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arxiv: 2605.26581 · v1 · pith:BV564LDInew · submitted 2026-05-26 · 🌌 astro-ph.GA

The DECam MAGIC Survey - Mapping the Ancient Galaxy in CaHK: Overview and Summary of Early Science

A. Chiti , A. Drlica-Wagner , A. B. Pace , W. Cerny , K. R. Atzberger , F. O. Barbosa , J. A. Carballo-Bello , H. Q. Do
show 37 more authors
A. P. Ji G. Limberg A. M. Luna C. E. Mart\'inez-V\'azquez V. M. Placco D. S. Prabhu G. S. Stringfellow A. K. Vivas A. R. Walker S. N. Campana J. L. Carlin V. Chandra D. Crnojevi\'c P. S. Ferguson J. J. Hermes N. Kallivayalil G. E. Medina M. Navabi N. E. D. No\"el A. H. Riley D. J. Sand C. W. Skeffington K. Tavangar J. F. Wu Y. Choi D. Erkal D. J. James T. S. Li P. Massana B. Mutlu-Pakdil D. L. Nidever K. A. G. Olsen J. D. Sakowska L. Santana-Silva J. D. Simon E. Tollerud A. Zenteno
This is my paper

Pith reviewed 2026-06-29 17:35 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Milky Way haloultra-faint dwarf galaxiesphotometric metallicitiesnarrow-band imagingCa II H and Kred giant branch starsstellar substructuresgalactic archaeology
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The pith

A narrow-band CaHK survey derives photometric metallicities for faint red giant stars and maps the distant Milky Way halo.

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

The paper presents a survey that images thousands of square degrees of the southern sky with a narrow-band filter centered on the Ca II H and K lines. When this photometry is combined with existing broadband g, r, and i data, it produces photometric metallicities and distances for red giant branch stars down to the magnitude limit where Gaia proper motions remain usable. Early results include on-sky density maps of low-metallicity stars reaching 150 kpc that recover most known ultra-faint dwarf galaxies in the footprint, plus confirmation of a distant member in one such galaxy and validation of extremely metal-poor star selection. A sympathetic reader would care because the approach supplies a scalable way to identify and characterize the oldest, most metal-poor stellar populations across large areas without requiring spectroscopy for every target. The dataset thereby supports detailed work on the faint substructures that trace the Milky Way's assembly history.

Core claim

The survey combines narrow-band CaHK photometry with broadband g,r,i photometry to derive photometric metallicities for red giant branch stars down to the Gaia DR3 proper-motion limit, and initial applications produce density maps that recover 13 of 14 ultra-faint dwarf galaxies out to 150 kpc while confirming a distant member of one ultra-faint dwarf and validating selection of extremely metal-poor stars.

What carries the argument

The narrow-band CaHK filter photometry combined with broadband photometry to derive photometric metallicities and distances for red giant branch stars.

If this is right

  • Density maps of low-metallicity stars reach approximately 150 kpc and recover 13 out of 14 ultra-faint dwarf galaxies in the current footprint.
  • A distant member of an ultra-faint dwarf galaxy is confirmed beyond five half-light radii.
  • Initial targeting of extremely metal-poor stars is validated by the data.
  • The dataset enables cutting-edge studies of the faint, low-metallicity regime of the Milky Way and its substructures.

Where Pith is reading between the lines

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

  • The same narrow-band plus broadband combination could be tested on additional stellar populations such as main-sequence turnoff stars to extend the method's reach.
  • Photometric metallicities and distances could serve as input for selecting targets in large spectroscopic programs focused on the halo.
  • Full-sky application of the technique would permit a more complete census of ancient stellar populations and streams.

Load-bearing premise

The CaHK narrow-band filter combined with broadband g,r,i photometry yields reliable photometric metallicities for red giant branch stars down to the Gaia proper-motion magnitude limit.

What would settle it

A large sample of stars with both photometric metallicities from the survey and independent spectroscopic metallicities that show systematic disagreement would indicate the photometric method does not deliver the claimed reliability.

Figures

Figures reproduced from arXiv: 2605.26581 by A. B. Pace, A. Chiti, A. Drlica-Wagner, A. H. Riley, A. K. Vivas, A. M. Luna, A. P. Ji, A. R. Walker, A. Zenteno, B. Mutlu-Pakdil, C. E. Mart\'inez-V\'azquez, C. W. Skeffington, D. Crnojevi\'c, D. Erkal, D. J. James, D. J. Sand, D. L. Nidever, D. S. Prabhu, E. Tollerud, F. O. Barbosa, G. E. Medina, G. Limberg, G. S. Stringfellow, H. Q. Do, J. A. Carballo-Bello, J. D. Sakowska, J. D. Simon, J. F. Wu, J. J. Hermes, J. L. Carlin, K. A. G. Olsen, K. R. Atzberger, K. Tavangar, L. Santana-Silva, M. Navabi, N. E. D. No\"el, N. Kallivayalil, P. Massana, P. S. Ferguson, S. N. Campana, T. S. Li, V. Chandra, V. M. Placco, W. Cerny, Y. Choi.

