adsabs/AstroCLIMB huggingface dataset:
Paper: Galactic Contribution to the High-energy Neutrino Flux Found in Track-like IceCube Events
Authors: Y. Y. Kovalev, A. V. Plavin, S. V. Troitsky
Figure caption: Distribution of the median absolute Galactic latitude, ∣b∣med, for 107 samples simulated under the assumption of the null hypothesis of the neutrino flux isotropy. The orange line indicates the value of ∣b∣med = 21° for the sample of observed events. Note the log scale in the vertical axis.
Paper: Galactic Contribution to the High-energy Neutrino Flux Found in Track-like IceCube Events
Authors: Y. Y. Kovalev, A. V. Plavin, S. V. Troitsky
Figure caption: Distributions of real (orange) and simulated (blue) events in the absolute Galactic latitude ∣b∣ of their arrival directions. The expected number of scrambled events in each bin is estimated by averaging 105 random samples.
Paper: Galactic Contribution to the High-energy Neutrino Flux Found in Track-like IceCube Events
Authors: Y. Y. Kovalev, A. V. Plavin, S. V. Troitsky
Figure caption: The median absolute Galactic latitude of events with muon energy above ﹩{E}_{\mu }^{\min }﹩ in the 10 yr IceCube muon-track catalog (top), and their fraction within 20° from the Galactic plane (bottom). Simulated confidence intervals are shown at a 68% level. The apparent wobble at high energies is due to a progressively smaller number of events.
Paper: Interacting Kilonovae: Long-lasting Electromagnetic Counterparts to Binary Mergers in the Accretion Disks of Active Galactic Nuclei
Authors: Jia Ren, Ken Chen, Yun Wang, Zi-Gao Dai
Figure caption: Same as Figure 2, but for SMBHs with accretion rate ﹩{\dot{M}}_{\bullet }={\dot{M}}_{\bullet ,\mathrm{Edd}}﹩.
Paper: Two Remarkably Luminous Galaxy Candidates at z ≈ 10–12 Revealed by JWST
Authors: Rohan P. Naidu, Pascal A. Oesch, Pieter van Dokkum, Erica J. Nelson, Katherine A. Suess, Gabriel Brammer, Katherine E. Whitaker, Garth Illingworth, Rychard Bouwens, Sandro Tacchella, Jorryt Matthee, Natalie Allen, Rachel Bezanson, Charlie Conroy, Ivo Labbe, Joel Leja, Ecaterina Leonova, Dan Magee, Sedona H. Price, David J. Setton, Victoria Strait, Mauro Stefanon, Sune Toft, John R. Weaver, Andrea Weibel
Figure caption: Summary of photometry and redshift solution for GL-z12. Top: 4.″5 × 4.″5 images spanning ≈0.9–4.5 μm centered on the z ≈ 12 candidate highlighted with white crosshairs. The source is well detected (>20σ) in F200W and all redder bands, and abruptly drops out in the bluer filters. Bottom left: photometry for the source is shown in purple, with upper limits for nondetections plotted at the 1σ level. The best-fit SED template from EAZY is shown in dark orange—a Lyman-break galaxy (LBG) at z = 12.2. The best-fit SED from EAZY constrained to lie at z < 6 is plotted in silver, which corresponds to a quiescent galaxy at z ≈ 3.5 whose Balmer break produces a drop-off across F200W and F150W. However, such a quiescent galaxy is predicted to be detected (>5σ) in bluer bands, and is at odds with the dramatic >1.8 mag break observed. Bottom right: probability distributions for the source redshift derived using EAZY (solid orange) and Prospector (dashed orange). We adopt a flat prior across the redshift range depicted (z = 0–20). The derived distributions are in excellent agreement and suggest a redshift of z ≈ 12, with negligible (EAZY) or no (Prospector) support for solutions at z < 10.
