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REVIEW 5 major objections 4 minor 84 references

Optical constraints on the coldest metal-poor population

T0 review · 5 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read The paper claims that the $z_{\rm PS1}-W1$ colour separates the coldest metal-poor brown dwarfs from solar-metallicity ones, and that adding $W1-W2$ lifts the temperature-metallicity degeneracy.

desk verdict A useful, careful dataset that doubles the optical sample of metal-poor T dwarfs and adds three parallaxes; the metallicity-colour claim is plausible, but the Y-dwarf extension rests on one non-independent pair and the abstract overstates the model failure. read the letter →

arxiv 2412.04393 v2 pith:R5XMHFSK submitted 2024-12-05 astro-ph.SR astro-ph.GA

Jerry Jun-Yan Zhang , Nicolas Lodieu , Eduardo L. Martín , María Rosa Zapatero Osorio , Victor J. S. Béjar , Valentin D. Ivanov , Henri M. J. Boffin , Tariq Shahbaz
show 5 more authors
Yakiv V. Pavlenko Rafael Rebolo Bartosz Gauza Nafise Sedighi Carlos Quezada
This is my paper · ORCID
classification astro-ph.SRastro-ph.GA
keywords TsubdwarfsYdwarfsmetal-poorbrowntrigonometricparallaxesopticalphotometryz_PS1-W1colourmetallicityindicatorultracoolatmospheres
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper tries to establish that the optical-to-infrared colour $z_{\rm PS1}-W1$, read together with the infrared colour $W1-W2$, can identify the coldest metal-poor brown dwarfs—T and Y subdwarfs—and separate their low metallicities from their temperatures. The authors double the sample of T subdwarfs with optical photometry from 12 to 24, add new trigonometric parallaxes for five candidates, and place the only known metal-poor Y dwarf candidate, the Accident, under five-band optical limits. They report that $z_{\rm PS1}-W1$ shifts redward as metallicity decreases for a fixed temperature, a trend the current atmosphere models do not reproduce. If the trend holds, this colour becomes a practical filter for finding these ancient, pristine objects in existing and upcoming deep surveys.

What carries the argument

The load-bearing object is the colour $z_{\rm PS1}-W1$, the difference between Pan-STARRS $z_{\rm PS1}$ and WISE W1 photometry, used as a metallicity indicator for the coldest substellar objects. It is combined with $W1-W2$ in colour-colour diagrams, where the two axes separate temperature (through the infrared slope) from metallicity (through the redward shift of the optical-infrared colour). The argument is carried by the doubled, homogenised sample of metal-poor T dwarfs, by new trigonometric parallaxes and benchmark companions (Wolf 1130C, Ross 19B) with spectroscopically known metallicities, and by isothermal tracks of the LOWZ and SONORA atmosphere models.

What would settle it

Obtain direct metallicities from near-infrared spectra of W0505, W0738, and the Accident; if any object with measured near-solar [Fe/H] still shows $z_{\rm PS1}-W1 \gtrsim 8$ mag, or a metal-poor object with [Fe/H] $\approx -0.5$ shows a colour near 6 mag, the claimed monotonic reddening trend in Fig. 5 is falsified.

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Extended reading notes

Core claim

The central claim is that $z_{\rm PS1}-W1$, combined with $W1-W2$, breaks the metallicity-temperature degeneracy for T dwarfs and plausibly for Y dwarfs. In the enlarged sample of 24 T subdwarfs, objects with $z_{\rm PS1}-W1 \gtrsim 6$ mag are all extreme subdwarfs ([Fe/H] $\lesssim -1.0$ dex) across spectral types T0 to T8, while solar-metallicity T dwarfs stay between about 4.5 and 5.5 mag. The Accident, the only potential metal-poor Y dwarf, has the reddest $z_{\rm PS1}-W1$ colour in the sample and is subluminous relative to the current Y-dwarf limit, consistent with a cold, very low-metallicity atmosphere. The paper confirms three more T subdwarfs (Wolf 1130C, W1553, W2217) and proposes Ross 19B and W0156 as Y subdwarf candidates. Neither the LOWZ nor the SONORA model grid predicts the observed reddening, which the authors attribute to underestimated suppression of the $z$-band flux by pressure-broadened alkali lines in dense, metal-poor atmospheres.

Load-bearing premise

The load-bearing premise is that the metallicities assigned in Table 7 are correct: for most of the 24 objects, [Fe/H] is not measured on the object itself but adopted from a subdwarf subclass, from the primary star in a binary, or from infrared colour loci.

