adsabs/AstroCLIMB huggingface dataset:
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: Top left: histogram of galaxies within 60′ of the cluster center for all galaxies (black dashed line), galaxies with redshifts before this study (solid black line), and galaxies with redshifts from this study (solid red line). Bottom left: differential spectroscopic completeness as a function of magnitude for data before this study (solid black line) and from this study (solid red line). Black and red dotted vertical lines show the magnitudes corresponding to the differential completeness of 50%. The magnitudes are 16.1 and 18.0 mag, respectively. Top right and bottom right: Same as the left panels, but for galaxies within 30′. The magnitudes at which the completeness is 50% are 16.1 mag for data before this study and 19.1 mag for data from this study.
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: Rotation velocity of the Perseus cluster. (Top left) Individual circles indicate the radial velocities of member galaxies within 27′ as a function of position angle θ. The black line represents the fitted curve according to Equation (3). (Top right) Difference between the mean velocities 〈v 1〉, 〈v 2〉 of member galaxies within 27′ in two regions divided by a line with position angle θ. (Bottom left and right) Same as the top panels, for galaxies in ﹩27^{\prime} \lt R\lt 60^{\prime} ﹩.
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: Radial velocity dispersion profile of galaxies. In both panels, the black circles represent the velocity dispersion of all member galaxies. (Top) Galaxies are divided into red member galaxies (red open circles) and blue member galaxies (blue crosses). (Bottom) Galaxies are divided by their absolute magnitude. Magenta squares represent bright member galaxies and cyan triangles represent faint member galaxies. Only bins with three or more galaxies are used. Error bars of galaxy velocity dispersion are resampling errors.
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: (a) Bottom left: Spectroscopic completeness of galaxies with r Petro,0 ≤ 18.0 as a function of R.A. and decl.. The field size is ﹩120^{\prime} \times 120^{\prime} ﹩ with its center aligned to the center of the Perseus cluster. Marginal completeness in the R.A. (top) and decl. (right) are also given. (b) Same as (a), but for the galaxies brighter than 19.1 mag in the ﹩60^{\prime} \times 60^{\prime} ﹩ field.
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: (Top) Distribution of r Petro,0 along redshift. Black dots represent individual galaxy redshifts before this study, while red dots represent galaxies observed with MMT/Hectospec. (Bottom) Black and red lines show the histogram of the whole galaxies with spectroscopic redshifts and galaxies whose redshifts are measured with MMT/Hectospec in the ﹩R\lt 60^{\prime} ﹩ region, respectively. The blue histogram shows the galaxies determined as cluster members.
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: Rotation profile of the Perseus cluster. (Top) Rotation amplitude. (Bottom) Position angle of the rotation axis. Values in blue triangles are measured with Hwang & Lee (2007) method and those in red circles with Manolopoulou & Plionis (2017). Error bars are resampling errors. The border between the inner region and the outer region is set to 27′ so that there is almost the same number of galaxies in each region.
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: Distribution of galaxies brighter than 19.1 mag within 30′. The radius of each circle is proportional to e  δ . The cluster center is marked with the red cross.
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: Histogram of Δ from Monte Carlo simulated clusters. The red vertical line indicates the Δ value of the real cluster.
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: Comparison of galaxy velocities and ICM velocities for regions with more than three galaxies. (Top) Radial velocity difference of the two components. (Bottom) Radial velocities of galaxies (blue circles), ICM from Hitomi results (green diamonds), and ICM from XMM-Newton results (red squares). The black circles in H3 and X2 indicate velocities of individual galaxies in the region, demonstrating that a single outlier galaxy in the region does not dominate the difference in the galaxy and ICM velocities.
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: Galaxy velocity map (left) and ICM bulk velocity map from Hitomi and XMM-Newton results (right). The galaxy velocity map is weighted with a Gaussian kernel of standard deviation 1.′5. Circles represent individual galaxies color coded according to their velocities, and the black cross is the center of the cluster.
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: Comparison of the results by our CausticSNUpy and the traditional Caustic App. (Top) Absolute difference in the caustic amplitude. (Bottom) Redshift diagram showing the caustics determined by CausticSNUpy (red line) and Caustic App (blue line). Purple crosses are galaxies identified as cluster members by both CausticSNUpy and Caustic App. Red squares and blue triangles are galaxies identified only by CausticSNUpy and Caustic App, respectively. Black open circles are non members as identified by both programs.
