adsabs/AstroCLIMB huggingface dataset:
Paper: The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters
Authors: Andrea S. J. Lin, Jessica E. Libby-Roberts, Jaime A. Alvarado-Montes, Caleb I. Cañas, Shubham Kanodia, Te Han, Leslie Hebb, Eric L. N. Jensen, Suvrath Mahadevan, Luke C. Powers, Tera N. Swaby, John Wisniewski, Corey Beard, Chad F. Bender, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Robert C. Frazier, Connor Fredrick, Michael Gully-Santiago, Samuel Halverson, Sarah E. Logsdon, Michael W. McElwain, Caroline Morley, Joe P. Ninan, Jayadev Rajagopal, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Daniel J. Stevens, Ryan C. Terrien, Jason T. Wright
Figure caption: GLS periodograms of available photometry from ASAS-SN (V, g, and combined). We combine V and g in an attempt to more robustly detect long-period signals, since the two bands have little time overlap. FAP levels of 0.1%, 1%, and 10% are marked as in Figure 10, and the tentative rotation period of 29.46 days is shown with a vertical dotted line.
Paper: The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters
Authors: Andrea S. J. Lin, Jessica E. Libby-Roberts, Jaime A. Alvarado-Montes, Caleb I. Cañas, Shubham Kanodia, Te Han, Leslie Hebb, Eric L. N. Jensen, Suvrath Mahadevan, Luke C. Powers, Tera N. Swaby, John Wisniewski, Corey Beard, Chad F. Bender, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Robert C. Frazier, Connor Fredrick, Michael Gully-Santiago, Samuel Halverson, Sarah E. Logsdon, Michael W. McElwain, Caroline Morley, Joe P. Ninan, Jayadev Rajagopal, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Daniel J. Stevens, Ryan C. Terrien, Jason T. Wright
Figure caption: TESS-SIP periodograms computed from both the TPFs and LCFs, neither of which display the periodicity seen in the PDCSAP fluxes.
Paper: The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters
Authors: Andrea S. J. Lin, Jessica E. Libby-Roberts, Jaime A. Alvarado-Montes, Caleb I. Cañas, Shubham Kanodia, Te Han, Leslie Hebb, Eric L. N. Jensen, Suvrath Mahadevan, Luke C. Powers, Tera N. Swaby, John Wisniewski, Corey Beard, Chad F. Bender, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Robert C. Frazier, Connor Fredrick, Michael Gully-Santiago, Samuel Halverson, Sarah E. Logsdon, Michael W. McElwain, Caroline Morley, Joe P. Ninan, Jayadev Rajagopal, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Daniel J. Stevens, Ryan C. Terrien, Jason T. Wright
Figure caption: GLS periodograms of available photometry from ZTF (zg and zr). Here we do not combine the bands as we did with the ASAS-SN data, since the zg and zr observations span the same time frame.
Paper: The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters
Authors: Andrea S. J. Lin, Jessica E. Libby-Roberts, Jaime A. Alvarado-Montes, Caleb I. Cañas, Shubham Kanodia, Te Han, Leslie Hebb, Eric L. N. Jensen, Suvrath Mahadevan, Luke C. Powers, Tera N. Swaby, John Wisniewski, Corey Beard, Chad F. Bender, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Robert C. Frazier, Connor Fredrick, Michael Gully-Santiago, Samuel Halverson, Sarah E. Logsdon, Michael W. McElwain, Caroline Morley, Joe P. Ninan, Jayadev Rajagopal, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Daniel J. Stevens, Ryan C. Terrien, Jason T. Wright
Figure caption: Corner plot of HPF RVs and activity indicators, with the Kendall τ coefficient included for each pair.
Paper: exoMMR: A New Python Package to Confirm and Characterize Mean Motion Resonances
Authors: Mariah G. MacDonald, Michael S. Polania Vivas, Skylar D'Angiolillo, Ashley N. Fernandez, Tyler Quinn
Figure caption: Results of our simulations of Kepler-80g. Here, we draw the mass and eccentricity from independent uniform distributions of U[0.0,1.0] M ⊕ and U[0.0,0.1], respectively. Left: entire parameter space, marking simulations as “Not Possible” (red) if the simulation went unstable or if the known three-body resonances circulated and “Possible” (blue) if both criteria are met. Right: heat map of same results, where black shows 0% of simulations met both stability and resonant criteria, and white shows 100% of simulations met both criteria. We find that, for Kepler-80g to be M  p  > 0.5 M ⊕, the eccentricity must be small, e < 0.005.
