adsabs/AstroCLIMB huggingface dataset:
Paper: MaNGA 8313-1901: Gas Accretion Observed in a Blue Compact Dwarf Galaxy?
Authors: Mengting Ju, 梦婷 居, Jun Yin, 君 尹, Rongrong Liu, 蓉蓉 刘, Lei Hao, 蕾 郝, Zhengyi Shao, 正义 邵, Shuai Feng, 帅 冯, Rogério Riffel, Chenxu Liu, 辰旭 刘, David V. Stark, Shiyin Shen, 世银 沈, Eduardo Telles, José G. Fernández-Trincado, Junfeng Wang, 俊峰 王, Haiguang Xu, 海光 徐, Dmitry Bizyaev, Yu Rong, 昱 容
Figure caption: The spectra of different components in the NE clump of MaNGA 8313-1901. In the upper panel, the observed spectrum in the NE clump is shown in light blue. The light orange line represents the estimated host component in the NE clump. The “pure” clump spectrum, i.e., the observed clump spectrum (light blue) subtracted by the estimated host spectrum (light orange), is shown in black. The yellow dashed spectrum shows the modeled clump spectrum constructed by Prospector (see the text for details). The residual of the modeled “pure” clump spectrum, i.e., the difference between the “pure” clump spectrum and the modeled one, is shown in the lower panel. The blue shaded area shows the 3σ error region of the observed spectrum.
Paper: MaNGA 8313-1901: Gas Accretion Observed in a Blue Compact Dwarf Galaxy?
Authors: Mengting Ju, 梦婷 居, Jun Yin, 君 尹, Rongrong Liu, 蓉蓉 刘, Lei Hao, 蕾 郝, Zhengyi Shao, 正义 邵, Shuai Feng, 帅 冯, Rogério Riffel, Chenxu Liu, 辰旭 刘, David V. Stark, Shiyin Shen, 世银 沈, Eduardo Telles, José G. Fernández-Trincado, Junfeng Wang, 俊峰 王, Haiguang Xu, 海光 徐, Dmitry Bizyaev, Yu Rong, 昱 容
Figure caption: The observed Hα velocity map (the left panel), the best-fit rotation model for the host galaxy (the middle panel), and the residuals (V obs − V model) of the Hα velocity field (the right panel) of MaNGA8313-1901.
Paper: MaNGA 8313-1901: Gas Accretion Observed in a Blue Compact Dwarf Galaxy?
Authors: Mengting Ju, 梦婷 居, Jun Yin, 君 尹, Rongrong Liu, 蓉蓉 刘, Lei Hao, 蕾 郝, Zhengyi Shao, 正义 邵, Shuai Feng, 帅 冯, Rogério Riffel, Chenxu Liu, 辰旭 刘, David V. Stark, Shiyin Shen, 世银 沈, Eduardo Telles, José G. Fernández-Trincado, Junfeng Wang, 俊峰 王, Haiguang Xu, 海光 徐, Dmitry Bizyaev, Yu Rong, 昱 容
Figure caption: Left: the metallicity map obtained via the R23 method. Middle: the metallicity map obtained via the direct T  e  method. Only 61 spaxels with significant O III λ4363 detections (S/N > 5) are shown. Right: the comparison between the metallicities obtained from the direct method and those obtained from the O3N2 method for the 61 spaxels in the middle panel. The red data points and the black data points represent the spaxels inside and outside the morphologically defined NE clump (the red circle in the middle panel), respectively. The gray line is the one-to-one correlation.
Paper: MaNGA 8313-1901: Gas Accretion Observed in a Blue Compact Dwarf Galaxy?
Authors: Mengting Ju, 梦婷 居, Jun Yin, 君 尹, Rongrong Liu, 蓉蓉 刘, Lei Hao, 蕾 郝, Zhengyi Shao, 正义 邵, Shuai Feng, 帅 冯, Rogério Riffel, Chenxu Liu, 辰旭 刘, David V. Stark, Shiyin Shen, 世银 沈, Eduardo Telles, José G. Fernández-Trincado, Junfeng Wang, 俊峰 王, Haiguang Xu, 海光 徐, Dmitry Bizyaev, Yu Rong, 昱 容
Figure caption: The zoomed-in spectra of the observed spectrum (the blue line), the host-component spectrum (the orange line), and the “pure” clump spectrum (the black line). From top left to bottom right, we show the D4000 absorption lines, Ca II λ3933, 3968, G4300, Mg b  λ5175, NaD λ5892, and Ca II λ8500, 8544, and emission lines Hβ and Hδ.
