adsabs/AstroCLIMB huggingface dataset:
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Coadded 15 minute lum observation of A2218 made by SUPERBIT during the 2019 engineering test flight.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: A detection of Fe I absorption in WASP-76b’s atmosphere. Left: the Mantis Network template cross-correlated with our spectra. The region plotted in gray was excluded due to the low quality of the data at the edge of the GRACES wavelength range. The 2500 K template is used. Top right: the 2D cross-correlation map. The white lines indicate the peak S/N, which corresponds to a >5σ detection of Fe I in WASP-76b’s atmosphere. Bottom right: a slice of the 2D cross-correlation map at the K  p  corresponding to the peak S/N. The signal is slightly offset from RV = 0 km s−1, indicative of winds in the exoplanet’s atmosphere.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The results of cross-correlating the 1D synthetic transmission spectrum containing only Ca II, H2, and He generated for WASP-76b’s atmosphere with our observations. The plot on the left shows the high-resolution 1D synthetic transmission spectrum generated using the methods described in Section 4.1.1. The plot to the top right shows the 2D K  p –RV map, with the peak correlation identified by the dotted white lines and the S/N indicated by the color bar. The plot to the bottom right shows a slice of the 2D map at the peak K  p  value. We detect Ca II in the atmosphere with this model at a significance of 4.5σ, with a measured K  p  of ﹩{204}_{-46}^{+35}﹩ km s−1 and a measured V center of −1.0 ﹩{}_{-4.8}^{+4.5}﹩ km s−1.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The results of cross-correlating the 1D synthetic transmission spectrum generated for WASP-76b’s atmosphere with our observations. The plot on the left shows the 2D K  p –RV map, with the peak correlation identified by the dotted white lines and the S/N indicated by the color bar. The plot on the right shows a slice of the 2D map at the K  p  value corresponding to the peak correlation. The atmosphere is detected at a significance of 6.0σ, with a measured K  p  of ﹩{182}_{-15}^{+12}﹩ km s−1 and a measured V center of −4.6 ± 2.1 km s−1. The latter could be interpreted as atmospheric wind.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: A detection of Ca II absorption in WASP-76b’s atmosphere. The plots are as described in the caption of Figure 5. The 2000 K template is used. Only orders containing Ca II lines were used in the analysis, meaning that no orders were excluded due to low data quality.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: A high-resolution 1D synthetic transmission spectrum generated for WASP-76b’s atmosphere using the methods described in Section 4.1.1. A number of spectral features can be seen, including a band of strong Fe I features at the blue end of the spectrum, strong absorption features due to Na I at ∼589 nm, and many absorption lines due to H2O at the red end of the spectrum.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: A detection of Na I absorption in WASP-76b’s atmosphere. The plots are as described in the caption of Figure 5. The 2000 K template is used. Due to the small number of lines present in the model, we opted to also include lines from the blue end of the spectrum. When these lines are excluded, the detection significance falls below 5σ.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: A tentative detection of Li I absorption in WASP-76b’s atmosphere. The plots are as described in the caption of Figure 5. While we do see a peak at 4.2σ near the expected location of the exoplanet’s atmosphere, the noise in the cross-correlation map prevents us from confidently labeling this as a detection. The 2500 K template was used, and six orders with low data quality containing only weak Li I lines at the blue end of the spectrum were excluded (shown in gray).
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The P–T profile generated for WASP-76b, as described in Section 4.1.1.
Paper: Octofitter: Fast, Flexible, and Accurate Orbit Modeling to Detect Exoplanets
Authors: William Thompson, Jensen Lawrence, Dori Blakely, Christian Marois, Jason Wang, Mosé Giordano, Timothy Brandt, Doug Johnstone, Jean-Baptiste Ruffio, S. Mark Ammons, Katie A. Crotts, Clarissa R. Do Ó, Eileen C. Gonzales, Malena Rice
Figure caption: Octofitter’s ability to recover planets from simulations of circular, face-on orbits as a function of the S/N per epoch and the number of epochs. Left: Recovered S/N. Cells above the yellow line would be detected with a 5σ threshold. The cell outlined in cyan corresponds to the data shown in Figure 2. Right: The same S/Ns relative to an ideal ﹩\sqrt{N}﹩ improvement with the number of epochs. We find that the S/N grows as expected unless the final, combined S/N is below ≈5. The recovered S/N falls off quickly below this value and levels off at approximately 1. This explains why the recovered S/N of 1 exceeds the injected value of 0.5 in the bottom left corner.
