adsabs/AstroCLIMB huggingface dataset:
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: The turbulence power spectra of the four high resolution 2563 runs shown in Figure 6, where Z/Z ⊙ = 0.3 and n = 0.1 cm−3, and ﹩{\dot{\epsilon }}_{i}﹩ being 0.01, 0.1, 1.0, and 10.0 erg s−1 g−1 from left to right. The bottom row plots the turbulence power spectra during steady-state turbulence, after t  s , 10t s, and 100t s, as well as k −5/3 reference lines representing the inertial regime of the Kolmogorov spectrum. The cyan colored region represents 1σ across the last 20 outputs of the steady-state turbulence epoch. The top row plots the power spectra from turbulence turnoff up to 100t s, with the color denoting ϵ  k . The value of t  s  is also shown across each of the four runs. Both the top and bottom row plots are smoothed using quintic polynomial splines for visualization purposes. The leftmost ﹩{\dot{\epsilon }}_{i}=0.01\,\mathrm{erg}\,{{\rm{s}}}^{-1}\,{{\rm{g}}}^{-1}﹩ column does not show a 100t s power spectrum since the simulation run ended before 100t s.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: The dissipation of the clumping factor 〈ρ 2〉/〈ρ〉2 − 1 over time. Consistent with previous plots, the colored lines show various binnings in initial simulation parameters across supersonic runs. The black line and shaded region shows the average and 1σ across all subsonic runs, and the dotted line shows 5σ across all time steps for all subsonic runs. Top: clumping factor dissipation binned in ﹩{\dot{\epsilon }}_{i}﹩. Bottom: clumping factor dissipation binned in n.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: Normalized (top two) and unnormalized (bottom two) energy dissipation curves over time. Specific energy is normalized by initial sound speed ﹩{c}_{s,0}^{2}﹩, and time is normalized by kinetic saturation time t  s . The shaded regions represent 1σ error regions, and each colored curve represents different values of ﹩{\dot{\epsilon }}_{i}﹩. The first and third plots show thermal energy, and the second and fourth plots show kinetic energy.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: Phase plots showing the time tracks of thermal vs. kinetic energy for 2563 resolution runs corresponding to Z/Z ⊙ = 0.3 and n = 0.1 cm−3. Stars denote the turbulence driving turnoff time where each curve begins, circular dots denote t  s , 10t s, and 100t s as one moves from the star and along the curve, and the squares denote t = 100 Myr. The black line represents the x = y line.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: A similar plot as Figure 5 but with curves binned in n as opposed to ﹩{\dot{\epsilon }}_{i}﹩. The shaded regions represent 1σ. The thermal energy (top) plot shows only Z/Z ⊙ = 1 runs with the shaded regions only representing variations in ﹩{\dot{\epsilon }}_{i}﹩, while the kinetic energy (bottom) plot shows all metallicity runs with the shaded regions representing variations in both Z and ﹩{\dot{\epsilon }}_{i}﹩. The black dotted line represents the specific thermal energy floor corresponding to the 1000 K temperature floor.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: A comparison between our thermal and kinetic dissipation curves and the kinetic dissipation curves of J. M. Stone et al. (1998; black), E. C. Ostriker et al. (1999; cyan), and E. C. Ostriker et al. (2001; magenta). The latter three curves show dissipation under artificial viscosity, an isothermal equation of state, and the presence of magnetic fields where ﹩B\,={\beta }^{-1/2}\times 1.4\,{\left(T/10\,{\rm{K}}\right)}^{1/2}(n/{10}^{2}\,{\mathrm{cm}}^{-3})\,\mu {\rm{G}}﹩ (so β = ∞ represents pure hydrodynamics). The cyan and magenta dissipation curves include self-gravity. t sc,0 represents the sound crossing time at turbulence turnoff, defined as L/c  s,0. The energies are normalized by sound speed squared ﹩{c}_{s,0}^{2}﹩ right at turbulence driving turnoff.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: 2D contour maps of the half energy dissipation timescales t  h , defined as ϵ(t  h ) = 0.5ϵ 0, across only supersonic runs. The blank regions on the top left above the diagonal represent subsonic runs, and the blank regions on the bottom represent supersonic runs, which did not dissipate half the component of energy in question. The first and second rows shows total energy, the middle third and fourth rows show thermal energy, and the bottom fifth and sixth rows show kinetic energy.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: Dimensionless dissipation timescales t  h , defined as ϵ(t  h ) = 0.5ϵ 0, for both kinetic (top) and thermal (bottom) energy as a function of ﹩{\dot{\epsilon }}_{i}﹩. Kinetic energy is normalized by t cross,0 while thermal energy is normalized by t cool,0. Kinetic dissipation timescales are additionally separated between supersonic (blue) and subsonic (black) runs.
