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Paper: The TESS-Keck Survey. XI. Mass Measurements for Four Transiting Sub-Neptunes Orbiting K Dwarf TOI–1246
Authors: Emma V. Turtelboom, Lauren M. Weiss, Courtney D. Dressing, Grzegorz Nowak, Enric Pallé, Corey Beard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Zachary R. Claytor, Fei Dai, Paul A. Dalba, Steven Giacalone, Erica Gonzales, Caleb K. Harada, Michelle L. Hill, Rae Holcomb, Judith Korth, Jack Lubin, Thomas Masseron, Mason MacDougall, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Ryan A. Rubenzahl, Nicholas Scarsdale, Keivan G. Stassun, Dakotah B. Tyler, Judah Van Zandt, Ian J. M. Crossfield, Hans J. Deeg, Benjamin Fulton, Davide Gandolfi, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Kristine W. F. Lam, Rafael Luque, Eduardo L. Martín, Giuseppe Morello, Jaume Orell-Miquel, Erik A. Petigura, Paul Robertson, Arpita Roy, Vincent Van Eylen, David Baker, Alexander A. Belinski, Allyson Bieryla, David R. Ciardi, Karen A. Collins, Neil Cutting, Devin J. Della-Rose, Taylor B. Ellingsen, E. Furlan, Tianjun Gan, Crystal L. Gnilka, Pere Guerra, Steve B. Howell, Mary Jimenez, David W. Latham, Maude Larivière, Kathryn V. Lester, Jorge Lillo-Box, Lindy Luker, Christopher R. Mann, Peter P. Plavchan, Boris Safonov, Brett Skinner, Ivan A. Strakhov, Justin M. Wittrock, Douglas A. Caldwell, Zahra Essack, Jon M. Jenkins, Elisa V. Quintana, George R. Ricker, Roland Vanderspek, S. Seager, Joshua N. Winn
Figure caption: Lomb–Scargle periodograms for the RV data, RV residuals from a four-planet fit, activity indicators, and spectral window function for TOI-1246 using Keck/HIRES and TNG/HARPS-N data (see legends). The vertical colored lines indicate the periods of the four transiting planets in the system (TOI-1246 b: purple, TOI-1246c: blue, TOI-1246 d: light blue, TOI-1246 e: pink). The green region indicates the range of likely periods for the fifth candidate planet. We consider the peaks at both 76 and 94 d, and choose to report the fifth candidate planet at 94 d in this work. In the top panel, the horizontal dashed lines represent the 1% and 0.1% false-alarm levels. In the second panel, we show two closely spaced horizontal dashed lines in the range of period space we consider. These lines represent the 99.99th percentile of 10,000 bootstrap samples of these residuals, in dark green (for the 76 d signal) and green (for the 94 d signal), and show that both of these signals are statistically significant.
Paper: The TESS-Keck Survey. XI. Mass Measurements for Four Transiting Sub-Neptunes Orbiting K Dwarf TOI–1246
Authors: Emma V. Turtelboom, Lauren M. Weiss, Courtney D. Dressing, Grzegorz Nowak, Enric Pallé, Corey Beard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Zachary R. Claytor, Fei Dai, Paul A. Dalba, Steven Giacalone, Erica Gonzales, Caleb K. Harada, Michelle L. Hill, Rae Holcomb, Judith Korth, Jack Lubin, Thomas Masseron, Mason MacDougall, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Ryan A. Rubenzahl, Nicholas Scarsdale, Keivan G. Stassun, Dakotah B. Tyler, Judah Van Zandt, Ian J. M. Crossfield, Hans J. Deeg, Benjamin Fulton, Davide Gandolfi, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Kristine W. F. Lam, Rafael Luque, Eduardo L. Martín, Giuseppe Morello, Jaume Orell-Miquel, Erik A. Petigura, Paul Robertson, Arpita Roy, Vincent Van Eylen, David Baker, Alexander A. Belinski, Allyson Bieryla, David R. Ciardi, Karen A. Collins, Neil Cutting, Devin J. Della-Rose, Taylor B. Ellingsen, E. Furlan, Tianjun Gan, Crystal L. Gnilka, Pere Guerra, Steve B. Howell, Mary Jimenez, David W. Latham, Maude Larivière, Kathryn V. Lester, Jorge Lillo-Box, Lindy Luker, Christopher R. Mann, Peter P. Plavchan, Boris Safonov, Brett Skinner, Ivan A. Strakhov, Justin M. Wittrock, Douglas A. Caldwell, Zahra Essack, Jon M. Jenkins, Elisa V. Quintana, George R. Ricker, Roland Vanderspek, S. Seager, Joshua N. Winn
Figure caption: RV data and models for the four transiting planets and a fifth nontransiting planet candidate. The top panel shows the complete RV time series (orange points are TNG/HARPS-N data, and red points are Keck/HIRES) with the preferred five-planet RV model overlaid in black and with residuals (rms = 4.3 m s−1) shown below. The five panels beneath this show the RV data phased to each planets’ orbital period (with binned data points in yellow and blue), with the other planets’ signals removed, and with the RV model overlaid in black.
