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REVIEW 3 major objections 4 minor 174 references

SDSS-IV MaStar: Quantification and Abatement of Interstellar Absorption in the Largest Empirical Stellar Spectral Library

T0 review · 3 major / 4 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read Milky Way interstellar gas plants spurious calcium and sodium lines in the largest star library, and the paper's cleaned version removes them, shifting galaxy ages, sodium abundances, and mass-function fits.

desk verdict Useful, practical ISM-cleaning of MaStar with one unresolved 3–4 sigma discrepancy between the two replacement methods for hot stars, exactly where the corrections are largest. read the letter →

arxiv 2502.09707 v1 pith:NRMGPBDV submitted 2025-02-13 astro-ph.GA

Kate H. R. Rubin , Kyle B. Westfall , Claudia Maraston , Daniel Thomas , Renbin Yan , J. Christopher Howk , Erick Aguirre , Kaelee S. Parker
show 1 more author
David R. Law
This is my paper · ORCID
classification astro-ph.GA
keywords interstellarabsorptionCaIIHandKlinesNaIDdoubletMaStarstellarlibrarypopulationsynthesisempiricalspectraltemplatesdustreddeningequivalentwidths
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 establishes that cool gas in the Milky Way imprints its own calcium and sodium absorption onto the spectra of thousands of stars in MaStar, the largest empirical stellar spectral library, and that this contamination is strong enough to distort galaxy science built on the library. Using high-resolution measurements of interstellar absorption toward a few thousand stellar sightlines, the authors build a model that predicts the contaminating line strength from a star's distance, latitude, and dust reddening, and they use it to produce corrected spectroscopy for roughly 80% of the 24,162-star catalog. The central demonstration is that simple stellar population models constructed from the original library artificially strengthen the Ca II K line by more than 20% in populations younger than 400 million years, and strengthen the Na I D line by more than 50% in starbursting systems and by more than 10% even in 10-billion-year-old populations. If the paper is right, analyses using the uncorrected library infer galaxy ages that are too young, sodium abundances that are too low, and initial mass functions that are too bottom-heavy, and the released cleaned spectra, templates, and SSP models offer a direct way to correct those biases.

What carries the argument

The central mechanism is an empirical scaling law for interstellar contamination: in each of six distance bins, the equivalent width of Ca II K and of each Na I D component is modeled as $W^{\rm ISM} = \beta + \alpha \log E_{\rm DustMap}$, with slope and intercept fit by MCMC likelihoods that include upper limits and intrinsic scatter, anchored to the high-resolution samples of Sembach et al., Munari & Zwitter, and Welsh et al. This predictor converts three readily available stellar quantities — distance, Galactic latitude, and dust reddening — into a predicted contaminating width, which in turn sets the thresholds ($W^{\rm ISM}$(Ca II K) < 0.07 Å, $W^{\rm ISM}$(Na I 5891) < 0.05 Å) that define the 6342-star 'low-ISM' reference sample. Replacement matching runs on a three-dimensional stellar-parameter distance $\Psi$ built from $\log g$, $\theta = 5040\ \mathrm{K}/T_{\rm eff}$, and $[\mathrm{Fe/H}]$; coadded low-ISM spectra are inserted into the windows 3912–3995 Å and 5873–5917 Å with Gaussian-tapered edges, and isolated hot stars instead receive ATLAS9-based BOSZ model profiles. The cleaned spectra are then passed through the established stellar-population construction to produce SSP templates whose line strengths, compared with SSPs built from the original library, quantify the bias.

What would settle it

Re-observe a sample of MaStar stars spanning the predicted contamination range at spectral resolution R ≳ 30,000, where interstellar Ca II and Na I components are narrow and kinematically separated from the broad stellar lines. If the measured interstellar equivalent widths disagree with the model's binned predictions for a substantial fraction of sightlines, or if the paper's 'cleaned' profiles do not match the interstellar-free photospheric lines seen at high resolution, the correction is wrong. A cheap version of this test is the paper's own internal check, in which SSPs built only from low-ISM stars agree with the fully cleaned SSPs at the 3–4% level: any regime where that agreement fails marks where the cleaning breaks down.