Editorial extensions

If this is right

  • If the $z_{\rm PS1}-W1$ colour is a reliable metallicity indicator, the coldest metal-poor population can be found photometrically in large-area surveys without spectroscopy of every candidate.
  • Objects with $z_{\rm PS1}-W1 \gtrsim 6$ mag should be prioritised as extreme subdwarf candidates ([Fe/H] $\leq -1.0$ dex) across spectral types T0 to T8.
  • Ross 19B and W0156, if confirmed as Y subdwarfs, would extend the proposed colour-metallicity relation into the coldest regime.
  • The new trigonometric parallaxes for W0422, W1553, and W2217 give the distances needed to place these objects on colour-magnitude sequences and test subluminosity.
  • The Accident's non-detection in five optical bands sets a 3-$\sigma$ upper limit that future models of cold, metal-poor Y atmospheres must reproduce.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the colour-metallicity relation is as steep as reported, surveys could rank brown-dwarf candidates by metallicity before any spectroscopy, turning the subdwarf class label into a quantitative colour scale.
  • The model-data gap points to pressure-broadened alkali opacity (Na I, K I) being underestimated in high-gravity, metal-poor atmospheres; recomputing synthetic $z$-band fluxes with updated line profiles is a direct test.
  • Ross 19B and W0156 may be a common-origin pair, but the paper notes the 9,900 au separation makes survival unlikely; a radial-velocity or abundance check on the primary could decide whether the two share a birth environment.
  • A falsifiable extension would be to measure $z_{\rm PS1}-W1$ for solar-metallicity Y dwarfs with better photometry; if any is as red as the Accident, the shift would be temperature-driven rather than metallicity-driven.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

5 major / 4 minor

Summary. The paper presents new deep optical observations and astrometry for a sample of metal-poor T and Y dwarf candidates. The authors solve trigonometric parallaxes for five T subdwarf candidates using two years of Omega2000 imaging, obtain z-band photometry for twelve additional candidates with GTC, VLT, and DES, and place deep upper limits on the only known metal-poor Y dwarf candidate, the Accident, in five optical bands. They compare the sample with field sequences and LOWZ/SONORA model atmospheres in colour-magnitude and colour-colour diagrams, confirm three new T subdwarfs (Wolf 1130C, W1553, W2217), propose Ross 19B and W0156 as possible Y subdwarf candidates, and argue that the z_PS1 - W1 colour, combined with W1 - W2, can break the metallicity-temperature degeneracy for T and possibly Y dwarfs, with a redward shift at lower metallicity that models do not fully reproduce.

Significance. If the metallicity-colour trend is real, the paper provides a practical photometric metallicity indicator for the coldest metal-poor population, with immediate applications to wide-area optical and infrared surveys such as Euclid, LSST, and Roman. The observational dataset is valuable: three new parallaxes, twelve new z-band detections, and deep five-band limits on the Accident substantially enlarge the small sample of T subdwarfs with optical photometry, and the benchmark comparison objects (Wolf 1130C, Ross 19B, W1810) are well chosen. The paper is honest about many caveats, including the unconfirmed nature of the classification scheme for T subdwarfs and the contamination issues affecting some photometry. However, the headline claim rests heavily on adopted metallicity ranges rather than direct measurements, and one of the two proposed Y subdwarf anchors (W0156) has a metallicity assigned from the same colour locus that is being tested; these issues need to be addressed before the trend can be considered established.

