adsabs/AstroCLIMB huggingface dataset:
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: The WISE color–color distributions for the Unclassified classification. These objects are characterized by low f W2/f W1 ratios, i.e., blue W1−W2 colors, and most are outside of typical mid-IR AGN selection criteria (see Table 6). Refer to Figure 1 for a description of the BPT delineations, WISE color–color selection criteria, and error bars plotted in black.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: Distributions of L AGN/L Tot for different mid-IR color selection criteria. On the left, the AGN luminosity is not corrected for extinction, while on the right, it is corrected for extinction. In the top panels, we show the count histograms, while in the bottom panels, we show the density histograms. The selection criterion presented in this work probes objects with a lower AGN contribution to the SED.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: Distributions of the probability that an AGN component results in a statistically better fit as generated with an F-Test for different mid-IR color selection criteria. In the top panel, we show the count histogram, while in the bottom panel, we show the density histogram. The selection criterion presented in this work probes objects with a lower evidence for an AGN in their SED.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VII. APOGEE DR17 [C/N]–Age Calibration
Authors: Taylor Spoo, Jamie Tayar, Peter M. Frinchaboy, Katia Cunha, Natalie Myers, John Donor, Steven R. Majewski, Dmitry Bizyaev, D. A. García-Hernández, Henrik Jönsson, Richard R. Lane, Kaike Pan, Penélope Longa-Peña, A. Roman-Lopes
Figure caption: A comparison between our DR16-based age calibration (left) and DR17-based age calibration (right) to asteroseismically determined ages from the APOKASC catalog (Pinsonneault et al. 2018). The gray-gradient shaded regions represent bins of field stars. The green circles, blue triangles, and red diamonds represent cluster member stars common to both samples for NGC 6791, NGC 6819, and NGC 6811, respectively. The horizontal dashed lines are the ages determined by Cantat-Gaudin et al. (2020) for each cluster. The diagonal dashed gray line represents the one-to-one relationship. The solid black line is the linear fit to the main trend of the field stars. Mean representative error bars are shown in each panel.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: We consider regions of mass-separation parameter space in which a companion to Kepler-1656b can reside. Regions ruled out by Gaia (blue), AO (tan), and Speckle imaging (red) are shown. The explored region encapsulating Kepler-1656c is outlined, and both Kepler-1656b and Kepler-1656c are overplotted for reference.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Top: change in Bayesian Information Criterion (BIC) comparing two-planet models and single-planet models. The trial period of the two-planet model is shown on the horizontal axis. The BIC favors P c ∼ 1920 days, corresponding to a second planet in the system. The BIC associated with eFAP = 0.001, above which peaks are considered true planets, is overplotted in red. Bottom: the same as the top panel, but comparing three-planet models to two-planet models. No peaks lie above the eFAP = 0.001 threshold, indicating no additional periodic signals are detected.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VII. APOGEE DR17 [C/N]–Age Calibration
Authors: Taylor Spoo, Jamie Tayar, Peter M. Frinchaboy, Katia Cunha, Natalie Myers, John Donor, Steven R. Majewski, Dmitry Bizyaev, D. A. García-Hernández, Henrik Jönsson, Richard R. Lane, Kaike Pan, Penélope Longa-Peña, A. Roman-Lopes
Figure caption: (left) [C/N] abundances vs. log(Age[yr]) for our cluster sample using only RGB stars from 46 clusters common to the OCCAM Survey and the Cantat-Gaudin data set. (right) The [C/N] abundance vs. ﹩\mathrm{log}(\mathrm{Age}[\mathrm{yr}])﹩ for clusters containing only RC stars in common between the OCCAM Survey and Cantat-Gaudin data set, which includes 21 clusters. Labels and calculation of calibrations are similar to Figure 3.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Left: residual RV time series of Kepler-1656 shows a long-term trend with P ≫ 100 days. Right: residual RVs are plotted vs. S HK. A Pearson r statistic of 0.51 and median activity signal of S HK = 0.15 indicate that stellar activity is not sufficient at explaining the variability in our RV time series.