Paper: The TESS-Keck Survey. XI. Mass Measurements for Four Transiting Sub-Neptunes Orbiting K Dwarf TOI–1246
Authors: Emma V. Turtelboom, Lauren M. Weiss, Courtney D. Dressing, Grzegorz Nowak, Enric Pallé, Corey Beard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Zachary R. Claytor, Fei Dai, Paul A. Dalba, Steven Giacalone, Erica Gonzales, Caleb K. Harada, Michelle L. Hill, Rae Holcomb, Judith Korth, Jack Lubin, Thomas Masseron, Mason MacDougall, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Ryan A. Rubenzahl, Nicholas Scarsdale, Keivan G. Stassun, Dakotah B. Tyler, Judah Van Zandt, Ian J. M. Crossfield, Hans J. Deeg, Benjamin Fulton, Davide Gandolfi, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Kristine W. F. Lam, Rafael Luque, Eduardo L. Martín, Giuseppe Morello, Jaume Orell-Miquel, Erik A. Petigura, Paul Robertson, Arpita Roy, Vincent Van Eylen, David Baker, Alexander A. Belinski, Allyson Bieryla, David R. Ciardi, Karen A. Collins, Neil Cutting, Devin J. Della-Rose, Taylor B. Ellingsen, E. Furlan, Tianjun Gan, Crystal L. Gnilka, Pere Guerra, Steve B. Howell, Mary Jimenez, David W. Latham, Maude Larivière, Kathryn V. Lester, Jorge Lillo-Box, Lindy Luker, Christopher R. Mann, Peter P. Plavchan, Boris Safonov, Brett Skinner, Ivan A. Strakhov, Justin M. Wittrock, Douglas A. Caldwell, Zahra Essack, Jon M. Jenkins, Elisa V. Quintana, George R. Ricker, Roland Vanderspek, S. Seager, Joshua N. Winn
Figure caption: Top panel: the times of Keck/HIRES and TNG/HARPS-N RV observations of TOI-1246, which were contemporaneous with TESS observations. Times are shown in BTJD, which is defined as BJDTDB - 2457000. BJDTDB is the Barycentric Julian Date in the Barycentric Dynamical Time standard. Middle panel: Flattened and normalized light curve of TOI-1246 derived from TESS PDCSAP photometry using the Lightkurve package (Lightkurve Collaboration et al. 2018). The times of full transits are indicated with dots below the light curve in various colors (TOI-1246 b: purple, TOI-1246c: blue, TOI-1246 d: light blue, TOI-1246 e: pink). A zoomed-in inset is shown of a single transit of TOI-1246 e with the best-fit model overlaid (see Section 4.1). Lower panel: raw TESS SAP photometry of TOI-1246 with a zoomed-in inset of sector 23 to illustrate intra-sector variability.