Watch

Extended reading notes

Core claim

The paper argues that the Milky Way's interstellar medium leaves its own absorption signature inside the MaStar empirical stellar library, and that the signature is large enough to bias galaxy science. At the library's R ~ 1800 resolution, interstellar Ca II λλ3934, 3969 and Na I λλ5891, 5897 absorption is blended into the stellar photospheric profiles of those transitions. The authors construct a model of the interstellar equivalent width as a function of stellar distance, Galactic latitude, and dust reddening, fit as $W^{\rm ISM} = \beta + \alpha \log E_{\rm DustMap}$ in six distance bins using high-resolution literature measurements. Applying this model to all 24,162 MaStar stars selects 6342 stars predicted to have negligible contamination ($W^{\rm ISM}$(Ca II K) < 0.07 Å and $W^{\rm ISM}$(Na I 5891) < 0.05 Å); for the remaining stars with close matches, the Na I D region (and, for stars with $T_{\rm eff} > 9000$ K, the Ca II region too) is replaced with coadded spectra of similar low-contamination stars, and 738 isolated hot stars receive matched ATLAS9-based BOSZ model profiles instead. The result is a cleaned library whose mean $W$(Ca II K) falls by 0.4–0.7 Å and whose mean $W$(Na I D) falls by 0.6–1.1 Å for hot stars ($T_{\rm eff} > 7610$ K) and by 0.1–0.2 Å for cooler stars. Constructed from the original library, simple stellar population models overestimate $W$(Ca II K) by ≥20% at ages below 400 Myr and overestimate the NaD index by ≥50% in starbursting systems and by ≥10% at ages above 10 Gyr. The cleaned stellar spectra, hierarchically clustered templates, and SSP libraries are released as public data products.

Load-bearing premise

The entire cleaning rests on one premise: that the high-resolution calcium and sodium absorption measurements made toward roughly two thousand stellar sightlines, binned by distance and reddening and converted through a dust map, correctly predict the interstellar absorption along every one of the 24,000 MaStar sightlines.

Editorial extensions

If this is right

  • Stellar-population fits to young and starbursting galaxies made with the original library underestimate stellar ages, because interstellar Ca II K mimics the strong calcium absorption that diagnoses A-type stars.
  • [Na/Fe] estimates in early-type galaxies from the NaD Lick index are systematically low by roughly 0.1–0.2 dex, and the paper argues the true sodium enhancement of massive ellipticals may reach +0.7 to +1.0 dex.
  • Spectroscopic IMF-slope constraints anchored on Na I transitions shift toward less bottom-heavy (more Milky Way-like) slopes once templates are corrected, and lower-mass ellipticals may move toward bottom-light slopes.
  • Down-the-barrel studies of Na I D as a tracer of galactic winds will overestimate the stellar contribution and underestimate the host-galaxy interstellar component in starbursts.
  • The public cleaned spectra, hierarchical cluster templates, and SSP libraries let existing galaxy surveys be re-fit without new observations, putting a quantitative bound on this systematic for each survey.

Reading between the lines

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

  • Editorial inference: the same contamination model could be applied to other moderate-resolution empirical libraries, re-deriving the NaD–[Na/Fe] calibration from a contamination-free sample to test how much the index–abundance slope shifts.
  • Editorial inference: the distance binning smooths over small-scale structure (the paper itself notes an absorbing 'wall' at 80 pc), so the model will be least reliable toward dense clouds and the Galactic plane; a version using the full 3D dust map rather than binned medians would directly test how often stars near such clouds are misclassified as low-ISM.
  • Editorial inference: the predicted interstellar widths for all 24,162 stars form a statistical absorption map of the local Milky Way that the paper does not exploit; cross-correlating these widths with known cloud and gas catalogs could calibrate Ca II and Na I columns against dust and 21 cm emission.
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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

3 major / 4 minor

Summary. The paper assesses the impact of Milky Way interstellar Ca II and Na I absorption on the SDSS-IV MaStar empirical stellar library. The authors build a model for W_ISM as a function of distance, Galactic latitude, and dust reddening from high-resolution literature samples (Sembach et al. 1993; Munari & Zwitter 1997; Welsh et al. 2010), apply it to 24,162 MaStar stars, identify 6,342 low-ISM sightlines, and replace the Ca II and Na I D profiles of 12,110 stars with coadded low-ISM spectra and of 738 hot stars with BOSZ theoretical templates. They release cleaned stellar spectra, hierarchically clustered templates, and SSP templates, and quantify the artificial enhancement of Ca II K and NaD indices in SSP models built from the original library.

