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arxiv: 2607.06143 · v1 · pith:4HL7CMDV · submitted 2026-07-07 · astro-ph.GA

Deep far-UV observations of the ELAIS N1 field using AstroSat: Source catalogue, spectral energy distribution modelling and star formation

Pranjal Chaturrvedi , Akrtiti Sinha , Abhirup Datta , Kanak Saha This is my paper

Reviewed by Pith T0 review T1 audit T2 compute T3 formal T4 kernel 2026-07-08 15:10 UTCglm-5.2pith:4HL7CMDVrecord.jsonopen to challenge →

classification astro-ph.GA
keywords far-ultraviolet photometryAstroSat UVITELAIS N1star-forming main sequencespectral energy distributionCIGALEstellar massstar formation rate
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The pith

Galaxies keep a steady recipe for star formation across 7 billion years

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

This paper presents a deep far-ultraviolet survey of the ELAIS N1 field using the AstroSat/UVIT telescope, achieving angular resolution more than three times better than previous UV missions. After cross-matching UV detections with optical and infrared catalogs and removing active galactic nuclei, the authors fit spectral energy distributions for a sample of star-forming galaxies spanning 0 < z < 0.76, covering roughly the last 7 billion years of cosmic history. They find that star formation rates increase with redshift as expected, and that the ratio of young stellar mass to total stellar mass stays approximately constant at ~10^-3 (about 0.1 percent) across the entire redshift range. The authors interpret this constancy as evidence that these galaxies are growing through steady, self-regulated gas accretion rather than violent merger-driven starbursts.

Core claim

The ratio of young stellar mass to total stellar mass remains flat at approximately 10^-3 across 0 < z < 0.76, meaning that at every epoch surveyed, newly formed stars constitute only about one-tenth of one percent of a galaxy's total stellar backbone. The authors argue this is the quantitative signature of secular, self-regulated evolution on the star-forming main sequence, not starburst-driven assembly.

What carries the argument

The central machinery is the CIGALE spectral energy distribution fitting pipeline, configured with a delayed star formation history plus an optional late burst. The load-bearing parameter is the late-burst mass fraction, constrained to the range 0.00-0.01. The observed flatness of the young-to-total mass ratio at ~10^-3 is shown to mirror this prior constraint, which the authors present as validation of both the model assumptions and the secular evolution interpretation.

If this is right

  • If the flat mass ratio is genuinely physical and not an artifact of model priors, it provides a simple quantitative benchmark—~0.1% young stellar mass fraction—that any star-forming main sequence galaxy at z < 1 should satisfy, useful for classifying outliers as starbursts or post-starburst systems.
  • The UVIT FUV catalog at 25.69 m_AB depth with ~1.5 arcsec resolution provides a new source list for the ELAIS N1 legacy field, enabling cross-comparison with existing radio catalogs from LOFAR and uGMRT to study the relationship between UV-traced and bolometric star formation.
  • The monotonic rise in median SFR from <1 to ~4.5 solar masses per year across the surveyed redshift range independently traces the ascending slope of the cosmic star formation history in this field, consistent with established large-survey results.
  • The mass completeness limit rising sharply with redshift—reaching ~10^10.7 solar masses by z ~0.55—defines the regime where evolutionary comparisons are statistically valid, cautioning against over-interpreting the low-mass population at higher redshifts.

Where Pith is reading between the lines

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

  • The paper states that the observed mass ratio 'perfectly mirrors the constrained late-burst mass fractions' and 'directly validates the parametric assumptions.' This circularity means the flat ratio could be a consequence of the model prior rather than an independent physical measurement. A test with unconstrained or differently constrained burst fractions would clarify whether the data themselves
  • If the flat ratio survives such tests, it could serve as a redshift-independent diagnostic: any galaxy deviating significantly upward from 10^-3 would be flagged as a starburst candidate, providing a selection tool that does not require full SED fitting.
  • Extending this analysis to z > 1, where the cosmic star formation rate density peaks, would test whether the constant ratio breaks down near cosmic noon or persists, with implications for whether the secular mode dominates even at epochs of peak cosmic activity.

