adsabs/AstroCLIMB huggingface dataset:
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Critical points for computing diagnostic symmetry metrics are plotted across the spectrum (F), its first derivative (F″), and its second derivative (F″), in yellow for local maxima (continuum average, continuum difference), blue for negative minima of the second derivative (small window, jerk distance), brown for extrema of the first derivative (mass center), and purple for the local minimum (depth). In this 0.8 nm portion of the spectra, the left-hand line is marked as asymmetric and the right-hand line as symmetric.
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Phase-folded velocity plots of the best-fit Keplerians corresponding to the MCMC fits of Figure 11 for the symmetric, 2σ lines (left) and the symmetric, 2σ, R > 0.3 lines (right). Median phase-binned points for each depth bin are shown in yellow for deep lines, blue for mid-depth lines, and purple for shallow lines. Unbinned, phase-folded RVs for each depth bin are shown in gray. Colored curves show the best-fit radvel models.
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: NEID bulk RVs of HD 26965 (purple) overlaid on the best-fit Keplerian solution from Ma et al. (2018). Within the errors of Ma et al. (2018; propagated to the NEID measurement epochs), the proposed Keplerian is significantly out of phase with the dominant 42-day signal in the NEID data.
Paper: Foreground Dust Properties toward the Cluster NGC 7380
Authors: Sadhana Singh, Jeewan C. Pandey, Thiem Hoang, Neelam Panwar, Biman J. Medhi, Vishal Joshi, Shashikiran Ganesh
Figure caption: The plot between Stokes parameters Q and U in the V band. The three groups are shown in three different colors. The figure does not show one highly dispersed star (#32).
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Left: bulk RV correlation slope (y-axis) vs. line depth (x-axis) for different line selection populations (left to right): all lines with a depth greater than 0.05, symmetric lines, symmetric lines with ∣2σ∣ confidence in the measurement of their correlation, and lines that additionally correlate with bulk RV with a Pearson’s R coefficient of ∣R∣ ≥ ∣0.3∣. Though the log plots show only the positively correlated lines, the integrated RV signals do include negatively correlated lines that meet the above thresholds (see legends). Right: the corresponding depth-bin-integrated RV time series for the populations described above, offset for clarity. All integrated RVs seem to share a similar signal. The legends denote how many lines were used to compute the RVs in each depth bin. The depth bins are chosen to yield comparable overall RV uncertainty in each depth bin (1–3 m s−1 photon-limited error). The bins are 0.05–0.2, 0.25–0.4, and 0.5–0.65 in normalized depth.
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Overview of FF’ injection recovery experiment, applied to the measured bulk RVs of HD 26965. A 1.5 m s−1 signal was injected at two different periods: 32 days (top) and 42 days (bottom). Each period sampled five different relative phases (t 0/P) between the Keplerian signal and the stellar rotation/activity signal. Our FF’ model was then applied to the combined RV data, and a single Keplerian was fit to the residuals. The recovered semiamplitudes (K) are shown in the right column. In the case where the phase of the planet is at or near the activity, the recovery of the planet signal is significantly degraded when relying on the FF’ model alone, while injected signals that are out of phase with the activity are generally recovered more reliably.
Paper: A Search for Temporal Atmospheric Variability of Kepler Hot Jupiters
Authors: Canis Li, Avi Shporer
Figure caption: Secondary-eclipse and transit depths for Kepler-1 b (TrES-2 b), Kepler-2 b (HAT-P-7 b), Kepler-5 b, Kepler-6 b, Kepler-7 b, and Kepler-8 b. For each target, the secondary eclipse (upper subpanel) and transit (lower subpanel) depths by quarter (black) and by four-quarter window (blue) are displayed. In addition, the depth determined from all quarters stitched together is shown in red, with the 1σ uncertainty shaded in light red. In the secondary eclipse subpanels a dotted line is plotted at zero depth, for reference, depending on the plotted relative flux range.