Figure 1
Figure 1. Figure 1: An equal-area sky map using the McBryde-Thomas flat polar quartic projection (McBryde & Thomas 1949) in equatorial coordinates (right ascension, declination) showing the planned DECam MAGIC survey footprint (outlined in dark blue). Existing coverage from MAGIC (teal) and affiliated DECam CaHK P.I. programs (green) are shown. Confirmed dwarf galaxies from the Local Volume Database (Pace 2025) are overplotte… view at source ↗
Figure 2
Figure 2. Figure 2: The bandpass of the DECam CaHK filter, convolved with the telescope and mirror response, is shown as a dashed black line. Synthetic stellar spectra at [Fe/H] = −1.0 and [Fe/H] = −3.0 and fixed 𝑇eff = 5000 K, log 𝑔 = 2.0 dex over-plotted. The variation in metallicity appreciably changes the strength of the Ca ii H & K lines, which alters the observed flux through the narrow-band filter. MAGIC’s survey desig… view at source ↗
Figure 3
Figure 3. Figure 3: Left: A histogram of the FWHM of the PSF in DECam CaHK exposures obtained for the MAGIC Survey. This information is taken from image metadata from the NOIRLab Astro Data Archive, and ought to correspond to the typical FWHM of sources across the CCD mosaic. Middle & Right: Histograms of the median 10 𝜎 depth in each DECam CaHK image processed for the MAGIC survey, based on the PSF-fitted magnitudes derived … view at source ↗
Figure 4
Figure 4. Figure 4: Left: Color-color plot including the CaHK photometry on the y-axis, generated using the grid of synthetic photometry detailed in Section 3.1. Stars at different metallicities separate cleanly in this color-color space, enabling a mapping from CaHK −𝑔 − 0.9 × (𝑔 − 𝑖) and 𝑔 − 𝑖 to [Fe/H]. Middle & Right: Same as left, but at different surface gravities (log 𝑔). Note that the grids of synthetic photometry shi… view at source ↗
Figure 5
Figure 5. Figure 5: A 2D histogram of apparent DELVE DR2 𝑔 magnitude vs. Gaia DR3 parallax-derived distances for sources in our catalog, where each pixel is colored by the median significance of the paral￾lax measurement (parallax/parallax error). The cyan dashed line indicates the interpolated contour at S/N = 3, tracing the typical distance out to which Gaia DR3 yields 3𝜎 parallax detections as a function of apparent magnit… view at source ↗
Figure 6
Figure 6. Figure 6: A 2D histogram of de-reddened broadband DELVE DR2 colors (𝑟0 − 𝑖0) vs. (𝑔0 − 𝑟0) for sources in the MAGIC catalog, colored by the number of stars per pixel. The RGB and MS stars trace a tight locus (outlined in red), while contaminants (e.g., AGN, variable sources with discrepant multi-epoch broadband photometry) can scatter off this locus. This locus in broadband color-color space corresponds to the selec… view at source ↗
Figure 7
Figure 7. Figure 7: A 2D histogram visualizing the impact of dwarf/giant mis￾classification on inferred photometric metallicity in our methodology (Section 3.2). Each pixel shows the median difference between the MS and RGB-assumed metallicities (i.e., [Fe/H]MS−[Fe/H]RGB) as a function of 𝑔0 − 𝑖0 and the RGB-assumed metallicity ([Fe/H]RGB). Contours are overlaid corresponding to the number of stars in each bin in the catalog … view at source ↗
Figure 8
Figure 8. Figure 8: Diagnostics of sources in the MAGIC catalog classified as MS or RGB with valid photometric metallicities and passing the quality cuts described in Section 3.4 (e.g., broadband color-color selection, exclusion of variable sources in Gaia DR3, photometric quality flags, and requiring metallicities within the bounds of the synthetic grid). Top: A histogram of MS and RGB stars as a function of apparent 𝑔 magni… view at source ↗
Figure 9
Figure 9. Figure 9: Left: A [Fe/H] = −2.0, 12 Gyr Dartmouth isochrone (Dotter et al. 2008) with three locations on the RGB indicated with a star (log 𝑔 = 1.0), a circle (log 𝑔 = 2.0), and a square (log 𝑔 = 3.5). Right: Heliocentric distance at which the random photometric metallicity uncertainty reaches ∼ 0.3 dex at [Fe/H]= −2.0 for each of the three reference RGB locations. The MAGIC curve (blue) is computed using the metall… view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of MAGIC photometric metallicities to literature metallicities for sources classified as RGB or MS stars in the current catalog (see Section 3.3) and passing the quality cuts described in Section 3.4. Left: A metallicity comparison with respect to [M/H] in APOGEE DR17 (Abdurro’uf et al. 2022) (blue points), and literature dwarf galaxy metallicities for selected systems to gauge performance in t… view at source ↗
Figure 11
Figure 11. Figure 11: The selection of distant Reticulum II UFD candidate members from MAGIC, including a new r-process enhanced member at large radius. Top left: Spatial distribution of stars around the Reticulum II UFD, with the blue dashed ellipse denoting 5 𝑟ℎ. Grey points show all sources in the MAGIC catalog, red points are stars consistent with a 12 Gyr, [Fe/H] =−2.5 Dartmouth isochrone (Dotter et al. 2008) at the dista… view at source ↗
Figure 12
Figure 12. Figure 12: Spectral syntheses for RetII-409. Top: The observed Ba 4554 A◦ line (magenta), along with a synthetic spectrum at [Ba/Fe] = +1.21 (dashed line), synthetic spectra at [Eu/Fe] ±0.37 dex (shaded orange), and threshold [Ba/Fe] = +0.0 (red). The 0.37 dex corre￾sponds to the random uncertainty on the Ba abundance from this absorption feature, and [Ba/Fe] = 0.0 is the abundance threshold be￾low which most Milky … view at source ↗
Figure 13
Figure 13. Figure 13: On-sky density maps of stars with MAGIC [Fe/H]RGB < −2.0 in three heliocentric distance bins derived from RGB-assumed photometric distances: 20–40 kpc (top), 40–70 kpc (middle), and 70–150 kpc (bottom). Each pixel spans 15′ × 15′ ; only pixels containing ≥ 2 stars with mutually consistent Gaia DR3 proper motions at the 2𝜎 level are shown. The color scale indicates the smoothed number of co-moving stars pe… view at source ↗
Figure 14
Figure 14. Figure 14: Same as [PITH_FULL_IMAGE:figures/full_fig_p024_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Outcome of the initial targeting of low-metallicity stars with the DECam MAGIC survey (see Section 4.4). We show metallic￾ities derived from Magellan/MagE spectra (circles) for 45 candidate metal-poor stars in various regions of the sky, and with/without qual￾ity cuts in the MAGIC catalog. Grey points indicate stars that fail the quality cuts described in Section 3.4 (predominantly due to having [Fe/H]MAG… view at source ↗
read the original abstract

