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Six new spectroscopic redshifts secure distances for bright SMILE radio AGN missing reliable z.

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2026-07-11 10:53 UTC pith:Z4U6YYWD

load-bearing objection Solid incremental data paper: six new spectroscopic redshifts for SMILE flat-spectrum sources, methods standard and cross-checked.

arxiv 2607.04959 v1 pith:Z4U6YYWD submitted 2026-07-06 astro-ph.CO astro-ph.GA

Spectroscopic redshifts of selected flat-spectrum radio sources I

Dmitry Blinov , Alberto Floris , Andreas Zezas , Carolina Casadio , Elias Kyritsis , Valentina Missaglia , Vangelis Pantoulas , Avinash Kumar This is my paper
classification astro-ph.CO astro-ph.GA
keywords Galaxy spectroscopyQuasarsRedshiftedSpectral line identificationmilli-lensesVLBIflat-spectrum radio sourcesSMILE
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The Search for Milli-Lenses (SMILE) needs reliable distances for roughly five thousand flat-spectrum radio-loud active galaxies so that milli-arcsecond VLBI image separations can be turned into physical sizes, false compact-symmetric-object contaminants can be rejected, and lensing statistics can be computed. Catalogs leave hundreds of targets without any redshift and nearly a thousand with only inconsistent photometric estimates. This first paper of a dedicated follow-up campaign reports optical spectra of the brightest such targets taken with the Skinakas 1.3 m telescope. Secure emission-line redshifts are obtained for six of the fifteen sources observed, with values that lie between the scattered photometric guesses and are precise enough for linear-scale work. The measurements close a concrete data gap that otherwise limits both the milli-lens search and broader population studies of the sample.

Core claim

New spectroscopic redshifts are measured for six SMILE targets previously lacking secure z_spec: J010341+423925 at 0.1230 ± 0.0002, J184835+213156 at 0.0854 ± 0.0006, J195141+480145 at 0.05586 ± 0.00002, J201414+063439 at 0.1486 ± 0.0008, J203142+162147 at 0.1349 ± 0.0003, and J222252+144119 at 0.0660 ± 0.0002, all derived from Gaussian fits to identified optical lines in Skinakas 1.3 m spectra.

What carries the argument

Weighted-mean redshift from Gaussian centroids of multiple emission lines (Hα, [N II], [O III], [O I], [S II], etc.), with uncertainties propagated from both the wavelength-calibration polynomial and the line-centroid fits, applied to continuum-normalized Skinakas spectra.

Load-bearing premise

That the optical object placed in the slit is the true counterpart of the radio source and that the lines used for the redshift are correctly identified rather than misassigned blends or noise spikes, especially in the lower-signal spectra.

What would settle it

An independent spectrum of any of the six sources that yields a statistically inconsistent redshift, or high-resolution imaging that shows the optical continuum used for the slit placement is not the radio AGN host.

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

0 major / 6 minor

Summary. This paper reports the first results of a spectroscopic follow-up campaign for the SMILE sample of ~5000 flat-spectrum radio sources. After compiling redshifts from multiple catalogs and finding 491 sources with no redshift and 948 with only photometric estimates (often discrepant), the authors observed 15 of the brightest targets lacking secure z_spec with the Skinakas 1.3 m telescope. They present newly measured spectroscopic redshifts for six sources (J010341+423925 z=0.1230±0.0002; J184835+213156 z=0.0854±0.0006; J195141+480145 z=0.05586±0.00002; J201414+063439 z=0.1486±0.0008; J203142+162147 z=0.1349±0.0003; J222252+144119 z=0.0660±0.0002), based on Gaussian fits to identified optical emission lines (primarily Hα, [N II], [O III], [O I], [S II]). Four additional sources later received independent spectroscopic redshifts (DESI, LAMOST, OCARS) that agree with the authors’ measurements within the quoted uncertainties, and five sources yielded no usable lines. Spectra, line identifications, and comparisons to photometric estimates are provided, with data to be released on Harvard Dataverse.

