adsabs/AstroCLIMB huggingface dataset:
Paper: Peculiar Orbital Characteristics of Earth Quasi-Satellite 469219 Kamo‘oalewa: Implications for the Yarkovsky Detection and Orbital Uncertainty Propagation
Authors: Shoucun Hu, Bin Li, Haoxuan Jiang, Gang Bao, Jianghui Ji
Figure caption: The top panels show the geocentric orbit of Kamo‘oalewa in the mean ecliptic reference frame of J2000.0 and the Sun–Earth rotating frame, respectively (both are projected from the direction of the north ecliptic pole). The bottom panels show the variations in the geocentric distance and apparent magnitude, respectively. The time span ranges from 2004 to 2022. The red circles mark up the observation epochs, while the green circles represent Earth’s Hill sphere.
Paper: Peculiar Orbital Characteristics of Earth Quasi-Satellite 469219 Kamo‘oalewa: Implications for the Yarkovsky Detection and Orbital Uncertainty Propagation
Authors: Shoucun Hu, Bin Li, Haoxuan Jiang, Gang Bao, Jianghui Ji
Figure caption: The two panels show the changes in Δa and Δλ for Kamo‘oalewa from 2000 to 2100 with the same initial states. Δa and Δλ are the differences of the semimajor axis and the mean longitude between the Yarkovsky-included and the gravity-only models. The difference between the blue lines and the red lines is that the former includes all the planetary gravitational perturbations while the latter includes all of those but Earth. The black dashed line is the Δa computed with the analytical method (Equation (2)). The value of A 2 in these figures is assumed to be −1.0 × 10−13 au day−2.
Paper: Peculiar Orbital Characteristics of Earth Quasi-Satellite 469219 Kamo‘oalewa: Implications for the Yarkovsky Detection and Orbital Uncertainty Propagation
Authors: Shoucun Hu, Bin Li, Haoxuan Jiang, Gang Bao, Jianghui Ji
Figure caption: Variations of the positional uncertainty from 2010 to 2030 for the solution S7 in different frames. The top two panels show the changes in the heliocentric frame for the Cartesian and RTN coordinates, respectively. The third panel shows the results for the RTN directions in the geocentric frame, and the bottom panel shows the results for the Cartesian coordinates in the geocentric Sun–Earth rotating frame.
Paper: Peculiar Orbital Characteristics of Earth Quasi-Satellite 469219 Kamo‘oalewa: Implications for the Yarkovsky Detection and Orbital Uncertainty Propagation
Authors: Shoucun Hu, Bin Li, Haoxuan Jiang, Gang Bao, Jianghui Ji
Figure caption: The two images of Kamo‘oalewa (inside the red circles) observed by SDSS. The left was observed at 11:16:48.5 and the right at 11:21:35.1 UTC on 2004 March 17.
Paper: Peculiar Orbital Characteristics of Earth Quasi-Satellite 469219 Kamo‘oalewa: Implications for the Yarkovsky Detection and Orbital Uncertainty Propagation
Authors: Shoucun Hu, Bin Li, Haoxuan Jiang, Gang Bao, Jianghui Ji
Figure caption: The probability density distributions of A 2 for the solutions S7 and ﹩{{\rm{S}}}_{7}^{* }﹩.
Paper: Peculiar Orbital Characteristics of Earth Quasi-Satellite 469219 Kamo‘oalewa: Implications for the Yarkovsky Detection and Orbital Uncertainty Propagation
Authors: Shoucun Hu, Bin Li, Haoxuan Jiang, Gang Bao, Jianghui Ji
Figure caption: Histograms of normalized O–C residuals of R.A. (α) and decl. (δ) for the solutions S6 and S7.
Paper: Peculiar Orbital Characteristics of Earth Quasi-Satellite 469219 Kamo‘oalewa: Implications for the Yarkovsky Detection and Orbital Uncertainty Propagation
Authors: Shoucun Hu, Bin Li, Haoxuan Jiang, Gang Bao, Jianghui Ji
Figure caption: Time evolution of uncertainty in the orbital elements from 2010 to 2030 for the solution S7.
