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Finding Quasars Behind the Galactic Plane: Spectroscopic Identifications of ~1300 New Quasars at |b|<=20 degree from LAMOST DR10

T0 review · 3 major / 6 minor · reviewed 2026-08-08 · deepseek-v4-flash

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Pith's one-line read This paper reports 1,982 spectroscopically confirmed quasars behind the Galactic plane, 1,338 of them new, from LAMOST DR10.

desk verdict A useful, honest survey catalog of 1,982 LAMOST-confirmed quasars behind the Galactic plane; the unquantified visual classification is a real soft spot but not a fatal one. read the letter →

arxiv 2502.05480 v1 pith:VBYK2GBZ submitted 2025-02-08 astro-ph.GA

Zhi-Ying Huo , Yuming Fu , Yang Huang , Haibo Yuan , Xue-Bing Wu , Maosheng Xiang , Xiao-Wei Liu , Bing Lyu
show 5 more authors
Hao Wu Jian Li Yanxia Zhang Yanli Ai Junjie Jin
This is my paper · ORCID
classification astro-ph.GA
keywords quasarsGalacticplaneLAMOSTDR10spectroscopiccatalogquasarcandidatesinterstellarmediumabsorptionastrometricreferenceframephotometricvariability
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

Behind the Milky Way's dust-obscured plane, spectroscopically confirmed quasars have been rare; this paper changes that count. Using variability- and color-selected candidates from Pan-STARRS1 and WISE photometry, the authors visually examined 3,486 LAMOST DR10 spectra and identified 1,982 quasars with |b| ≤ 20°, of which 1,338 are newly discovered. The resulting catalog gives astronomers a population of moderately bright (peak i ≈ 19.0 mag), intermediate-redshift (peak z ≈ 1.5) background sources behind the Galactic disk. Such quasars are useful as absorption-line probes of the Milky Way's interstellar medium and as faint, stable astrometric references for measuring stellar proper motions. The paper also reports Na D absorption in about half the spectra and a median Gaia parallax offset of −14.65 μas for the sample.

What carries the argument

The machinery is a two-stage selection-and-confirmation pipeline. First, quasar candidates come from the variability-based Pan-STARRS1 QSO catalog of Hernitschek et al. (2016) and the transfer-learning PS1+AllWISE GPQ catalog of Fu et al. (2021), with cuts at i ≈ 19.5–20.0 mag. Second, every LAMOST spectrum of a candidate is visually inspected by at least two co-authors using the ASERA tool, and an object is admitted when at least one or two broad emission lines match a quasar template; redshifts come from the same line matches. This visual step is the load-bearing mechanism because the automated 1D pipeline alone is not trusted for faint, low-S/N objects near the plane.

What would settle it

Take a random subset of the 1,338 newly identified quasars, especially those near z ≈ 1 with only one detected emission line, and re-observe them at higher spectral resolution or in the near-infrared; if a significant fraction show stellar absorption features or narrow line ratios instead of a broad quasar line, the visual-confirmation step is admitting contaminants.

Watch

Extended reading notes

Core claim

The paper's central claim is that a dedicated survey can systematically find quasars behind the Galactic plane rather than relying on serendipity. From 2,454 targeted quasar candidates observed by LAMOST through June 2022, 1,949 were confirmed as quasars by visual inspection of their spectra — a 79% success rate — and another 33 quasars came from objects originally targeted as stars or variables. After cross-matching with existing quasar catalogs, 1,338 of the total 1,982 are new. The sample concentrates at |b| ≈ 10°–20° and Galactic longitudes 240° < l < 90°, tracks the expected influences of dust extinction and stellar crowding, peaks at i ≈ 19.0 mag and z ≈ 1.5, and is presented as a public catalog with redshifts, magnitudes, astrometry, reddening, and Na D absorption flags.

Load-bearing premise

The load-bearing premise is that a spectrum with one or two broad emission lines, judged by eye, is really a quasar; for faint objects, especially near redshift 1 where only a single Mg II line falls in a low-throughput channel-overlap region, that judgment is not benchmarked against any measured false-positive rate.