Paper: Cloud Crushing and Dissipation of Uniformly Driven Adiabatic Turbulence in Circumgalactic Media
Authors: Alex Lv, Lile Wang, Renyue Cen, Luis C. Ho
Figure caption: The dissipation rate of specific total energy, normalized by initial sound speed ﹩{c}_{s,0}^{2}﹩, over time for supersonic (green) and subsonic runs (red). ﹩{ \mathcal M }﹩ follows the same definition as the one in Figure 2, which is v avg/c  s,0, and t  s  represent the kinetic energy saturation time. The shaded error regions represent 1σ.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: 3D run. Magnitude and components of the perturbation vorticity (relative to the basic state) in the ϕ = 0 meridional plane at t/T 0 = 444.64. Turbulent shear layers are numbered (1)–(6) at the midplane and (A)–(B) at z/H 0 = 2.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Components of the perturbation vorticity (relative to the basic state) in the midplane at t/T 0 = 444.64. The dotted lines indicate regions of width Δr/H 0 adjacent to each radial boundary that are affected by boundary conditions, as indicated later in the plot of the turbulent α(r) parameter.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Components of the perturbation vorticity (relative to the basic state) at z = 2H 0 and t/T 0 = 444.64.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Specific energy spectra of individual velocity components in the midplane. Averaged over the time interval t/T 0 ∈ [400.20, 452.55]; ϵ filter = 0.015. (a) With respect to the radial wavenumber, k  r . (b) With respect to the azimuthal wavenumber, m.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Profiles of u  z (r) near the r min boundary at z/H 0 = −2 for the axisymmetric run with a white-noise initial perturbation.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Effect of the strength of the Padé filter (ϵ filter) on specific energy spectra in the midplane. (a) With respect to the radial wavenumber, k  r . (b) With respect to the azimuthal wavenumber, m. The units of S  uu  are those of velocity squared, i.e., ﹩{({H}_{0}/{T}_{0})}^{2}﹩.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption:  δ ω  z  at z = 2H 0 centered at ϕ = 90° (t/T 0 = 444.64).
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Perturbation vorticity pdf for the 3D run at t/T 0 = 444.64 sampled at 128 meridional planes.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Terms in the transport Equation (32) for ∂ z (δ j  z ).
Paper: Evidence for Mass-dependent Evolution of Transitional Dwarf Galaxies in the Virgo Cluster
Authors: Suk Kim, Soo-Chang Rey, Youngdae Lee
Figure caption: (Main panel) Stellar mass (and r-band luminosity) vs. clustercentric distance for dwarf galaxies with different morphological types in the EVCC: dEs (red circles), dS0s (yellow circles), ETdG(bc)s (blue dots), and dIrrs (green dots). The distributions of dEs and dS0s are highlighted by the red fuzzy and black contours, respectively. (Upper panel) Fraction of bright galaxies (Mr<−16) against the clustercentric distance for dwarf galaxies of different types: red, yellow, blue, and green circles and lines for dEs, dS0s, ETdG(bc)s, and dIrrs, respectively. The bold solid curves are illustrated for each type of galaxy, obtained using a running average with a bin width of 2 deg and an incremental step of 0.1 deg. (Right panel) FUV – r CMD for different types of dwarf galaxies. The symbols and contours are identical to those in the main panel. The red vertical line denotes the color cut of FUV − r = 5.5, which is used to differentiate between star-forming and quiescent galaxies.