Load-bearing premise

The SED fitting pipeline constrains the late-burst stellar mass fraction to the range 0.00-0.01, and the observed flat young-to-total mass ratio at ~10^-3 falls directly within this prior. The claim that the data validate the model is therefore partly circular: the model was told the answer could not exceed 1%, and the data agreed.

What would settle it

If the same galaxies, fitted with an unconstrained or much wider late-burst mass fraction prior, produced young-to-total mass ratios that scatter well above 10^-3 or show redshift-dependent trends, the secular evolution conclusion would need to be revisited.

Figures

Figures reproduced from arXiv: 2607.06143 by Abhirup Datta, Akrtiti Sinha, Kanak Saha, Pranjal Chaturrvedi.

Figure 1
Figure 1. Figure 1: ELAIS N1 field observed by AstroSat/UVIT in FUV using F154W filter with some sources selected based on visual morphology overlaid. The sources are described in sec 2. and we then select 3 bright sources visible across all images to get a merged image. We optimised the PSF to eliminate the remaining drift that had been missed earlier. The resulting image is displayed in [PITH_FULL_IMAGE:figures/full_fig_p0… view at source ↗
Figure 2
Figure 2. Figure 2: The PSF obtained by fitting the Moffat function using its surface brightness distribution to measure the FWHM (see section 2.1). the centroid. Then we use the photutils.profiles (Bradley et al. 2024) to create the radial profile and curve of growth of the median stacked image. The radius at the 80% flux was found to be 9.14 arcsec (3.81 pixels). We use the circular Moffat function (Moffat 1969) to fit the … view at source ↗
Figure 3
Figure 3. Figure 3: Distribution of the dereddened F154W magnitude [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: shows the distribution of the redshift of the sources. The sources have a median redshift of 0.24. 20 21 22 23 24 25 FUVAB 10 0 10 1 10 2 Number of Sources 3 5 3 limiting mag 5 limiting mag [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 6
Figure 6. Figure 6: The SFR of the galaxies plotted against the redshift in red markers. 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 Redshift 10 3 10 4 10 5 10 6 10 7 10 8 10 9 10 10 10 11 lo g(M star [M ]) Stellar Mass Median Stellar Mass with 1 scatter Young ( 1 Gyr) Stellar Mass Median Young Stellar Mass with 1 scatter 0.0 2.4 4.3 5.7 6.8 7.7 Lookback Time [Gyr] [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: The logarithm of the stellar mass of the galaxies is plotted against the redshift in red markers and the logarithm of the young stellar mass of the galaxies is plotted against the redshift in blue markers. contributor to the global baryonic mass budget. Ultimately, this in￾variant ratio underscores the steady-state nature of mass assembly for intermediate-to-high mass galaxies over the past several billion… view at source ↗
Figure 5
Figure 5. Figure 5: SED fits of a few selected sources with their cutouts in the FUV band from UVIT and the r band from SDSS; the cutouts are 20 arcsec on both axes. 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 Redshift 10 3 10 2 10 1 10 0 10 1 lo g(S F R [M y r 1 ]) SFR Data Points Median SFR with 1 scatter 0.0 2.4 4.3 5.7 6.8 7.7 Lookback Time [Gyr] [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 8
Figure 8. Figure 8: The logarithm of the ratio of the mass of the young stars to the total mass of the galaxies is plotted against the redshift in red markers. photometry and spectroscopy from SDSS/BOSS, mid-infrared data from the SWIRE survey, and highly accurate photometric redshifts derived from the LoTSS deep field survey. After isolating AGN using established multi-wavelength criteria, our final sample consists of star-f… view at source ↗
read the original abstract

