arxiv: 2605.05298 · v1 · submitted 2026-05-06 · 🌌 astro-ph.GA

Recognition: unknown

Kinematic Stratification in Extremely Red Quasars Revealed by JWST

Jack M. M. Neustadt , Nadia L. Zakamska , Yu-Ching Chen , Andrey Vayner , Fred Hamann , Marie Wingyee Lau , Serena Perrotta , Kate Rowlands

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Sylvain Veilleux Dominika Wylezalek

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Pith reviewed 2026-05-08 16:03 UTC · model grok-4.3

classification 🌌 astro-ph.GA

keywords extremely red quasarsJWST spectroscopyemission line kinematicskinematic deblendingdust obscurationscattered lightspectral energy distributions

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The pith

Modeling of JWST spectra separates emission lines in extremely red quasars into distinct kinematic components that indicate velocity- and density-stratified gas on multiple scales.

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

The paper examines JWST spectra of extremely red quasars to study the complex shapes of their rest-frame optical emission lines. By fitting and separating these lines into multiple kinematic parts, the analysis points to gas that is organized in layers with different speeds and densities across a range of distances from the central source. The work also uses broader wavelength data to show that the quasars are heavily hidden by dust, with only a small fraction of light scattered toward us. The study focuses on one object, J0834, where the line profiles are especially clear to decompose. This separation helps map how gas moves and is structured around these obscured active nuclei.

Core claim

Our modeling allows us to deblend the lines and separate the emission into distinct kinematic components that imply velocity- and density-stratified gas structures on a range of physical scales within the ERQs. The kinematics of the UV and optical emission lines largely agree, but the UV lines are dominated by scattered light while the optical emission-line ratios indicate a combination of scattered and obscured emission. The spectral energy distributions are consistent with a significantly dust-obscured central source with a small amount of relatively-unobscured UV/optical flux scattered into our line-of-sight.

What carries the argument

Kinematic deblending of rest-frame optical emission lines into separate velocity components that trace stratified gas.

If this is right

Gas around these quasars is organized into layers that differ in speed and density across scales from the broad-line region outward.
UV light reaches us mostly by scattering while optical lines include both scattered and direct but obscured contributions.
The overall energy output is dominated by a central source hidden behind large amounts of dust.
Kinematic agreement between UV and optical lines suggests the scattering occurs in a region that shares the same bulk motion as the emitting gas.

Where Pith is reading between the lines

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

The same deblending technique could be applied to other dust-obscured active galaxies to test whether stratification is common.
If the layers correspond to distinct physical radii, future multi-wavelength monitoring could measure time delays between components and map the geometry.
The scattered-light fraction may set the observed redness of these objects and could be used to estimate the covering factor of the obscuring material.

Load-bearing premise

The different kinematic components seen in the line profiles correspond to physically separate gas regions rather than being produced by projection effects, unresolved multiple sources, or fitting degeneracies.

What would settle it

High-resolution integral-field spectroscopy or adaptive-optics imaging that shows all kinematic components arising from the same spatial location or from a single unresolved structure would undermine the stratified-gas interpretation.

Figures

Figures reproduced from arXiv: 2605.05298 by Andrey Vayner, Dominika Wylezalek, Fred Hamann, Jack M. M. Neustadt, Kate Rowlands, Marie Wingyee Lau, Nadia L. Zakamska, Serena Perrotta, Sylvain Veilleux, Yu-Ching Chen.

**Figure 1.** Figure 1: — JWST NIRSpec spectra of the ERQs. Prominent emission lines are labeled. The gap in the spectra is due to the gap between the NRS1 and NRS2 channels. For analysis of spectral lines, we subtract out the continuum model shown by the dotted lines. do not expect the Balmer decrement to be lower than the Case B limit. For J0834, we need multiple spectral templates to include [O I] and [N II] to model the obse… view at source ↗

**Figure 2.** Figure 2: — Observed and modeled spectral profiles for the J0834 Hβ + [O III] (left) and Hα emission (right) along with residuals (bottom). The colors correspond to the four templates from Tab. 2. 4700 4800 4900 5000 0 1 2 3 4 C o n tin u u m-s u b t r a c t e d f 0834-A + 0834-C 0834-B + 0834-D 6300 6400 6500 6600 6700 0834-A + 0834-C (scaled) 0834-B + 0834-D (scaled) 8000 6000 4000 2000 0 2000 4000 Velocity [km s … view at source ↗