Paper: Evidence for Mass-dependent Evolution of Transitional Dwarf Galaxies in the Virgo Cluster
Authors: Suk Kim, Soo-Chang Rey, Youngdae Lee
Figure caption: PPS diagram of dwarf galaxies with various morphological types in the EVCC: dEs (red circles), dS0s (yellow circles), ETdG(bc)s (blue dots), and dIrrs (green dots). The y-axis is the line-of-sight velocity relative to the cluster mean radial velocity (Δv), normalized by the velocity dispersion of the Virgo cluster (σcl). Open squares denote ETdGs exhibiting SF with FUV − r < 5.5. The black dashed curve indicates the escape velocity of the Virgo cluster. The red solid curve delimits the region where the ram pressure exceeds the restoring force provided by the gravitational potential of a galaxy with a stellar mass of ~108M⊙. The dotted line represents the virialized region.
Paper: Evidence for Mass-dependent Evolution of Transitional Dwarf Galaxies in the Virgo Cluster
Authors: Suk Kim, Soo-Chang Rey, Youngdae Lee
Figure caption: (Top and middle panels) PPS diagrams of bright (Mr < −16, top panels) and faint (Mr > −16, middle panels) dEs (left panels), and dS0s (right panels). Filled circles with various colors represent galaxies in different regions: yellow for the stripped region, red for the virialized region, green for the recently infall region, and blue for outside the escape velocity curve. All curves are identical to those shown in Figure 5. (Bottom panels) Luminosity distributions of dS0s (left panel) and dEs (right panel) in each region of the PPS diagram. The colors of the curves denote different regions and correspond to the colors of the galaxies shown in both the upper and middle panels.
Paper: Evidence for Mass-dependent Evolution of Transitional Dwarf Galaxies in the Virgo Cluster
Authors: Suk Kim, Soo-Chang Rey, Youngdae Lee
Figure caption: Fraction of morphological types as a function of the projected clustercentric distance for dEs and dIrrs (top panel), and dS0s and ETdG(bc)s (bottom panel). The fractions of the different morphological types are shown as filled circles, and the number of galaxies for each filled circle is indicated. The solid and dashed curves indicate the fractions obtained from the EVCC and VCC, respectively. The bold solid curves for the EVCC in both panels are obtained by a running average with a bin width of 2 deg and an incremental step of 0.1 deg. The linear black solid lines are linear least-square fits to the fractions of dEs (top panel) and dS0s (bottom panel) in the outer region beyond 3.5 deg (∼0.7Rvir).
Paper: Evidence for Mass-dependent Evolution of Transitional Dwarf Galaxies in the Virgo Cluster
Authors: Suk Kim, Soo-Chang Rey, Youngdae Lee
Figure caption: (a), (b), and (c) Projected spatial distributions of galaxies with different morphological types. Panel (a) shows the spatial distribution of dEs (red circles) and dS0s (yellow circles) in the VCC. Panels (b) and (c) show the spatial distributions of dEs (red circles)/dS0s (yellow circles)/ETdG(bc)s (blue dots) and dIrrs (green crosses) in the EVCC, respectively. (d) Cumulative radial distributions of different morphological types in the EVCC as a function of the distance from the M87 (black cross in panels (a), (b), and (c). Various line types provide distributions for dEs, dS0s, ETdG(bc)s, dIrrs, Es, and late-type (Sa–Sd) galaxies.
Paper: Evidence for Mass-dependent Evolution of Transitional Dwarf Galaxies in the Virgo Cluster
Authors: Suk Kim, Soo-Chang Rey, Youngdae Lee
Figure caption: Examples of four VCC dEs reclassified as dS0s in the EVCC. In each galaxy, the left panel denotes the g-, r-, and i-band combined color image of DECaLS data, which provides greater depth than the SDSS image. The right panel shows the residual image provided by DECaLS resulting from the ellipse fit and the subsequent modeling of the light distribution. The residual images clearly show unambiguous disk substructures, including spiral arms for EVCC 586 and EVCC 1154, a bar for EVCC 250, and a disk for EVCC 1162.