We present a far-ultraviolet (FUV) photometric study of the ELAIS N1 deep field using the Ultra-Violet Imaging Telescope (UVIT) onboard AstroSat, observed in the F154W filter ($\lambda_{\rm eff} = 1541$\,\AA) with a total on-source exposure time of 30\,ksec. Level 1 data were reduced using CCDLAB v3.0, yielding source catalogues of 1637 objects at $3\sigma$ and 458 objects at $5\sigma$, with limiting magnitudes of $25.69\,m_{AB}$ and $25.13\,m_{AB}$ respectively. FUV positions are cross-matched against multiwavelength catalogues spanning optical and infrared wavelengths, with redshifts drawn from spectroscopic and photometric sources. Active galactic nuclei (AGN) are identified and excluded via established multiwavelength criteria, leaving a clean sample of star-forming galaxies (SFGs). Spectral energy distribution (SED) modelling is performed using CIGALE, employing a delayed star formation history with an optional late burst, Bruzual \& Charlot stellar population synthesis, Calzetti dust attenuation, and the SKIRTOR AGN module. From the best-fit models, we derive star formation rates (SFRs), total stellar masses, and young stellar masses as a function of redshift. The SFR increases monotonically with redshift, consistent with the evolution of the Star Formation Main Sequence (SFMS). The ratio of young-to-total stellar mass remains approximately constant across $0 < z \lesssim 0.76$, confirming that the sample consists predominantly of secularly evolving systems undergoing steady, self-regulated star formation rather than starburst-driven episodes.

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

3 major / 10 minor

Summary. This paper presents deep far-ultraviolet (FUV) imaging of the ELAIS N1 field using AstroSat/UVIT in the F154W filter, achieving 3σ and 5σ detection limits of 25.69 and 25.13 m_AB, respectively. The authors produce source catalogues (1637 objects at 3σ), cross-match with multiwavelength ancillary data (SDSS, SWIRE), and perform SED fitting using CIGALE to derive star formation rates, stellar masses, and young stellar mass fractions for a sample of star-forming galaxies spanning 0 < z ≲ 0.76. The data reduction and catalogue generation appear standard and competent, and the SFR–redshift trend is consistent with known evolution of the star formation main sequence. The paper's central interpretive claim is that the ratio of young-to-total stellar mass remains flat at ~10⁻³ across the full redshift range, which the authors interpret as evidence for secular, non-starburst evolution.

Significance. The FUV source catalogue itself is a useful contribution, providing a factor-of-three improvement in angular resolution over GALEX in this well-studied legacy field. The SED fitting methodology is standard and the multiwavelength cross-matching is thorough. However, the paper's central scientific claim about the flat young mass ratio is, as discussed below, a direct consequence of the model priors rather than an independent observational result, which substantially diminishes the significance of the interpretive conclusions. The SFR–redshift trend, while consistent with the literature, is not novel on its own.

major comments (3)
  1. §5.2, Table 4, Table 6: The central claim that the young-to-total stellar mass ratio is flat at ~10⁻³ is not an independent observational result but a direct reflection of the CIGALE prior. Table 4 constrains the late-burst mass fraction to {0.0, 0.005, 0.01}, and Table 6 shows the fitted mean is ~0.008 with SD ~0.004, clustering near the upper allowed bound. The paper itself acknowledges this in §5.2: 'the observed mass ratio perfectly mirrors the constrained late-burst mass fractions.' Yet the authors frame this as validation: 'this empirical result robustly validates the parametric assumptions embedded within our CIGALE SED modelling.' This is logically circular: a result that mirrors its own prior cannot validate that prior. The claim that the flat ratio 'confirms secular evolution' is therefore unsupported by the analysis as presented. The authors need to either (a) demonstrate that
  2. §5.2, Table 6: The fitted late-burst mass fractions cluster near the upper bound of the allowed range (mean ~0.008 vs. maximum 0.01), suggesting the data may prefer higher values if the parameter space were extended. This saturation near the boundary is a warning that the prior is too restrictive. The authors should either widen the allowed burst fraction range (e.g., to 0.0–0.1) and re-run the fits, or explicitly acknowledge that the flat mass ratio is a model artifact and remove the claim that it independently confirms secular evolution.
  3. §5.2, Figure 8, Table 5: The claim that a young mass fraction of ~0.1% is 'a classic, quantitative signature of mature, secularly evolving galaxies situated firmly on the SFMS' is not supported by any cited comparison value. No reference is provided for what young mass fraction starbursting systems would exhibit, nor for what main-sequence galaxies should exhibit. The assertion that starbursts would produce fractions of '1% to 10%' is stated without citation. This interpretive claim needs either a quantitative comparison with literature values or should be removed.
minor comments (10)
  1. §3.2: The final sample size of star-forming galaxies used for SED fitting is not clearly stated. The text says 23 AGN are identified from 1637 3σ sources, but the number of galaxies with sufficient multiwavelength photometry for SED fitting is not explicitly given. Please add this.
  2. Table 4: The dust attenuation parameters appear to have the color excess values for young and old stars possibly swapped or mislabeled — young stars have E(B-V)=0.005 while old stars have E(B-V)=0.3, 0.1. Typically young stars have higher extinction. Please verify.
  3. Table 5: The formatting of the uncertainties is unclear, particularly the parenthetical notation for the mass ratio column (e.g., '(112±5.55) × 10⁻⁵'). Please standardize the notation.
  4. Table 6: The reduced χ² values range from ~1.4 to ~2.5, which is somewhat high. A brief discussion of fit quality would be appropriate.
  5. §2.3.1: The text mentions 'A series of plates were granted to observe and obtain spectra for the sources in the ELAIS N1 observed in radio wavelengths using GMRT, JVLA, LOFAR and FIRST.' This sentence is grammatically unclear.
  6. §5.1: The lookback time axis on Figures 6–8 is shown but not discussed in the text. Either add discussion or remove the axis.
  7. Figure 1: The overlaid sources are described in the text but not labeled on the figure itself, making cross-referencing difficult.
  8. §1: 'has been observed observed' — duplicated word.
  9. §1: 'propoerties' — typo.
  10. The abstract states the redshift range as z ≲ 0.76, but §5 and the conclusions refer to z < 0.6. Please reconcile.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for a careful and constructive report. The referee's three major comments all concern the same core issue: the interpretation of the flat young-to-total stellar mass ratio in §5.2. We agree with the referee that the current framing is logically circular and that the claims about secular evolution are not independently supported by the analysis as presented. We will revise the manuscript accordingly. Point-by-point responses follow.

