adsabs/AstroCLIMB huggingface dataset:
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: The Hα emission profiles of stars selected from the LAMOST MRS DR7 database with various morphological features. (a) J000003.86+635429.6 with a single emission peak, (b) J011902.35+581920.2 with symmetric double emission peaks, (c) J021126.95+575606.1, and (d) J023542.54+503801.6 with a narrow emission peak superimposed on top of an absorption profile.
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: The left panel plots the distribution of the number of observations for the full sample of 334 CBe stars found from the LAMOST MRS DR7 database, and the right panel plots the distribution of the observational baseline (ΔMJD = MJDmax – MJDmin) of the sample stars. The full sample is shown by the solid bar, and the 183 new detections are shown by hatched bars.
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: The Hα emission profiles superimposed with an absorption shell line identified from the LAMOST MRS DR7 database. (a) J000025.64+623946.1 (Type 1), (b) J011341.79+590557.3 (Type 2), (c) J021815.09+571016.0 (Type 3), and (d) J052101.98+280757.3 (Type 3).
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: The Hα absorption profiles superimposed with a shell line identified from the LAMOST MRS DR7 database. (a) J051301.34+393000.7 (Type 1), (b) J000237.33+582833.3 (Type 2), and (c) J033334.11+493245.1 (Type 3).
Paper: Three-month Monitoring of the Variability toward W51 IRS2 with Ammonia, Water, and Methanol Transitions
Authors: Yan-Kun Zhang, Xi Chen, Andrej M. Sobolev, Zhi-Qiang Shen, Bin Li, Zhang Zhao
Figure caption: Left three panels: comprehensive statistical diagrams for all the nonmetastable (upper two panels) and metastable (lower panel) NH3 quasi-thermal transitions that show decreases in their integrated intensities from mid-March to April 1 during the monitoring. The nonmetastable NH3 transitions are further divided into two groups, depending on the differences between the two quantum numbers of J and K, i.e., J − K ≠ 1 (upper panel) and J − K = 1 (central panel). Middle two panels: comprehensive statistical diagrams for some para-NH3 quasi-thermal transitions that show increases in their integrated intensities from mid-March to April 1. For the left and middle panels, a 3σ integrated intensity is drawn as a downward arrow if the transition is not detected at a specific epoch. Right two panels: statistical histograms for the ammonia quasi-thermal transitions with increases (upper panel) and decreases (lower panel) in the integrated intensities from mid-March to April 1.
Paper: Three-month Monitoring of the Variability toward W51 IRS2 with Ammonia, Water, and Methanol Transitions
Authors: Yan-Kun Zhang, Xi Chen, Andrej M. Sobolev, Zhi-Qiang Shen, Bin Li, Zhang Zhao
Figure caption: Diagrams of the variability of the peak flux density in different methanol maser transitions during the four-epoch monitoring. The 3 rms is drawn as a red downward arrow if the transitions are not detected at a specific epoch. For maser transitions with a single peak, the variability diagram is presented with blue dotted lines; for maser transitions with multiple peaks detected, the variability diagram is presented with dotted lines in multiple colors to distinguish them.
Paper: Three-month Monitoring of the Variability toward W51 IRS2 with Ammonia, Water, and Methanol Transitions
Authors: Yan-Kun Zhang, Xi Chen, Andrej M. Sobolev, Zhi-Qiang Shen, Bin Li, Zhang Zhao
Figure caption: Diagrams of the variability of the peak flux density in different ammonia maser transitions during the four-epoch monitoring. The 3 rms is drawn as a red downward arrow if the transitions are not detected at a specific epoch. For maser transitions with a single peak detected, the variability diagram is presented with blue dotted lines; for maser transitions with multiple peaks detected, the variability diagram is presented with dotted lines in different colors to distinguish them.
Paper: Three-month Monitoring of the Variability toward W51 IRS2 with Ammonia, Water, and Methanol Transitions
Authors: Yan-Kun Zhang, Xi Chen, Andrej M. Sobolev, Zhi-Qiang Shen, Bin Li, Zhang Zhao
Figure caption: A diagram of the variability of the five main velocity components in the 22.235 GHz H2O maser spectra shown in Figure 3.
