adsabs/AstroCLIMB huggingface dataset:
Paper: Up, Up, and Away: Winds and Dynamical Structure as a Function of Altitude in the Ultrahot Jupiter WASP-76b
Authors: Aurora Y. Kesseli, Hayley Beltz, Emily Rauscher, I. A. G. Snellen
Figure caption: Binary-mask CCFs for Cr I (top), V I (middle) and Mn I (bottom). The CCF masks have been split into two different opacity bins and coadded in the planet’s rest frame in a similar manner as Figure 4. As in Figure 4, we have also plotted the Gaussian fits to each CCF with dotted lines of the same color, and the peak radial velocity of the fitted Gaussian as a vertical dashed line. Even though the CCFs are noisier than the Fe I CCF, we still measure an SNR >3.5 in each case, and >4.5 in most cases. For all three species we observe the same pattern where the CCFs created using the stronger lines are less blueshifted than the CCFs created using the weaker lines.
Paper: Up, Up, and Away: Winds and Dynamical Structure as a Function of Altitude in the Ultrahot Jupiter WASP-76b
Authors: Aurora Y. Kesseli, Hayley Beltz, Emily Rauscher, I. A. G. Snellen
Figure caption: Comparison between the 1D, phase-averaged CCFs for the real atmospheric signal (black solid line) and the three different model atmospheres described in Section 3 that have been injected into the data (colored solid lines). We also plot the central radial velocity that was obtained by fitting a Gaussian to each CCF with a dashed vertical line. We find that the models underestimate that Fe signal strength at all altitudes, but that this underestimation is worst at the top of the atmosphere, where the Fe in the planet likely is absorbing above the top of the model atmosphere (10−5 bars), therefore we do not perform any comparisons between the GCM models and the strong-line bin for the remainder of the paper to avoid biasing our analysis. We also see that in all cases the models predict the signal to be less blueshifted than the data show.
Paper: Up, Up, and Away: Winds and Dynamical Structure as a Function of Altitude in the Ultrahot Jupiter WASP-76b
Authors: Aurora Y. Kesseli, Hayley Beltz, Emily Rauscher, I. A. G. Snellen
Figure caption: CCFs where the three different models are injected into the data at many times the expected signal strength to create “zero-noise" model CCFs. As with the data, the CCFs are created with only the middle Fe I lines (left three panels) and only the weak Fe I lines (right three panels). The CCFs are also split into the phases covering the beginning of the transit (ϕ −, light red) and end of the transit (ϕ +, maroon). The real Fe I signal from the planet is also plotted in the same manner in transparent blue (ϕ −) and black (ϕ +).
Paper: Stealth Non-standard-model Confined Flare Eruptions: Sudden Reconnection Events in Ostensibly Inert Magnetic Arches from Sunspots
Authors: Ronald L. Moore, Sanjiv K. Tiwari, Navdeep K. Panesar, V. Aparna, Alphonse C. Sterling
Figure caption: The R. L. Moore et al. (2001) schematic of the standard model for confined flare eruptions and ejective flare eruptions in lone bipolar active regions. Solid curves are magnetic field lines. The dashed curve is the active region's PIL. The elongated shaded feature in the first panel is a filament of dark chromospheric-temperature plasma suspended in the active region's sheared core field above the PIL. Dark areas are flare ribbons at the feet of reconnected field lines. The background ragged arc is the chromospheric limb.
Paper: Pursuing Truth: Improving Retrievals on Mid-infrared Exo-Earth Spectra with Physically Motivated Water Abundance Profiles and Cloud Models
Authors: Björn S. Konrad, Sascha P. Quanz, Eleonora Alei, Robin Wordsworth
Figure caption:  P−T fits (top row) and flux residuals (bottom row) for the retrievals on the simulated R = 100, S/N = 20 Earth spectrum. Each column provides the results for a different retrieval model (from left to right: ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{C}},\mathrm{CF}}﹩, ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CF}}﹩, and ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩). Color-shaded areas indicate retrieval percentiles (from light to dark colors: 5%−95%, 15%−85%, 25%−75%, and 35%−65%). In the P−T figures, white squares mark the true surface conditions (P 0, T 0), and white circles the true P−T structure. The inlay in the top right of the P−T panel shows the retrieved constraints on the surface conditions. In the flux residual figures, the gray-shaded area indicates the assumed 1σ photon noise level.