Significance. If the cleaning procedure is reliable, this is a valuable data product: it would remove a previously unquantified Milky Way ISM contamination from the largest empirical stellar library, with direct consequences for galaxy spectral fitting and stellar population synthesis. The public releases of cleaned spectra, HC templates, and SSP templates are concrete strengths, and the demonstration that NaD enhancements persist at the >10% level at old ages is an important, falsifiable result. The paper also contains a careful treatment of telluric contamination (Appendix A). The significance is conditional on resolving a 3-4 sigma disagreement between the empirical and theoretical cleaning methods for hot stars, which is the central load-bearing issue.

major comments (3)
  1. [Section 3.3, Figure 14] This is a major comment.
  2. [Section 2.2-2.3] This is a major comment.
  3. [Section 3.6.4] This is a major comment.
minor comments (4)
  1. [Table 3 and Section 3.4] This is a minor comment.
  2. [Section 3.5] This is a minor comment.
  3. [Figure 13] This is a minor comment.
  4. [Equation (1) and Section 2.2] This is a minor comment.

Circularity Check

1 steps flagged · score 3.0 of 10

No central circularity: the ISM model is externally calibrated and the cleaning reduces to a measured spectral replacement; however, one self-referential robustness check and an unresolved BOSZ/coadd offset qualify the validation.

  1. self definitional [Section 3.6.4, Fig. 17]
    "To test the robustness of our cleaning procedure, we have constructed an additional set of SSP templates using only our original “low-ISM” sample of stars. ... These profiles are very similar, and in some cases nearly identical, to those of the cleaned templates. ... We conclude from this comparison that our procedure for ISM removal is indeed robust, and does not introduce unwanted artifacts into our final cleaned SSP templates."

    The cleaned SSPs are built from spectra whose Ca II/Na I regions have been replaced with coadds of the low-ISM stars, while the comparison SSPs are constructed directly from those same low-ISM stars. Both template sets therefore draw on the identical low-ISM pool, so near-identical Na I D profiles are expected by construction rather than being an independent confirmation that the low-ISM sample is genuinely free of interstellar absorption. Presenting this agreement as evidence that the cleaning is robust overstates its evidentiary value: it mainly checks the internal bookkeeping of the replacement procedure, not whether the model-selected low-ISM profiles are truly intrinsic.

full rationale

The central cleaning claim does not reduce to its inputs. The W_ISM model is primarily calibrated to high-resolution external literature sightlines (Sembach et al. 1993; Munari & Zwitter 1997; Welsh et al. 2010), with MaStar hot-star measurements included as supplementary data points in the fits; applying the resulting relation to MaStar is a standard calibration exercise rather than a definitional derivation. The reported reductions in W(Ca II K) and W(NaI D) are measured differences between original spectra and the replacement coadds or BOSZ models, not fitted parameters renamed as predictions. Likewise, the SSP enhancements are computed by comparing original and cleaned SSPs; they are not algebraically forced to equal the model's W_ISM. The internal robustness check in Section 3.6.4 is self-referential, as noted above, but it is not the central claim. The paper itself flags an unresolved 3–4σ offset between BOSZ and empirical low-ISM coadds for the eleven hottest stars in Section 3.3, with opposite interpretations that would shift the cleaned products in opposite directions; this is a correctness risk, not evidence of circular derivation. Self-citations to Lazarz et al. (2022) and Maraston et al. (2020) are externally published methodological inputs and are not used to forbid alternatives or to define the target result. Overall, the derivation is substantially independent even though one validation step is partly tautological.