Paper: Asteroseismological Analysis of the Non-Blazhko RRab Star EPIC 248846335 in the LAMOST–Kepler/K2 Project
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Xueying Hu, Bo Zhang, Jiaxin Wang, Gao-Chao Liu, Gang Meng, Gianni Catanzaro, Antonio Frasca, Haotian Wang, Weikai Zong
Figure caption: The radial velocity curves and their corresponding variations in radius. (a), (b) The radial velocities determined from the blue- and red-arm MRS of LAMOST DR9 are marked in blue and red, respectively. (c), (d) The variations in radius calculated based on the radial velocities estimated from the blue- and red-arm MRS using Equation (5), respectively.
Paper: A Search for Temporal Atmospheric Variability of Kepler Hot Jupiters
Authors: Canis Li, Avi Shporer
Figure caption: Phase-folded light curve of Kepler-488 b’s secondary eclipse (left) and transit (right), with the model light curve plotted in orange. The long-cadence observations are marked by the gray points in the background, and the solid black circles denote the binned light curve. The nuisance signal modeled by the GP has already been subtracted. The blue line denotes the secondary eclipse depth. The vertical orange dotted line is the center phase of the secondary eclipse, shown to be offset from the expected phase (0.00) assuming a circular orbit (see Section 4.2 for more details). The increase in the scatter of the in-transit residuals (bottom-right panel) is caused by spot-crossing events.
Paper: A Search for Temporal Atmospheric Variability of Kepler Hot Jupiters
Authors: Canis Li, Avi Shporer
Figure caption: Secondary-eclipse and transit depths for Kepler-12 b, Kepler-13 b (KOI-13 b), Kepler-15 b, Kepler-17 b, Kepler-18 c, and Kepler-41 b. Refer to Figure 1 for details.
Paper: Asteroseismological Analysis of the Non-Blazhko RRab Star EPIC 248846335 in the LAMOST–Kepler/K2 Project
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Xueying Hu, Bo Zhang, Jiaxin Wang, Gao-Chao Liu, Gang Meng, Gianni Catanzaro, Antonio Frasca, Haotian Wang, Weikai Zong
Figure caption: Determination of the best-fit model (residual r) of Sets A, B, C, and D. For better visibility, in panels (a), (c), (e), and (g), 1/r 2 is plotted as a function of mass (m ⊙) and T eff with the corresponding color scale for the four different sets of convective parameters; in panels (b), (d), (f), and (h), 1/r 2 is plotted as a function of metallicity ([Fe/H]) and luminosity (L ⊙) with the corresponding color scale for the four different sets of convective parameters.
Paper: A Search for Temporal Atmospheric Variability of Kepler Hot Jupiters
Authors: Canis Li, Avi Shporer
Figure caption: Secondary-eclipse and transit depths for Kepler-76 b, Kepler-412 b, Kepler-427 b, Kepler-488 b, and Kepler-1658 b. Refer to Figure 1 for details.
Paper: A Search for Temporal Atmospheric Variability of Kepler Hot Jupiters
Authors: Canis Li, Avi Shporer
Figure caption: Targets with clear seasonal variations (variability in the transit depth at 1 yr, or four quarters) not already plotted in Figure 1 or Figure 2. The upper and lower panel show Kepler-74 b and Kepler-471 b, respectively.
Paper: Asteroseismological Analysis of the Non-Blazhko RRab Star EPIC 248846335 in the LAMOST–Kepler/K2 Project
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Xueying Hu, Bo Zhang, Jiaxin Wang, Gao-Chao Liu, Gang Meng, Gianni Catanzaro, Antonio Frasca, Haotian Wang, Weikai Zong
Figure caption: (a) Light curves of EPIC 248846335 extracted with LightKurve (Barentsen et al. 2018, 2021); (b) the phase-folded light curve in the fundamental period.