Paper: exoMMR: A New Python Package to Confirm and Characterize Mean Motion Resonances
Authors: Mariah G. MacDonald, Michael S. Polania Vivas, Skylar D'Angiolillo, Ashley N. Fernandez, Tyler Quinn
Figure caption: Probability of an injected planet in Kepler-80 in linear space (left) and semi-log space (right). Here, we color the region based on the percentage of simulations that remained stable and have librating three-body resonant angles at the end of the 5 × 105 yr integration. We explore a range of masses from 0.5 M ⊕ to 5M  J  and initialize the injected planet at e = 0.0 and i = 90°. We find that any planet with P > 50 days, regardless of mass, is allowed. Planets closer to this must be part of the resonant chain if they are massive; otherwise, the resonances are broken and the system often becomes unstable. Interior to P < 20 days, the system usually goes unstable from an excited planet.
Paper: exoMMR: A New Python Package to Confirm and Characterize Mean Motion Resonances
Authors: Mariah G. MacDonald, Michael S. Polania Vivas, Skylar D'Angiolillo, Ashley N. Fernandez, Tyler Quinn
Figure caption: Distribution of percentages of simulations with librating angles. We note two modes, roughly separated by an absolute minimum at 53%. We use the cutoff of 90%, marked by the blue dashed line, to confirm a resonance.
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: Distributions of parallax (left) and PM (right) of member candidates. The left panel displays the parallaxes and their associated errors. We plot stars that are brighter than 18 mag in the G RP band and have parallaxes greater than three times the associated errors. In the left panel, dashed lines indicate the boundary used to search for genuine members between 1.0 and 3.5 kpc. The right panel exhibits the PM distributions of member candidates between 1.0 and 3.5 kpc. Only stars with parallaxes greater than their associated errors are considered for analysis. The ellipse in the right panel shows the region confined within five times the standard deviation from the weighted mean PMs, where the inverse of the squared PM error is used as the weight value. The selected members are shown by red dots.
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: Color–magnitude diagram of stars in the W5 region. Blue dots, black triangles, green squares, black open squares, red dots, and red open circles represent early-type stars, Class I, Class II, YSOs with a transitional disk, Hα emission stars, and Hα emission star candidates, respectively. The photometric data of these stars were taken from Gaia EDR3 (Gaia Collaboration et al. 2021).
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: Distribution of distances (left) and RVs (right). In order to compute a reliable distance to W5, we used members with parallaxes larger than 10 times the associated errors. Bin sizes of 0.2 kpc and 1.2 km s−1 were used to obtain the distance distribution and RV distribution, respectively. The red curves represents the best-fit Gaussian distributions.
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: Spatial distribution of members in W5. The size of dots is proportional to the brightness of individual stars. The positions of stars are relative to the reference coordinate R.A. = 02h 54m 45.ˢ80, decl. = ﹩+60^\circ \ 22^{\prime} \ 04\buildrel{\prime\prime}\over{.} 3﹩ (J2000).
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: Relation between the number of groups and inertia values. The number of groups was obtained from the elbow value of the inertia curve. The elbow value of 8 was determined from the point of intersection of the two red straight lines. See the main text for detail.
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: CMD of the selected members. The symbols are the same as in Figure 1.
Paper: Terrestrial- and Neptune-mass Free-Floating Planet Candidates from the MOA-II 9 yr Galactic Bulge Survey
Authors: Naoki Koshimoto, Takahiro Sumi, David P. Bennett, Valerio Bozza, Przemek Mróz, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Marginalized posterior distributions of (t E, θ E) calculated using the MCMC method for the 12 short-timescale events with the best-fit t E values smaller than 1 day. The prior was corrected so that it becomes uniform in (﹩\mathrm{log}{t}_{{\rm{E}}}﹩, ﹩\mathrm{log}{\theta }_{{\rm{E}}}﹩), although the MCMC was performed with the uniform prior in (1/t E, t *). The two gray dashed lines indicate relative proper-motion values of μ rel = 0.8 mas yr−1 and μ rel = 20 mas yr−1, between which most events reside considering the structure of our Galaxy.
