adsabs/AstroCLIMB huggingface dataset:
Paper: X-Ray Spectra of Black Hole X-Ray Binaries with Returning Radiation
Authors: Temurbek Mirzaev, Cosimo Bambi, Askar B. Abdikamalov, Jiachen Jiang, Honghui Liu, Shafqat Riaz, Swarnim Shashank
Figure caption: Radial profile of the ionization parameter ξ in the simulations shown in Figure 4. The Eddington-scaled luminosity of the source is λ = 0.01 (left panel) and λ = 0.1 (right panel). Dashed green curves are for ρ = L corona/L disk = 0, dashed–dotted red curves are for ρ = 1, and solid blue curves are for ρ = 100. The curves in the same style in the same panel refer to the ionization parameter calculated, without including (lower curves) and including (upper curves) the returning radiation of the reflection spectrum.
Paper: X-Ray Spectra of Black Hole X-Ray Binaries with Returning Radiation
Authors: Temurbek Mirzaev, Cosimo Bambi, Askar B. Abdikamalov, Jiachen Jiang, Honghui Liu, Shafqat Riaz, Swarnim Shashank
Figure caption: As in Figure 4 for ρ = 1 and different values of the coronal height h. From left to right: h = 3, 5, 10, and 20 r g.
Paper: X-Ray Spectra of Black Hole X-Ray Binaries with Returning Radiation
Authors: Temurbek Mirzaev, Cosimo Bambi, Askar B. Abdikamalov, Jiachen Jiang, Honghui Liu, Shafqat Riaz, Swarnim Shashank
Figure caption: As in Figure 2 for λ = 0.1.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: Spectroheliogram images constructed from the spectrograph raster for the FUV Si IV λ1402 line (left) and the photospheric continuum far out in the NUV Mg II line wing (right). The dashed black line shows the location of the slit position for the image shown in Figure 1. The blue contours show regions of high H2 intensity, and the red contours show regions where there is saturation in the bright C II or Si IV lines. The dark horizontal line at solar Y = –242″ comes from the alignment fiducial at the top of the spectrograph slit, and missing data occur at two different time steps in each of the channels, shown by the black vertical lines.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: The relative contribution to the upper-level populations for the first three upper levels in the Lyman band, which produce the strongest H2 lines seen in the IRIS FUV spectra. For each upper level, the contribution of each line is shown for each baseline model (FALC, XCO, F2) indicated by the hue, and the intensity multiplier is indicated by the hue saturation. The highest multipliers have the brightest hue. Bright emission lines in this wavelength range are shown by the dotted lines.
Paper: Molecular Hydrogen Line Identifications in Solar Flares Observed by IRIS: Lower Atmospheric Structure from Radiometric Analysis
Authors: Sarah A. Jaeggli, Adrian N. Daw
Figure caption: Radiance of the λ1396.223 H2 line as a function of the spectral radiance at the wavelength of the λ1335.969 H2 line pumped by C II to populate the common (0,0) upper level. The individual curves include all multipliers for a particular baseline model. The dashed and solid lines show the results from the optically thin and optically thick calculation for the H2 line emission, respectively. The ratio of the H2 line intensity to its pump provides a way to distinguish between different atmospheric models.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: The scaling exponents H, a DFA, h CMA, and 1 + χ  H  for each of the five IBEX energy channels when analyzing either the original flux time series of Figures 2 and 3 or the D7 flux time series of Figure 8. When these four scaling exponents lead to a statistically significant result that shows a difference (anisotropy) between north (blue) and south (red), the corresponding p-value to obtain such a result by chance is given in green. The method to obtain these p-values is described in Appendix B.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: Time series of flux of the energy channels NE1 to NE5 for the north pole.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: Time series of flux of the energy channels SE1 to SE5 for the south pole.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: The original flux of the energy channel NE5 (blue crosses), together with least-squares fit by an eighth-order polynomial (cyan continuous line). The residual is depicted by the magenta squares.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: The original flux of the energy channels NE5 (cyan crosses) and SE5 (magenta circles), together with the corresponding eighth-order polynomial fits (blue and red, respectively) that are used to remove the effect of solar cycle. The corresponding HHT sums from the trend down to the sixth IMF are also shown in dark blue for north and brown for south. Notice that the latter curves reveal a delay of about 2 yr in the maxima achieved after the rebound that follows their minima.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: The original flux of the energy channel NE5 (blue crosses), together with the sum (cyan) of the trend and the last two IMFs of its HHT used for detrending. The residual is depicted by the magenta squares.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: The Fourier transform power spectrum S(T) of the original ENA flux time series recorded by the energy channel NE5 (blue) vs. the period T together with that after Wiener filtering (pink, labeled final). The latter power spectrum leads to the residual shown in pink in Figure 7 plus a constant. The Fourier transform power spectrum has been normalized to unity so that ﹩{\int }_{0}^{{f}_{s}/2}S(f){df}=1﹩, where f  s  is the sampling frequency of 14.61 yr−1.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: The original flux of the energy channel NE5 (blue crosses), together with the sum (cyan) of the Wiener-filtered signal plus a constant (c = 0.00573427556) to eliminate the mean value of the residual. The residual is depicted by the magenta squares.