major comments (5)
  1. [Section 3.3, Table 7, Fig. 5] The central metallicity-colour trend in Fig. 5 is calibrated against adopted [Fe/H] ranges rather than measured abundances for 20 of the 24 objects. Because the sd/esd/usd subclass assignments used to set many of these ranges are themselves derived from the same IR colour-colour loci (e.g., Meisner et al. 2023c) that define the sample selection, the monotonic reddening in Fig. 5 may partly reflect the classification scheme rather than a physical metallicity effect. Please add a robustness test: restrict the left panel to objects with metallicity from spectra or primaries (W0004, W0301, W1019, W1553, W1810, Wolf 1130C, Ross 19B, W0711) and show whether the trend persists; alternatively, re-derive the trend using broad metallicity bins with a Monte Carlo propagation of the subclass-to-[Fe/H] mapping. This is required for the abstract's claim that the colour 'shifts redward when metallicity decreases.'
  2. [Section 3.3, Fig. 5] W0156's adopted metallicity (-0.28 to -0.52 dex) is assigned solely because it lies adjacent to Ross 19B and the LOWZ -0.5 dex track in colour space (Meisner et al. 2023c), and the paper itself notes that 'it is not surprising that W0156 aligns with Ross 19B as an outlier.' Plotting W0156 in both panels of Fig. 5 and using it as a proposed Y subdwarf candidate is therefore circular. Remove W0156 from the right panel, or clearly flag it as a non-independent point, and explicitly state how the Y-dwarf extension of the trend is supported by the remaining objects (Ross 19B plus the Accident's limit).
  3. [Section 3.3, Table 7] Ross 19B's metallicity is inherited from Ross 19A across a 9900 au projected separation, and the paper itself argues that the system is dynamically fragile at its age given a total mass of only 0.4 M_sun. If the system is a chance alignment rather than a bound binary, the adopted [Fe/H] is invalid and Ross 19B does not anchor the Y-dwarf panel. Please add a quantitative chance-alignment estimate using local densities of M subdwarfs and late-T/Y dwarfs or, failing that, show the right panel of Fig. 5 with Ross 19B removed and discuss how the claim is weakened.
  4. [Section 2.1.3, Table 3, Fig. 1] W0422's astrometric solution has chi^2_nu = 4.21, much worse than the other four targets, and the paper calls it 'rather poor,' yet W0422 is used in the colour-magnitude diagrams to argue for a 'possible colder nature' or 'probable slightly low metallicity.' With a 24 mas parallax uncertainty, the absolute magnitude is uncertain by roughly a magnitude; either propagate this uncertainty visibly in Fig. 1 or exclude W0422 from the subdwarf-confirmation statements until better astrometry is available.
  5. [Abstract and Section 3.3] The claim that the z_PS1 - W1 reddening is 'not predicted by models' is stronger than the analysis supports. The LOWZ models do predict a redward shift for objects cooler than about 900 K; what fails is the quantitative extent, since the observed colours are redder than the 500-K track by 1-2 mag. The abstract should say 'not fully predicted' or 'under-predicted,' matching the more careful wording used in the body of Section 3.3.
minor comments (4)
  1. [Section 3.4] The z_PS1 - W1 values quoted for W0505 and W0738 (8.01 and 8.45 mag) appear to be swapped relative to Table 6, where W0505 gives 26.09 - 17.64 = 8.45 mag and W0738 gives 25.23 - 17.22 = 8.01 mag. Please correct the text.
  2. [Abstract and Section 3.4] The statement that 'The Accident has the reddest z_PS1 - W1 colour among our sample' should be phrased as the reddest limit, since the object is not detected in the optical bands and its lower limit is comparable to the measured colour of W0505.
  3. [Section 2.2.5] For the three objects measured with both aperture and PSF photometry (W0523, W1019, W2014), please report the consistency check explicitly (e.g., the magnitude differences) so the reader can judge the effect of crowding on the final values.
  4. [Figure 5 caption] The caption describes the isothermal curves as 'orange,' but the curves in the figure are not clearly distinguishable from the LOWZ model tracks; please use a distinct colour or line style and call it out in the legend.

Circularity Check

3 steps flagged · score 5.0 of 10

Y-dwarf extension of the z_PS1-W1 metallicity trend is partly self-defined: W0156's [Fe/H] is set by its IR colour locus, and the two outliers are reclassified to anchor the Y panel.

  1. self definitional [Section 3.3, paragraph introducing Fig. 5 outliers; right panel of Fig. 5]
    "Since the metallicity of W0156 was constrained by Ross 19B (Meisner et al. 2023c), it is not surprising that W0156 aligns with Ross 19B as an outlier."

    The same section states: 'Meisner et al. (2023c) assigned W0156 a metallicity between -0.4 to -0.5 dex because of the adjacent locus to the Ross 19B and the LOWZ model track of -0.5 dex in the colour space. We adopted the same metallicity as that of Ross 19B.' Thus W0156's [Fe/H] was set by its IR colour proximity to Ross 19B and to a LOWZ isometallicity track. The paper then places Ross 19B and W0156 in the right panel of Fig. 5 and reads their location as evidence that z_PS1-W1 traces metallicity for Y dwarfs. The alignment of W0156 with Ross 19B in that panel is guaranteed by the colour-space assignment, so this data point cannot independently support the claimed Y-dwarf metallicity indicator.

  2. fitted input called prediction [Section 3.3, opening paragraph; Table 7]
    "With the exception of Wolf 1130C and Ross 19B, which have spectroscopically determined metallicities derived from their M dwarf primaries, the metallicities of the remaining objects are estimated based on metallicity subclass classifications obtained through spectroscopy or photometry. This classification of subdwarfs has been a long debated topic and it has not been fully established for T subdwarfs yet because of lack of objects across the whole spectral type range."

    For most of the 24 objects the [Fe/H] value is not measured but imported from sd/esd/usd labels, and several of those labels are assigned from IR colours (e.g., W0505 is 'an extreme T subdwarf based on its infrared colours'; W0738 and W2217 from 'similar colours to the two known extreme T subdwarfs'). The z_PS1-W1 axis of Fig. 5 includes W1, the same band used in the IR colour-colour loci that set the metallicity axis, so the monotonic reddening with 'decreasing metallicity' is in part a correlation between z_PS1-W1 and an IR-colour-derived label sharing the W1 band. The paper's own caveat that the subclass system 'has not been fully established for T subdwarfs yet' concedes that the input scale is uncalibrated.

1 more flagged steps
  1. other [Section 3.3, 'We identify Ross 19B and W0156 as two outliers' paragraph; right panel of Fig. 5]
    "Ignoring the possibility of wrong photometry, in the colour-magnitude diagrams, Ross 19B appears extremely subluminous compared to solar-metallicity T dwarf counterparts. It would likely be a colder object, a Y subdwarf, sharing the same chemical component with the primary."