Paper: Terrestrial- and Neptune-mass Free-Floating Planet Candidates from the MOA-II 9 yr Galactic Bulge Survey
Authors: Naoki Koshimoto, Takahiro Sumi, David P. Bennett, Valerio Bozza, Przemek Mróz, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curves of the four short events with OGLE data (blue) during magnification (MOA-9y-570, MOA-9y-671, MOA-9y-2202 (OGLE-2014-BLG-0617), MOA-9y-3945). The red lines indicate the best-fit model by using both MOA and OGLE data.
Paper: Terrestrial- and Neptune-mass Free-Floating Planet Candidates from the MOA-II 9 yr Galactic Bulge Survey
Authors: Naoki Koshimoto, Takahiro Sumi, David P. Bennett, Valerio Bozza, Przemek Mróz, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curves of the short-timescale microlensing candidates with t E < 1 day.
Paper: Confirming Resonance in Three Transiting Systems
Authors: Tyler Quinn, Mariah G. MacDonald
Figure caption: Example evolution of the orbital periods, eccentricities, inclinations, all four two-body resonant angles, and the three-body resonant angle of the three planets of Kepler-254. We find that the two-body angle Θ c,d  librates in nearly all of our simulations, the two-body angle Θ b,c  only librates in approximately 40%, and the corresponding three-body angle circulates in each one. The initial values for this simulation were drawn from independent, normal distributions, as described in Section 2 and summarized in Table 1. We integrate this simulation beyond 10 Myr for visualization purposes.
Paper: Autoencoding Galaxy Spectra. II. Redshift Invariance and Outlier Detection
Authors: Yan Liang, Peter Melchior, Sicong Lu, Andy Goulding, Charlotte Ward
Figure caption: The autoencoder SPENDER generates a rest frame and observed spectrum reconstruction. It is trained with a conventional fidelity loss, which compares separately input spectra ( x  1,  x  2) to their redshifted and resampled reconstructions ( x  1″,  x  2″). In this work, we added a novel similarity loss, which links the distance in latent space ∣ s  1 −  s  2∣ between two spectra to their distance in rest frame ﹩| {{\boldsymbol{x}}}_{1}^{\prime} -{{\boldsymbol{x}}}_{2}^{{\prime} }| ﹩. Spectra of two physically similar galaxies observed at different redshifts (z 1, z 2), for which the underlying rest-frame models are very similar, will thus yield similar latent vectors. To further improve the encoding stability, we minimize an additional consistency loss defined as the latent distances between the input spectra and its artificially redshifted augment ∣ s  i −  s  i,aug∣. After training the autoencoder, we train a normalizing flow to map the complicated latent distribution of the entire SDSS galaxy sample to a Gaussian base distribution through a series of invertible transformations, which allows efficient computation of the probability of any given sample.
Paper: Autoencoding Galaxy Spectra. II. Redshift Invariance and Outlier Detection
Authors: Yan Liang, Peter Melchior, Sicong Lu, Andy Goulding, Charlotte Ward
Figure caption: Euclidean distance distribution in latent space for randomly selected galaxy pairs (Δ s  rand, blue) and original-augment pairs (Δ s  aug). Augmented spectra stem from the original spectra by artificially altering the redshifts. If the encoder is redshift invariant, Δ s  aug = 0. The three panels refer to the result of training with different terms in the loss function Equation (2). Optimizing the full loss function (bottom) significantly reduces Δ s  aug, while increasing Δ s  rand, i.e., increasing the separation of different spectral types in latent space.
Paper: Autoencoding Galaxy Spectra. II. Redshift Invariance and Outlier Detection
Authors: Yan Liang, Peter Melchior, Sicong Lu, Andy Goulding, Charlotte Ward
Figure caption: UMAP embedding of the latent variables for all 531,890 SDSS galaxy spectra, color-coded by redshifts (top left), stellar masses (top right), specific star-formation rates (lower left), and dust attenuation in rest-frame V band (lower right). The lower right histograms show the distribution of physical properties of ∼2000 samples located inside a small box (marked black/white) in the UMAP space.
Paper: Autoencoding Galaxy Spectra. II. Redshift Invariance and Outlier Detection
Authors: Yan Liang, Peter Melchior, Sicong Lu, Andy Goulding, Charlotte Ward
Figure caption: Left: observed spectrum (black) of a galaxy from the test sample at z = 0.02, its reconstruction (red), and reconstructions of augmented spectra with artificially altered redshifts (color-coded). Zoomed-in versions are shown on the top. The colored bar in the middle-left shows the observed wavelength range of the augments. Right: UMAP-embedded latent space distribution of the entire SDSS galaxy sample. The white circle marks the example spectrum, and the triangles mark its augments.