Paper: MaNGA 8313-1901: Gas Accretion Observed in a Blue Compact Dwarf Galaxy?
Authors: Mengting Ju, 梦婷 居, Jun Yin, 君 尹, Rongrong Liu, 蓉蓉 刘, Lei Hao, 蕾 郝, Zhengyi Shao, 正义 邵, Shuai Feng, 帅 冯, Rogério Riffel, Chenxu Liu, 辰旭 刘, David V. Stark, Shiyin Shen, 世银 沈, Eduardo Telles, José G. Fernández-Trincado, Junfeng Wang, 俊峰 王, Haiguang Xu, 海光 徐, Dmitry Bizyaev, Yu Rong, 昱 容
Figure caption: The i-band image of the HSC survey. We draw four white circles to highlight the small knots that we find.
Paper: The Mouse That Squeaked: A Small Flare from Proxima Cen Observed in the Millimeter, Optical, and Soft X-Ray with Chandra and ALMA
Authors: Ward S. Howard, Meredith A. MacGregor, Rachel Osten, Jan Forbrich, Steven R. Cranmer, Isaiah Tristan, Alycia J. Weinberger, Allison Youngblood, Thomas Barclay, R. O. Parke Loyd, Evgenya L. Shkolnik, Andrew Zic, David J. Wilner
Figure caption: X-ray to millimeter light curves of the flare aligned to the barycentric JD Chandra peak time of 2,458,609.751 (TDB). The Chandra light curve with adaptive binning is shown in panel (A). An inset image at a fixed temporal resolution of 1 min in panel (A) shows a possible increase in X-ray flux near the time of the first ALMA peak. A large increase during the X-ray decay phase correlates well with both LCOGT U-band and ALMA flux increases in panels (B) and (C). On the right, a binned X-ray light curve (D) and the median energy (E) and plasma temperature (F) are shown. Grey lines are the times of ALMA peaks.
Paper: The Mouse That Squeaked: A Small Flare from Proxima Cen Observed in the Millimeter, Optical, and Soft X-Ray with Chandra and ALMA
Authors: Ward S. Howard, Meredith A. MacGregor, Rachel Osten, Jan Forbrich, Steven R. Cranmer, Isaiah Tristan, Alycia J. Weinberger, Allison Youngblood, Thomas Barclay, R. O. Parke Loyd, Evgenya L. Shkolnik, Andrew Zic, David J. Wilner
Figure caption: While stellar flares can reach high temperatures and emission measures (EM), Chandra HETG spectra place the May 6 event squarely in the temperature–EM regime of M/X-class solar flares. Panel (A): zeroth- and first-order HETG flare spectra (black) are fit with an APEC temperature model (orange). The integrated temperature is close to the 12.8 MK median of the MASME temperatures in Figure 1. Panel (B): best-fit integrated temperature and EM compared with a range of solar and stellar flares (Osten et al. 2010, 2016; Getman et al. 2021). Dots are stellar flares, triangles are solar flares. Highlighted flares are color-coded, with gray flares being the Getman et al. (2021) main-sequence stellar flare sample. Our X1-analog is comparable to two M1.4 and X4.8 class solar flares from White et al. (2005). The Getman et al. (2021) stellar T–EM fit is shown and used to estimate the EM of our flare. Panels (C) and (D): time evolution of the flare's estimated temperature and potential EM compared with a stellar superflare (Osten et al. 2010), a typical stellar flare (Güdel et al. 2004), and two solar flares from White et al. (2005).
Paper: Direct Optimal Mapping for 21 cm Cosmology: A Demonstration with the Hydrogen Epoch of Reionization Array
Authors: Zhilei Xu, 智磊 徐, Jacqueline N. Hewitt, Kai-Feng Chen, Honggeun Kim, Joshua S. Dillon, Nicholas S. Kern, Miguel F. Morales, Bryna J. Hazelton, Ruby Byrne, Nicolas Fagnoni, Eloy de Lera Acedo, Zara Abdurashidova, Tyrone Adams, James E. Aguirre, Paul Alexander, Zaki S. Ali, Rushelle Baartman, Yanga Balfour, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, Carina Cheng, David R. DeBoer, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Randall Fritz, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Jack Hickish, Daniel C. Jacobs, Austin Julius, MacCalvin Kariseb, Joshua Kerrigan, Piyanat Kittiwisit, Saul A. Kohn, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, Anita Loots, Yin-Zhe Ma, David Harold Edward MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Tshegofalang Mosiane, Steven G. Murray, Abraham R. Neben, Bojan Nikolic, Hans Nuwegeld, Aaron R. Parsons, Nipanjana Patra, Samantha Pieterse, Jonathan C. Pober, Nima Razavi-Ghods, James Robnett, Kathryn Rosie, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter Van Van Wyngaarden, Peter K. G. Williams, Haoxuan Zheng
Figure caption: Map validation with simulated visibilities. Top: Global Sky Model (GSM08; de Oliveira-Costa et al. 2008) at 166 MHz before and after convolving with the PSF. Because of the grating lobes in the PSF (Figure 4), the convolved GSM08 looks different from the original GSM08. Middle: the DOM map from simulated visibilities before and after adding noise. Bottom: the residual maps after subtracting the convolved GSM08 from the middle row. The one without noise shows 10−7 residuals. The one with noise shows random patterns at ∼10% level. The reduced-χ 2 value (Section 4.2) is also shown in the noise residual.
