adsabs/AstroCLIMB huggingface dataset:
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption: Example output of NGC 7682 from the isophotal ellipse modeling. The x-axis gives the semimajor axis of the isophotal ellipse in arcseconds, while the y-axis shows the model ellipticity, major axis position angle in degrees, and surface brightness in log counts.
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption: The total system throughput for the HST WFC3 direct imaging filters (F502N, FQ508N, and F547M), including the quantum efficiency of the CCD detectors. The gray shaded region shows the centroid of the [O III] λ5007 emission line for z = 0–0.02.
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption: Example HST STIS archival spectra of NGC 7682, showing the prominent emission lines useful for AGN analysis. The top spectrum shows the G430L filter and the bottom shows the G750M filter. Each plot is a summation of 20 bins along the slit (about 1″) centered on the AGN nucleus.
Paper: On the Physical Nature of Lyα Transmission Spikes in High-redshift Quasar Spectra
Authors: Hanjue Zhu, 涵珏 朱, Nickolay Y. Gnedin, Camille Avestruz
Figure caption: EBM model performance, measured using the 1 − r 2 “missing-variance” metric, as a function of redshift for models trained with different input combinations. Each panel corresponds to a different reionization history. As a baseline, with H I number density (n H I ) and temperature (T) as inputs, the model predictions are highly accurate. Then n H I  is replaced by combinations of baryon number density (n  b ) with ionization parameters, ﹩{{ \mathcal F }}_{\nu }﹩ (representing the cosmic background) and ﹩{{ \mathcal G }}_{\nu }﹩ (representing the local ionizing sources). The results indicate that ﹩{{ \mathcal F }}_{\nu }﹩ is the predominant component of ionizing radiation.
Paper: On the Physical Nature of Lyα Transmission Spikes in High-redshift Quasar Spectra
Authors: Hanjue Zhu, 涵珏 朱, Nickolay Y. Gnedin, Camille Avestruz
Figure caption: Normalized average contributions (scaled to sum to one) of IGM properties to Lyα flux prediction. Each panel corresponds to a different reionization history. In intermediate and early reionization scenarios, the contribution of n  b  decreases with increasing redshift, while the impact of ﹩{{ \mathcal G }}_{\nu }﹩ grows, aligning with the expected greater influence of local ionization at higher redshifts. A similar, yet nonmonotonic trend is observed in the late reionization scenario, indicative of a universe still undergoing rapid reionization.
Paper: On the Physical Nature of Lyα Transmission Spikes in High-redshift Quasar Spectra
Authors: Hanjue Zhu, 涵珏 朱, Nickolay Y. Gnedin, Camille Avestruz
Figure caption: Distribution of mean opacities in 50 h −1 cMpc LOSs for the combination of the three CROC simulations (thick dashed lines). Thin solid lines and bands show the observational data from G. D. Becker et al. (2015) and S. E. I. Bosman et al. (2018). The three CROC simulations together marginally match the distribution of opacities (at least at z > 5.5).
Paper: On the Physical Nature of Lyα Transmission Spikes in High-redshift Quasar Spectra
Authors: Hanjue Zhu, 涵珏 朱, Nickolay Y. Gnedin, Camille Avestruz
Figure caption: An example of nonequilibrium effects along a random LOS. Top: n H I , ﹩{n}_{{\rm{H}}\,{\rm{I}}}^{\mathrm{eq}}﹩ calculated assuming ionization equilibrium and rescaled n  b  as a function of LOS position. Bottom: ratio of n H I  and ﹩{n}_{{\rm{H}}\,{\rm{I}}}^{\mathrm{eq}}﹩ as a function of LOS position. A noticeable deviation from equilibrium coincides with a drop in n  b , suggesting the presence of a shock at this location.
Paper: On the Physical Nature of Lyα Transmission Spikes in High-redshift Quasar Spectra
Authors: Hanjue Zhu, 涵珏 朱, Nickolay Y. Gnedin, Camille Avestruz
Figure caption: Normalized average transmitted flux as a function of distance from galaxies. We show measurements using both the simulated spectra and spectra generated, assuming a spatially uniform photoionization rate (Γ). Points with error bars reference measurements from R. A. Meyer et al. (2019); brighter blue points show the original measurement and lighter blue points show the measurement with the rescaled mean flux (see the text for details). The observed flux suppression at small distances in both data sets suggests that galaxies are not the primary cause since galaxies influence IGM properties through Γ.