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Adopted a two-planet Keplerian model for the Kepler-1656 system. (a) Black points are RVs and the blue line shows our maximum a posteriori model. (b) Model residuals are shown in black. (c) Observations are phase-folded over the inner planet period and the phase-folded Keplerian model is overplotted. RVs binned in 0.08 units of orbital phase are shown in red. (d) Observations are phase-folded over the outer planet period, phase-folded Keplerian model is overplotted.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Schematic of a hierarchical triple system containing Kepler-1656b (M b) on a tight inner orbit and a companion (M c) on a distant, possibly inclined outer orbit around their host star (M ⋆). Note that the sizes of the planets and their orbits are not drawn to scale.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VII. APOGEE DR17 [C/N]–Age Calibration
Authors: Taylor Spoo, Jamie Tayar, Peter M. Frinchaboy, Katia Cunha, Natalie Myers, John Donor, Steven R. Majewski, Dmitry Bizyaev, D. A. García-Hernández, Henrik Jönsson, Richard R. Lane, Kaike Pan, Penélope Longa-Peña, A. Roman-Lopes
Figure caption: Median [C/N] ratio of open cluster star members, as derived in DR14 (green circles) and DR17 (purple squares), vs. ﹩\mathrm{log}(\mathrm{Ages}[\mathrm{yr}﹩]), where these ages are provided by Cantat-Gaudin et al. (2020). The green dotted–dashed line and purple dashed line represent the linear fit for DR14 and DR17, respectively. The plot shows a systematic shift from DR14 data to DR17 data.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: H-R diagram comparing the 58 M-dwarf TOIs in our sample (the larger, outlined circles) to the full sample of TOIs listed in the ExoFOP TOI table. This plot uses stellar temperature and distance values obtained from the ExoFOP TOI table, and we calculated absolute magnitude values using the stellar temperature and radius values listed in this table. The color of each point corresponds to the distance. The black line represents the temperature cutoff for our sample (Teff < 4000 K). Discussion of the three M-dwarf TOIs that are elevated above the Main Sequence occurs in Section 3.5.
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: (a) Time-domain scatter as a function of TESS magnitude for stars observed in 20 second cadence between Sectors 27 and 36. Symbols show 20 second light curves binned to 2 minute cadence (cyan circles) and original 2 minute light curves (red diamonds) for each sector. Gray points mark stars likely dominated by stellar variability (see text). (b) Same as panel (a) but binning light curves to 1 hr cadence. (c) Ratio of the time-domain scatter for the two data sets shown in panel (a), retaining only stars not dominated by stellar variability (i.e., each point in panel (c) is the ratio of a cyan circle and red diamond in panel (a)). The dashed line marks unity and orange circles show median bins. (d) Same as panel (c) but for the binned light curves shown in panel (b).
Paper: The TESS-Keck Survey. VIII. Confirmation of a Transiting Giant Planet on an Eccentric 261 Day Orbit with the Automated Planet Finder Telescope 
Authors: Paul A. Dalba, Stephen R. Kane, Diana Dragomir, Steven Villanueva, Karen A. Collins, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Benjamin Fulton, Howard Isaacson, Judah Van Zandt, Andrew W. Howard, Daniel P. Thorngren, Steve B. Howell, Natalie M. Batalha, Ashley Chontos, Ian J. M. Crossfield, Courtney D. Dressing, Daniel Huber, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Casey L. Brinkman, Steven Giacalone, Michelle L. Hill, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Paul Benni, Pat Boyce, Thomas M. Esposito, E. Girardin, Didier Laloum, Pablo Lewin, Christopher R. Mann, Franck Marchis, Richard P. Schwarz, Gregor Srdoc, Jana Steuer, Thirupathi Sivarani, Athira Unni, Nora L. Eisner, Tara Fetherolf, Zhexing Li, Xinyu Yao, Joshua Pepper, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Christopher J. Burke, Jason D. Eastman, Michael B. Lund, David R. Rodriguez, Pamela Rowden, Eric B. Ting, Jesus Noel Villaseñor
Figure caption: All ground-based data acquired in the transit ephemeris refinement effort for TOI-2180 b. These data have not been detrended against airmass variations. The transit model is shown in panel (a) for comparison only (i.e., we are not suggesting that occurred at that time). The light and dark shaded regions denote the 2σ and 1σ transit windows, respectively, calculated from the final ephemeris in Table 3. Data sets plotted with a color were used to refine the orbital period of TOI-2180 b, whereas those in gray are shown only for completeness. These data are summarized in Table 4 and will be made available upon request.
