 李, Xianfei Zhang, Lifei Ye, Mengjie Li, Liu Long, Tiancheng Sun, Yuqin Chen
Figure caption: Histograms of the uncertainties for the measured mode frequencies (top), line widths (middle), and amplitudes (bottom) are shown, with line widths and amplitudes presented as relative uncertainties.
Paper: Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
Authors: Jianzhao Zhou, 建召 周, Shaolan Bi, 少兰 毕, Yaguang Li, 亚光 李, Jie Yu, Tanda Li, 坦达 李, Xianfei Zhang, Lifei Ye, Mengjie Li, Liu Long, Tiancheng Sun, Yuqin Chen
Figure caption: Corner diagram of the posterior distributions of TIC 141280255 by fitting mixed modes.
Paper: Identifying Carbon Star Candidates from LAMOST DR11 and SDSS DR18 Based on a Parallel Feature Recognition Method
Authors: Lichan Zhou, 立婵 周, Jianghui Cai, 江辉 蔡, Haifeng Yang, 海峰 杨, Ali Luo, 阿理 罗, Yinbi Li, 荫碧 李, Chenhui Shi, 晨辉 史, Boyu Zhang, 博宇 张, Jianing Tian, 佳宁 田, Yinan Yuan, 艺楠 员, Yuqing Yang, 雨晴 杨
Figure caption: Spectra of four types of carbon stars from LAMOST (L. Li et al. 2024), containing a Ba star, C-H star, C-N star, and C-R star. Carbon molecular bands (C2, CN) are a common feature of these carbon stars. Besides, spectra of each type of them show various features: Ba star: Ba II line at 4554 Å and Sr II line at Å are marked by green lines; C-H star: G band at 4300 Å and P-branch at 4342 Å are labeled with text, respectively, and Ba II line at 4554 Å and 6496 Å are marked by green lines; C-N star: weak flux at λ < 4000 Å and even λ < 5000 Å are marked in the spectra; C-R star: we highlight the Ca I line at 4226 Å.
Paper: Identifying Carbon Star Candidates from LAMOST DR11 and SDSS DR18 Based on a Parallel Feature Recognition Method
Authors: Lichan Zhou, 立婵 周, Jianghui Cai, 江辉 蔡, Haifeng Yang, 海峰 杨, Ali Luo, 阿理 罗, Yinbi Li, 荫碧 李, Chenhui Shi, 晨辉 史, Boyu Zhang, 博宇 张, Jianing Tian, 佳宁 田, Yinan Yuan, 艺楠 员, Yuqing Yang, 雨晴 杨
Figure caption: Carbon stars identification based on parallel feature recognition. It consists of two parts. Part 1: feature recognition based on parallel interval representation methods. It includes data parallelism and computing parallelism. The blue module represents data parallelism. It contains n nodes, and each node is equipped with four accelerate units. The spectra are evenly distributed to these accelerate units of each node for parallel computation. In the upper-right corner, the local and global structures of the C2 and CN molecular bands on the spectrum are marked in yellow. The gray module refers to computing parallelism based on accelerate units. It distributes data in seven regions of data of the C2 and CN molecular bands to multiple threads on a single accelerate unit for parallelly constructing intervals, thereby improving efficiency. The intervals obtained by each thread are concatenated to obtain the interval features of the spectrum. Through the parallel computing intervals using multiple nodes with multiple accelerate units, the interval features of all spectra are obtained. Part 2: carbon stars identification based on KNN classification model. It mainly contains candidate classification by KNN classification and crossmatching with current catalogs to obtain final carbon star candidates.
Paper: Identifying Carbon Star Candidates from LAMOST DR11 and SDSS DR18 Based on a Parallel Feature Recognition Method
Authors: Lichan Zhou, 立婵 周, Jianghui Cai, 江辉 蔡, Haifeng Yang, 海峰 杨, Ali Luo, 阿理 罗, Yinbi Li, 荫碧 李, Chenhui Shi, 晨辉 史, Boyu Zhang, 博宇 张, Jianing Tian, 佳宁 田, Yinan Yuan, 艺楠 员, Yuqing Yang, 雨晴 杨
Figure caption: The number of carbon star subclasses. (a) The carbon stars from LAMOST DR11. Blue shows the number of old carbon stars. And the number of new carbon stars identified is marked in gray. (b) The carbon stars from SDSS DR18. Blue shows the number of old carbon stars. And the number of new carbon stars identified is marked in orange.