Paper: Pursuing Truth: Improving Retrievals on Mid-infrared Exo-Earth Spectra with Physically Motivated Water Abundance Profiles and Cloud Models
Authors: Björn S. Konrad, Sascha P. Quanz, Eleonora Alei, Robin Wordsworth
Figure caption: Ground truths and disk-integrated MIR spectra for the NP, SP, and EqC Earth views introduced in Section 2.3.2. Solid lines indicate the data for January, and dashed lines represent the month of July. Color-shaded areas indicate the uncertainties on the data. Left column: ground truth P−T profiles. Center column: ground truth abundance profiles for CO2, O3, CH4, and H2O. Right column: R = 50 disk-integrated monthly averaged Earth spectra. The color-shaded areas indicate the S/N = 10 LIFESIM noise level.
Paper: Pursuing Truth: Improving Retrievals on Mid-infrared Exo-Earth Spectra with Physically Motivated Water Abundance Profiles and Cloud Models
Authors: Björn S. Konrad, Sascha P. Quanz, Eleonora Alei, Robin Wordsworth
Figure caption: Posteriors from retrievals on the simulated R = 100, S/N = 20 Earth spectrum. Here, L(·) stands for ﹩{\mathrm{log}}_{10}(\cdot )﹩. Thick black lines indicate pressure-independent ground truths. Thin gray lines show the true H2O abundance at 1 bar (solid line) and at 10−1 bar (dashed line). The different markers represent the retrieval models: orange circles—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{C}},\mathrm{CF}}﹩, green squares—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CF}}﹩, and blue triangles—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩. The colored lines indicate the 16%–84% posterior percentiles. For the ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CF}}﹩ and ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩ models, which assume variable H2O profiles, we provide both the retrieved H2O abundance at P 0 (dark marker color) and at 1 dex below P 0 (light marker color).
Paper: JADES: Spectroscopic Confirmation and Proper Motion for a T-Dwarf at 2 kpc
Authors: Kevin N. Hainline, Francesco D'Eugenio, Fengwu Sun, Jakob M. Helton, Brittany E. Miles, Mark S. Marley, Ben W. P. Lew, Jarron M. Leisenring, Andrew J. Bunker, Phillip A. Cargile, Stefano Carniani, Daniel J. Eisenstein, Ignas Juodžbalis, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer
Figure caption: (Top) 1D NIRSpec PRISM spectrum for JADES-GS-BD-9, with ATMO2020++ (red) LOWZ (blue), and Sonora Elf Owl (orange) fits. The best-fit parameters are shown in the legend above. We split the spectrum to help focus on the near-IR (left) and 3–5 μm region (right). (Bottom) Residuals for the three fits. All three models match the observed spectrum within the uncertainties, and all three predict a subsolar metallicity for the brown dwarf.
Paper: JADES: Spectroscopic Confirmation and Proper Motion for a T-Dwarf at 2 kpc
Authors: Kevin N. Hainline, Francesco D'Eugenio, Fengwu Sun, Jakob M. Helton, Brittany E. Miles, Mark S. Marley, Ben W. P. Lew, Jarron M. Leisenring, Andrew J. Bunker, Phillip A. Cargile, Stefano Carniani, Daniel J. Eisenstein, Ignas Juodžbalis, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer
Figure caption: A comparison of the position of JADES-GS-BD-9 (first row) and three nearby bright galaxies (second, third, and fourth rows) in the 2022 JADES images (left column), 2023 JADES images (middle column), and in a difference image of the 2 yr (right column). We can see that, while JADES-GS-BD-9 has a proper motion shown by the changing centroid position and positive and negative flux in the difference image, the other nearby galaxies show no motions or significant residuals.
Paper: Pursuing Truth: Improving Retrievals on Mid-infrared Exo-Earth Spectra with Physically Motivated Water Abundance Profiles and Cloud Models
Authors: Björn S. Konrad, Sascha P. Quanz, Eleonora Alei, Robin Wordsworth
Figure caption:  P−T and abundance profiles assumed for the simulated Earth input spectrum (Section 2.3.1). Top-left panel: assumed Earth-like P−T structure (solid blue line) and position of the cloud layer (dotted red line). Top-right panel: vertical profiles of the considered atmospheric gases. Bottom panel: calculated cloud-free (dashed green line), cloudy (dashed–dotted red line), and partially cloudy (f C = 0.67; solid black line) Earth spectra. The gray-shaded area indicates the S/N = 20 photon noise level assumed for the partially cloudy input spectrum.