Paper: Asteroseismological Analysis of the Non-Blazhko RRab Star EPIC 248846335 in the LAMOST–Kepler/K2 Project
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Xueying Hu, Bo Zhang, Jiaxin Wang, Gao-Chao Liu, Gang Meng, Gianni Catanzaro, Antonio Frasca, Haotian Wang, Weikai Zong
Figure caption: Hertzsprung–Russell diagram for comparison between the best-matching model to the star EPIC 248846335 and the HB models. Masses of models and evolutionary tracks are color-coded as indicated in the legend. The black circle is the optimal model of Set A given in Table 5. The blue and red dashed lines represent the blue and red edges of the instability strip (Fadeyev 2019), respectively.
Paper: Asteroseismological Analysis of the Non-Blazhko RRab Star EPIC 248846335 in the LAMOST–Kepler/K2 Project
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Xueying Hu, Bo Zhang, Jiaxin Wang, Gao-Chao Liu, Gang Meng, Gianni Catanzaro, Antonio Frasca, Haotian Wang, Weikai Zong
Figure caption: Upper panel: comparison between the RV curve (red) provided by the red-arm MRS of LAMOST DR9 and that produced by the RSP module of MESA. Bottom panel: the residuals of this comparison.
Paper: Asteroseismological Analysis of the Non-Blazhko RRab Star EPIC 248846335 in the LAMOST–Kepler/K2 Project
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Xueying Hu, Bo Zhang, Jiaxin Wang, Gao-Chao Liu, Gang Meng, Gianni Catanzaro, Antonio Frasca, Haotian Wang, Weikai Zong
Figure caption: Upper panel: comparison between the light curve (gray) observed by K2 and that produced by the RSP modules of MESA. Bottom panel: the residuals of this comparison.
Paper: Asteroseismological Analysis of the Non-Blazhko RRab Star EPIC 248846335 in the LAMOST–Kepler/K2 Project
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Xueying Hu, Bo Zhang, Jiaxin Wang, Gao-Chao Liu, Gang Meng, Gianni Catanzaro, Antonio Frasca, Haotian Wang, Weikai Zong
Figure caption: Upper panel: comparison between the RV curve (blue) provided by the blue-arm MRS of LAMOST DR9 and that produced by the RSP module of MESA. Bottom panel: the residuals of this comparison.
Paper: Modeling Circumstellar Gas Emission around a White Dwarf Using CLOUDY 
Authors: Siyi Xu, 偲艺 许, Sherry Yeh, Laura. K. Rogers, Amy Steele, Erik Dennihy, Alexandra E. Doyle, P. Dufour, Beth L. Klein, Christopher J. Manser, Carl Melis, Tinggui Wang, Alycia J. Weinberger
Figure caption: The complete spectra of Gaia J0611−6931 with flux calibration anchored to the SkyMapper photometry (red dots). The light blue, dark blue, and orange lines represent data from HST/COS, VLT/X-SHOOTER (UVB and VIS arms), and Gemini/Flamingos-2, respectively. The gray dots are data from the X-SHOOTER NIR arm and are only used for facilitating line identifications. The black lines mark emission features listed in Table 2.
Paper: Modeling Circumstellar Gas Emission around a White Dwarf Using CLOUDY 
Authors: Siyi Xu, 偲艺 许, Sherry Yeh, Laura. K. Rogers, Amy Steele, Erik Dennihy, Alexandra E. Doyle, P. Dufour, Beth L. Klein, Christopher J. Manser, Carl Melis, Tinggui Wang, Alycia J. Weinberger
Figure caption: A zoomed-in view around the Mg II 2796 Å region. The black line is the data, with the gray area indicating the uncertainty. The green line is the best-fit atmospheric model, where photospheric absorptions from Mg II are detected (Rogers et al. 2024). There are additional broad Mg II emission lines from the circumstellar gas.