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: Top: CTIO echelle slit positions 1–10 overplotted on the HST F658N (left) and X-ray Chandra 0.5–7.0 keV (right) images. The X-ray image is displayed in logarithmic scale. Bottom: CTIO 4 m Hα echellograms displayed with spatial scale and extent matching the slit positions plotted in the top panels. The slit numbers are marked in the upper left corners in red. A thick dashed line is plotted at the bulk ISM velocity of 272 km s−1, and two auxiliary thin dashed lines are plotted at ±100 km s−1 offsets, respectively. Magenta arrows point at examples of high-velocity features emanating from the quiescent ISM velocity, and cyan arrows point at examples of discrete high-velocity cloudlets. Pixels affected by cosmic-ray hits have been fixed by interpolation between adjacent unaffected pixels. The Hα line profiles in boxes 2–E (blue), 2–W (red), 9–N (blue), and 9–S (red) are presented in Figure 6.
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: Left panel: ASKAP 1420 MHz map smoothed to match the angular resolution of the 888 MHz map. Right panel: spectral index map. Both panels are overplotted with contours from the 888 MHz map shown in Figure 3. In the spectral index map, only the regions with 888 MHz flux density >15σ are shown, where σ ∼ 4 × 10−4 Jy beam−1. The plus sign marks the position of the pulsar. The dashed lines connect the radio/X-ray arc, PWN, pulsar, and the bright patches of emission inside and outside the X-ray-emitting regions. The very steep negative spectral index near the east edge of the map is part of the 30 Dor giant H II region.
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: Top left: Chandra X-ray image in the 0.5–7.0 keV band shown in logarithm scale. The contour levels are 2.3 × 10−9, 3.7 × 10−9, 8.0 × 10−9, 1.4 × 10−8, 5.0 × 10−8, 5.0 × 10−7, and 1.0 × 10−6 counts s−1 cm−2, extracted from the X-ray image smoothed by a Gaussian filter with σ = 4″. Top right: ASKAP 888 MHz image shown in square root scale. The contour levels are 0.007, 0.01, 0.02, 0.03, 0.04, 0.07, 0.1, and 0.2 Jy beam−1. Bottom left: Chandra X-ray image overplotted with the radio contours from the top right panel. Bottom right: HST Hα image overplotted with the X-ray contours (green) from the top left panel and radio contours (red) from the top right panel. The white plus sign marks the position of the pulsar PSR J0537−6910.
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: Same as Figure 4, but the echellograms in the bottom panels are displayed with a different intensity scale to accentuate the faint high-velocity features.
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: Top panel: Hα velocity profiles extracted from boxes 2–E (blue) and 2–W (red) along slit position 2. Bottom panel: Hα velocity profiles extracted from boxes 9–N (blue)and 9–S (red) along slit position 9. The box positions are marked in Figure 4. The fainter profile has been multiplied by a factor given in the upper right corner of the panel to match the peak of the brighter profile. The instrumental FWHM measured from the telluric lines is ∼18 km s−1; thus, even the narrow profiles are resolved.
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: The HST F555W image of the SNR 30 Dor B and its environment. The spectral types of massive stars from the VLT-FLAMES Tarantula Survey (Evans et al. 2011) are marked, with O and B stars in cyan and magenta, respectively. Late-type supergiants and Wolf-Rayet stars are marked in green. The 16 ms pulsar in the SNR is marked with a white plus sign. The 3′-diameter circle marks a rough boundary of the OB association LH99 (Lucke & Hodge 1970).
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: [S II]/Hα ratio maps derived from the 4 m MOSAIC images (left) and MCELS images (right). The white spots in the MOSAIC map are caused by saturated star images. The red plus sign marks the position of the pulsar.
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: Left: close-up HST Hα image of 30 Dor B. Right: HST Hα image with sharp filaments marked. The white plus sign marks the position of the pulsar PSR J0537−6910.
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: Close-up of shocked cloudlets.
Paper: The Prospect of Detecting Volcanic Signatures on an ExoEarth Using Direct Imaging
Authors: Colby M. Ostberg, Scott D. Guzewich, Stephen R. Kane, Erika Kohler, Luke D. Oman, Thomas J. Fauchez, Ravi K. Kopparapu, Jacob Richardson, Patrick Whelley
Figure caption: The globally averaged TP profiles (upper panel), H2O vapor abundance profiles (middle panel), and volcanic aerosol abundance profiles (lower panel) of the 30 Gt eruption exoEarth for every 12 months of the simulation. The corresponding profile of the baseline simulation is shown for reference.