    Ross 19B has an assigned metallicity of only about -0.4 dex yet a z_PS1-W1 colour as red as extreme subdwarfs, which contradicts the T-dwarf trend. Rather than treating this as a counterexample, the paper reclassifies Ross 19B (and W0156) as Y subdwarf candidates and moves them to the right panel of Fig. 5, where their colours are then said to be consistent with their mildly low metallicities. The Y-dwarf extension is therefore built from the two reclassified outliers plus the Accident's upper limit, with no independent Y-subdwarf metallicity calibration; the re-labelling prevents the outliers from falsifying the relation.

full rationale

The new optical photometry, limiting magnitudes, and trigonometric parallaxes are genuine independent measurements, and the T-dwarf portion of the z_PS1-W1 metallicity relation does have support from several objects with NIR spectra and from the benchmark Wolf 1130C/Ross 19A metallicities. However, the headline extension to Y dwarfs is not self-contained. The only two objects used to anchor the right panel of Fig. 5 are Ross 19B, whose metallicity is inherited from a 9900-au primary and whose Y classification is inferred from the same subluminosity/colour being explained, and W0156, whose metallicity was assigned from its IR colour adjacency to Ross 19B and a LOWZ track, as the paper itself concedes. The T-dwarf trend is also weakened by the fact that most [Fe/H] values in Table 7 are subclass-based estimates rather than measured abundances, with the paper warning that the subclass system has not been fully established for T subdwarfs. Because the central T-dwarf claim retains independent content but the Y-dwarf extension is partly defined into existence and the two strongest outliers are reclassified rather than tested, the circularity score is 5 rather than 0 or 10.

Assumptions & free parameters 2 free parameters · 6 assumptions · 0 invented entities

The central claim rests on adopted metallicities and on the choice of model parameters for the comparison grids, rather than on new physical entities. The paper itself flags most of these assumptions, but they are load-bearing: changing the metallicity scale or the model parameters would change the strength of the claimed trend and the claimed model failure.

free parameters (2)
  • Adopted metallicity ranges (Table 7) = various; e.g., W0422: -0.3 to -1.7 dex, W0738: -0.5 to -2.0 dex
    For 15 of 24 objects, [Fe/H] is assigned from subdwarf class (sd, esd, usd) or from a companion star, not measured for the object itself. These assignments set the horizontal axis of Fig. 5, on which the claimed z_PS1 - W1 metallicity trend is based.
  • Model parameters for comparison curves = log g = 5.0, log10 Kzz = 2, C/O = 0.55
    The LOWZ and SONORA model tracks are evaluated at fixed gravity, mixing, and C/O. The conclusion that models under-predict the red optical colours depends on this choice; other parameter combinations might reproduce the data.
assumptions (6)
  • domain assumption All components of a multiple system have a similar chemical composition.
    Used in Section 3.3 to transfer the metallicity of Wolf 1130A to Wolf 1130C and Ross 19A to Ross 19B; the latter transfer is explicitly questioned later in the paper.
  • domain assumption Subdwarf classes map to fixed metallicity intervals (sd: -0.3 to -1.0 dex, esd: -1.0 to -1.7 dex, usd: below -1.7 dex).
    Section 3.3 uses this mapping to assign [Fe/H] ranges to every object lacking a direct measurement; the paper notes this classification is not established for T subdwarfs.
  • domain assumption Relative-to-absolute parallax correction is negligible because reference sources have Gaia parallaxes near 1 mas.
    Section 2.1.3; no correction was applied, and the argument rests on the reference-field statistics.
  • domain assumption The Omega2000 pixel scale derived for W1810 (449.45 mas/pix) applies to all five target fields.
    Section 2.1.3; the adopted scale converts pixel offsets to milliarcseconds for the new parallaxes.
  • domain assumption The z' to z_PS1 filter transformations computed from T dwarf standards and Y dwarf models are valid for metal-poor subdwarfs.
    Section 2.2.5; the model/standard corrections are applied to all objects; if subdwarf spectra differ, the z_PS1 - W1 colours are systematically shifted.
  • domain assumption Fixed model parameters log g = 5.0, log10 Kzz = 2, and solar C/O = 0.55 are representative for these objects.
    Section 3.2; both LOWZ and SONORA comparison grids are evaluated at one point in parameter space, and the conclusion that models cannot produce the red colour relies on this.