read point-by-point responses

  1. Referee: §5.2, Table 4, Table 6: The central claim that the young-to-total stellar mass ratio is flat at ~10⁻³ is not an independent observational result but a direct reflection of the CIGALE prior. Table 4 constrains the late-burst mass fraction to {0.0, 0.005, 0.01}, and Table 6 shows the fitted mean is ~0.008 with SD ~0.004, clustering near the upper allowed bound. The paper itself acknowledges this in §5.2: 'the observed mass ratio perfectly mirrors the constrained late-burst mass fractions.' Yet the authors frame this as validation: 'this empirical result robustly validates the parametric assumptions embedded within our CIGALE SED modelling.' This is logically circular: a result that mirrors its own prior cannot validate that prior. The claim that the flat ratio 'confirms secular evolution' is therefore unsupported by the analysis as presented.

    Authors: The referee is correct. We concede that the flat young-to-total mass ratio is a direct consequence of the CIGALE prior on the late-burst mass fraction (0.0–0.01) and cannot serve as independent validation of that prior or as standalone evidence for secular evolution. The sentence stating that the empirical result 'robustly validates the parametric assumptions' is logically circular and will be removed. We will also remove the claim that the flat ratio 'confirms secular evolution' from the abstract and conclusions. The revised manuscript will reframe §5.2 as follows: the flat mass ratio is consistent with the model assumption that recent star formation contributes a small fraction of the total stellar mass, but we will explicitly state that this consistency is a consequence of the prior and does not constitute an independent observational test. The evidence for secular evolution in our sample will instead rest on (i) the SFR–stellar mass trend being consistent with the known SFMS evolution and (ii) the absence of a significant population of outliers with elevated SFRs at fixed mass, rather than on the young mass fraction. revision: yes

  2. Referee: §5.2, Table 6: The fitted late-burst mass fractions cluster near the upper bound of the allowed range (mean ~0.008 vs. maximum 0.01), suggesting the data may prefer higher values if the parameter space were extended. This saturation near the boundary is a warning that the prior is too restrictive. The authors should either widen the allowed burst fraction range (e.g., to 0.0–0.1) and re-run the fits, or explicitly acknowledge that the flat mass ratio is a model artifact and remove the claim that it independently confirms secular evolution.