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: Close-up images for two crowded regions in Figure 10. The small cluster in the left panel is TLD 1.
Paper: The Prospect of Detecting Volcanic Signatures on an ExoEarth Using Direct Imaging
Authors: Colby M. Ostberg, Scott D. Guzewich, Stephen R. Kane, Erika Kohler, Luke D. Oman, Thomas J. Fauchez, Ravi K. Kopparapu, Jacob Richardson, Patrick Whelley
Figure caption: The reflectance spectrum of the 30 Gt eruption exoEarth for every six months of the simulation. Absorption features are labeled with their corresponding molecules. Both panels show the same spectra, but the upper panel is on a log scale, while the lower panel is scaled linearly. There is variation in the size of the O3 absorption feature and in the slope of the spectra between 0.3 and 0.6 μm due to fluctuations in volcanic aerosol abundance throughout the simulation. The change in slope of the spectrum also affects the location of the continuum. The size of the H2O features change throughout the simulation because the eruptions cause an influx of volcanic aerosols and H2O vapor into the upper atmosphere.
Paper: The Prospect of Detecting Volcanic Signatures on an ExoEarth Using Direct Imaging
Authors: Colby M. Ostberg, Scott D. Guzewich, Stephen R. Kane, Erika Kohler, Luke D. Oman, Thomas J. Fauchez, Ravi K. Kopparapu, Jacob Richardson, Patrick Whelley
Figure caption: The reflectance spectra of the 30 Gt eruption exoEarth in month 11 of the simulation (upper panel) and the transmittances of the major molecular species in its atmosphere (lower panel). The most prominent absorption feature in the UV is caused by O3. Absorption by SO2 occurs in the UV around 0.3 μm, but it is overshadowed by O3 and O2 absorption. The VIS bandpass has a single O2 absorption band and multiple H2O absorption bands. The NIR bandpass includes three H2O absorption bands at 1.15, 1.4, and 1.85 μm.
Paper: The Prospect of Detecting Volcanic Signatures on an ExoEarth Using Direct Imaging
Authors: Colby M. Ostberg, Scott D. Guzewich, Stephen R. Kane, Erika Kohler, Luke D. Oman, Thomas J. Fauchez, Ravi K. Kopparapu, Jacob Richardson, Patrick Whelley
Figure caption: The reflectance spectrum of the 15 Gt eruption exoEarth in month 71 of the simulation with and without absorption from O3, H2O, or O2. The left panel shows the UV spectrum without O3 absorption. The middle panel shows the VIS spectrum without O2 and H2O absorption. The right panel shows the NIR spectrum without H2O absorption.
Paper: The Prospect of Detecting Volcanic Signatures on an ExoEarth Using Direct Imaging
Authors: Colby M. Ostberg, Scott D. Guzewich, Stephen R. Kane, Erika Kohler, Luke D. Oman, Thomas J. Fauchez, Ravi K. Kopparapu, Jacob Richardson, Patrick Whelley
Figure caption: The reflectance spectra for each month of the baseline exoEarth simulation in comparison to months 12 and 96 of the 15 Gt eruption. Both plots show the same spectra, but the upper panel is on a log scale, and the lower panel is scaled linearly.
Paper: The Cycles of Alpha Centauri: Double Dipping of AB
Authors: Thomas Ayres
Figure caption: FUV spectral landscape of the Fe XII coronal forbidden lines. The left panel is for 1241; the right panel is for 1349. The coronal lines are hatched. The y-axis is the bolometrically normalized flux density. Five stars are in the comparison: Procyon (upper, green), α Cen A (middle, blue), α Cen B (lower middle, red), and the noncoronal red giants α Boo (K1 III; lower, orange) and γ Cru (M3 III; lower, black). The (shifted) zero-points of α Cen A and Procyon are thick blue tick marks at either side of the panels, those for α Boo and γ Cru are thick orange, and the α Cen B zero-point is red. The black curve in the left panel, partly covered by the α Cen A tracing, is a simulation of the C I recombination spectrum (same zero-point as A). Shaded vertical bands in both panels highlight incidental emission (and absorption) lines. The strong (unmarked) feature at 1242.8 Å is the longward component of hot subcoronal N V, weak or absent in the two red giants.
