pith. sign in

arxiv: 2605.26142 · v1 · pith:KUKPIAMAnew · submitted 2026-05-22 · 🌌 astro-ph.IM · astro-ph.EP· astro-ph.SR

From Hubble to HWO: Bridging the Frontier of White Dwarf Exoplanet Science

Laura K. Rogers , Siyi Xu , Martin Barstow , Simon Blouin , Amy Bonsor , Andrew M. Buchan , Sarah L. Casewell , Tim Cunningham
show 15 more authors
John Debes Patrick Dufour Boris Gansicke Joseph Guidry Ted von Hippel Mukremin Kilic Erika Le Bourdais Carl Melis Lou Baya Ould Rouis Judith Provencal Melinda Soares-Furtado Andrew Swan Isabella Trierweiler Zachary Vanderbosch Jamie Williams
This is my paper

Pith reviewed 2026-06-30 14:27 UTC · model grok-4.3

classification 🌌 astro-ph.IM astro-ph.EPastro-ph.SR
keywords white dwarfsexoplanet compositionUV spectroscopypolluted white dwarfsHSTHabitable Worlds ObservatoryJWST synergy
0
0 comments X

The pith

Preserving HST's UV spectroscopy through 2035 is required to measure exoplanet compositions from polluted white dwarfs and prepare for JWST and HWO.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

White dwarf stars accrete material from disrupted exoplanets, and up to half show metal lines that reveal the bulk composition of that material. High-resolution UV spectra are needed to detect key volatile elements like C, N, O and rock-forming elements like Fe, Si, Mg that cannot be fully accessed otherwise. HST with COS and STIS is currently the only instrument able to obtain these spectra at the required resolution and sensitivity. The paper argues that continued access to this capability is necessary both to build a statistically useful sample on its own and to provide essential context for infrared observations with JWST and ultraviolet planning for the future Habitable Worlds Observatory. Without it, the link between observed pollution and the interior structure and habitability potential of exoplanetary bodies would remain incomplete through the next decade.

Core claim

High-resolution UV spectra from HST remain the only near-term means to detect the full set of volatile and rock-forming elements in polluted white dwarfs, and continued observations through at least 2035 are required to deliver statistically significant composition measurements, supply critical groundwork for HWO, and create a powerful synergy with JWST data on the same systems.

What carries the argument

High-resolution (R>15,000) UV spectroscopy of photospheric metal lines in polluted white dwarfs, which reveals the elemental abundances of accreted exoplanetary material.

If this is right

  • A statistically significant sample of exoplanetary bulk compositions becomes measurable using only current facilities.
  • JWST mid-infrared observations of the same white dwarfs can be interpreted with complete elemental inventories rather than partial ones.
  • HWO ultraviolet instrument requirements and target selection can be informed by real performance data from HST on the same science case.
  • Habitability studies gain access to volatile-element abundances that are otherwise inaccessible.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If HST UV time is deprioritized, the field would face a multi-year gap in composition data that cannot be filled by ground-based or other space facilities.
  • The same UV data sets could also constrain the timing and efficiency of planetesimal delivery in white dwarf systems, an implication not developed in the paper.
  • Extending the argument to other white dwarf science, such as atmospheric studies of the white dwarfs themselves, would strengthen the case for instrument preservation but is left implicit.

Load-bearing premise

No other facility will be able to deliver the required high-resolution UV spectra of polluted white dwarfs before the mid-2030s.

What would settle it

Detection and publication of a statistically useful sample of polluted white dwarf UV spectra at R>15,000 from any instrument other than HST COS or STIS before 2035.

Figures

Figures reproduced from arXiv: 2605.26142 by Amy Bonsor, Andrew M. Buchan, Andrew Swan, Boris Gansicke, Carl Melis, Erika Le Bourdais, Isabella Trierweiler, Jamie Williams, John Debes, Joseph Guidry, Judith Provencal, Laura K. Rogers, Lou Baya Ould Rouis, Martin Barstow, Melinda Soares-Furtado, Mukremin Kilic, Patrick Dufour, Sarah L. Casewell, Simon Blouin, Siyi Xu, Ted von Hippel, Tim Cunningham, Zachary Vanderbosch.