Paper: On the Acceleration Site of Anomalous Cosmic Rays: Voyager 2 Observations of Their Anisotropy in the Heliosheath
Authors: A. C. Cummings, J. Kóta, J. D. Richardson, J. S. Rankin, B. C. Heikkila
Figure caption: Top panel: R components of the observed anisotropy flow vector (labeled CRS δ) and of the C-G anisotropy flow vector (labeled Compton–Getting δ) for all 51 good-fit rolls. The C-G values are from the PLS VR speeds on the roll days, with data removed during the rolls, divided by the C-G factor F in Tables 1 and 2 of A. C. Cummings et al. (2021). Bottom panel: resulting diffusive R component of the ACR anisotropy flow vector formed from the difference of the observed δ R and the δ CG, i.e., δ R–δ CG. The vertical lines mark the termination shock (dotted) and heliopause (dashed) crossings.
Paper: On the Acceleration Site of Anomalous Cosmic Rays: Voyager 2 Observations of Their Anisotropy in the Heliosheath
Authors: A. C. Cummings, J. Kóta, J. D. Richardson, J. S. Rankin, B. C. Heikkila
Figure caption: Top panel: uncorrected angle of the solar wind flow in the R–T plane vs. time. The blue circles represent long-term averages and the green squares show the data for the days of the magrols. Middle panel: same as the top panel except for the RN angle. Bottom left panel: histogram of differences between RT angles for the magrol days and the long-term average for the period in which the magrol occurs. The vertical lines mark the ±1σ values from the mean. Magrol days beyond the 1σ limits were eliminated from the analysis. Bottom right panel: same as bottom left panel except for the RN angle.
Paper: On the Acceleration Site of Anomalous Cosmic Rays: Voyager 2 Observations of Their Anisotropy in the Heliosheath
Authors: A. C. Cummings, J. Kóta, J. D. Richardson, J. S. Rankin, B. C. Heikkila
Figure caption: T and N components of the diffusive anisotropy flow vectors as described in the main text.
Paper: On the Acceleration Site of Anomalous Cosmic Rays: Voyager 2 Observations of Their Anisotropy in the Heliosheath
Authors: A. C. Cummings, J. Kóta, J. D. Richardson, J. S. Rankin, B. C. Heikkila
Figure caption: Top panel: uncorrected RT flow angle (open symbols) and the corrected angle (solid symbols) vs. time. The solid blue circles represent long-term averages where the correction can be accurately estimated. The green squares represent data from the days of selected magrols. The selection and correction procedures are described in the main text. Bottom panel: same as top panel except for the RN angle.
Paper: On the Acceleration Site of Anomalous Cosmic Rays: Voyager 2 Observations of Their Anisotropy in the Heliosheath
Authors: A. C. Cummings, J. Kóta, J. D. Richardson, J. S. Rankin, B. C. Heikkila
Figure caption: Top panel: T components of the measured anisotropy vectors from A. C. Cummings et al. (2021) for the final 25 selected roll days. In addition, the C-G components are shown and based on the corrected solar wind speeds from PLS and the C-G factors, F, which are from Tables 1 and 2 in A. C. Cummings et al. (2021). Bottom panel: same as top panel except for the N component.
Paper: On the Acceleration Site of Anomalous Cosmic Rays: Voyager 2 Observations of Their Anisotropy in the Heliosheath
Authors: A. C. Cummings, J. Kóta, J. D. Richardson, J. S. Rankin, B. C. Heikkila
Figure caption: Top panel: corrected solar wind T component from PLS data for selected magrols. Bottom panel: same as top panel except for N component. The correction is for the out-of-FOV effect described in the main text.
Paper: On the Acceleration Site of Anomalous Cosmic Rays: Voyager 2 Observations of Their Anisotropy in the Heliosheath
Authors: A. C. Cummings, J. Kóta, J. D. Richardson, J. S. Rankin, B. C. Heikkila
Figure caption: Color contours (blue is low, red is high) of simulated ACR proton intensities around the TS. At low energies (∼0.5 MeV, panel (a)) ACR fluxes are organized by the TS: intensities increase sharply at/near the TS and remain at about the same level beyond the TS. At higher ACR energies (∼12 MeV, panel (b)) ACR fluxes continue to increase beyond the TS on the front side and have maximum intensity at the tailside of the TS. The TS is modeled as an offset circle (dashed blue line); the tightly wound spiral field is shown between 60 and 80 au only. Computations start at 60 au from the Sun. Dotted lines on both panels indicate V2's trajectory. The open squares in panel (a) show V2's position at the TS crossing and 5.3 yr later. The asterisk in panel (b) shows V2's position when the spacecraft has direct magnetic connection to the very back of the TS.