Paper: The Cycles of Alpha Centauri: Double Dipping of AB
Authors: Thomas Ayres
Figure caption: Differential light curves of α Cen AB and Procyon for high-S/N chromospheric and subcoronal emissions (black filled circles), the two Fe XII forbidden lines (green), and X-rays (red). Tracings are shifted vertically for clarity. Each time series was separately normalized to the average of the values between the vertical dashed lines. Horizontal lines mark the zero levels. Error bars of the weak Fe XII lines are shown explicitly for (σ  L / < f  L  > ) ≥ 10 %. “1355” refers to chromospheric O I; “1549” refers to subcoronal C IV.
Paper: The Cycles of Alpha Centauri: Double Dipping of AB
Authors: Thomas Ayres
Figure caption: Time series of sensitivity-corrected, calibrated X-ray fluxes (0.1–2.4 keV) of α Cen AB and Procyon (same color-coding as in Figure 2), expressed as L X/L BOL. Small gray points represent daily solar X-ray irradiances over the declining phase of sunspot Cycle 23 (left side), the whole of Cycle 24 (middle), and the rise of current Cycle 25 (right side). Black filled circles are 81-day averages (three rotations).
Paper: The Cycles of Alpha Centauri: Double Dipping of AB
Authors: Thomas Ayres
Figure caption: X-rays (red filled circles) plus scaled, blend-corrected Fe XII (black filled circles) of α Cen B over the span of the several joint Chandra/HST programs since SM4. Photometric uncertainty of the combined Fe XII flux is shown explicitly when larger than the symbol size (≥5%). The gray curve is the Chandra/XMM-Newton X-ray time series advanced by 16 yr (two B cycles).
Paper: The Cycles of Alpha Centauri: Double Dipping of AB
Authors: Thomas Ayres
Figure caption: Time series of Chandra HRC-I CRs of α Cen A (blue filled circles), α Cen B (red), and Procyon (green). One-sided error bars (from the flare-filtering method) indicate degree of variability where significant. Gray crosses to the left are averages of XMM-Newton CRs of B, scaled to HRC-I. The slanted yellow line corresponds to a decline of 3.5% per year post-2016 for Procyon.
Paper: The Cycles of Alpha Centauri: Double Dipping of AB
Authors: Thomas Ayres
Figure caption: Recent Chandra HRC-I images of α Cen AB. North is up, east to the left. The snapshots share the same reverse gray scale for the intensities (counts s−1 pixel−1). The x- and y-axes are relative sky coordinates, centered on the primary star (A; blue cross-hairs). The secondary (B) is circled in red. Dotted curves indicate the orbital path of B: note the increasing AB separation in recent years.
Paper: A Rotating Accretion Disk around MWC 297, a Young B1.5Ve Star
Authors: Göran Sandell, William Vacca
Figure caption:  12CO and 13CO υ = 1–0 absorption lines. The 12CO and 13CO profiles are plotted with solid and dashed lines, respectively. The lines are identified in the lower left corner of the image. The velocity of the emission lines, centered at 0 km s−1, is marked with a gray vertical line. The optically thick 12CO υ = 1–0 R(0) line appears flat-topped, much broader, and shifted in velocity relative to 12CO 1–0 R(4) and 13CO 1–0 R(2), which are optically thin. This is because there is a second, colder redshifted cloud component, which is optically thick in the 12CO 1–0 R(0) line. It is also seen in the 13CO 1–0 line as a strong redshifted wing. The 0 km s−1velocity corresponds to a V lsr = 6.7 km s−1.
Paper: A Rotating Accretion Disk around MWC 297, a Young B1.5Ve Star
Authors: Göran Sandell, William Vacca
Figure caption: The iSHELL spectrum showing the υ = 1–0 12CO lines in absorption. The wavelength region is split into two for clarity. The transitions R(3), R(2), R(1), and R(0) are at the top, and P(1),  P(2), P(3), and P(4) are at the bottom, left to right. Regions of strong telluric absorption have been blanked out. The fainter double-peaked emission lines are from higher rotational rotation transitions. The strong hydrogen lines Pfβ and Huϵ are also seen. The model fit to the absorption lines is overlaid in red.
Paper: A Rotating Accretion Disk around MWC 297, a Young B1.5Ve Star
Authors: Göran Sandell, William Vacca
Figure caption: An example illustrating the extraction of absorption-line profiles. The observed emission line, in this case the 12CO υ = 1–0 R(4), is plotted in black; the scaled template profile is plotted in red; and the resulting absorption profile is plotted in green. The baseline around the absorption profile (green) is quite flat and centered at 0.
