adsabs/AstroCLIMB huggingface dataset:
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: Intercept (a) and the slope (b) of the fitted F and FO-mode PR relations for Z = 0.004 and Y = 0.25, Z = 0.008 and Y = 0.25, Z = 0.02 and Y = 0.28 (taken from De Somma et al. 2020b), and Z = 0.03 and Y = 0.28 for a fixed mixing length parameter of α ml = 1.5, and as a function of the various assumptions about the ML relation (see the main text and labels for more details).
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: Intercept (a) and the slope (b) of the fitted canonical F and FO-mode PR relations for Z = 0.004 and Y = 0.25, Z = 0.008 and Y = 0.25, Z = 0.02 and Y = 0.28 (taken from De Somma et al. 2020b), and Z = 0.03 and Y = 0.28 as a function of the mixing length parameter (see the main text and labels for more details).
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: Comparison between theoretical F and FO-mode amplitudes (solid green lines and dashed blue lines, respectively) and Z = 0.004 F- and FO-mode data (green points and blue plus, respectively.) The upper panel and middle panels show the comparison for canonical ML relation with α ml = 1.5 and α ml = 1.7, respectively, while the bottom panel shows the comparison for noncanonical ML relation (case B) with α ml = 1.5.
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: The same as Figure 24 but for the G RP Gaia band.
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: The same as Figure 22 but for Z = 0.008.
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: The same as Figure 22 but for the G RP Gaia band.
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: Left: fragmentation ﹩{\sigma }_{{}^{3}\mathrm{He}}﹩ and pickup ﹩{\sigma }_{{d}^{3}\mathrm{He}}﹩ cross sections. Black dashed line is the adapted total cross section. Fragmentation measurements are taken from Meyer (1972, a review), Griffiths & Harbison (1969), Nicholls et al. (1972), Jung et al. (1973), Bizard et al. (1977), Webber (1990), Glagolev et al. (1993), Abdullin et al. (1993), Abdullin et al. (1994), and Blinov et al. (2001). Pickup measurements are taken from Meyer (1972, a review), Griffiths & Harbison (1969), Nicholls et al. (1972), Jung et al. (1973), Glagolev et al. (1993), Abdullin et al. (1993), Abdullin et al. (1994), and Blinov et al. (2001). Middle: tritium production cross section. The data are taken from Meyer (1972, a review), Jung et al. (1973), Nicholls et al. (1972), Bizard et al. (1977), Webber (1990), Glagolev et al. (1993), Abdullin et al. (1993), Abdullin et al. (1994), and Blinov et al. (2001). Right: deuterium production cross section. The data are taken from Meyer (1972, review), Jung et al. (1973), Webber (1990), Glagolev et al. (1993), Abdullin et al. (1993), Abdullin et al. (1994), and Blinov et al. (2001).
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: Cross-section data for the reaction pp → π + + d (blue squares; Cartwright et al. 1953; Meshcheryakov et al. 1955; Meshcheryakov & Neganov 1955; Neganov & Parfenov 1958; Sachs et al. 1958; Turkot et al. 1963; Bugg et al. 1964; Chapman et al. 1964; Overseth et al. 1964; Heinz et al. 1968; Richard-Serre et al. 1970), and for the inverse reaction π + + d → pp (red open diamonds; Durbin et al. 1951; Rogers & Lederman 1957; Rose 1967; Axen et al. 1976; Ritchie et al. 1981; Boswell et al. 1982; Ritchie et al. 1983), which were converted using Equation (G8). The solid black curve is the fit for Equation (G13).
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: A fit to the cross section ﹩{\sigma }_{{}^{3}\mathrm{He}\to d}﹩ together with data. Colored lines show separate components, and the black dashed line is the adapted total cross section. Data points are taken from Meyer (1972, Figure 4), Griffiths & Harbison (1969), Blinov et al. (1986), and Glagolev et al. (1993).
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: Inelastic cross sections for the reactions α + α, α + 12C, and α + 56F. Lines: black, Barashenkov & Polansky routines (Appendix F.3); blue, modified Tripathi et al. formalism (Appendix F.2).
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: Left: calculations of production of 3He, 3H, and 2H in p+A (A = 12, 58) reactions. Right: calculations of production of 3He, 3H, and 2H in α + A (A = 12, 58) reactions. Calculations are done using the formalism described by Coste et al. (2012) and reproduced in Appendix G.5.
