adsabs/AstroCLIMB huggingface dataset:
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Same as Figure 1, but including a GP to the model. The gold dashed line is the same model in Figure 1 without GP, and the brown solid line is the model with GP. The bottom panel shows the difference between those two lines in ppm units. It is clear how the use of a GP is not only degenerate with the phase curve parameters, but also affects both the transit and eclipse depths.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Transmission spectrum of TOI-1685 b using NIRSpec/G395H. Top: individual transmission spectrum from the Eureka! (purple), Tiberius (red), and ExoTIC-JEDI (orange) data reductions. Bottom: Difference between each data reduction in units of their standard deviation.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Difference between the white light curves from each data reduction. Each panel shows the MAD of the data. Apart from the presence of a small linear trend (−34 ppm day−1 in NRS1 and 64 ppm day−1 in NRS2), the differences follow a Gaussian distribution, indicating that the presence and properties of correlated noise are pipeline-independent.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Position of TOI-1685 b in a mass–radius diagram. Internal composition models of rocky planets from L. Zeng et al. (2016). The change in radius from the highest precision of JWST observations compared to TESS makes the density of TOI-1685 b even more consistent with Earth than previously reported.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: GP-only component of the model shown in Figure 9 for NRS1 and NRS2. Despite having similar amplitudes and variability timescales, the correlated noise properties in NRS1 are different from those of NRS2.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: TOI-1685 b’s measured dayside NRS2 brightness temperature ratio (﹩{ \mathcal R }﹩) in the context of other rocky exoplanets as a function of irradiation temperature (the substellar temperature of a blackbody). Point size is proportional to planet size. TOI-1685 b follows the trend of blackbody-like emission for ∼1000–2000 K planets, suggesting no significant atmospheres and dark surfaces. The most compelling evidence for atmospheres has come from planets hot enough to vaporize rock. Data are taken from, in order of increasing irradiation temperature: TRAPPIST-1 c (S. Zieba et al. 2023), TRAPPIST-1 b (averaged from MIRI F1280W and F1500W, E. Ducrot et al. 2025), LTT 1445 A b (P. Wachiraphan et al. 2025), GJ 1132 b (Q. Xue et al. 2024), LHS 1478 b (P. August et al. 2025), TOI-1468 b (E. Valdés et al. 2025), GJ 486 b (M. Weiner Mansfield et al. 2024), LHS 3844 b (L. Kreidberg et al. 2019), GJ 1252 b (I. J. M. Crossfield et al. 2022), GJ 367 b (M. Zhang et al. 2024), TOI-431 b (C. Monaghan et al. 2025), 55 Cnc e (R. Hu et al. 2024), and K2-141 b (S. Zieba et al. 2022).
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Results of running the residuals of the low-resolution spectroscopic light curves through a Lomb–Scargle periodogram. (a) A gallery of the residuals from the Eureka! pipeline for each spectroscopic channel. (b) The periodogram results. The color of the lines between panels a and b is for the same white light or spectroscopic channel. The residuals show uncorrelated noise at periods of <0.5 hr. The left two panels are for NRS1; the right two panels are for NRS2.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Examples of poorly fitting emission forward models of atmospheres and their associated temperature–pressure profiles using HELIOS. We also include blackbody models with albedos derived from the best-fit NRS2 phase curve amplitude (Aeff = 0) and prayer-bead eclipse spectrum (Aeff = 0.2), corresponding to dayside temperatures of 1390 K and 1320 K, respectively. Compared to atmospheric models, the observed eclipse spectrum is relatively featureless, and in all tested atmospheres, the airless basaltic model is preferred.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Contour plot showing the NRS2 derived effective albedo and heat redistribution efficiency (ε) for TOI-1685 b compared to estimates for solar system bodies from Q. Xue et al. (2024), M. Weiner Mansfield et al. (2024). Black and gray error bars represent the 1σ (84%) and 2σ (95%) upper limits for ε, respectively. The red arrow indicates the maximum Tp,day for a blackbody (assuming Aeff = 0 and ϵ = 0.) We adopt AB = 0.119, 0.75, 0.306, 0.250, and 0.11 for Mercury, Venus, Earth, Mars, and the Moon, respectively. Since the solar system’s terrestrial planets are not tidally locked, we estimate their heat redistribution efficiency using their polar and equatorial temperatures with a given effective albedo. The results are 1σ consistent with the (mostly) airless Moon, Mercury, and Mars and highly inconsistent with Earth-like or Venus-like heat redistribution.