adsabs/AstroCLIMB huggingface dataset:
Paper:  KPM: A Flexible and Data-driven K-process Model for Nucleosynthesis
Authors: Emily J. Griffith, David W. Hogg, Julianne J. Dalcanton, Sten Hasselquist, Bridget Ratcliffe, Melissa Ness, David H. Weinberg
Figure caption: Abundance distributions and KPM parameters for C+N, α, and light odd-Z elements. First column: observed abundance distributions in [X/Mg] vs. [Mg/H]. Second column: the predicted [X/Mg] vs. [Mg/H] abundance distribution of the fiducial model plus estimated noise. By comparing the first two columns, we can evaluate the success of KPM in reproducing the observed abundance distributions. Third column: process vector components ﹩{q}_{\mathrm{CC},j}^{Z}﹩ (thin, purple) and ﹩{q}_{\mathrm{Ia},j}^{Z}﹩ (thick, orange) from this work (G24; solid, dark lines) and W22 (light, dashed lines). Overall offsets between the solid and dashed lines are driven largely by our normalization, which places the [Mg/Fe] plateau at +0.4, rather than +0.3 in W22. Fourth column: distribution of fractional contribution from the prompt process (﹩{f}_{{ij}}^{\mathrm{CC}}﹩) predicted by the fiducial model. We plot the median ﹩{f}_{{ij}}^{\mathrm{CC}}﹩ values of the low-Ia (orange square) and high-Ia (purple circle) populations in the solar metallicity bin from W22 for comparison. All density plots are logarithmically scaled.
Paper:  KPM: A Flexible and Data-driven K-process Model for Nucleosynthesis
Authors: Emily J. Griffith, David W. Hogg, Julianne J. Dalcanton, Sten Hasselquist, Bridget Ratcliffe, Melissa Ness, David H. Weinberg
Figure caption: The same as Figure 2, but for Fe-peak elements and Ce.
Paper:  KPM: A Flexible and Data-driven K-process Model for Nucleosynthesis
Authors: Emily J. Griffith, David W. Hogg, Julianne J. Dalcanton, Sten Hasselquist, Bridget Ratcliffe, Melissa Ness, David H. Weinberg
Figure caption: Left: distribution of our stellar sample in Z (kpc) vs. R (kpc), where (0, 0) is the Galactic center. Center: distribution of stellar distances (kpc). Right: distribution of stellar eccentricity. Our stellar sample spans the Galactic disk, but the majority of our stars are within 3.5 kpc of the Sun and have kinematics consistent with in situ origin.
Paper: TOI-1994b: A Low-mass Eccentric Brown Dwarf Transiting A Subgiant Star
Authors: Emma Page, Joshua Pepper, Duncan Wright, Joseph E. Rodriguez, Robert A. Wittenmyer, Stephen R. Kane, Brett Addison, Timothy Bedding, Brendan P. Bowler, Thomas Barclay, Karen A. Collins, Phil Evans, Jonathan Horner, Eric L. N. Jensen, Marshall C. Johnson, John Kielkopf, Ismael Mireles, Peter Plavchan, Samuel N. Quinn, S. Seager, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Joshua N. Winn, George Zhou, Carl Ziegler
Figure caption: Surface gravity and effective temperature of 39 stars hosting transiting brown dwarf companions. The colors indicate the mass of the brown dwarf companions. TOI-1994b is marked with a red “x.” The horizontal dashed line indicates ﹩{log}(g)\,=\,4.1﹩ as the transition between main sequence and evolved subgiant stars as in Stassun et al. (2018).
Paper: The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System
Authors: Anmol Desai, Emma V. Turtelboom, Caleb K. Harada, Courtney D. Dressing, David R. Rice, Joseph M. Akana Murphy, Casey L. Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Michelle L. Hill, Tara Fetherolf, Steven Giacalone, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Alex S. Polanski, Malena Rice, Paul Robertson, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Allyson Bieryla, Lars A. Buchhave, Jon M. Jenkins, Veselin B. Kostov, Alan M. Levine, Jorge Lillo-Box, M. Paegert, Markus Rabus, S. Seager, Keivan G. Stassun, Eric B. Ting, David Watanabe, Joshua N. Winn
Figure caption: Top: RV measurements from APF/Levy (green squares) and Keck/HIRES (blue diamonds). For clarity, the RV offsets determined from the joint RV and transit fit (see Section 4.3) for each instrument have been subtracted from the data, and the respective jitter terms have been combined with the instrumental uncertainties to produce the error bars. Bottom: flattened and normalized TESS PDCSAP flux light curve.
