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Planet bulk density vs. all rocky elements cons...

Planet bulk density vs. all rocky elements considered in our analysis in [X/Fe] form. As...

Aida Behmard et al, The Astronomical Journal 170 5

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[Mg/Fe] vs. [Fe/H] for stars that host our rock...

[Mg/Fe] vs. [Fe/H] for stars that host our rocky planet sample, as well as all main-sequ...

Aida Behmard et al, The Astronomical Journal 170 5

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All small (RP ≤ 1.8 R⊕), rocky planets from the...

All small (RP ≤ 1.8 R⊕), rocky planets from the Exoplanet Archive (J. L. Christiansen et...

Aida Behmard et al, The Astronomical Journal 170 5

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Planet bulk density vs. all rocky elements cons...

Planet bulk density vs. all rocky elements considered in our analysis in [X/H] form. Roc...

Aida Behmard et al, The Astronomical Journal 170 5

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Rocky planet densities vs. host star [Mg/Fe] fo...

Rocky planet densities vs. host star [Mg/Fe] for planets hosted by both FGK (circles) an...

Aida Behmard et al, The Astronomical Journal 170 5

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Uncompressed (blue) and bulk (green) rocky plan...

Uncompressed (blue) and bulk (green) rocky planet densities vs. host star [Mg/Fe] for pl...

Aida Behmard et al, The Astronomical Journal 170 5

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Comparison of the Ca II absorption feature in t...

Comparison of the Ca II absorption feature in the Keck HIRES spectra of WD 0644+025 from...

Sabrina Poulsen et al, The Astronomical Journal 171 3

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Probability distributions for the age, initial ...

Probability distributions for the age, initial mass, and final mass of WD 0644+025 deriv...

Sabrina Poulsen et al, The Astronomical Journal 171 3

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A squared-stretch false-color image of WD 0644+...

A squared-stretch false-color image of WD 0644+025, constructed from F1000W (blue), F150...

Sabrina Poulsen et al, The Astronomical Journal 171 3

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This contrast curve reports the flux ratio of o...

This contrast curve reports the flux ratio of our central aperture relative to the stand...

Sabrina Poulsen et al, The Astronomical Journal 171 3

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Top: the measured SED of WD 0644+025 (black squ...

Top: the measured SED of WD 0644+025 (black squares) compared to a DA cooling model with...

Sabrina Poulsen et al, The Astronomical Journal 171 3

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Orbital distance as a function of companion mas...

Orbital distance as a function of companion mass consistent with the observed mid-infrar...

Sabrina Poulsen et al, The Astronomical Journal 171 3

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Normalized HIRES spectrum (black) with our best...

Normalized HIRES spectrum (black) with our best-fit model (red). The two left panels sho...

Sabrina Poulsen et al, The Astronomical Journal 171 3

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Dust disk models fit to 10 and 15 μm excess det...

Dust disk models fit to 10 and 15 μm excess detections for WD 0644+025. The N. P. Baller...

Sabrina Poulsen et al, The Astronomical Journal 171 3

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Strength of CO2 detections at (a) 1.21 μm, (b) ...

Strength of CO2 detections at (a) 1.21 μm, (b) 1.44 μm, (c) 1.52 μm, and (d) 1.63 μm wit...

Celeste Hagee et al, The Astronomical Journal 171 3

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Illustrates the balancing act of keeping therma...

Illustrates the balancing act of keeping thermal noise minimal while maximizing the dete...

Celeste Hagee et al, The Astronomical Journal 171 3

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Top: required SNR for a strong CO2 detection at...

Top: required SNR for a strong CO2 detection at 1.44 μm (a), 1.52 μm (b), and 1.63 μm (c...

Celeste Hagee et al, The Astronomical Journal 171 3

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Minimum SNR required for a strong CO2 detection...

Minimum SNR required for a strong CO2 detection at each bandpass center for the three hi...

Celeste Hagee et al, The Astronomical Journal 171 3

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CO2 and CO spectral features at varying abundan...

CO2 and CO spectral features at varying abundances from 0.8 to 2.0 μm. It plots waveleng...

Celeste Hagee et al, The Astronomical Journal 171 3

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Detectability strength of (a) Proterozoic-like,...

Detectability strength of (a) Proterozoic-like, (b) Archean-like, and (c) Venus-like CO2...

Celeste Hagee et al, The Astronomical Journal 171 3

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Varying detection strength of CO2 with respect ...

Varying detection strength of CO2 with respect to CO2 abundance (on the x-axis) and SNR ...

Celeste Hagee et al, The Astronomical Journal 171 3

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Strength of CO detections at SNRs of 3, 8, 12, ...

Strength of CO detections at SNRs of 3, 8, 12, 16, and 20 with the highest CO abundance,...

Celeste Hagee et al, The Astronomical Journal 171 3

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Top: required SNR for a strong CO2 detection at...

Top: required SNR for a strong CO2 detection at 1.44 μm (a), 1.52 μm (b), and 1.63 μm (c...

Celeste Hagee et al, The Astronomical Journal 171 3

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Minimum SNR required to achieve a strong CO2 de...

Minimum SNR required to achieve a strong CO2 detection at each bandpass center for four ...

Celeste Hagee et al, The Astronomical Journal 171 3

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TESS observations of TIC 399725538 distributed ...

TESS observations of TIC 399725538 distributed in BJD (top panel) and orbital phase (sec...

Jae Woo Lee et al, The Astronomical Journal 171 3

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