Significance. Reliable spectroscopic redshifts are a practical bottleneck for the SMILE milli-lens search and for VLBI population studies more generally: they convert angular scales to physical sizes (critical for rejecting compact symmetric objects), enable luminosity estimates, and enter lensing cross-section calculations. The paper supplies six new secure z_spec values for bright CLASS/SMILE sources that previously lacked them, validates the reduction and line-fitting pipeline against four independent later measurements, and documents the remaining incompleteness. The contribution is incremental observational data rather than a new method or statistical result, but it is carefully executed, transparent about non-detections, and directly usable by the community. Strengths include multi-line redshifts with propagated uncertainties, explicit photometric comparisons, and planned public release of the normalized spectra.

minor comments (6)
  1. Section 3.4 and 3.5 (J201414+063439, J203142+162147): average SNR per pixel is ~6 and the spectra are shown both raw and Savitzky–Golay smoothed. A short quantitative note on how the smoothing window was chosen and whether line centroids were measured on the raw or smoothed data would strengthen reproducibility for the lower-SNR cases.
  2. Section 2: the wavelength solution uses a second-degree polynomial over ~15 He/Ne/Ar lines (5850–8520 Å) with RMS residuals recorded per exposure. Reporting the typical RMS (or a range) in the text or Table 1 would help readers assess the contribution of the dispersion solution to the final redshift uncertainties.
  3. Table 1 and Section 3.7: the classification column follows OCARS (G, AL, AQ, V). A one-sentence reminder in the table note that these are literature classifications (not derived from the new spectra) would avoid any ambiguity, especially for the BL Lac candidates that showed no lines.
  4. Section 3.1–3.6: photometric redshifts from PS1-STRM, 2MPZ, CatGlobe, QZO, etc., are quoted with heterogeneous precision and error bars. A brief remark that the photometric uncertainties are catalog-reported (and often underestimate catastrophic failures) would clarify why the spectroscopic values are preferred even when they lie near the photometric means.
  5. Figure captions: Figures 4 and 5 note that the black line is a smoothed version; stating the filter parameters (window length, polynomial order) in the caption or methods would be useful for readers who re-use the spectra.
  6. Minor typographical consistency: “N II” vs “[N II]” and “H 6563” vs “Hα” appear interchangeably in the text and figure labels; standardizing on the conventional spectroscopic notation would improve readability.

Circularity Check

0 steps flagged

No circularity: spectroscopic redshifts are measured directly from observed emission-line centroids against laboratory rest wavelengths, independent of photometric inputs or self-cited premises.

full rationale

This is a straightforward observational data paper. The six new redshifts (and four confirmatory ones) are obtained by identifying optical emission lines in Skinakas spectra, fitting Gaussians to their centroids, and computing the weighted mean redshift relative to laboratory rest wavelengths (Section 2 and 3). Photometric catalog values are used only for target selection and post-hoc consistency checks; they do not enter the spectroscopic z calculation. Self-citations (Casadio et al. 2021 for the SMILE sample definition; later DESI/LAMOST/OCARS matches) supply context or external validation, not load-bearing premises that force the reported z values. There is no fitted parameter re-labeled as a prediction, no uniqueness theorem imported from the authors, and no ansatz smuggled via citation. The derivation chain is self-contained against external laboratory wavelengths and the raw spectra; circularity score is therefore zero.

Axiom & Free-Parameter Ledger

0 free parameters · 3 axioms · 0 invented entities

The paper is an observational redshift catalog. It relies on standard spectroscopic practice and laboratory rest wavelengths rather than free parameters or newly invented physical entities. The main domain assumptions are correct optical–radio association and correct line identification.

axioms (3)
  • domain assumption Laboratory rest wavelengths of common AGN emission lines (Hα 6563 Å, [N II] 6548/6583 Å, [O III] 4959/5007 Å, [O I] 6300 Å, [S II] 6716/6731 Å, etc.) are known to high accuracy and can be used to convert observed centroids into redshift.
    Invoked throughout §2–3 when converting fitted line positions to z.
  • domain assumption The optical continuum source placed in the slit is the counterpart of the CLASS radio position (within the stated positional consistency).
    Stated for each source in §3; one counter-example (J182911+272924) is identified as a star via Gaia proper motion and spectrum.
  • domain assumption A second-degree polynomial wavelength solution from ~15 He/Ne/Ar lines spanning 5850–8520 Å is adequate for the required redshift precision.
    Described in the data-reduction section; RMS residuals are recorded but not tabulated per exposure.

pith-pipeline@v1.1.0-grok45 · 16067 in / 2304 out tokens · 16569 ms · 2026-07-11T10:53:30.884640+00:00 · methodology

