adsabs/AstroCLIMB huggingface dataset:
Paper: Resonant Excitation of Planetary Eccentricity due to a Dispersing Eccentric Protoplanetary Disk: A New Mechanism of Generating Large Planetary Eccentricities
Authors: Jiaru Li, Dong Lai
Figure caption: Eigenstates of the “planet + disk” system,  S  − and  S  +, as functions of the disk mass M d. The top panel shows the ratio S p/S d of the two eigenstates. The dashed line marks the M d when ω d = ω p,d. The middle panel shows the corresponding eccentricity ratio E p/E d. The bottom panel shows the eigenvalues g − and g +. The values of ω d and ω p,d are also shown for comparison. The inset plot zooms in to where M d is between 8 × 10−3 M ⋆ and 9 × 10−3 M ⋆. It covers the region around the avoided crossing, which is where g − and g + are closest to each other.
Paper: Resonant Excitation of Planetary Eccentricity due to a Dispersing Eccentric Protoplanetary Disk: A New Mechanism of Generating Large Planetary Eccentricities
Authors: Jiaru Li, Dong Lai
Figure caption: Fundamental eccentric modes of the fiducial disk. The solid curves are the real parts of the E m(r)'s, while the dashed curves are the imaginary parts. The top panel shows the modes when M d = 0.15M ⋆, with the e-mode in black and the s-mode in red. The middle and the bottom panels are for M d = 0.05M ⋆ and 10−3 M ⋆; both cases allow only e-modes (black) but not s-modes. The s-mode has a frequency ω d,m = (0.012 − 0.001i)ΩK,0, where ΩK,0 = ΩK(r 0). The e-mode frequencies are ω d,m = 0.010ΩK,0, 0.002ΩK,0, and −0.0003ΩK,0 for M d = 0.15M ⋆, 0.05M ⋆, and 10−3 M ⋆, respectively. The disk surface density profile is shown as the gray curve for reference in each panel. The value of the Toomre Q parameter (Toomre 1964) is greater than 1.74 throughout the whole disk when M d = 0.15M ⋆.
Paper: Resonant Excitation of Planetary Eccentricity due to a Dispersing Eccentric Protoplanetary Disk: A New Mechanism of Generating Large Planetary Eccentricities
Authors: Jiaru Li, Dong Lai
Figure caption: Frequencies of the fundamental eccentric modes of the fiducial disk as functions of M d. The e-mode is shown in black, and the s-mode is in red. The s-mode can only exist when the disk is massive (i.e., in the gray region). The solid curves show the real parts of the frequencies (in units of the Keplerian frequency at the disk inner radius), which represent the precession rates of the modes. The dashed curves show the imaginary parts, corresponding to the growth rates of the modes. The e-mode always has ﹩{\mathfrak{I}}({\omega }_{{\rm{d}},{\rm{m}}})=0﹩.
Paper: Resonant Excitation of Planetary Eccentricity due to a Dispersing Eccentric Protoplanetary Disk: A New Mechanism of Generating Large Planetary Eccentricities
Authors: Jiaru Li, Dong Lai
Figure caption: Time evolution of the planet eccentricity in our parameter studies. From top to bottom, each panel shows the results for systems that are the same as the fiducial (see Figure 3) but with different planet semimajor axis a p, planet mass M p, and disk decay timescale τ d, respectively. The orange curves in all panels are the same as the E p curve in Figure 3.
Paper: Resonant Excitation of Planetary Eccentricity due to a Dispersing Eccentric Protoplanetary Disk: A New Mechanism of Generating Large Planetary Eccentricities
Authors: Jiaru Li, Dong Lai
Figure caption: Planet–disk eccentricity evolution for disks with different τ d (the same runs as shown in the bottom panel of Figure 4). The upper and lower panel show ratio ∣S p/S d∣ and ∣E p/E d∣, respectively. The gray curve in each panel shows the path of the eccentricity eigenmode  S  + for reference.
Paper: Resonant Excitation of Planetary Eccentricity due to a Dispersing Eccentric Protoplanetary Disk: A New Mechanism of Generating Large Planetary Eccentricities
Authors: Jiaru Li, Dong Lai
Figure caption: Same as Figure 6 but shows the evolution of the systems with a slightly nonzero initial planet E p, such that the initial condition is exactly in the eccentricity eigen state  S  +.