Assumptions & free parameters 14 free parameters · 7 assumptions · 0 invented entities

The central claims rest on an empirical calibration with 54 fitted W_ISM model parameters, hand-chosen selection thresholds, and several domain assumptions about dust maps, stellar parameters, and model atmospheres. No new physical entities are introduced.

free parameters (14)
  • alpha_CaIIK_six_bins = 0.01, 0.05, -0.01, 0.22, 0.36, 0.17 Angstrom per log E_DustMap
    Slope of W_ISM versus log E_DustMap for Ca II K fitted to Sembach/Munari/Welsh data in six distance bins (Table 1).
  • beta_CaIIK_six_bins = 0.04, 0.14, 0.12, 0.40, 0.57, 0.57 Angstrom
    Intercept of the W_ISM relation for Ca II K in six distance bins (Table 1).
  • sigma_intr_CaIIK_six_bins = 0.03, 0.09, 0.12, 0.08, 0.06, 0.13 Angstrom
    Intrinsic scatter of the W_ISM relation for Ca II K (Table 1).
  • alpha_NaI5891_six_bins = 0.03, 0.11, 0.12, 0.60, 0.68, 0.66 Angstrom per log E_DustMap
    Slope of W_ISM versus log E_DustMap for Na I 5891 in six distance bins (Table 1).
  • beta_NaI5891_six_bins = 0.17, 0.29, 0.35, 0.84, 0.99, 0.98 Angstrom
    Intercept of the W_ISM relation for Na I 5891 (Table 1).
  • sigma_intr_NaI5891_six_bins = 0.09, 0.10, 0.17, 0.13, 0.11, 0.17 Angstrom
    Intrinsic scatter of the W_ISM relation for Na I 5891 (Table 1).
  • alpha_NaI5897_six_bins = 0.04, 0.12, 0.16, 0.54, 0.60, 0.63 Angstrom per log E_DustMap
    Slope of W_ISM versus log E_DustMap for Na I 5897 in six distance bins (Table 1).
  • beta_NaI5897_six_bins = 0.15, 0.26, 0.35, 0.71, 0.84, 0.83 Angstrom
    Intercept of the W_ISM relation for Na I 5897 (Table 1).
  • sigma_intr_NaI5897_six_bins = 0.07, 0.08, 0.14, 0.11, 0.09, 0.13 Angstrom
    Intrinsic scatter of the W_ISM relation for Na I 5897 (Table 1).
  • Distance bin boundaries = 0.0, 0.2, 0.4, 1.0, 2.0, 4.0, 20.0 kpc
    Hand-chosen bins in which the W_ISM relations are fitted separately; the bin edges affect the predicted W_ISM and therefore which stars are flagged low-ISM.
  • Low-ISM threshold for CaII K = 0.07 Angstrom
    Hand-relaxed from 0.05 to 0.07 Angstrom to improve parameter-space sampling (Section 2.3).
  • Low-ISM threshold for NaI 5891 = 0.05 Angstrom
    Hand-chosen criterion defining the standard low-ISM sample.
  • Supersolar low-ISM thresholds = 0.4 Angstrom (CaII K), 0.15 Angstrom (NaI 5891)
    Relaxed thresholds for the [Z/H]=+0.35 SSPs because few supersolar low-ISM stars exist (Section 3.6.2).
  • Psi replacement thresholds = 0.2 with N>=10, 0.6 with N>=5, 1.0 with N>=1
    Hand-chosen parameter-space distance thresholds controlling which coadd is used for empirical replacement (Section 3.2).
assumptions (7)
  • domain assumption The literature samples of Sembach et al. (1993), Munari & Zwitter (1997), and Welsh et al. (2010) are representative of interstellar CaII and NaI absorption toward all MaStar sightlines after distance and reddening scaling.
    Used in Sections 2.2-2.3 to build and apply the W_ISM model; if the scaling misses environmental variations, the low-ISM classification and cleaning are biased.
  • domain assumption The Green et al. (2019) 3D dust map and the Lazarz et al. (2022) relation AV = 3.31 E_DustMap - 0.076 give accurate reddening and extinction for every MaStar star.
    Distances and E_DustMap feed the W_ISM model; calibration errors propagate directly into predicted contamination.
  • domain assumption Stars with similar Teff, log g, and [Fe/H] have statistically interchangeable CaII and NaI D profiles.
    Coadd replacement in Sections 3.1-3.2 assumes this; it is tested only within the low-ISM sample, not against high-resolution observations of the same stars.
  • domain assumption BOSZ/ATLAS9 theoretical spectra correctly predict intrinsic CaII and NaI D profiles for Teff > 9000 K.
    Used for 738 stars lacking empirical matches; Section 3.3 reports a 3-4 sigma offset versus empirical coadds for the 11 stars where both are available.
  • domain assumption MaStar median stellar parameters and Gaia EDR3 photogeometric distances are sufficiently accurate for parameter matching.
    Parameter uncertainties enter Psi and could cause mismatched replacements; the paper notes Teff uncertainties up to 7861 K for A stars.
  • domain assumption Telluric absorption near NaI D is negligible for most sightlines.
    Appendix A quantifies 0.1-0.2 Angstrom effects for a small minority of spectra, and these are not corrected in the released data.
  • standard math Affine-invariant MCMC sampling and Gaussian likelihoods yield unbiased parameter estimates for the W_ISM relations.
    Section 2.2 uses emcee with noninformative priors; no formal proof of convergence is provided beyond the stated chain lengths.