Paper: Pursuing Truth: Improving Retrievals on Mid-infrared Exo-Earth Spectra with Physically Motivated Water Abundance Profiles and Cloud Models
Authors: Björn S. Konrad, Sascha P. Quanz, Eleonora Alei, Robin Wordsworth
Figure caption: H2O profiles calculated using the condensation model (Section 2.1.1) for the EqC Jul Earth view (Section 2.3.2). Left panel: the ground truth P−T profile for the EqC Jul view of Earth. Right panel: the ground truth H2O profile as a thick blue line together with the H2O profiles calculated for different ﹩{\delta }_{{{\rm{H}}}_{2}{\rm{O}}}﹩ values.
Paper: Pursuing Truth: Improving Retrievals on Mid-infrared Exo-Earth Spectra with Physically Motivated Water Abundance Profiles and Cloud Models
Authors: Björn S. Konrad, Sascha P. Quanz, Eleonora Alei, Robin Wordsworth
Figure caption: Noise models for the R = 100, S/N = 20 spectra. The blue dashed line shows the photon noise assumed for the simulated Earth spectrum. The LIFESIM noise assumed for the disk-integrated Earth spectra is shown as solid red lines. Both noise models reach an S/N of 20 at 11.2 μm (indicated by the black dotted lines).
Paper: Pursuing Truth: Improving Retrievals on Mid-infrared Exo-Earth Spectra with Physically Motivated Water Abundance Profiles and Cloud Models
Authors: Björn S. Konrad, Sascha P. Quanz, Eleonora Alei, Robin Wordsworth
Figure caption:  P−T fits (top row) and flux residuals (bottom row) for the retrievals on the R = 100, S/N = 10 EqC Jul spectrum of Earth. Each column provides the results for a different retrieval model (from left to right: ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{C}},\mathrm{CF}}﹩, ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CF}}﹩, and ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩). Color-shaded areas indicate retrieval percentiles (from light to dark colors: 5%–95%, 15%–85%, 25%–75%, and 35%–65%). In the P−T figures, white squares mark the true surface conditions (P 0, T 0), and white circles the true P−T structure. The inlay in the top right of the P−T panel shows the retrieved constraints on the surface conditions (P 0, T 0) for the ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{C}},\mathrm{CF}}﹩ case. For the ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CF}}﹩ and ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩ scenario, the inlay shows the pressure and temperature where the atmosphere becomes opaque (P Op., T Op.). In the flux residual figures, the gray-shaded area indicates the assumed 1σ LIFESIM noise level.
Paper: Pursuing Truth: Improving Retrievals on Mid-infrared Exo-Earth Spectra with Physically Motivated Water Abundance Profiles and Cloud Models
Authors: Björn S. Konrad, Sascha P. Quanz, Eleonora Alei, Robin Wordsworth
Figure caption: Posteriors from retrievals on the six disk-integrated Earth spectra for the S/N = 10 LIFESIM noise scenarios. Here, L(·) stands for ﹩{\mathrm{log}}_{10}(\cdot )﹩. Thick black lines indicate pressure-independent ground truths. Thin gray lines show the ground truth abundances at different atmospheric pressures (solid: 1 bar; dashed: 10−1 bar; dashed–dotted: 10−2 bar; dotted: 10−3 bar). The markers represent the retrieval models: orange circles—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{C}},\mathrm{CF}}﹩, green squares—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CF}}﹩, and blue triangles—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩. The colored lines indicate the 16%–84% posterior percentiles. For the ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CF}}﹩ and ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩ models, which assume variable H2O profiles, we provide both the retrieved H2O abundance at the pressure P Op. where the atmosphere becomes optically thick (dark marker color) and at 1 dex below P Op. (light marker color).
Paper: Pursuing Truth: Improving Retrievals on Mid-infrared Exo-Earth Spectra with Physically Motivated Water Abundance Profiles and Cloud Models
Authors: Björn S. Konrad, Sascha P. Quanz, Eleonora Alei, Robin Wordsworth
Figure caption: Posteriors from retrievals on the six disk-integrated Earth spectra for the S/N = 20 LIFESIM noise scenarios. Here, L(·) stands for ﹩{\mathrm{log}}_{10}(\cdot )﹩. Thick black lines indicate pressure-independent ground truths. Thin gray lines show the ground truth abundances at different atmospheric pressures (solid: 1 bar; dashed: 10−1 bar; dashed–dotted: 10−2 bar; dotted: 10−3 bar). The markers represent the retrieval models: orange circles—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{C}},\mathrm{CF}}﹩, green squares—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CF}}﹩, and blue triangles—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩. The colored lines indicate the 16%–84% posterior percentiles. For the ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CF}}﹩ and ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩ models, which assume variable H2O profiles, we provide both the retrieved H2O abundance at the pressure P Op. where the atmosphere becomes optically thick (dark marker color) and at 1 dex below P Op. (light marker color).