Paper: Direct Optimal Mapping for 21 cm Cosmology: A Demonstration with the Hydrogen Epoch of Reionization Array
Authors: Zhilei Xu, 智磊 徐, Jacqueline N. Hewitt, Kai-Feng Chen, Honggeun Kim, Joshua S. Dillon, Nicholas S. Kern, Miguel F. Morales, Bryna J. Hazelton, Ruby Byrne, Nicolas Fagnoni, Eloy de Lera Acedo, Zara Abdurashidova, Tyrone Adams, James E. Aguirre, Paul Alexander, Zaki S. Ali, Rushelle Baartman, Yanga Balfour, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, Carina Cheng, David R. DeBoer, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Randall Fritz, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Jack Hickish, Daniel C. Jacobs, Austin Julius, MacCalvin Kariseb, Joshua Kerrigan, Piyanat Kittiwisit, Saul A. Kohn, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, Anita Loots, Yin-Zhe Ma, David Harold Edward MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Tshegofalang Mosiane, Steven G. Murray, Abraham R. Neben, Bojan Nikolic, Hans Nuwegeld, Aaron R. Parsons, Nipanjana Patra, Samantha Pieterse, Jonathan C. Pober, Nima Razavi-Ghods, James Robnett, Kathryn Rosie, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter Van Van Wyngaarden, Peter K. G. Williams, Haoxuan Zheng
Figure caption: Residual maps at 166 MHz. The figure is designed as a subtraction equation showing residuals with different components subtracted. All maps share the same sky patch and color bar range as annotated on the left map. Left column: after subtracting the convolved GLEAM catalogs (Hurley-Walker et al. 2017, 2019) from the HERA map, the residual map starts to show diffuse emission patterns. Center column: from top to bottom are convolved Global Sky Model 2008 (GSM08; de Oliveira-Costa et al. 2008), convolved Global Sky Model 2016 (GSM16; Zheng et al. 2017b), and convolved Byrne21 map (Byrne et al. 2022). GSM08 contains the two brightest point sources, while neither GSM16 nor Byrne21 contains point sources. GSM08, less so for GSM16, also shows vertical stripes. Right column: residual maps after further subtracting the GSM08, GSM16, and Byrne21 maps. Both the GSM08 and the GSM16 residuals increase the amplitude of the residual map. The morphology of their residual maps resembles that of the sky models themselves, indicating that they do not represent the observed diffuse emission. The Byrne21 map, however, shows a similar diffuse pattern as observed in the GLEAM-subtracted residual at large scales. Reduced-χ 2 values are also presented for each of the residual maps as in Table 1.
Paper: Direct Optimal Mapping for 21 cm Cosmology: A Demonstration with the Hydrogen Epoch of Reionization Array
Authors: Zhilei Xu, 智磊 徐, Jacqueline N. Hewitt, Kai-Feng Chen, Honggeun Kim, Joshua S. Dillon, Nicholas S. Kern, Miguel F. Morales, Bryna J. Hazelton, Ruby Byrne, Nicolas Fagnoni, Eloy de Lera Acedo, Zara Abdurashidova, Tyrone Adams, James E. Aguirre, Paul Alexander, Zaki S. Ali, Rushelle Baartman, Yanga Balfour, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, Carina Cheng, David R. DeBoer, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Randall Fritz, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Jack Hickish, Daniel C. Jacobs, Austin Julius, MacCalvin Kariseb, Joshua Kerrigan, Piyanat Kittiwisit, Saul A. Kohn, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, Anita Loots, Yin-Zhe Ma, David Harold Edward MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Tshegofalang Mosiane, Steven G. Murray, Abraham R. Neben, Bojan Nikolic, Hans Nuwegeld, Aaron R. Parsons, Nipanjana Patra, Samantha Pieterse, Jonathan C. Pober, Nima Razavi-Ghods, James Robnett, Kathryn Rosie, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter Van Van Wyngaarden, Peter K. G. Williams, Haoxuan Zheng
Figure caption: Full eigenvalue spectrum of C from mapping the HERA data. The eigenvalues are displaced in descending order, with blue for the positive and orange for the negative. The negative values have the absolute values at the machine-error levels, and are artificially ordered to the right side of the plot instead of scattering around zero with the positive eigenvalues. Different from Figure 6, there is not a clear cut in this eigenvalue spectrum. This is because we combined 20 time integrations in this mapping. The sky rotation adds information beyond what the same array measures at one time, smoothing the drop we saw in Figure 6. We choose to include the first 1000 eigenvectors (red-shaded region) for the reduced-χ 2 calculation.