Paper: Octofitter: Fast, Flexible, and Accurate Orbit Modeling to Detect Exoplanets
Authors: William Thompson, Jensen Lawrence, Dori Blakely, Christian Marois, Jason Wang, Mosé Giordano, Timothy Brandt, Doug Johnstone, Jean-Baptiste Ruffio, S. Mark Ammons, Katie A. Crotts, Clarissa R. Do Ó, Eileen C. Gonzales, Malena Rice
Figure caption: Sample plot output from Octofitter using data from the HD 91312 system. The top row visualizes the orbital posterior compared with velocity measurements of the host. The horizontal bars in the proper motion panels show the time spans over which the average velocity was measured. The middle row shows the posterior compared with astrometry measurements in the plane of the sky and in the separation and position angle over time. The bottom row shows the orbital posterior in physical coordinates to compliment the astrometry plot. The rightmost panel shows a deprojected view of the system where orbits have been rotated face on and to place periastron at the bottom. The conventions used by Octofitter are described in Appendix A.
Paper: Octofitter: Fast, Flexible, and Accurate Orbit Modeling to Detect Exoplanets
Authors: William Thompson, Jensen Lawrence, Dori Blakely, Christian Marois, Jason Wang, Mosé Giordano, Timothy Brandt, Doug Johnstone, Jean-Baptiste Ruffio, S. Mark Ammons, Katie A. Crotts, Clarissa R. Do Ó, Eileen C. Gonzales, Malena Rice
Figure caption: GPI sequences used for simulations in this section. Each image was normalized to have the same average contrast at 200 mas separation from the star (just outside the edge of the mask). The images displayed above contain a simulated planet orbiting CCW at an average of just S/N 1 per epoch, spaced one month apart. Given these data, the model recovers the simulated planet at S/N 7.
Paper: Octofitter: Fast, Flexible, and Accurate Orbit Modeling to Detect Exoplanets
Authors: William Thompson, Jensen Lawrence, Dori Blakely, Christian Marois, Jason Wang, Mosé Giordano, Timothy Brandt, Doug Johnstone, Jean-Baptiste Ruffio, S. Mark Ammons, Katie A. Crotts, Clarissa R. Do Ó, Eileen C. Gonzales, Malena Rice
Figure caption: Comparison of θ (blue, second last row) and τ (yellow, last row) parameterizations of the same orbital posterior. The θ marginal posterior is nearly Gaussian and has simple relationships with all other orbital parameters. By contrast, the τ marginal posterior is less informative and has complex relationships to ω and Ω. Complex structures in a posterior decrease sampling efficiency and could in some cases lead to biased results.
Paper: Octofitter: Fast, Flexible, and Accurate Orbit Modeling to Detect Exoplanets
Authors: William Thompson, Jensen Lawrence, Dori Blakely, Christian Marois, Jason Wang, Mosé Giordano, Timothy Brandt, Doug Johnstone, Jean-Baptiste Ruffio, S. Mark Ammons, Katie A. Crotts, Clarissa R. Do Ó, Eileen C. Gonzales, Malena Rice
Figure caption: Joint modeling of AMI and RV data. A–C: Recovered χ 2 maps at each independent AMI epoch created using Fouriever (presented in Kammerer et al. 2023). D and E: joint RV and AMI posteriors visualized as an RV time series (D) and orbit posterior in the plane of the sky (E).
Paper: Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane
Authors: S. Kent, E. Neilsen, K. Honscheid, D. Rabinowitz, E. F. Schlafly, J. Guy, D. Schlegel, J. García-Bellido, T. S. Li, E. Sanchez, J. Silber, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A. Gontcho, J. Jimenez, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, J. Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, M. Rezaie, A. J. Ross, G. Rossi, M. Schubnell, H. Seo, Gregory Tarlé, B. A. Weaver, R. Zhou, Z. Zhou, H. Zou
Figure caption: Close-up view of GFA assembly, showing the location of the two GIFs attached to each assembly. The layout of the pinhole pattern is also shown. Pinholes are 10 μm in diameter. Out of 10 such assemblies around the periphery of the DESI focal plane, six are used for guiding and field acquisition (the others being used for focus and alignment).
Paper: Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane
Authors: S. Kent, E. Neilsen, K. Honscheid, D. Rabinowitz, E. F. Schlafly, J. Guy, D. Schlegel, J. García-Bellido, T. S. Li, E. Sanchez, J. Silber, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A. Gontcho, J. Jimenez, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, J. Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, M. Rezaie, A. J. Ross, G. Rossi, M. Schubnell, H. Seo, Gregory Tarlé, B. A. Weaver, R. Zhou, Z. Zhou, H. Zou
Figure caption: Astrometric residuals per GFA as a function of the position angle with respect to the zenith (measured CCW around the DESI focal plane) in the CCD X (red) and Y (blue) directions for a set of fields in the SW at zenith distance 45°. Solid lines are a model fit.