Paper: A Metallicity Catalog of Very Metal-poor Main-sequence Turn-off and Red Giant Stars from LAMOST DR10
Authors: Xiangyu Li, Huiling Chen, Yang Huang, Huawei Zhang, Timothy C. Beers, Linxuan Zhu, Jifeng Liu
Figure caption: Top row: comparison of metallicities (left) and CaT EWs (right) estimated by Method 1 with results from Gaia RVS spectroscopy. Second row: comparison with spectroscopic surveys such as APOGEE DR17 (left) and GALAH DR3 (right). Third row: comparison with metal-poor samples from high-resolution spectroscopy such as PASTEL and SAGA (left) and H. Li et al. (2022) (right). Bottom row: comparison with metallicity catalogs from M. Xiang et al. (2019) (left) and C. Wang et al. (2022) (right). The number of matches (n), median offset (μ), and standard deviation (σ) of [Fe/H] and ΣCa are shown at the top of each panel. The orange lines represent the 1:1 line.
Paper: A Metallicity Catalog of Very Metal-poor Main-sequence Turn-off and Red Giant Stars from LAMOST DR10
Authors: Xiangyu Li, Huiling Chen, Yang Huang, Huawei Zhang, Timothy C. Beers, Linxuan Zhu, Jifeng Liu
Figure caption: Left: comparison of the sum of the EWs of three CaT lines, W8500 + W8544 + W8664, for the high-SNR VMP sample using the Gaussian-fitting method and direct integration method. Right: comparison of two definitions of ΣCa: the sum of the three lines W8500 + W8544 + W8664, and 1.24 times the sum of the last two lines 1.24 × (W8544 + W8664). The number of samples (n), median offset (μ), and standard deviation (σ) are shown at the top. The orange line represents the 1:1 line.
Paper: A Metallicity Catalog of Very Metal-poor Main-sequence Turn-off and Red Giant Stars from LAMOST DR10
Authors: Xiangyu Li, Huiling Chen, Yang Huang, Huawei Zhang, Timothy C. Beers, Linxuan Zhu, Jifeng Liu
Figure caption: Color–magnitude diagram of stars in LAMOST DR10. The black rectangle indicates our empirical cut for MSTO and red giant stars, defined by 0.4 < GBP − GRP < 1.6 and −4.0 < MG < 6.5. The blue data points represent the full stellar sample from LAMOST DR10, while the orange data points represent the VMP stars identified by Method 1. These stars exhibit a good agreement with the PARSEC isochrone for [Fe/H] = −2.0 and an age of 10 Gyr, shown as the red-dotted line.
Paper: A Metallicity Catalog of Very Metal-poor Main-sequence Turn-off and Red Giant Stars from LAMOST DR10
Authors: Xiangyu Li, Huiling Chen, Yang Huang, Huawei Zhang, Timothy C. Beers, Linxuan Zhu, Jifeng Liu
Figure caption: Normalized spectra and fitted CaT lines for four example stars in this work. OBSID stands for LAMOST DR10 unique spectrum ID. These examples cover the main range of metallicities and SNRs of our samples. The blue line represents the normalized spectra, and the orange line represents the fitted CaT lines.
Paper: A Metallicity Catalog of Very Metal-poor Main-sequence Turn-off and Red Giant Stars from LAMOST DR10
Authors: Xiangyu Li, Huiling Chen, Yang Huang, Huawei Zhang, Timothy C. Beers, Linxuan Zhu, Jifeng Liu
Figure caption: The correlation between metallicity and the CaT index, Gaia BP − RP color (left), and surface gravity (right). The metallicities are estimated by Method 1, while the surface gravity values are estimated by LASP. This color map shows that metallicity has a strong relationship with the CaT index, Gaia BP − RP color, and surface gravity.
Paper: A Metallicity Catalog of Very Metal-poor Main-sequence Turn-off and Red Giant Stars from LAMOST DR10
Authors: Xiangyu Li, Huiling Chen, Yang Huang, Huawei Zhang, Timothy C. Beers, Linxuan Zhu, Jifeng Liu
Figure caption: Left: distribution of the VMP sample in Galactic coordinates. The red-dashed line represents the celestial equator. This VMP sample covers a large area of the sky in the Northern Hemisphere. Right: distribution of the magnitudes of the VMP sample. More than 7000 stars in this VMP catalog are brighter than G ∼ 16.
