adsabs/AstroCLIMB huggingface dataset:
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Top row: transit search lightcurve plot for MISHAPS_F47T_S11_01004730 from night 1403 showing a S/N = 8.7 detection. The images in the middle and right of the row are the in-transit stacked difference image and the reference image. Middle: detrended (blue) and target-centered (cyan) lightcurves of the night 1403 transit. The lines show transiting planet fits to each lightcurve. The target-centered lightcurve is shifted so that the model baselines match. Bottom row: time series of target-centered difference images of the target on the same night showing the evolution of dipoles. The last image in the sequence is the reference image.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Example of a candidate rejected for a clear blend. The lightcurve of the detection is plotted on the left with the search’s model. The stacked in-transit difference image and reference image are shown in the middle and right panels, respectively. Though the lightcurves seem to indicate a clear longer-duration eclipse, inspection of the images leads us to reject this candidate.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Positions of all high-quality (DOPHOT flag = 1) star detections in our field (black points) and our target stars (red points), with the candidates highlighted. The rejected candidates are given by the blue circles, and the EBs are given by the yellow squares. The large missing section in the center is due to our removing the central CCDs from our data set. The rest of the seemingly missing sections are due to either faulty CCDs (middle left, bottom middle) or not having enough stars meeting our requirements to have those sections appear populated.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: r-band lightcurves from survey night 1225 for MISHAPS_F47T_S9_01005029 (left), MISHAPS_F47T_S10_01006025 (middle), and MISHAPS_F47T_S10_01010875 (right). The detrended lightcurves are plotted in teal circles, and the target-centered lightcurves are plotted in purple triangles. Each lightcurve showed a similar dip at roughly the same time in the original detrended r-band lightcurves, but the target-centered photometry was able to remove this signal, indicating a likely systemic error in the difference images for this time period.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Two-dimensional plots of the detection efficiencies of our pipeline, estimated in bins of Rp and P. The top panel shows ﹩{\epsilon }_{{\rm{\det }}}﹩ for the search algorithm, the middle panel shows ϵZoo for the Zooniverse vetting, and the bottom panel shows the overall efficiency incorporating the transit probability (e.g., ﹩{P}_{{\rm{tr}}}{\epsilon }_{{\rm{\det }}}{\epsilon }_{{\rm{Zoo}}}﹩). The bins are color-coded by efficiency, and the numbers labeling each bin give the respective detection efficiency and 1σ errors in percent.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Efficiencies of our transit search and Zooniverse vetting, binned as a function of planet radius Rp (top left), orbital period P (top right), r magnitude (bottom left), and impact parameter b (bottom right). The yellow-triangle lines show our detection efficiency ﹩{\epsilon }_{{\rm{\det }}}﹩, the blue-square lines show our Zooniverse vetting efficiency ϵZoo, the red-diamond lines show our transit probability Ptransit, and the black-circle lines show the combined efficiencies.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Lightcurves and stacked in-eclipse difference images for EB candidates. The lightcurves of each detection are shown in the left column, with the r-band data plotted in blue, and the z-band data plotted in red. The middle column shows the stacked in-eclipse difference images for each detection, and the right column shows the reference image for side-by-side comparison.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Same as Figure 10, but plotting detection efficiencies in bins of Rp and r magnitude.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: CMD for our field (black points) with our targets (red points) and candidates highlighted. The rejected candidates are given by the blue circles, and the EBs are given by the yellow squares.
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Original reflectance spectra of Pholus (left; S. Fornasier et al. 2009) and Bienor (right; A. Alvarez-Candal et al. 2008), normalized at 550nm. Overlaid are the new extrapolated, smoothed “spectra” that are used to convert to SEDs and obtain color estimates. Below are the LSST filter throughputs for wavelength range reference. Note that Bienor’s spectrum has been smoothed starting at ∼750 nm in order to account for the increased noise in the proceeding range.