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Pith. "Pith review of Optical constraints on the coldest metal-poor population." pith.science (2026). https://pith.science/paper/R5XMHFSK

@misc{pith2026241204393,
  author       = {Pith},
  title        = {Pith review of: Optical constraints on the coldest metal-poor population},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/R5XMHFSK}},
  note         = {Machine review of arXiv:2412.04393}
}
abstract

The coldest metal-poor population made of T and Y dwarfs are archaeological tracers of our Galaxy because they are very old and have kept the pristine material. The optical properties of these objects are important to characterise their atmospheric properties. We aim at characterising further the optical properties of ultracool metal-poor population with deep far-red optical images and parallax determinations. With a two-year baseline, we solved trigonometric parallaxes of the five metal-poor T dwarf candidates using Calar-Alto 3.5-m telescope. We obtained $z'$-band photometry for the other 12 metal-poor T dwarf candidates using 10.4-m Gran Telescopio Canarias, the 8.2-m European Southern Observatory Very Large Telescope, and the Dark Energy Survey, increasing the sample of T subdwarfs with optical photometry from 12 to 24. We report a 3-$\sigma$ limit for the only potential metal-poor Y dwarf, a.k.a., the Accident in five optical bands using the Gran Telescopio Canarias. We compared these objects with a known subdwarf benchmark and solar-metallicity dwarfs in colour-magnitude and colour-colour diagrams, as well as with state-of-the-art theoretical ultracool models. We confirm three more T subdwarfs and show that the Accident is subluminous compared to the current Y dwarf limit. Additionally, we propose two more Y subdwarf candidates. We emphasise that the $z_{PS1} - W1$ colour combining with the $W1 - W2$ colour could break the metallicity-temperature degeneracy for T and possibly for Y dwarfs. The $z_{PS1} - W1$ colour shifts redward when metallicity decreases for a certain temperature, which is not predicted by models. The Accident has the reddest $z_{PS1} - W1$ colour among our sample. The $z_{PS1} - W1$ colour will be useful to search for other examples of this cold and old population in upcoming and existing deep optical and infrared large-area surveys.

Figures

Figures reproduced from arXiv: 2412.04393 by the authors.

Figure 1
Figure 1. Colours vs. absolute zPS 1 magnitude diagrams of metal-poor T dwarf candidates (blue crosses), using trigonometric paral￾laxes obtained from this work and from the literature, zPS 1 photometry from this work and from Zhang et al. (2023) and infrared photometry from the literature. The parallax of W1810 comes from Lodieu et al. (2022). For the Accident (black cross and ar￾row), the parallax is from (Kirkpatrick et al… view at source ↗
Figure 2
Figure 2. Updated W1−W2 vs zAB −W1 and J −W2 vs zAB −W1 colour–colour diagrams with more metal-poor T, Y dwarf candidates compared to the one of Zhang et al. (2023). All the metal-poor T dwarf candidates are labeled with blue crosses and arrows and the Accident is labeled with the black cross and arrow. We overplotted solar-metallicity M, L, and T sequences from Pan-STARRS (yellow stars, orange squares and red dots, respectiv… view at source ↗
Figure 3
Figure 3. The same as Fig [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: W1− W2 vs J − W1 colour–colour diagrams of all metal￾poor T dwarf candidates (blue crosses and arrows) in [PITH_FULL_IMAGE:figures/full_fig_p010_4.png]
Figure 5
Figure 5. Figure 5: zPS 1 − W1 colour against metallicity for T and Y dwarfs. The vertical error bars are the photometric errors and the horizontal bars are the adopted metallicity ranges ( [PITH_FULL_IMAGE:figures/full_fig_p011_5.png]
Figure 6
Figure 6. Figure 6: zPS 1 −W1 colour against spectral type. The solid blue cir￾cle indicates that the object has an NIR spectrum. All the objects have a spectral type uncertainty of one subtype, unless specified differently in [PITH_FULL_IMAGE:figures/full_fig_p013_6.png]

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Works this paper leans on

84 extracted references · 53 canonical work pages

  1. [1]

    Abbott, T. M. C., Abdalla, F. B., Allam, S., et al. 2018, ApJS, 239, 18

    2018

  2. [2]

    Abbott, T. M. C., Adamów, M., Aguena, M., et al. 2021, ApJS, 255, 20

    2021

  3. [3]

    F., Allard, F., Hauschildt, P

    Allard, N. F., Allard, F., Hauschildt, P. H., Kielkopf, J. F., & Machin, L. 2003, A&A, 411, L473

    2003

  4. [4]

    F., Kielkopf, J

    Allard, N. F., Kielkopf, J. F., Myneni, K., & Blakely, J. N. 2024, A&A, 683, A188

    2024

  5. [5]

    F., Myneni, K., Blakely, J

    Allard, N. F., Myneni, K., Blakely, J. N., & Guillon, G. 2023, A&A, 674, A171

    work page 2023

  6. [6]

    F., Spiegelman, F., & Kielkopf, J

    Allard, N. F., Spiegelman, F., & Kielkopf, J. F. 2016, A&A, 589, A21

    work page 2016

  7. [7]

    1998, The Messenger, 94, 1 Astropy Collaboration, Price-Whelan, A

    Appenzeller, I., Fricke, K., Fürtig, W., et al. 1998, The Messenger, 94, 1 Astropy Collaboration, Price-Whelan, A. M., Lim, P. L., et al. 2022, ApJ, 935, 167 Astropy Collaboration, Price-Whelan, A. M., Sip˝ocz, B. M., et al. 2018, AJ, 156, 123 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33 3 http://www.astropy.org Ar...

    work page 1998

  8. [8]

    A., Bizenberger, P., & Storz, C

    Bailer-Jones, C. A., Bizenberger, P., & Storz, C. 2000, in Society of Photo- Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 4008, Op- tical and IR Telescope Instrumentation and Detectors, ed. M. Iye & A. F. Moorwood, 1305–1316

    work page 2000

Show all 84 references
  1. [9]

    Baumeister, H., Bizenberger, P., Bayler-Jones, C. A. L., et al. 2003, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 4841, Instrument Design and Performance for Optical/Infrared Ground-based Telescopes, ed. M. Iye & A. F. M. Moorwood, 343...