Paper: The TESS-Keck Survey. VIII. Confirmation of a Transiting Giant Planet on an Eccentric 261 Day Orbit with the Automated Planet Finder Telescope 
Authors: Paul A. Dalba, Stephen R. Kane, Diana Dragomir, Steven Villanueva, Karen A. Collins, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Benjamin Fulton, Howard Isaacson, Judah Van Zandt, Andrew W. Howard, Daniel P. Thorngren, Steve B. Howell, Natalie M. Batalha, Ashley Chontos, Ian J. M. Crossfield, Courtney D. Dressing, Daniel Huber, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Casey L. Brinkman, Steven Giacalone, Michelle L. Hill, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Paul Benni, Pat Boyce, Thomas M. Esposito, E. Girardin, Didier Laloum, Pablo Lewin, Christopher R. Mann, Franck Marchis, Richard P. Schwarz, Gregor Srdoc, Jana Steuer, Thirupathi Sivarani, Athira Unni, Nora L. Eisner, Tara Fetherolf, Zhexing Li, Xinyu Yao, Joshua Pepper, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Christopher J. Burke, Jason D. Eastman, Michael B. Lund, David R. Rodriguez, Pamela Rowden, Eric B. Ting, Jesus Noel Villaseñor
Figure caption: Giant planet mass–metallicity correlation shown with the Thorngren et al. (2016) sample (circles), TOI-2180 b (square), and two recently published Kepler long-period giant planets (triangles): Kepler-1514 b (P ≈ 218 days) and Kepler-1704 b (P ≈ 989 days). Blue and red indicate orbital periods below and above 100 days, respectively. The dashed lines and shaded 1σ regions indicate separate regressions to these two sets of planets. The slopes of these fits are discrepant to 2.6σ, hinting that the mass–metallicity correlation for giant planets may be dependent upon orbital properties.
Paper: The TESS-Keck Survey. VIII. Confirmation of a Transiting Giant Planet on an Eccentric 261 Day Orbit with the Automated Planet Finder Telescope 
Authors: Paul A. Dalba, Stephen R. Kane, Diana Dragomir, Steven Villanueva, Karen A. Collins, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Benjamin Fulton, Howard Isaacson, Judah Van Zandt, Andrew W. Howard, Daniel P. Thorngren, Steve B. Howell, Natalie M. Batalha, Ashley Chontos, Ian J. M. Crossfield, Courtney D. Dressing, Daniel Huber, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Casey L. Brinkman, Steven Giacalone, Michelle L. Hill, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Paul Benni, Pat Boyce, Thomas M. Esposito, E. Girardin, Didier Laloum, Pablo Lewin, Christopher R. Mann, Franck Marchis, Richard P. Schwarz, Gregor Srdoc, Jana Steuer, Thirupathi Sivarani, Athira Unni, Nora L. Eisner, Tara Fetherolf, Zhexing Li, Xinyu Yao, Joshua Pepper, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Christopher J. Burke, Jason D. Eastman, Michael B. Lund, David R. Rodriguez, Pamela Rowden, Eric B. Ting, Jesus Noel Villaseñor
Figure caption: Subset of long-period (P > 20 days) giant (M  P  > 0.2 M J) exoplanets with measured mass and radii sized to show their hosts’ V-band magnitudes. Object TOI-2180 b is labeled and drawn with a dashed line. Of the four planets with the brightest host stars, TOI-2180 b has the longest period by far, demonstrating how it is a valuable extension of the parameter space of temperate Jupiters.
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: (a) Stellar radius versus effective temperature of the ≈4900 unique stars with T eff < 8000 K observed with TESS 20 second cadence observations during the first 10 sectors of the extended mission, color-coded by TESS magnitude T (capped at T < 16 mag). (b) Stellar radius versus TESS magnitude for the sample shown in panel (a). Compact stars (such as hot subdwarfs and white dwarfs) are excluded from both panels.
Paper: The TESS-Keck Survey. VIII. Confirmation of a Transiting Giant Planet on an Eccentric 261 Day Orbit with the Automated Planet Finder Telescope 
Authors: Paul A. Dalba, Stephen R. Kane, Diana Dragomir, Steven Villanueva, Karen A. Collins, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Benjamin Fulton, Howard Isaacson, Judah Van Zandt, Andrew W. Howard, Daniel P. Thorngren, Steve B. Howell, Natalie M. Batalha, Ashley Chontos, Ian J. M. Crossfield, Courtney D. Dressing, Daniel Huber, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Casey L. Brinkman, Steven Giacalone, Michelle L. Hill, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Paul Benni, Pat Boyce, Thomas M. Esposito, E. Girardin, Didier Laloum, Pablo Lewin, Christopher R. Mann, Franck Marchis, Richard P. Schwarz, Gregor Srdoc, Jana Steuer, Thirupathi Sivarani, Athira Unni, Nora L. Eisner, Tara Fetherolf, Zhexing Li, Xinyu Yao, Joshua Pepper, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Christopher J. Burke, Jason D. Eastman, Michael B. Lund, David R. Rodriguez, Pamela Rowden, Eric B. Ting, Jesus Noel Villaseñor
Figure caption: Set of (a, M  P ) models consistent with the measured RV trend and curvature at the 1σ (dark) and 2σ (light) levels. We rule out semimajor axes corresponding to orbital periods shorter than the observing baseline, as well as companion masses too low to produce the minimum RV amplitude.