Paper: Regulation of Solar Wind Electron Temperature Anisotropy by Collisions and Instabilities
Authors: Peter H. Yoon, Chadi S. Salem, Kristopher G. Klein, Mihailo M. Martinović, Rodrigo A. López, Jungjoon Seough, Muhammad Sarfraz, Marian Lazar, Shaaban M. Shaaban
Figure caption: Examples of exact vs. approximate dispersion relations. (Top) Real frequency and growth rate for EMEC instability (case 21). Solid curves are exact numerical solutions based upon Equation (B1), while the dashed curves are approximate solutions, Equation (B2), except that γ is multiplied with f scale = 0.625. (Bottom) Real frequency and growth rate for EFH instability (case 71). Solid curves are exact numerical solutions based upon Equation (B1), while the dashed curves are approximate solutions based on Equation (B4), except that γ is multiplied with f scale = 0.95.
Paper: Regulation of Solar Wind Electron Temperature Anisotropy by Collisions and Instabilities
Authors: Peter H. Yoon, Chadi S. Salem, Kristopher G. Klein, Mihailo M. Martinović, Rodrigo A. López, Jungjoon Seough, Muhammad Sarfraz, Marian Lazar, Shaaban M. Shaaban
Figure caption: Combined results of combined dynamical ensemble calculation where the final states, plotted with black dots, are displayed against the backdrop of 2D solar wind electron frequency distribution. The final states are the same as those shown in Figures 2 and 4.
Paper: On the Physical Nature of Lyα Transmission Spikes in High-redshift Quasar Spectra
Authors: Hanjue Zhu, 涵珏 朱, Nickolay Y. Gnedin, Camille Avestruz
Figure caption:  n H I , sampled along LOSs vs. ﹩{n}_{{\rm{H}}\,{\rm{I}}}^{\mathrm{eq}}﹩, calculated with Equation (8) assuming ionization equilibrium at z = 5.25. Colors show the number counts in each hexbin. We observe significant deviations of many data points from the equilibrium line.
Paper: Solar Vortex Tubes. III. Vorticity and Energy Transport
Authors: Suzana S. A. Silva, Gary Verth, Istvan Ballai, Erico L. Rempel, Sergiy Shelyag, Luiz A. C. A. Schiavo, Tiago F. P. Gomes, Viktor Fedun
Figure caption: Close view of vortices: #7 (a), (d), (g),#8 (b), (e), (h), #12 (c), (f), (i) at t = 0 s. Panels (a), (b), and (c): The vortex tube is crossed by x–y planes colored by the temperature, and the black arrows provide the orientation of the horizontal component of the Lorentz force. The velocity field direction is indicated by the LIC, and the white contour depicts the vortex boundary at each height level. Panels (a)–(c): x–y plane placed at z = 1.1 Mm (d)–(f); z = 1.3 Mm (g)–(i); and z = 1.5 Mm (j)–(l).
Paper: Solar Vortex Tubes. III. Vorticity and Energy Transport
Authors: Suzana S. A. Silva, Gary Verth, Istvan Ballai, Erico L. Rempel, Sergiy Shelyag, Luiz A. C. A. Schiavo, Tiago F. P. Gomes, Viktor Fedun
Figure caption: The angular averages of kinetic ﹩\left\langle {E}_{k}\right\rangle ﹩, magnetic ﹩\left\langle {E}_{m}\right\rangle ﹩, internal ﹩\left\langle {E}_{i}\right\rangle ﹩ energies, and ratios of kinetic to magnetic 〈E  k /E  m 〉 energies along the vortex radius from the center, r = 0, to the boundary r = R. The radial profiles are shown for vortices #7 (a), (d), (g), #8 (b), (e), (h), and #12 (c), (f), (i) at different heights: H = 0.1 Mm (a), (b), (c); H = 0.3 Mm (d), (e), (f); H = 0.5 Mm (g), (h), (i).