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Cite this review

Pith. "Pith review of SDSS-IV MaStar: Quantification and Abatement of Interstellar Absorption in the Largest Empirical Stellar Spectral Library." pith.science (2026). https://pith.science/paper/NRMGPBDV

@misc{pith2026250209707,
  author       = {Pith},
  title        = {Pith review of: SDSS-IV MaStar: Quantification and Abatement of Interstellar Absorption in the Largest Empirical Stellar Spectral Library},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NRMGPBDV}},
  note         = {Machine review of arXiv:2502.09707}
}
abstract

We assess the impact of CaII 3934,3969 and NaI 5891,5897 absorption arising in the interstellar medium (ISM) on the SDSS-IV MaNGA Stellar Library (MaStar) and produce corrected spectroscopy for 80% of the 24,162-star catalog. We model the absorption strength of these transitions as a function of stellar distance, Galactic latitude, and dust reddening based upon high-spectral resolution studies. With this model, we identify 6342 MaStar stars that have negligible ISM absorption ($W^\mathrm{ISM}$(CaII K) $<0.07$ Ang and $W^\mathrm{ISM}$(NaI 5891) $<0.05$ Ang). For 12,110 of the remaining stars, we replace their NaI D profile (and their CaII profile for effective temperatures $T_{\rm eff}>9000$ K) with a coadded spectrum of low-ISM stars with similar $T_{\rm eff}$, surface gravity, and metallicity. For 738 additional stars with $T_{\rm eff}>9000$ K, we replace these spectral regions with a matching ATLAS9-based BOSZ model. This results in a mean reduction in $W$(CaII K) ($W$(NaI D)) of $0.4-0.7$ Ang ($0.6-1.1$ Ang) for hot stars ($T_{\rm eff}>7610$ K), and a mean reduction in $W$(NaI D) of $0.1-0.2$ Ang for cooler stars. We show that interstellar absorption in simple stellar population (SSP) model spectra constructed from the original library artificially enhances $W$(CaII K) by $\gtrsim20\%$ at young ages ($<400$ Myr); dramatically enhances the strength of stellar NaI D in starbursting systems (by ${\gtrsim}50\%$); and enhances stellar NaI D in older stellar populations (${\gtrsim}10$ Gyr) by ${\gtrsim}10\%$. We provide SSP spectra constructed from the cleaned library, and discuss the implications of these effects for stellar population synthesis analyses constraining stellar age, [Na/Fe] abundance, and the initial mass function.

Figures

Figures reproduced from arXiv: 2502.09707 by the authors.