Paper: The TESS-Keck Survey. XI. Mass Measurements for Four Transiting Sub-Neptunes Orbiting K Dwarf TOI–1246
Authors: Emma V. Turtelboom, Lauren M. Weiss, Courtney D. Dressing, Grzegorz Nowak, Enric Pallé, Corey Beard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Zachary R. Claytor, Fei Dai, Paul A. Dalba, Steven Giacalone, Erica Gonzales, Caleb K. Harada, Michelle L. Hill, Rae Holcomb, Judith Korth, Jack Lubin, Thomas Masseron, Mason MacDougall, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Ryan A. Rubenzahl, Nicholas Scarsdale, Keivan G. Stassun, Dakotah B. Tyler, Judah Van Zandt, Ian J. M. Crossfield, Hans J. Deeg, Benjamin Fulton, Davide Gandolfi, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Kristine W. F. Lam, Rafael Luque, Eduardo L. Martín, Giuseppe Morello, Jaume Orell-Miquel, Erik A. Petigura, Paul Robertson, Arpita Roy, Vincent Van Eylen, David Baker, Alexander A. Belinski, Allyson Bieryla, David R. Ciardi, Karen A. Collins, Neil Cutting, Devin J. Della-Rose, Taylor B. Ellingsen, E. Furlan, Tianjun Gan, Crystal L. Gnilka, Pere Guerra, Steve B. Howell, Mary Jimenez, David W. Latham, Maude Larivière, Kathryn V. Lester, Jorge Lillo-Box, Lindy Luker, Christopher R. Mann, Peter P. Plavchan, Boris Safonov, Brett Skinner, Ivan A. Strakhov, Justin M. Wittrock, Douglas A. Caldwell, Zahra Essack, Jon M. Jenkins, Elisa V. Quintana, George R. Ricker, Roland Vanderspek, S. Seager, Joshua N. Winn
Figure caption: Spectral energy distribution of TOI-1246. Red symbols represent the observed photometric measurements, and the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit Kurucz atmosphere model (black). We observe some NUV excess that implies moderate stellar activity for this star.
Paper: The TESS-Keck Survey. XI. Mass Measurements for Four Transiting Sub-Neptunes Orbiting K Dwarf TOI–1246
Authors: Emma V. Turtelboom, Lauren M. Weiss, Courtney D. Dressing, Grzegorz Nowak, Enric Pallé, Corey Beard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Zachary R. Claytor, Fei Dai, Paul A. Dalba, Steven Giacalone, Erica Gonzales, Caleb K. Harada, Michelle L. Hill, Rae Holcomb, Judith Korth, Jack Lubin, Thomas Masseron, Mason MacDougall, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Ryan A. Rubenzahl, Nicholas Scarsdale, Keivan G. Stassun, Dakotah B. Tyler, Judah Van Zandt, Ian J. M. Crossfield, Hans J. Deeg, Benjamin Fulton, Davide Gandolfi, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Kristine W. F. Lam, Rafael Luque, Eduardo L. Martín, Giuseppe Morello, Jaume Orell-Miquel, Erik A. Petigura, Paul Robertson, Arpita Roy, Vincent Van Eylen, David Baker, Alexander A. Belinski, Allyson Bieryla, David R. Ciardi, Karen A. Collins, Neil Cutting, Devin J. Della-Rose, Taylor B. Ellingsen, E. Furlan, Tianjun Gan, Crystal L. Gnilka, Pere Guerra, Steve B. Howell, Mary Jimenez, David W. Latham, Maude Larivière, Kathryn V. Lester, Jorge Lillo-Box, Lindy Luker, Christopher R. Mann, Peter P. Plavchan, Boris Safonov, Brett Skinner, Ivan A. Strakhov, Justin M. Wittrock, Douglas A. Caldwell, Zahra Essack, Jon M. Jenkins, Elisa V. Quintana, George R. Ricker, Roland Vanderspek, S. Seager, Joshua N. Winn
Figure caption: TESS light curves phased at the orbital periods of the four transiting planets. Gray data are individual data points, black data points are binned data, and the overlaid curves are our best-fit GP and TTV model (TOI-1246 b: purple, TOI-1246c: blue, TOI-1246 d: light blue, TOI-1246 e: pink). Residuals are shown beneath each plot.