Paper: Three-month Monitoring of the Variability toward W51 IRS2 with Ammonia, Water, and Methanol Transitions
Authors: Yan-Kun Zhang, Xi Chen, Andrej M. Sobolev, Zhi-Qiang Shen, Bin Li, Zhang Zhao
Figure caption: Diagrams of the variability of the integrated intensity of the CH3OH transitions detected during the four-epoch observations. The 3σ integrated intensity is drawn as a downward arrow if the transition was not detected at a specific epoch. The upper panel shows transitions with increasing integrated intensity from mid-March to April 1, while the lower panel shows transitions with decreasing integrated intensity over that period.
Paper: Three-month Monitoring of the Variability toward W51 IRS2 with Ammonia, Water, and Methanol Transitions
Authors: Yan-Kun Zhang, Xi Chen, Andrej M. Sobolev, Zhi-Qiang Shen, Bin Li, Zhang Zhao
Figure caption: The upper panel shows the H2O maser spectra detected during the four-epoch observations with TMRT toward W51 IRS2. The lower panel shows a spectrogram of the H2O maser features for the four-epoch observations to compare the maser variability.
Paper: Three-month Monitoring of the Variability toward W51 IRS2 with Ammonia, Water, and Methanol Transitions
Authors: Yan-Kun Zhang, Xi Chen, Andrej M. Sobolev, Zhi-Qiang Shen, Bin Li, Zhang Zhao
Figure caption: The NH3 spectra extracted from Figures 1–5 in Henkel et al. (2013), which shows the maser component at a velocity of 45 km s−1 detected from 1995 to 2012 by the 100 m Effelsberg Telescope toward W51 IRS2. Notably, the (12, 12) and (9, 9) ammonia transitions detected in their work are beyond our K-band monitoring.
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: The distribution of measured EW values for 286,501 spectra from Hα λ6565 and the Mg I b triplet ( ∼ λ5200) are shown by the black cross. A sample of 261,647 early-type stellar spectra were retained by keeping stars with measured EW < 10.0 for Hα λ6565 and EW < 1.2 for the Mg I b triplet (the black cross under the red horizontal solid line). By applying a reddening-free parameter from Comerón & Pasquali (2005) using observations obtained from the 2MASS all-sky survey, we further rejected 3787 K- and M-type stars in the sample (blue cross). Our final working sample narrows down to a collection of 257,860 early-type stellar spectra.
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: The spectra of stars J023209.36+560939.5 (panel (a)) and J071536.32–001018.3 (panel (b)) were observed in the red band from the LAMOST MRS. Left panels: multiple locations of the valley pixels (blue star) and peak pixels (blue triangle) were determined from the Hα profile over the wavelength region of 6551–6579 Å. Right panels: by adopting a Bartlett window smoothing approach from Bartlett (1950), the location of the peak pixels with local maximum flux values is determined. Based on the S/N of the spectra, a window size of 15 pixels was chosen to smooth the profile over selected wavelength regions for J023209.36+560939.5, and the smoothed spectra are shown by the red line and overplotted on the observed spectrum shown in black (top-right panel). A window size of 9 pixels was selected in the case of J071536.32–001018.3 (bottom-right panel).
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: A broad representation of the morphological features for the Be candidate spectra is selected for the training sample of ResNet. The spectra included examples of single-peaked (panel (a)) and double-peaked emission profiles (panel (b)), emission profiles superimposed on the bottom of broad absorption profiles (panels (c) and (d)), and shell-line profiles (panels (e) and (f)). The valley pixels, peak pixels, and the smoothed portion of the profile are labeled on the plot in each panel in the same format as Figure 3.
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: The spectra for Be star HD 250854 (with LAMOST designation of J060334.97+221938.6) observed in both blue and red arms from LAMOST are shown in black on the top panels. The spline fits for the spectrum recorded in each arm are shown in red. The rectified spectrum for each band is shown in the bottom panel and has a continuum value about unity.
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: Example spectra for non-Be stars with Hα absorption profiles randomly selected from the sample of 257,860 as discussed in Section 3.