Figure 1
Figure 1. Figure 1: The logarithmic number ratios of elemental abundances (ordered in increasing volatility/decreasing condensation temperature) relative to Mg for the planetary material accreting onto four white dwarfs, normalized to solar composition (black dashed line at [X/Mg] = 0) for (a) Earth-like material (M. Jura et al. 2015), (b) icy water-rich material (S. Xu et al. 2017), (c) mantle-rich material (L. K. Rogers et … view at source ↗
Figure 2
Figure 2. Figure 2: Number of white dwarfs as a function of GALEX FUV magnitude. The blue histogram represents the existing GALEX detections (R. E. Wall et al. 2023), while the orange distribution highlights the expected UVEX detections from the white dwarf sample (N. P. Gentile Fusillo et al. 2021). The black line marks the magnitude limit of COS/130M at 1310 ˚A, where a signal to noise ratio (SNR) of at least 10 can be obta… view at source ↗
Figure 3
Figure 3. Figure 3: (a) JWST MIRI Spectrum of the disk around GD 362 from W. T. Reach et al. (2025) with a model fit showing the minerals contributing to the emissivity. (b) Comparison of the composition of the planetary material accreting onto the white dwarf with that derived from the disk. (insert, c) HST spectra of GD 362 showing lines from S, Si and Fe from S. Xu et al. (2013). This highlights how HST UV spectroscopy rev… view at source ↗
read the original abstract

White dwarf stars, the endpoint of stellar evolution for 97% of stars in our Milky Way, offer a unique and powerful window into the bulk elemental composition of rocky exoplanetary bodies. Up to 50% of single white dwarfs are observed with photospheric metal lines from accreted exoplanetary bodies (called 'polluted' white dwarfs), and spectroscopic observations reveal the bulk composition of this material. High-resolution (R>15,000) UV spectra are essential for detecting many elements present in the material, such as the volatile elements imperative for habitability studies (C, N, O, P, S) and key rock-forming elements required to constrain interior structure (e.g. Fe, Si, Mg, Al, Ni). HST, through its COS and STIS spectrographs, remains the only facility capable of performing this science in the near future. Looking to the next decade, the scientific case for continued HST UV observations of polluted white dwarfs is compelling on three fronts (i) as a standalone to enable the bulk composition of exoplanetary material to be measured in a statistically significant sample, (ii) as essential groundwork for the Habitable Worlds Observatory (HWO), and (iii) in a powerful synergy with JWST, to enable characterization of the bulk mineralogy and bulk elemental composition of exoplanetary material. This white paper argues that continued UV spectroscopic capabilities with HST is a high-return investment for white dwarf and exoplanet science, and preserving and prioritizing HST's UV capabilities through at least 2035 is crucial to maximize the scientific return from HST, JWST, and HWO.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript is a white paper advocating for continued prioritization of high-resolution (R>15,000) UV spectroscopy with HST/COS and STIS on polluted white dwarfs through at least 2035. It claims that up to 50% of single white dwarfs show photospheric metals from accreted exoplanetary bodies, that UV spectra are required to access volatiles (C, N, O, P, S) and rock-forming elements (Fe, Si, Mg, Al, Ni), and that HST is the only near-term facility capable of this work. The case is made on three fronts: enabling statistically significant standalone samples, providing essential groundwork for HWO, and enabling synergy with JWST for bulk mineralogy and composition.

Significance. If the uniqueness claim is substantiated, the paper would supply a focused advocacy document useful for facility planning and multi-mission coordination in exoplanet and white-dwarf science. It correctly highlights the diagnostic power of UV lines for habitability-related volatiles and interior-structure constraints, drawing on established literature percentages and capabilities. No new quantitative derivations, error budgets, or sample statistics are introduced.