**Figure 3.** Figure 3: — Left: The Hβ and [O III] emission profiles associated with Templates 0834-A and -C (cyan) and 0834-B and -D (orange). The two profiles are constructed by subtracting the other templates from the total emission (see Sec. 3.2). Center: Same as the previous panel, but for the Hα and [N II] emission profiles. Right: The Hα and [O III] profiles of Templates 0834-A and -C. In addition to showing the [O III] do… view at source ↗

**Figure 4.** Figure 4: — Red optical and NIR spectrum of J0834. We use the widths and offsets of Templates 0834-A, 0834-B, and 0834-C to fit the emission profiles of He I λ5876, [O I] λλ6300,64, O I λ8446, as well as a group of miscellaneous identified lines: He I λ7065, [Ar III] λ7136, [O II] λλ7320,31, and [Ni II] λ7378 (the identification of the [N II] line is uncertain). We highlight the lack of detected O I λ7774 emission. … view at source ↗

**Figure 5.** Figure 5: — Top: Velocity profiles of the O I λ8446 line from the JWST spectrum and the O I λ1304 line from the SDSS and XShooter spectra. The JWST spectrum is scaled to match the flux of the UV spectra with an observed O I λ1304:λ8446 flux ratio of 1:3–5, depending on the scaling used. We also include the template fits to the O I λ8446 profile that are also shown in view at source ↗

**Figure 6.** Figure 6: — Kinematic profiles of Fe II λ5169 compared to O I λ8446 and Hβ. The profiles largely agree with each other, albeit the peaks of the Fe II emission are slightly offset from the other two lines. This is strong evidence for two Fe II kinematic components – one linked to Template 0834-A and one from -B. we do for J0834 in Section 3, focusing on the most important features of each ERQ view at source ↗

**Figure 7.** Figure 7: — Smoothed X-Shooter spectra (dark red) and error spectra (red) combined with JWST spectrum (black) for J0834. We highlight the prominent UV bump created by Fe II emission. We also mark out telluric features (gray filled) that are relevant for the ground-based X-Shooter spectra. TABLE 3 Modeled templates for other ERQs ERQ Template Offset FWHM Hα/Hβ log [O III]/Hβ log [N II]/Hα log [O I]/Hα log [S II]/Hα [… view at source ↗

**Figure 9.** Figure 9: — Model fits to the Hβ emission for J0832 (top) and J1232 (bottom). The JWST spectra are shown in black, the XShooter spectra is shown in red, and smoothed versions of the X-Shooter spectra are shown in dark red. Our model fits where the blue wing is constrained by the fit to Hα are shown in gray. Our extrapolated models are able to capture the Hβ emission of the X-Shooter spectrum, despite having no info… view at source ↗

**Figure 10.** Figure 10: — UV to MIR SEDs of our ERQs. The solid lines are the JWST (black) and archival spectra (X-Shooter - dark red, SDSS - dark blue, GNIRS - green), and the solid colored circles are the archival SDSS and WISE photometry. Atmospheric absorption bands are shaded gray. The dotted brown line is the best-fit torus template, the dotted gold line is the best-fit scattered light template, and the dashed grey line co… view at source ↗

**Figure 11.** Figure 11: — Full SED of our ERQs. The UV to MIR SED models are the same as in Sec. 5. The predicted torus template flux is plotted as a brown dotted line. The QSO1 template is plotted as a blue dotted line. The ALMA, VLA, and FIRST fluxes are plotted as blue, red, and green stars, respectively. The Rieke et al. (2009) SF SED is plotted as a dotted green line, and it is scaled to match the difference between the obs… view at source ↗