Paper: The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System
Authors: Anmol Desai, Emma V. Turtelboom, Caleb K. Harada, Courtney D. Dressing, David R. Rice, Joseph M. Akana Murphy, Casey L. Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Michelle L. Hill, Tara Fetherolf, Steven Giacalone, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Alex S. Polanski, Malena Rice, Paul Robertson, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Allyson Bieryla, Lars A. Buchhave, Jon M. Jenkins, Veselin B. Kostov, Alan M. Levine, Jorge Lillo-Box, M. Paegert, Markus Rabus, S. Seager, Keivan G. Stassun, Eric B. Ting, David Watanabe, Joshua N. Winn
Figure caption: Lomb–Scargle periodogram of (a) all RV observations, (b) Keck/HIRES RVs, (c) APF/Levy RVs, (d) Keck/HIRES window function, (e) APF/Levy window function, and (f) S-values. The vertical green line marks the 37 day period, and the gray-shaded region marks the 300–500 day range. The long-period peak seen in the periodogram of the full RV data set is not present in the APF data, and is at a period similar to that of a significant peak in the HIRES window function. The dark red dashed line represents the 0.1% false alarm level. Data consisting of Gaussian noise with no periodic signal would produce peaks of this height (or above) in <0.1% of samples. The red dashed line is the 1% false alarm level.
Paper: The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System
Authors: Anmol Desai, Emma V. Turtelboom, Caleb K. Harada, Courtney D. Dressing, David R. Rice, Joseph M. Akana Murphy, Casey L. Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Michelle L. Hill, Tara Fetherolf, Steven Giacalone, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Alex S. Polanski, Malena Rice, Paul Robertson, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Allyson Bieryla, Lars A. Buchhave, Jon M. Jenkins, Veselin B. Kostov, Alan M. Levine, Jorge Lillo-Box, M. Paegert, Markus Rabus, S. Seager, Keivan G. Stassun, Eric B. Ting, David Watanabe, Joshua N. Winn
Figure caption: Lomb–Scargle periodogram of APF/Levy RV data (blue) and 100 simulations of APF/Levy observations of a two-planet TOI-1751 system. The period of TOI-1751 b is indicated by a vertical green line. The peaks in the periodogram of the simulated data are consistently higher than those of the real data at ∼400 days.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Left: The raw light curves extracted from TESS FFIs for three example stars in the DIAmante data that were later found to have DTARPS-S candidate transiting planets. Right: Plot of autocorrelation present in the light curve as a function of lag in units of the 30 minute FFI cadence. The p-value from the Ljung–Box test is 0 for all three light curves, indicating that the flux values of the light curves are autocorrelated.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: The DIAmante light curves for three example stars in Figure 3 after the removal of trends, ramping effects, and outliers (Section 2.5). The autocorrelation functions on the right show that autoregressive structure is still present in all three light curves.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: The residuals after the best-fit ARIMA model has been subtracted from the differenced light curves for three example stars in Figure 3. The three plots on the right show the amount of autocorrelation present in the light curve as a function of time step between points. The Ljung–Box test shows that two of three ARIMA residuals are consistent with Gaussian white noise.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: The AutoRegressive Planet Search process. Blue boxes represent steps in the ARPS analysis covered in this paper. Orange boxes represent steps in ARPS covered in Paper II.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: The transformation of the shape of the transit from the original light curve by the differencing step of the ARIMA processing into the double-spike shape (Caceres et al. 2019b).
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: The differenced light curves for three example stars in Figure 3 with autocorrelation functions.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). II. Hundreds of New TESS Candidate Exoplanets
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Examples of FP light curves. These are the light curves from the DIAmante survey prior to ARPS analysis, folded with the TCF peak period. Top left: The depth of the transit from the best TCF periodogram peak is too deep. Top right: The even and odd transits have different depths. Bottom left: The secondary transit is too deep. Bottom right: Photometric curvature is present in the phase-folded light curve.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). II. Hundreds of New TESS Candidate Exoplanets
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Comparison between the refined DTARPS period and the reported periods for different groups of objects: NASA/TOI confirmed planets (upper left); M20 candidates (upper right); candidates from other surveys (lower left); and our synthetic injected planets (Paper I). The bottom left panel contains both planet candidates (gold squares) and previously identified FPs (blue x’s). Open symbols represent objects rejected by vetting. The dashed lines indicate the 2:1, 1:1, and 1:2 ratios between the reported and DTARPS period.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). II. Hundreds of New TESS Candidate Exoplanets
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Plot of σ  P  and σ  T  for matches between the 7377 DTARPS-S analysis list objects and the full DIAmante data set of ∼1 million stars. The red shaded region represents the pairs of points removed as likely ephemeris matches. The limit for σ  P  is set to 2.807 or a 0.5% difference or less in the periods between two sources. The limit for σ  T  is set to 1.281 or a 20% difference or less in the epoch of first transits of two sources.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). II. Hundreds of New TESS Candidate Exoplanets
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Comparison between the refined DTARPS radius and the reported radii for different groups of objects with reported radii and the planetary injections from the positive training set of the RF classifier. The bottom left panel contains both planet candidates (in gold squares) and previously identified FPs (in blue x’s). The bottom right panel is from Paper I. The open points are plotted by the radius from their TCF periodogram peak. The dashed lines indicate the 2:1, 1:1, and 1:2 ratios between the reported radius and the DTARPS radius.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). II. Hundreds of New TESS Candidate Exoplanets
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Astrometric analysis of DTARPS-S candidates from Gaia DR2 observations. The red lines in each plot show the upper boundary for a Level 1 candidate. The red boundaries are from Evans (2018). (Left) Significance of the astrometric excess noise and astrometric goodness of fit in the along-scan direction for DTARPS-S candidates. (Right) Standard deviation of the radial velocity measurements. The red boundary is from Montalto et al. (2020).