Paper: Two Remarkably Luminous Galaxy Candidates at z ≈ 10–12 Revealed by JWST
Authors: Rohan P. Naidu, Pascal A. Oesch, Pieter van Dokkum, Erica J. Nelson, Katherine A. Suess, Gabriel Brammer, Katherine E. Whitaker, Garth Illingworth, Rychard Bouwens, Sandro Tacchella, Jorryt Matthee, Natalie Allen, Rachel Bezanson, Charlie Conroy, Ivo Labbe, Joel Leja, Ecaterina Leonova, Dan Magee, Sedona H. Price, David J. Setton, Victoria Strait, Mauro Stefanon, Sune Toft, John R. Weaver, Andrea Weibel
Figure caption: Summary of photometry and redshift solution for GL-z10, similar to Figure 1. Top: GL-z10 is well detected in all but the two bluest bands. Bottom left: the best-fit low-z solution (quiescent galaxy at z ≈ 2.5) is disfavored by the F115W image, where a >5σ detection is expected. In addition to the JWST data (dark purple), we measure HST photometry (light purple) for this source from data acquired by the BUFFALO program (Steinhardt et al. 2020). The HST data are fully consistent with the JWST data as well as the best-fit SED. Bottom right: the EAZY and Prospector posteriors agree on a z ≈ 10 galaxy.
Paper: Two Remarkably Luminous Galaxy Candidates at z ≈ 10–12 Revealed by JWST
Authors: Rohan P. Naidu, Pascal A. Oesch, Pieter van Dokkum, Erica J. Nelson, Katherine A. Suess, Gabriel Brammer, Katherine E. Whitaker, Garth Illingworth, Rychard Bouwens, Sandro Tacchella, Jorryt Matthee, Natalie Allen, Rachel Bezanson, Charlie Conroy, Ivo Labbe, Joel Leja, Ecaterina Leonova, Dan Magee, Sedona H. Price, David J. Setton, Victoria Strait, Mauro Stefanon, Sune Toft, John R. Weaver, Andrea Weibel
Figure caption: Constraints on the bright end of the UV LF at z ∼ 10–13. The current JWST data allow us to derive a first estimate of the number density of galaxies with M UV ∼ − 21 at these redshifts (purple star). While this estimate lies a factor ∼10× above the extrapolation of the Schechter function constraints to z = 11.5 from Bouwens et al. (2021) (dashed black line), they are in very good agreement with extrapolated double power-law LFs from Bowler et al. (2020) (black solid line). In fact, GN-z11 (orange star) is also consistent with the double power-law LF. Other LF estimates and upper limits at z ∼ 10 are shown as open symbols (see the legend for references). Simulated predictions are shown from the UniverseMachine models at z ∼ 11 and z ∼ 12 (dotted lines) and from the Delphi model at z ∼ 11 (darker gray shaded region).
Paper: Two Remarkably Luminous Galaxy Candidates at z ≈ 10–12 Revealed by JWST
Authors: Rohan P. Naidu, Pascal A. Oesch, Pieter van Dokkum, Erica J. Nelson, Katherine A. Suess, Gabriel Brammer, Katherine E. Whitaker, Garth Illingworth, Rychard Bouwens, Sandro Tacchella, Jorryt Matthee, Natalie Allen, Rachel Bezanson, Charlie Conroy, Ivo Labbe, Joel Leja, Ecaterina Leonova, Dan Magee, Sedona H. Price, David J. Setton, Victoria Strait, Mauro Stefanon, Sune Toft, John R. Weaver, Andrea Weibel
Figure caption: Absolute UV magnitude vs. redshift for a representative sample of known galaxies in the first billion years of the universe. Galaxies with photometric redshifts, sourced from Bouwens et al. (2022), are shown as points, and those with spectroscopic redshifts compiled from the literature as squares. The candidates presented in this work are depicted as purple stars, and populate a hitherto unoccupied region of parameter space. The brightness of these sources present a unique opportunity to efficiently extend the spectroscopic frontier to the first few 100 Myr after the Big Bang.
Paper: Two Remarkably Luminous Galaxy Candidates at z ≈ 10–12 Revealed by JWST
Authors: Rohan P. Naidu, Pascal A. Oesch, Pieter van Dokkum, Erica J. Nelson, Katherine A. Suess, Gabriel Brammer, Katherine E. Whitaker, Garth Illingworth, Rychard Bouwens, Sandro Tacchella, Jorryt Matthee, Natalie Allen, Rachel Bezanson, Charlie Conroy, Ivo Labbe, Joel Leja, Ecaterina Leonova, Dan Magee, Sedona H. Price, David J. Setton, Victoria Strait, Mauro Stefanon, Sune Toft, John R. Weaver, Andrea Weibel
Figure caption: Comparison of SEDs (left) and p(z) distributions (right) derived based on initial NIRCam calibrations available at the time of the ERS data release (light blue) with results based on updated calibrations used in this Paper (orange). Photometry from the initial calibrations is shown in the left panels in transparent purple, and from the updated calibrations in solid purple. The SEDs are broadly similar, with the updated calibrations implying slightly lower redshifts for both sources. The high-redshift nature of these sources remains secure.