Paper: Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane
Authors: S. Kent, E. Neilsen, K. Honscheid, D. Rabinowitz, E. F. Schlafly, J. Guy, D. Schlegel, J. García-Bellido, T. S. Li, E. Sanchez, J. Silber, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A. Gontcho, J. Jimenez, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, J. Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, M. Rezaie, A. J. Ross, G. Rossi, M. Schubnell, H. Seo, Gregory Tarlé, B. A. Weaver, R. Zhou, Z. Zhou, H. Zou
Figure caption: Left: pattern of astrometric residuals for each GFA for a field near the zenith. The green arrow points toward the zenith. Right: same for a field at a zenith distance of 55°.
Paper: Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane
Authors: S. Kent, E. Neilsen, K. Honscheid, D. Rabinowitz, E. F. Schlafly, J. Guy, D. Schlegel, J. García-Bellido, T. S. Li, E. Sanchez, J. Silber, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A. Gontcho, J. Jimenez, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, J. Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, M. Rezaie, A. J. Ross, G. Rossi, M. Schubnell, H. Seo, Gregory Tarlé, B. A. Weaver, R. Zhou, Z. Zhou, H. Zou
Figure caption: Exaggerated view of the focal plane deformation pattern for the field shown at the right in Figure 6. The peak amplitude is 0.″18. The axis units are arbitrary.
Paper: Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane
Authors: S. Kent, E. Neilsen, K. Honscheid, D. Rabinowitz, E. F. Schlafly, J. Guy, D. Schlegel, J. García-Bellido, T. S. Li, E. Sanchez, J. Silber, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A. Gontcho, J. Jimenez, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, J. Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, M. Rezaie, A. J. Ross, G. Rossi, M. Schubnell, H. Seo, Gregory Tarlé, B. A. Weaver, R. Zhou, Z. Zhou, H. Zou
Figure caption: Schematic layout of the focal plane (left) and side view of the Mayall telescope (right) showing the major DESI hardware systems relevant to PlateMaker.
Paper: Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane
Authors: S. Kent, E. Neilsen, K. Honscheid, D. Rabinowitz, E. F. Schlafly, J. Guy, D. Schlegel, J. García-Bellido, T. S. Li, E. Sanchez, J. Silber, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A. Gontcho, J. Jimenez, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, J. Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, M. Rezaie, A. J. Ross, G. Rossi, M. Schubnell, H. Seo, Gregory Tarlé, B. A. Weaver, R. Zhou, Z. Zhou, H. Zou
Figure caption: Flowchart showing the basic steps of the astrometric calibration process.
Paper: Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane
Authors: S. Kent, E. Neilsen, K. Honscheid, D. Rabinowitz, E. F. Schlafly, J. Guy, D. Schlegel, J. García-Bellido, T. S. Li, E. Sanchez, J. Silber, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A. Gontcho, J. Jimenez, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, J. Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, M. Rezaie, A. J. Ross, G. Rossi, M. Schubnell, H. Seo, Gregory Tarlé, B. A. Weaver, R. Zhou, Z. Zhou, H. Zou
Figure caption: Layout of guider GFAs on the DESI focal plane with various coordinate systems labeled. The parallactic angle ψ is the position angle of the zenith relative to the north. The position angle of a typical GFA relative to the zenith is marked as θ.
Paper: Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane
Authors: S. Kent, E. Neilsen, K. Honscheid, D. Rabinowitz, E. F. Schlafly, J. Guy, D. Schlegel, J. García-Bellido, T. S. Li, E. Sanchez, J. Silber, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A. Gontcho, J. Jimenez, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, J. Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, M. Rezaie, A. J. Ross, G. Rossi, M. Schubnell, H. Seo, Gregory Tarlé, B. A. Weaver, R. Zhou, Z. Zhou, H. Zou
Figure caption: Distortion patterns for the two nonaxisymmetric modes induced by the ADC.
