adsabs/AstroCLIMB huggingface dataset:
Paper: Orbits of the Irregular Satellites of Uranus and Neptune
Authors: Marina Brozović, Robert A. Jacobson
Figure caption: Osculating eccentricities, inclinations, and arguments of pericenter for the objects in the Kozai–Lidov resonance. For better visibility of the periodic changes, we plot 5 kyr as opposed to 30 kyr. The reference planes for inclinations were orbital planes of Uranus and Neptune around the Sun, α = 271.°93 and δ = 66.°37 and α = 273.°48 and δ = 67.°70. These are mean orbital poles at 2000 January 1, 12:00:00 TDB, which we obtained by fitting a precessing ellipse to de441 planetary ephemeris.
Paper: Orbits of the Irregular Satellites of Uranus and Neptune
Authors: Marina Brozović, Robert A. Jacobson
Figure caption: Comparison between a precessing ellipse model and an integrated orbit for Francisco (black line) and Caliban (gray line) for 6000 yr. The differences are projected into along-the-track (in-orbit), radial, and transverse (out-of-plane) directions. Note that time zero does not refer to the epoch for the mean elements. The horizontal axis represents the calendar time.
Paper: Orbits of the Irregular Satellites of Uranus and Neptune
Authors: Marina Brozović, Robert A. Jacobson
Figure caption: Orbital phase space for the irregular satellites of Neptune. The rest of the figure caption is the same as for Figure 10. The Hill radius for Neptune is 0.7771 au.
Paper: Orbits of the Irregular Satellites of Uranus and Neptune
Authors: Marina Brozović, Robert A. Jacobson
Figure caption: Comparison between a precessing ellipse model and an integrated orbit for Nereid (black line) and Halimede (gray line). The rest of the caption is the same as for Figure 6.
Paper: Orbits of the Irregular Satellites of Uranus and Neptune
Authors: Marina Brozović, Robert A. Jacobson
Figure caption: Orbital phase space for the irregular satellites of Uranus. Black dots show osculating semimajor axis multiplied by sines and cosines of the osculating inclination, while the colored outlines show the pericenter-to-apocenter variation, 2ae, for the duration of 30 kyr. The reference plane for inclinations is the ecliptic. The Hill radius for Uranus is 0.4864 au.
Paper: Orbits of the Irregular Satellites of Uranus and Neptune
Authors: Marina Brozović, Robert A. Jacobson
Figure caption: Representation of the Kozai–Lidov dynamics in the Uranian (Margaret) and Neptunian (Sao and Neso) systems. The top panels show osculating (e cos(ω), e sin(ω)), while the bottom panels show the osculating argument of pericenter for 30 kyr.
Paper: Orbits of the Irregular Satellites of Uranus and Neptune
Authors: Marina Brozović, Robert A. Jacobson
Figure caption: Plane-of-sky position uncertainties for the irregular satellites of Neptune from 2020 to 2050 for an observer on Earth.
Paper: Orbits of the Irregular Satellites of Uranus and Neptune
Authors: Marina Brozović, Robert A. Jacobson
Figure caption: Plane-of-sky position uncertainties for the irregular satellites of Uranus from 2020 to 2050 for an observer on Earth.
Paper: Activity and Rotation of Nearby Field M Dwarfs in the TESS Southern Continuous Viewing Zone
Authors: Francys Anthony, Alejandro Núñez, Marcel A. Agüeros, Jason L. Curtis, J.-D. do Nascimento Jr., João M. Machado, Andrew W. Mann, Elisabeth R. Newton, Rayna Rampalli, Pa Chia Thao, Mackenna L. Wood
Figure caption: Top: Hα EW as a function of Gaia (G − G RP) color and spectral type for stars in our sample. Blue circles indicate stars with Gaia’s RUWE ≤ 1.2, and orange triangles stars with RUWE > 1.2; the latter are potential unresolved binary or higher-order systems. Bottom: a comparison of the active fraction of M dwarfs in our sample (black squares and line) to that for the sample of M dwarfs with SDSS spectra of West et al. (2011, gray pentagons and line). We define active/inactive stars following the Hα EW–(G − G RP) boundary relation in Kiman et al. (2021).
