adsabs/AstroCLIMB huggingface dataset:
Paper: A High-Eccentricity Warm Jupiter Orbiting TOI-4127
Authors: Arvind F. Gupta, Jonathan M. Jackson, Guillaume Hébrard, Andrea S. J. Lin, Keivan G. Stassun, Jiayin Dong, Steven Villanueva, Diana Dragomir, Suvrath Mahadevan, Jason T. Wright, Jose M. Almenara, Cullen H. Blake, Isabelle Boisse, Pía Cortés-Zuleta, Paul A. Dalba, Rodrigo F. Díaz, Eric B. Ford, Thierry Forveille, Robert Gagliano, Samuel Halverson, Neda Heidari, Shubham Kanodia, Flavien Kiefer, David w. Latham, Michael W. McElwain, Ismael Mireles, Claire Moutou, Joshua Pepper, George R. Ricker, Paul Robertson, Arpita Roy, Martin Schlecker, Christian Schwab, S. Seager, Avi Shporer, Guđmundur Stefánsson, Ryan C. Terrien, Eric B. Ting, Joshua N. Winn, Allison Youngblood
Figure caption: Projected transit ephemeris for TOI-4127 b for the 60 orbits following the transit detected in Sector 20. The 1, 2, and 3σ uncertainties on the ephemeris are shown as progressively lighter, gray shaded regions. Past and future transit times are indicated by vertical orange bars, and the observed transits in Sectors 20, 26, and 53 are indicated in green, blue, and pink, respectively, to match the light curves in Figure 1. We expect the ephemeris to remain precise to better than 25 minutes, or 10% of the transit duration, through early 2029.
Paper: A High-Eccentricity Warm Jupiter Orbiting TOI-4127
Authors: Arvind F. Gupta, Jonathan M. Jackson, Guillaume Hébrard, Andrea S. J. Lin, Keivan G. Stassun, Jiayin Dong, Steven Villanueva, Diana Dragomir, Suvrath Mahadevan, Jason T. Wright, Jose M. Almenara, Cullen H. Blake, Isabelle Boisse, Pía Cortés-Zuleta, Paul A. Dalba, Rodrigo F. Díaz, Eric B. Ford, Thierry Forveille, Robert Gagliano, Samuel Halverson, Neda Heidari, Shubham Kanodia, Flavien Kiefer, David w. Latham, Michael W. McElwain, Ismael Mireles, Claire Moutou, Joshua Pepper, George R. Ricker, Paul Robertson, Arpita Roy, Martin Schlecker, Christian Schwab, S. Seager, Avi Shporer, Guđmundur Stefánsson, Ryan C. Terrien, Eric B. Ting, Joshua N. Winn, Allison Youngblood
Figure caption: In-transit TESS data for TOI-4127 b, folded to the fitted orbital period. In the top panel, we plot the Sector 20 and Sector 26 data in green and blue, respectively, and the Sector 53 data in pink, to match the light curves shown in Figure 1. We include both the binned (30 minutes cadence) and unbinned (2 minutes cadence) Sector 53 transit data. We show the best-fit model in black and 3σ uncertainties in gray, and we plot the residuals to this fit in the bottom panel.
Paper: A High-Eccentricity Warm Jupiter Orbiting TOI-4127
Authors: Arvind F. Gupta, Jonathan M. Jackson, Guillaume Hébrard, Andrea S. J. Lin, Keivan G. Stassun, Jiayin Dong, Steven Villanueva, Diana Dragomir, Suvrath Mahadevan, Jason T. Wright, Jose M. Almenara, Cullen H. Blake, Isabelle Boisse, Pía Cortés-Zuleta, Paul A. Dalba, Rodrigo F. Díaz, Eric B. Ford, Thierry Forveille, Robert Gagliano, Samuel Halverson, Neda Heidari, Shubham Kanodia, Flavien Kiefer, David w. Latham, Michael W. McElwain, Ismael Mireles, Claire Moutou, Joshua Pepper, George R. Ricker, Paul Robertson, Arpita Roy, Martin Schlecker, Christian Schwab, S. Seager, Avi Shporer, Guđmundur Stefánsson, Ryan C. Terrien, Eric B. Ting, Joshua N. Winn, Allison Youngblood
Figure caption: Generalized Lomb–Scargle periodograms for the full RV data set (top) and residuals (bottom). We mark the best-fit orbital period with a dashed red line. No periodic signals are prominent in the residuals.