Paper: Two Remarkably Luminous Galaxy Candidates at z ≈ 10–12 Revealed by JWST
Authors: Rohan P. Naidu, Pascal A. Oesch, Pieter van Dokkum, Erica J. Nelson, Katherine A. Suess, Gabriel Brammer, Katherine E. Whitaker, Garth Illingworth, Rychard Bouwens, Sandro Tacchella, Jorryt Matthee, Natalie Allen, Rachel Bezanson, Charlie Conroy, Ivo Labbe, Joel Leja, Ecaterina Leonova, Dan Magee, Sedona H. Price, David J. Setton, Victoria Strait, Mauro Stefanon, Sune Toft, John R. Weaver, Andrea Weibel
Figure caption: Results of the GALFIT morphology analysis for our two sources (GL-z10 top and GL-z12 bottom). The different columns from left to right correspond to the original data (in the F444W filter), the model, and the residual. The sizes and Sérsic profiles of both sources are well constrained. GL-z10 shows some clear extension, consistent with a disk galaxy of 0.7 kpc at z ∼ 11. GL-z12 appears quite compact with an estimated size of 0.5 kpc.
Paper: The Emission Properties of RRAT J0139+3336 at 1.25 GHz
Authors: Jintao Xie, Jingbo Wang, Na Wang, Feifei Kou, Shuangqiang Wang, Shengnan Sun
Figure caption: Left: the polarization profile at 1.25 GHz, including total intensity (black curve), linear polarization (red curve), and circular polarization (blue curve). Upper panel shows the linear polarization position angle in degrees, and green curve represents the fitting result using RVM model. Right: the results of fitting an RVM curve for each (α, β) combination. The reduced chi-squared of the fit is expressed in terms of color depth, with darker blue values corresponding to a better fit. The black contours correspond to 1σ−, 2σ−, and 3σ confidence boundaries. The green areas indicate the constraints given according to certain theoretical assumptions and observed parameters.
Paper: The Emission Properties of RRAT J0139+3336 at 1.25 GHz
Authors: Jintao Xie, Jingbo Wang, Na Wang, Feifei Kou, Shuangqiang Wang, Shengnan Sun
Figure caption: Fitting a sample of single-pulse spectral indices for RRAT J0139+3336. The spectral index fit for each single pulse corresponds to the single pulse in Figure 1. Each pulse spectral index fit has the same frequency and flux density scales. The scaled mean flux density is obtained from Equation (5) and is plotted against frequency in logarithmic space.
Paper: The Emission Properties of RRAT J0139+3336 at 1.25 GHz
Authors: Jintao Xie, Jingbo Wang, Na Wang, Feifei Kou, Shuangqiang Wang, Shengnan Sun
Figure caption: Normalized cumulative distribution of pulse peak flux (upper panel) and the energy (the lower panel) for single pulses detected. The best-fit log-normal is shown in the red dashed curve. In addition we fit the distribution with a pure Weibull (blue), gamma (green), power law (orange), and exponential (black), respectively, which cannot describe the observed distribution well. The numbers in the legend are the p values corresponding to the fitted distributions.
Paper: The Emission Properties of RRAT J0139+3336 at 1.25 GHz
Authors: Jintao Xie, Jingbo Wang, Na Wang, Feifei Kou, Shuangqiang Wang, Shengnan Sun
Figure caption: The distribution of 152 single-pulse spectral indices for RRAT J0139+3336.
Paper: The Emission Properties of RRAT J0139+3336 at 1.25 GHz
Authors: Jintao Xie, Jingbo Wang, Na Wang, Feifei Kou, Shuangqiang Wang, Shengnan Sun
Figure caption: Histogram of the distribution of interval pulses between subsequent pulses; the solid red line is the result of fitting with an exponential distribution.
Paper: Reconciling Parker Solar Probe Observations and Magnetohydrodynamic Theory
Authors: Tommaso Alberti, Simone Benella, Giuseppe Consolini, Mirko Stumpo, Roberto Benzi
Figure caption: The joint distribution of the values of the normalized cross-helicity σ  C  and the normalized residual energy σ  R  within two heliocentric ranges: close to the Sun (R ∈ [0.1, 0.3] au) and far away (R ∈ [0.6–0.8] au). The color bar is the percentage ratio between the counts in each bin and the total number of calibrated (good quality) data points.