Paper: The TESS-Keck Survey. XI. Mass Measurements for Four Transiting Sub-Neptunes Orbiting K Dwarf TOI–1246
Authors: Emma V. Turtelboom, Lauren M. Weiss, Courtney D. Dressing, Grzegorz Nowak, Enric Pallé, Corey Beard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Zachary R. Claytor, Fei Dai, Paul A. Dalba, Steven Giacalone, Erica Gonzales, Caleb K. Harada, Michelle L. Hill, Rae Holcomb, Judith Korth, Jack Lubin, Thomas Masseron, Mason MacDougall, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Ryan A. Rubenzahl, Nicholas Scarsdale, Keivan G. Stassun, Dakotah B. Tyler, Judah Van Zandt, Ian J. M. Crossfield, Hans J. Deeg, Benjamin Fulton, Davide Gandolfi, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Kristine W. F. Lam, Rafael Luque, Eduardo L. Martín, Giuseppe Morello, Jaume Orell-Miquel, Erik A. Petigura, Paul Robertson, Arpita Roy, Vincent Van Eylen, David Baker, Alexander A. Belinski, Allyson Bieryla, David R. Ciardi, Karen A. Collins, Neil Cutting, Devin J. Della-Rose, Taylor B. Ellingsen, E. Furlan, Tianjun Gan, Crystal L. Gnilka, Pere Guerra, Steve B. Howell, Mary Jimenez, David W. Latham, Maude Larivière, Kathryn V. Lester, Jorge Lillo-Box, Lindy Luker, Christopher R. Mann, Peter P. Plavchan, Boris Safonov, Brett Skinner, Ivan A. Strakhov, Justin M. Wittrock, Douglas A. Caldwell, Zahra Essack, Jon M. Jenkins, Elisa V. Quintana, George R. Ricker, Roland Vanderspek, S. Seager, Joshua N. Winn
Figure caption: Observed—Computed plots for TOI-1246 d (left) and TOI-1246 e (right). The shaded area of each bar represents the one- and three-sigma standard deviations of each TTV measurement. Both planets show strong evidence of TTVs. Transit number 2 of TOI-1246 e was not fully observed by TESS, leading to a larger error bar on the TTV measurement.
Paper: The TESS-Keck Survey. XI. Mass Measurements for Four Transiting Sub-Neptunes Orbiting K Dwarf TOI–1246
Authors: Emma V. Turtelboom, Lauren M. Weiss, Courtney D. Dressing, Grzegorz Nowak, Enric Pallé, Corey Beard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Zachary R. Claytor, Fei Dai, Paul A. Dalba, Steven Giacalone, Erica Gonzales, Caleb K. Harada, Michelle L. Hill, Rae Holcomb, Judith Korth, Jack Lubin, Thomas Masseron, Mason MacDougall, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Ryan A. Rubenzahl, Nicholas Scarsdale, Keivan G. Stassun, Dakotah B. Tyler, Judah Van Zandt, Ian J. M. Crossfield, Hans J. Deeg, Benjamin Fulton, Davide Gandolfi, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Kristine W. F. Lam, Rafael Luque, Eduardo L. Martín, Giuseppe Morello, Jaume Orell-Miquel, Erik A. Petigura, Paul Robertson, Arpita Roy, Vincent Van Eylen, David Baker, Alexander A. Belinski, Allyson Bieryla, David R. Ciardi, Karen A. Collins, Neil Cutting, Devin J. Della-Rose, Taylor B. Ellingsen, E. Furlan, Tianjun Gan, Crystal L. Gnilka, Pere Guerra, Steve B. Howell, Mary Jimenez, David W. Latham, Maude Larivière, Kathryn V. Lester, Jorge Lillo-Box, Lindy Luker, Christopher R. Mann, Peter P. Plavchan, Boris Safonov, Brett Skinner, Ivan A. Strakhov, Justin M. Wittrock, Douglas A. Caldwell, Zahra Essack, Jon M. Jenkins, Elisa V. Quintana, George R. Ricker, Roland Vanderspek, S. Seager, Joshua N. Winn
Figure caption: Sector 14 TESS Target Pixel File for TOI-1246 with the SPOC pipeline aperture overlaid in red. TOI-1246 is indicated with a white cross and labeled as target 1. The Gaia DR2 sources in the field are shown by red dots, scaled in size to the difference in magnitude with TOI-1246. The TESS pixel scale is 21 arcsecpixel−1.