Paper: A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang, Byeong-Gon Park
Figure caption: Contours of galaxy number density (black line) overlaid on the X-ray intensity map. The galaxy number density is estimated with a Gaussian kernel of standard deviation 10′.
Paper: The TESS-Keck Survey. XX. 15 New TESS Planets and a Uniform RV Analysis of All Survey Targets
Authors: Alex S. Polanski, Jack Lubin, Corey Beard, Joseph M. Akana Murphy, Ryan Rubenzahl, Michelle L. Hill, Ian J. M. Crossfield, Ashley Chontos, Paul Robertson, Howard Isaacson, Stephen R. Kane, David R. Ciardi, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Erik A. Petigura, Lauren M. Weiss, Isabel Angelo, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Molly R. Kosiarek, Andrew W. Mayo, Mason G. MacDougall, Teo Močnik, Daria Pidhorodetska, Malena Rice, Lee J. Rosenthal, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Samuel W. Yee, David R. Coria, Shannon D. Dulz, Joel D. Hartman, Aaron Householder, Sarah Lange, Andrew Langford, Emma M. Louden, Jared C. Siegel, Emily A. Gilbert, Erica J. Gonzales, Joshua E. Schlieder, Andrew W. Boyle, Jessie L. Christiansen, Catherine A. Clark, Rachel B. Fernandes, Michael B. Lund, Arjun B. Savel, Holden Gill, Charles Beichman, Rachel Matson, Elisabeth C. Matthews, E. Furlan, Steve B. Howell, Nicholas J. Scott, Mark E. Everett, John H. Livingston, Irina O. Ershova, Dmitry V. Cheryasov, Boris Safonov, Jorge Lillo-Box, David Barrado, María Morales-Calderón
Figure caption: Mass–radius diagram for the full TKS sample (blue) in comparison to the all known exoplanets with a ≥3σ mass. Markers are scaled according to the mass precision (size ∝M/σ  M ), while triangles represent 3σ upper limits. Points outlined in gold represent newly confirmed and validated planets in our sample. The region outlined in black represents the region of M-R space shown in more detail in Figure 4.
Paper: The TESS-Keck Survey. XX. 15 New TESS Planets and a Uniform RV Analysis of All Survey Targets
Authors: Alex S. Polanski, Jack Lubin, Corey Beard, Joseph M. Akana Murphy, Ryan Rubenzahl, Michelle L. Hill, Ian J. M. Crossfield, Ashley Chontos, Paul Robertson, Howard Isaacson, Stephen R. Kane, David R. Ciardi, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Erik A. Petigura, Lauren M. Weiss, Isabel Angelo, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Molly R. Kosiarek, Andrew W. Mayo, Mason G. MacDougall, Teo Močnik, Daria Pidhorodetska, Malena Rice, Lee J. Rosenthal, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Samuel W. Yee, David R. Coria, Shannon D. Dulz, Joel D. Hartman, Aaron Householder, Sarah Lange, Andrew Langford, Emma M. Louden, Jared C. Siegel, Emily A. Gilbert, Erica J. Gonzales, Joshua E. Schlieder, Andrew W. Boyle, Jessie L. Christiansen, Catherine A. Clark, Rachel B. Fernandes, Michael B. Lund, Arjun B. Savel, Holden Gill, Charles Beichman, Rachel Matson, Elisabeth C. Matthews, E. Furlan, Steve B. Howell, Nicholas J. Scott, Mark E. Everett, John H. Livingston, Irina O. Ershova, Dmitry V. Cheryasov, Boris Safonov, Jorge Lillo-Box, David Barrado, María Morales-Calderón
Figure caption: Contrast curves for TOI-1443 from Gemini-NIRI (blue) and SAI Speckle Polarimeter (black). The 1σ error for the NIRI contrast curve is given as the blue envelope. A companion is observed for TOI-1443 at ∼0.″5 that is not detected in Gaia DR3.