**Figure 12.** Figure 12: — Velocity profiles of the Hα (dark red) and [O III] (dark blue) emission for each ERQ. We scale the [O III] and Hα to each other for better visual comparison. We also plot the centroids of our model templates from Tab. 2 and 3 as colored dotted lines, where the colors are the same as Figs. 2 and 8. by variations in the NIR SED due to different potential torus structures (Stalevski et al. 2016; Mart´ınez-… view at source ↗

read the original abstract

We analyze the spectra of the central nuclei of extremely red quasars (ERQs) observed as part of the JWST ERS Q3D program. We focus on the complex kinematic structures of the prominent rest-frame optical emission lines. Our modeling allows us to deblend the lines and separate the emission into distinct kinematic components that imply velocity- and density-stratified gas structures on a range of physical scales within the ERQs. Supplementing the JWST data with archival data, we analyze the spectral energy distributions (SEDs) of the ERQs and find they are consistent with a significantly dust-obscured central source with a small amount of relatively-unobscured UV/optical flux that is scattered into our line-of-sight. While the kinematics of the UV and optical emission lines largely agree, the UV lines are dominated by scattered light. In contrast, the optical emission-line ratios indicate a combination of scattered and obscured emission. Our analysis focuses on one ERQ, J0834, because its distinct spectroscopic features allow the emission to be easily decomposed into separate kinematic components.

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.

Desk Editor's Note private letter to a colleague

New JWST spectra on ERQs give a clean kinematic split in one object but the jump to stratified gas structures rests on untested assumptions about the fits.

read the letter

The main thing to know is that this paper uses JWST ERS Q3D spectra on extremely red quasars and shows that the optical lines in J0834 can be deblended into distinct kinematic components. Those components, plus the SEDs from archival data, are presented as evidence for velocity- and density-stratified gas on different scales around an obscured central source with some scattered light reaching us. The UV and optical kinematics line up reasonably well, while the optical line ratios point to a mix of scattered and obscured emission. The analysis stays focused on the nucleus and highlights why J0834 is easier to work with than most ERQs. That part is straightforward and uses the new data productively. The decomposition itself looks credible for this source because the features separate without obvious forcing. The soft spot is the physical interpretation. The abstract states that the modeling implies stratified structures, yet it gives no numbers on component selection, fit uncertainties, or direct comparisons to other explanations such as projection effects or multiple unresolved regions. The UV-optical agreement is noted but does not rule out a single structure viewed at different depths. Since the work centers on one object, the broader claim for ERQs as a class depends on how typical the clean split really is. This is for researchers who follow high-redshift obscured AGN and feedback. Someone already working on quasar outflows or dust geometry would get value from the spectra and the deblending approach. I would send it to peer review. The observations are fresh enough and the analysis detailed enough that referees can check the fitting steps and decide whether the stratification reading holds.

Referee Report

2 major / 2 minor

Summary. The manuscript analyzes JWST ERS Q3D spectra of extremely red quasars (ERQs), focusing on the object J0834 whose distinct features permit straightforward deblending of rest-frame optical emission lines into multiple kinematic components. These components are interpreted as evidence for velocity- and density-stratified gas structures on a range of physical scales. Archival data are used to construct SEDs consistent with a heavily dust-obscured central engine plus a small scattered UV/optical component; UV and optical kinematics largely agree, but the UV lines are dominated by scattered light while optical ratios indicate mixed scattered and obscured emission.

Significance. If the kinematic decomposition is shown to be robust and physically unique, the work would supply new, spatially unresolved but kinematically resolved constraints on the multi-scale gas flows and obscuration geometry in ERQs, directly informing AGN unification and feedback models. The JWST data provide the first high-S/N rest-optical spectroscopy capable of separating these components in this population.

major comments (2)

[Spectral line deblending and kinematic analysis of J0834] The central claim that the adopted multi-component decomposition corresponds to physically distinct, stratified gas structures (rather than projection effects, unresolved sources, or non-unique fits) is load-bearing. In the spectral modeling of J0834, quantitative model-comparison statistics (e.g., ΔBIC or ΔAIC between single- and multi-Gaussian models for [O III] and Hβ) and explicit tests of alternative geometries are required to exclude degeneracies.
[Emission-line ratio analysis and physical interpretation] The interpretation of density stratification from optical line ratios assumes the components are physically distinct and that ionization and density can be uniquely assigned. The manuscript should report the full error budget on the derived densities and velocities, including covariance between components, and test whether a single stratified structure viewed at different optical depths can reproduce the observed UV/optical agreement.

minor comments (2)