Paper: Direct Optimal Mapping for 21 cm Cosmology: A Demonstration with the Hydrogen Epoch of Reionization Array
Authors: Zhilei Xu, 智磊 徐, Jacqueline N. Hewitt, Kai-Feng Chen, Honggeun Kim, Joshua S. Dillon, Nicholas S. Kern, Miguel F. Morales, Bryna J. Hazelton, Ruby Byrne, Nicolas Fagnoni, Eloy de Lera Acedo, Zara Abdurashidova, Tyrone Adams, James E. Aguirre, Paul Alexander, Zaki S. Ali, Rushelle Baartman, Yanga Balfour, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, Carina Cheng, David R. DeBoer, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Randall Fritz, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Jack Hickish, Daniel C. Jacobs, Austin Julius, MacCalvin Kariseb, Joshua Kerrigan, Piyanat Kittiwisit, Saul A. Kohn, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, Anita Loots, Yin-Zhe Ma, David Harold Edward MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Tshegofalang Mosiane, Steven G. Murray, Abraham R. Neben, Bojan Nikolic, Hans Nuwegeld, Aaron R. Parsons, Nipanjana Patra, Samantha Pieterse, Jonathan C. Pober, Nima Razavi-Ghods, James Robnett, Kathryn Rosie, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter Van Van Wyngaarden, Peter K. G. Williams, Haoxuan Zheng
Figure caption: Eigenvalues of C in descending order for the one-integration simulation data. A clear drop is seen around the one-hundred-and-eightieth eigenmode. Thus, we choose the first 180 eigenvalues for the figure-of-merit calculation. The red-shaded region shows the selected eigenmodes.
Paper: Direct Optimal Mapping for 21 cm Cosmology: A Demonstration with the Hydrogen Epoch of Reionization Array
Authors: Zhilei Xu, 智磊 徐, Jacqueline N. Hewitt, Kai-Feng Chen, Honggeun Kim, Joshua S. Dillon, Nicholas S. Kern, Miguel F. Morales, Bryna J. Hazelton, Ruby Byrne, Nicolas Fagnoni, Eloy de Lera Acedo, Zara Abdurashidova, Tyrone Adams, James E. Aguirre, Paul Alexander, Zaki S. Ali, Rushelle Baartman, Yanga Balfour, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, Carina Cheng, David R. DeBoer, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Randall Fritz, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Jack Hickish, Daniel C. Jacobs, Austin Julius, MacCalvin Kariseb, Joshua Kerrigan, Piyanat Kittiwisit, Saul A. Kohn, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, Anita Loots, Yin-Zhe Ma, David Harold Edward MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Tshegofalang Mosiane, Steven G. Murray, Abraham R. Neben, Bojan Nikolic, Hans Nuwegeld, Aaron R. Parsons, Nipanjana Patra, Samantha Pieterse, Jonathan C. Pober, Nima Razavi-Ghods, James Robnett, Kathryn Rosie, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter Van Van Wyngaarden, Peter K. G. Williams, Haoxuan Zheng
Figure caption: A wide-field map at 166 MHz. Observations across R.A. 1–3 h are composed for this map. This map covers 5° around the HERA zenith path. Previous examples cover the central part of this field.