Paper: Persistent Behavior in Energetic Neutral Atom Time Series from IBEX
Authors: N. V. Sarlis, G. Livadiotis, D. J. McComas, M. Alimaganbetov, N. A. Schwadron, K. Fairchild
Figure caption: Time series of D7 flux for the energy channels E1–E5 for the north pole (left column) and the south pole (right column), where the peaks that are beyond 3 standard deviations (3σ) have been removed.
Paper: A Modified Initial Mass Function of the First Stars with Explodability Theory under Different Enrichment Scenarios
Authors: Ruizheng Jiang, Gang Zhao, Haining Li, Qianfan Xing
Figure caption: Inferred progenitor mass distributions under (a) monoenrichment and (b) the dual-enrichment assumption, along with their best-fit IMFs and relative residuals based on different explodability constraints. The black circles with solid lines, red triangles with solid lines, and brown dashed lines represent the best-fit standard power law, explodability-modifying power-law distributions, and combined log-normal power law, respectively. For a detailed definition of parameters in the legends, please refer to Sections 5.1–5.3.
Paper: A Modified Initial Mass Function of the First Stars with Explodability Theory under Different Enrichment Scenarios
Authors: Ruizheng Jiang, Gang Zhao, Haining Li, Qianfan Xing
Figure caption: Baryonic remnant masses of different supernova models. The remnant maximum can be set to either 1.94 M ⊙ or 2.35 M ⊙.
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: Quenched fractions as a function of stellar mass. SAGA satellites, corrected for incompleteness, are shown in both panels as solid green circles with Poisson error bars. Left: We plot the uncorrected confirmed satellite quenched fractions (open green squares), which agree with the completeness-corrected values for the Gold sample (gold bar) but increasingly deviate toward the Silver sample (gray bar). The 1σ system-to-system scatter for the 101 individual SAGA systems is shown by the light green shaded region. A subsample of 18 SAGA hosts in Local Group–like systems is shown as the dotted green line and is statistically indistinguishable from the full sample. Black stars represent MW satellites. Right: We compare to the ELVES Survey (Carlsten et al. 2022), which classifies satellites using a color-only criterion. We plot the full sample of 28 ELVES hosts (orange open squares) and a subsample of 14 ELVES hosts matching the SAGA MW criteria (solid orange squares, −23 > M  K  > − 24.6).
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: Top: Optical grz-composite DECaLs images of example satellite galaxies in the SAGA Survey. Red circles are the fiber coverage of the spectroscopic redshift measurement. Bottom: GALEX NUV/FUV-composite images for the same objects, with the aperture (green) used to measure NUV flux (the larger of r eff or the 6″ GALEX PSF). The image title lists the satellite’s stellar mass and whether it is classified as star-forming (SF) or quenched (Q). Satellites in the left two columns are in the Gold sample; the right three columns are Silver sample satellites. All images are ﹩0\buildrel{\,\prime}\over{.} 75﹩ on a side.
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: NUV-based star formation rates (SFR, left) and specific star formation rates (sSFR, right) vs. stellar mass for all SAGA satellites with GALEX coverage (358 of 378 satellites). Circles indicate NUV detections; triangles are NUV upper limits. The GALEX NUV data are shallower than our Hα observations (color-coding), which we use to detect satellites. We plot SAGA hosts (gray squares) and the LMC/SMC (stars, see Section 7.2 for references). In both panels, the dotted line indicates ﹩\mathrm{log}[{\mathrm{sSFR}}_{\mathrm{NUV}}/{\mathrm{yr}}^{-1}]=-11﹩. Vertical dashed lines indicate the stellar mass limits of our Gold (M ⋆ > 107.5 M ⊙) and Silver (107.5 > M ⋆ > 106.75 M ⊙) samples.