Paper: Solar Vortex Tubes. III. Vorticity and Energy Transport
Authors: Suzana S. A. Silva, Gary Verth, Istvan Ballai, Erico L. Rempel, Sergiy Shelyag, Luiz A. C. A. Schiavo, Tiago F. P. Gomes, Viktor Fedun
Figure caption: Close view of vortices #7 (a), (d), (g), (j), #8 (b), (e), (h), (k), and #12 (c), (f), (i), (l) at t = 0 s. Panels (a), (b), (c): The vortex tube is crossed by x–y planes colored by the z-component of the MHD Poynting flux, S  z , and the black arrows provide the orientation of the horizontal component of the velocity field. Panels (d)–(l): x–y plane placed at z = 1.1 Mm (d)–(f); 1.3 Mm (g)–(i); and 1.5 Mm (j)–(l) colored by S  z  and the velocity field direction indicated by the LIC. The white contour indicates the vortex boundary at each height level.
Paper: Solar Vortex Tubes. III. Vorticity and Energy Transport
Authors: Suzana S. A. Silva, Gary Verth, Istvan Ballai, Erico L. Rempel, Sergiy Shelyag, Luiz A. C. A. Schiavo, Tiago F. P. Gomes, Viktor Fedun
Figure caption: The average S  zV , S  zH , and S  z  along the vortex radius from the center, r = 0, to the boundary r = R. The radial profiles are shown for vortex #7 (a), (d), (g), #8 (b), (e), (h), and #12 (c), (f), (i) at different heights: H = 0.1 Mm (a), (b), (c); H = 0.3 Mm (d), (e), (f); H = 0.5 Mm (g), (h), (i).
Paper: Solar Vortex Tubes. III. Vorticity and Energy Transport
Authors: Suzana S. A. Silva, Gary Verth, Istvan Ballai, Erico L. Rempel, Sergiy Shelyag, Luiz A. C. A. Schiavo, Tiago F. P. Gomes, Viktor Fedun
Figure caption: First panel is the same as Figure 1 in a different perspective. The second (third) panel shows the vortices immersed in the volume rendering of the normalized viscous heating (squared current density).
Paper: Asteroseismology of the Nearby K Dwarf σ Draconis Using the Keck Planet Finder and TESS
Authors: Marc Hon, Daniel Huber, Yaguang Li, Travis S. Metcalfe, Timothy R. Bedding, Joel Ong, Ashley Chontos, Ryan Rubenzahl, Samuel Halverson, Rafael A. García, Hans Kjeldsen, Dennis Stello, Daniel R. Hey, Tiago Campante, Andrew W. Howard, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley D. Baker, Jerry Edelstein, Chris Smith, Benjamin J. Fulton, Josh Walawender, Max Brodheim, Matt Brown, Dwight Chan, Fei Dai, William Deich, Colby Gottschalk, Jason Grillo, Dave Hale, Grant M. Hill, Bradford Holden, Aaron Householder, Howard Isaacson, Yuzo Ishikawa, Sharon R. Jelinsky, Marc Kassis, Stephen Kaye, Russ Laher, Kyle Lanclos, Chien-Hsiu Lee, Scott Lilley, Ben McCarney, Timothy N. Miller, Joel Payne, Erik A. Petigura, Claire Poppett, Michael Raffanti, Constance Rockosi, Dale Sanford, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Roger Smith, Jim Thorne, John Valliant, Adam Vandenberg, Shin Ywan Wang, Edward Wishnow, Truman Wold, Sherry Yeh, Ashley Baker, Sarbani Basu, Megan Bedell, Heather M. Cegla, Ian Crossfield, Courtney Dressing, Xavier Dumusque, Heather Knutson, Dimitri Mawet, John O'Meara, Guđmundur Stefánsson, Johanna Teske, Gautam Vasisht, Sharon Xuesong Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: (a, b) Location of σ Dra on asteroseismic diagrams relative to M = 0.7 − 1.0 M ⊙ models with a metallicity within 2 standard deviations of σ Dra’s [Fe/H] at Y  i  = 0.277 and α = 1.9. The grid of models is emulated using modelflows (M. Hon et al. 2024). Panel (a) shows the position of σ Dra on the δ ν 01−Δν diagram. Given σ Dra’s age of 4.54 ± 0.92 Gyr, the highlighted points in panel (b) show models with δ ν 02 within 2 standard deviations from the star’s age and Δν. The δ ν 02 interval spanned by such models is indicated by horizontal lines. This range of predicted δ ν 02 is shown in σ Dra’s observed collapsed échelle diagram in panel (c), which is annotated with mode spherical degrees. The spectrum used to construct this diagram is smoothed using a 3 μHz boxcar filter, while the collapsed échelle diagram is background subtracted and normalized by dividing by the height of the collapsed l = 0 mode profile.