    2003

  2. [10]

    Best, W. M. J., Liu, M. C., Magnier, E. A., & Dupuy, T. J. 2020, AJ, 159, 257

    2020

  3. [11]

    Best, W. M. J., Liu, M. C., Magnier, E. A., & Dupuy, T. J. 2021, AJ, 161, 42

    2021

  4. [12]

    Best, W. M. J., Magnier, E. A., Liu, M. C., et al. 2018, ApJS, 234, 1

    2018

  5. [13]

    D., Caselden, D., et al

    Brooks, H., Kirkpatrick, J. D., Caselden, D., et al. 2022, AJ, 163, 47

    2022

  6. [14]

    J., Kirkpatrick, J

    Burgasser, A. J., Kirkpatrick, J. D., Brown, M. E., et al. 2002, ApJ, 564, 421

    2002

  7. [15]

    J., Schneider, A

    Burgasser, A. J., Schneider, A. C., Meisner, A. M., et al. 2024, arXiv e-prints, arXiv:2411.01378

    2024 arXiv

  8. [16]

    J., Witte, S., Helling, C., et al

    Burgasser, A. J., Witte, S., Helling, C., et al. 2009, ApJ, 697, 148

    2009

  9. [17]

    K., Lucas, P

    Burningham, B., Leggett, S. K., Lucas, P. W., et al. 2010, MNRAS, 404, 1952

    2010

  10. [18]

    V ., et al

    Burningham, B., Smith, L., Cardoso, C. V ., et al. 2014, MNRAS, 440, 359

    2014

  11. [19]

    & Sharp, C

    Burrows, A. & Sharp, C. M. 1999, ApJ, 512, 843

    1999

  12. [20]

    & V olobuyev, M

    Burrows, A. & V olobuyev, M. 2003, ApJ, 583, 985

    2003

  13. [21]

    2000, in Optical and IR Telescope Instrumentation and Detectors, V ol

    Cepa, J., Aguiar-Gonzalez, M., Gonzalez-Escalera, V ., et al. 2000, in Optical and IR Telescope Instrumentation and Detectors, V ol. 4008, SPIE, 623–631

    2000

  14. [22]

    2023, A&A, 671, A119

    Chabrier, G., Baraffe, I., Phillips, M., & Debras, F. 2023, A&A, 671, A119

    2023

  15. [23]

    C., Magnier, E

    Chambers, K. C., Magnier, E. A., Metcalfe, N., et al. 2016, arXiv e-prints, arXiv:1612.05560

    2016 arXiv

  16. [24]

    C., Kirkpatrick, J

    Cushing, M. C., Kirkpatrick, J. D., Gelino, C. R., et al. 2011, ApJ, 743, 50

    2011

  17. [25]

    C., Looper, D., Burgasser, A

    Cushing, M. C., Looper, D., Burgasser, A. J., et al. 2009, ApJ, 696, 986

    2009

  18. [26]

    M., Skrutskie, M

    Cutri, R. M., Skrutskie, M. F., van Dyk, S., et al. 2003, 2MASS All Sky Catalog of point sources

    2003

  19. [27]

    2008, A&A, 482, 961

    Delorme, P., Delfosse, X., Albert, L., et al. 2008, A&A, 482, 961

    2008

  20. [28]

    S., Bezawada, N., Black, M., et al

    Dhillon, V . S., Bezawada, N., Black, M., et al. 2021, MNRAS, 507, 350

    2021

  21. [29]

    M., et al

    Freudling, W., Romaniello, M., Bramich, D. M., et al. 2013, A&A, 559, A96

    2013

  22. [30]

    E., Scholz, R

    Gizis, J. E., Scholz, R. D., Irwin, M., & Jahreiss, H. 1997, MNRAS, 292, L41

    1997

  23. [31]

    Goodman, S. J. 2021, Research Notes of the American Astronomical Society, 5, 178

    2021

  24. [32]

    J., Schneider, A

    Greco, J. J., Schneider, A. C., Cushing, M. C., Kirkpatrick, J. D., & Burgasser, A. J. 2019, AJ, 158, 182

    2019

  25. [33]

    D., Metchev, S., Gagné, J., & Faherty, J

    Kellogg, K., Kirkpatrick, J. D., Metchev, S., Gagné, J., & Faherty, J. K. 2018, AJ, 155, 87