Editorial extensions

If this is right

  • The 1,982-object catalog lifts the density of confirmed quasars in the |b| ≤ 20° region and provides targets for absorption-line studies of the Milky Way's ISM/IGM along previously poorly probed sight lines.
  • The bright, compact quasars can serve as extragalactic reference points for improving the Gaia-based celestial reference frame near the Galactic plane, where quasar density was lowest.
  • About half the spectra show Na D absorption, so the catalog offers a ready-made set of background light sources for mapping neutral gas and dust in the disk.
  • The 79% confirmation rate for targeted candidates shows that photometric variability plus infrared color selection is efficient even in crowded, dusty fields.
  • The authors estimate that the ongoing LAMOST phase III survey will add roughly 5,000 more such quasars, meaning the present catalog is an early installment of a larger sample.

Reading between the lines

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

  • My inference: the same candidate-selection plus visual-confirmation recipe could be applied to other multi-fiber spectroscopic surveys to extend quasar samples even closer to the plane, where LAMOST's declination limit of −10° cannot reach.
  • My inference: the unquantified visual-classification step means the 'confirmed' label should be read as 'high-confidence candidate'; a future paper could measure the false-positive rate by re-observing a random subsample, and until then the 79% success rate applies to candidates, not to the verified purity of the final catalog.
  • My inference: the reported Gaia parallax and proper-motion offsets, measured with this small sample near the plane, suggest that quasar-based calibration can quantify the spatial variation of Gaia astrometric systematics in the zone of avoidance; a larger phase III sample would make those calibration maps much tighter.
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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 / 6 minor

Summary. The paper reports a catalog of 1982 spectroscopically confirmed quasars at |b| <= 20 degrees from LAMOST DR10, of which 1338 are newly identified. Candidates were drawn from the Hernitschek et al. (2016) variability-selected sample and the Fu et al. (2021) transfer-learning color/motion-selected sample, plus serendipitous LAMOST QSO classifications. All 3486 spectra of 3030 unique targets were visually inspected by at least two co-authors using the ASERA tool, with redshifts measured from one or two emission lines; quasars near z~1 are identified from a single Mg II line in the 5700-5900 Angstrom channel-overlap region. The paper presents the catalog with positions, magnitudes, redshifts, Gaia astrometry, and Na D absorption flags, and discusses spatial, magnitude, and redshift distributions, Gaia zero-point offsets, and preliminary Na D results. The headline contribution is the public catalog itself, which fills a known gap in quasar coverage near the Galactic plane.

Significance. If reliable, the catalog is a valuable community resource: it roughly doubles the number of spectroscopically confirmed quasars at |b| <= 20 deg, enables ISM/IGM absorption-line studies along low-latitude sightlines, and can inform Gaia astrometric reference-frame work. The paper ships a public catalog with a DOI, machine-readable FITS, and clearly documented columns, and it includes explicit visual verification of every spectrum by multiple co-authors. However, the central reliability claim — that these are all quasars — rests entirely on unquantified visual classification. The absence of a false-positive estimate, inter-inspector agreement measure, or control sample is the main weakness. If even a modest fraction of the single-line Mg II identifications are spurious, the headline count and the derived astrometric offsets would be affected. The scientific payoff is real, but the catalog's value depends on a reliability quantification that is currently missing.