Paper: A Metallicity Catalog of Very Metal-poor Main-sequence Turn-off and Red Giant Stars from LAMOST DR10
Authors: Xiangyu Li, Huiling Chen, Yang Huang, Huawei Zhang, Timothy C. Beers, Linxuan Zhu, Jifeng Liu
Figure caption: The MCMC result for the coefficients in Equation (2). The values at the top of the columns represent the median offset and 1σ standard deviation of the coefficients. This figure shows good fitting results, indicating that the coefficients are reliable.
Paper: A Metallicity Catalog of Very Metal-poor Main-sequence Turn-off and Red Giant Stars from LAMOST DR10
Authors: Xiangyu Li, Huiling Chen, Yang Huang, Huawei Zhang, Timothy C. Beers, Linxuan Zhu, Jifeng Liu
Figure caption: Top row: comparison between metallicities estimated by Method 1 and Method 2 (left) and comparison between metal-poor samples from Method 2 and Gaia RVS spectroscopy (right). Second row: comparison with spectroscopic surveys such as APOGEE DR17 (left) and GALAH DR3 (right). Third row: comparison with metal-poor samples from high-resolution spectroscopy such as PASTEL and SAGA (left) and H. Li et al. (2022) (right). Bottom row: comparison with metallicity catalogs from M. Xiang et al. (2019) (left) and C. Wang et al. (2022) (right). The number of matches (n), median offset (μ), and standard deviation (σ) of [Fe/H] are shown at the top of each panel. The orange lines represent the 1:1 line.
Paper: A Metallicity Catalog of Very Metal-poor Main-sequence Turn-off and Red Giant Stars from LAMOST DR10
Authors: Xiangyu Li, Huiling Chen, Yang Huang, Huawei Zhang, Timothy C. Beers, Linxuan Zhu, Jifeng Liu
Figure caption: Top row: the [Ca/Fe] distribution of metal-poor stars in this work using measurements from APOGEE (left) and GALAH (right). Bottom row: the distribution of [Fe/H] measured in this work vs. the [Ca/Fe] measured by APOGEE (left) and GALAH (right).
Paper: The Karl G. Jansky Very Large Array Local Group L-Band Survey (LGLBS)
Authors: Eric W. Koch, Adam K. Leroy, Erik W. Rosolowsky, Laura Chomiuk, Julianne J. Dalcanton, Nickolas M. Pingel, Sumit K. Sarbadhicary, Snežana Stanimirović, Fabian Walter, Haylee N. Archer, Alberto D. Bolatto, Michael P. Busch, Hongxing Chen, Ryan Chown, Harrisen Corbould, Serena A. Cronin, Jeremy Darling, Thomas Do, Jennifer Donovan Meyer, Cosima Eibensteiner, Deidre Hunter, Rémy Indebetouw, Preshanth Jagannathan, Amanda A. Kepley, Chang-Goo Kim, Shin-Jeong Kim, Timea O. Kovacs, Joshua Marvil, Eric J. Murphy, Claire E. Murray, Jürgen Ott, D.J. Pisano, Mary Putman, Daniel R. Rybarczyk, Julia Roman-Duval, Karin Sandstrom, Eva Schinnerer, Evan D. Skillman, Adam Smercina, Ioana Stelea, Jay Strader, Jiayi Sun, Devisree Tallapaneni, Elizabeth Tarantino, Vicente Villanueva, Daniel R. Weisz, Thomas G. Williams, Tony Wong
Figure caption: Measured H I intensity (left panel), column density (center panel), and mass per beam sensitivity (right panel) using observations of our central IC 10 pointing. Each color corresponds to a different array configuration or combination of array configurations (see the legend). The points connected by lines for each color show the effect of varying the weighting scheme used to grid the data (from uniform, through robust with Briggs parameter −2 to 2, to natural weighting). The left panel shows the rms noise for 21 cm intensity in an individual Δv = 0.4 km s−1 channel. The middle panel shows the implied column density sensitivity given the measured noise and integrating over a 10 km s−1 width. The right panel shows the mass sensitivity per beam, also assuming a 10 km s−1 velocity integration window. The gray dashed lines in the left and center panels indicate the expectation from statistical averaging of a constant noise map. Deviations from this reflect the loss of sensitivity when fewer baselines are included at coarse resolution. The solid gray lines in the center panel note the target resolution and sensitivity goals for the survey at the finest (4﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 at 7 × 1019 cm−2) and coarsest (48﹩\mathop{.}\limits^{\unicode{x02033}}﹩6 at 6 × 1018 cm−2) scales. We reach within ∼20% of the target sensitivity at 4﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 and moderately exceed the target sensitivity at 48﹩\mathop{.}\limits^{\unicode{x02033}}﹩6.