Paper: Left Ringing: Betelgeuse Illuminates the Connection between Convective Outbursts, Mode Switching, and Mass Ejection in Red Supergiants
Authors: Morgan MacLeod, Andrea Antoni, Caroline D. Huang, Andrea Dupree, Abraham Loeb
Figure caption: Slices through the computational domain of radial velocity relative to the stellar center as the hot convective plume rises. Positive velocities indicate outflow, while negative velocities inflow in this frame of reference. The upper panels slice through the stellar envelope in the x–y plane. The lower panels show slices at a radius of 770 R ⊙ at the same times. The hot fluid, initially located at (x, y) = ( + 335 R ⊙, 0), begins rising and spreading over several hundred days as it breaks out of the stellar envelope.
Paper: Left Ringing: Betelgeuse Illuminates the Connection between Convective Outbursts, Mode Switching, and Mass Ejection in Red Supergiants
Authors: Morgan MacLeod, Andrea Antoni, Caroline D. Huang, Andrea Dupree, Abraham Loeb
Figure caption: Betelgeuse’s light and line-of-sight radial velocity curves in the interval 2012–2023. The upper panel shows V-band magnitudes tabulated by the AAVSO, with times of photometric minima marked. The lower panel shows radial velocities from STELLA (Granzer et al. 2022), with times of radial velocity maxima marked. The systemic velocity is 20.57 km s−1. In each case, we show a smoothed-spline fit to the curves, from which the maxima and minima are identified. In the radial velocity data, we also show a best-fit sine curve for the long secondary period.
Paper: Left Ringing: Betelgeuse Illuminates the Connection between Convective Outbursts, Mode Switching, and Mass Ejection in Red Supergiants
Authors: Morgan MacLeod, Andrea Antoni, Caroline D. Huang, Andrea Dupree, Abraham Loeb
Figure caption: Radial structure of a MESA 1D stellar evolution model approximating Betelgeuse, where we plot the mass density, pressure, and radial convective Mach number in the three panels. We compare to spherically averaged quantities from the initial state of our hydrodynamic simulation, before a pressure perturbation is added. The pressure perturbation itself is shown in red, with the values of individual zones plotted directly.
Paper: Left Ringing: Betelgeuse Illuminates the Connection between Convective Outbursts, Mode Switching, and Mass Ejection in Red Supergiants
Authors: Morgan MacLeod, Andrea Antoni, Caroline D. Huang, Andrea Dupree, Abraham Loeb
Figure caption: Left: power spectrum of radial velocities during, and following, the breakout of the convective plume. The initial injection of power into moderate degree modes (l ∼ 3–4) decays over time in intensity and dissipates to smaller scales through convective turbulence. Right: integrated power in low-degree (l ≤ 8) and high-degree (l > 8) modes as a function of time. The power in the large-scale, low-degree oscillations decays exponentially in time, as predicted by the theory of convective dissipation.
Paper: Left Ringing: Betelgeuse Illuminates the Connection between Convective Outbursts, Mode Switching, and Mass Ejection in Red Supergiants
Authors: Morgan MacLeod, Andrea Antoni, Caroline D. Huang, Andrea Dupree, Abraham Loeb
Figure caption: Line-of-sight velocity post-processed from the surface of our simulation snapshots at r = 770 R ⊙. Here, we imagine observers in the ±x directions, and compute the disk-averaged line-of-sight velocity, where negative values imply outflow from the star toward the observer. An observer facing the breakout of the plume (+x direction) sees an extended period of negative velocities. By contrast, an observer in the opposite direction sees little effect. Variability due to the evolving properties of convective plumes is exhibited from both viewing angles.