Figure 1
Figure 1. Equivalent widths of the Ca II K (light and dark blue) and Na I 5897 (orange and red) transitions measured from the Rodr´ıguez-Merino et al. (2005) theoretical spectral templates. Measurements for solar-metallicity model spectra are shown in light blue and orange, and measurements for models with twice solar-metallicity are shown in dark blue and red. Measurements that fall below the range in W shown are indicated a… view at source ↗
Figure 2
Figure 2. Spectroscopy of the ten stars with the highest Teff,med in the high-quality MaStar sample. Each pair of stacked panels shows the same spectrum in windows surrounding the Ca II K and Na I λλ5891, 5897 transitions on top and bottom, respectively. Velocities are computed relative to the Ca II K λ3934 and Na I λ5897 rest wavelengths, and the gray vertical lines indicate these transitions along with the relative velocity… view at source ↗
Figure 3
Figure 3. Equivalent widths of interstellar Ca II K (top row), Na I 5891 (middle row), and Na I 5897 (bottom row) vs. EDustMap reported from analysis of high-spectral-resolution stellar spectroscopy by Sembach et al. (1993), Munari & Zwitter (1997), and Welsh et al. (2010). Detections and 2.5σ upper limits (reported by Welsh et al. 2010) are indicated with solid black circles and downward-pointing triangles, respectively. Eac… view at source ↗
Figures from the paper (24 more)
Figure 4
Figure 4. Figure 4: Cumulative distributions of log WISM for interstellar Ca II K (top row), Na I 5891 (middle row), and Na I 5897 (bottom row) for sightlines having EDustMap < 0.01 reported from analysis of stellar spectroscopy by Sembach et al. (1993), Munari & Zwitter (1997), and Welsh…
Figure 5
Figure 5. Figure 5: Top: Frequency distributions of EDustMap values for 23,991 MaStar targets having EDustMap ≥ 0, binned by spectral type as indicated in the legend. The smooth curves show continuous probability density curves corresponding to each histogram. Bottom: Frequency distributi…
Figure 6
Figure 6. Figure 6: The distribution of equivalent widths arising from interstellar absorption for the MaStar stellar sample, as predicted by the modeling described in Section 2.2. Distributions of WISM(Ca II K), WISM(Na I 5891), and WISM(Na I 5897) values are shown in the left, middle, a…
Figure 7
Figure 7. Figure 7: Stellar parameter distributions for the ≈24,000 unique stars in the MaStar sample (black). Each panel shows objects having [Fe/H] values between those listed at the top left. Red points indicate those stars with predicted ISM absorption strengths WISM(Ca II K) < 0.05 ˚…
Figure 8
Figure 8. Figure 8: Stellar parameter distributions for the full MaStar sample. Each panel shows objects having [Fe/H] values between those listed at the top left. Stars are color-coded by Ψmin, a measure of their distance in this parameter space from the nearest low-ISM sightline. The bl…
Figure 9
Figure 9. Figure 9: Demonstration of our spectral coadding algorithm for stars selected within Ψthresh = 0.4 of the parameter locations labeled ‘3’ (rows (a)-(d)) and ‘7’ (rows (e)-(h)) in [PITH_FULL_IMAGE:figures/full_fig_p013_9.png]
Figure 10
Figure 10. Figure 10: Left panels: The equivalent width of the Ca II K (top) and Na I D (bottom) transitions in the spectral coadds described in Section 3.1 as a function of Ψthresh (with Ψ representing the 3D parameter space distance from the parameter space location of each coadd). Point…
Figure 11
Figure 11. Figure 11: The distributions of the change in the Ca II K equivalent width in spectra “cleaned” with a replacement coadd relative to the original stellar spectra (∆W = Worig − Wcoadd) as a function of Ψthresh. Only sightlines that are not considered “low-ISM” and for which we ca…
Figure 12
Figure 12. Figure 12: Same as [PITH_FULL_IMAGE:figures/full_fig_p017_12.png]
Figure 13