Paper: Activity and Rotation of Nearby Field M Dwarfs in the TESS Southern Continuous Viewing Zone
Authors: Francys Anthony, Alejandro Núñez, Marcel A. Agüeros, Jason L. Curtis, J.-D. do Nascimento Jr., João M. Machado, Andrew W. Mann, Elisabeth R. Newton, Rayna Rampalli, Pa Chia Thao, Mackenna L. Wood
Figure caption: TESS light curves for M dwarfs in our sample observed during the first year of its mission. Dashed vertical lines indicate the start and end of each observing sector. The number of each sector is labeled at the bottom. Each light curve is labeled with the star’s 2MASS designation and the P rot obtained from our GLS analysis. Panel (a) shows examples of stars with P rot <15 days, which we considered our upper limit for confident P rot measurements based exclusively on TESS data. Panel (b) shows examples of light curves where we measured P rot > 15 days, and thus considered unreliable. The first two stars in panel (b) have P rot measurements in Howard et al. (2020) that disagree with those measured here by more than 20%. As for the third star, while its light curve shows plausible modulations on a timescale of ≈40 days, we lack any ancillary data to confirm the TESS-derived P rot.
Paper: Activity and Rotation of Nearby Field M Dwarfs in the TESS Southern Continuous Viewing Zone
Authors: Francys Anthony, Alejandro Núñez, Marcel A. Agüeros, Jason L. Curtis, J.-D. do Nascimento Jr., João M. Machado, Andrew W. Mann, Elisabeth R. Newton, Rayna Rampalli, Pa Chia Thao, Mackenna L. Wood
Figure caption:  L Hα /L bol as a function of R o for our southern CVZ sample and for the M dwarfs of Newton et al. (2017, gray circles). Blue circles indicate stars in our sample with RUWE ≤ 1.2, and orange triangles with RUWE > 1.2. The arrows indicate upper limits for stars in our sample with Hα indistinguishable from zero; for these stars we assumed an EW upper limit of −0.5 Å to measure their L Hα /L bol upper limit. The black line is the best fit from Newton et al. (2017).
Paper: Activity and Rotation of Nearby Field M Dwarfs in the TESS Southern Continuous Viewing Zone
Authors: Francys Anthony, Alejandro Núñez, Marcel A. Agüeros, Jason L. Curtis, J.-D. do Nascimento Jr., João M. Machado, Andrew W. Mann, Elisabeth R. Newton, Rayna Rampalli, Pa Chia Thao, Mackenna L. Wood
Figure caption: Gaia CMDs showing the distribution of stars with EW and P rot measurements in our sample. Left: the circles are color-coded according to the EW value using the color bar at the bottom left. Gray circles are stars to which we assigned EW = 0 (see Section 3.2). Stars without spectroscopy are indicated with × symbols. The open squares indicate stars with reliable P rot (see Section 3.1). Right: the circles are color-coded according to the P rot value using the color bar at the bottom left. Gray circles are stars in our sample with no P rot measurement or unreliable determination.
Paper: Activity and Rotation of Nearby Field M Dwarfs in the TESS Southern Continuous Viewing Zone
Authors: Francys Anthony, Alejandro Núñez, Marcel A. Agüeros, Jason L. Curtis, J.-D. do Nascimento Jr., João M. Machado, Andrew W. Mann, Elisabeth R. Newton, Rayna Rampalli, Pa Chia Thao, Mackenna L. Wood
Figure caption:  P rot vs. Gaia (G − G RP) color for stars in our sample, represented with square symbols. Black circles indicate stars with RUWE > 1.2. The distribution for Praesepe single stars (≈700 Myr old; from Rampalli et al. 2021) is plotted in gray in the background. The squares are color-coded according to the Hα EW value using the color bar at the bottom left. The horizontal dash line indicates our upper limit in P rot space when calculating P rot from TESS light curves (see Section 3.1).
Paper: Activity and Rotation of Nearby Field M Dwarfs in the TESS Southern Continuous Viewing Zone
Authors: Francys Anthony, Alejandro Núñez, Marcel A. Agüeros, Jason L. Curtis, J.-D. do Nascimento Jr., João M. Machado, Andrew W. Mann, Elisabeth R. Newton, Rayna Rampalli, Pa Chia Thao, Mackenna L. Wood
Figure caption: Gaia CMD showing our targets (blue circles: RUWE ≤ 1.2; orange triangles: RUWE > 1.2) with, for comparison, 32,000 cool dwarfs in the TESS southern CVZ from the Stassun et al. (2019) catalog (gray dots).
Paper: Activity and Rotation of Nearby Field M Dwarfs in the TESS Southern Continuous Viewing Zone
Authors: Francys Anthony, Alejandro Núñez, Marcel A. Agüeros, Jason L. Curtis, J.-D. do Nascimento Jr., João M. Machado, Andrew W. Mann, Elisabeth R. Newton, Rayna Rampalli, Pa Chia Thao, Mackenna L. Wood
Figure caption: Spectra of five of our M dwarfs ranging in mass from 0.13 to 0.56 M ⊙. Four of these spectra were obtained using Goodman on SOAR or GMOS on Gemini-South; the fifth is an archival spectrum obtained with HARPS on the 3.6 m ESO telescope, La Silla. Left: each spectrum is labeled with the star’s 2MASS designation and mass. The spectra are normalized to the flux at 6555 Å and smoothed to a resolution R ≈ 1000. Right: a close-up of the Hα line, the location of which is indicated with a vertical dotted line.