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Histogram on top of the median apparent magnitude of discovered Centaurs in the r band, separated by G08, S19, and Hybrid definitions, overplotted with a dashed line of the limiting magnitude in the LSST r. Below is a histogram of the same sample’s absolute r-band magnitudes.
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Number of Centaurs that would obtain at least three colors in ugrizy. Each bar represents the fraction of each subsample of discovered objects that would pass the color metrics defined in M. E. Schwamb et al. (2023), with the actual number of Centaurs this represents above each bar. Panel (a) highlights those passing the metrics with an S/N ≥ 5 cut, whereas panel (b) highlights the same but for an S/N ≥ 25 cut as was used in the OSSOS survey.
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Histogram showing the number of 10,000 simulations of each trial N0 value for the Hybrid definition that match the G08 sample scaling of N(H  < 13.7) = 21,400. The dashed line represents the mean value of the distribution, and the shaded region is the 95% confidence interval.
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Cumulative histograms of the number of observations each object detected in each sample will obtain, broken down by filter—excluding those observations that fall within the COSMOS DDF. Note that for all of these plots the x-axis is cut off at 250 for readability; however, the G08 sample extends to ∼800, the S19 sample extends to ∼650, and the Hybrid sample extends to ∼900 owing to objects entering DDFs. The reported median values in the legends include these values.
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Cumulative histogram (with a bin size of 1 day) of the discovery rates of the different Centaur definitions over the 10 yr LSST lifetime. Red dashed lines demark yearly boundaries for the survey, with labels above each block to highlight the year of operation. We highlight the points of 50% (open triangle), 80% (open square), and 90% (open circle) completion for each population.
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Scatter plots of the orbital spaces covered by discovered objects, similar to Figure 2. Once again the columns represent the three respective definitions, whereas the top row represents Centaur eccentricity as a function of semimajor axis, and the bottom row represents Centaur inclination as a function of perihelion distance.
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Example phase curves across all ugrizy filters for a randomly sampled object from the G08 sample. There are no uy-band phase curves here, as they do not have enough observations passing metrics for quality phase curves. All filters that do pass the metrics have been overplotted with the linear fit to the data as determined in the text.
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Histograms of the ecliptic latitudes for each of the G08 (red), S19 (green), and Hybrid (blue) definitions at the time of each object’s discovery.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: Ground-based photometry of HD 35843 b from LCOGT, MEarth, and the Next Generation Transit Survey (NGTS) along with the best-fit transit light curve from the joint TESS + ESPRESSO fit in red. Blue curves account for the potential transit timing variations (TTVs) discussed in Section 3.5.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: Left: Gemini speckle imaging contrast curves of HD 35843 (TOI 4189), with insets showing the images for each filter. Right: high-resolution speckle imaging and contrast curve from SOAR.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: Top: full TESS PDCSAP light curve of HD 35843. Transits of HD 35843 c are marked with dashed magenta lines. Bottom: zoom-in view of the three individual transits from Sectors 6, 32, and 33 along with the best-fit transit light curve.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: A periodogram of the accumulated WASP-South data, showing the absence of any rotational modulation. The horizontal line is the estimated 1% likelihood false-alarm level (the highest peak near 30 days is caused by the residual effects of moonlight, propagating through the reduction pipeline at a low level).
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: TESS target pixel files of HD 35843 (TIC 7422496) for all five sectors of observations made using tpfplotter (A. Aller et al. 2020). The SPOC photometric aperture is highlighted in each panel.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: ESPRESSO RVs for HD 35843 and best-fit RV curve for the two-planet system.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: Period–radius diagram of confirmed and validated sub-Neptunes as of this writing. Magenta diamonds denote long-period (P > 40 days) planets with upper limits on their masses, masses from TTVs, or RV masses that are loosely constrained (<3σ). Cyan triangles mark well-constrained masses (>3σ). The gold star marks the subject of this paper, HD 35843 c.