Paper: Systematically Measuring Ultradiffuse Galaxies (SMUDGes). IV. Ultradiffuse Satellites of Milky Way Analogs
Authors: Hina Goto, Dennis Zaritsky, Ananthan Karunakaran, Richard Donnerstein, David J. Sand
Figure caption: Comparison of pair separation distributions derived from the three redshift slices in the upper panel: 4500 < cz/km s−1 < 5500 (blue circles); 5500 < cz/km s−1 < 6500 (gray squares); 6500 < cz/km s−1 < 7500 (red triangles). We have decreased the bin size to 20 kpc and overplot the newly fitted model curves for each of the three redshift slices. In the lower panel we show the average of the three slices with the uncertainties reflecting the error in the mean using standard deviation of those values rather than the Poisson uncertainties shown in the upper panel.
Paper: Systematically Measuring Ultradiffuse Galaxies (SMUDGes). IV. Ultradiffuse Satellites of Milky Way Analogs
Authors: Hina Goto, Dennis Zaritsky, Ananthan Karunakaran, Richard Donnerstein, David J. Sand
Figure caption: UDG-MWA pair surface density for the 4500 < cz/(km s−1) < 5500 slice per UDG. The pairs are defined by their projected separation. The upper panel shows the distribution in linear units, while the lower one in logarithmic units. The power law + background model fit is performed in linear space but shown in both panels. Error bars are plotted, but are mostly within the symbols themselves. We discuss the apparent underestimation of the uncertainties in the text.
Paper: Systematically Measuring Ultradiffuse Galaxies (SMUDGes). IV. Ultradiffuse Satellites of Milky Way Analogs
Authors: Hina Goto, Dennis Zaritsky, Ananthan Karunakaran, Richard Donnerstein, David J. Sand
Figure caption:  S UDG, derived from the nearest redshift slice, vs. host halo mass. We adopt the MW mass estimate of Shen et al. (2022) to represent our MWAs. The plot, the fitted relationship, and other measurements are adopted directly from Karunakaran & Zaritsky (2023), and the original measurements referenced in the legend (Román & Trujillo 2017b; Mancera Piña et al. 2019; van der Burg et al. 2016, 2017; Janssens et al. 2019; Yagi et al. 2016; Forbes et al. 2020; La Marca et al. 2022a; Venhola et al. 2022).
Paper: Systematically Measuring Ultradiffuse Galaxies (SMUDGes). IV. Ultradiffuse Satellites of Milky Way Analogs
Authors: Hina Goto, Dennis Zaritsky, Ananthan Karunakaran, Richard Donnerstein, David J. Sand
Figure caption: Distribution of inferred absolute magnitudes of UDG satellites when working within the 4500 < cz/(km s−1) < 5500 slice. Although many of the galaxies are likely to be false pairs, this plot shows the type of UDG satellites to which we are sensitive.
Paper: Systematically Measuring Ultradiffuse Galaxies (SMUDGes). IV. Ultradiffuse Satellites of Milky Way Analogs
Authors: Hina Goto, Dennis Zaritsky, Ananthan Karunakaran, Richard Donnerstein, David J. Sand
Figure caption: Pair surface density as a function of UDG color for the lowest redshift sample. UDG-MWA pairs that include a UDG classified as red are shown in the red circles, while those classified as blue are shown as blue squares. Dashed lines are power law plus flat background fits to the data.
Paper: EXPRES. IV. Two Additional Planets Orbiting ρ Coronae Borealis Reveal Uncommon System Architecture
Authors: John M. Brewer, Lily L. Zhao, Debra A. Fischer, Rachael M. Roettenbacher, Gregory W. Henry, Joe Llama, Andrew E. Szymkowiak, Samuel H. C. Cabot, Sam A. Weiss, Chris McCarthy
Figure caption: The FWHM of the CCF is a measure of line shape changes typically associated with stellar activity. A Lomb–Scargle periodogram of the CCF FWHM (blue) shows several significant periods that do not coincide with the window function (gray), including one at 28.9 days with a possible order three harmonic at 84.9 days (VanderPlas 2018). None of the other activity indicators we measured had any significant periodicity. The 28.9 day period could indicate the rotation period of the star; it is also close to window function periods produced by avoiding observations close to the Moon. Vertical lines indicate periods with FAPs <0.1% and are labeled in the legend. Horizontal lines indicate FAPs of 3%, 1%, and 0.1%.