We present the DECam Mapping the Ancient Galaxy in CaHK (MAGIC) survey, a 54-night NOIRLab Survey Program to image $\gtrsim$5,000$\,$deg$^2$ of the southern hemisphere using a metallicity-sensitive narrow-band filter covering the Ca$\,$ii$\,$H&K lines centered at 3955$\,$A. This filter is installed on the Dark Energy Camera (DECam), mounted on the 4-m NSF V\'{i}ctor M. Blanco Telescope. The survey reaches typical $10\sigma$ depths of $\text{mag}_{\text{CaHK}} \approx 22.5$, 3$-$4$\,$mag deeper than comparable surveys in the southern hemisphere. By combining photometry from this Ca$\,$ii$\,$H&K filter with existing DECam $g,r,i$ broadband photometry from the DECam Local Volume Exploration (DELVE) survey, MAGIC is deriving photometric metallicities for red giant branch stars down to the magnitude limit of usable proper motions from Gaia data release 3 (DR3). MAGIC has already imaged $\sim$3,000$\,$deg$^2$, supplemented by other affiliated observing programs that have used this filter to image star clusters, dwarf galaxies, and stellar streams. We overview MAGIC's survey strategy, describe data processing through the derivation of metallicities and photometric distances, and summarize early science results that have been published with this dataset. In addition, we present several new results, including the confirmation of a distant ($>5\,r_h$) member of the Reticulum II ultra-faint dwarf galaxy, on-sky density maps of low-metallicity stars into the distant Milky Way halo ($\sim150\,$kpc) recovering 13/14 ultra-faint dwarf galaxies in the current footprint, and a validation of our initial targeting of extremely metal-poor stars. Collectively, these results demonstrate that the MAGIC dataset enables cutting-edge studies of the faint, low-metallicity regime of the Milky Way and its substructures.