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Ratio of the time-domain scatter for 20 second cadence data binned to 2 minute cadence and original 2 minute cadence light curves as a function of TESS magnitude for the first orbit (orange circles) and second orbit (blue triangles) of Sector 34 to test the impact of pointing jitter on the relative precision of the two light-curve products (see text). Filled symbols show median bins in steps of 1 mag. The dashed line marks unity.
Paper: Search for Intermediate-mass Black Holes at Low Redshift with Intra-night Variability
Authors: Lael Shin, Jong-Hak Woo, Donghoon Son, Hojin Cho, Taewoo Kim, Elena Gallo, Wonseok Kang
Figure caption: Spectral decomposition of the 24 broad Hα candidates whose estimated M BH is smaller than 106 M ⊙. The first and third columns show the best-fit model with an Hα broad component for each emission line region. The second and forth columns show the best-fit model without an Hα broad component. The stellar continuum subtracted spectrum is plotted in black, and the blue line shows the best-fit model composed of narrow Gaussian components (magenta) and an Hα broad component (red). At the bottom of each panel, the residuals between the spectrum and the best-fit model are plotted in black.
Paper: Search for Intermediate-mass Black Holes at Low Redshift with Intra-night Variability
Authors: Lael Shin, Jong-Hak Woo, Donghoon Son, Hojin Cho, Taewoo Kim, Elena Gallo, Wonseok Kang
Figure caption: The correlations of RMSHα  with M BH, L Hα , and σ Hα . The 11 candidates having a large variability amplitude selected in Section 4.1 are plotted in orange, and the other candidates with weak variability are plotted in blue. A typical error is shown in the upper right corner. The solid lines show the best linear fit for the 11 variable candidates.
Paper: Search for Intermediate-mass Black Holes at Low Redshift with Intra-night Variability
Authors: Lael Shin, Jong-Hak Woo, Donghoon Son, Hojin Cho, Taewoo Kim, Elena Gallo, Wonseok Kang
Figure caption: Continuum (blue) and Hα (red) light curves of the 20 candidates. The total error (thin line) is composed of the measurement error (thick line) and the systematic error from differential photometry. Note that for the Hα light curves, we only present the photometry results from narrowband filters. The ID assigned in this work is shown in the upper left corner of the panel.
Paper: Search for Intermediate-mass Black Holes at Low Redshift with Intra-night Variability
Authors: Lael Shin, Jong-Hak Woo, Donghoon Son, Hojin Cho, Taewoo Kim, Elena Gallo, Wonseok Kang
Figure caption: Images of the 20 candidates observed with the Hα focused filter (see Table 2). North is up and the east is to the left. The 5″, 10″, and 15″ apertures are denoted with cyan circles. The ID assigned in this study is shown in the upper left corner of each panel.
Paper: Searching for Diamagnetic Blob Accretion in the 74 day K2 Observation of V2400 Ophiuchi
Authors: Andrew Langford, Colin Littlefield, Peter Garnavich, Mark R. Kennedy, Simone Scaringi, Paula Szkody
Figure caption: The Lomb–Scargle periodogram of the entire K2 V2400 Oph data set. The notable frequencies, (ω − Ω), (ω), and 2(ω − Ω), 3(ω − Ω), are identifiable within the power spectrum. The long duration of the K2 light curve allows for precise measurements of the notable frequencies. Low-frequency quasiperiodic oscillations (QPOs) are identified between 2 and 9 cycles d−1.
Paper: ExoVista: A Suite of Planetary System Models for Exoplanet Studies
Authors: Christopher C. Stark
Figure caption: Example astrometric position extracted from a planetary system model generated by exoVista. The gravitational influence of companions stars and photometric asymmetries within the system are not included.