Paper: A High-Eccentricity Warm Jupiter Orbiting TOI-4127
Authors: Arvind F. Gupta, Jonathan M. Jackson, Guillaume Hébrard, Andrea S. J. Lin, Keivan G. Stassun, Jiayin Dong, Steven Villanueva, Diana Dragomir, Suvrath Mahadevan, Jason T. Wright, Jose M. Almenara, Cullen H. Blake, Isabelle Boisse, Pía Cortés-Zuleta, Paul A. Dalba, Rodrigo F. Díaz, Eric B. Ford, Thierry Forveille, Robert Gagliano, Samuel Halverson, Neda Heidari, Shubham Kanodia, Flavien Kiefer, David w. Latham, Michael W. McElwain, Ismael Mireles, Claire Moutou, Joshua Pepper, George R. Ricker, Paul Robertson, Arpita Roy, Martin Schlecker, Christian Schwab, S. Seager, Avi Shporer, Guđmundur Stefánsson, Ryan C. Terrien, Eric B. Ting, Joshua N. Winn, Allison Youngblood
Figure caption: Reconstructed NESSI speckle images and 5σ contrast curves for TOI-4127. Observations were taken simultaneously at 532 nm with the blue camera (left-hand inset image) and at 832 nm with the red camera (right-hand inset image). The contrast curves indicate the limiting magnitude difference at which bound or background stars could be detected for separations up to 1.″2.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: Results of running various sky-SB estimation algorithms (Methods 1–9) on simulated HST WFC3/IR F125W images, where % Error=(Measured Sky—Input Sky)/Input Sky ×100%. The solid colored lines represent the linear best fit for binned data where each bin contains 10–11 simulated images. Methods listed with an asterisk (*) are able to account for sky gradients and are thus included in the right panel. Left: algorithm performance on simulated images with no sky gradient, plotted against the known, true sky-SB rms of the simulated image. Right: algorithm performance on simulated images with a sky gradient, plotted against the known sky gradient of the image.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: SKYSURF sky-SB SED for ecliptic latitudes within 40° of the poles. Each black point is an ACS/WFC (square), WFC3/UVIS (circle), or WFC3/IR (triangle) median sky-SB measurement. The error bar is the standard error in unique positions in the sky and the sky-SB measurement error, added in quadrature (see Equation (3)). Only filters with at least two unique positions are plotted. We compare our measurements to comparable measurements of the sky-SB taken near the ecliptic poles with space telescopes or sounding rockets (Hauser et al. 1998; Bernstein et al. 2002; Giavalisco et al. 2002; Matsuura et al. 2017; Carleton et al. 2022), a model of ZL emission (Aldering 2001), and measurements of ZL emission (Kawara et al. 2017). Overall, SKYSURF sky-SB measurements agree well with other models and predictions, although some offsets remain present in studies where the light from discrete objects is not removed (Hauser et al. 1998; Bernstein et al. 2002; Matsuura et al. 2017).