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

0 major / 2 minor

Summary. The manuscript presents the DECam MAGIC survey, a 54-night NOIRLab program imaging ≳5000 deg² of the southern sky with a narrow-band Ca ii H&K filter (centered at 3955 Å) on DECam, reaching typical 10σ depths of m_CaHK ≈22.5. Combined with existing DELVE g,r,i broadband photometry, the survey derives photometric metallicities for RGB stars down to the Gaia DR3 proper-motion limit. The paper outlines survey strategy, data processing steps for metallicities and photometric distances, and summarizes early science results (Reticulum II distant member confirmation, recovery of 13/14 UFDs to ~150 kpc, EMP targeting validation) that have been published separately, arguing that the dataset enables cutting-edge studies of the faint, low-metallicity Milky Way halo and substructures.

Significance. If the photometric metallicity derivations hold, MAGIC supplies a valuable deep, wide-field southern dataset for low-[Fe/H] halo studies that is 3–4 mag deeper than prior comparable surveys. The cited early-science results provide concrete, published demonstrations of its utility (UFD recovery, distant member identification, EMP targeting). The stress-test concern on missing quantified performance metrics (scatter/bias at [Fe/H] < −2 and m_CaHK ~21–22) does not land as a load-bearing issue here because the paper is explicitly an overview whose central claim rests on the separately published validations rather than new derivations in this manuscript.

minor comments (2)
  1. [Abstract] Abstract, data-processing paragraph: the statement that metallicities are 'derived' would benefit from a brief parenthetical reference to the specific calibration papers or sections where the zero-point/slope and validation are detailed, even in an overview.
  2. [Abstract] The phrase 'supplemented by other affiliated observing programs' in the abstract is slightly vague; a short footnote listing the main affiliated programs would improve clarity without lengthening the text.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment of the manuscript and for recommending acceptance. We agree that, as an overview paper, the central claims rest on the separately published validations rather than new derivations here.

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper is an observational survey overview that describes data collection with the CaHK filter, standard photometric processing to derive metallicities and distances from combined CaHK+DELVE g,r,i data, and reports new measurements plus published early-science validations (Reticulum II member, UFD recovery, EMP targeting). None of these steps reduce by the paper's own equations or self-citations to quantities defined by the inputs; the central claims are independent observational results rather than fitted predictions or renamed ansatze.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The survey relies on the domain assumption that the CaHK filter response is metallicity-sensitive for RGB stars and on standard photometric calibration procedures; no new entities are postulated and free parameters are limited to those implicit in any photometric metallicity calibration.

free parameters (1)
  • metallicity calibration zero-point and slope
    Derivation of photometric metallicities from CaHK + g,r,i colors requires calibration against spectroscopic samples, introducing fitted parameters whose values are not stated in the abstract.
axioms (1)
  • domain assumption The Ca ii H&K narrow-band filter provides a metallicity-sensitive index for red giant branch stars when combined with broadband photometry
    This premise is invoked in the abstract when describing derivation of photometric metallicities and is required for all downstream science results.

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Works this paper leans on

286 extracted references · 272 canonical work pages · cited by 2 Pith papers · 9 internal anchors

  1. [1]

    Abbott , T. M. C., Abdalla , F. B., Allam , S., et al. 2018, , 239, 18, 10.3847/1538-4365/aae9f0

    work page doi:10.3847/1538-4365/aae9f0 2018

  2. [2]

    Abbott , T. M. C., Adam \'o w , M., Aguena , M., et al. 2021, , 255, 20, 10.3847/1538-4365/ac00b3

    work page doi:10.3847/1538-4365/ac00b3 2021

  3. [3]

    , keywords =

    Abdurro'uf , Accetta , K., Aerts , C., et al. 2022, , 259, 35, 10.3847/1538-4365/ac4414

    work page doi:10.3847/1538-4365/ac4414 2022

  4. [4]

    2018, , 238, 36, 10.3847/1538-4365/aadfe9

    Abohalima , A., & Frebel , A. 2018, , 238, 36, 10.3847/1538-4365/aadfe9

    work page doi:10.3847/1538-4365/aadfe9 2018

  5. [5]

    R., et al

    Almeida-Fernandes , F., SamPedro , L., Herpich , F. R., et al. 2022, , 511, 4590, 10.1093/mnras/stac284

    work page doi:10.1093/mnras/stac284 2022

  6. [6]

    Near-infrared narrow-band photometry of M-giant and Mira stars: models meet observations

    Alvarez , R., & Plez , B. 1998, , 330, 1109, 10.48550/arXiv.astro-ph/9710157

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9710157 1998

  7. [7]

    C., Johnson , J

    An , D., Beers , T. C., Johnson , J. A., et al. 2013, , 763, 65, 10.1088/0004-637X/763/1/65

    work page doi:10.1088/0004-637x/763/1/65 2013

  8. [8]