    2018

  26. [34]

    D., Gelino, C

    Kirkpatrick, J. D., Gelino, C. R., Cushing, M. C., et al. 2012, ApJ, 753, 156

    2012

  27. [35]

    D., Martin, E

    Kirkpatrick, J. D., Martin, E. C., Smart, R. L., et al. 2019, ApJS, 240, 19

    2019

  28. [36]

    D., Schneider, A., Fajardo-Acosta, S., et al

    Kirkpatrick, J. D., Schneider, A., Fajardo-Acosta, S., et al. 2014, ApJ, 783, 122 Kovács, Z., Mall, U., Bizenberger, P., Baumeister, H., & Röser, H.-J. 2004, in So- ciety of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 5499, Optical and Infrared Dete...

    2014

  29. [37]

    J., Faherty, J

    Kuchner, M. J., Faherty, J. K., Schneider, A. C., et al. 2017, ApJ, 841, L19

    2017

  30. [38]

    W., Mierle, K., Blanton, M., & Roweis, S

    Lang, D., Hogg, D. W., Mierle, K., Blanton, M., & Roweis, S. 2010, AJ, 139, 1782

    2010

  31. [39]

    K., Tremblin, P., Phillips, M

    Leggett, S. K., Tremblin, P., Phillips, M. W., et al. 2021, ApJ, 918, 11 Lépine, S., Rich, R. M., & Shara, M. M. 2007, ApJ, 669, 1235

    2021

  32. [40]

    C., Dupuy, T

    Liu, M. C., Dupuy, T. J., Bowler, B. P., Leggett, S. K., & Best, W. M. J. 2012, ApJ, 758, 57

    2012

  33. [41]

    1999, ApJ, 519, 793

    Lodders, K. 1999, ApJ, 519, 793

    1999

  34. [42]

    2019, A&A, 628, A61

    Lodieu, N., Allard, F., Rodrigo, C., et al. 2019, A&A, 628, A61

    2019

  35. [43]

    Lodieu, N., Béjar, V . J. S., & Rebolo, R. 2013, A&A, 550, L2

    2013

  36. [44]

    R., Martín, E

    Lodieu, N., Zapatero Osorio, M. R., Martín, E. L., Rebolo López, R., & Gauza, B. 2022, A&A, 663, A84

    2022

  37. [45]

    R., Martín, E

    Lodieu, N., Zapatero Osorio, M. R., Martín, E. L., Solano, E., & Aberasturi, M. 2010, ApJ, 708, L107

    2010

  38. [46]

    Luhman, K. L. 2014, ApJ, 786, L18

    2014

  39. [47]

    Luhman, K. L. & Sheppard, S. S. 2014, ApJ, 787, 126

    2014

  40. [48]

    L., Tremblin, P., Alves de Oliveira, C., et al

    Luhman, K. L., Tremblin, P., Alves de Oliveira, C., et al. 2024, AJ, 167, 5

    2024

  41. [49]

    N., Mann, A

    Mace, G. N., Mann, A. W., Skiff, B. A., et al. 2018, ApJ, 854, 145

    2018

  42. [50]

    M., et al

    Mainzer, A., Bauer, J., Cutri, R. M., et al. 2014, ApJ, 792, 30

    2014

  43. [51]

    S., Saumon, D., Visscher, C., et al

    Marley, M. S., Saumon, D., Visscher, C., et al. 2021, ApJ, 920, 85

    2021

  44. [52]

    Marocco, F., Eisenhardt, P. R. M., Fowler, J. W., et al. 2021, ApJS, 253, 8 Martín, E. L., Zhang, J. Y ., Esparza, P., et al. 2021, A&A, 655, L3 Martín, E. L., Zhang, J. Y ., Lanchas, H., et al. 2024, A&A, 686, A73

    2021

  45. [53]

    M., Schneider, A

    Meisner, A. M., Schneider, A. C., Burgasser, A. J., et al. 2021, ApJ, 915, 120

    2021

  46. [54]

    A., Menanteau, F., et al

    Morganson, E., Gruendl, R. A., Menanteau, F., et al. 2018, PASP, 130, 074501

    2018

  47. [55]

    J., Morley, C

    Mukherjee, S., Fortney, J. J., Morley, C. V ., et al. 2024, ApJ, 963, 73

    2024

  48. [56]

    N., Burningham, B., Jones, H

    Murray, D. N., Burningham, B., Jones, H. R. A., et al. 2011, MNRAS, 414, 575

    2011

  49. [57]

    1995, nature, 378, 463

    Nakajima, T., Oppenheimer, B., Kulkarni, S., et al. 1995, nature, 378, 463

    1995

  50. [58]

    R., Charbonneau, D., Irwin, J., et al

    Newton, E. R., Charbonneau, D., Irwin, J., et al. 2014, AJ, 147, 20

    2014

  51. [59]

