adsabs/AstroCLIMB huggingface dataset:
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: Color light-curve metrics for observing strategies with nightly pairs in the same vs. different filters (v1.5 simulations). The baseline (reference) simulation with the default scheduler configuration for this cadence experiment is the first entry on the left. All values have been normalized by this simulation’s output. The gray shading outlines changes that are within ±5% of the baseline simulation.
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: Changing the ideal nightly pair separation (v1.7 simulations). The baseline (reference) simulation with the default scheduler configuration for this cadence experiment is the first entry on the left. All values have been normalized by this simulation’s output. The gray shading outlines changes that are within ±5% of the baseline simulation. Top: discovery metrics. Bottom: light-curve inversion metrics.
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: The impact of adding a requirement for three “good seeing” (seeing < 0.″8) images per year in various bandpasses (v2.0 simulations). The baseline (reference) simulation with the default scheduler configuration for this cadence experiment is the first entry on the left. All values have been normalized by this simulation’s output. The baseline_v2.1_10yrs includes the good seeing requirement for r and i bands as the default. The gray shading outlines changes that are within ±5% of the baseline simulation. Top: discovery metrics. Bottom: light-curve inversion metrics.
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: Investigating ways of reducing extra repeat visits and redistributing (v2.1 simulations). The baseline (reference) simulation with the default scheduler configuration for this cadence experiment is the first entry on the left. All values have been normalized by this simulation’s output. The gray shading outlines changes that are within ±5% of the baseline simulation. Top: discovery metrics. Bottom: light-curve inversion metrics.
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: Investigating ways of reducing the gaps between g-band visits over a month (v1.7 simulations). The baseline (reference) simulation with the default scheduler configuration for this cadence experiment is the first entry on the left. All values have been normalized by this simulation’s output. The gray shading outlines changes that are within ±5% of the baseline simulation. Top: discovery metrics. Bottom: light-curve inversion metrics.
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: The number of Jupiter Trojan detections (of a simulated sample population of 5000 objects) in the COSMOS DDF over the course of the baseline_v2.2_10yrs simulation. This simulation starts the LSST in 2023 October. By 7 yr into the survey, both Jupiter Trojan clouds have traversed across the COSMOS DDF.
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: Impact of various third visit scenarios (v2.0 simulations). The baseline (reference) simulation with the default scheduler configuration for this cadence experiment is the first entry on the left. All values have been normalized by this simulation’s output. The gray shading outlines changes that are within ±5% of the baseline simulation. Top: discovery metrics. Bottom: light-curve inversion metrics. We have truncated the y-axis for visibility in the light-curve inversion metrics plot. The fraction of the Jupiter Trojan detections in some of these runs compared to the baseline is lower than 0.4 and off the bottom edge.
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: Impact of various rolling cadence scenarios (v2.0 simulations). The baseline (reference) simulation with the default scheduler configuration for this cadence experiment is the first entry on the left. The baseline simulation has a two-band rolling cadence implemented with no rolling in the Galactic plane and NES. All values have been normalized by this simulation’s output. The gray shading outlines changes that are within ±5% of the baseline simulation. Top: discovery metrics. Bottom: light-curve inversion metrics. Note: The light-curve inversion plot has been truncated for clarity. The Jupiter Trojans extend beyond the plot for the six_rolling_ns6_rw0.9_v2.0_10yrs.
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: Impact of varying the time allocated to the DDFs (v2.0 simulations). The baseline (reference) simulation with the default scheduler configuration for this cadence experiment is the first entry on the left. All values have been normalized by this simulation’s output. The gray shading outlines changes that are within ±5% of the baseline simulation. Top: discovery metrics. Bottom: light-curve inversion metrics.
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: Comparison of the sky coverage with greater than 825 deg2 (in cyan) and 750 deg2 (in black) for v2.0 cadence simulations with various options for third repeat visits. The baseline (reference) simulation with the default scheduler configuration for this cadence experiment is the first entry on the left.
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: Snapshot of the cumulative number of on-sky visits in all filters as a function of a subset of rolling cadence scenarios simulated at Year 3.5 (v2.0 simulations). The plots are centered on α = 0 and δ = 0. R.A. and decl. lines are marked every 30°.
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: Fit results of KIC 4377638. The K95+ model (solid red line) fitted to the phase-folded light curve (black dots) in the top panel. The lower panel shows the residuals of the fit. The dashed red line indicates a zero-point. Note: the plot shows phases (0)–(2) to make the fitting results clear, and phases (1)–(2) are an exact copy of phases (0)–(1).
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: Results of fitting KIC 7591456 to Equation (5). The dashed blue line is the K95+ model (the first item in Equation (5)), and the dashed yellow line is the sinusoidal signal (the second item in Equation (5)). The solid green line is the superposition of the blue and yellow lines (Equation (5)).