Paper: Reconciling Parker Solar Probe Observations and Magnetohydrodynamic Theory
Authors: Tommaso Alberti, Simone Benella, Giuseppe Consolini, Mirko Stumpo, Roberto Benzi
Figure caption: The radial dependence of the reduced cross-helicity σ  C  (blue) and the residual energy σ  R  (red).
Paper: Reconciling Parker Solar Probe Observations and Magnetohydrodynamic Theory
Authors: Tommaso Alberti, Simone Benella, Giuseppe Consolini, Mirko Stumpo, Roberto Benzi
Figure caption: As in Figure 3 but separating slow (V < 400 km s−1, upper panels) and fast (V > 400 km s−1, lower panels) solar wind intervals.
Paper: CME-related Large Decreases in the Differential Phase Delay of Tianwen-1 DOR Signals
Authors: Qingbao He, Zhichao Wang, Qinghui Liu, Kaijun Liu, Li Guo
Figure caption: Solar wind parameters from 2021 March 21 to 26 (a)–(g) and from 2021 June 17 to 23 (h)–(n). From top to bottom in each column, the red curves display the solar wind density, speed, temperature, total magnetic field, and the three magnetic field components in the radial–tangential–normal coordinates (B  R , B  T , and B  N ) observed by STEREO A, respectively. The blue curves in Figure 3(a)–(d) present the solar wind density, speed, temperature, and the total magnetic field near Earth. The two pairs of green vertical dashed lines delineate the VLBI observation time ranges on 2021 March 23 and June 18, respectively. The three black vertical dashed lines in each column mark the front shocks, sheath regions, and the trailing edges of the CMEs observed by STEREO A.
Paper: CME-related Large Decreases in the Differential Phase Delay of Tianwen-1 DOR Signals
Authors: Qingbao He, Zhichao Wang, Qinghui Liu, Kaijun Liu, Li Guo
Figure caption: Differential phase delays and their corresponding TEC changes (right axes) during selected time intervals on 2020 July 31 (a), 2021 March 23 (b), and 2021 June 18 (c), respectively. The differential phase delay in (a) contains the influence of the Earth's ionosphere, while the ionosphere contribution has been removed in the differential phase delays shown in (b) and (c). The red curve in (a) is the Earth's ionosphere TEC change calculated from GNSS data.
Paper: CME-related Large Decreases in the Differential Phase Delay of Tianwen-1 DOR Signals
Authors: Qingbao He, Zhichao Wang, Qinghui Liu, Kaijun Liu, Li Guo
Figure caption: Solar wind structures on 2021 March 23 (a) and 2021 June 18 (b) predicted by the WSA–Enlil model. The Earth and Mars positions and the corresponding DOR signal path are also marked.
Paper: CME-related Large Decreases in the Differential Phase Delay of Tianwen-1 DOR Signals
Authors: Qingbao He, Zhichao Wang, Qinghui Liu, Kaijun Liu, Li Guo
Figure caption: White-light solar corona images observed by SOHO/LASCO-C3 on 2021 March 20 (a) and 2021 June 15 (b). The black arrows point to the CMEs.
Paper: The Halo Bias inside Cosmic Voids
Authors: Giovanni Verza, Carmelita Carbone, Alessandro Renzi
Figure caption: The p v(r) and q v(r) parameters, along the void profile, of the multiplicity function associated to our HMF model in Equation (6), fitted to simulated measurements in stacked void shells, for voids traced by halos with M ≥ 1013 h −1 M ⊙ at z = 1.05, 0.49, 0. The upper panels show the 68% and 95% confidence level in the p–q plane. The contour colors denote the distance from the void center according to the color bar on the right, and the black stars, together with the dotted–dashed blue and dotted orange lines, represent p U and q U. The lower panels show the same quantities as a function of r: p v(r) is represented by the blue solid lines, q v(r) by the orange dashed lines, p U by the blue dashed–dotted horizontal lines, and q U by the orange dotted horizontal lines. Note that the p and q axes in the lower panels have a different scale with respect to the upper panels.
