adsabs/AstroCLIMB huggingface dataset:
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: The Johnson B photometric data for HD 182735, phased with the 2.07866 day−1 frequency and time of minimum from Table 11.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Least-squares frequency spectra of the HD 210719 Johnson B data set. The arrow in the top panel indicates the single detected frequency of 1.54237 day−1. The bottom panel is the frequency spectrum resulting when the 1.54237 day−1 frequency is fixed. The same frequency was found in the Johnson V data set.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: The Johnson B photometric data for HD 210719, phased with the 1.54237 day−1 frequency and time of minimum from Table 11.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: H-R diagram showing the location of the 9 new γ Dor variables discovered in this paper (filled circles) along with the 64 γ Dor stars previously discovered or confirmed in our APT program (open circles), taken from the list of 73 stars in Table 12. The dotted lines indicate the boundaries of the δ Sct instability strip, converted from those of Breger (2000). The dashed lines show the observed limits of the γ Dor variables taken from Fekel et al. (2003) and unchanged in this paper.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Panel (a): gray points show effective temperature and apparent magnitude mKep of stars observed by Kepler; red points are stars that pass the selection criteria described in Section 2. Panel (b): same as panel (a) but for planet hosts. Panel (c): same as panel (a) but showing Gaia absolute G-band magnitude MG and Bp − Rp color. The boundaries of our main-sequence filter are shown as red dashed lines. Panel (d): same as panel (c) but for planet hosts.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Venn diagram illustrating the number of host stars belonging to various samples described in this paper. CXM: 888 stars in the extended stellar-mass sample described in Section 2 that forms the basis of the exoplanet demographic work described in Sections 6 and 7. DR1: 1305 stars from Petigura et al. (2017). DR2: 411 stars with new spectra presented in this work.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: The black lines show a segment of HIRES spectra containing the Mg I b triplet for seven representative spectra observed by our team to illustrate the spectral resolution R ≥ 60,000 and S/N ≥ 20 pixel−1 (see Section 3). The red lines are SpecMatch-Empirical fits (see Section 4.1).
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Fractional precision of Rp, R⋆, and Rp/R⋆ for the planets in the CXM sample.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Properties of host stars in the filtered CXM sample described in Section 5.2. Panel (a): stellar mass and metallicity. Panel (b): stellar radius and effective temperature. The color scale conveys the isochrone age uncertainty in dex (half the difference between the 84th and 16th percentiles of the age posterior). Panel (c): stellar metallicity and age. Panel (d): stellar mass and age where the color scale is equivalent to panel (b). Several stars have ages exceeding 14 Gyr for reasons we explain in Section 4.2. We discuss correlations between mass, metallicity, and age in Section 6.2.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Panel (a): sizes and orbital periods of detected planets after applying the filters described in Section 5.2. The contours show a Gaussian kernel density estimate (KDE) of the number density of planets in this space. The kernel bandwidth is 0.029 dex in Rp and 0.18 dex in P, as shown by the symbol labeled “bw.” The “uncert” symbol shows the median Rp uncertainty (P uncertainties are smaller than the line width). Panels (b)–(d): same as panel (a), except that the x-axis is Sinc, M⋆, and [Fe/H], and the kernel bandwidths along the horizontal axes are 0.30, 0.061, and 0.1.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Zoomed-in version of Figure 6 highlighting the radius gap, which is visible in all projections. In the M⋆ projection, the typical sub-Neptune becomes larger with M⋆, while the super-Earths remain the same size. The bands are power-law fits of the radius gap (see Section 6.1).
