adsabs/AstroCLIMB huggingface dataset:
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption: The spectra of all 54 DIBs detected in the 0.91–1.33 μm range. The spectra of β Ori (the top spectrum), HD210191 (the second spectrum from the top), Cyg OB2 No. 12 (the third spectrum from the top), and Wd1 W33 (the bottom spectrum) are shown in each panel. The horizontal axis shows the line-of-sight velocities that were calculated with the rest-frame wavelengths shown in Table 3. The spectra are shifted by the velocities that were measured using DIB λ10780, to align the DIBs. The regions that are contaminated with strong telluric absorption lines are interpolated from the surrounding regions, which the strong telluric absorption lines do not contaminate. The interpolated and original spectra are shown using the thick and thin lines, respectively. The spectra are shown with gray lines in cases where the DIBs could not be evaluated, owing to the blending of the other features. The detected DIBs are indicated by the yellow areas. The marks with the black thin lines that are sometimes plotted above the spectra show DIBs and candidates that appear in the panels of other DIBs.
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption: Distributions of the numbers (upper panel), total EWs (middle panel), and ∑ i  f  i  N  i  (lower panel) of the DIBs. The horizontal axes indicate the wavelength, and the bin size is 500  Å. The inset panel in the lower panel shows a detailed view of the histograms at λ > 7500  Å. The colors indicate the same factors as in Figure 7.
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption: Distributions of the numbers (upper panel), total EWs (middle panel), and ∑ i  f  i  N  i  (lower panel) of the DIBs. The horizontal axes indicate the wavenumber, and the bin size is 1000 cm−1. The inset in the lower panel shows a detailed view of the histograms at ν < 13,000 cm−1. The colors indicate the same EW ranges as in Figure 7.
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption: Wavenumber densities of the DIB numbers (top panel), EWs (middle panel), and the sums of the products of the oscillator strength and column density (lower panel), after considering the observational biases. See the main text for the sampled wavelength region and the threshold used for the depth of the DIBs. The horizontal bars indicate the sampled ranges. The vertical bars in the top panel show the square roots of the numbers of DIBs, that is, the Poisson uncertainties of the DIB numbers. As a reference, we also plot the data for the H-band DIBs with open circles, to see their trend at longer wavelengths. Note that the effects of the observational biases were not considered for these points.
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption: FWHM distribution of the DIBs for HD147889. The upper and lower panels show the DIBs in the optical (5000 < λ < 6500  Å) and NIR (9100 < λ < 13300  Å) wavelength ranges, respectively. The left, middle, and right panels show the FWHMs measured in wavelengths, normalized by wavelength, and measured in wavenumbers, respectively. The dashed lines show the FWHMs corresponding to the spectral resolutions. The black bars show the DIBs with central depths larger than 0.009.
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption: Upper panel: the EWs of the DIBs detected toward No. 12 in the range of 0.91–1.33 μm. The circles show the DIBs detected or confirmed in H15 (blue), and the DIBs detected in this study (red). The black squares show the DIBs detected in the literature (Joblin et al. 1990; Foing & Ehrenfreund 1994; Groh et al. 2007). The green diamonds show the DIBs detected in Ebenbichler et al. (2022). The light blue triangles show the candidate DIBs in this study. Lower panel: transmittance spectrum of the atmosphere. The spectrum is synthesized using ATRAN. The locations of the Paschen H I lines and C2 Phillips bands are also shown.
Paper: Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I. Newly Identified Bands
Authors: Satoshi Hamano, Naoto Kobayashi, Hideyo Kawakita, Keiichi Takenaka, Yuji Ikeda, Noriyuki Matsunaga, Sohei Kondo, Hiroaki Sameshima, Kei Fukue, Shogo Otsubo, Akira Arai, Chikako Yasui, Hitomi Kobayashi, Giuseppe Bono, Ivo Saviane
Figure caption: Number density (top) and EW density (bottom) distributions toward Cyg OB2 No. 12. The bin width is 500 Å in all panels. The black, gray, and white bars show DIBs with EW > 100 m Å, 10 < EW < 100 m Å, and EW < 10 m Å, respectively.