Paper: The Halo Bias inside Cosmic Voids
Authors: Giovanni Verza, Carmelita Carbone, Alessandro Renzi
Figure caption: Stacked density profiles for voids traced by halos with M ≥ 1013 h −1 M ⊙ at redshifts z = 0, 0.49, 1.05 (left), and for various minimum halo masses, M = 2.5 × 1012 h −1 M ⊙, 1013 h −1 M ⊙, 2.5 × 1013 h −1 M ⊙, at z = 1.05 (right). The solid lines show the density profiles in the halo distributions, ﹩{\delta }_{{\rm{h}}}^{{\rm{v}}}(r)﹩, the dashed lines in the underlying matter distribution, ﹩{\delta }_{{\rm{m}}}^{{\rm{v}}}(r)﹩, within the halo-traced voids. The transparent lines show the analytical profile, ﹩{\delta }_{{\rm{m}}}^{{\rm{A}}}(r)﹩, of Hamaus et al. (2014a) fitted against ﹩{\delta }_{{\rm{m}}}^{{\rm{v}}}(r)﹩.
Paper: The Emission Properties of RRAT J0139+3336 at 1.25 GHz
Authors: Jintao Xie, Jingbo Wang, Na Wang, Feifei Kou, Shuangqiang Wang, Shengnan Sun
Figure caption: Sample of single pulses of RRAT J0139+3336. The dedispersed frequency-time plot for the single pulse is displayed in the top panel. The black line in the bottom panel of each plot shows the pulse profile after accumulating the frequencies, and the red line is the fitted multi-Gaussian Gaussian template. The green dashed line indicates the difference between the fitted line and the observed profile. Red numbers are the index of single pulses.
Paper: Observational Inference on the Delay Time Distribution of Short Gamma-Ray Bursts
Authors: Michael Zevin, Anya E. Nugent, Susmita Adhikari, Wen-fai Fong, Daniel E. Holz, Luke Zoltan Kelley
Figure caption: Constraints on DTD parameters when including all host associations with P cc ≤ 0.20 in the inference (filled blue), as well as three subsets that only include samples that have P cc ≤ 0.02 (yellow; Gold Association), samples that have spectroscopic redshifts (green), and samples that have spectroscopic redshifts and P cc ≤ 0.02 (pink). The contours show the 50% and 90% credible regions, with dotted lines marking the median for each marginalized distribution. The gray dashed lines in the panels plotting the marginal distributions show the prior distribution for each parameter, which is uniform for all parameters of the DTD. Both kernel density estimates and binned histograms are shown for the marginal distributions.
Paper: Observational Inference on the Delay Time Distribution of Short Gamma-Ray Bursts
Authors: Michael Zevin, Anya E. Nugent, Susmita Adhikari, Wen-fai Fong, Daniel E. Holz, Luke Zoltan Kelley
Figure caption: Expected merger rate evolution of BNSs based on our DTD constraints. The black line (right axis) shows the SFR density evolution from Madau & Fragos (2017). The colored lines (left axis) match the set of samples used in the inference as in Figure 1 and show the predicted BNS comoving merger rate density for random draws from our DTD parameter inference, assuming their progenitor stars are born according to the SFR density of Madau & Fragos (2017). The black dashed line shows the expected BNS merger rate evolution assuming fiducial DTD values of α = −1, ﹩{t}_{\min }=10\,\mathrm{Myr}﹩, and ﹩{t}_{\max }=14\,\mathrm{Gyr}﹩. The shaded gray region shows the local BNS merger rate density constraints from Abbott et al. (2021b).
Paper: Observational Inference on the Delay Time Distribution of Short Gamma-Ray Bursts
Authors: Michael Zevin, Anya E. Nugent, Susmita Adhikari, Wen-fai Fong, Daniel E. Holz, Luke Zoltan Kelley
Figure caption: DTDs constructed from random draws of our posterior distribution. The colored lines match the set of samples used in the inference as in Figure 1. The black solid, dashed, and dotted lines show fiducial DTDs with power-law slopes α of −1, −1.5, and −2, respectively, for comparison. We show this set of fiducial distributions for ﹩{t}_{\min }=10\,\mathrm{Myr}﹩ and ﹩{t}_{\min }=100\,\mathrm{Myr}﹩, with ﹩{t}_{\max }﹩ fixed at 100 Gyr.
Paper: The Emission Properties of RRAT J0139+3336 at 1.25 GHz
Authors: Jintao Xie, Jingbo Wang, Na Wang, Feifei Kou, Shuangqiang Wang, Shengnan Sun
Figure caption: The solid gray line indicates the ACF of the dynamic spectrum with signal-to-noise ratios above 60 at the observed frequency, and the solid red line is their best-fit Gaussian model.