Paper: Direct Optimal Mapping for 21 cm Cosmology: A Demonstration with the Hydrogen Epoch of Reionization Array
Authors: Zhilei Xu, 智磊 徐, Jacqueline N. Hewitt, Kai-Feng Chen, Honggeun Kim, Joshua S. Dillon, Nicholas S. Kern, Miguel F. Morales, Bryna J. Hazelton, Ruby Byrne, Nicolas Fagnoni, Eloy de Lera Acedo, Zara Abdurashidova, Tyrone Adams, James E. Aguirre, Paul Alexander, Zaki S. Ali, Rushelle Baartman, Yanga Balfour, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, Carina Cheng, David R. DeBoer, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Randall Fritz, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Jack Hickish, Daniel C. Jacobs, Austin Julius, MacCalvin Kariseb, Joshua Kerrigan, Piyanat Kittiwisit, Saul A. Kohn, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, Anita Loots, Yin-Zhe Ma, David Harold Edward MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Tshegofalang Mosiane, Steven G. Murray, Abraham R. Neben, Bojan Nikolic, Hans Nuwegeld, Aaron R. Parsons, Nipanjana Patra, Samantha Pieterse, Jonathan C. Pober, Nima Razavi-Ghods, James Robnett, Kathryn Rosie, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter Van Van Wyngaarden, Peter K. G. Williams, Haoxuan Zheng
Figure caption: Maps from HERA data and convolved GLEAM catalogs (Wayth et al. 2015) at 166 MHz. Left: the HERA map. Right: GLEAM catalogs (Hurley-Walker et al. 2017, 2019) convolved by the PSF. The GLEAM catalogs miss some diffuse emission in the map, especially between point sources.
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: CMD of the 109 stars used for our binarity analysis. Stars surrounded by open circles are the 32 bMS and rMS stars used for SED fitting. Gray star labels show targets discarded from the binarity analysis because of their high rotational velocities. The dotted box shows the region where 87% of stars have been analyzed spectroscopically. Single and binary stars verified by BINOCS are represented by green triangles and solid points, respectively, color coded by the derived mass ratios. Three lower-MS stars with a binarity that cannot be determined through SED fitting are marked by gray crosses. Small gray dots are other cluster member stars for which spectroscopy is not available or which lack complete photometric data in the eight prerequisite passbands.
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: (a) Histograms of the binary mass-ratio distributions of the sample objects subjected to SED fitting located within the dashed box in Figure 10 (blue dashed lines) and lower-MS stars (red dashed lines). (b) CMD of the 32 split-MS stars used for SED fitting, classified based on their derived mass ratios. The dotted box shows the same region as that in Figure 10.
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: Normalized distribution of the ﹩v\sin i﹩ of 10,000 synthetic stars (red dashed line) for a flat distribution of v within the range of 200 km s−1 and 300 km s−1 and a uniform distribution of the directions of the spin axes in a run, along with the ﹩v\sin i﹩ distribution of rMS stars (gray bars).
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: Mean synchronization timescales vs. different binary separations a/R for the 10 slowly rotating stars (﹩v\sin i\lt 100\,\mathrm{km}{\,}^{-1}﹩) located within the dotted box of Figure 10. The gray shade represents the 1σ standard deviation of the synchronization time. The dashed line indicates 90 Myr, i.e., the best-fitting age of NGC 2422.
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: (a) Selection of NGC 2422 cluster members based on their stellar proper motions (see the text for details). The inset shows the isodensity contours at ρ = 1000 yr2 mas−2 (black) and ρ = 2000 yr2 mas−2 (red) of stars within the green dashed circle. (b) Distribution of the parallaxes (ϖ) as a function of Gaia G-band magnitudes of cluster members (red dots), candidate members selected only based on proper motions (blue dots), and field stars (gray dots). The corresponding number distributions are shown using the same colors in the inset, except for the field stars. The dashed polygon encloses the ϖ range of the cluster members. The solid and dashed vertical lines in the inset show the ϖ  a  of the cluster members and the range of ϖ  a  ± σ  ϖ , respectively. (c) CMD of the member stars (red dots) and the field stars (gray dots). (d) Magnified view of the CMD within the dashed box in panel (c), where the split pattern is most evident. The left subpanel shows the mean uncertainties in the G magnitudes and G BP − G RP colors in the corresponding G magnitude ranges.
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: (a) Stellar ﹩v\sin i﹩ (including the 2σ uncertainties) vs. stellar color deviations, Δ(G BP − G RP), of the bMS, rMS, and uMS stars. The distributions of the color deviations and ﹩v\sin i﹩ are shown in the top and right panels. The double-lined spectroscopic binary system is enclosed by an open square. (b) Cumulative distributions of ﹩v\sin i﹩ for bMS and rMS stars. The two dashed vertical lines represent ﹩v\sin i=160\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩ (left) and 250 km s−1 (right), respectively.