Figure 13. Figure 13: The distributions of the change in Ca II K (left-hand panels) and Na I D (right-hand panels) equivalent widths in spectra “cleaned” with a replacement coadd relative to the original stellar spectra (∆W = Worig −Wcoadd). Only sightlines that are not considered “low-ISM…
Figure 14
Figure 14. Figure 14: Top panels: The difference in the W measured for Ca II K (left) and Na I D (right) in the spectra “cleaned” with BOSZ theoretical templates and that measured in the original spectra, plotted vs. Teff,med. Bottom panels: Same as above, for the difference in W measured …
Figure 15
Figure 15. Figure 15: The transparent histogram in each panel 3 2 1 0 1 2 3 W(CaII K) (Å) 10 2 10 1 10 0 10 1 0.44 Å Density Distribution 3 2 1 0 1 2 3 W(CaII K) (Å) 10 2 10 1 10 0 10 1 0.65 Å 3 2 1 0 1 2 3 W(CaII K) (Å) 10 2 10 1 10 0 10 1 0.49 Å 2 1 0 1 2 3 W(NaI D) (Å) 10 2 10 1 10 0 10…
Figure 16
Figure 16. Figure 16: Comparison of hierarchically-clustered MaStar spectral templates constructed without correction for ISM absorption (black) and from our “cleaned” spectral sample (orange). Each pair of stacked panels shows the same template at the locations of the Ca II K and Na I λλ5…
Figure 17
Figure 17. Figure 17: Comparison of MaStar SSP spectral templates constructed without correction for ISM absorption (black) and from our “cleaned” spectral sample (orange). Results for SSP templates constructed solely from low-ISM stars as described in Section 3.6.4 are shown with dashed c…
Figure 18
Figure 18. Figure 18: The difference between the NaD spectral index measured in the original MaStar spectra and that measured in the cleaned spectra vs. stellar [Fe/H]. Left: NaDorig − NaDclean for dwarf stars (with log g > 4) divided into three temperature bins. Each point shows the avera…
Figure 19
Figure 19. Figure 19: The difference between W(Ca II K) measured in the original MaStar spectra and that measured in the cleaned spectra vs. stellar [Fe/H] for O/B/A-type stars. Results for dwarf stars (with log g > 4) are shown with small dark blue circles, and results for giant stars are…
Figure 20
Figure 20. Figure 20: Fractional enhancement due to interstellar absorption of the equivalent width of Ca II K (gray) and the NaD spectral index (purple) for solar-metallicity (solid) and [Z/H] = −1.35 (dashed-dotted) SSPs. The violet curves show the fractional NaD enhancement estimated re…
Figure 21
Figure 21. Figure 21: Distributions of the atmospheric conditions for all high-quality exposures used in “good” visit spectra in the MaStar library. This includes all spectra with no MASTAR QUAL flags set. The median of each distribution is indicated in dark blue, with the 16th- and 84th-p…
Figure 22
Figure 22. Figure 22: Panels (a)-(f ): The atmospheric transmission spectrum predicted by TelFit/LBLRTM for Apache Point Obser￾vatory for an air mass = 1.1, 30% relative humidity, atmospheric pressure = 730 mmHg, and an air temperature of 5.5 ◦C is shown in orange. The black spectra show a…
Figure 23
Figure 23. Figure 23: The BOSZ model spectra (black), telluric absorption models (orange and red), and combined spectra (cyan) shown in [PITH_FULL_IMAGE:figures/full_fig_p036_23.png]
Figure 24
Figure 24. Figure 24: Equivalent width enhancement due to telluric absorption within the Na I D spectral window predicted by TelFit/LBLRTM for APO. All models shown adopt atmospheric pressures of 730 mmHg. Each contour shows the full range of equivalent width enhancements exhibited by the …
Figure 25
Figure 25. Figure 25: Comparison of hierarchically-clustered MaStar spectral templates constructed without correction for ISM absorption (black) and from our “cleaned” spectral sample (orange). This is a multipage continuation of [PITH_FULL_IMAGE:figures/full_fig_p038_25.png]
Figure 25
Figure 25. Figure 25: – continued [PITH_FULL_IMAGE:figures/full_fig_p039_25.png]
Figure 25
Figure 25. Figure 25: – continued [PITH_FULL_IMAGE:figures/full_fig_p040_25.png]

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