Paper: Modeling Circumstellar Gas Emission around a White Dwarf Using CLOUDY 
Authors: Siyi Xu, 偲艺 许, Sherry Yeh, Laura. K. Rogers, Amy Steele, Erik Dennihy, Alexandra E. Doyle, P. Dufour, Beth L. Klein, Christopher J. Manser, Carl Melis, Tinggui Wang, Alycia J. Weinberger
Figure caption: A comparison between the observed Ca II 8500 Å line (black line with gray shading representing the uncertainties) and the models with different radial extents of the disk (colored lines). In the top panel, the models were scaled differently to match the overall emission line flux. In the bottom panel, the scaling factors are the same for all the models. Under the assumptions that the gas is optically thin with a constant density, the shape of the line profile is very sensitive to the outer radius of the gas. The model that best matches the observed line profile has a radial extent from 20R wd to 100R wd.
Paper: Modeling Circumstellar Gas Emission around a White Dwarf Using CLOUDY 
Authors: Siyi Xu, 偲艺 许, Sherry Yeh, Laura. K. Rogers, Amy Steele, Erik Dennihy, Alexandra E. Doyle, P. Dufour, Beth L. Klein, Christopher J. Manser, Carl Melis, Tinggui Wang, Alycia J. Weinberger
Figure caption: A compilation of all the unblended and resolved emission features listed in Table 2. The O I 8448 doublet is also included because the separation is only 0.1 Å. For each emission line, the continuum flux is normalized to 1 and then offset for clarity. The velocity is shown in the reference frame of the white dwarf; therefore, the narrow photospheric absorption lines in Ca II 3935 Å and O I 8448 Å appear to be at 0 km s−1. The black dashed line marks an FWZI of 1530 km s−1, which is the average width of these lines.
Paper: Modeling Circumstellar Gas Emission around a White Dwarf Using CLOUDY 
Authors: Siyi Xu, 偲艺 许, Sherry Yeh, Laura. K. Rogers, Amy Steele, Erik Dennihy, Alexandra E. Doyle, P. Dufour, Beth L. Klein, Christopher J. Manser, Carl Melis, Tinggui Wang, Alycia J. Weinberger
Figure caption: A top-down view of the geometry of the gas disk. The white dwarf is the blue star, and the gas disk is modeled as circular rings. For each small patch in the disk, the line-of-sight velocity V d,α  can be directly computed, and the emissivity can be obtained from CLOUDY.
Paper: Modeling Circumstellar Gas Emission around a White Dwarf Using CLOUDY 
Authors: Siyi Xu, 偲艺 许, Sherry Yeh, Laura. K. Rogers, Amy Steele, Erik Dennihy, Alexandra E. Doyle, P. Dufour, Beth L. Klein, Christopher J. Manser, Carl Melis, Tinggui Wang, Alycia J. Weinberger
Figure caption:  CLOUDY models’ prediction of the observed line flux as a function of the number density of each element (i.e., the curve of growth). The optically thin regions are marked as transparent circles, while the optically thick regions are marked as solid circles. The optical depth is measured radially. The shaded area represents the 3σ range of the observed line flux listed in Table 2. Most of the emission lines appear to be optically thick.
Paper: Modeling Circumstellar Gas Emission around a White Dwarf Using CLOUDY 
Authors: Siyi Xu, 偲艺 许, Sherry Yeh, Laura. K. Rogers, Amy Steele, Erik Dennihy, Alexandra E. Doyle, P. Dufour, Beth L. Klein, Christopher J. Manser, Carl Melis, Tinggui Wang, Alycia J. Weinberger
Figure caption: Logarithmic number ratios of different heavy elements with respect to hydrogen in the circumstellar gas around Gaia J0611−6931 (blue dots) and the polluted atmosphere of Gaia J0611−6931 (red plus signs). Relatively speaking, the upper limit to silicon is the most constraining in the circumstellar gas.