major comments (3)
  1. [Section 4] The classification procedure is stated as 'all those spectra with at least one or two emission lines matching to the quasar template are identified as quasars,' but no quantitative reliability measure is provided. There is no false-positive rate, no inter-inspector agreement statistic, and no control sample of known non-quasars. This matters most for the z~1 subset, where the paper itself notes that only Mg II is detected in the 5700-5900 Angstrom overlap region and that 'spike- or trough-like artifacts may appear in the flux-calibrated spectra.' Since the headline claims of 1982 confirmed quasars and 1338 new discoveries depend on these visual identifications, please provide an estimate of the contamination rate (e.g., by re-observing a subset, by cross-matching against independent spectroscopy in overlapping survey regions, or by quantifying how many spectra were classified on a single line versus multiple lines).
  2. [Table 2 / Section 4] The catalog has no column distinguishing secure multi-line identifications from tentative single-line identifications, and no redshift-quality flag. For a catalog paper, this is a load-bearing omission: users cannot assess which entries are most reliable, and future follow-up programs cannot prioritize targets accordingly. Please add a quality flag (e.g., 'single-line' vs 'multi-line', or an analog of SDSS ZWARNING) and report the number of quasars in each class. This would also make the vulnerability of the z~1 subset explicit and testable.
  3. [Section 5.3] The astrometric zero-point offsets (parallax median -14.65 microarcsec, PM offsets -2.11 and -2.41 microarcsec/yr) are presented as an 'examination' of the sample's utility. These values are meaningful only if the catalog is nearly pure; any stellar contaminants or misclassified emission-line objects would bias the offsets. Because the purity is unquantified, the astrometric conclusions are not yet robust. Please either (a) estimate the impact of plausible contamination on the reported offsets, or (b) reframe this section as purely illustrative, with a clear caveat that the offsets should be revisited once a purity estimate is available.
minor comments (6)
  1. [Section 3] There is a typo: 'an angular diameter of the field of view of is 5 deg' should read '...field of view is 5 deg.'
  2. [Section 5.1] 'the later can reach ~100 deg^-2' should be 'the latter can reach...'.
  3. [Figure 2 caption] The caption reads 'GPQ candidates (i 20 mag)'; the inequality symbol appears missing. It should be 'i <= 20 mag'.
  4. [Section 4] The phrase 'at least one or two emission lines' is internally ambiguous; it should be expressed as either 'at least one' or 'at least two' with a clear definition of what constitutes a secure identification.
  5. [Section 1] The reference to 'Xu et al. 2025, in preparation' is not part of the published literature and should either be updated to a citable reference or removed.
  6. [Section 5.4] The Na D detection flag is binary ('Y'/'N'), but the text notes that many spectra are contaminated by nightglow or have low S/N. Please clarify whether 'N' means 'no detection' or 'not measurable,' and consider adding a third flag for uncertain cases.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the central catalog result is grounded in independent LAMOST spectra, not in the photometric candidate inputs.

full rationale

The paper's central claim is the spectroscopic identification of 1982 quasars, 1338 of them new, at |b| <= 20 deg from LAMOST DR10. The derivation chain is observational rather than theoretical: photometric variability/color candidate catalogs (Hernitschek et al. 2016; Fu et al. 2021) were used only to assign fibers, and the confirming evidence is the LAMOST spectra themselves, which were visually examined against quasar emission-line templates. The paper does not fit a parameter and then rename it a prediction; nor does it define 'quasar' in terms of the candidate catalog. The self-citations to Fu et al. (2021, 2022), Huo et al. (2017), and Huo et al. (2010, 2013, 2015) affect target selection and the new/known flag, but the spectroscopic confirmation is independent of those citations. The reliability concern about z~1 objects identified from a single Mg II line in the low-throughput channel-overlap region is a classification-purity and correctness risk, not a circularity of the argument: the classification is still made from the spectra rather than from the inputs. No equation in the paper reduces the output to the input, and no load-bearing claim is justified solely by an author self-citation. The catalog is therefore self-contained in the sense required for a circularity finding, and the appropriate score is 0.

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

The central result is an observational catalog, not a mathematical derivation, so there are no fitted free parameters and no invented entities. The catalog's validity rests on standard survey assumptions: template-based spectral classification, the reliability of external candidate catalogs and external data products, and the accuracy of cross-matching to decide new versus known status.

assumptions (6)
  • domain assumption Spectra with one or two broad emission lines matching a quasar template are quasars.
    Section 4: visual identification of 1982 quasars uses this rule; no false-positive rate is reported.
  • domain assumption Hernitschek et al. (2016) and Fu et al. (2021) candidate catalogs select real quasars with adequate purity and completeness.
    Section 2: all LAMOST GPQ targets come from these catalogs; the authors note purity estimates depend on the validation set.
  • domain assumption LAMOST 1D pipeline produces reliable wavelength calibration, flux calibration, and initial QSO/STAR/GALAXY classification.
    Section 3: classifications and redshifts from the pipeline are used, with visual inspection as a check.
  • domain assumption Cross-matching with Milliquas v8 and the listed prior catalogs correctly separates new from known quasars.
    Section 4: the new/known flag in the catalog depends on this cross-match.
  • domain assumption Gaia DR3 astrometry has well-behaved errors at the tens of microarcsecond level for these sources.
    Section 5.3: median parallax and proper-motion offsets are interpreted as zero-point estimates.
  • domain assumption Planck E(B-V) map traces the extinction that limits quasar detection at low latitudes.
    Section 5.1 and Table 2: dust extinction and success-rate correlations are based on this map.