Paper: The TESS-Keck Survey. XX. 15 New TESS Planets and a Uniform RV Analysis of All Survey Targets
Authors: Alex S. Polanski, Jack Lubin, Corey Beard, Joseph M. Akana Murphy, Ryan Rubenzahl, Michelle L. Hill, Ian J. M. Crossfield, Ashley Chontos, Paul Robertson, Howard Isaacson, Stephen R. Kane, David R. Ciardi, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Erik A. Petigura, Lauren M. Weiss, Isabel Angelo, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Molly R. Kosiarek, Andrew W. Mayo, Mason G. MacDougall, Teo Močnik, Daria Pidhorodetska, Malena Rice, Lee J. Rosenthal, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Samuel W. Yee, David R. Coria, Shannon D. Dulz, Joel D. Hartman, Aaron Householder, Sarah Lange, Andrew Langford, Emma M. Louden, Jared C. Siegel, Emily A. Gilbert, Erica J. Gonzales, Joshua E. Schlieder, Andrew W. Boyle, Jessie L. Christiansen, Catherine A. Clark, Rachel B. Fernandes, Michael B. Lund, Arjun B. Savel, Holden Gill, Charles Beichman, Rachel Matson, Elisabeth C. Matthews, E. Furlan, Steve B. Howell, Nicholas J. Scott, Mark E. Everett, John H. Livingston, Irina O. Ershova, Dmitry V. Cheryasov, Boris Safonov, Jorge Lillo-Box, David Barrado, María Morales-Calderón
Figure caption: A flowchart of our algorithm for homogeneous determination of planet masses.
Paper: The TESS-Keck Survey. XX. 15 New TESS Planets and a Uniform RV Analysis of All Survey Targets
Authors: Alex S. Polanski, Jack Lubin, Corey Beard, Joseph M. Akana Murphy, Ryan Rubenzahl, Michelle L. Hill, Ian J. M. Crossfield, Ashley Chontos, Paul Robertson, Howard Isaacson, Stephen R. Kane, David R. Ciardi, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Erik A. Petigura, Lauren M. Weiss, Isabel Angelo, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Molly R. Kosiarek, Andrew W. Mayo, Mason G. MacDougall, Teo Močnik, Daria Pidhorodetska, Malena Rice, Lee J. Rosenthal, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Samuel W. Yee, David R. Coria, Shannon D. Dulz, Joel D. Hartman, Aaron Householder, Sarah Lange, Andrew Langford, Emma M. Louden, Jared C. Siegel, Emily A. Gilbert, Erica J. Gonzales, Joshua E. Schlieder, Andrew W. Boyle, Jessie L. Christiansen, Catherine A. Clark, Rachel B. Fernandes, Michael B. Lund, Arjun B. Savel, Holden Gill, Charles Beichman, Rachel Matson, Elisabeth C. Matthews, E. Furlan, Steve B. Howell, Nicholas J. Scott, Mark E. Everett, John H. Livingston, Irina O. Ershova, Dmitry V. Cheryasov, Boris Safonov, Jorge Lillo-Box, David Barrado, María Morales-Calderón
Figure caption: The mass–radius space for planets below 4 R ⊕ in the TKS sample. Points are color-coded based on the planets’ equilibrium temperature, while the size is scaled according their mass significance: larger points have a more precise mass measurement. Points outlined in gold are planets whose mass constraints are newly published in this work. Blue contours represent a Gaussian Kernel Density Estimate (KDE) of all known exoplanets around FGK stars. We show the composition tracks for pure iron, an Earth-like composition, and a 50/50 water-silicate mix (Zeng et al. 2019). In addition, we include the photoevaporation mass–radius distributions from Rogers et al. (2023).
Paper: The TESS-Keck Survey. XX. 15 New TESS Planets and a Uniform RV Analysis of All Survey Targets
Authors: Alex S. Polanski, Jack Lubin, Corey Beard, Joseph M. Akana Murphy, Ryan Rubenzahl, Michelle L. Hill, Ian J. M. Crossfield, Ashley Chontos, Paul Robertson, Howard Isaacson, Stephen R. Kane, David R. Ciardi, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Erik A. Petigura, Lauren M. Weiss, Isabel Angelo, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Molly R. Kosiarek, Andrew W. Mayo, Mason G. MacDougall, Teo Močnik, Daria Pidhorodetska, Malena Rice, Lee J. Rosenthal, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Samuel W. Yee, David R. Coria, Shannon D. Dulz, Joel D. Hartman, Aaron Householder, Sarah Lange, Andrew Langford, Emma M. Louden, Jared C. Siegel, Emily A. Gilbert, Erica J. Gonzales, Joshua E. Schlieder, Andrew W. Boyle, Jessie L. Christiansen, Catherine A. Clark, Rachel B. Fernandes, Michael B. Lund, Arjun B. Savel, Holden Gill, Charles Beichman, Rachel Matson, Elisabeth C. Matthews, E. Furlan, Steve B. Howell, Nicholas J. Scott, Mark E. Everett, John H. Livingston, Irina O. Ershova, Dmitry V. Cheryasov, Boris Safonov, Jorge Lillo-Box, David Barrado, María Morales-Calderón
Figure caption: Top: periodogram analysis of all RVs for HIP 1532 b in our data set, first subtracting any offsets and the Gaussian process, then removing the best-fit planet signal (first three panels). We also show a periodogram of the S-indices and the RV window function (last two panels). The planet period is given is shown with the blue vertical line, while the rotation period of the star is in purple. The 1% false-alarm probability (FAP) is the horizontal blue dashed line. Middle: the best-fit Keplerian orbital plus Gaussian process model (blue line). We add in quadrature the jitter terms in Table 6 with the measurement errors for each RV. Residuals to the one-planet fit are shown in the bottom panel. Bottom: RVs phase-folded to the orbital ephemeris of planet b.