Paper: Long-term Multiband Near-infrared Variability of the Blazar OJ 287 during 2007–2021
Authors: Alok C. Gupta, Pankaj Kushwaha, L. Carrasco, Haiguang Xu, Paul J. Wiita, G. Escobedo, A. Porras, E. Recillas, Y. D. Mayya, V. Chavushyan, Beatriz Villarroel, Zhongli Zhang
Figure caption: Multiband NIR variability LCs of the blazar OJ 287 during 2007 December–2021 November. From bottom to top, the left panels show J-, H-, and Ks-calibrated magnitudes, respectively. The right panels show how many measurements fall into each equal bin, the widths of which are assigned through the Knuth method (Knuth 2006) and differ slightly for each band. The magenta, red, and blue vertical lines, respectively, mark the first sighting of a rather sharp NIR–optical spectral break in end May 2013 and the flux peaks of the double-peaked outbursts of the ∼12 yr QPO seen in end 2015 and mid-2019. The horizontal cyan lines mark the durations of the brightest X-ray activity phases as reported in the literature.
Paper: Long-term Multiband Near-infrared Variability of the Blazar OJ 287 during 2007–2021
Authors: Alok C. Gupta, Pankaj Kushwaha, L. Carrasco, Haiguang Xu, Paul J. Wiita, G. Escobedo, A. Porras, E. Recillas, Y. D. Mayya, V. Chavushyan, Beatriz Villarroel, Zhongli Zhang
Figure caption: DCF plots using the zDCF method between NIR J, H, and Ks bands for the total duration of observations. The time-lag and DCF values are given on the x-axis and y-axis, respectively.
Paper: Three-month Monitoring of the Variability toward W51 IRS2 with Ammonia, Water, and Methanol Transitions
Authors: Yan-Kun Zhang, Xi Chen, Andrej M. Sobolev, Zhi-Qiang Shen, Bin Li, Zhang Zhao
Figure caption: An overview of the W51A region. The TMRT beam is overlaid as a circle on a background extracted from Ginsburg et al. (2017). All the well-known subregions—including the target in this work—are labeled with arrows. The colored background is a combination of millimeter emission lines and continuum emission detected with ALMA: C18O 2−1 in blue, CH3OH 42 − 31 in orange, HC3N 24−23 in purple, and the 1.3 mm continuum in green. In addition, the Very Large Array Ku-band free–free continuum emission is shown with the white haze (Ginsburg et al. 2016).
Paper: Long-term Multiband Near-infrared Variability of the Blazar OJ 287 during 2007–2021
Authors: Alok C. Gupta, Pankaj Kushwaha, L. Carrasco, Haiguang Xu, Paul J. Wiita, G. Escobedo, A. Porras, E. Recillas, Y. D. Mayya, V. Chavushyan, Beatriz Villarroel, Zhongli Zhang
Figure caption: As in Figure 1 for the NIR color variability for the entire duration of these observations of OJ 287. The panels on the right show the spectral index histogram.
Paper: Long-term Multiband Near-infrared Variability of the Blazar OJ 287 during 2007–2021
Authors: Alok C. Gupta, Pankaj Kushwaha, L. Carrasco, Haiguang Xu, Paul J. Wiita, G. Escobedo, A. Porras, E. Recillas, Y. D. Mayya, V. Chavushyan, Beatriz Villarroel, Zhongli Zhang
Figure caption: NIR spectral index variation with time and J-band magnitude covering the entire observation period of OJ 287. The panels on the right show the spectral index histogram.
Paper: Long-term Multiband Near-infrared Variability of the Blazar OJ 287 during 2007–2021
Authors: Alok C. Gupta, Pankaj Kushwaha, L. Carrasco, Haiguang Xu, Paul J. Wiita, G. Escobedo, A. Porras, E. Recillas, Y. D. Mayya, V. Chavushyan, Beatriz Villarroel, Zhongli Zhang
Figure caption: As in Figure 3 for NIR color–magnitude plots for OJ 287.