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Cite this review

Pith. "Pith review of Finding Quasars Behind the Galactic Plane: Spectroscopic Identifications of ~1300 New Quasars at |b|<=20 degree from LAMOST DR10." pith.science (2026). https://pith.science/paper/VBYK2GBZ

@misc{pith2026250205480,
  author       = {Pith},
  title        = {Pith review of: Finding Quasars Behind the Galactic Plane: Spectroscopic Identifications of ~1300 New Quasars at |b|<=20 degree from LAMOST DR10},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/VBYK2GBZ}},
  note         = {Machine review of arXiv:2502.05480}
}
read the original abstract

Quasars behind the Galactic plane (GPQs) are excellent tracers to probe the chemistry and kinematics of the interstellar/intergalactic medium (ISM/IGM) of the Milky Way along sight lines via absorption line spectroscopy. Moreover, the quasars located at low Galactic latitudes will fill the gap in the spatial distribution of known quasars near the Galactic plane, and can be used to construct an astrometric reference frame for accurate measurements of proper motions (PMs) of stars, and substructures of the Milky Way. We started a survey of background quasars in the low Galactic latitude region since the LAMOST phase II survey in 2017. Quasar candidates have been selected from the optical and infrared photometric data of Pan-STARRS1 and WISE surveys based on their variability and color properties. In this paper, we present a sample of 1982 spectroscopically confirmed GPQs with |b| <= 20 degree based on LAMOST Data Release 10 (DR10). Among them, 1338 are newly discovered. Most GPQs are located around 240<l<90 degree, and the spatial distributions are non-uniform. These GPQs have a magnitude distribution with a peak at i-mag 19.0, and mostly around 18.0-19.5mag. The peak of redshift distributions is around ~1.5, and most GPQs have redshifts between 0.3 and 2.5. Our finding demonstrates the potential discovery space for the GPQs from the spectroscopic surveys and the promising applications for future research.

Figures

Figures reproduced from arXiv: 2502.05480 by the authors.

Figure 1
Figure 1. Spatial distributions of the 1338 LAMOST newly identified GPQs (magenta crosses) in Galactic coordinates. Blue crosses represent known GPQs listed in Im et al. (2007), Huo et al. (2017) and Fu et al. (2022), while grey dots represent QSOs/AGNs or candidates from the Milliquas (Flesch 2023). 20° 0° 20° b GPQ candidates (i 20 mag) from Fu et al. (2021) + Hernitschek et al. (2016) 20° 0° 20° b =60 =0 = 10 GPQ candidate… view at source ↗
Figure 2
Figure 2. Sky density of the GPQ candidates from the combination list of Hernitschek et al. (2016) and Fu et al. (2021) with Declination ≥ −30◦ and i ≤ 20.0 mag (top panel), spatial distribution of the 2454 GPQ candidates with LAMOST fiber assigned (middle panel), and that of the 1949 confirmed GPQs from the 2454 GPQ candidates (bottom panel). The middle and bottom panels are overlaid with the Planck Collaboration et al. (201… view at source ↗
Figure 3
Figure 3. The distributions of the number of the LAMOST observed GPQ candidates (grey line) and the corresponding confirmed GPQs (magenta line) along the Galactic Latitude (top-left) and dust extinction E(B − V ) (bottom-left); success rate of quasar identifications along the Galactic latitude (top-right) and dust extinction (bottom-right). In addition to the two main factors mentioned above, there are other factors involved.… view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: PS1 i-band mean magnitude (left panel) and redshift (right panel) distributions of the 1982 GPQs from LAMOST DR10, including 1338 newly discovered and 644 known quasars. The right panel of [PITH_FULL_IMAGE:figures/full_fig_p010_4.png]
Figure 5
Figure 5. Figure 5: Panel a: Distributions of parallax (black solid line ), PM of right ascension (red solid line) and declination (blue solid line) from Gaia DR3, and their best-fitting Gaussian models (dotted lines) for the 1982 GPQs from LAMOST DR10. The median and standard deviation v…
Figure 6
Figure 6. Figure 6: LAMOST Spectrum of quasar J001945.00+484559.3 (black) at redshift z = 1.527 with composite quasar spectrum overlaid (blue solid line, Vanden Berk et al. 2001), and identified emission lines labeled (blue dash-dotted line). The red dash-dotted lines indicate the laborat…
Figure 7
Figure 7. Figure 7: Radial velocities along the Galactic longitude measured from D2 lines for about one hundred LAMOST GPQs with relatively better Na D absorption line detections. PS1 and WISE surveys. The spatial distribution of this GPQ sample exhibits significant non-uniformity, attrib…

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