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). II. Hundreds of New TESS Candidate Exoplanets
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Number of light curves rejected for each step in the vetting process as a function of the RF prediction value. Level 1 objects satisfied all vetting criteria, while Level 2 objects passed a vetting test only marginally. FP = False Positive, FA = False Alarm.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). II. Hundreds of New TESS Candidate Exoplanets
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Example of an FA light curve. The top panel shows the TCF periodogram with highest-S/N period marked. The bottom panel shows no evident transit in the folded light curve after autoregressive noise is removed. This case had a low TCF S/N and an RF prediction value only marginally above the threshold of 0.30.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: Bottom panels: the predicted R = 30,000 [Ne II] line profiles (colored lines) without (left) and with (right) a 15 au dust cavity compared to the data from Pascucci et al. (2020; gray). Each line represents a model with a different inner radius (with increasingly dark colors indicating larger values) for a mass-loss rate of 1–3 × 10−8 M ☉ yr−1 and the hiLX_TCha_sUV spectrum. Both the models and the data are normalized to an integrated value of unity. Top panels: the summary statistics (FWHM and centroid shift) of the modeled lines compared to those of the data (black cross). The colors are as in the bottom panel, with circles being for b = 1.5 and crosses for b = 1.0.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: Left: a comparison between the estimated intrinsic HWHMeff of the [Ne II] 12.81 μm emission (x-axis) and [Ar II] 6.98 μm emission (y-axis) for the fiducial set of synthetic images. The average of the values obtained from the observations with the two standard stars is indicated by the black marker with the error bars calculated as half their difference. Upper limits (no extension detected) are indicated by triangles. Right: a comparison between spherical radius containing 97% (dashed), 95% (dotted–dashed), and 50% (dotted) of the [Ar II] and [Ne II] flux shown for model sets with two different mass-loss rates. In each panel, point sizes indicate the inner radius of the model.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: As with Figure 1 but for r in = r  G . Note the change in scale of the panels to accommodate the larger scales on which the wind is ionized.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: As with Figure 1 but for a gas density 10 times lower.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: As with Figure 12 but for the [O I] line and shown at a resolution of R = 45,000 to match the data.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: As with Figure 12 but excluding emission from outside a 0.″4 slit oriented N-S.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: As with Figure 9 but for [Ar II] 6.98 μm emission. No extension is detected for either PSF: we indicate this by marking the endpoints of the line with triangles.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption:  The F444W brightness and [F356W]−[F444W] color of our detected sources are compared against 440 Myr isochrones as a function of planet mass. Three evolutionary-radiative models are considered –AMES-Cond (solid line), BEX-HELIOS (dotted), and BEX-petitCODE with clouds (dashed). Masses from 0.5 to 10  M Jup are marked on each isochrone. In the lower left-hand corner the source IDs are omitted for clarity, but from left to right are: S6, S3, S1, S9, and S4.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Top: Three-panel images showing data, model, and residuals for NIRCam S1 at F356W (left) and F444W (right). Bottom: The MCMC post-processing analysis gives the (x, y) position in pixels, the relative flux, and a correlation length, a Gaussian hyperparameter. This fit shows robust detections at both wavelengths. The same analysis is applied to all sources discussed in Table 3.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: SED of S1 fitted to the model SEDs for three archetypal active galaxies, Markarian 231 (gray), average Seyfert 2 (blue), or NGC6240 (red) at redshifts of z = (0.80, 0.21, and 0.56, respectively) using templates from the Spitzer SWIRE catalog (Polletta et al. 2007).
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Same as Figure 12, but for source 5.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Same as Figure 12, but for S2.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Same as Figure 12, but for source HST #1.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Same as Figure 12, but for source 3.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Same as Figure 12, but for source 4.