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: The left panels are analogous to Figure 7(a), except we have split the planet sample into three bins of stellar mass. The right panels show the ORD of planets ﹩{df}/d\mathrm{log}P/d\mathrm{log}{R}_{p}﹩. The maximum ORD increases with decreasing M⋆ (note different color scales). Regions of low planet detectability, defined as ntrial < 50, are gray. The typical sub-Neptune size grows with M⋆, while super-Earths have a nearly constant size. The bands show fits to the radius gap.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Same as Figure 8, except the x-axis is incident bolometric flux.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Points show the recovery rate of the Kepler planet detection pipeline of simulated planets injected by Christiansen et al. (2020) as a function of MES. The curve shows the parametric model we used to account for pipeline incompleteness in our occurrence calculations described in Section 7.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Mean size of super-Earths with P < 30 days and sub-Neptunes with P < 100 days. Over M⋆ = 0.5–1.4 M⊙, the average sub-Neptune grows from 2.1 to 2.6 R⊕ with a slope of ﹩\alpha \,=\,d\mathrm{log}{R}_{p}/d\mathrm{log}{M}_{\star }﹩ = 0.23 ± 0.04. The mean super-Earth has a nearly constant size of 1.35 R⊕ with α = −0.01 ± 0.03. Wu (2019) reported α = 0.25 for both populations and is shown by the dashed lines. Our sub-Neptune results are consistent with this index, but our super-Earth results are inconsistent at 8σ.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Panel (a): posterior probability density of the mean number of sub-Neptunes per star f⋆ with P = 1–300 days for three stellar-mass bins. Dashed lines show the 25%, 50%, and 75% quartiles. Panel (b) shows the period breakpoint P0. Panel (c) shows the flux breakpoint Sinc,0. Panels (d)–(f) are the same as panels (a)–(c) but for super-Earths. The mean occurrence in panel (d) corresponds to P = 1–30 days. For both classes of planets, there is a decline in total occurrence with increasing M⋆. For the sub-Neptunes, P0 ranges from ≈7.0 to 9.6 days, consistent to 40%; for the super-Earths, P0 is ≈2.7–5.1 days, consistent to a factor of 2. For the sub-Neptunes, the breakpoint Sinc,0 increases by a factor of 9 from ﹩{27}_{-6}^{+6}﹩ to ﹩{244}_{-55}^{+64}﹩ S⊕ between the low- and high-mass bin. For the super-Earths, the breakpoint also increases with stellar mass from ﹩{89}_{-31}^{+35}﹩ to ﹩{615}_{-152}^{+159}﹩ S⊕, a factor of 7 increase.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Panel (a): period distribution of sub-Neptunes for three bins of stellar mass. The points show the number of planets per star in period bins that are 0.25 dex wide. We modeled the ORD df/dP as a smooth broken power law, which we fit to the unbinned planet population over P = 1–300 days (see Section 7.3). The bands show the credible range of ﹩{df}/d\mathrm{log}P\times 0.25﹩ dex. The height of each curve at a particular P is the number of planets per star within a 0.25 dex period interval centered at P. Panel (b): same as panel (a) except for super-Earths where the fits extend to 30 days. Panels (c) and (d): same as panels (a) and (b) except showing incident flux distribution. The vertical axis has the following interpretation: number of planets per star within a 0.5 dex flux interval.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Panels (a)–(c): period distribution of super-Earths (green) and sub-Neptunes (blue) for different bins of stellar mass. Points and curves are the same as shown in Figure 13 but grouped according to stellar mass as opposed to planet size. The vertical bands show the range of credible period breakpoints P0. For all stellar-mass bins, P0 is smaller for super-Earths than for sub-Neptunes. Panels (d)–(f): same as panels (a)–(c), but the x-axis is incident stellar flux. The flux breakpoint Sinc,0 increases with stellar mass, but the relative offset between the two populations is nearly constant.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Toy model to explore how a correlation between host star mass M⋆ and planet core mass Mc impacts super-Earth and sub-Neptune sizes when photoevaporation drives mass loss. Panels (a)–(c) show the distributions of Mc, envelope fraction fenv, and planet size Rp at the time of disk dispersal (t ∼ 10 Myr). Here low-mass stars have a lower maximum core mass than high-mass stars: for M⋆ ≈ 0.6 M⊙, ﹩{M}_{{\rm{c}},\max ,1}\approx 10\,{M}_{\oplus };﹩ for M⋆ ≈ 1.2 M⊙, ﹩{M}_{{\rm{c}},\max ,2}\approx 20\,{M}_{\oplus }﹩. Planets have a broad distribution of envelope fractions fenv ≈ 0.3%–30% and a broad distribution of sizes. Panels (d)–(f) show the same properties after the period of rapid photoevaporation (t ∼ 100 Myr). Cores up to Mcrit have been stripped bare. We have approximated the time-integrated XUV flux to be independent of M⋆, so Mcrit is also independent of M⋆ (see Section 8.1). Photoevaporation bifurcates the fenv distribution into two modes with fenv ≈ 0% and 3%. The largest super-Earths have ﹩{R}_{\mathrm{crit}}/{R}_{\oplus }\approx {({M}_{\mathrm{crit}}/{M}_{\oplus })}^{0.25}﹩, so Rcrit is independent of M⋆. The smallest sub-Neptunes barely retained their envelopes and have Rp ≈ 2Rcrit. The largest sub-Neptune size is set by an fenv ≈ 3% envelope atop an ﹩{M}_{{\rm{c}},\max }﹩ core or ﹩{R}_{\max }=2{({M}_{{\rm{c}},\max }/{M}_{\oplus })}^{0.25}﹩. Since ﹩{M}_{{\rm{c}},\max }\propto {M}_{\star }﹩, ﹩{R}_{\max }\propto {M}_{\star }^{0.25}﹩. The model is equally applicable to the core-powered framework, except mass is lost over ∼1 Gyr timescales.