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Model eclipse spectra of possible low-albedo surface types from R. Hu et al. (2012; using the surface model and updated albedo profiles of B. P. Coy et al. 2024) in units of brightness temperature, ignoring the opposition surge effect. High brightness temperatures at low wavelengths are due to the contribution from reflected light. The Bond albedo of these surfaces is 0.13 for metal-rich, 0.20 for Fe-oxidized, 0.24 for basaltic, and 0.49 for ultramafic. For comparison, we derive Aeff = 0.2 ± 0.1 from the prayer-bead eclipse spectrum. Black points represent our prayer-bead eclipse spectrum, whereas gray points show simulated observations of 10 eclipses with MIRI LRS using PandExo (N. E. Batalha et al. 2017), assuming an ultramafic surface.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Eureka! reduced spectroscopic light curves in the wavelength-integration plane for NRS1 (left) and NRS2 (right). The planet transit can be seen by eye at around integration number 2400. The two white vertical lines in NRS2 are masked bad columns. The color gradient in NRS2 is a consequence of the decreasing signal to noise as a function of wavelength in this detector. The same effect is seen in the blue end of NRS1, but much less noticeable.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: White light phase curves of TOI-1685 b from NRS1 (left column) and NRS2 (right column) from JWST as in Figure 1. Top: Tiberius data reduction. Bottom: ExoTIC-JEDI data reduction. Circles show binned data every 25 integrations to improve visualization.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Same as Figure 18 but for the ExoTIC-JEDI reduction.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Same as Figure 18 but for the Tiberius reduction.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Posterior distributions of fitted parameters from the NRS1 white light curve analysis. As discussed in Section 3.3.3, we performed the prayer-bead method on the Eureka! reduction with MCMC, resulting in 4370 values of median and ±1σ. We then re-created 4370 Gaussian distributions using these medians and ±1σ, each with 1000 points, and plotted the 1σ, 2σ, and 3σ contours of the distributions on this figure. The median and ±1σ of the distributions are shown with black dashed and dotted lines, while the original results from Eureka! analysis are shown with red lines. Clearly, the prayer-bead analysis provides us with larger error bars, thus avoiding underestimations of the true uncertainties.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Results of the PCA for NRS1 (left three panels) and NRS2 (right three panels). We created 20 independent eigenvectors using the PCA functionality in scikit-learn. We show the results for a single spectroscopic channel (λcen = 4.143 ± 0.017). Top: black is the reduced spectroscopic light curve. Red is the light curve after it has been correlated against the four “best” eigenvectors, shown in the middle panel. Bottom: results of the Lomb–Scargle periodogram on the four eigenvectors in the middle plot.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Posterior distributions of fitted parameters from the NRS2 white light curve analysis. See the caption of Figure 22 for more information.
Paper: The Fraction of Polar-aligned Circumbinary Disks
Authors: Ted M. Johnson, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow
Figure caption: Grid of dynamical states for 106 RKF simulations of a system with eb = 0.4 and j = 0.1. This grid can be run for any combination of (eb,  j), and integrating over the polar region computes the fraction of systems in which a disk would evolve to a polar state.✎
Paper: The Fraction of Polar-aligned Circumbinary Disks
Authors: Ted M. Johnson, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow
Figure caption: Example of system simulation and state determination. This figure tracks the orbital parameters of a third body with j = 0.05 orbiting a 1M⊙ binary with equal-mass stars and eb = 0.4. Initially, ﹩{\rm{\Omega }}=\frac{\pi }{2}﹩ in all cases.✎
Paper: The Fraction of Polar-aligned Circumbinary Disks
Authors: Ted M. Johnson, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow
Figure caption: MC results (points) for eb = 0.4, j = 0.66, and fb = 0.5 compared to RKF results for the same setup (contour lines). At this value of j all circulating orbits have the same secular behavior regardless of the orbit being prograde or retrograde. The regions interior to the black contour lines are initial conditions which allow polar librating orbits according to the RKF method. Note that some points that REBOUND classify as polar fall outside the RKF polar region. The MC result gives fpolar = 0.47 ± 0.03 while the RKF result gives fpolar = 0.43 with numerical error on the order of 104. The point marked “Unknown” represents a system whose state could not be determined after 10,000 orbits of the third body due to a relatively long dynamical timescale and has been factored into the MC uncertainty. The MC simulation results used to generate this figure can be downloaded at doi:10.5281/zenodo.14736363 ✎ ✎
Paper: The Fraction of Polar-aligned Circumbinary Disks
Authors: Ted M. Johnson, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow
Figure caption: Effect of j on the precession timescale as calculated in Equation (21). Top: Ratio between the numerically computed precession timescale and the analytic solution for a massless ring. To compute the solid lines, the inclination is fixed, and only j varies. Twice the orbit switches between prograde circulation and libration, and the timescale becomes very long at that boundary. For the dashed lines, i is held 5∘ away from a stationary point. In the librating case, this stationary point is given by Equation (15) of R. G. Martin & S. H. Lubow (2019). In the circulating case, the stationary point is coplanar. For all simulations, the step size is Δj = 10−3, and we assume eb = 0.4, f = 0.5, ab/r = 1/5, and Ω0 = π/2. Bottom: (i, Ω) tracks for all 2000 simulations that compose the solid line in the top panel. The arrow points to the initial conditions for every line (marked by the red point). The divergence of the different tracks is due to the change of j only.✎
Paper: The Fraction of Polar-aligned Circumbinary Disks
Authors: Ted M. Johnson, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow
Figure caption: Polar disk fraction fpolar as a function of j for various distributions ﹩{p}_{{e}_{\,\rm{b}\,}}({e}_{\,\rm{b}\,})﹩. All cases assume isotropic distributions of initial angular momentum. In the thermal case, ﹩{p}_{{e}_{\,\rm{b}\,}}({e}_{\,\rm{b}\,})\propto {e}_{\,\rm{b}\,}﹩. In the uniform case, ﹩{p}_{{e}_{\,\rm{b}\,}}({e}_{\,\rm{b}\,})=\,\rm{const}\,﹩. The case labeled eb < 0.1 uses a uniform distribution, but restricts the domain to eb ∈ [0, 0.1). These three distributions are shown in the inset. The dashed line cases fix eb at a particular value. Notice the maximum that occurs at j ≈ 0.5. This occurs because the appearance of crescent orbits at j = jcr (R. G. Martin & S. H. Lubow 2019, Equation (A3)) makes the parameter space that eventually evolves to polar very large.✎
Paper: The Fraction of Polar-aligned Circumbinary Disks
Authors: Ted M. Johnson, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow
Figure caption: Same as Figure 4, but with the mutual inclination distribution given by Equation (15) that is plotted in the inset, normalized by ﹩\sin i﹩. This normalization shows that the probability-per-unit-area on the unit sphere becomes very high at i = 0 (coplanar alignment) when σ is small (dashed (σ = π/2) and dotted (σ = π/8) lines), but it is uniform everywhere in the isotropic case (σ → ∞, solid line). The main figure shows that for low j, low σ (low inclination preference) decreases fpolar. For high j, low σ (low inclination preferences) lowers the value that fpolar tends to as eb → 0.✎
Paper: The Fraction of Polar-aligned Circumbinary Disks
Authors: Ted M. Johnson, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow
Figure caption: Same as Figure 1, but with a mask over the region where tp > tdisk. Parameters used are an equal-mass binary with Mb = M⊙, eb = 0.4, j = 0.1, ab = 1 au, r/ab = 30, and tdisk = 106 yr. Note that 40% of initial conditions remain misaligned in this setup, but this fraction is near zero when r/ab = 20 and near 1 when r/ab = 40. Not shown are versions of this figure where eb and j have been varied. We have found that up to 85% of simulations remain misaligned when eb = 10−6, but if j is subsequently increased to 10, then that becomes 1%.✎
Paper: The Fraction of Polar-aligned Circumbinary Disks
Authors: Ted M. Johnson, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow
Figure caption: Polar fraction as a function of eb for various values of j. Each line is computed via a numerical integration of Equation (6), assuming an isotropic distribution of i. For low j, the polar fraction is a strong function of eb. However, as j increases, fpolar becomes insensitive to the binary eccentricity (except for the case that eb ≈ 1). Note that fpolar(eb ≈ 0) is maximized when j = 0.5.✎
Paper: The Fraction of Polar-aligned Circumbinary Disks
Authors: Ted M. Johnson, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow
Figure caption: Same as Figure 5, but with the mutual inclination distribution given by Equation (15). A preference for lower mutual inclinations (lower values of σ, see dashed and dotted lines) leads to lower fpolar in all cases. See the inset of Figure 6 for a visualization of the various i distributions.✎
Paper: 100 Proof: H I Observations of 100 Nearby Dwarf Galaxies with the 100 m Green Bank Telescope
Authors: Aleksandra E. Nazarova, John M. Cannon, Igor D. Karachentsev, Dmitry I. Makarov, Maksim I. Chazov, Lila Schisgal, William St. John
Figure caption: Upper panel: distribution of 105 observed dwarf galaxies according to m21 magnitude and B magnitude corrected for Galactic extinction. Three diagonal lines indicate a ratio μ = Mgas/M* equal to 0.1, 1, and 10. For undetected galaxies the ﹩{m}_{21}=20\mathop{.}\limits^{m}0﹩ is assigned. Bottom panel: distribution of 77 GBT-detected dwarf galaxies according to m21 magnitude and B magnitude corrected for Galactic extinction combined with 266 late-type (T = 9, 10) dwarf galaxies in the Local Volume with TRGB distance estimates. Three diagonal lines correspond to μ equal to 0.1, 1, and 10.