Paper: Three-month Monitoring of the Variability toward W51 IRS2 with Ammonia, Water, and Methanol Transitions
Authors: Yan-Kun Zhang, Xi Chen, Andrej M. Sobolev, Zhi-Qiang Shen, Bin Li, Zhang Zhao
Figure caption: Rotation diagrams for the CH3OH quasi-thermal transitions detected during the four-epoch observations. The panels from top to bottom are in the order of 2020 January 8, March 20, April 1, and April 7. The blue, red, and purple straight lines represent the best fits to the methanol transitions with E  u /κ in the ranges of 20−60 K, 60−115 K, and 115−200 K, respectively. For transitions that were observed but not detected, the 3 rms value for the integrated intensity is given as a downward arrow that presents the upper limit of the integrated intensity.
Paper: Three-month Monitoring of the Variability toward W51 IRS2 with Ammonia, Water, and Methanol Transitions
Authors: Yan-Kun Zhang, Xi Chen, Andrej M. Sobolev, Zhi-Qiang Shen, Bin Li, Zhang Zhao
Figure caption: Rotation diagrams for the NH3 quasi-thermal transitions detected during the four-epoch observations. The panels from top to bottom are in the order of 2020 January 8, March 20, April 1, and April 7. The blue, red, and purple straight lines represent the best fits to the ammonia transitions with E  u /κ in the ranges of <300 K, 300−610 K, and 610−1200 K, respectively. For transitions that were observed but not detected, the 3 rms value for the integrated intensity is given as a downward arrow that presents the upper limit of the integrated intensity.
Paper: Three-month Monitoring of the Variability toward W51 IRS2 with Ammonia, Water, and Methanol Transitions
Authors: Yan-Kun Zhang, Xi Chen, Andrej M. Sobolev, Zhi-Qiang Shen, Bin Li, Zhang Zhao
Figure caption: Variations of the rotation temperatures of the NH3 (left panel) and CH3OH (right panel) with observing time. According to the division scheme of E  u /κ, the ranges of <300 K, 300−610 K, and 610−1200 K correspond to the outer, middle, and inner layers of the molecular core for the ammonia transitions, respectively. For the methanol transitions, the E  u /κ ranges of 20−60 K, 60−115 K, and 115−200 K correspond to the outer, middle, and inner layers of the molecular core, respectively.
Paper: MSWIM2D: Two-dimensional Outer Heliosphere Solar Wind Modeling
Authors: Timothy B. Keebler, Gábor Tóth, Bertalan Zieger, Merav Opher
Figure caption: Modeled solar wind speed in the ecliptic plane from 1997 May 17. Panel (a) shows the full model domain from radial distances of 1 to 75 au, while (b) has been limited to ±10 au to show detail. The circle at the center of (b) represents the inner boundary of Earth’s orbit at 1 au. Note that velocity variations follow a spiral pattern that wraps around multiple times, corresponding to a quasiperiodic behavior over multiple solar rotations. Also note that features become more diffuse toward the outer boundary (see the discussion in Section 3.2).
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: Venn diagram showing the overlap of the three selection criteria for the LzLCS: O32 = [O III]/[O II] flux ratio (top left), UV slope parameterized by spectral index β (top right), and star formation rate surface density ΣSFR (bottom center).
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: Example spatial cross section of the two-dimensional spectrum for a nonemitter (left), marginally detected LCE (center) and well-detected LCE (right) from the LzLCS. The black line represents the nonionizing starlight continuum, the gray line represents the model dark current, red line represents the LyC scaled to the same median background counts as the starlight profile, and the gray hatched stripe represents the spectral extraction aperture.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: LyC measurements (circles) and upper limits (triangles) for the combined LzLCS and published samples show the HST/COS LyC flux sensitivity limits as a function of redshift. The increase in sensitivity with redshift is due primarily to the location of the LyC on the COS detector.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: Distribution of rest-frame Hβ equivalent width (EW) values for galaxies in the LzLCS (solid) with detected LyC (dark gray) and undetected LyC (light gray). For comparison, we include the EWs for LCE candidates with published HST/COS spectra (hatched) with detected LyC (black) and undetected LyC (gray). Error bars represent the 1σ Poisson binomial uncertainty in each histogram bin.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: The same as Figure 6 but for [O III]λ5007/[O II]λ3727, 29  = O32.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: The same as Figure 6 but for ﹩12+{\mathrm{log}}_{10}({\rm{O}}/{\rm{H}})﹩.