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read the original abstract

We present the first results of a spectroscopic campaign carried out as part of the Search for Milli-Lenses (SMILE) program, which aims to constrain the prevalence of gravitational lens systems on milli-arcsecond angular scales (milli-lenses) using high-resolution Very Long Baseline Interferometry (VLBI) imaging. The SMILE parent sample contains ~ 5000 radio-loud active galaxies, selected as a flux-limited, complete subsample of CLASS (The Cosmic Lens All-Sky Survey) sources. We compiled redshift information for the full sample from multiple literature and catalog sources and found that 491 sources have no available redshift estimate, either spectroscopic or photometric. A further 948 sources have only photometric redshifts, many of which show substantial discrepancies between catalogs. Reliable redshifts are essential for VLBI radio-source studies because they convert angular measurements into physical linear scales, enable estimates of intrinsic luminosities and jet kinematics, and allow robust cosmological and population studies. To address this key limitation for lensing and population studies, we initiated a dedicated spectroscopic campaign to secure reliable redshifts for as many targets as possible. This paper focuses on the brightest sources in the SMILE sample. We report newly determined spectroscopic redshifts for 6 targets out of 15 observed with the Skinakas 1.3 m telescope.

Figures

Figures reproduced from arXiv: 2607.04959 by Alberto Floris, Andreas Zezas, Avinash Kumar, Carolina Casadio, Dmitry Blinov, Elias Kyritsis, Valentina Missaglia, Vangelis Pantoulas.

Figure 1
Figure 1. Figure 1: Spectrum of GB6 J010341+423925 with identified lines. [O I] λ6300˚A, Hα and N II λ6583˚A lines and derived a redshift of z = 0.1230±0.0002 based on these lines. A few other less prominent lines are visible in the spectrum; these are consistent with [O III] λ4959˚A and the S II (λλ6716, 6731˚A) blend based on the measured z. Our spectroscopic redshift is comfortably close to the mean of the photometric esti… view at source ↗
Figure 2
Figure 2. Figure 2: The SNR per pixel ranges from 3 to 19, with an average value of 12. We identified the 5000 5500 6000 6500 7000 7500 8000 8500 Wavelength [Å] 200 100 0 100 Relative flux C IV 5801 C IV 5812 [O I] 6300 [N II] 6548 H 6563 [N II] 6583 GB6J184835+213156 (z=0.0854±0.0006) [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Spectrum of GB6 J195141+480145 with identified lines. doublets, along with Hα. Fitting these lines yields z = 0.05586 ± 0.00002. This value is consistent with the photometric redshift from PS1-STRM given the statistical uncertainties of this catalog (e.g., σ(∆znorm) ≈ 0.03). 3.4. J201414+063439 GB6 J201414+063439 (RA = 20:14:14.9, Dec = 06:34:37.2) is positionally consistent with a source of r = 18.54m in … view at source ↗
Figure 4
Figure 4. Figure 4: Spectrum of GB6 J201414+063439 with identified lines. The original spectrum is shown in gray, while the black line shows the smoothed version. Hα and N II λ6583˚A. Using these lines, we measured z = 0.1486 ± 0.0008, which falls between the two photometric estimates. 3.5. J203142+162147 GB6 J203142+162147 (RA = 20:31:42.1, Dec = 16:22:07.4) has r = 18.41m in PS1-DR2. Pho￾tometric redshift estimates of 0.117… view at source ↗
Figure 5
Figure 5. Figure 5: Spectrum of GB6 J203142+162147 with identified lines. The original spectrum is shown in gray, while the black line shows the smoothed version. λ6583˚A, and O I λ6300˚A. Using these lines, we measured z = 0.1349 ± 0.0003, which lies between the photometric redshifts reported in PS1-STRM and QZO. 3.6. J222252+144119 GB6 J222252+144119 (RA = 22:22:51.4, Dec = 14:41:13.6) is positionally consistent with a prom… view at source ↗
Figure 6
Figure 6. Figure 6: Spectrum of GB6 J222252+144119 with identified lines. λ6583˚A, and [S II] λ6716˚A, we measured z = 0.0660 ± 0.0002. A possible [O I] λ6300˚A and [S III] λ6312˚A blend is also visible, but was not used in the redshift determination. Our redshift estimate is broadly consistent with all photometric estimates. 3.7. Other sources For four additional sources, we obtained optical spectra at a time when no spectro… view at source ↗

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Reference graph

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