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: SKYSURF sky-SB SED for different ecliptic latitude (b, where each bin includes the absolute value of b) bins and Sun angle (s) bins. As the Sun angle can be correlated with the ecliptic latitude, the bottom plot has a fixed range in the ecliptic latitude of −30° < b < 30°. Each point is an ACS/WFC (squares), WFC3/UVIS (circles), or WFC3/IR (triangles) 3σ-clipped median sky-SB measurement. The error bars are scaled in the same way described in Figure 7.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: SKYSURF sky-SB measurements vs. ecliptic latitude for WFC3/IR, zoomed in to show the range between 0 and 0.5 MJy sr−1. The large scatter in points in the F105W filter at −45° is due to observations of the Hubble Ultra Deep Field, where the 1.083 μm emission line (Brammer et al. 2014) present in this filter likely contaminated some of these measurements. As an example of the sky-SB measurements we expect, we include the F125W, F140W, and F160W sech curves from Figure 2 of SKYSURF–2, which are derived to match Kelsall et al. (1998) zodiacal model predictions. Our measurements fall conservatively within these limits.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: Comparison of the Pro-med and Pro-5th algorithms. The error bars show the 16th and 84th percentiles of the y-axis distributions. Left: median ratio of the Pro-med sky-SB divided by the Pro-5th sky-SB. The bluest filters are excluded because the sky-SB is nearly zero, such that the ratios become extreme values. Right: median difference in the Pro-Med and Pro-5th methods. The left y-axis is in units of MJy sr−1, and the right axis is in units of nW m−2 sr−1 at 0.6 μm.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: Example simulated images. The custom galaxy sampling method (left column) employs a distribution of galaxy parameters based on Windhorst et al. (2011). The Cosmic Evolution Survey (COSMOS) galaxy sampling method randomly selects galaxies from the COSMOS (van der Wel et al. 2014) F125W database. The top images have no sky gradient added, while the bottom images have a sky gradient imposed on them.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: SKYSURF sky-SB measurements vs. ecliptic latitude for three example filters. We compare the Pro-med method (green) to the Pro-5th method (orange). As an example of the sky-SB measurements we expect, we include the WFC3/IR F160W sech curve from Figure 2 of SKYSURF–2, which is derived to match Kelsall COBE/DIRBE model predictions. Our measurements fall conservatively within these limits.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: Median sky-SB rms for each filter. The error bars show the 16th and 84th percentiles of the rms distributions. The sky-SB rms trends seen here are likely due to the different pixel sizes of each camera.
Paper: SKYSURF-4: Panchromatic Hubble Space Telescope All-Sky Surface-brightness Measurement Methods and Results
Authors: Rosalia O'Brien, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Delondrae Carter, Scott Tompkins, Sarah Caddy, Seth H. Cohen, Haley Abate, Richard G. Arendt, Jessica Berkheimer, Annalisa Calamida, Stefano Casertano, Simon P. Driver, Connor Gelb, Zak Goisman, Norman Grogin, Daniel Henningsen, Isabela Huckabee, Scott J. Kenyon, Anton M. Koekemoer, Darby Kramer, John Mackenty, Aaron Robotham, Steven Sherman
Figure caption: SKYSURF sky-SB measurements vs. ecliptic latitude for ACS/WFC, zoomed in to show the range between 0 and 0.5 MJy sr−1.
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: Top: projected starspots on TOI-3884's stellar surface for a polar starspot with a stellar spin axis tilt of −65° and λ = 75° using the APO SDSS ﹩{r}^{{\prime} }﹩ filter transit observed on 2022 June 3 assuming a spot temperature of 2900 K and a photospheric temperature of 3200 K (spot contrast of 0.7 for ﹩{r}^{{\prime} }﹩ band). The large blue spot in the middle has a relative radius R spot/R  s  = 0.31, with the two smaller blue spots having radii R spot/R  s  = 0.22 and 0.11, respectively, and the red starspots corresponding to the same starspots shown in Figure 9. The fractional spotted area in the transit chord for the blue stellar surface features assuming that there are no spots anywhere else on the star is 4%. Middle: best-fit starspot model for the oblique (not aligned) system (blue line) compared to the no starspot transit model (cyan line), with the APO ﹩{r}^{{\prime} }﹩-band data shown as black points with error bars. The red line is the STSP model created by extending the SDSS ﹩{i}^{{\prime} }﹩ polar spot model to the SDSS ﹩{r}^{{\prime} }﹩ contrast. Bottom: residuals from the best-fit starspot model (blue points) and scaled from the SDSS ﹩{i}^{{\prime} }﹩ polar spot model (red points).
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: TSM as a function of planetary equilibrium temperature for all planets with a known (>3σ) mass and T eq cooler than 1000 K. Points are colored based on their host star’s effective temperature, with planets around M dwarfs denoted with solid coloring. The approximate temperature when ammonia appears in a planet’s atmosphere (assuming equilibrium chemistry) is denoted with the black dashed line. TOI-3884b (blue circle) possesses one of the highest TSMs of any non–hot Jupiter and the highest TSM for planets <500 K.