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: Top: The SAGA quenched fraction (solid green) decreases with increasing projected distance from host (d proj). We plot only the Gold satellites to minimize completeness corrections. While the quenched fraction of the full ELVES sample (open orange squares) is higher at all radii, the matched sample largely agrees with SAGA (solid orange squares). Bottom: Cumulative radial distribution function of SAGA quenched (red) vs. star-forming satellites (blue) with projected distance from host. The shaded regions represent the contribution from incompleteness correction. Vertical bars indicate the radius enclosing half of the satellites in each population. Quenched galaxies are more radially concentrated than star-forming satellites at the same stellar mass.
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: The star formation–stellar mass sequence (SFS) for SAGA satellites based on our NUV SFRs (left) and Hα SFRs (middle). Quenched satellites have been removed; triangles indicated NUV upper limits but are not used to determine binned properties. Binned mean and scatter (squares) for each sample are plotted, along with linear fits to the combined Gold+Silver sample for the NUV (blue) and Hα (red). Right: A direct comparison between SFR indicators, where η is defined as the ratio of the Hα to NUV SFR. The mean binned value of η is consistent with zero (green squares), indicating that the satellite quenching timescale is longer than 100 Myr.
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: A SAGA satellite is defined as quenched (Q, red) or star-forming (SF, blue) based on combined criteria in Hα EW and NUV specific star formation rate (sSFRNUV). Circles indicate galaxies with detected flux in GALEX NUV. Triangles indicate upper NUV limits. Galaxies with no GALEX coverage are plotted as squares at the top of the plot. Error bars are shown only for objects lying near the quenched boundaries (solid lines). Star-forming galaxies in the upper left are those for which the central optical fiber clearly missed outer regions of star formation (see Section 3.1).
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Mass–semimajor axis constraints for a potentially undetected perturbing planet within the disk. The blank white region in the center indicates the possible parameter space for an undetected inner planetary perturber on a circular orbit within the disk plane. The pink lines correspond to the minimum Laplace radius (the r out of the disk; see Equation (7)) and sets the minimum possible mass for the planet at a given semimajor axis a  pl . The purple line shows the upper bound on a  p  set by the mean motion resonance overlap argument (Equation (9)). The gray lines exclude planets within MIRI MRS 3σ and 5σ detection limits. Note also that the region outside the disk, marked in black, is unstable due to perturbations from η Tel B (Section 6.1).
Paper: Sigmoid Eruption Associated with the X9.3 Flare from AR 12673 Drives the Gradual Solar Energetic Particle Event on 2017 September 6
Authors: Stephanie L. Yardley, David H. Brooks
Figure caption: (a) 94 Å image of AR 12673 on 2017 September 6 at 11:49:28 UT just prior to the second SEP event taken by the Atmospheric Imaging Assembly (AIA; J. R. Lemen et al. 2012) onboard the Solar Dynamics Observatory (SDO; W. D. Pesnell et al. 2012). The red (blue) contours correspond to the line-of-sight magnetic field taken by the Helioseismic and Magnetic Imager (HMI; P. H. Scherrer et al. 2012) on board SDO saturated at a level of 300 G (−300 G). The black rectangle represents the FOV of the Hinode/EIS observations taken ∼8 hr earlier. (b) The GOES-13 X-ray flux during the period 2017 September 4–12. The dashed lines represent the peak of each flare occurring during this period with the shaded regions indicating the duration of each flare. The green ovals show the occurrence and velocity of the CMEs that originated from AR 12673. The circle fraction represents the width of the CME taken from the SOHO LASCO CME catalog (https://cdaw.gsfc.nasa.gov/CME_list/).
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Corner plot for the orbitize! (S. Blunt et al. 2020) derivation of the η Tel B orbital parameters using the P. H. Nogueira et al. (2024) companion mass Gaussian prior of M = 47 ± 0.15M  J .
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Corner plot for the orbitize! (S. Blunt et al. 2020) derivation of the η Tel B orbital parameters using a relaxed primary mass prior of M = 2.2 ± 0.1 (C. H. Chen et al. 2014).
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Corner plot for the best-fit properties of η Tel B derived from a BT-SETTL (CIFIST) model grid fit using species (T. Stolker et al. 2020).