Paper: The TESS-Keck Survey. XI. Mass Measurements for Four Transiting Sub-Neptunes Orbiting K Dwarf TOI–1246
Authors: Emma V. Turtelboom, Lauren M. Weiss, Courtney D. Dressing, Grzegorz Nowak, Enric Pallé, Corey Beard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Zachary R. Claytor, Fei Dai, Paul A. Dalba, Steven Giacalone, Erica Gonzales, Caleb K. Harada, Michelle L. Hill, Rae Holcomb, Judith Korth, Jack Lubin, Thomas Masseron, Mason MacDougall, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Ryan A. Rubenzahl, Nicholas Scarsdale, Keivan G. Stassun, Dakotah B. Tyler, Judah Van Zandt, Ian J. M. Crossfield, Hans J. Deeg, Benjamin Fulton, Davide Gandolfi, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Kristine W. F. Lam, Rafael Luque, Eduardo L. Martín, Giuseppe Morello, Jaume Orell-Miquel, Erik A. Petigura, Paul Robertson, Arpita Roy, Vincent Van Eylen, David Baker, Alexander A. Belinski, Allyson Bieryla, David R. Ciardi, Karen A. Collins, Neil Cutting, Devin J. Della-Rose, Taylor B. Ellingsen, E. Furlan, Tianjun Gan, Crystal L. Gnilka, Pere Guerra, Steve B. Howell, Mary Jimenez, David W. Latham, Maude Larivière, Kathryn V. Lester, Jorge Lillo-Box, Lindy Luker, Christopher R. Mann, Peter P. Plavchan, Boris Safonov, Brett Skinner, Ivan A. Strakhov, Justin M. Wittrock, Douglas A. Caldwell, Zahra Essack, Jon M. Jenkins, Elisa V. Quintana, George R. Ricker, Roland Vanderspek, S. Seager, Joshua N. Winn
Figure caption: Top: sensitivity curve and zoomed-in image in K band of TOI-1246 using Keck/NIRC2. Bottom: AO image of TOI-1246 using Keck/NIRC2. We see a companion at ∼ 4″ to the NE of TOI-1246, which does not significantly affect our analysis.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: Violin plots showing the Gaussian KDE for three different versions of the r-band magnitude difference. (Left) Magnitude difference between the brightest and second-brightest group galaxies, (middle) the difference between the brightest and third-brightest group galaxies, (right) and the difference the between the brightest and fourth-brightest group galaxies. For all three metrics, the unbent sample sits at a higher magnitude difference.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: A cumulative histogram of photometric uncertainties from DECaLS. The red line is drawn at an uncertainty of 0.04, which is the redshift uncertainty cutoff for the FoF algorithm. This winds up including 70% of the galaxies in DECaLS, with the rest falling above that cutoff.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: Density measures for groups hosting bent (purple) and unbent (red) radio galaxies. (Top) The group density, measured within 0.5 Mpc of the group center. (Bottom) The environmental density, measured from 0.5 Mpc to 2 Mpc of the group center.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: Normalized distributions of the number of galaxies occupying the same groups as bent and unbent radio galaxies. This distribution only includes groups with at least three members and excludes all groups with more than 100 members. This results in us excluding seven groups hosting bent doubles and two groups hosting unbent doubles.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: A normalized histogram of distance to nearest neighbors using the results of the FoF algorithm on the DECaLS data.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: Comparison of the radii of groups hosting bent and unbent radio AGN.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: The difference between the photometric redshift measured by Zou et al. (2019) and the spectroscopic redshift measured by SDSS as a function of the spectroscopic redshift.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: A color–mass plot using k-corrected absolute magnitudes from DECaLS of unbent and bent doubles, along with galaxies identified as group members.
Paper: Earth as a Proxy Exoplanet: Simulating DSCOVR/EPIC Observations Using the Earth Spectrum Simulator
Authors: Lixiang Gu, Zhao-Cheng Zeng, Siteng Fan, Vijay Natraj, Jonathan H. Jiang, David Crisp, Yuk L. Yung, Yongyun Hu
Figure caption: (a) Land reflectance map, calculated using the Ross–Thick–Li–Sparse model (Roujean et al. 1992). (b) Ocean reflectance map, calculated using the Cox–Munk model (Cox & Munk 1954). (c) Surface pressure map. (d) Column integrated ozone map. (e) Total aerosol optical depth map. (f) Total cloud optical depth. (g) Laboratory reflectance data for seven surface types. Snow (300 ∼ 340 nm) and wetland (300 ∼ 400 nm) reflectance are partly extrapolated in the UV channels, using the nearest available value. Wetland, shrub, snow, lichen, and grass data are taken from the USGS Spectral Library (Kokaly et al. 2017). Desert and tree data are from the RELAB spectral database (Pieters & Hiroi 2004). (h) Fixed vertical profiles used for water vapor, oxygen, and temperature. All maps are for the 551 nm channel and have the same viewing geometry of EPIC at 9:08 UTC, 2016 April 5.
Paper: Earth as a Proxy Exoplanet: Simulating DSCOVR/EPIC Observations Using the Earth Spectrum Simulator
Authors: Lixiang Gu, Zhao-Cheng Zeng, Siteng Fan, Vijay Natraj, Jonathan H. Jiang, David Crisp, Yuk L. Yung, Yongyun Hu
Figure caption: Correlation between simulated and observed disk-integrated reflectance deviations. The x- and y-axis values correspond to the observations and simulations, respectively, which are also the red and blue lines in Figure 5, respectively. The gray line denotes a 1:1 correspondence.