Paper: Left Ringing: Betelgeuse Illuminates the Connection between Convective Outbursts, Mode Switching, and Mass Ejection in Red Supergiants
Authors: Morgan MacLeod, Andrea Antoni, Caroline D. Huang, Andrea Dupree, Abraham Loeb
Figure caption: Radial velocities relative to the stellar center along a ray located along the x-axis of the computational domain. For readability, velocities are smoothed with a 100 R ⊙ moving top-hat kernel. In this time series, the outflowing motion of the hot convective plume decreases in intensity as the plume spreads and begins to break out.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: The probability distribution functions of column densities derived by the DLA fitting (orange line) and the Lyα profile fitting (green line). In the top panel, the histograms are normalized by the total numbers of galaxies showing DLA system (31) or Lyα emission line (28 after excluding the J0808+3948 active galactic nucleus), respectively. In the middle panel, the histogram is weighted by the covering fraction of low-N H I  and high-N H I  paths: (1 − f  C ) and f  C , respectively. The black dashed line represents the combined distribution over the ∼1018–1022 cm−2 range for CLASSY galaxies. In the bottom panel, we present the distribution of column densities for three types of Lyα profiles. The black dashed line indicates the galaxies with only Lyα emission, the gray dashed–dotted line indicates the galaxies with Lyα emission in the bottom of DLA system, and the dotted line indicates the galaxies with only DLA systems. The resulting distribution remains bimodal regardless of the details of the weighting and subsample.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: The left panel shows the side view of HST/COS observation. We adopt a continuous shell geometry, which contains different column-density regions as dark blue and light blue. This is somewhat an oversimplification as the ISM can be clumpy, but should be the simplest way to illustrate the ISM in galaxies. We note the scale length of different regions in this figure does not indicate their physical scale length. We use the gray shaded regions to indicate the parts that are missed by the HST/COS aperture. The right panel shows the zoom-in structure of a small slab of the outflowing shell. The yellow, light blue, and dark blue indicate the LyC-thin, low-N H I , and high-N H I  paths, respectively. The gray and green lines show the radiative transfer processes of the continuum and Lyα photons. We mark the covering fraction of different column density channels. The rightmost spectra represent the emergent Lyα profiles along different regions. The low-N H I  channels lead to the Lyα emission line, but the high-N H I  channels lead to the DLA system. The observed Lyα spectrum is a combination of those Lyα profiles, and thus, the residual flux in the bottom of the DLA profile equals the covering fraction of low-N H I  channels.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption:                          ﹩{f}_{\mathrm{esc}}^{\mathrm{Ly}\alpha }﹩ (top) and Δv Ly α  (bottom) vs. O32 ratio. The O32 ratio is defined as [O III] λ5007/[O II] λ3727. We color-code the circles based on their UV half-light radius. The yellow circles have a UV half-light radius larger than 0.″4, which corresponds to the COS unvignetting aperture. We overplot the data in the literature to expand the dynamic range. The gray dots indicate the dwarf galaxies at z ∼ 0.1–0.4 from Yang et al. (2017). The gray Y-shape markers indicate the local dwarf galaxies at z ∼ 0.02–0.07 with extreme O32 ratios from Izotov et al. (2020).
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: Lyα red peak asymmetry vs. Lyα peak separation. The gray, blue, and pink shaded regions correspond to three different regimes of LyC leakage: small leakage (gray), leakage through low-N H I  holes (small holes, red), and leakage by the full break (large density-bounded holes, blue), respectively. We overplot the known leakers from Izotov et al. (2016, 2018a, 2018b) as gray squares. The red squares highlight six galaxies (J0942+3547, J0944-0038, J1253-0312, J1323-0132, J1418+2102, J1545+0858), which have net Lyα trough flux, suggesting they might be LyC leakers.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption:                          ﹩{v}_{\mathrm{Si}\,{\rm\small{II}}}^{\mathrm{outflow}}﹩ vs. ﹩{v}_{\mathrm{trough}}^{{\rm{L}}y\alpha }﹩. The top panel adopts the ﹩{v}_{\mathrm{Si}\,{\rm\small{II}}}^{\mathrm{outflow}}﹩ measured by the single-Voigt fitting (K. Parker et al. 2023, in preparation), and the bottom panel adopts the ﹩{v}_{\mathrm{Si}\,{\rm\small{II}}}^{\mathrm{outflow}}﹩ measured by a double-Gaussian fitting (Xu et al. 2022). The dashed lines indicate the 1:1 relationship. The Si II absorbers are multiphase, including neutral hydrogen in addition to the mostly ionized phase. By comparing ﹩{v}_{\mathrm{trough}}^{{\rm{L}}y\alpha }﹩ and ﹩{v}_{\mathrm{Si}\,{\rm\small{II}}}^{\mathrm{outflow}}﹩, we are able to distinguish ionization status of the ISM.