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: Sample of transiting M-dwarf planets that have precise mass measurements (>3σ). (a) Mass–radius plane showing the small sample (∼15) of giant planets (R  p  > 4 R ⊕) orbiting M dwarfs (T eff < 4000 K), color-coded by T eff. (b) The masses for all M-dwarf planets as a function of T eff, showing how TOI-3884b stands out in terms of its stellar host. Transiting planets are shown as circles, whereas RV-only (m sini) detections are shown as squares. The clump of planets at ∼2600 K represents the TRAPPIST-1 system (Grimm et al. 2018).
Paper: An In-depth Look at TOI-3884b: A Super-Neptune Transiting an M4Dwarf with Persistent Starspot Crossings
Authors: Jessica E. Libby-Roberts, Maria Schutte, Leslie Hebb, Shubham Kanodia, Caleb I. Cañas, Guðmundur Stefánsson, Andrea S. J. Lin, Suvrath Mahadevan, Winter Parts(they/them), Luke Powers, John Wisniewski, Chad F. Bender, William D. Cochran, Scott A. Diddams, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Andrew Monson, Joe P. Ninan, Brock A. Parker, Lawrence W. Ramsey, Paul Robertson, Christian Schwab, Tera N. Swaby, Ryan C. Terrien
Figure caption: Transmission spectra generated with ExoTransmit for a 100× solar metallicity atmosphere in chemical equilibrium with gray-absorber aerosol layer at 10 and 100 μm. Simulated data are created using PandExo for two transits of JWST/NIRSpec and based on the cloud-free model. The two dominant absorbers, water and methane, are labeled for reference, though other molecules, including ammonia, are also included in the models.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Map of star counts with 10.5 < H  s  < 22 mag, N source(l, b), in our source catalogs generated by genstars. Most of stars in the region ∣b∣ < 0.°5 and ∣l∣ < 1.°5 belong to the NSD component, yielding high stellar density. However, owing to the high extinction, the number of sources is small in the Galactic center and the Galactic plane.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Photometric precision of PRIME as a function of the H-band magnitude when each observation epoch will be composed of twelve 9 s co-added dithered exposures and take 160 s including overhead, assuming no blending and typical seeing. The black line shows the photometric precision assuming the sky background is 13.6 mag arcsec−2. The gray region shows the photometric precision assuming the sky background is (13.0–14.2 mag arcsec−2. The red and blue dotted lines indicate the saturation limit in a single read and the faint magnitude limit for a 5σ.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Examples of simulated microlensing events whose planetary perturbation are detectable with the PRIME microlensing survey. The insets show the zoom-in of planetary signatures. The red dots show the synthetic data points with a 16 minute cadence. The planetary model for each event is shown in the orange line. The gray dotted lines show the best-fit single-lens models.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Schematic view of our simulation to estimate the detection efficiency of both microlensing events and planets at specific (l,b). For each Galactic coordinate and for each observation cadence, a Monte Carlo simulation is performed to calculate the detectability of 100,000 microlensing events.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Same as Figure 3, but for the planetary microlensing events that do not pass the detection criteria of the planetary signatures. The observation cadence is 32 minutes in these examples.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Planet detection maps along each line of sight. Each plot shows the number of detections with 16, 32, 48, and 96 minute cadences. This figure is obtained by multiplying the number of microlensing detections, N ML(l, b) (Figure 13), and the mean detection efficiency of planets, ϵ PL, which is obtained by averaging over all fields, over masses of 0.1 < M  p  < 105 M ⊕, and semimajor axis values of 0.3 < a < 30 au and corrected by a modified cool-planet frequency based on Penny et al. (2019). The planet detection map with a 16 minute cadence (upper left panel) is used to determine the order of the observation fields in Section 5.1. Each white square shows a 1.45 deg2 FOV field. The field numbers are ranked by the expected number of planet detections summed across each square.
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Field locations for the PRIME microlensing survey for each observation strategy considered in this work, plotted over the planet detection map with a 16 minute cadence. The top and middle panels show the observation strategies, S1–S4, described in Section 5.1. The bottom panel shows the spatially uniform survey including the Galactic center and the Galactic plane described in Section 6.1. The field numbers are ranked by their expectation of planet detections (Figure 15). Each square shows a 1.45 deg2 FOV field, where the red, green, blue, and white colors indicate cadences of 16, 32, 48, and 96 minutes, respectively. The gray region shows the assumed field placement for the Roman microlensing survey (Penny et al. 2019).