Paper: 100 Proof: H I Observations of 100 Nearby Dwarf Galaxies with the 100 m Green Bank Telescope
Authors: Aleksandra E. Nazarova, John M. Cannon, Igor D. Karachentsev, Dmitry I. Makarov, Maksim I. Chazov, Lila Schisgal, William St. John
Figure caption: Upper panel: magnitude vs. line width relation for nearby dwarf galaxies detected with the GBT. The horizontal bars indicate the standard errors of W50. The dashed line displays the Tully–Fisher relation, Equation (10). Bottom panel: magnitude vs. line width relation for the same galaxies but with a correction for galaxy inclination according to Equation (13).
Paper: 100 Proof: H I Observations of 100 Nearby Dwarf Galaxies with the 100 m Green Bank Telescope
Authors: Aleksandra E. Nazarova, John M. Cannon, Igor D. Karachentsev, Dmitry I. Makarov, Maksim I. Chazov, Lila Schisgal, William St. John
Figure caption: Images of 77 H I-detected nearby late-type dwarf galaxies taken from DESI Legacy Imaging Surveys. Each image side is ﹩{2}^{{\prime} }﹩; north is to the top and east is to the left.
Paper: 100 Proof: H I Observations of 100 Nearby Dwarf Galaxies with the 100 m Green Bank Telescope
Authors: Aleksandra E. Nazarova, John M. Cannon, Igor D. Karachentsev, Dmitry I. Makarov, Maksim I. Chazov, Lila Schisgal, William St. John
Figure caption: Images of 28 undetected nearby late-type dwarf galaxies taken from DESI Legacy Imaging Surveys (KKR56 from PanSTARRS). Each image side is ﹩2^{\prime} \rm{}\,\rm{}\,﹩; north is to the top and east is to the left.
Paper: 100 Proof: H I Observations of 100 Nearby Dwarf Galaxies with the 100 m Green Bank Telescope
Authors: Aleksandra E. Nazarova, John M. Cannon, Igor D. Karachentsev, Dmitry I. Makarov, Maksim I. Chazov, Lila Schisgal, William St. John
Figure caption: H I spectra of 77 dwarf galaxies detected with GBT. The H I flux integrals and W50 values are given above each panel.
Paper: Acceleration of C IV and Si IV Broad Absorption Lines in Quasar SDSS J140058.79+260619.4
Authors: Ying-Ru Lin, Wei-Jian Lu
Figure caption: Spectra of the quasar SDSS J1400+2606 acquired at two distinct epochs. The y-axis in the upper panel is scaled in units of 10−17 erg s−1 cm−2. Two dashed vertical blue lines, spanning both panels, designate the C IV and Si IV emission lines, respectively. The upper panel shows original spectra (solid), with the black curve representing the MJD 53852 spectrum, while the red curve represents the MJD 56093 spectrum. The dashed curves are their pseudocontinuum fittings. The upper x-axis represents blueshift velocity (103 km s−1) referenced to the C IV and Si IV doublet’s strongest lines. The 1σ uncertainty ranges are shown as solid black and red lines at the panel base. The lower panel shows the pseudocontinuum-normalized spectra corresponding to the original spectra in the upper panel. Solid black horizontal bars delineate the BALs apparent in the spectra. The dotted vertical lines accentuate the central positions of the C IV and Si IV BALs of system A.
Paper: Acceleration of C IV and Si IV Broad Absorption Lines in Quasar SDSS J140058.79+260619.4
Authors: Ying-Ru Lin, Wei-Jian Lu
Figure caption: Profile comparison of the C IV (panels (a) and (b)) and Si IV (panels (c) and (d)) BALs of System A. Panels (a) and (c): original pseudocontinuum-normalized spectra from two-epoch observations (MJD 53852 in black, MJD 56093 in red), showing velocity shift signatures. The line centers of the BAL troughs are marked by vertical dotted lines. Panels (b) and (d): the same profiles after applying a velocity shift correction to the MJD 56093 spectra to align them with the MJD 53852 epoch.
Paper: Acceleration of C IV and Si IV Broad Absorption Lines in Quasar SDSS J140058.79+260619.4
Authors: Ying-Ru Lin, Wei-Jian Lu
Figure caption: Spectra of three quasars exhibit potential velocity shifts in their absorption lines. Plotting conventions (line styles, color codes, and scaling) adhere to Figure 1’s framework.
Paper: Acceleration of C IV and Si IV Broad Absorption Lines in Quasar SDSS J140058.79+260619.4
Authors: Ying-Ru Lin, Wei-Jian Lu
Figure caption: Light curve of J1400+2606 from the CRTS. Vertical black and red dashed lines indicate the timing of the SDSS and BOSS spectral observations, respectively.