[Throughout] Clarify the exact velocity ranges and line-ratio criteria used to label each kinematic component (broad, intermediate, narrow) so that the stratification claim can be reproduced from the tabulated fits.
[Abstract and introduction] The abstract states that decomposition is 'easy' for J0834; add a brief quantitative comparison (e.g., number of components needed and reduced χ²) with the other ERQs in the Q3D sample to justify the focus.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed comments on our manuscript. We appreciate the recognition of the potential significance of our JWST-based kinematic analysis of ERQs. We address each major comment below, providing the strongest honest defense of our approach while agreeing to incorporate additional quantitative tests and error analyses in a revised version.

read point-by-point responses

Referee: [Spectral line deblending and kinematic analysis of J0834] The central claim that the adopted multi-component decomposition corresponds to physically distinct, stratified gas structures (rather than projection effects, unresolved sources, or non-unique fits) is load-bearing. In the spectral modeling of J0834, quantitative model-comparison statistics (e.g., ΔBIC or ΔAIC between single- and multi-Gaussian models for [O III] and Hβ) and explicit tests of alternative geometries are required to exclude degeneracies.

Authors: We agree that quantitative model comparison is important for supporting the robustness of the decomposition. In the revised manuscript we will add explicit ΔBIC and ΔAIC values comparing single-Gaussian versus multi-Gaussian models for [O III] and Hβ, which will demonstrate the statistical preference for the adopted multi-component fit. We will also expand the discussion of alternative geometries (projection effects, unresolved sources) and explain why the distinct, well-separated kinematic features in J0834—combined with consistency between the optical decomposition and the independently derived SED—favor a stratified interpretation over degeneracies. Full radiative-transfer modeling of every alternative is beyond the scope of this observational paper, but the added statistics and targeted discussion will address the concern directly. revision: yes
Referee: [Emission-line ratio analysis and physical interpretation] The interpretation of density stratification from optical line ratios assumes the components are physically distinct and that ionization and density can be uniquely assigned. The manuscript should report the full error budget on the derived densities and velocities, including covariance between components, and test whether a single stratified structure viewed at different optical depths can reproduce the observed UV/optical agreement.

Authors: We will revise the manuscript to include a complete error budget on the derived densities and velocities, explicitly reporting covariances between the kinematic components. We will also add a targeted test and discussion of whether a single stratified structure viewed at varying optical depths could reproduce the observed UV/optical kinematic agreement. Our current analysis indicates that the component-specific line ratios require a mix of scattered and obscured emission, but we will quantify this comparison in the revision to strengthen the physical interpretation. revision: yes

Circularity Check

0 steps flagged

No circularity: observational deblending and interpretation are self-contained

full rationale

The paper reports new JWST spectra of ERQs, applies standard multi-component Gaussian modeling to deblend rest-frame optical lines, and interprets the resulting kinematic components as evidence for velocity- and density-stratified gas. No equations, fitted parameters, or self-citations are shown that reduce the central claim to its own inputs by construction. The analysis draws on archival SED data and conventional AGN line-ratio diagnostics without self-referential loops or uniqueness theorems imported from prior author work. The interpretation that deblending implies physical stratification is presented as a reading of the data rather than a mathematical necessity.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard astrophysical assumptions about emission-line formation in AGN environments and dust scattering; no new entities are postulated, and free parameters are limited to standard line-fitting values.

free parameters (1)

kinematic component velocities and densities
Fitted parameters used to deblend emission lines into distinct components.

axioms (2)

domain assumption Emission lines in AGN can be decomposed into physically distinct kinematic components corresponding to stratified gas.
Invoked to interpret deblended components as velocity- and density-stratified structures.
domain assumption SEDs of ERQs can be modeled as dust-obscured central sources with scattered UV/optical flux.
Used to interpret the combination of JWST and archival data.

pith-pipeline@v0.9.0 · 5536 in / 1437 out tokens · 52152 ms · 2026-05-08T16:03:26.319095+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

300 extracted references · 284 canonical work pages · 8 internal anchors

[1]

, keywords =

The Intermediate-line Region in Active Galactic Nuclei. , keywords =. doi:10.3847/0004-637X/831/1/68 , archivePrefix =. 1606.00284 , primaryClass =

work page doi:10.3847/0004-637x/831/1/68
[2]

arXiv , author =:1912.02905 , journal =

The 16th Data Release of the Sloan Digital Sky Surveys: First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra. , keywords =. doi:10.3847/1538-4365/ab929e , archivePrefix =. 1912.02905 , primaryClass =

work page doi:10.3847/1538-4365/ab929e 1912
[3]

arXiv e-prints , keywords =

The Wide Field Infrared Survey Telescope: 100 Hubbles for the 2020s. arXiv e-prints , keywords =
[4]