Paper: The GALPROP Cosmic-ray Propagation and Nonthermal Emissions Framework: Release v57
Authors: T. A. Porter, G. Jóhannesson, I. V. Moskalenko
Figure caption: CR source density and X CO Galactocentric radial distributions used for the 2D CR propagation model parameter optimization example. CR source distributions: SNR (solid, red) and pulsar (long dashed, red). X CO distributions: constant (solid, black) and R dependent (long dashed, black). The CR source density is normalized at the solar system’s location. Note the different scales for the left and right axes.
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: Top: numerical accretion disk transfer function for LSST ugrizy filters calculated for the following set of parameters: SMBH mass M = 2 · 108 M ⊙, L/L Edd ∼ 0.1, η = 0.1, disk inclination of 45◦, and azimuth angle of 0◦. Dashed vertical lines mark the theoretical centroid delay (Equation (5)) for comparison with the peaks for each transfer function (values given in the upper-right corner). Middle: convolution (in colors) of transfer function and a sinusoid of 2.5 days period (shown in dashed black). Bottom: synthetic LSST light curves obtained by convolution of the driving light curve, the flux of which is scaled (black line) and inclined AD transfer function shown in top panel. Different bands are plotted with the same color coding in all plots.
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: Schematic comparison of emission patterns across viewing angles for different AD models as given by the phenomenological approximation of Campitiello et al. (2018; see their Figure 2). The classical nonrelativistic model (dashed blue line) is compared with relativistic models with a = − 1 (dark blue curve), a = 0 (dark purple curve), a ∼ 0.8 (red curve), and a = 0.998 (orange curve). The radial axis is the observed efficiency ﹩{\eta }_{{\rm{o}}}=\tfrac{{L}^{{\rm{o}}}}{\dot{M}{c}^{2}}﹩, i.e., given by the observed luminosity normalized on the accretion rate (which is the same for each model). The plot plane is the accretion disk plane. The main axis of all models is in the direction of 0◦, assuming azimuthal symmetry with respect to this direction. A distant observer is at the left of the figure.
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: Distribution of ratio of the time delay calculated from a relativistic and a classical spacetime approximation, when a → 1. The inclination of the observer is set to ﹩i=\tfrac{\pi }{3}﹩, the region extent to 10r g, and the SMBH mass is 108 M ⊙. The dark green color depicts a ratio value of ∼1.075. The small white circle is a ‘plunging region’ inside the marginally stable orbit of r ms = 1.24r g. The color bar shows the ratio between relativistic and classical time lags. The ratio is highest where the light-bending effects are largest, i.e., near the SMBH. As the distance increases, the ratio approaches 1, because spacetime is almost flat.
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: Flat accretion disk time delay distributions (﹩\tau (r,\theta ,i)=r(1+\cos \theta \sin i)/c﹩), as seen by a distant observer, for various inclinations i given on top of each plot. The theoretical observer position is to the bottom at infinity. The color bar (in units of days) indicates time lag values. Distributions are deformed from circular to elliptical and becomes parabolic for the extreme inclination i = π/2. The observer will witness the re-emitted light arriving with delays ranging from 0 to ﹩2r(1+\cos \theta \sin i)/c﹩, with a bulk average delay of ﹩r(1+\cos \theta \sin i)/c﹩ for radius r and azimuth θ of the reprocessing site, with r ∈ [0, 10] lt-days. Our disk model reiterates the concept of isodelay surfaces as described in Peterson (2006) and Starkey et al. (2016).
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: Left: distribution of quasars per expected time lag with respect to the u-band filter based on an ideal set of uniform distributed masses in the range 106–1010 M ⊙. Right: PDF of expected time lag with respect to the u band for the 208 quasars sample from Liu et al. (2019) and Shen et al. (2011) catalogs located in COSMOS.