major comments (2)
  1. [Abstract] Abstract: The statement that 'HST, through its COS and STIS spectrographs, remains the only facility capable of performing this science in the near future' is load-bearing for all three advocacy fronts yet is asserted without any comparison of wavelength coverage, resolving power, or sensitivity against other current or approved instruments (ground-based or space-based) through 2035. A dedicated assessment is required to support the timeline and prioritization recommendation.
  2. [Abstract] Abstract (three fronts paragraph): The standalone-sample, HWO-groundwork, and JWST-synergy arguments each presuppose HST exclusivity; without an explicit facility-comparison section or table, the degree to which each front depends specifically on HST (versus partial coverage elsewhere) cannot be evaluated.
minor comments (2)
  1. The abstract would be strengthened by including one or two concrete quantitative examples (e.g., number of elements detected per target or typical S/N achieved) drawn from the cited HST literature.
  2. Consider adding a short table listing the key elements, their diagnostic UV transitions, and the minimum resolution/sensitivity needed; this would make the technical requirements more transparent.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed review and constructive criticism. The comments correctly identify that the uniqueness claim for HST is central to the paper's three advocacy arguments yet is presented without explicit supporting comparisons. We will revise the manuscript by adding a dedicated facility-comparison section and table to substantiate the claims.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The statement that 'HST, through its COS and STIS spectrographs, remains the only facility capable of performing this science in the near future' is load-bearing for all three advocacy fronts yet is asserted without any comparison of wavelength coverage, resolving power, or sensitivity against other current or approved instruments (ground-based or space-based) through 2035. A dedicated assessment is required to support the timeline and prioritization recommendation.

    Authors: We agree that the assertion requires explicit substantiation. In the revised manuscript we will insert a new section (approximately Section 2) that systematically compares HST/COS and STIS capabilities (R > 15 000, wavelength coverage 1150–3200 Å, sensitivity for faint white-dwarf targets) against all relevant ground-based (e.g., VLT/UVES, Keck/HIRES, noting atmospheric cutoff below ~3000 Å and limited access to key volatile lines) and space-based facilities (current or approved) expected to be operational through 2035. The section will quantify why no other platform provides equivalent high-resolution UV access to C, N, O, P, S, Fe, Si, Mg, Al, and Ni lines in the near term, thereby supporting the 2035 timeline. revision: yes

  2. Referee: [Abstract] Abstract (three fronts paragraph): The standalone-sample, HWO-groundwork, and JWST-synergy arguments each presuppose HST exclusivity; without an explicit facility-comparison section or table, the degree to which each front depends specifically on HST (versus partial coverage elsewhere) cannot be evaluated.

    Authors: We concur that the three fronts rest on the exclusivity claim and that the current text does not allow the reader to assess partial alternatives. The new comparison section will explicitly map each front to the comparison results: (i) standalone statistical samples require the full volatile and rock-forming element set accessible only at HST resolution and sensitivity; (ii) HWO groundwork depends on the same UV lines for calibration and target selection; (iii) JWST synergy for mineralogy likewise needs the UV elemental abundances that ground-based or lower-resolution facilities cannot supply. A summary table will tabulate which elements and science cases are lost without HST. revision: yes

Circularity Check

0 steps flagged

No circularity detected in derivation chain

full rationale

The paper asserts that HST/COS/STIS remains the only near-term facility for the required high-resolution UV spectroscopy but presents this as a direct factual premise rather than deriving it from any equations, fitted inputs, self-citations, or prior author work. No self-definitional loops, predictions that reduce to fits, uniqueness theorems imported from self-citations, or ansatzes smuggled via citations appear in the text. The central advocacy claim for HST prioritization through 2035 rests on stated capabilities and synergies without reducing by construction to its own inputs, rendering the argument self-contained.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No mathematical model, free parameters, or new physical entities are introduced; the document relies on established astronomical facts about white dwarf pollution rates and instrument capabilities.

pith-pipeline@v0.9.1-grok · 5934 in / 1070 out tokens · 24406 ms · 2026-06-30T14:27:09.253337+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

45 extracted references · 43 canonical work pages

  1. [1]

    P., Hollands, M

    Bhattacharjee, S., Vanderbosch, Z. P., Hollands, M. A., et al. 2025, arXiv e-prints, arXiv:2502.05502, doi: 10.48550/arXiv.2502.05502

    work page doi:10.48550/arxiv.2502.05502 2025

  2. [2]

    J., Hollands, M., et al

    Bonsor, A., Carter, P. J., Hollands, M., et al. 2020, MNRAS, 492, 2683, doi: 10.1093/mnras/stz3603

    work page doi:10.1093/mnras/stz3603 2020

  3. [3]

    M., Bonsor, A., Rogers, L

    Buchan, A. M., Bonsor, A., Rogers, L. K., et al. 2024, MNRAS, 532, 2705, doi: 10.1093/mnras/stae1608

    work page doi:10.1093/mnras/stae1608 2024

  4. [4]

    M., Bonsor, A., Shorttle, O., et al

    Buchan, A. M., Bonsor, A., Shorttle, O., et al. 2022, MNRAS, 510, 3512, doi: 10.1093/mnras/stab3624

    work page doi:10.1093/mnras/stab3624 2022

  5. [5]