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption:  v DLA vs. ﹩{v}_{\mathrm{trough}}^{{\rm{L}}y\alpha }﹩ (top) and ﹩{v}_{\mathrm{Si}\,{\rm\small{II}}}^{\mathrm{outflow}}﹩ (bottom). Here, we adopt the ﹩{v}_{\mathrm{Si}\,{\rm\small{II}}}^{\mathrm{outflow}}﹩ measured by K. Parker et al. (2023, in preparation). The gray dashed lines indicate the 1:1 relationship. In the bottom panel, we separate the sample based on whether their spectra have Lyα emission lines. We notice the O I absorption line of one galaxy (J0938+5428, open square) is contaminated by the refilling O I emission line. Thus, we adopt the velocity of C II absorption line, and we use a black dashed line to connect them. The good agreement suggests that the gas in low-N H I  has same velocity as the gas in high-N H I  channels.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: Best-fit Lyα spectra (red) for 29 CLASSY galaxies using the residual stellar continuum and a Gaussian redshift prior with σ = 120 km s−1 (second attempt). The spectra are normalized by the peak flux, and the orange dashed lines indicate the continuum level for each object. Every input Lyα profile is successfully reproduced by tlac model. We use the green lines to show the residual and manually shift it by −0.1 for better illustration. The gray dashed lines indicate the zero level of the residual.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: The Lyα trough velocity measured from spectrum vs. the outflow velocity estimated by the shell model. Top panel: the ﹩{v}_{\mathrm{trough}}^{{\rm{L}}y\alpha }﹩ is measured based on the spectroscopic redshift. Bottom panel: the ﹩{v}_{\mathrm{trough}}^{{\rm{L}}y\alpha }﹩ is measured based on the redshift from tlac profile fitting. We plot the measurements from both the z-unconstrained fitting (open circle, Section 3.2.2) and the z-constrained fitting (solid circle, Section 3.3). The dashed line indicates the 1:1 relationship.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: Best-fit Lyα spectra (red) for 29 CLASSY galaxies using the total stellar continuum and a Gaussian redshift prior with σ = 120 km s−1 (first attempt). The spectra are normalized by the peak flux, and the orange dashed lines indicate the continuum level for each object. Clearly, the Lyα spectra of J0938+5428, J0944+3442, J1044+0353, J1119+5130, J1144+4012, J1416+1223, and J1521+0759 have failed to be reproduced. We use the green lines to show the residual and manually shift it by −0.1 for better illustration. The gray dashed lines indicate the zero level of the residual.
Paper: Solar–Stellar Connection: X-Ray Flares to Energetic (E > 10 MeV) Particle Events
Authors: S. W. Kahler, A. G. Ling
Figure caption: Comparisons of numbers of SEP/Type II and non-SEP events binned by associated peak X-ray flare sizes Fp. Each peak-flux bin has roughly the same number (117) of total events.
Paper: Solar–Stellar Connection: X-Ray Flares to Energetic (E > 10 MeV) Particle Events
Authors: S. W. Kahler, A. G. Ling
Figure caption: Comparisons of numbers of SEP/Type II and non-SEP events binned by associated peak X-ray flare durations TD. Each duration time size bin has roughly the same number (117) of total events.
Paper: Solar–Stellar Connection: X-Ray Flares to Energetic (E > 10 MeV) Particle Events
Authors: S. W. Kahler, A. G. Ling
Figure caption: Comparisons of numbers of SEP/Type II and non-SEP events binned by associated peak X-ray flare temperature Tm . Each peak-temperature bin has roughly the same number (112) of total events.
Paper: Solar–Stellar Connection: X-Ray Flares to Energetic (E > 10 MeV) Particle Events
Authors: S. W. Kahler, A. G. Ling
Figure caption: Comparisons of numbers of SEP/Type II and non-SEP events binned by associated X-ray flare rise times TR. Each rise-time bin has roughly the same number (117) of total events.
Paper: Solar–Stellar Connection: X-Ray Flares to Energetic (E > 10 MeV) Particle Events
Authors: S. W. Kahler, A. G. Ling
Figure caption: Medians of peak temperature Tm , log duration time TD, log rise time TR, and log decay time C2 as a function of log Fp for the No SEP, No Type II and SEP or Type II samples.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The distribution of the negative (left panels) and positive (right panels) medians of JAVELIN distributions for 100 mock light curves with no input lag. From top to bottom, the light curves have been subsampled with the long season LSST u- and y-band cadence, the baseline u- and y-band cadence, the baseline g- and z-band cadence, and the baseline g- and z-band cadence + LCO cadence.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: Distribution of the long lags recovered by JAVELIN for 100 mock light curves with input lags of −50 and 7 days (left panel), −130 and 9 days (middle panel), and −400 and 12 days (right panel). The dashed vertical line shows the input long lag. The green and light blue distributions are for mock light curves with the baseline v2.0 LSST cadence for the u and y band and g and z band, respectively. In addition to the baseline LSST cadence, the distributions shown in pink have an LCO observation taken roughly every 10 days in each LSST observing gap. These LCO observations amount to around 18 observations in each gap, or per year, for a total of around 180 observations.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The distributions of the long lags recovered by the maximum-likelihood method for 100 light curves with input lags of −50 and 7 days (left panel) and −130 and 9 days (right panel). The orange and green distributions are for mock light curves with the long season and baseline v2.0 LSST cadences, respectively, for the u and y band. The dashed vertical line shows the input long lag.