Paper: A Rotating Accretion Disk around MWC 297, a Young B1.5Ve Star
Authors: Göran Sandell, William Vacca
Figure caption: The ring model for T = 1500 K and a log density of 18.2 cm−2 in red overlaid on the observed M-band spectrum. 13CO needs to be scaled by 6 to match the line profiles. The line transitions are marked, and the rovibrational bands they belong to are indicated at the top for 12CO and at the bottom for 13CO 1–0. Regions of strong telluric absorption have been blanked out.
Paper: Verification of Gaia Data Release 3 Single-lined Spectroscopic Binary Solutions With Three Transiting Low-mass Secondaries
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Keyi Ding, 可怿 丁, Samuel K. Grunblatt, Theron Carmichael, Allyson Bieryla, Joseph E. Rodriguez, Jack Schulte, Noah Vowell, George Zhou, Samuel N. Quinn, Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, David W. Latham, Douglas A. Caldwell, M. M. Fausnaugh, Christina Hedges, Jon M. Jenkins, Hugh P. Osborn, S. Seager
Figure caption: Comparison between the observed magnitudes for the three systems and the isochrone-derived magnitudes of the combined binary system (in the case of BD+45 1593) or the primaries (in the case of TYC 2010-124-1 and UCAC4 515-012898). For each filter, we plot filled circles to represent the observed magnitudes and unfilled circles to represent the isochrone-inferred magnitudes. We plot the relative transmission for each filter obtained from the SVO Filter Profile Service (Rodrigo et al. 2012; Rodrigo & Solano 2020) above its photometric pair. There is a discontinuity on the wavelength axis at the top of each plot between the 2MASS magnitudes and AllWISE magnitudes. The Tycho-2 magnitudes for TYC 2010-124-1 are close to the catalog’s limit of reliability (Høg et al. 2000). The B  T  magnitude difference corresponds to 2.1σ, which is unsurprising given the number of comparisons in our sample. However, the V  T  magnitude difference corresponds to 3.2σ, which we attribute to underestimated random uncertainties or systematic uncertainties at the faint end of the Tycho-2 photometric calibration. The consistency and overall small offsets between the observed and isochrone-inferred magnitudes demonstrate that our method of deriving the host stars’ parameters is robust, especially when UV photometry is available.
Paper: Verification of Gaia Data Release 3 Single-lined Spectroscopic Binary Solutions With Three Transiting Low-mass Secondaries
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Keyi Ding, 可怿 丁, Samuel K. Grunblatt, Theron Carmichael, Allyson Bieryla, Joseph E. Rodriguez, Jack Schulte, Noah Vowell, George Zhou, Samuel N. Quinn, Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, David W. Latham, Douglas A. Caldwell, M. M. Fausnaugh, Christina Hedges, Jon M. Jenkins, Hugh P. Osborn, S. Seager
Figure caption: Doppler curves for BD+45 1593, TYC 2010-124-1, and UCAC4 515-012898 based on their Gaia DR3 and ground-based SB1 solutions. We plot 2000 partially transparent blue lines to represent individual solutions sampled from normal distributions of the Gaia Doppler semiamplitude, eccentricity, and argument of periastron, with the standard deviation of each distribution representing the reported error on its respective parameter. Gaia’s reported uncertainties on each parameter are derived from the variance-covariance matrix of the solution, but the matrix itself is not reported; we therefore do not correct for it in this plot. We plot the individual precision ground-based radial velocity measurements and their uncertainties as light blue circles with black borders and error bars. We plot the Doppler curves inferred from these data as dashed black lines. The agreement between the Gaia and precision ground-based SB1 solutions demonstrates the fidelity of the Gaia SB1 solutions at low Doppler semiamplitude.
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: BASTI Models of the the red-giant branches of stellar populations having the same solar abundances but differing in ages, ranging from 6 Gyr (blue points, to the left) up to 14 Gyr (red points, to the right). Note that the color range spanned by these models at the TRGB is very small (0.08 mag) in (V−I) with a trend toward bluer colors and fainter TRGB magnitudes with decreasing age. The full run of color and magnitude with age is shown as a downward slanting arrow in Figure 7 (left and right panels).