adsabs/AstroCLIMB huggingface dataset:
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The upper panel shows the results of the maximum-likelihood solution for NGC 4365. The abscissa is the galaxy’s true distance modulus, the ordinate is the number of PNe within 2.5 mag of M*, normalized to the amount of bolometric light sampled, and the contours are drawn at 0.5σ intervals. The lower panel marginalizes over the PN/light variable.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The observed PNLF for NGC 4418 binned into 0.2 mag intervals. Open circles denote data beyond the completeness limit; the error bars show the small number counting statistics (Gehrels 1986), and the curve shows Equation (2) shifted by the best-fit apparent distance modulus of (m − M) = 32.66.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The top panels show the continuum images for the nuclear fields of NGC 1404 (left) and NGC 1351 (right). The PSF stars are identified with colored markers. The middle panels show the wavelength dependence of the stars’ PSFs’ by plotting their best-fit FWHMs. The data are fit with a second-degree polynomial. The lower panels show the residuals from this fit, with the brightest star on the bottom and the faintest on the top. Each curve is offset by 1.0 from the previous curve for clarity. The colors correspond to those shown in the images. Note the large residuals associated with the fainter stars.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: NGC 1351 PSF star radial plots, obtained from the image shown in Figure 61.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: Composite [O III] on-band map of NGC 1385 with pointings P1–P5 identified. Our PN candidates are circled in blue and labeled; red circles without labels are objects classified as H II regions or SNRs. PNe and SNRs identified by Scheuermann et al. (2022) are shown in magenta and orange, respectively.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: NGC 1404 PSF star aperture corrections as a function of wavelength, obtained from the image shown in Figure 61. PSF stars S1–S5 are shown from top to bottom.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: NGC 1351 PSF star aperture corrections as a function of wavelength, obtained from the image shown in Figure 61. PSF stars S1–S4 are shown from top to bottom.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: NGC 1404 PSF star radial plots, obtained from the image shown in Figure 61.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Illustrations of the four typical shapes of the spectral line profiles observed in IRC+10216: flat topped (e.g., HC5H, optically thin, spatially unresolved), double peaked (e.g., 13CO, optically thin, spatially resolved), truncated parabolic (e.g., SiO, optically thick, spatially resolved), and parabolic (e.g., CO, optically thick, spatially unresolved). The solid black line shows the observed spectrum, and the solid red line represents the spectral line profile fitted by the shell function. The rest frequency of separable spectral lines are in MHz, and the molecule’s name is displayed in the upper right corner of each panel. All of the detected spectra from this survey are included in Appendix C.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: An overall spectral line survey toward IRC+10216 in the 3 mm band by the PMO 13.7 m radio telescope. The rest frequency scale was obtained by adopting a radial velocity of −26.5 km s−1. The X-axis denotes the rest frequency (GHz), and the Y-axis depicts T mb (kelvin). On the upper panel, spectral lines with T mb greater than 1.3 K are marked, while those with T mb greater than 350 mK are marked on the lower panel.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Same as Figure F1 but for SiS.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: NIRCam CMDs of WLM in select filter combinations. Panels (a), (b), and (c) show the CMDs for the SW (F090W−F150W), LW (F250M−F430M), and an example SW/LW (F090W−F250M) filter combination. The left side of each plot shows CMDs of all objects detected, while the right sides are CMDs of stars that passed the culling criteria described in Section 3.5. The SW CMD of WLM is the deepest ever constructed for a galaxy that is not within the viral radius of the MW. A number of stellar evolution sequences are quite tight (e.g., RGB, subgiant branch, young MS), in line with the exquisite S/N. Panel (b) shows the LW-only CMD, which shows a bright AGB star sequence, a bright RGB, and a well-populated RC. The increased scatter below the RC is the result of culling criteria applied only to SW data. Panel (c) shows an example SW–LW CMD. As with panel (a), a number of clear sequences emerge. The CMD nearly reaches the oldest MSTO, despite the LW filter being a medium band.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: The spatial distribution of objects and stars detected by DOLPHOT in our NIRCam imaging of Draco II. Left: A density map (∼50 × 50 pixel bins) of the ∼5.1 × 105 objects reported in the raw DOLPHOT catalog. The spatial distribution of objects shows a number of features, including saturated foreground stars and background galaxies. The other prominent features are the diffuse object overdensities that are present in chips A3, B3, and B4. These are the result of persistence from the previous program (1022), which was staring at/near Mars, Jupiter, and Saturn for ∼12 hr in order to test the fine guidance sensor. Right: The density map of the ∼1.1 × 103 stars that passed the catalog culling criteria listed in Section 3.5. These criteria removed the vast majority of obvious artifacts (e.g., corresponding to saturated stars, diffraction spikes) as well as eliminated most of the contamination from persistence.