Paper: Earth as a Proxy Exoplanet: Simulating DSCOVR/EPIC Observations Using the Earth Spectrum Simulator
Authors: Lixiang Gu, Zhao-Cheng Zeng, Siteng Fan, Vijay Natraj, Jonathan H. Jiang, David Crisp, Yuk L. Yung, Yongyun Hu
Figure caption: Time-averaged Earth spectrum. The red and blue lines represent the observed and simulated results, respectively. The shaded area denotes the standard deviation in each channel.
Paper: Earth as a Proxy Exoplanet: Simulating DSCOVR/EPIC Observations Using the Earth Spectrum Simulator
Authors: Lixiang Gu, Zhao-Cheng Zeng, Siteng Fan, Vijay Natraj, Jonathan H. Jiang, David Crisp, Yuk L. Yung, Yongyun Hu
Figure caption: EPIC (a) observed and (b) synthetic reflectance images in 10 channels at 9:08 UTC, 2016 April 5.
Paper: Earth as a Proxy Exoplanet: Simulating DSCOVR/EPIC Observations Using the Earth Spectrum Simulator
Authors: Lixiang Gu, Zhao-Cheng Zeng, Siteng Fan, Vijay Natraj, Jonathan H. Jiang, David Crisp, Yuk L. Yung, Yongyun Hu
Figure caption: (a) Singular values for the full observation (black; ∼5000 time points; normalized by a factor of 0.26), subsampled observation (red; ∼300 time points, same as the number of simulation time points), and simulated (blue) light curves. (b) Eigenvectors (spectra) of the first six PCs of the full observation (black), subsampled observation (red), and simulated (blue) light curves. The text in each panel denotes the PC index for the three sets of data. PC3 and PC4 are switched between the simulations and observations for a clearer comparison.
Paper: Earth as a Proxy Exoplanet: Simulating DSCOVR/EPIC Observations Using the Earth Spectrum Simulator
Authors: Lixiang Gu, Zhao-Cheng Zeng, Siteng Fan, Vijay Natraj, Jonathan H. Jiang, David Crisp, Yuk L. Yung, Yongyun Hu
Figure caption: Histograms of liquid cloud-covered pixel reflectance for observation (red) and simulation (blue) for the 10 EPIC channels.
Paper: Earth as a Proxy Exoplanet: Simulating DSCOVR/EPIC Observations Using the Earth Spectrum Simulator
Authors: Lixiang Gu, Zhao-Cheng Zeng, Siteng Fan, Vijay Natraj, Jonathan H. Jiang, David Crisp, Yuk L. Yung, Yongyun Hu
Figure caption: Same as Figure 8, but for ice cloud-covered pixels.
Paper: Earth as a Proxy Exoplanet: Simulating DSCOVR/EPIC Observations Using the Earth Spectrum Simulator
Authors: Lixiang Gu, Zhao-Cheng Zeng, Siteng Fan, Vijay Natraj, Jonathan H. Jiang, David Crisp, Yuk L. Yung, Yongyun Hu
Figure caption: Time series of disk-integrated reflectance deviation from the time average. Red and blue lines denote observed and simulated results, respectively.
Paper: Earth as a Proxy Exoplanet: Simulating DSCOVR/EPIC Observations Using the Earth Spectrum Simulator
Authors: Lixiang Gu, Zhao-Cheng Zeng, Siteng Fan, Vijay Natraj, Jonathan H. Jiang, David Crisp, Yuk L. Yung, Yongyun Hu
Figure caption: EPIC (a) observed and (b) synthetic reflectance images in 10 channels at 14:47 UTC, 2016 August 7. The purple and blue boxes indicate examples of midlatitude front and tropical deep convective cloud, respectively.
Paper: The Perkins INfrared Exosatellite Survey (PINES) I. Survey Overview, Reduction Pipeline, and Early Results
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, David Gracia, Johanna M. Vos, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty, Christopher Theissen, Eric Agol, Julie N. Skinner, Sheila Sagear
Figure caption: Top: histogram of apparent J-band magnitudes of targets in the PINES sample. Bottom: histogram of spectral types.