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Corner plot for the derivation of the η Tel B orbital parameters using orbitize! (S. Blunt et al. 2020), as discussed in Section 5.2.
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Corner plot for the orbitize! (S. Blunt et al. 2020) derivation of the η Tel B orbital parameters using only the relative astrometry included in the P. H. Nogueira et al. (2024) orvara fit.
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Corner plot for the orbitize! (S. Blunt et al. 2020) derivation of the η Tel B orbital parameters using the P. H. Nogueira et al. (2024) initial distribution positions and priors.
Paper: Near-infrared Spectroscopy of the Sun and Solar Analog Star HD 76151: Compiling an Extensive Line List in the Y, J, H, and K Bands
Authors: Sena Aleyna Şentürk, Timur Şahin, Ferhat Güney, Selçuk Bilir, Mahmut Marışmak
Figure caption: An example of the solar analysis performed with the MOOG LTE line analysis code in the optical and NIR is shown. The upper panel, top, and middle panels, respectively, show the determination of the photospheric model atmosphere parameters for the Sun (KPNO-OPTICAL and KPNO-NIR) as a function of the LEP and the reduced EW using the MOOG stellar atmosphere code. The lower panel is for the HARPS and IGRINS spectra of HD 76151. The solid dashed lines in all panels represent least-squares fits to the data. The bottom panels show the wavelength distribution of the abundances calculated for the Fe lines in both panels.
Paper: Near-infrared Spectroscopy of the Sun and Solar Analog Star HD 76151: Compiling an Extensive Line List in the Y, J, H, and K Bands
Authors: Sena Aleyna Şentürk, Timur Şahin, Ferhat Güney, Selçuk Bilir, Mahmut Marışmak
Figure caption: The Galactic orbit and birth radii of HD 76151 for three different age values in the Z × R gc (a) and R gc × t (b) diagrams. The filled yellow circles and triangles show the today and birth positions, respectively. The red arrow is the motion vector of HD 76151 today. The green and pink dotted lines show the orbit when parameter errors of the input values are considered, while the green and pink filled triangles represent the birthplaces of the HD 76151 based on the lower and upper error estimates.
Paper: Near-infrared Spectroscopy of the Sun and Solar Analog Star HD 76151: Compiling an Extensive Line List in the Y, J, H, and K Bands
Authors: Sena Aleyna Şentürk, Timur Şahin, Ferhat Güney, Selçuk Bilir, Mahmut Marışmak
Figure caption: The standard deviation of the Ti, Cr, and Fe abundances from the suite of Ti I, Cr I, Fe I, and Fe II lines as a function of ξ.
Paper: Near-infrared Spectroscopy of the Sun and Solar Analog Star HD 76151: Compiling an Extensive Line List in the Y, J, H, and K Bands
Authors: Sena Aleyna Şentürk, Timur Şahin, Ferhat Güney, Selçuk Bilir, Mahmut Marışmak
Figure caption: The faint blue area in the image represents the errors in the model parameters (ΔT eff =  88 K, ﹩{\rm{\Delta }}\mathrm{log}g\,=﹩ 0.16 cgs) obtained from the HARPS spectrum of HD 76151 in the optical region (filled blue star symbol), while the faint red area represents the errors in the model parameters (ΔT eff = 178 K, ﹩{\rm{\Delta }}\mathrm{log}g\,=﹩ 0.25 cgs) obtained from the IGRINS spectrum of HD 76151 in the IR (filled red star symbol). The model parameters from both optical and IR are represented by a filled purple star symbol.
Paper: Near-infrared Spectroscopy of the Sun and Solar Analog Star HD 76151: Compiling an Extensive Line List in the Y, J, H, and K Bands
Authors: Sena Aleyna Şentürk, Timur Şahin, Ferhat Güney, Selçuk Bilir, Mahmut Marışmak
Figure caption: NIR solar spectrum (black) and the NIR spectrum of HD 76151 (turquoise). The BASS2000 solar spectrum used by D. T. Andreasen et al. (2016) [AN16] (green) and the NIR telluric KPNO spectrum (red) are also included. The neutral and ionized Fe lines reported by J. Meléndez & B. Barbuy (1999) [MB99], D. T. Andreasen et al. (2016) [AN16], J. T. Rayner et al. (2009) [RA09], and Borrero et al. (2003) [BO03] are included as colored dots. The black and red dotted vertical lines indicate the lines used in this study and included in the study of D. T. Andreasen et al. (2016), respectively.