Paper: Asteroseismology of the Nearby K Dwarf σ Draconis Using the Keck Planet Finder and TESS
Authors: Marc Hon, Daniel Huber, Yaguang Li, Travis S. Metcalfe, Timothy R. Bedding, Joel Ong, Ashley Chontos, Ryan Rubenzahl, Samuel Halverson, Rafael A. García, Hans Kjeldsen, Dennis Stello, Daniel R. Hey, Tiago Campante, Andrew W. Howard, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley D. Baker, Jerry Edelstein, Chris Smith, Benjamin J. Fulton, Josh Walawender, Max Brodheim, Matt Brown, Dwight Chan, Fei Dai, William Deich, Colby Gottschalk, Jason Grillo, Dave Hale, Grant M. Hill, Bradford Holden, Aaron Householder, Howard Isaacson, Yuzo Ishikawa, Sharon R. Jelinsky, Marc Kassis, Stephen Kaye, Russ Laher, Kyle Lanclos, Chien-Hsiu Lee, Scott Lilley, Ben McCarney, Timothy N. Miller, Joel Payne, Erik A. Petigura, Claire Poppett, Michael Raffanti, Constance Rockosi, Dale Sanford, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Roger Smith, Jim Thorne, John Valliant, Adam Vandenberg, Shin Ywan Wang, Edward Wishnow, Truman Wold, Sherry Yeh, Ashley Baker, Sarbani Basu, Megan Bedell, Heather M. Cegla, Ian Crossfield, Courtney Dressing, Xavier Dumusque, Heather Knutson, Dimitri Mawet, John O'Meara, Guđmundur Stefánsson, Johanna Teske, Gautam Vasisht, Sharon Xuesong Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Comparison of the amplitude of radial mode of σ Dra with those from other cool dwarfs with published measurements. Two scalings of the mode amplitudes are shown, differing in terms of the exponent (s = 0.7, dotted curve; s = 1.5, solid curve). The L/M relations are shown using a 4.57 Gyr, solar-metallicity isochrone computed with the PAdova and TRieste Stellar Evolution Code (PARSEC; A. Bressan et al. 2012). The values of ﹩\mathrm{log}{{\boldsymbol{ \mathcal R }}}_{\mathrm{HK}}^{{\prime} }﹩ for all other stars besides ϵ Ind A (E. E. Mamajek & L. A. Hillenbrand 2008) are adopted from J. Gomes da Silva et al. (2021). For T eff, values for ϵ Ind A and 70 Oph A are from A. D. Rains et al. (2020), while those for other stars are from H. Bruntt et al. (2010).
Paper: Asteroseismology of the Nearby K Dwarf σ Draconis Using the Keck Planet Finder and TESS
Authors: Marc Hon, Daniel Huber, Yaguang Li, Travis S. Metcalfe, Timothy R. Bedding, Joel Ong, Ashley Chontos, Ryan Rubenzahl, Samuel Halverson, Rafael A. García, Hans Kjeldsen, Dennis Stello, Daniel R. Hey, Tiago Campante, Andrew W. Howard, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley D. Baker, Jerry Edelstein, Chris Smith, Benjamin J. Fulton, Josh Walawender, Max Brodheim, Matt Brown, Dwight Chan, Fei Dai, William Deich, Colby Gottschalk, Jason Grillo, Dave Hale, Grant M. Hill, Bradford Holden, Aaron Householder, Howard Isaacson, Yuzo Ishikawa, Sharon R. Jelinsky, Marc Kassis, Stephen Kaye, Russ Laher, Kyle Lanclos, Chien-Hsiu Lee, Scott Lilley, Ben McCarney, Timothy N. Miller, Joel Payne, Erik A. Petigura, Claire Poppett, Michael Raffanti, Constance Rockosi, Dale Sanford, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Roger Smith, Jim Thorne, John Valliant, Adam Vandenberg, Shin Ywan Wang, Edward Wishnow, Truman Wold, Sherry Yeh, Ashley Baker, Sarbani Basu, Megan Bedell, Heather M. Cegla, Ian Crossfield, Courtney Dressing, Xavier Dumusque, Heather Knutson, Dimitri Mawet, John O'Meara, Guđmundur Stefánsson, Johanna Teske, Gautam Vasisht, Sharon Xuesong Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Age and activity of σ Dra relative to a sample of 5497 K dwarfs with subsolar metallicities from the L. Ye et al. (2024) Kepler-LAMOST catalog of FGK dwarfs with isochrone-derived ages. The dashed line represents the adopted relation ﹩\mathrm{log}{{\boldsymbol{ \mathcal R }}}_{\mathrm{HK}}^{\prime} =-0.061\mathrm{log}\tfrac{\mathrm{Age}}{\mathrm{Gyr}}-4.244﹩ that describes the age–activity relation for stars within this mass and metallicity bin. The value of ﹩\mathrm{log}{{\boldsymbol{ \mathcal R }}}_{\mathrm{HK}}^{\prime} ﹩ for σ Dra is adopted from S. Boro Saikia et al. (2018), while its age is derived from this study.