    2019, The Messenger, 175, 30, doi: 10.18727/0722-6691/5122 Cˆ ot´ e, P., Woods, T

    Chiappini, C., Minchev, I., Starkenburg, E., et al. 2019, The Messenger, 175, 30, doi: 10.18727/0722-6691/5122 Cˆ ot´ e, P., Woods, T. E., Hutchings, J. B., et al. 2025, Journal of Astronomical Telescopes, Instruments, and Systems, 11, 042202, doi: 10.1117/1.JATIS.11.4.042202

    work page doi:10.18727/0722-6691/5122 2019

  6. [6]

    E., Klein, B

    Doyle, A. E., Klein, B. L., Dufour, P., et al. 2023, ApJ, 950, 93, doi: 10.3847/1538-4357/acbd44 Dr¸ a˙ zkowska, J. 2026, A&A, 709, A36, doi: 10.1051/0004-6361/202659169

    work page doi:10.3847/1538-4357/acbd44 2023

  7. [7]

    S., G¨ ansicke, B

    Farihi, J., Brinkworth, C. S., G¨ ansicke, B. T., et al. 2011, ApJL, 728, L8, doi: 10.1088/2041-8205/728/1/L8

    work page doi:10.1088/2041-8205/728/1/l8 2011

  8. [8]

    Farihi, J., Su, K. Y. L., Melis, C., et al. 2025, arXiv e-prints, arXiv:2501.18338, doi: 10.48550/arXiv.2501.18338

    work page doi:10.48550/arxiv.2501.18338 2025

  9. [9]

    T., Melis, C., et al

    Farihi, J., Noor, H. T., Melis, C., et al. 2026, MNRAS, doi: 10.1093/mnras/stag176 G¨ ansicke, B. T., Koester, D., Farihi, J., et al. 2012, MNRAS, 424, 333, doi: 10.1111/j.1365-2966.2012.21201.x Gentile Fusillo, N. P., Tremblay, P.-E., Cukanovaite, E., et al. 2021, MNRAS, 508, 3877, doi: 10.1093/mnras/stab2672

    work page doi:10.1093/mnras/stag176 2026

  10. [10]

    R., Timmes, F

    Hinkel, N. R., Timmes, F. X., Young, P. A., Pagano, M. D., & Turnbull, M. C. 2014, AJ, 148, 54, doi: 10.1088/0004-6256/148/3/54

    work page doi:10.1088/0004-6256/148/3/54 2014

  11. [11]

    C., Dalton, G

    Jin, S., Trager, S. C., Dalton, G. B., et al. 2024, MNRAS, 530, 2688, doi: 10.1093/mnras/stad557

    work page doi:10.1093/mnras/stad557 2024

  12. [12]

    2003, ApJL, 584, L91, doi: 10.1086/374036

    Jura, M. 2003, ApJL, 584, L91, doi: 10.1086/374036

    work page doi:10.1086/374036 2003

  13. [13]

    2015, ApJ, 799, 109, doi: 10.1088/0004-637X/799/1/109

    Jura, M., Dufour, P., Xu, S., et al. 2015, ApJ, 799, 109, doi: 10.1088/0004-637X/799/1/109

    work page doi:10.1088/0004-637x/799/1/109 2015

  14. [14]

    2009, AJ, 137, 3191, doi: 10.1088/0004-6256/137/2/3191

    Jura, M., Farihi, J., & Zuckerman, B. 2009, AJ, 137, 3191, doi: 10.1088/0004-6256/137/2/3191

    work page doi:10.1088/0004-6256/137/2/3191 2009

  15. [15]

    A., Plank, T., Newman, S., et al

    Kelley, K. A., Plank, T., Newman, S., et al. 2010, Journal of Petrology, 51, 1711, doi: 10.1093/petrology/egq036

    work page doi:10.1093/petrology/egq036 2010

  16. [16]

    T., & Farihi, J

    Koester, D., G¨ ansicke, B. T., & Farihi, J. 2014, A&A, 566, A34, doi: 10.1051/0004-6361/201423691

    work page doi:10.1051/0004-6361/201423691 2014

  17. [17]

    arXiv e-prints , keywords =

    Kulkarni, S. R., Harrison, F. A., Grefenstette, B. W., et al. 2021, arXiv e-prints, arXiv:2111.15608, doi: 10.48550/arXiv.2111.15608

    work page doi:10.48550/arxiv.2111.15608 2021

  18. [18]