Paper: Activity and Rotation of Nearby Field M Dwarfs in the TESS Southern Continuous Viewing Zone
Authors: Francys Anthony, Alejandro Núñez, Marcel A. Agüeros, Jason L. Curtis, J.-D. do Nascimento Jr., João M. Machado, Andrew W. Mann, Elisabeth R. Newton, Rayna Rampalli, Pa Chia Thao, Mackenna L. Wood
Figure caption: Our field dwarf sample, binned by distance (top panel) and stellar mass (bottom). The fraction of stars with spectra is shown in blue, that with both spectra and P rot measurements in red, and that with neither in gray.
Paper: TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion
Authors: Jack Lubin, Judah Van Zandt, Rae Holcomb, Lauren M. Weiss, Erik A Petigura, Paul Robertson, Joseph M. Akana Murphy, Nicholas Scarsdale, Konstantin Batygin, Alex S. Polanski, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Arpita Roy, Corey Beard, Sarah Blunt, Ashley Chontos, Fei Dai, Paul A. Dalba, Kaz Gary, Steven Giacalone, Michelle L. Hill, Andrew Mayo, Teo Močnik, Molly R. Kosiarek, Malena Rice, Ryan A. Rubenzahl, David W. Latham, S. Seager, Joshua N. Winn, Kaz Gary
Figure caption: GLS periodograms of the combined time series of Keck/HIRES and APF data. The two data sets were first filtered by removing instrumental offsets and the trend and curvature according to the best-fit parameters from our preferred model. In each descending panel, we have removed one planet at a time. The bottom panel shows the window function of the time series.
Paper: TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion
Authors: Jack Lubin, Judah Van Zandt, Rae Holcomb, Lauren M. Weiss, Erik A Petigura, Paul Robertson, Joseph M. Akana Murphy, Nicholas Scarsdale, Konstantin Batygin, Alex S. Polanski, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Arpita Roy, Corey Beard, Sarah Blunt, Ashley Chontos, Fei Dai, Paul A. Dalba, Kaz Gary, Steven Giacalone, Michelle L. Hill, Andrew Mayo, Teo Močnik, Molly R. Kosiarek, Malena Rice, Ryan A. Rubenzahl, David W. Latham, S. Seager, Joshua N. Winn, Kaz Gary
Figure caption: (a) Our complete RV time series with our preferred model (blue); (b) residuals including trend and curvature. Data collected from Keck/HIRES are shown as black circles, while data from the APF are shown by green diamonds.
Paper: TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion
Authors: Jack Lubin, Judah Van Zandt, Rae Holcomb, Lauren M. Weiss, Erik A Petigura, Paul Robertson, Joseph M. Akana Murphy, Nicholas Scarsdale, Konstantin Batygin, Alex S. Polanski, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Arpita Roy, Corey Beard, Sarah Blunt, Ashley Chontos, Fei Dai, Paul A. Dalba, Kaz Gary, Steven Giacalone, Michelle L. Hill, Andrew Mayo, Teo Močnik, Molly R. Kosiarek, Malena Rice, Ryan A. Rubenzahl, David W. Latham, S. Seager, Joshua N. Winn, Kaz Gary
Figure caption: The phase-folded RV time series for each planet with periods less than our baseline. Red circles are bins of size 0.08 phase.
Paper: TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion
Authors: Jack Lubin, Judah Van Zandt, Rae Holcomb, Lauren M. Weiss, Erik A Petigura, Paul Robertson, Joseph M. Akana Murphy, Nicholas Scarsdale, Konstantin Batygin, Alex S. Polanski, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Arpita Roy, Corey Beard, Sarah Blunt, Ashley Chontos, Fei Dai, Paul A. Dalba, Kaz Gary, Steven Giacalone, Michelle L. Hill, Andrew Mayo, Teo Močnik, Molly R. Kosiarek, Malena Rice, Ryan A. Rubenzahl, David W. Latham, S. Seager, Joshua N. Winn, Kaz Gary
Figure caption: Phase-folded light curves for each of the transiting planets, with our best-fit model overlaid and residuals below.