Paper: EXPRES. IV. Two Additional Planets Orbiting ρ Coronae Borealis Reveal Uncommon System Architecture
Authors: John M. Brewer, Lily L. Zhao, Debra A. Fischer, Rachael M. Roettenbacher, Gregory W. Henry, Joe Llama, Andrew E. Szymkowiak, Samuel H. C. Cabot, Sam A. Weiss, Chris McCarthy
Figure caption: Best four-planet fit to all EXPRES data with S/N ≥ 200 with residuals (panel a). The rms scatter to the residuals of the model to these 153 measurements is 1.20 m s−1. Phased plots for planets (b)–(e) are shown in the panels with those labels. Orange points in all panels are individual observations with error bars inflated by the stellar jitter term in the model. Larger red points are phase binned. We still lack complete phase coverage for planet d, as the period is slightly longer than an observing season. There are only three nights of data from 2020.
Paper: EXPRES. IV. Two Additional Planets Orbiting ρ Coronae Borealis Reveal Uncommon System Architecture
Authors: John M. Brewer, Lily L. Zhao, Debra A. Fischer, Rachael M. Roettenbacher, Gregory W. Henry, Joe Llama, Andrew E. Szymkowiak, Samuel H. C. Cabot, Sam A. Weiss, Chris McCarthy
Figure caption: Dynamical evolution of the four planets around ρ CrB. Each of the four columns corresponds to a planet. The results of three different dynamical simulations with system inclinations of 90° (i.e., edge-on), 50°, and 20° assuming all planets are coplanar are shown in blue, orange, and green, respectively. The percent change in the semimajor axis of each planet at each time step is shown in the top row; the eccentricity of each planet is shown in the bottom row.
Paper: EXPRES. IV. Two Additional Planets Orbiting ρ Coronae Borealis Reveal Uncommon System Architecture
Authors: John M. Brewer, Lily L. Zhao, Debra A. Fischer, Rachael M. Roettenbacher, Gregory W. Henry, Joe Llama, Andrew E. Szymkowiak, Samuel H. C. Cabot, Sam A. Weiss, Chris McCarthy
Figure caption: Posterior distributions of stellar parameters (mass, radius, and ﹩{\mathrm{log}}_{10}{\rm{age}}﹩) fit using isochrones Python package show smooth distributions and are in good agreement with all of our observables. The star is a 10.2 Gyr subgiant, but it is a 0.95 M ⊙ main-sequence star with a slightly subsolar metallicity.
Paper: EXPRES. IV. Two Additional Planets Orbiting ρ Coronae Borealis Reveal Uncommon System Architecture
Authors: John M. Brewer, Lily L. Zhao, Debra A. Fischer, Rachael M. Roettenbacher, Gregory W. Henry, Joe Llama, Andrew E. Szymkowiak, Samuel H. C. Cabot, Sam A. Weiss, Chris McCarthy
Figure caption: Distribution of uncertainties for the 153 observations obtained between May 2020 and May 2023. The mean uncertainty is 0.37 m s−1. The earliest observations were taken at slightly lower S/N, and cloudy nights or those with bad seeing and correspondingly longer exposure times have slightly increased uncertainties.
Paper: EXPRES. IV. Two Additional Planets Orbiting ρ Coronae Borealis Reveal Uncommon System Architecture
Authors: John M. Brewer, Lily L. Zhao, Debra A. Fischer, Rachael M. Roettenbacher, Gregory W. Henry, Joe Llama, Andrew E. Szymkowiak, Samuel H. C. Cabot, Sam A. Weiss, Chris McCarthy
Figure caption: Periodogram to the residuals to a three-planet fit, with planets at 39.8, 102.2, and 283.8 days. The highest peak (12.9 days) has an FAP = 1.0 × 10−6, indicating a possible fourth planet. The four highest peaks are labeled in the plot along with the 3%, 1%, and 0.1% FAP levels. No significant power was found at longer periods, which are not shown. A periodogram of the residuals to a four-planet fit showed no significant peaks.