    2021, ApJ, 920, 156, doi: 10.3847/1538-4357/ac1354

    Lai, S., Dennihy, E., Xu, S., et al. 2021, ApJ, 920, 156, doi: 10.3847/1538-4357/ac1354

    work page doi:10.3847/1538-4357/ac1354 2021

  19. [19]

    , keywords =

    Lodders, K., Bergemann, M., & Palme, H. 2025, SSRv, 221, 23, doi: 10.1007/s11214-025-01146-w

    work page doi:10.1007/s11214-025-01146-w 2025

  20. [20]

    Lodders, K., Palme, H., & Gail, H. P. 2009, Landolt Börnstein, 4B, 712, doi: 10.1007/978-3-540-88055-4 34

    work page doi:10.1007/978-3-540-88055-4 2009

  21. [21]

    McDonough, W. F. 2003, Treatise on Geochemistry, 2, 568, doi: 10.1016/B0-08-043751-6/02015-6

    work page doi:10.1016/b0-08-043751-6/02015-6 2003

  22. [22]

    T., Farihi, J., Kenyon, S

    Noor, H. T., Farihi, J., Kenyon, S. J., et al. 2025, MNRAS, 543, 1602, doi: 10.1093/mnras/staf1380

    work page doi:10.1093/mnras/staf1380 2025

  23. [23]

    2026, ApJ, 997, 358, doi: 10.3847/1538-4357/ae2c7d Ould Rouis, L

    Okuya, A., Okuzumi, S., Takigawa, A., & Enomoto, H. 2026, ApJ, 997, 358, doi: 10.3847/1538-4357/ae2c7d Ould Rouis, L. B., Hermes, J. J., G¨ ansicke, B. T., et al. 2024, ApJ, 976, 156, doi: 10.3847/1538-4357/ad86bb

    work page doi:10.3847/1538-4357/ae2c7d 2026

  24. [24]

    T., Kuchner, M

    Reach, W. T., Kuchner, M. J., von Hippel, T., et al. 2005, ApJL, 635, L161, doi: 10.1086/499561

    work page doi:10.1086/499561 2005

  25. [25]

    T., Lisse, C., von Hippel, T., & Mullally, F

    Reach, W. T., Lisse, C., von Hippel, T., & Mullally, F. 2009, ApJ, 693, 697, doi: 10.1088/0004-637X/693/1/697

    work page doi:10.1088/0004-637x/693/1/697 2009

  26. [26]

    T., Kilic, M., Lisse, C

    Reach, W. T., Kilic, M., Lisse, C. M., et al. 2025, ApJ, 994, 195, doi: 10.3847/1538-4357/ae11a9

    work page doi:10.3847/1538-4357/ae11a9 2025

  27. [27]

    K., Bonsor, A., Xu, S., et al

    Rogers, L. K., Bonsor, A., Xu, S., et al. 2024a, MNRAS, 527, 6038, doi: 10.1093/mnras/stad3557

    work page doi:10.1093/mnras/stad3557

  28. [28]

    K., Bonsor, A., Xu, S., et al

    Rogers, L. K., Bonsor, A., Xu, S., et al. 2024b, MNRAS, 532, 3866, doi: 10.1093/mnras/stae1520

    work page doi:10.1093/mnras/stae1520

  29. [29]

    K., Bonsor, A., Le Bourdais, ´E., et al

    Rogers, L. K., Bonsor, A., Le Bourdais, ´E., et al. 2025, MNRAS, 542, 293, doi: 10.1093/mnras/staf1221

    work page doi:10.1093/mnras/staf1221 2025

  30. [30]

    T., Williams, J

    Sahu, S., G¨ ansicke, B. T., Williams, J. T., et al. 2025, MNRAS, 543, 223, doi: 10.1093/mnras/staf1424 SDSS Collaboration, Adamane Pallathadka, G.,

    work page doi:10.1093/mnras/staf1424 2025

  31. [31]

    2025, arXiv e-prints, arXiv:2507.07093, doi: 10.48550/arXiv.2507.07093

    Aghakhanloo, M., et al. 2025, arXiv e-prints, arXiv:2507.07093, doi: 10.48550/arXiv.2507.07093

    work page doi:10.48550/arxiv.2507.07093 2025

  32. [32]