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: Same as Figure 1 for KIC 8112039. We have added five colored synthetic light curves with ω of 0°, 30°, 60°, 120°, 150°, and the other six parameters equal to those of our fitting results.
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: Histograms of orbital parameters for the HBSs in this work. The period, eccentricity, inclination, and argument of periastron (ω) are in panels (a)−(d), respectively.
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: Seven systems without morphology of the heartbeat signal. Same as Figure 1.
Paper: A Multitransition Methanol Survey toward a Large Sample of High-mass Star-forming Regions
Authors: J. Y. Zhao, J. S. Zhang, Y. X. Wang, J. J. Qiu, Y. T. Yan, H. Z. Yu, J. L. Chen, Y. P. Zou
Figure caption: The 13CH3OH rotational diagram of our sample. The solid line is the fit to the E-type 13CH3OH (solid squares) and the dashed line to the A-type 13CH3OH (empty circles). The fit results are shown in the upper right corner.
Paper: A Multitransition Methanol Survey toward a Large Sample of High-mass Star-forming Regions
Authors: J. Y. Zhao, J. S. Zhang, Y. X. Wang, J. J. Qiu, Y. T. Yan, H. Z. Yu, J. L. Chen, Y. P. Zou
Figure caption: Left panel: Line width of CH3OH 00,0 → 1−1,1 vs. line width of CH3OH 80,8 → 71,7 line. The dashed line indicates both lines have equal values of line width. Right panel: Histograms of the line widths for CH3OH 80,8 → 71,7 (solid lines) and CH3OH 00,0 → 1−1,1 (dashed lines).
Paper: A Multitransition Methanol Survey toward a Large Sample of High-mass Star-forming Regions
Authors: J. Y. Zhao, J. S. Zhang, Y. X. Wang, J. J. Qiu, Y. T. Yan, H. Z. Yu, J. L. Chen, Y. P. Zou
Figure caption: Distributions of the column density (left panel) and the relative abundance (right panel) for A-type (dashed lines) and E-type CH3OH (solid lines) in our sample.
Paper: A Multitransition Methanol Survey toward a Large Sample of High-mass Star-forming Regions
Authors: J. Y. Zhao, J. S. Zhang, Y. X. Wang, J. J. Qiu, Y. T. Yan, H. Z. Yu, J. L. Chen, Y. P. Zou
Figure caption: The spectra of the newly detected 95 GHz CH3OH masers from our survey.
Paper: A Multitransition Methanol Survey toward a Large Sample of High-mass Star-forming Regions
Authors: J. Y. Zhao, J. S. Zhang, Y. X. Wang, J. J. Qiu, Y. T. Yan, H. Z. Yu, J. L. Chen, Y. P. Zou
Figure caption: The line width of the CH3OH transition lines vs. the bolometric luminosity, with solid lines for the linear fit.
Paper: Data-driven Uncertainty Quantification of the Wave Telescope Technique: General Equations and Demonstration Using HelioSwarm
Authors: T. Broeren, K. G. Klein
Figure caption: A numerical experiment using the wave telescope technique to identify wavevectors using a single perfectly shaped four-spacecraft configuration (χ = 0, L = 1, ﹩{d}_{\max }=\sqrt{2}﹩). We plot the median value of error in wavevector identification as a function of wavevector magnitude.
Paper: Data-driven Uncertainty Quantification of the Wave Telescope Technique: General Equations and Demonstration Using HelioSwarm
Authors: T. Broeren, K. G. Klein
Figure caption: Using our equations of effective error μ eff and σ, we plot how many orders of magnitude of wavevectors ﹩\bar{k}﹩ can be reconstructed with two different measures of accuracy and precision. The left panel shows how many orders of ﹩\bar{k}﹩ can be reconstructed such that μ eff is less than 10%. The right panel shows how many orders of ﹩\bar{k}﹩ can be reconstructed such that μ eff + 2σ is less than 20%.
Paper: Data-driven Uncertainty Quantification of the Wave Telescope Technique: General Equations and Demonstration Using HelioSwarm
Authors: T. Broeren, K. G. Klein
Figure caption: In the left panel we plot the errors found using four-spacecraft configurations with 0.1 ≤ χ < 0.2 as black dots. We note that we can distinguish the aliased points with a simple threshold at ﹩\mathrm{Error}=400{\bar{k}}^{-1}﹩. In the right panel we plot the probability that a wavevector reconstruction is aliased at each magnitude ﹩\bar{k}﹩.
Paper: Data-driven Uncertainty Quantification of the Wave Telescope Technique: General Equations and Demonstration Using HelioSwarm
Authors: T. Broeren, K. G. Klein
Figure caption: For each nine-spacecraft HelioSwarm configuration, NEWTSS selects the subset of spacecraft that minimizes the quantity μ eff + 2σ at each wavevector magnitude k. We plot the resulting minimized effective error and 2σ associated with the hour 205 HelioSwarm DRM configuration in the top-left panel. In the other panels, we show the number of spacecraft N in the selected subset, the characteristic size L of that subset, and the shape of that subset χ.