Paper: The TESS-Keck Survey. XX. 15 New TESS Planets and a Uniform RV Analysis of All Survey Targets
Authors: Alex S. Polanski, Jack Lubin, Corey Beard, Joseph M. Akana Murphy, Ryan Rubenzahl, Michelle L. Hill, Ian J. M. Crossfield, Ashley Chontos, Paul Robertson, Howard Isaacson, Stephen R. Kane, David R. Ciardi, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Erik A. Petigura, Lauren M. Weiss, Isabel Angelo, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Molly R. Kosiarek, Andrew W. Mayo, Mason G. MacDougall, Teo Močnik, Daria Pidhorodetska, Malena Rice, Lee J. Rosenthal, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Samuel W. Yee, David R. Coria, Shannon D. Dulz, Joel D. Hartman, Aaron Householder, Sarah Lange, Andrew Langford, Emma M. Louden, Jared C. Siegel, Emily A. Gilbert, Erica J. Gonzales, Joshua E. Schlieder, Andrew W. Boyle, Jessie L. Christiansen, Catherine A. Clark, Rachel B. Fernandes, Michael B. Lund, Arjun B. Savel, Holden Gill, Charles Beichman, Rachel Matson, Elisabeth C. Matthews, E. Furlan, Steve B. Howell, Nicholas J. Scott, Mark E. Everett, John H. Livingston, Irina O. Ershova, Dmitry V. Cheryasov, Boris Safonov, Jorge Lillo-Box, David Barrado, María Morales-Calderón
Figure caption: A comparison of mass measurements for the 62 planets in our sample for which masses had been published previously. Black stars indicate the literature value comes from a TKS publication, while blue circles indicate a mass publication outside of our survey. The insets show the comparison for objects exceeding 500 M ⊕(upper left) and a zoomed-in view of the dense region between 5 and 14 M ⊕(lower right).
Paper: The TESS-Keck Survey. XX. 15 New TESS Planets and a Uniform RV Analysis of All Survey Targets
Authors: Alex S. Polanski, Jack Lubin, Corey Beard, Joseph M. Akana Murphy, Ryan Rubenzahl, Michelle L. Hill, Ian J. M. Crossfield, Ashley Chontos, Paul Robertson, Howard Isaacson, Stephen R. Kane, David R. Ciardi, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Erik A. Petigura, Lauren M. Weiss, Isabel Angelo, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Molly R. Kosiarek, Andrew W. Mayo, Mason G. MacDougall, Teo Močnik, Daria Pidhorodetska, Malena Rice, Lee J. Rosenthal, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Samuel W. Yee, David R. Coria, Shannon D. Dulz, Joel D. Hartman, Aaron Householder, Sarah Lange, Andrew Langford, Emma M. Louden, Jared C. Siegel, Emily A. Gilbert, Erica J. Gonzales, Joshua E. Schlieder, Andrew W. Boyle, Jessie L. Christiansen, Catherine A. Clark, Rachel B. Fernandes, Michael B. Lund, Arjun B. Savel, Holden Gill, Charles Beichman, Rachel Matson, Elisabeth C. Matthews, E. Furlan, Steve B. Howell, Nicholas J. Scott, Mark E. Everett, John H. Livingston, Irina O. Ershova, Dmitry V. Cheryasov, Boris Safonov, Jorge Lillo-Box, David Barrado, María Morales-Calderón
Figure caption: Left: A comparison of RV-measured masses to those predicted by the empirical mass–radius relations Weiss & Marcy (2014) and Chen & Kipping (2017). Blue points highlight planets that achieved a 5σ mass significance, while the unfilled point represent the full sample. Right: The mass residual (measured minus predicted) as a function of stellar and planetary parameters (from top): RV semi-amplitude, planetary insolation flux, stellar mass, and stellar metallicity. Pearson and Spearman correlation coefficients are given for both the 5σ sample and the full sample (in brackets).