Paper: Asteroseismology of the Nearby K Dwarf σ Draconis Using the Keck Planet Finder and TESS
Authors: Marc Hon, Daniel Huber, Yaguang Li, Travis S. Metcalfe, Timothy R. Bedding, Joel Ong, Ashley Chontos, Ryan Rubenzahl, Samuel Halverson, Rafael A. García, Hans Kjeldsen, Dennis Stello, Daniel R. Hey, Tiago Campante, Andrew W. Howard, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley D. Baker, Jerry Edelstein, Chris Smith, Benjamin J. Fulton, Josh Walawender, Max Brodheim, Matt Brown, Dwight Chan, Fei Dai, William Deich, Colby Gottschalk, Jason Grillo, Dave Hale, Grant M. Hill, Bradford Holden, Aaron Householder, Howard Isaacson, Yuzo Ishikawa, Sharon R. Jelinsky, Marc Kassis, Stephen Kaye, Russ Laher, Kyle Lanclos, Chien-Hsiu Lee, Scott Lilley, Ben McCarney, Timothy N. Miller, Joel Payne, Erik A. Petigura, Claire Poppett, Michael Raffanti, Constance Rockosi, Dale Sanford, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Roger Smith, Jim Thorne, John Valliant, Adam Vandenberg, Shin Ywan Wang, Edward Wishnow, Truman Wold, Sherry Yeh, Ashley Baker, Sarbani Basu, Megan Bedell, Heather M. Cegla, Ian Crossfield, Courtney Dressing, Xavier Dumusque, Heather Knutson, Dimitri Mawet, John O'Meara, Guđmundur Stefánsson, Johanna Teske, Gautam Vasisht, Sharon Xuesong Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Mode identification of σ Dra’s oscillation spectrum from TESS photometry. (a) Extracted radial (l = 0) and dipole (l = 1) oscillation mode frequencies plotted on the échelle diagram of the smoothed power spectrum. (b, c) Comparison of observed mode frequencies with those predicted by the best-fitting stellar model by the TM2 modeling team (Section 4.1), which returned a reduced χ 2 value of 1.02.
Paper: Asteroseismology of the Nearby K Dwarf σ Draconis Using the Keck Planet Finder and TESS
Authors: Marc Hon, Daniel Huber, Yaguang Li, Travis S. Metcalfe, Timothy R. Bedding, Joel Ong, Ashley Chontos, Ryan Rubenzahl, Samuel Halverson, Rafael A. García, Hans Kjeldsen, Dennis Stello, Daniel R. Hey, Tiago Campante, Andrew W. Howard, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley D. Baker, Jerry Edelstein, Chris Smith, Benjamin J. Fulton, Josh Walawender, Max Brodheim, Matt Brown, Dwight Chan, Fei Dai, William Deich, Colby Gottschalk, Jason Grillo, Dave Hale, Grant M. Hill, Bradford Holden, Aaron Householder, Howard Isaacson, Yuzo Ishikawa, Sharon R. Jelinsky, Marc Kassis, Stephen Kaye, Russ Laher, Kyle Lanclos, Chien-Hsiu Lee, Scott Lilley, Ben McCarney, Timothy N. Miller, Joel Payne, Erik A. Petigura, Claire Poppett, Michael Raffanti, Constance Rockosi, Dale Sanford, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Roger Smith, Jim Thorne, John Valliant, Adam Vandenberg, Shin Ywan Wang, Edward Wishnow, Truman Wold, Sherry Yeh, Ashley Baker, Sarbani Basu, Megan Bedell, Heather M. Cegla, Ian Crossfield, Courtney Dressing, Xavier Dumusque, Heather Knutson, Dimitri Mawet, John O'Meara, Guđmundur Stefánsson, Johanna Teske, Gautam Vasisht, Sharon Xuesong Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: A comparison of identified oscillation modes (Table 1) from (a) TESS photometric data with those from (b) KPF RV data, highlighting the differences in the observed width of the oscillation power excess across the two data sets.