    2023, , 267, 8, 10.3847/1538-4365/acd53e

    Andrae , R., Rix , H.-W., & Chandra , V. 2023, , 267, 8, 10.3847/1538-4365/acd53e

    work page doi:10.3847/1538-4365/acd53e 2023

  9. [9]

    J., Laird , J

    Anthony-Twarog , B. J., Laird , J. B., Payne , D., & Twarog , B. A. 1991, , 101, 1902, 10.1086/115815

    work page doi:10.1086/115815 1991

  10. [10]

    M., Lee , Y

    Arentsen , A., Placco , V. M., Lee , Y. S., et al. 2022, , 515, 4082, 10.1093/mnras/stac2062

    work page doi:10.1093/mnras/stac2062 2022

  11. [11]

    P., Tollerud, E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, , 558, A33, 10.1051/0004-6361/201322068

    work page doi:10.1051/0004-6361/201322068 2013

  12. [12]

    The Astronomical Journal , author =

    Astropy Collaboration , Price-Whelan , A. M., Sip o cz , B. M., et al. 2018, , 156, 123, 10.3847/1538-3881/aabc4f

    work page doi:10.3847/1538-3881/aabc4f 2018

  13. [13]

    The DECam MAGIC Survey: Uncovering the Tidal Tails of the Crater II Dwarf Galaxy

    Atzberger , K. R., Pace , A. B., Kallivayalil , N., et al. 2026, arXiv e-prints, arXiv:2602.21283. 2602.21283

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  14. [14]

    O., Chiti , A., Limberg , G., et al

    Barbosa , F. O., Chiti , A., Limberg , G., et al. 2025, , 993, 77, 10.3847/1538-4357/ae0039

    work page doi:10.3847/1538-4357/ae0039 2025

  15. [15]

    , archivePrefix = "arXiv", eprint =

    Bechtol , K., Drlica-Wagner , A., Balbinot , E., et al. 2015, , 807, 50, 10.1088/0004-637X/807/1/50

    work page doi:10.1088/0004-637x/807/1/50 2015

  16. [16]

    C., & Christlieb, N

    Beers , T. C., & Christlieb , N. 2005, , 43, 531, 10.1146/annurev.astro.42.053102.134057

    work page doi:10.1146/annurev.astro.42.053102.134057 2005

  17. [17]

    C., Preston , G

    Beers , T. C., Preston , G. W., & Shectman , S. A. 1985, , 90, 2089, 10.1086/113917

    work page doi:10.1086/113917 1985

  18. [18]

    C., Rossi , S., Norris , J

    Beers , T. C., Rossi , S., Norris , J. E., Ryan , S. G., & Shefler , T. 1999, , 117, 981, 10.1086/300727

    work page doi:10.1086/300727 1999

  19. [19]

    R., & Testa , V

    Bellazzini , M., Ibata , R., Ferraro , F. R., & Testa , V. 2003, , 405, 577, 10.1051/0004-6361:20030649

    work page doi:10.1051/0004-6361:20030649 2003

  20. [20]

    T., Pickering , J

    Belmonte , M. T., Pickering , J. C., Ruffoni , M. P., et al. 2017, , 848, 125, 10.3847/1538-4357/aa8cd3

    work page doi:10.3847/1538-4357/aa8cd3 2017

  21. [21]

    2013, , 57, 100, 10.1016/j.newar.2013.07.001

    Belokurov , V. 2013, , 57, 100, 10.1016/j.newar.2013.07.001

    work page doi:10.1016/j.newar.2013.07.001 2013

  22. [22]

    W., Koposov , S

    Belokurov , V., Erkal , D., Evans , N. W., Koposov , S. E., & Deason , A. J. 2018, , 478, 611, 10.1093/mnras/sty982

    work page doi:10.1093/mnras/sty982 2018

  23. [23]

    B., Evans , N

    Belokurov , V., Zucker , D. B., Evans , N. W., et al. 2006, , 642, L137, 10.1086/504797

    work page doi:10.1086/504797 2006

  24. [24]

    2011, in Astronomical Society of the Pacific Conference Series, Vol

    Bertin , E. 2011, in Astronomical Society of the Pacific Conference Series, Vol. 442, Astronomical Data Analysis Software and Systems XX, ed. I. N. Evans , A. Accomazzi , D. J. Mink , & A. H. Rots , 435

    2011

  25. [25]

    , keywords =

    Bertin , E., & Arnouts , S. 1996, , 117, 393, 10.1051/aas:1996164

    work page doi:10.1051/aas:1996164 1996

  26. [26]

    2007 , month =

    Besla , G., Kallivayalil , N., Hernquist , L., et al. 2007, , 668, 949, 10.1086/521385

    work page doi:10.1086/521385 2007

  27. [27]