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: Corner plot showing the PDFs of the time lags of the synthetic light curves with DDFs COSMOS (blue) and ECDFS (orange) sampling (left) and homogeneous 1 day (blue) and 5 day (orange) sampling (right). The distribution for each time lag independently is shown in the histograms along the diagonal, and the 2D distributions are shown as contour plots in the other panels. The dashed black lines are the true time lag values inferred from the AD model. The contour levels of the 2D joint probability densities are at the 1σ and 2σ regions.
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: The comparison of metric values above the Nyquist threshold (y-axis) for the measurement of 5 day time lags in six DDFs, for various OpSim strategies indicated on the x-axis and six of the LSST filters stated in the legend. The solid lines serve as guides for the eye. The horizontal black line indicates the metric threshold. DDFs are indicated in the titles of panels. The passbands u, g, r, i, z, and y are denoted by blue, orange, green, red, violet, and brown, respectively.
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: Comparison of mean 5σ depth (left column), mean sampling (middle column), and mean cumulative season length (right column) for different observing strategies (x-axis) in DDFs and ugrizy filters. The solid lines guide the eye. The mean 5σ depths of the non-r and r bands are close. This means that objects as bright as 21 will still be seen in those bands for these overlapping cadences in DDF. Also, fainter objects in the non-r band will be observable in the r band. The passbands u, g, r, i, z, y are denoted with blue, orange, green, red, violet, and brown, respectively.
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: The same as Figure 11 but for different DDFs.
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: Zoom-in of metric values (indicated in color bars) in DDFs for different cadence strategies (given in panel titles) for the r, g, and i bands. Upper row: COSMOS. Middle row: first and second panels: ECDFS; third panel: EDFS_a. Bottom row: EDFS_a.
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: The same as Figure 7, but for XMM in the top row, ELAISS1 in the middle row, and EDFS_b in the bottom row.
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: Examples of simulated quintets of LSST light curves for quasars in the LSST DDFs. We simulate the light curves over a period of 10 yr with multi_short_v2.0_10yrs cadences. The error bars are set at 0.005 mag rms.
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: The expected number of quasars for which time lag could be measured with respect to the u band, in the main LSST filters as a function of the redshift, for fiducial 10 deg2 survey area and fiducial cadence of 1 day.
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: From top to bottom, the left panels show the FO-mode theoretical amplitudes for the G BP and G RP Gaia bands and the F814W and F160W HST-WFC3 bands for Z = 0.004 and Y = 0.25 (dashed magenta line), Z = 0.008 and Y = 0.25 (dashed blue line), Z = 0.02 and Y = 0.28 (dashed cyan line), and Z = 0.03 and Y = 0.28 (dashed green line) at fixed mixing length parameter of α ml = 1.5 and ML relation case A. The right panels show the same plots but for the F-mode models (solid lines with the same color code as in the left panels).
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: From top to bottom, the left panels show the F-mode canonical theoretical amplitudes (solid lines) in the G BP and G RP Gaia bands and the F814W and F160W HST-WFC3 bands for Z = 0.004 and Y = 0.25, for various assumptions of the α ml parameters, while the right panels show the same F-mode theoretical amplitudes for various assumptions about the ML relation at a fixed mixing length parameter of α ml = 1.5.
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: The same as Figure 15 but for Z = 0.03 and Y = 0.28.
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: The same as Figure 12 but with the theoretical parallaxes obtained by applying the PW relation for Z = 0.02.
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: The same as Figure 15 but for the FO-mode models.
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: The same as Figure 15 but for Z = 0.008 and Y = 0.25.
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: The same as Figure 15 but for Z = 0.02 and Y = 0.28.
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: The same as Figure 16 but for Z = 0.02 and Y = 0.28.
Paper: An Updated Metal-dependent Theoretical Scenario for Classical Cepheids
Authors: Giulia De Somma, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Silvio Leccia, Ilaria Musella
Figure caption: The same as Figure 16 but for Z = 0.008 and Y = 0.25.
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: CR intensities at the solar system’s location for nuclei (left) and primary electrons (right). For the nuclei the primary species are protons and helium-4, with the secondary deuterons and 3He produced during the propagation through the ISM. The individual species’ spectral intensities are labeled, but should be sufficiently distinct. The steady-state solutions (Section 4.2) are shown for all nuclei species as the solid black lines. The time-dependent solutions taken at 50 kyr intervals over the 2.5 Myr “sampling” interval (see text) are shown as the overlaid red lines. For the primary electrons, we use instead a time-series representation to show the fluctuations for the intensities due to the finite source lifetime and rapid cooling. In this panel, the steady-state intensity is overlaid as the long dashed line at the respective energies shown. The corresponding time-dependent solution intensities at the same energies for the 50 kyr sampling over the 2.5 Myr epoch are shown as the solid red lines.