Paper: Modeling Circumstellar Gas Emission around a White Dwarf Using CLOUDY 
Authors: Siyi Xu, 偲艺 许, Sherry Yeh, Laura. K. Rogers, Amy Steele, Erik Dennihy, Alexandra E. Doyle, P. Dufour, Beth L. Klein, Christopher J. Manser, Carl Melis, Tinggui Wang, Alycia J. Weinberger
Figure caption: Gas temperature as a function of the radial extent of the gas from CLOUDY calculations (blue dots). The dust temperature using the model from Jura (2003; brown dots) and assuming a blackbody (red dots) is also shown for comparison. It is difficult for the dust and gas to coexist, given the large temperature difference.
Paper: Modeling Circumstellar Gas Emission around a White Dwarf Using CLOUDY 
Authors: Siyi Xu, 偲艺 许, Sherry Yeh, Laura. K. Rogers, Amy Steele, Erik Dennihy, Alexandra E. Doyle, P. Dufour, Beth L. Klein, Christopher J. Manser, Carl Melis, Tinggui Wang, Alycia J. Weinberger
Figure caption: The blackbody line ratios as a function of gas temperature. The shaded area represents the 3σ range of the observed line flux. With the possible exception of Si, all the other line ratios can be explained as the blackbody ratios.
Paper: Modeling Circumstellar Gas Emission around a White Dwarf Using CLOUDY 
Authors: Siyi Xu, 偲艺 许, Sherry Yeh, Laura. K. Rogers, Amy Steele, Erik Dennihy, Alexandra E. Doyle, P. Dufour, Beth L. Klein, Christopher J. Manser, Carl Melis, Tinggui Wang, Alycia J. Weinberger
Figure caption: A comparison between the observed line profile (black line with gray shaded region indicating 1σ uncertainties) and our model prediction (orange line) for Si I 12274 Å. The blue line represents the continuum flux.
Paper: A MIRI Search for Planets and Dust around WD 2149+021
Authors: Sabrina Poulsen, John Debes, Misty Cracraft, Susan E. Mullally, William T. Reach, Mukremin Kilic, Fergal Mullally, Loic Albert, Katherine Thibault, J. J. Hermes, Thomas Barclay, Elisa V. Quintana
Figure caption: JWST/MIRI mass sensitivity for WD 2149+021. The solid red line denotes our mass sensitivity for WD 2149+021 from unresolved infrared excesses and directly imaged companions assuming the median age (3 Gyr). The resolved limit is based on the contrast curve (Figure 6), which has been converted into a planet sensitivity in F1500W. The dashed line represents infrared excess mass sensitivity assuming that close-in planets are irradiated by the white dwarf. The orange lines are the infrared excess limits from previous Spitzer and HST direct-imaging observations of other white dwarfs. Symbols in blue represent planets with initial semimajor axes >3 au, the approximate orbital radius where planets are expected to survive post-main-sequence evolution (Mustill & Villaver 2012). Planet semimajor axes are expanded to account for adiabatic mass loss without tidal effects. Our observations would be sensitive to 55% of these known planet companions, if they were present in orbit around WD 2149+021. We also overplot the two known white dwarf exoplanet candidates with semimajor axes <10 au. Exoplanet data provided by the NASA Exoplanet Science Institute (2020).
Paper: A MIRI Search for Planets and Dust around WD 2149+021
Authors: Sabrina Poulsen, John Debes, Misty Cracraft, Susan E. Mullally, William T. Reach, Mukremin Kilic, Fergal Mullally, Loic Albert, Katherine Thibault, J. J. Hermes, Thomas Barclay, Elisa V. Quintana
Figure caption: This contrast curve reports the flux ratio of our central aperture relative to the standard deviation of the background at varying radial distances for two of our filters, F550W (top) and F1500W (bottom). The blue dashed lines are located at the median contrast level for each filter, and are reported as the associated limiting mass by interpolating the 3 Gyr Bex model. On the F1500W contrast curve, an additional line in green has been added to show the contrast level expected for a 1 M Jup companion, also based on the 3 Gyr Bex model. Finally, the red dashed line shows the contrast level for our own Jupiter (4.6 Gyr) based on synthetic spectra generated using the Planetary Spectrum Generator (Villanueva et al. 2018), which has been scaled to the distance of WD 2149+021.