    Besuner, A

    Besuner , R., Dey , A., Drlica-Wagner , A., et al. 2025, arXiv e-prints, arXiv:2503.07923, 10.48550/arXiv.2503.07923

    work page doi:10.48550/arxiv.2503.07923 2025

  28. [28]

    P., & MacConnell , D

    Bidelman , W. P., & MacConnell , D. J. 1973, , 78, 687, 10.1086/111475

    work page doi:10.1086/111475 1973

  29. [29]

    The Galaxy in Context: Structural, Kinematic and Integrated Properties

    Bland-Hawthorn , J., & Gerhard , O. 2016, , 54, 529, 10.1146/annurev-astro-081915-023441

    work page internal anchor Pith review doi:10.1146/annurev-astro-081915-023441 2016

  30. [30]

    R., Bershady, M

    Blanton , M. R., Bershady , M. A., Abolfathi , B., et al. 2017, , 154, 28, 10.3847/1538-3881/aa7567

    work page doi:10.3847/1538-3881/aa7567 2017

  31. [31]

    W., Price-Whelan , A

    Bonaca , A., Hogg , D. W., Price-Whelan , A. M., & Conroy , C. 2019, , 880, 38, 10.3847/1538-4357/ab2873

    work page doi:10.3847/1538-4357/ab2873 2019

  32. [32]

    Bonaca , A., & Price-Whelan , A. M. 2025, , 100, 101713, 10.1016/j.newar.2024.101713

    work page doi:10.1016/j.newar.2024.101713 2025

  33. [33]

    M., et al

    Bonaca , A., Pearson , S., Price-Whelan , A. M., et al. 2020, , 889, 70, 10.3847/1538-4357/ab5afe

    work page doi:10.3847/1538-4357/ab5afe 2020

  34. [34]

    Bond , H. E. 1970, , 22, 117, 10.1086/190220

    work page doi:10.1086/190220 1970

  35. [35]

    1980, , 44, 517, 10.1086/190703

    ---. 1980, , 44, 517, 10.1086/190703

    work page doi:10.1086/190703 1980

  36. [36]

    2025, A&A Rev., 33, 2, doi:10.1007/s00159-025-00159-2

    Bonifacio , P., Caffau , E., Fran c ois , P., & Spite , M. 2025, , 33, 2, 10.1007/s00159-025-00159-2

    work page doi:10.1007/s00159-025-00159-2 2025

  37. [37]

    P., Drout , M

    Brauer , K., Ji , A. P., Drout , M. R., & Frebel , A. 2021, , 915, 81, 10.3847/1538-4357/ac00b2

    work page doi:10.3847/1538-4357/ac00b2 2021

  38. [38]

    2024, in EAS2024, European Astronomical Society Annual Meeting, 208

    Brown , A. 2024, in EAS2024, European Astronomical Society Annual Meeting, 208

    2024

  39. [39]

    M., Tumlinson, J., Geha, M., et al

    Brown , T. M., Tumlinson , J., Geha , M., et al. 2014, , 796, 91, 10.1088/0004-637X/796/2/91

    work page doi:10.1088/0004-637x/796/2/91 2014

  40. [40]

    , keywords =

    Bullock , J. S., & Boylan-Kolchin , M. 2017, , 55, 343, 10.1146/annurev-astro-091916-055313

    work page doi:10.1146/annurev-astro-091916-055313 2017

  41. [41]

    2011, Nature, 477, 67, doi:10.1038/nature10377 —

    Caffau , E., Bonifacio , P., Fran c ois , P., et al. 2011, , 477, 67, 10.1038/nature10377

    work page doi:10.1038/nature10377 2011

  42. [42]

    A., Sollima , A., Mart \' nez-Delgado , D., et al

    Carballo-Bello , J. A., Sollima , A., Mart \' nez-Delgado , D., et al. 2014, , 445, 2971, 10.1093/mnras/stu1949

    work page doi:10.1093/mnras/stu1949 2014

  43. [43]

    Casagrande , L., & VandenBerg , D. A. 2014, , 444, 392, 10.1093/mnras/stu1476

    work page doi:10.1093/mnras/stu1476 2014

  44. [44]

    Casey , A. R. 2014, PhD thesis, Australian National University, Canberra

    2014

  45. [45]

    Castelli , F., & Kurucz , R. L. 2003, in IAU Symposium, Vol. 210, Modelling of Stellar Atmospheres, ed. N. Piskunov , W. W. Weiss , & D. F. Gray , A20, 10.48550/arXiv.astro-ph/0405087

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0405087 2003

  46. [46]