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: NIRCam CMDs of Draco II in select filter combinations. Panels (a), (b), and (c) show the CMDs for the SW (F090W−F150W), LW (F360M−F480M), and an example SW/LW (F090W−F360M) filter combination. The SW CMD of Draco II (panel (a)) is the deepest ever (i.e., it reaches the lowest stellar mass) constructed for a galaxy outside the MW itself. It includes a clearly defined MS kink. Panel (b) shows the LW-only CMD, which is essentially vertical at a color of ∼0 due to the lack of temperature sensitivity in the F360M−F480M filter combination. Panel (c) shows an example SW–LW CMD (F090W−F360M), which extends below the MS kink before photometric scatter washes out the stellar sequence. This depth is impressive for a medium-band LW filter. For both CMDs that include the LW filter, specific LW culling criteria may reduce some of the noise in the CMD, particularly at the faint end.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: The NIRISS CMD of M92, excluding the third exposure. The left panel shows all objects detected, the right panel shows the stars that passed the culling criteria. Compared to the SW NIRCam CMD in Figure 2, the NIRISS CMDs cover a smaller dynamic range in luminosity, owing to saturation effects at the bright end and lower sensitivity at the faint end. The diagonal feature of stars at F090W ∼ 20 corresponds to objects in image artifacts that were not removed by the applied culling criteria. The increased scatter in this CMD, relative to the SW NIRCam CMD, is due to the combination of lower S/N as well as WebbPSF models that are not as well matched to the observed PSFs.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: The spatial distribution of objects and stars detected by DOLPHOT in our NIRCam imaging of WLM. Left: A density map (∼50 × 50 pixel bins) of the ∼1.7 × 106 objects reported in the raw DOLPHOT catalog. The spatial distribution of detected objects is fairly uniform, with a slight gradient toward chip A1, which is positioned closest to the center of the galaxy. Additional features include a high density of sources that trace saturated stars and a lower density of sources in the SW chip gaps. Right: The density map of the ∼4.6 × 105 stars that passed the catalog culling criteria listed in Section 3.5. These criteria removed the vast majority of obvious artifacts (e.g., corresponding to saturated stars, diffraction spikes). The density of stars increases toward chip A1, which is closest to the center of the galaxy.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: The spatial distribution of objects and stars detected by DOLPHOT in our NIRISS imaging of M92. Left: A density map (∼50 × 50 pixel bins) of the ∼1.3 × 105 objects reported in the raw DOLPHOT catalog. The spatial distribution of detected objects is uniform. Some artifacts (e.g., bright stars, claws; Rigby et al. 2023) are visible. Right: The density map of the ∼2.9 × 103 stars that passed the catalog culling criteria listed in Section 3.5. These criteria removed the vast majority of obvious artifacts (e.g., corresponding to saturated stars, diffraction spikes), leaving a sparse sampling of stars. This low density is expected, given that the field is located at ∼5 half-light radii.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: The spatial distribution of objects and stars detected by DOLPHOT in our NIRISS imaging of WLM. Left: A density map (∼50 × 50 pixel bins) of the ∼1.6 × 105 objects reported in the raw DOLPHOT catalog. The spatial distribution of detected objects is fairly uniform. Holes in the spatial distribution mainly correspond to saturated pixels that were entirely masked by DOLPHOT. Right: The density map of the ∼1.3 × 104 stars that passed the catalog culling criteria listed in Section 3.5. There is a modest spatial gradient that increases in the direction of the main body of the galaxy.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: The NIRISS CMD of WLM. The left panel shows all objects detected; the right panel shows the stars that passed the culling criteria. The NIRISS CMD has a similar depth to the NIRCam CMD, albeit with increased scatter. In part, the scatter is due to the lower sensitivity of NIRISS in these filters, along with the less accurate NIRISS WebbPSF models. As expected, due to its location outside the main body of the galaxy, the NIRISS CMD lacks a stellar population younger than a few Gyr and is much more sparsely populated.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: The completeness and photometric uncertainty for the M92 NIRCam F090W and F150W data computed from artificial star tests. The top panel shows the completeness function for each filter. The bottom panels show the recovered minus the input magnitude difference for ASTs that pass the same culling criteria as applied to the photometry. The 50% completeness limits are m F090W = 26.4, and m F150W = 25.4. Both filters have a bias consistent with zero.