Paper: The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
Authors: Erik A. Petigura, James G. Rogers, Howard Isaacson, James E. Owen, Adam L. Kraus, Joshua N. Winn, Mason G. MacDougall, Andrew W. Howard, Benjamin Fulton, Molly R. Kosiarek, Lauren M. Weiss, Aida Behmard, and Sarah Blunt
Figure caption: Panel (a): predicted planet sizes as a function of stellar metallicity in the core-powered models of Gupta & Schlichting (2020). Here M⋆ and age were fixed at 1.0 M⊙ and 3 Gyr. Panel (c): relative number density of detected planets (not occurrence). Panel (e): same as panel (c), except we have normalized the number density by its integral along columns of constant [Fe/H] to accentual features at low/high [Fe/H]. In the Gupta & Schlichting (2020) models, the typical sub-Neptune is expected to grow with metallicity according to Rp ∝ Zβ, with β = 0.1. We observed β = −0.01 ± 0.02 and show the predicted β = 0.1 dependence for comparison in panels (c) and (e). The lack of detectable variation in sub-Neptune size with metallicity when such a trend is predicted in the core-powered models points to missing or incomplete physics, perhaps involving the treatment of envelope opacity (see Section 8.2). Panel (b): same as panel (a) except that M⋆ and [Fe/H] were fixed to 1.0 M⊙ and 0.0 dex, and age was allowed to vary. Panels (d) and (f): same as panels (c) and (e) except for age. The sub-Neptunes are expected to shrink with time according to Rp ∝ tγ, with γ = −0.1. While we observed γ = −0.01 ± 0.03, we could not conclusively rule out a γ = −0.1 dependence given the age uncertainties (see Section 8.3).
Paper: The Solar Neighborhood. XLIX. New Discoveries and Orbits of M-dwarf Multiples with Speckle Interferometry at SOAR
Authors: Eliot Halley Vrijmoet, Andrei Tokovinin, Todd J. Henry, Jennifer G. Winters, Elliott Horch, and Wei-Chun Jao
Figure caption: Venn diagram illustrating the three subsets of the SOAR sample of nearby M dwarfs. The area of each circle is proportional to the number of targets in that subset, but the overlapping regions are not to scale. Each circle is labeled with a reference to the subset’s source: “0.9 m PB” for targets showing perturbations (PBs) in the RECONS astrometry program at the CTIO 0.9 m, “Lit. mult.” for known literature multiples, and “DR2 sus.” for systems suspected to be multiples based on their Gaia DR2 results. The number of targets is given under each subset name, and the numbers in the overlapping sections indicate the number of targets common to multiple subsets.
Paper: The Solar Neighborhood. XLIX. New Discoveries and Orbits of M-dwarf Multiples with Speckle Interferometry at SOAR
Authors: Eliot Halley Vrijmoet, Andrei Tokovinin, Todd J. Henry, Jennifer G. Winters, Elliott Horch, and Wei-Chun Jao
Figure caption: Separation ρ in arcsec and magnitude difference in I band for each observation that resolved a companion, excluding those for which the data were exceptionally noisy (“:” flag in Table 2). The 41 mas formal diffraction limit of SOAR is indicated with the vertical dotted line. This sample is intentionally focused on the closer pairs (≲1.″0) that are more likely to show orbital motion over our 3 yr campaign.
Paper: The Solar Neighborhood. XLIX. New Discoveries and Orbits of M-dwarf Multiples with Speckle Interferometry at SOAR
Authors: Eliot Halley Vrijmoet, Andrei Tokovinin, Todd J. Henry, Jennifer G. Winters, Elliott Horch, and Wei-Chun Jao
Figure caption: Five visual orbits for binaries resolved at SOAR, plus one spectroscopic orbit that was fit simultaneously with the corresponding visual orbit for LHS 501 AC. For the visual orbits, blue lines denote the fit, filled circles are SOAR observations, and open circles are observations added from the literature. Red arrows indicate the direction of motion of the secondary star around the primary, and the black star and dotted line denote the primary star and line of periastron, respectively. In the spectroscopic orbit (bottom right panel), the points and solid line are the observations and fit, respectively, for the primary component, and the open points and dashed line are the observations and fit for the secondary. Left to right, top to bottom: G 131-26 AB, 2MA 0015-1636 AB, LP 993-115 BC, SCR 0533-4257 AB, LHS 501 AC visual orbit, and LHS 501 AC radial velocity orbit (observations from Baroch et al. 2018). Sources for additional visual observations are specified in Table 4.