    Swan, A., Gaensicke, B., Izquierdo, P., & et al. 2026,

    2026

  33. [33]

    L., Doyle, A

    Trierweiler, I. L., Doyle, A. E., & Young, E. D. 2023, The Planetary Science Journal, 4, 136, doi: 10.3847/PSJ/acdef3

    work page doi:10.3847/psj/acdef3 2023

  34. [34]

    L., Melis, C., Le Bourdais, ´E., et al

    Trierweiler, I. L., Melis, C., Le Bourdais, ´E., et al. 2025, ApJ, 993, 53, doi: 10.3847/1538-4357/ae003d

    work page doi:10.3847/1538-4357/ae003d 2025

  35. [35]

    A., Rappaport, S., et al

    Vanderburg, A., Johnson, J. A., Rappaport, S., et al. 2015, Nature, 526, 546, doi: 10.1038/nature15527

    work page doi:10.1038/nature15527 2015

  36. [36]

    E., Kilic, M., Bergeron, P., & Leiphart, N

    Wall, R. E., Kilic, M., Bergeron, P., & Leiphart, N. D. 2023, MNRAS, 523, 4067, doi: 10.1093/mnras/stad1699

    work page doi:10.1093/mnras/stad1699 2023

  37. [37]

    T., G¨ ansicke, B

    Williams, J. T., G¨ ansicke, B. T., Sahu, S., et al. 2025, MNRAS, 541, 1377, doi: 10.1093/mnras/staf1034

    work page doi:10.1093/mnras/staf1034 2025

  38. [38]

    J., G¨ ansicke, B

    Wilson, D. J., G¨ ansicke, B. T., Koester, D., et al. 2014, MNRAS, 445, 1878, doi: 10.1093/mnras/stu1876

    work page doi:10.1093/mnras/stu1876 2014

  39. [39]

    L., & Dufour, P

    Xu, S., Barstow, M., Buchan, A., Bourdais, E. L., & Dufour, P. 2026, in Astronomical Society of the Pacific Conference

    2026

  40. [40]

    542, Astronomical Society of the Pacific Conference Series, ed

    Series, Vol. 542, Astronomical Society of the Pacific Conference Series, ed. J. C. Lee, J. Noviello, S. LaMassa, & M. Postman, 61, doi: 10.26624/GRGT3979

    work page doi:10.26624/grgt3979

  41. [41]

    2013, ApJ, 766, 132, doi: 10.1088/0004-637X/766/2/132 7

    Xu, S., Jura, M., Klein, B., Koester, D., & Zuckerman, B. 2013, ApJ, 766, 132, doi: 10.1088/0004-637X/766/2/132 7

    work page doi:10.1088/0004-637x/766/2/132 2013

  42. [42]

    K., & Blouin, S

    Xu, S., Rogers, L. K., & Blouin, S. 2024, arXiv e-prints, arXiv:2404.15425, doi: 10.48550/arXiv.2404.15425

    work page doi:10.48550/arxiv.2404.15425 2024

  43. [43]

    2017, ApJL, 836, L7, doi: 10.3847/2041-8213/836/1/L7

    Xu, S., Zuckerman, B., Dufour, P., et al. 2017, ApJL, 836, L7, doi: 10.3847/2041-8213/836/1/L7

    work page doi:10.3847/2041-8213/836/1/l7 2017

  44. [44]

    Xu, S., Su, K. Y. L., Rogers, L. K., et al. 2018, ApJ, 866, 108, doi: 10.3847/1538-4357/aadcfe

    work page doi:10.3847/1538-4357/aadcfe 2018

  45. [45]

    N., & H¨ unsch, M

    Zuckerman, B., Koester, D., Reid, I. N., & H¨ unsch, M. 2003, ApJ, 596, 477, doi: 10.1086/377492 All Authors and Affiliations Lead Authors: Laura K. Rogers ,1,∗ Siyi Xu (许偲艺) ,1 Co-authors: Martin Barstow ,2 Simon Blouin ,3 Amy Bonsor ,4 Andrew M. Buchan ,5 Sarah L. Casewell ,2 Tim Cunningham ,6 John Debes ,7 Patrick Dufour ,8, 9, 10 Boris G¨ansicke ,5 Jo...

    work page doi:10.1086/377492 2003