Paper: Asteroseismology of the Nearby K Dwarf σ Draconis Using the Keck Planet Finder and TESS
Authors: Marc Hon, Daniel Huber, Yaguang Li, Travis S. Metcalfe, Timothy R. Bedding, Joel Ong, Ashley Chontos, Ryan Rubenzahl, Samuel Halverson, Rafael A. García, Hans Kjeldsen, Dennis Stello, Daniel R. Hey, Tiago Campante, Andrew W. Howard, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley D. Baker, Jerry Edelstein, Chris Smith, Benjamin J. Fulton, Josh Walawender, Max Brodheim, Matt Brown, Dwight Chan, Fei Dai, William Deich, Colby Gottschalk, Jason Grillo, Dave Hale, Grant M. Hill, Bradford Holden, Aaron Householder, Howard Isaacson, Yuzo Ishikawa, Sharon R. Jelinsky, Marc Kassis, Stephen Kaye, Russ Laher, Kyle Lanclos, Chien-Hsiu Lee, Scott Lilley, Ben McCarney, Timothy N. Miller, Joel Payne, Erik A. Petigura, Claire Poppett, Michael Raffanti, Constance Rockosi, Dale Sanford, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Roger Smith, Jim Thorne, John Valliant, Adam Vandenberg, Shin Ywan Wang, Edward Wishnow, Truman Wold, Sherry Yeh, Ashley Baker, Sarbani Basu, Megan Bedell, Heather M. Cegla, Ian Crossfield, Courtney Dressing, Xavier Dumusque, Heather Knutson, Dimitri Mawet, John O'Meara, Guđmundur Stefánsson, Johanna Teske, Gautam Vasisht, Sharon Xuesong Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Left: RV time series of σ Dra using the KPF. Also presented are the median-subtracted FWHM (ΔFWHM) and median-subtracted bisector inverse slope (ΔBIS) based on measurements tabulated in Table 3, as well as the SNR across the green and red cameras. Right: example of a fit to the normalized KPF CCF of σ Dra for a single spectrum. The CCF was computed using a binary spectral mask, as described in Section 3.
Paper: Asteroseismology of the Nearby K Dwarf σ Draconis Using the Keck Planet Finder and TESS
Authors: Marc Hon, Daniel Huber, Yaguang Li, Travis S. Metcalfe, Timothy R. Bedding, Joel Ong, Ashley Chontos, Ryan Rubenzahl, Samuel Halverson, Rafael A. García, Hans Kjeldsen, Dennis Stello, Daniel R. Hey, Tiago Campante, Andrew W. Howard, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley D. Baker, Jerry Edelstein, Chris Smith, Benjamin J. Fulton, Josh Walawender, Max Brodheim, Matt Brown, Dwight Chan, Fei Dai, William Deich, Colby Gottschalk, Jason Grillo, Dave Hale, Grant M. Hill, Bradford Holden, Aaron Householder, Howard Isaacson, Yuzo Ishikawa, Sharon R. Jelinsky, Marc Kassis, Stephen Kaye, Russ Laher, Kyle Lanclos, Chien-Hsiu Lee, Scott Lilley, Ben McCarney, Timothy N. Miller, Joel Payne, Erik A. Petigura, Claire Poppett, Michael Raffanti, Constance Rockosi, Dale Sanford, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Roger Smith, Jim Thorne, John Valliant, Adam Vandenberg, Shin Ywan Wang, Edward Wishnow, Truman Wold, Sherry Yeh, Ashley Baker, Sarbani Basu, Megan Bedell, Heather M. Cegla, Ian Crossfield, Courtney Dressing, Xavier Dumusque, Heather Knutson, Dimitri Mawet, John O'Meara, Guđmundur Stefánsson, Johanna Teske, Gautam Vasisht, Sharon Xuesong Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Oscillations of σ Dra as observed using KPF RV measurements (panels (a)–(b)) in comparison with observations using TESS photometry (panels (c)–(f)). The left column presents oscillation power spectra, whereas the right column presents their corresponding frequency échelle diagrams.