Paper: Mass Transfer as an Explanation for the Lifetime Travel Time Discrepancy in IT Librae
Authors: Peter Wysocki, Douglas Gies, Katherine Shepard, Kathryn Lester, and Jerome Orosz
Figure caption: Residuals from the linear ephemeris fit of the primary eclipse time vs. Cycle Number (E) for IT Lib.
Paper: Mass Transfer as an Explanation for the Lifetime Travel Time Discrepancy in IT Librae
Authors: Peter Wysocki, Douglas Gies, Katherine Shepard, Kathryn Lester, and Jerome Orosz
Figure caption: Radial-velocity curve for IT Lib. The primary data are shown in black and the secondary data in white.
Paper: Mass Transfer as an Explanation for the Lifetime Travel Time Discrepancy in IT Librae
Authors: Peter Wysocki, Douglas Gies, Katherine Shepard, Kathryn Lester, and Jerome Orosz
Figure caption: Comparison of the Kepler K2 light curve and the model ELC light curve for the best-fit parameters. The Kepler K2 light curve has been binned in phase to ease the comparison between the model and data. Phase zero is the time of primary eclipse. The flux is in units of electrons per second. The bottom section shows the residuals from the fit.
Paper: Mass Transfer as an Explanation for the Lifetime Travel Time Discrepancy in IT Librae
Authors: Peter Wysocki, Douglas Gies, Katherine Shepard, Kathryn Lester, and Jerome Orosz
Figure caption: Reconstructed and model spectra for the wavelength range of 4542−4592 Å. The reconstructed spectra are in pink, and the model spectra are in green, with the primary component being offset to a larger normalized flux. The order showcases the Si III λλ4552, 4567, 4574 absorption features.
Paper: Mass Transfer as an Explanation for the Lifetime Travel Time Discrepancy in IT Librae
Authors: Peter Wysocki, Douglas Gies, Katherine Shepard, Kathryn Lester, and Jerome Orosz
Figure caption: Reconstructed and model spectra for the wavelength range of 4627−4655 Å. The reconstructed spectra are in pink, and the model spectra are in green, with the primary component being offset to a larger normalized flux. The order showcases the N II λλ4630, 4643 and O II λλ4638, 4641, 4649 (plus other weaker blends).
Paper: Mass Transfer as an Explanation for the Lifetime Travel Time Discrepancy in IT Librae
Authors: Peter Wysocki, Douglas Gies, Katherine Shepard, Kathryn Lester, and Jerome Orosz
Figure caption: Reconstructed and model spectra for the wavelength range of 5029−5060 Å. The reconstructed spectra are in pink, and the model spectra are in green, with the primary component being offset to a larger normalized flux. The order showcases the He I λ5047, N II λ5045, S II λ5032, and Si II λλ5041, 5056 absorption features.
Paper: Mass Transfer as an Explanation for the Lifetime Travel Time Discrepancy in IT Librae
Authors: Peter Wysocki, Douglas Gies, Katherine Shepard, Kathryn Lester, and Jerome Orosz
Figure caption: Combined reconstructed and model spectra for the wavelength range of 4815–4910 Å from two adjacent echelle orders. The reconstructed spectra are in black, and the model spectra are in red for the primary and blue for the secondary. This plot showcases the Hβ λ4861 absorption feature. The absorption feature for the secondary may show the impact of infilling due to mass transfer.
Paper: Mass Transfer as an Explanation for the Lifetime Travel Time Discrepancy in IT Librae
Authors: Peter Wysocki, Douglas Gies, Katherine Shepard, Kathryn Lester, and Jerome Orosz
Figure caption: Reconstructed and model spectra for the wavelength range of 6550−6595 Å. The reconstructed spectra are in pink, and the model spectra are in green, with the primary component being offset to a larger normalized flux. The order showcases the Hα λ6563 and C II λλ6578, 6582 absorption features.
Paper: Mass Transfer as an Explanation for the Lifetime Travel Time Discrepancy in IT Librae
Authors: Peter Wysocki, Douglas Gies, Katherine Shepard, Kathryn Lester, and Jerome Orosz
Figure caption: Fit to the observed SED of IT Lib using temperatures derived from the spectral analysis of the component stars.
Paper: Mass Transfer as an Explanation for the Lifetime Travel Time Discrepancy in IT Librae
Authors: Peter Wysocki, Douglas Gies, Katherine Shepard, Kathryn Lester, and Jerome Orosz
Figure caption: An HRD for stars of IT Lib’s primary and secondary masses, 9.6 and 4.18 M⊙. Overlaid on each evolutionary track are the stars’ actual luminosities and temperatures, along with the uncertainty. Notice that the primary and, in particular, the secondary are above the evolutionary track. This suggests that its evolution was altered through binary mass exchange (Section 8).