Paper: Data-driven Uncertainty Quantification of the Wave Telescope Technique: General Equations and Demonstration Using HelioSwarm
Authors: T. Broeren, K. G. Klein
Figure caption: We use NEWTSS to select the subset of spacecraft that minimizes the value of μ eff + 2σ at each wavevector magnitude k (as in Figure 9). We plot the resulting value of μ eff + 2σ over the first 2 weeks of HelioSwarm’s Phase-B science mission for each wavevector magnitude k. The white dots outline the 20% error value, the red dashes highlight the hour 205 configuration from Figure 9.
Paper: Data-driven Uncertainty Quantification of the Wave Telescope Technique: General Equations and Demonstration Using HelioSwarm
Authors: T. Broeren, K. G. Klein
Figure caption: For a nine-spacecraft configuration there are ﹩{\sum }_{n=4}^{9}{C}_{n}^{9}=382﹩ subsets of at least four spacecraft. For each of these subsets, NEWTSS uses our learned equations to predict the effective error of the wave telescope technique at each wavevector magnitude k. This is done for the example configuration of hour 205 of the HelioSwarm Phase B DRM. See Appendix C for a breakdown of the shapes and sizes of all 382 of these N ∈ {4, 5, 6, 7, 8, 9} spacecraft subsets.
Paper: Data-driven Uncertainty Quantification of the Wave Telescope Technique: General Equations and Demonstration Using HelioSwarm
Authors: T. Broeren, K. G. Klein
Figure caption: An example plane wave is simulated using six spacecraft. We use the adaptive  k  search Algorithm 1 to define an adaptive mesh that allows us to identify the peak value of P(ω,  k ) while minimizing function evaluations. We display the values of ﹩{\boldsymbol{k}}\in [\bar{k},{k}_{\theta },{k}_{\phi }]﹩ that are scanned using this procedure as black lines. We see that the identified peak corresponds to the true wavevector of the plane wave (shown as red dashes). We overlay contours at three values P (blue, green, cyan lines) on the upper panel. We also display the computed values of ﹩P(\bar{k})﹩ (blue crosses) on the lower panel.
Paper: Data-driven Uncertainty Quantification of the Wave Telescope Technique: General Equations and Demonstration Using HelioSwarm
Authors: T. Broeren, K. G. Klein
Figure caption: Using our data set and learned equations for μ and σ, we check what proportion of points fall within the threshold μ ± σ 0 σ for values of σ 0 in the interval [−3, 3]. For ease of visualization, we have taken the log10 of the error value found. Therefore, if our equations perfectly fit the data, we expect that the CDF of a standard normal distribution (shown as black dashes) would be identical.
Paper: Data-driven Uncertainty Quantification of the Wave Telescope Technique: General Equations and Demonstration Using HelioSwarm
Authors: T. Broeren, K. G. Klein
Figure caption: From hour 205 of the science phase of the Phase-B DRM of HelioSwarm, we compute the elongation, planarity, and characteristic sizes of all subsets of the nine-spacecraft configuration which contain N ∈ {4, 5, 6, 7, 8, 9} spacecraft. The black lines represent the shape threshold χ = 1.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Color composites for the LARS 1–10 galaxies. Two panels are shown for each galaxy with the ID number connecting the corresponding panels. The left subpanel for each galaxy shows a stellar continuum composite using the HST I-, B-, and U-band images for the RGB channels. The scale bar in these panels has a length of 5 kpc. The right panel for each galaxy shows a composite of red (Hα), blue (Lyα), and green (stellar continuum in the FUV at the wavelength of Lyα). The Lyα maps have been adaptively smoothed to enhance the contrast and be able to show the low-surface-brightness parts of the galaxy.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Left panel: emission-line diagnostics for the sample. The gray shaded region shows the density of galaxies from SDSS DR8. All but one of the galaxies fall in the region dominated by emission from H II regions. Right panel: galaxy main-sequence diagram using data from the JHU-DR8 derivation of stellar masses and SFRs. Note that Tol 1214 and Tol 1247 do not have SDSS data, and emission-line data from other sources (see Table 1) are used. LARS 9 is not included in the MPA–JHU-DR8 catalogs; for this galaxy, we use SFR and stellar mass from the Granada Flexible Stellar Population Synthesis analysis of DR14 data (Montero-Dorta et al. 2016). Note the majority of galaxies in the sample are not included in the DR9+ stellar mass and emission-line property catalogs, which is why we chose to use DR8 for this comparison.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Left panel: the Lyα vs. the FUV luminosity of the galaxies in this sample. Diagonal dashed lines show different limits of W Lyα . Right panel: f esc vs. W Lyα  for the galaxies. In addition to a linear fit to the current data, the relation from Sobral & Matthee (2019) is shown.