    A., Wolf, C., Bessell, M

    Onken, C. A., Wolf, C., Bessell, M. S., et al. 2024, arXiv e-prints, arXiv:2402.02015

    2024

  52. [60]

    S., Folkner, W

    Park, R. S., Folkner, W. M., Williams, J. G., & Boggs, D. H. 2021, AJ, 161, 105

    2021

  53. [61]

    V ., Zhukovska, S

    Pavlenko, Y . V ., Zhukovska, S. V ., & V olobuev, M. 2007, Astronomy Reports, 51, 282

    2007

  54. [62]

    W., Tremblin, P., Baraffe, I., et al

    Phillips, M. W., Tremblin, P., Baraffe, I., et al. 2020, A&A, 637, A38

    2020

  55. [63]

    J., Gomes, J., Day-Jones, A

    Pinfield, D. J., Gomes, J., Day-Jones, A. C., et al. 2014, MNRAS, 437, 1009

    2014

  56. [64]

    1995, Nature, 377, 129

    Rebolo, R., Osorio, M., & Martín, E. 1995, Nature, 377, 129

    1995

  57. [65]

    & Solano, E

    Rodrigo, C. & Solano, E. 2020, in XIV .0 Scientific Meeting (virtual) of the Span- ish Astronomical Society, 182

    2020

  58. [66]

    2012, SVO Filter Profile Service Version 1.0, IVOA Working Draft 15 October 2012

    Rodrigo, C., Solano, E., & Bayo, A. 2012, SVO Filter Profile Service Version 1.0, IVOA Working Draft 15 October 2012

    2012

  59. [67]

    R., Muirhead, P

    Rojas-Ayala, B., Covey, K. R., Muirhead, P. S., & Lloyd, J. P. 2012, ApJ, 748, 93

    2012

  60. [68]

    C., Best, W

    Sanghi, A., Liu, M. C., Best, W. M. J., et al. 2023, ApJ, 959, 63

    2023

  61. [69]

    I., Hubbard, W

    Saumon, D., Bergeron, P., Lunine, J. I., Hubbard, W. B., & Burrows, A. 1994, ApJ, 424, 333

    1994

  62. [70]

    C., Burgasser, A

    Schneider, A. C., Burgasser, A. J., Gerasimov, R., et al. 2020, ApJ, 898, 77

    2020

  63. [71]

    C., Cushing, M

    Schneider, A. C., Cushing, M. C., Kirkpatrick, J. D., et al. 2015, ApJ, 804, 92

    2015

  64. [72]

    C., Meisner, A

    Schneider, A. C., Meisner, A. M., Gagné, J., et al. 2021, ApJ, 921, 140

    2021

  65. [73]

    Scholz, R. D. 2010, A&A, 510, L8

    2010

  66. [74]

    K., & Gupchup, J

    Sivarani, T., Lépine, S., Kembhavi, A. K., & Gupchup, J. 2009, ApJ, 694, L140

    2009

  67. [75]

    C., Martín, E

    Solano, E., Gálvez-Ortiz, M. C., Martín, E. L., et al. 2021, MNRAS, 501, 281

    2021

  68. [76]

    Stetson, P. B. 1987, PASP, 99, 191

    1987

  69. [77]

    1986, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol

    Tody, D. 1986, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 627, Instrumentation in astronomy VI, ed. D. L. Crawford, 733

    1986

  70. [78]

    1993, in Astronomical Society of the Pacific Conference Series, V ol

    Tody, D. 1993, in Astronomical Society of the Pacific Conference Series, V ol. 52, Astronomical Data Analysis Software and Systems II, ed. R. J. Hanisch, R. J. V . Brissenden, & J. Barnes, 173

    1993

  71. [79]

    D., Shapiro, S

    Weinberg, M. D., Shapiro, S. L., & Wasserman, I. 1987, ApJ, 312, 367

    1987

  72. [80]

    Woolf, V . M. & Wallerstein, G. 2006, PASP, 118, 218

    2006

  73. [81]

    Y ., Lodieu, N., & Martín, E

    Zhang, J. Y ., Lodieu, N., & Martín, E. L. 2023, A&A, 678, A105

    2023

  74. [82]

    H., Burgasser, A

    Zhang, Z. H., Burgasser, A. J., Gálvez-Ortiz, M. C., et al. 2019, MNRAS, 486, 1260

    2019

  75. [83]

    H., Galvez-Ortiz, M

    Zhang, Z. H., Galvez-Ortiz, M. C., Pinfield, D. J., et al. 2018, MNRAS, 480, 5447

    2018

  76. [84]

    30" 20" 10

    Zhang, Z. H., Pinfield, D. J., Gálvez-Ortiz, M. C., et al. 2017, MNRAS, 464, 3040 Article number, page 15 of 19 A&A proofs: manuscript no. no_bold3 Appendix A: Astrometry for five metal-poor T dwarf candidates. 50 0 RA (mas) Fit Omega2000 0.0 0.2 0.4 0.6 0.8 1.0 1.2 time (yr) ...

    2017

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