Paper: New Insights on 30 Dor B Revealed by High-quality Multiwavelength Observations
Authors: Wei-An Chen, 韋安 陳, Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Shutaro Ueda, 周太朗 上田, Kuo-Song Wang, 國松 王, Sheng-Yuan Liu, 聖元 呂, Bo-An Chen, 柏安 陳
Figure caption: Multiband images of 30 Dor B. All images use an “inverted colormap” with high values in black and low values in white. The top row shows the Hα, [S II], and [O III] images taken with the MOSAIC camera on the Blanco 4 m telescope. The white spots are bright stars that are saturated in the MOSAIC images. The middle row shows the Hα image from HST, [S II]/Hα ratio from 4 m MOSAIC images (see Figure 8 for ratio maps with color bar), and X-ray 0.5–7.0 keV band image (log scale) from 2.18 Ms Chandra ACIS observations. The bottom row shows the radio image at 888 MHz from ASKAP (square root scale, with the beam plotted in the lower left corner) and IRAC 8 μm and MIPS 24 μm images from Spitzer. The red plus sign in each panel marks the position of the pulsar PSR J0537−6910.
Paper: Astrophysical Distance Scale. VII. A Self-consistent, Multiwavelength Calibration of the Slopes and Relative Zero Points for the Run of Luminosity with the Color of Stars Defining the Tip of the Red Giant Branch
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: The individual traces (in blue) of the tip of the red-giant branch in VIJHK and in 3.6 & 4.5 μm (the latter two having identical slopes). The TRGB I-band slope is flat blue line. Below it is a red line, +0.3 mag fainter, going through larger yellow dots that are the tracer stars used to define the color–color plots shown in this paper.
Paper: Astrophysical Distance Scale. VII. A Self-consistent, Multiwavelength Calibration of the Slopes and Relative Zero Points for the Run of Luminosity with the Color of Stars Defining the Tip of the Red Giant Branch
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: The trends of RGB isochrones with metallicity for alpha-enhanced models (in the right panel) and solar models (in the left panel). The horizontal dashed lines are at the approximate level of the brightest TRGB stars (at −4.037 mag) having a solar mixture; the solid horizontal line marks the level of the TRGB (at −4.050 mag) for ɑ-enhanced models. See text for additional details.
Paper: Astrophysical Distance Scale. VII. A Self-consistent, Multiwavelength Calibration of the Slopes and Relative Zero Points for the Run of Luminosity with the Color of Stars Defining the Tip of the Red Giant Branch
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: The trends, with increasing wavelength (bandpass) of the absolute magnitude of TRGB stars at the blue [(J−K) = 0.6 mag] metal-poor end and at the red [(J−K) = 1.2 mag] metal-rich end of the fits shown in Figure 6. The thin black lines indicate where the F115W filter on JWST/NIRCam is expected to show its slanting tip, which, because of that band’s slightly blue effective wavelength (ground-based J), it will be slightly fainter overall and slightly shallower in its slope than the J-band values shown here and elsewhere. The JWST absolute mean-magnitude zero point is set at the fiducial color [F115W–F365W] = 1.34 mag, corresponding to (J−K) = 1.00 mag.
Paper: Astrophysical Distance Scale. VII. A Self-consistent, Multiwavelength Calibration of the Slopes and Relative Zero Points for the Run of Luminosity with the Color of Stars Defining the Tip of the Red Giant Branch
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: (V−I) vs (J−K) color–color Plots. Left Panel: stars are selected to be +0.3 (±0.1) mag below the I-band TRGB. Right Panel: stars are chosen to be +0.4 (±0.1) mag below the TRGB. No significant difference is found between these two solutions for color–color correlation used in Equation (1).
Paper: Astrophysical Distance Scale. VII. A Self-consistent, Multiwavelength Calibration of the Slopes and Relative Zero Points for the Run of Luminosity with the Color of Stars Defining the Tip of the Red Giant Branch
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: Color–color transformation plots: upper plot: (I−J) to (J−K), middle plot: (I−H) to (J−K), and lower plot: (I−K) to (J−K). Solid red lines are the adopted linear fits to the data. Yellow points represent one in five of the blue data points and are overplotted to give a visual sense of the surface density of points in high-overlap regions.
Paper: Astrophysical Distance Scale. VII. A Self-consistent, Multiwavelength Calibration of the Slopes and Relative Zero Points for the Run of Luminosity with the Color of Stars Defining the Tip of the Red Giant Branch
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: NIR color–magnitude diagrams centered on the TRGB in J, H, and K vs. (J−K), top to bottom. The red slanting line is defined by the color–color transformations shown in three panels of Figure 2.
Paper: Astrophysical Distance Scale. VII. A Self-consistent, Multiwavelength Calibration of the Slopes and Relative Zero Points for the Run of Luminosity with the Color of Stars Defining the Tip of the Red Giant Branch
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: Rotated color–color plots for (J−K) vs. the mid-infrared blended colors: (J−3.6) and (J−4.5) in the left and right panels, respectively. See text for additional details.