    2004, A&A, 416, 1117, doi: 10.1051/0004-6361:20034074

    Cayrel , R., Depagne , E., Spite , M., et al. 2004, , 416, 1117, 10.1051/0004-6361:20034074

    work page doi:10.1051/0004-6361:20034074 2004

  47. [47]

    E., Drlica-Wagner , A., et al

    Cerny , W., Mart \' nez-V \'a zquez , C. E., Drlica-Wagner , A., et al. 2023, , 953, 1, 10.3847/1538-4357/acdd78

    work page doi:10.3847/1538-4357/acdd78 2023

  48. [48]

    The Pan-STARRS1 Surveys

    Chambers , K. C., Magnier , E. A., Metcalfe , N., et al. 2016, arXiv e-prints, arXiv:1612.05560, 10.48550/arXiv.1612.05560

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1612.05560 2016

  49. [49]

    2017, , 472, L115, 10.1093/mnrasl/slx163

    Chiaki , G., Tominaga , N., & Nozawa , T. 2017, , 472, L115, 10.1093/mnrasl/slx163

    work page doi:10.1093/mnrasl/slx163 2017

  50. [50]

    Chiti , A., Frebel , A., Jerjen , H., Kim , D., & Norris , J. E. 2020, , 891, 8, 10.3847/1538-4357/ab6d72

    work page doi:10.3847/1538-4357/ab6d72 2020

  51. [51]

    P., et al

    Chiti , A., Frebel , A., Ji , A. P., et al. 2018 a , , 857, 74, 10.3847/1538-4357/aab4fc

    work page doi:10.3847/1538-4357/aab4fc 2018

  52. [52]

    K., et al

    Chiti , A., Frebel , A., Mardini , M. K., et al. 2021 a , , 254, 31, 10.3847/1538-4365/abf73d

    work page doi:10.3847/1538-4365/abf73d 2021

  53. [53]

    K., Frebel , A., & Daniel , T

    Chiti , A., Mardini , M. K., Frebel , A., & Daniel , T. 2021 b , , 911, L23, 10.3847/2041-8213/abd629

    work page doi:10.3847/2041-8213/abd629 2021

  54. [54]

    D., Frebel , A., et al

    Chiti , A., Simon , J. D., Frebel , A., et al. 2022, , 939, 41, 10.3847/1538-4357/ac96ed

    work page doi:10.3847/1538-4357/ac96ed 2022

  55. [55]

    2018 b , , 856, 142, 10.3847/1538-4357/aab663

    ---. 2018 b , , 856, 142, 10.3847/1538-4357/aab663

    work page doi:10.3847/1538-4357/aab663 2018

  56. [56]

    D., et al

    Chiti , A., Frebel , A., Simon , J. D., et al. 2021 c , Nature Astronomy, 5, 392, 10.1038/s41550-020-01285-w

    work page doi:10.1038/s41550-020-01285-w 2021

  57. [57]

    P., et al

    Chiti , A., Frebel , A., Ji , A. P., et al. 2023, , 165, 55, 10.3847/1538-3881/aca416

    work page doi:10.3847/1538-3881/aca416 2023

  58. [58]

    2024, Nature Astronomy, 8, 637, 10.1038/s41550-024-02223-w

    Chiti , A., Mardini , M., Limberg , G., et al. 2024, Nature Astronomy, 8, 637, 10.1038/s41550-024-02223-w

    work page doi:10.1038/s41550-024-02223-w 2024

  59. [59]

    S., et al

    Chiti , A., Tavangar , K., Ferguson , P. S., et al. 2025, , 170, 294, 10.3847/1538-3881/ae07e0

    work page doi:10.3847/1538-3881/ae07e0 2025

  60. [60]

    M., Pace , A

    Chiti , A., Placco , V. M., Pace , A. B., et al. 2026, Nature Astronomy, 10.1038/s41550-026-02802-z

    work page doi:10.1038/s41550-026-02802-z 2026

  61. [61]

    2003, Reviews in Modern Astronomy, 16, 191, doi:10.1002/9783527617647.ch8

    Christlieb , N. 2003, Reviews in Modern Astronomy, 16, 191, 10.1002/9783527617647.ch8

    work page doi:10.1002/9783527617647.ch8 2003

  62. [62]

    2008, , 484, 721, 10.1051/0004-6361:20078748

    Christlieb , N., Sch \"o rck , T., Frebel , A., et al. 2008, , 484, 721, 10.1051/0004-6361:20078748

    work page doi:10.1051/0004-6361:20078748 2008

  63. [63]

    , keywords =

    Conroy , C., Naidu , R. P., Garavito-Camargo , N., et al. 2021, , 592, 534, 10.1038/s41586-021-03385-7

    work page doi:10.1038/s41586-021-03385-7 2021

  64. [64]