Paper: Pursuing Truth: Improving Retrievals on Mid-infrared Exo-Earth Spectra with Physically Motivated Water Abundance Profiles and Cloud Models
Authors: Björn S. Konrad, Sascha P. Quanz, Eleonora Alei, Robin Wordsworth
Figure caption: Posteriors from the retrievals on the EqC Jul spectra of Earth (LIFESIM S/N = 10; R = 50, 100). Here, L(·) stands for ﹩{\mathrm{log}}_{10}(\cdot )﹩. Thick black lines indicate pressure-independent ground truths. Thin gray lines show the ground truth abundances at different atmospheric pressures (solid: 1 bar; dashed: 10−1 bar; dashed–dotted: 10−2 bar; dotted: 10−3 bar). The markers represent the retrieval models: orange circles—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{C}},\mathrm{CF}}﹩, green squares—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CF}}﹩, and blue triangles—﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩. The colored lines indicate the 16%–84% posterior percentiles. For the ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CF}}﹩ and ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩ models, which assume variable H2O profiles, we provide both the retrieved H2O abundance at the pressure P Op. where the atmosphere becomes optically thick (dark marker color) and at 1 dex below P Op. (light marker color).
Paper: Pursuing Truth: Improving Retrievals on Mid-infrared Exo-Earth Spectra with Physically Motivated Water Abundance Profiles and Cloud Models
Authors: Björn S. Konrad, Sascha P. Quanz, Eleonora Alei, Robin Wordsworth
Figure caption: Corner plot for the f C, R pl, and T 0 posteriors (in blue) for the retrieval with the ﹩{{\boldsymbol{ \mathcal M }}}_{{\rm{V}},\mathrm{CL}}﹩ forward model on the simulated R = 100, S/N = 20 Earth spectrum. The black dashed lines and the circular orange markers indicate the parameter ground truths.
Paper: From the Shadows: The Impact of Nightside Thermal Emission on Ultrahot Jupiter Transmission Spectrum Retrievals
Authors: John A. Kappelmeier, Ryan J. MacDonald, Nikole K. Lewis
Figure caption: Impact of nightside emission on multidimensional transmission spectra of the ultrahot Jupiter WASP-33b. Upper left: model transmission spectra of WASP-33b including nightside thermal emission (red; via Equations (1) and (5)) and without nightside emission (blue). For clarity, both spectra are shown binned to a spectral resolution of R = 100. Lower left: residuals between the transmission spectra with and without nightside thermal emission. The model differences significantly increase with wavelength. Right: 2D geometry of the corresponding WASP-33b model. Stellar rays pass through the day–night terminator, emerging from the nightside, such that the observer sees both transmitted starlight and nightside thermal emission.
Paper: From the Shadows: The Impact of Nightside Thermal Emission on Ultrahot Jupiter Transmission Spectrum Retrievals
Authors: John A. Kappelmeier, Ryan J. MacDonald, Nikole K. Lewis
Figure caption: Expected biases in the observed transit depth at 5 μm for confirmed transiting exoplanets with known planetary radii and semimajor axes. Each dot represents one of these confirmed exoplanets. The x-axis represents the ratio between the estimated nightside temperature (see Equation (9)) and the temperature of the host star. The y-axis represents the ratio between the planetary and stellar radius for each exoplanet. Planets with a higher expected bias caused by nightside emission (as calculated from Equation (8)) are shown with a brighter color on a log scale. The exoplanet we focused our paper on, WASP-33b, is indicated on the plot as a star for comparison. Data from https://exoplanet.eu/ (accessed on 2024 May 14).
Paper: From the Shadows: The Impact of Nightside Thermal Emission on Ultrahot Jupiter Transmission Spectrum Retrievals
Authors: John A. Kappelmeier, Ryan J. MacDonald, Nikole K. Lewis
Figure caption: Schematic diagram illustrating the role of nightside emission during an ultrahot Jupiter transit. The stellar flux from the host star transmits through the exoplanet’s atmosphere before reaching the observer, encoding information about its atmospheric properties. The transmission spectrum can be affected by chemical composition gradients between the dayside and nightside, represented here by the relative numbers of TiO and VO molecules shown on each hemisphere. The observer also receives thermal flux from the planetary nightside. The final transmission spectrum is thus influenced by both the day–night atmospheric property gradients along the path of the stellar rays and the nightside thermal emission. Multidimensional models are therefore required to jointly consider how the nightside affects transmitted starlight and thermal emission. Hot Jupiter concept art adapted from NASA/JPL-Caltech/T. Pyle.