Paper: Metallicities and Refined Stellar Parameters for 52 Cool Dwarfs with Transiting Planets and Planet Candidates
Authors: Rebecca Gore, Steven Giacalone, Courtney D. Dressing, Emma V. Turtelboom, Ashley Schroeder, Charles D. Fortenbach, Kevin K. Hardegree-Ullman, Jon K. Zink, Andrew W. Mayo, Joshua E. Schlieder, Jessie L. Christiansen
Figure caption: Distribution of stellar masses and metallicities for low-mass stars with at least one small planet (R p < 4 R ⊕;  left) or at least one giant planet (R p > 4 R ⊕;  right). Black dots are the masses and metallicities of stars with T eff < 4300 K, ﹩\mathrm{log}g\gt 4﹩, and M ⋆ < 0.7 M ⊙ collected from the NASA Exoplanet Archive, which were calculated using a variety of techniques. Red circles are stars in our sample with at least one confirmed planet. Blue squares are stars in our sample with no confirmed planets but at least one planet candidate. The gray bars are 1σ uncertainties. The histograms on the right of each panel are the normalized density distributions of all points combined. In general, our measured values agree well with previously reported values of similar systems.
Paper: Metallicities and Refined Stellar Parameters for 52 Cool Dwarfs with Transiting Planets and Planet Candidates
Authors: Rebecca Gore, Steven Giacalone, Courtney D. Dressing, Emma V. Turtelboom, Ashley Schroeder, Charles D. Fortenbach, Kevin K. Hardegree-Ullman, Jon K. Zink, Andrew W. Mayo, Joshua E. Schlieder, Jessie L. Christiansen
Figure caption: Derived stellar parameters, as discussed in Section 4, plotted against the respective values listed in the EPIC (orange) and the TIC (light blue). Squares indicate stars with at least one confirmed planet, circles indicate stars with only planet candidates, and crosses indicate stars with only false positives or no planet candidates. The solid red line in each panel denotes the 1-to-1 line. In general, our values agree well with the values in the TIC and likely provide improved accuracy over those in the EPIC using stellar models. In many cases, we provide parameters with a greater precision than either catalog.
Paper: Metallicities and Refined Stellar Parameters for 52 Cool Dwarfs with Transiting Planets and Planet Candidates
Authors: Rebecca Gore, Steven Giacalone, Courtney D. Dressing, Emma V. Turtelboom, Ashley Schroeder, Charles D. Fortenbach, Kevin K. Hardegree-Ullman, Jon K. Zink, Andrew W. Mayo, Joshua E. Schlieder, Jessie L. Christiansen
Figure caption: Hertzsprung–Russell diagram using the updated values of our observed stars from Section 4 (blue circles). For reference, all TESS Objects of Interest are plotted in the background (gray circles).
Paper: Metallicities and Refined Stellar Parameters for 52 Cool Dwarfs with Transiting Planets and Planet Candidates
Authors: Rebecca Gore, Steven Giacalone, Courtney D. Dressing, Emma V. Turtelboom, Ashley Schroeder, Charles D. Fortenbach, Kevin K. Hardegree-Ullman, Jon K. Zink, Andrew W. Mayo, Joshua E. Schlieder, Jessie L. Christiansen
Figure caption: The same as Figure 5, but for systems with only one detected planet or planet candidate (left) and systems with multiple detected planets or planet candidates (right).