Paper: On the Acceleration Site of Anomalous Cosmic Rays: Voyager 2 Observations of Their Anisotropy in the Heliosheath
Authors: A. C. Cummings, J. Kóta, J. D. Richardson, J. S. Rankin, B. C. Heikkila
Figure caption: Predicted T component of the diffusive anisotropy of 0.5–35 MeV ACR protons along V2's trajectory as function of the time elapsed from the shock crossing (vertical dashed line labeled TS). The observations for the 0.5–35 MeV interval (solid symbols) are year averages from the top panel of Figure 6. Negative values imply a tail-to-nose streaming; the advection by the solar wind has been removed. The solid black line represents the total diffusive anisotropy predicted for the entire V2 0.5–35 MeV energy interval. The horizontal dotted line denotes zero diffusive anisotropy. The other dashed lines show the anisotropies in five different subintervals to indicate the expected energy dependence of the anisotropy. The vertical dotted line at ∼3.6 yr shows the location where V2 has the best/direct magnetic connection to the tail of the TS (asterisk in panel (b) of Figure 7).
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Apparent r′ magnitude vs. intrinsic (dereddened) ﹩(r^{\prime} -i^{\prime} )﹩ color. RBs and BWs are shown as red and black circles, respectively, with corresponding values taken from PS1 catalog magnitudes. The periodic variables and spider candidates identified in this work are marked with orange circles and different green symbols for each system, respectively. For both variables and candidates we plot the average value computed from their light curves, with dotted lines indicating their magnitude range on the y-axis and the standard deviation of their color on the x-axis.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: The γ-ray variability vs. γ-ray curvature significance plot, where all Fermi-LAT 3FGL sources are shown as gray filled circles, unidentified objects are shown as black open circles, identified pulsars are shown as blue filled circles, and COBIPULSE candidates are shown as red filled circles.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Top left panel: PDM periodogram of the r′-band light curve of J0737. Bottom left panel: zoom-in of the deepest minimum in the periodogram found at P best = 0.3548 ± 0.0005 days. Top right panel: light curves of J0737 in the g′, r′, and i′ optical bands folded on P best and reference epoch (minimum light) T 0 = 57336.219 MJD, with two cycles shown for display purposes. Bottom right panel: observed color curves of J0737 folded on P best.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Top left panel: PDM periodogram performed on the r′-band light curve of J2221. Bottom left panel: zoom-in of the deepest minimum in the periodogram found at P best = 0.165 ± 0.004 days. Top right panel: light curves of J2221 in the g′, r′, and i′ optical bands folded on P best and reference epoch T 0 = 57343.939 MJD, with two cycles shown for display purposes. Bottom right panel: observed color curves of J2221 folded on P best.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Top left panel: PDM periodogram performed on the r′-band light curve of J2117-A. Bottom left panel: zoom-in of the minimum in the periodogram found at P best = 0.0984 ± 0.0003 days. Top right panel: light curves of J2117-A in the g′, r′, and i′ optical bands folded at the photometric period P ZTF = 0.12664 days and reference epoch T 0 = 59025.415 MJD, estimated from the periodicity search on ZTF data, where two cycles are shown for display purposes. Bottom right panel: observed color curves of J2117-A folded at P ZTF.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Top left panel: PDM periodogram performed on the r′-band light curve of J2117-B. Bottom left panel: zoom-in of the minimum in the periodogram found at P best = 0.0959 ± 0.0003 days. Top right panel: light curves of J2117-B in the g′, r′, and i′ optical bands folded at the photometric period P ZTF = 0.2209805 days and reference epoch T 0 = 58745.308 MJD, estimated from the periodicity search on ZTF data, where two cycles are shown for display purposes. Bottom right panel: observed color curves of J2117-B folded at P ZTF.