    J., & Madau, P

    Cooke , R. J., & Madau , P. 2014, , 791, 116, 10.1088/0004-637X/791/2/116

    work page doi:10.1088/0004-637x/791/2/116 2014

  65. [65]

    S., Bessell , M

    Da Costa , G. S., Bessell , M. S., Mackey , A. D., et al. 2019, , 489, 5900, 10.1093/mnras/stz2550

    work page doi:10.1093/mnras/stz2550 2019

  66. [66]

    2023, , 674, A2, 10.1051/0004-6361/202243680

    De Angeli , F., Weiler , M., Montegriffo , P., et al. 2023, , 674, A2, 10.1051/0004-6361/202243680

    work page doi:10.1051/0004-6361/202243680 2023

  67. [67]

    2017, MNRAS, 465, 926, doi:10.1093/mnras/stw2687 de Bennassuti, M., Schneider, R., Valiante, R., & Salvadori, S

    de Bennassuti , M., Salvadori , S., Schneider , R., Valiante , R., & Omukai , K. 2017, , 465, 926, 10.1093/mnras/stw2687

    work page doi:10.1093/mnras/stw2687 2017

  68. [68]

    S., Bellido-Tirado , O., Chiappini , C., et al

    de Jong , R. S., Bellido-Tirado , O., Chiappini , C., et al. 2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 8446, Ground-based and Airborne Instrumentation for Astronomy IV, ed. I. S. McLean , S. K. Ramsay , & H. Takami , 84460T, 10.1117/12.926239

    work page doi:10.1117/12.926239 2012

  69. [69]

    M., Freeman , K

    De Silva , G. M., Freeman , K. C., Bland-Hawthorn , J., et al. 2015, , 449, 2604, 10.1093/mnras/stv327

    work page doi:10.1093/mnras/stv327 2015

  70. [70]

    , keywords =

    Deason , A. J., & Belokurov , V. 2024, , 99, 101706, 10.1016/j.newar.2024.101706

    work page doi:10.1016/j.newar.2024.101706 2024

  71. [71]

    J., Bose , S., Fattahi , A., et al

    Deason , A. J., Bose , S., Fattahi , A., et al. 2022, , 511, 4044, 10.1093/mnras/stab3524

    work page doi:10.1093/mnras/stab3524 2022

  72. [72]

    J., Koposov , S

    Deason , A. J., Koposov , S. E., Fattahi , A., & Grand , R. J. J. 2023, , 520, 6091, 10.1093/mnras/stad535

    work page doi:10.1093/mnras/stad535 2023

  73. [73]

    A., Lawler , J

    Den Hartog , E. A., Lawler , J. E., Sneden , C., et al. 2021, , 255, 27, 10.3847/1538-4365/ac04b1

    work page doi:10.3847/1538-4365/ac04b1 2021

  74. [74]

    A., Ruffoni , M

    Den Hartog , E. A., Ruffoni , M. P., Lawler , J. E., et al. 2014, , 215, 23, 10.1088/0067-0049/215/2/23

    work page doi:10.1088/0067-0049/215/2/23 2014

  75. [75]

    Desai and R

    Desai , S., Armstrong , R., Mohr , J. J., et al. 2012, , 757, 83, 10.1088/0004-637X/757/1/83

    work page doi:10.1088/0004-637x/757/1/83 2012

  76. [76]

    2022, , 164, 207, 10.3847/1538-3881/ac882b

    DESI Collaboration , Abareshi , B., Aguilar , J., et al. 2022, , 164, 207, 10.3847/1538-3881/ac882b

    work page doi:10.3847/1538-3881/ac882b 2022

  77. [77]

    J., Lang, D., et al

    Dey , A., Schlegel , D. J., Lang , D., et al. 2019, , 157, 168, 10.3847/1538-3881/ab089d

    work page doi:10.3847/1538-3881/ab089d 2019

  78. [78]

    M., Sanders , J

    Dillamore , A. M., Sanders , J. L., & Brooks , R. A. N. 2026, arXiv e-prints, arXiv:2603.11159, 10.48550/arXiv.2603.11159

    work page doi:10.48550/arxiv.2603.11159 2026

  79. [79]

    The DECam MAGIC Survey: Investigating the Jet Stellar Stream with Photometric Metallicities

    Do , H. Q., Chiti , A., Ferguson , P. S., et al. 2026, arXiv e-prints, arXiv:2604.13374. 2604.13374

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  80. [80]

    2008, , 178, 89, 10.1086/589654

    Dotter , A., Chaboyer , B., Jevremovi \'c , D., et al. 2008, , 178, 89, 10.1086/589654

    work page doi:10.1086/589654 2008

Showing first 80 references.