Paper: The TESS-Keck Survey. XX. 15 New TESS Planets and a Uniform RV Analysis of All Survey Targets
Authors: Alex S. Polanski, Jack Lubin, Corey Beard, Joseph M. Akana Murphy, Ryan Rubenzahl, Michelle L. Hill, Ian J. M. Crossfield, Ashley Chontos, Paul Robertson, Howard Isaacson, Stephen R. Kane, David R. Ciardi, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Erik A. Petigura, Lauren M. Weiss, Isabel Angelo, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Molly R. Kosiarek, Andrew W. Mayo, Mason G. MacDougall, Teo Močnik, Daria Pidhorodetska, Malena Rice, Lee J. Rosenthal, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Samuel W. Yee, David R. Coria, Shannon D. Dulz, Joel D. Hartman, Aaron Householder, Sarah Lange, Andrew Langford, Emma M. Louden, Jared C. Siegel, Emily A. Gilbert, Erica J. Gonzales, Joshua E. Schlieder, Andrew W. Boyle, Jessie L. Christiansen, Catherine A. Clark, Rachel B. Fernandes, Michael B. Lund, Arjun B. Savel, Holden Gill, Charles Beichman, Rachel Matson, Elisabeth C. Matthews, E. Furlan, Steve B. Howell, Nicholas J. Scott, Mark E. Everett, John H. Livingston, Irina O. Ershova, Dmitry V. Cheryasov, Boris Safonov, Jorge Lillo-Box, David Barrado, María Morales-Calderón
Figure caption: Top: periodogram analysis of all RVs for TOI–1173 b in our data set, first subtracting any offsets, then removing the best-fit planet signal (first two panels). We also show a periodogram of the S-indices and the RV window function (last two panels). The planet period is given is shown with the blue vertical line, while the 1% false-alarm probability (FAP) is the horizontal blue dashed line. Middle: the best-fit Keplerian orbital model (blue line). We add in quadrature the jitter terms in Table 6 with the measurement errors for each RV. Residuals to the one-planet fit are shown in the bottom panel. Bottom: RVs phase-folded to the orbital ephemeris of planet b.
Paper: The TESS-Keck Survey. XX. 15 New TESS Planets and a Uniform RV Analysis of All Survey Targets
Authors: Alex S. Polanski, Jack Lubin, Corey Beard, Joseph M. Akana Murphy, Ryan Rubenzahl, Michelle L. Hill, Ian J. M. Crossfield, Ashley Chontos, Paul Robertson, Howard Isaacson, Stephen R. Kane, David R. Ciardi, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Erik A. Petigura, Lauren M. Weiss, Isabel Angelo, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Lea A. Hirsch, Rae Holcomb, Molly R. Kosiarek, Andrew W. Mayo, Mason G. MacDougall, Teo Močnik, Daria Pidhorodetska, Malena Rice, Lee J. Rosenthal, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Samuel W. Yee, David R. Coria, Shannon D. Dulz, Joel D. Hartman, Aaron Householder, Sarah Lange, Andrew Langford, Emma M. Louden, Jared C. Siegel, Emily A. Gilbert, Erica J. Gonzales, Joshua E. Schlieder, Andrew W. Boyle, Jessie L. Christiansen, Catherine A. Clark, Rachel B. Fernandes, Michael B. Lund, Arjun B. Savel, Holden Gill, Charles Beichman, Rachel Matson, Elisabeth C. Matthews, E. Furlan, Steve B. Howell, Nicholas J. Scott, Mark E. Everett, John H. Livingston, Irina O. Ershova, Dmitry V. Cheryasov, Boris Safonov, Jorge Lillo-Box, David Barrado, María Morales-Calderón
Figure caption: Top: The number of observations obtained broken down by science case. The vertical dashed lines represent the N obs targets set in Chontos et al. (2022). Bottom: The median time difference between observations (cadence) for our targets broken down by science case.