Paper: The Emission Properties of RRAT J0139+3336 at 1.25 GHz
Authors: Jintao Xie, Jingbo Wang, Na Wang, Feifei Kou, Shuangqiang Wang, Shengnan Sun
Figure caption: A dynamic spectrum of the single pulses from RRAT J0139+3336 at 1.25 GHz.
Paper: Reconciling Parker Solar Probe Observations and Magnetohydrodynamic Theory
Authors: Tommaso Alberti, Simone Benella, Giuseppe Consolini, Mirko Stumpo, Roberto Benzi
Figure caption: (From top to bottom) The plasma bulk speed V, the Alfvén speed ﹩{V}_{{\rm{A}}}=21.8\,\tfrac{B}{\sqrt{n}}﹩ (B in units of nT, n in units of cm−3), and the PSP radial distance to the Sun R. Dark and light blue lines in the top panel refer to slow (V < 400 km s−1) and fast (V > 400 km s−1) solar wind intervals, respectively.
Paper: Galactic Contribution to the High-energy Neutrino Flux Found in Track-like IceCube Events
Authors: Y. Y. Kovalev, A. V. Plavin, S. V. Troitsky
Figure caption: Arrival directions (white dots) of the 70 IceCube events studied in the present work superimposed on the all-sky gamma-ray map, equatorial coordinates. The black star denotes the Galactic center. The color in the map reflects the intensity of the gamma-ray flux with energies above 1 GeV observed by Fermi-LAT (https://svs.gsfc.nasa.gov/14090), with the emission from the Galactic plane clearly seen. Fermi sky map credit: NASA/DOE/Fermi LAT Collaboration.
Paper: Discovery of a Binary-origin Classical Cepheid in a Binary System with a 59 day Orbital Period 
Authors: Bogumił Pilecki, Ian B. Thompson, Felipe Espinoza-Arancibia, Richard I. Anderson, Wolfgang Gieren, Weronika Narloch, Javier Minniti, Grzegorz Pietrzyński, Mónica Taormina, Giuseppe Bono, Gergely Hajdu
Figure caption: Example evolutionary tracks for stars with masses expected for components of OGLE-LMC-CEP-1347 assuming single star evolution. The position of the Cepheid with a 1O period of 0.690 day and the corresponding instability strip are shown. The hypothetical position of the companion with the same age as the Cepheid clearly contradicts the observational data (it should be cooler than the Cepheid).
Paper: Discovery of a Binary-origin Classical Cepheid in a Binary System with a 59 day Orbital Period 
Authors: Bogumił Pilecki, Ian B. Thompson, Felipe Espinoza-Arancibia, Richard I. Anderson, Wolfgang Gieren, Weronika Narloch, Javier Minniti, Grzegorz Pietrzyński, Mónica Taormina, Giuseppe Bono, Gergely Hajdu
Figure caption: (Left) Orbital radial velocity curves with a preliminary orbital solution. The 1O mode variation for the Cepheid was subtracted. The orbit is circular and different semiamplitudes indicate the companion is about two times less massive. (Right) Pulsational RV curve for 1O mode with orbital variation removed. High scatter of the Cepheid RVs around the fits comes from the unaccounted 2O pulsation. Measurement errors are smaller than the plotting points.(The data used to create this figure are available.)
Paper: Discovery of a Binary-origin Classical Cepheid in a Binary System with a 59 day Orbital Period 
Authors: Bogumił Pilecki, Ian B. Thompson, Felipe Espinoza-Arancibia, Richard I. Anderson, Wolfgang Gieren, Weronika Narloch, Javier Minniti, Grzegorz Pietrzyński, Mónica Taormina, Giuseppe Bono, Gergely Hajdu
Figure caption:  I-band light curves showing variability for the first (1O) and second-overtone (2O) modes with the same y-axis span. Data come from the OGLE project (Soszyński et al. 2017) and were disentangled to show variability in each mode separately.
Paper: Discovery of a Binary-origin Classical Cepheid in a Binary System with a 59 day Orbital Period 
Authors: Bogumił Pilecki, Ian B. Thompson, Felipe Espinoza-Arancibia, Richard I. Anderson, Wolfgang Gieren, Weronika Narloch, Javier Minniti, Grzegorz Pietrzyński, Mónica Taormina, Giuseppe Bono, Gergely Hajdu
Figure caption: Broadening function profiles of the Cepheid (blue) and the companion (red) for one of the UVES spectra. The signal from the Cepheid is ∼4 times stronger indicating the companion is significantly fainter (see text).