Paper: Constraints on Compact Dark Matter from the Nonobservation of Gravitational-wave Strong Lensing
Authors: A. Barsode, S. J. Kapadia, P. Ajith
Figure caption: Distribution of the ratio of μ 1 calculated assuming double or single lensing. Vertical dashed lines indicate the 10th and 90th percentile bounds.
Paper: A View of the Long-term Spectral Behavior of Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, E. M. Cackett, J. A. García, J. M. Miller, D. R. Wilkins
Figure caption: The overall flux of the system is poorly correlated with the inner disk radius. We see the lowest flux states display some degree of truncation, as stated in D. L. Moutard et al. (2023), but there are also higher flux states that are truncated just as heavily, if not more so. To test whether the observed disk truncation is caused by magnetic fields surrounding the NS, we plot the magnetosphere radius for various limits. Assuming our magnetic field upper limit (red dashed line) is well characterized by the lowest flux point does not yield a magnetosphere radius consistent with most measured R in values. If instead we use a different low flux, seemingly truncated observation to characterize the magnetic field strength (blue dashed line), we find a slightly better relation, though it still cannot be concluded that the magnetic field is the sole source of inner disk truncation in this system. k  A , f ang, and η are all degenerate, so it is possible to make these magnetic field radii very small or very large, even using reasonable values for this parameter.
Paper: A View of the Long-term Spectral Behavior of Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, E. M. Cackett, J. A. García, J. M. Miller, D. R. Wilkins
Figure caption: A comparison of the reduced χ 2 values for the observations when fit only with a continuum vs. when fit with a reflection component. We see that a reflection component significantly improves the reduced χ 2 statistics for all observations. This should not be understood as a robust statistical comparison of the models but rather as a quick reference to determine whether a reflection component significantly improves the fit quality. The values shown here correspond to an average χ 2 improvement of ∼1566 for the additional 6 dof. Note: the two models are binned differently for readability.
Paper: A View of the Long-term Spectral Behavior of Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, E. M. Cackett, J. A. García, J. M. Miller, D. R. Wilkins
Figure caption: An example of three unfolded NICER spectra with the relevant model components. We show here (a) the lowest flux observation, obsid = 4701010301, (b) an intermediate flux observation, obsid = 1050020236, and the highest flux observation, obsid = 1050020252. These display the range of fluxes we see across these observations, as well as the most relevant components for various fluxes. In (a), we see the power law is dominant and remains relatively flat out to the highest energies, while in (c) the cutoff and preference for a stronger thermal component becomes more apparent. In each, the O VIII feature is visible around 0.7 keV.
Paper: A View of the Long-term Spectral Behavior of Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, E. M. Cackett, J. A. García, J. M. Miller, D. R. Wilkins
Figure caption: The hardness–intensity diagram for the soft color (1.1–2.0 keV/0.5–1.1 keV) and the hard color (3.8–6.8 keV/2.0–3.8 keV), as well as the color–color diagram for all 51 observations. The observations are binned into 150 s segments for clarity. We see that the hard color stays relatively constant throughout all observations, but the soft color varies more distinctly over time.
Paper: A View of the Long-term Spectral Behavior of Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, E. M. Cackett, J. A. García, J. M. Miller, D. R. Wilkins
Figure caption: Long-term MAXI light curve in blue points with the start date of each observation overlaid as dashed lines. The top row of plots highlights specific 20 days regions of the light curve, demonstrating that the source is captured in various states. These zoomed-in plots also display the quasiperiodic nature of the flux of the source.
Paper: A View of the Long-term Spectral Behavior of Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, E. M. Cackett, J. A. García, J. M. Miller, D. R. Wilkins
Figure caption: Shown here are the six archival NuSTAR spectra. The five most recent spectra have comparable slopes in the higher energy bands, but the earliest observation, 30363002002, is noticeably different. This means that we cannot effectively use NuSTAR observations that are not simultaneous with NICER observations to constrain continuum parameters for the broader study.
Paper: A View of the Long-term Spectral Behavior of Ultracompact X-Ray Binary 4U 0614+091
Authors: D. L. Moutard, R. M. Ludlam, E. M. Cackett, J. A. García, J. M. Miller, D. R. Wilkins
Figure caption: Shown are the fluxes of each component for each observation plotted against the overall flux of the system. In general, the component fluxes are well correlated with the overall flux (spearman rank ≥0.75), with the exception of the power-law flux, which is anticorrelated (spearman rank ∼ −0.5).