Paper: TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion
Authors: Jack Lubin, Judah Van Zandt, Rae Holcomb, Lauren M. Weiss, Erik A Petigura, Paul Robertson, Joseph M. Akana Murphy, Nicholas Scarsdale, Konstantin Batygin, Alex S. Polanski, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Arpita Roy, Corey Beard, Sarah Blunt, Ashley Chontos, Fei Dai, Paul A. Dalba, Kaz Gary, Steven Giacalone, Michelle L. Hill, Andrew Mayo, Teo Močnik, Molly R. Kosiarek, Malena Rice, Ryan A. Rubenzahl, David W. Latham, S. Seager, Joshua N. Winn, Kaz Gary
Figure caption: TESS photometry from sectors 15–19, 21, 22, 24, and 25, highlighting the transits of the three sub-Neptunes, which are indicated by color-coded arrows. Our RV model’s predicted transit midpoint times for planet e are shown by vertical dashed red lines, along with 3σ error windows as light-red shaded regions. The predicted ∼8 hr transit duration (for a central transit) is shown by dark-red shading. An additional transit window occurred in Sector 23, when the star was not visible in any TESS cameras.
Paper: TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion
Authors: Jack Lubin, Judah Van Zandt, Rae Holcomb, Lauren M. Weiss, Erik A Petigura, Paul Robertson, Joseph M. Akana Murphy, Nicholas Scarsdale, Konstantin Batygin, Alex S. Polanski, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Arpita Roy, Corey Beard, Sarah Blunt, Ashley Chontos, Fei Dai, Paul A. Dalba, Kaz Gary, Steven Giacalone, Michelle L. Hill, Andrew Mayo, Teo Močnik, Molly R. Kosiarek, Malena Rice, Ryan A. Rubenzahl, David W. Latham, S. Seager, Joshua N. Winn, Kaz Gary
Figure caption: A mass–radius diagram highlighting the HD 191939 transiting planets. Larger marker sizes correspond to more precise mass measurements, excluding the HD 191939 planets. Planet d’s marker represents the 2σ upper limit, and its arrow points back to the median value. Gray points are from the NASA Exoplanet Archive as of 2021 July 1, with cuts to include only 2σ masses or better.
Paper: TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion
Authors: Jack Lubin, Judah Van Zandt, Rae Holcomb, Lauren M. Weiss, Erik A Petigura, Paul Robertson, Joseph M. Akana Murphy, Nicholas Scarsdale, Konstantin Batygin, Alex S. Polanski, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Arpita Roy, Corey Beard, Sarah Blunt, Ashley Chontos, Fei Dai, Paul A. Dalba, Kaz Gary, Steven Giacalone, Michelle L. Hill, Andrew Mayo, Teo Močnik, Molly R. Kosiarek, Malena Rice, Ryan A. Rubenzahl, David W. Latham, S. Seager, Joshua N. Winn, Kaz Gary
Figure caption: Constraints on the mass and semimajor axis of planet f. The green region shows values that are consistent with the measured RV trend and curvature. The blue region shows values that are consistent with the Hipparcos/Gaia astrometry. The red region shows the values consistent with both RV and astrometry. Dark and light regions indicate the 1σ and 2σ confidence intervals, respectively. Planet f is likely between 2 and 11  M  J , orbiting between 2.6 and 7.0  au.
Paper: TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion
Authors: Jack Lubin, Judah Van Zandt, Rae Holcomb, Lauren M. Weiss, Erik A Petigura, Paul Robertson, Joseph M. Akana Murphy, Nicholas Scarsdale, Konstantin Batygin, Alex S. Polanski, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Arpita Roy, Corey Beard, Sarah Blunt, Ashley Chontos, Fei Dai, Paul A. Dalba, Kaz Gary, Steven Giacalone, Michelle L. Hill, Andrew Mayo, Teo Močnik, Molly R. Kosiarek, Malena Rice, Ryan A. Rubenzahl, David W. Latham, S. Seager, Joshua N. Winn, Kaz Gary
Figure caption: Details on the Laplace–Lagrange analysis. Left: the inclination curves for each planet when planet e is given a starting value of I  e  = 0.°5 vs. I  e  = 6.°0. When the mutual inclination of the three is small enough for all three to transit together, the line is opaque. Right: the percent of time during which the inner three planets transit depends on the inclination of planet e. The vertical black dashed line indicates the nominal maximum inclination for which we would expect planet e to still transit. The horizontal red dashed line indicates the 10% threshold for our conservative estimate on the upper limit to the giant planet’s inclination.