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: The relative difference for solutions generated using the solvers for different grid discretizations and time/spatial sampling. Left panel: Exp solver solutions at 60 pc (green lines) and 200 pc (red lines) after 10 kyr using tangent grid discretization with the central pixels 4 (triple dotted–dashed), 8 (dot short dashed), and 16 pc (dot long dashed), respectively. Right panel: CN (red, cyan lines) and Exp (black line) solver solutions at 200 pc after 100 kyr. Short dashed lines are for the CN solver using time stepping of 100 yr, while long dashed lines use time stepping of 10 yr. The different color lines for the CN solutions are for tangent grid discretistations with central pixel 8 pc (red) and 16 pc (cyan), respectively. The Exp solution is shown only for the 8 pc discretization because the 16 pc case is essentially the same.
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: Inelastic cross sections for the reactions p+d, p + 3He, p + 4He, p + 7Li, p + 12C, p + 16O, p + 27Al, p + 40Ca, and p + 56F. The data are taken from the database posted at https://www.oecd-nea.org/dbdata/bara.html. Data for the p+d reaction are taken from Carlson et al. (1973). Lines: black, Barashenkov & Polansky routines (Appendix F.3); blue, modified Tripathi et al. formalism (Appendix F.2); green, corrected Wellisch & Axen formalism (Appendix F.1).
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: Very-high-energy γ-ray emission longitude profiles averaged over −5° < b < 5° for total (left; sum of π 0 decay and IC), and IC scattering (right) for the time-dependent and steady-state SA100 modeling configurations. Line colors: black, SA100 steady-state solution; red, SA100 time-dependent solution at 50 kyr intervals over the 2.5 Myr sampling duration for the simulation (see text). Note all profiles include the attendant pair-absorption attenuation calculated using the same R12 ISRF model as for the IC energy losses/γ-ray production.
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: Comparison between analytic and numerical solutions for 10 kyr (left) and 50 kyr (right) for 60 and 200 pc locations from the grid center. Line coding: black solid, analytic; red long dashed, CN; green dashed–dotted, Exp. The numeric solutions have been multiplied by factors 2 (CN) and 0.5 (Exp) for clarity.
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: Synchrotron radiation longitude profiles averaged over −5° < b < 5° for the SA0, SA50, and SA100 source models used by the example. Line colors: black, SA100 source density; orange, SA50 source density; cyan, SA0 source density. Line styles: solid, total electrons including primary and secondaries produced via inelastic CR nuclei interactions with the gas; long dashed, primary electrons only.
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: The CR proton (left) and electron (right) differential energy densities at the Galactic plane for the SA100 steady-state (SS) solution (top panels) and the time-dependent discrete (TDD) solution (bottom panels). The solar system’s location is marked by the yellow star. The time-dependent solution sample is taken at 102.5 Myr, at the end of the simulation epoch.
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: IC intensities at (left to right) 100, 200, 300, and 340 kyr, respectively, for the inhomogeneous diffusion example, based on the “Scenario C” model described by the work of Jóhannesson et al. (2019). Upper row is at 1.23 TeV and lower row is at 10 GeV γ-ray energies. The white solid horizontal line in each figure shows the Galactic plane.
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: Very-high-energy γ-ray emission longitude profiles averaged over −5° < b < 5° for π 0 decay (left) and IC scattering (right) for the different modeling configurations. Line styles: solid, SA100 source density; long dashed, SA50 source density; dotted, SA0 source density. Line colors: black, R12 ISRF model; red, F98 ISRF model.
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: Coadded depth in DDFs for different observing strategies in the u,g,r,i filters. The best strategy for AD RM is also the deepest in all bands.
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: The same as Figure A13, but for the z, y filters.
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: Metric realization on six_rolling and u_long_ms_30 cadences. DDFs are prominent in the i band (panels (a) and (e)) and the r band (panels (b) and (g)).
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: Metric realization on short_exp cadences. Metric run emphasizes two fields in the u band (panels (c), (g), and (k)).