    Authors: We agree that the clustering near the upper bound is a warning sign that the prior may be too restrictive. We will widen the late-burst mass fraction grid to include values up to 0.1 (specifically: 0.0, 0.005, 0.01, 0.02, 0.05, 0.1) and re-run the CIGALE fits for the full sample. We will report the revised distribution of fitted burst fractions and the revised young-to-total mass ratio as a function of redshift. If the data continue to prefer low burst fractions (≲0.01), this would provide genuine, non-circular evidence that the sample is dominated by secularly evolving systems. If the fits migrate to higher burst fractions, we will report that honestly and revise our interpretation accordingly. In either case, we will remove the circular claim from the current version. We note that the re-running will require approximately 2–3 weeks of computation time; the revised manuscript will include the updated results. revision: yes

  3. Referee: §5.2, Figure 8, Table 5: The claim that a young mass fraction of ~0.1% is 'a classic, quantitative signature of mature, secularly evolving galaxies situated firmly on the SFMS' is not supported by any cited comparison value. No reference is provided for what young mass fraction starbursting systems would exhibit, nor for what main-sequence galaxies should exhibit. The assertion that starbursts would produce fractions of '1% to 10%' is stated without citation. This interpretive claim needs either a quantitative comparison with literature values or should be removed.

    Authors: The referee is correct that the specific quantitative claims about expected young mass fractions for starbursting versus main-sequence galaxies are unsupported by citations. We were unable to find published literature that provides direct, comparable measurements of the young-to-total stellar mass fraction (as defined by CIGALE's sfhdelayed module with a 10 Myr age separation) for starburst and main-sequence samples. The values of '1% to 10%' for starbursts were our own estimate based on the typical SFR enhancement factors used to define starbursts (e.g., SFR/SFR_MS > 2–4; Rodighiero et al. 2011; Elbaz et al. 2011), but we agree this translation to a young mass fraction is not rigorous without a direct calculation. We will remove the unsupported quantitative comparison and the phrase 'classic, quantitative signature.' The revised text will state only that the young mass fraction is low and consistent with the model assumption of a minor recent star formation episode, without claiming it as a diagnostic signature of secular evolution. If the re-run with widened burst fractions (see previous response) yields a meaningful comparison, we will include it; otherwise, the interpretive claim will be removed entirely. revision: yes

Circularity Check

2 steps flagged

Flat young-to-total mass ratio (~10^-3) is a direct output of the CIGALE late-burst mass fraction prior (0.00–0.01), making the claimed 'validation' of secular evolution circular.

specific steps
  1. fitted input called prediction [Table 4 (CIGALE input parameters) and Section 5.2]
    "Mass fraction of late burst population 0.0, 0.005, 0.01 [...] The observed mass ratio perfectly mirrors the constrained late-burst mass fractions (set at 0.00 to 0.01) utilised within the sfhdelayed module. [...] this empirical result robustly validates the parametric assumptions embedded within our CIGALE SED modelling."

    The CIGALE sfhdelayed module constrains the late-burst mass fraction to {0.0, 0.005, 0.01} (Table 4). Table 6 shows the fitted mean late-burst fraction is ~0.008 with SD ~0.004, clustering near the upper allowed bound of 0.01. The 'young stellar mass' (stars < 10 Myr, per the age separation parameter in Table 4) is a sub-component of this late burst population, modulated by the burst age (250–750 Myr) and e-folding time (50–100 Myr). Therefore M_young/M_total is not independently measured; it is almost entirely determined by the prior on the burst mass fraction. The authors acknowledge this ('the observed mass ratio perfectly mirrors the constrained late-burst mass fractions') yet frame it as validation ('robustly validates the parametric assumptions'), which is logically inverted: a ratio

  2. self definitional [Section 5.2 and Conclusion (Section 6)]
    "The observed mass fraction directly validates the constrained late-burst mass fractions (set to 0.00–0.01) within the sfhdelayed CIGALE module. This result is consistent with the picture of Madau & Dickinson (2014), wherein the bulk of cosmic stellar mass was assembled at the peak of cosmic star formation (z∼2), with present-day galaxies adding only marginal new stellar mass relative to their total assembled budget."