Paper: TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion
Authors: Jack Lubin, Judah Van Zandt, Rae Holcomb, Lauren M. Weiss, Erik A Petigura, Paul Robertson, Joseph M. Akana Murphy, Nicholas Scarsdale, Konstantin Batygin, Alex S. Polanski, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Arpita Roy, Corey Beard, Sarah Blunt, Ashley Chontos, Fei Dai, Paul A. Dalba, Kaz Gary, Steven Giacalone, Michelle L. Hill, Andrew Mayo, Teo Močnik, Molly R. Kosiarek, Malena Rice, Ryan A. Rubenzahl, David W. Latham, S. Seager, Joshua N. Winn, Kaz Gary
Figure caption: TTVs of the transiting planets over the duration of the TESS photometry. We do not detect significant TTVs for any of the transiting planets over the observing baseline.
Paper: TESS-Keck Survey. IX. Masses of Three Sub-Neptunes Orbiting HD 191939 and the Discovery of a Warm Jovian plus a Distant Substellar Companion
Authors: Jack Lubin, Judah Van Zandt, Rae Holcomb, Lauren M. Weiss, Erik A Petigura, Paul Robertson, Joseph M. Akana Murphy, Nicholas Scarsdale, Konstantin Batygin, Alex S. Polanski, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Arpita Roy, Corey Beard, Sarah Blunt, Ashley Chontos, Fei Dai, Paul A. Dalba, Kaz Gary, Steven Giacalone, Michelle L. Hill, Andrew Mayo, Teo Močnik, Molly R. Kosiarek, Malena Rice, Ryan A. Rubenzahl, David W. Latham, S. Seager, Joshua N. Winn, Kaz Gary
Figure caption: All multiplanet systems with 5σ masses and radii for small planets (R  p  < 10 R ⊕, M  p  < 100 M ⊕) with TSMs > 20. Planets are plotted by mass and arranged vertically in order of host star effective temperature (hotter at the top). HD 191939 b and c have TSM values that are individually among the best in the sub-Neptune population and are unique in having the same host star. Due to planet d’s weak mass measurement, it appears in this plot unfilled. HD 191939 is the only system to date with multiple planets with TSMs greater than 100 that also does not saturate JWST.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: Imaged substellar companions with dynamical masses and bolometric luminosities. Cooling tracks of stars, brown dwarfs, and giant planets from Burrows et al. (1997) are shown in green, blue, and orange, respectively. HD 47127 B (Bowler et al. 2021a) and HD 4113 C (Cheetham et al. 2018) are not included in this plot due to their lack of published bolometric luminosities. The eclipsing brown dwarf binaries 2MASS J05352184-0546085 (Stassun et al. 2006) and 2MASS J15104786-2818174 Aab (Triaud et al. 2020), along with the transiting brown dwarf companion CWW 89Ab (Beatty et al. 2018), have measured dynamical masses but have not been spatially resolved. Unlike most brown dwarfs with dynamical masses, HD 984 B is young and offers an opportunity to assess substellar evolutionary models in an untested region of luminosity–age space near the substellar boundary.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: S/N of HD 984 B in PSF-subtracted NIRC2 images as a function of the number of PCA components. We find that a 16-component reduction produces the highest S/N of 40.7 for the 2019 epoch. An 11-component reduction produces the highest S/N of 34.9 for the 2020 epoch. We thus adopt these numbers of components for our PSF subtraction.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: PSF-subtracted images of HD 984 B taken with NIRC2 in 2019 July (left) and 2020 July (right). The color bar corresponds to the flux in each reduced image in units of ﹩\mathrm{DN}/{\rm{s}}﹩. The images are oriented so that north is up and east is to the left.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: Results of our negative PSF injection. The top panels are the PSF-subtracted images of HD 984 B from our 2019 July and 2020 July NIRC2 data sets. The bottom panels show the results after injecting negative PSF templates with the best-fit separations, position angles, and flux ratios. The elevated noise in the lower-right portion of the images is due to poorer PSF subtraction closer to the host star.
Paper: Dynamical Mass of the Young Substellar Companion HD 984 B
Authors: Kyle Franson, Brendan P. Bowler, Timothy D. Brandt, Trent J. Dupuy, Quang H. Tran, G. Mirek Brandt, Yiting Li, Adam L. Kraus
Figure caption: Posterior distributions of HD 984 B astrometry from our 2019 July (left) and 2020 July (right) NIRC2 data sets. The diagonal panels show the marginalized distributions for each parameter. The off-diagonal panels display 2D joint posterior distributions with 1σ, 2σ, 3σ, and 4σ contours. Astrometry is measured via a negative companion injection approach that uses MCMC to explore the parameter space. All corner plots in this study are produced using corner (Foreman-Mackey 2016).