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 theoretical PR relations for the F-mode pulsators and α ml = 1.5 are compared to independent results available in the literature. The different panels show the results for different metallicity values, increasing from top (Z = 0.004) to bottom (Z = 0.03), and different cases for the assumed ML relation: A (left panels), B (middle panels), and C (right panels). In each panel, a (x-axis) and b (y-axis) with their uncertainties for all the considered assumptions are plotted. The theoretical results of this work are indicated with black symbols, while the literature results are plotted using different colors (see the labels). The dark and light gray areas indicate the 1σ error and 3σ intervals, respectively, of the a and b values of our PR relations.
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: As in Figure 5, but subtracting the PR relations for Z = 0.006 and Z = 0.002 provided by Anderson et al. (2016), from the one obtained in this work for Z = 0.004 and α ml = 1.5, as a function of the pulsational period. The top and bottom panels show the results for the F and FO-mode pulsators, respectively. The left panels contain the results for the canonical case A while the central and right panels contain the results for the noncanonical cases B and C, respectively. In each panel, the residuals for Z = 0.006 and Z = 0.002 are plotted using light blue and orange dots, respectively.
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: Parallax differences between the theoretical parallaxes obtained by adopting the PWZ relation and Gaia parallaxes (ϖ  T  − ϖ  G ) as a function of Gaia EDR3 parallax ϖ  G , for F-mode Galactic Cepheids.
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: This figure shows the residuals, obtained by subtracting the PR relations for F pulsators provided by Bono et al. (1998) from the ones derived in this work, chosen as fiducial lines, as a function of the pulsational period. In the top, central, and bottom panels, the results for Z = 0.004, Z = 0.008, and Z = 0.02 are shown, respectively. In each panel, different ML assumptions are represented with different colors: light blue dots for the canonical case A, and orange dots for the noncanonical case B.
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: F and FO ISs for Z = 0.004 and Y = 0.25, Z = 0.008 and Y = 0.25, Z = 0.02 and Y = 0.28, and Z = 0.03 and Y = 0.28 pulsators for a fixed case A ML relation for the various assumptions about the superadiabatic convective efficiency (left panels) and at a fixed mixing length parameter of α ml = 1.5 for the assumed A, B, and C ML relations (right 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: Locations of F and FO-mode pulsators (green plus and blue points, respectively) for Z = 0.004 (upper panels), Z = 0.008 (middle panels), and Z = 0.02 (bottom panels) in the log(P–G) plane. The solid and dashed black lines are the theoretical F and FO-mode IS boundaries, respectively, for the labeled ML and α ml assumptions.
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 for cadences from baseline and carina observing strategies for observed time lags of 1, 2, 3, and 5 days. The color bar displays metric values above the Nyquist threshold, which have been scaled for improved visual presentation in the Aitoff projection of celestial coordinates.
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 A1 but for euclid_dither1 and euclid_dither3 observing strategies. In all metric simulations, three DDFs stand out. For better color visibility in the right column, the metric threshold is multiplied by XXX.
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 realizations on cadences from long_gaps_nightsoff observing strategy. The first row of panels shows the fields (in the third and fourth area from the left of the main meridian) suitable for calculating 1–3 day delays. DDFs appear in the bottom row with better metric realization in the i band than in the r band.
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 from footprint observing strategies. There is only one prominent field in each panel (except panel (g)) slightly varying in position on the sky.
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 for cadences from footprint observing strategies, continued. In contrast to Figure A3, DDFs appear in panels (e) and (f).
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 rolling_all_sky_ns2 cadences continued. DDFs appear in all panels.
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 rolling_all_sky_ns2 cadences. Panels (a)–(c) show the fields (in the fourth area from the left of the main meridian) suitable for calculating 1–3 day delays. DDFs appear in panels (d) and (e).
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 multishort cadences continued. DDFs appear in all panels except (b), (c), 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 multishort cadences. DDFs appear in panel (l).
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 a fixed mixing length parameter of α ml = 1.5 for Z = 0.004 and Y = 0.25 (black dots), Z = 0.008 and Y = 0.25 (light blue dots), Z = 0.02 and Y = 0.28 (green dots), and Z = 0.03 and Y = 0.28 (orange dot). The coefficients of the FO-mode pulsators are not shown for Z = 0.03 because the models were too few to allow for an accurate regression.