Paper: A MIRI Search for Planets and Dust around WD 2149+021
Authors: Sabrina Poulsen, John Debes, Misty Cracraft, Susan E. Mullally, William T. Reach, Mukremin Kilic, Fergal Mullally, Loic Albert, Katherine Thibault, J. J. Hermes, Thomas Barclay, Elisa V. Quintana
Figure caption: Top: the measured SED of WD 2149+021 inluding archival photometry (black squares) and JWST MIRI photometry (blue squares), compared to a DA cooling model with T eff = 17,480 K and ﹩\mathrm{log}g﹩ = 8.01 (red squares). Overplotted is the CALSPEC spectrum for WD 2149+021 (black line). Bottom: the residuals in units of sigma. The observed JWST MIRI photometry matches the expected photospheric flux to within 3 times the absolute flux calibration uncertainties (dashed lines) of ∼3%
Paper: A MIRI Search for Planets and Dust around WD 2149+021
Authors: Sabrina Poulsen, John Debes, Misty Cracraft, Susan E. Mullally, William T. Reach, Mukremin Kilic, Fergal Mullally, Loic Albert, Katherine Thibault, J. J. Hermes, Thomas Barclay, Elisa V. Quintana
Figure caption: Probabilty distributions for the age, initial mass, and final mass of WD 2149+021 derived using wdwarfdate (Kiman et al. 2022). The values T eff = 17,753 ± 72 K and log g = 8.01 ± 0.01 were used for input values. The DA cooling models (Bédard et al. 2020), MIST-based initial-final mass relation (IFMR; Cummings et al. 2018), and [Fe/H] = 0.0, v/vcrit = 0.0 (Choi et al. 2016; Dotter 2016) were chosen for the model WD, model IFMR, and isochrone of the progenitor star, respectively.
Paper: A MIRI Search for Planets and Dust around WD 2149+021
Authors: Sabrina Poulsen, John Debes, Misty Cracraft, Susan E. Mullally, William T. Reach, Mukremin Kilic, Fergal Mullally, Loic Albert, Katherine Thibault, J. J. Hermes, Thomas Barclay, Elisa V. Quintana
Figure caption: The expected flux for WD 2149+021 with 3 Gyr old companions of varying mass, normalized to the expected flux of WD 2149+021 with no companions, for each of the four MIRI filters used. From left to right, these filters are F560W (purple), F770W (blue), F1500W (green), and F2100W (yellow). With current absolute flux calibration reported to be 3% or better in all filters, the dotted and dashed horizontal lines denote a 3σ and 5σ confidence, respectively. Companions above 2 M Jup were modeled using cloudless Sonora Bobcat grid models (Marley et al. 2021), and companions below 2 M Jup were modeled using cloudless Bex models (Linder et al. 2019).
Paper: A MIRI Search for Planets and Dust around WD 2149+021
Authors: Sabrina Poulsen, John Debes, Misty Cracraft, Susan E. Mullally, William T. Reach, Mukremin Kilic, Fergal Mullally, Loic Albert, Katherine Thibault, J. J. Hermes, Thomas Barclay, Elisa V. Quintana
Figure caption: F1500W flux vs. F2100W/F560W flux ratio for all point sources detected in the WD 2149+021 field. Overplotted is a 0.1 and 10 Gyr isochrone constructed from a combination of Sonora Bobcat and Bex models, bracketing planets formed during post-main-sequence evolution to the upper limit to the total age uncertainty (6.5 Gyr; Figure 3) of WD 2149+021.