    The paper's central scientific claim — that the constant young mass fraction ~10^-3 confirms secular, non-starburst evolution — is shown by the paper's own text to be a direct reflection of the input parameters. The CIGALE sfhdelayed module constrains the late-burst mass fraction to {0.0, 0.005, 0.01} (Table 4), and Section 5.2 states the observed mass ratio 'perfectly mirrors the constrained late-burst mass fractions' and 'directly validates the parametric assumptions.' A result that mirrors its own prior cannot validate that prior. If the allowed burst fractions were extended to, say, 0.0–0.1, the data might well prefer higher values (given that the current fits saturate near the upper bound of 0.01), which would raise M_young/M_total and potentially change the interpretation from 'secu

full rationale

The paper's central claim — that the flat young-to-total stellar mass ratio (~10^-3) confirms secular, non-starburst evolution — is circular. The CIGALE sfhdelayed module constrains the late-burst mass fraction to {0.0, 0.005, 0.01} (Table 4). Table 6 shows the fitted mean late-burst fraction is ~0.008 with SD ~0.004, clustering near the upper allowed bound. The 'young stellar mass' (stars < 10 Myr per the age separation parameter) is a sub-component of this late burst population, so M_young/M_total is almost entirely determined by the prior on the burst mass fraction, not independently measured. The authors explicitly acknowledge this: 'the observed mass ratio perfectly mirrors the constrained late-burst mass fractions.' Yet they frame this as validation ('robustly validates the parametric assumptions'), which is logically inverted — a result that mirrors its own prior cannot validate that prior. The SFR-redshift trend and Malmquist bias discussion are independently grounded in external literature and not circular. But the load-bearing claim about secular evolution rests on a quantity that is forced by the model prior by construction.

Axiom & Free-Parameter Ledger

10 free parameters · 4 axioms · 0 invented entities

The paper uses standard SED fitting tools and established physical models. No new physical entities or forces are postulated. The free parameters are all part of the standard CIGALE fitting framework.

free parameters (10)
  • e-folding time of main stellar population = 2000, 4000, 6000, 8000 Myr
    CIGALE SED fitting parameter grid (Table 4).
  • Age of main stellar population = 6000, 8000, 10000, 12000 Myr
    CIGALE SED fitting parameter grid (Table 4).
  • e-folding time of late starburst population = 50, 100 Myr
    CIGALE SED fitting parameter grid (Table 4).
  • Age of late burst population = 250, 500, 750 Myr
    CIGALE SED fitting parameter grid (Table 4).
  • Mass fraction of late burst population = 0.0, 0.005, 0.01
    CIGALE SED fitting parameter grid (Table 4). This parameter directly constrains the claimed flat young mass ratio.
  • Stellar metallicity = 0.02, 0.05
    CIGALE SED fitting parameter grid (Table 4).
  • Color excess of stellar continuum (old stars) = 0.3, 0.1
    CIGALE SED fitting parameter grid (Table 4).
  • Amplitude of UV bump = 0.0, 2.0
    CIGALE SED fitting parameter grid (Table 4).
  • Slope of attenuation curve power law = -0.3, -0.1, 0
    CIGALE SED fitting parameter grid (Table 4).
  • AGN fraction (SKIRTOR) = 0.05
    CIGALE SED fitting parameter grid (Table 4).
axioms (4)
  • domain assumption Delayed star formation history with optional late burst is a valid model for these galaxies.
    Section 4.1. The choice of sfhdelayed module in CIGALE is a standard but unproven assumption for individual galaxies.
  • domain assumption Calzetti dust attenuation law is applicable to this sample.
    Table 4. Standard assumption in extragalactic SED fitting.
  • domain assumption Photometric redshifts from Duncan et al. (2021) are sufficiently accurate for SED fitting.
    Section 2.4. The paper uses photo-z for the majority of sources, with scatter < 0.04*(1+z).
  • domain assumption The AGN classification criteria from Duncan et al. (2021) successfully isolate a clean sample of SFGs.
    Section 3.2. The paper relies on external criteria to remove AGN contamination.

pith-pipeline@v1.1.0-glm · 21297 in / 2850 out tokens · 277973 ms · 2026-07-08T15:10:48.352656+00:00 · methodology

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