F., Arzoumanian, Z., Baker, P

The NANOGrav 12.5 yr Data Set: Wideband Timing of 47 Millisecond Pulsars. , keywords =. doi:10.3847/1538-4365/abc6a1 , archivePrefix =. 2005.06495 , primaryClass =

work page doi:10.3847/1538-4365/abc6a1 2005
[5]

, keywords =

Spectropolarimetry of high-redshift obscured and red quasars. , keywords =. doi:10.1093/mnras/sty1685 , archivePrefix =. 1806.10138 , primaryClass =

work page doi:10.1093/mnras/sty1685
[6]

1986, ApJ, 308, 23, doi: 10.1086/164475

Recurrent Outbursts in the Broad-Line Region of NGC 1566. , keywords =. doi:10.1086/164475 , adsurl =

work page doi:10.1086/164475
[7]

New quasar lenses from double component fitting

The STRong lensing Insights into the Dark Energy Survey (STRIDES) 2016 follow-up campaign - II. New quasar lenses from double component fitting. , keywords =. doi:10.1093/mnras/sty2172 , archivePrefix =. 1805.12151 , primaryClass =

work page doi:10.1093/mnras/sty2172 2016
[8]

ARA&A , keywords =

Unified models for active galactic nuclei and quasars. , keywords =. doi:10.1146/annurev.aa.31.090193.002353 , adsurl =

work page doi:10.1146/annurev.aa.31.090193.002353
[9]

2018, , 616, A17, 10.1051/0004-6361/201833234

Gaia Data Release 2. Catalogue validation. , keywords =. doi:10.1051/0004-6361/201833234 , archivePrefix =. 1804.09375 , primaryClass =

work page doi:10.1051/0004-6361/201833234
[10]

R., et al

JWST MIRI flight performance: The Medium-Resolution Spectrometer. , keywords =. doi:10.1051/0004-6361/202346489 , archivePrefix =. 2303.13469 , primaryClass =

work page doi:10.1051/0004-6361/202346489
[11]

, keywords =

Detection of the Buried Active Galactic Nucleus in NGC 6240 with the Infrared Spectrograph on the Spitzer Space Telescope. , keywords =. doi:10.1086/500040 , archivePrefix =. astro-ph/0511381 , primaryClass =

work page doi:10.1086/500040
[12]

The NANOGrav 11-year Data Set: Pulsar-timing Constraints On The Stochastic Gravitational-wave Background

, year =. arXiv , doi =:1801.02617 , keywords =

work page Pith review arXiv
[13]

MID-INFRARED SELECTION OF ACTIVE GALACTIC NUCLEI WITH THE<i>WIDE-FIELD INFRARED SURVEY EXPLORER</i>. II. PROPERTIES OF<i>WISE</i>-SELECTED ACTIVE GALACTIC NUCLEI IN THE NDWFS BOÖTES FIELD

Mid-infrared Selection of Active Galactic Nuclei with the Wide-field Infrared Survey Explorer. II. Properties of WISE-selected Active Galactic Nuclei in the NDWFS Bo \"o tes Field. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/772/1/26 , adsurl =

work page doi:10.1088/0004-637x/772/1/26
[14]

, keywords =

Half of the Most Luminous Quasars May Be Obscured: Investigating the Nature of WISE-Selected Hot Dust-Obscured Galaxies. , keywords =. doi:10.1088/0004-637X/804/1/27 , archivePrefix =. 1408.1092 , primaryClass =

work page doi:10.1088/0004-637x/804/1/27
[15]

doi:10.17226/26141 , adsurl =

National Academies of Sciences, Engineering, and Medicine. Pathways to Discovery in Astronomy and Astrophysics for the 2020s. doi:10.17226/26141

work page doi:10.17226/26141
[16]

P., Tollerud, E

Astropy: A community Python package for astronomy. , keywords =. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

work page doi:10.1051/0004-6361/201322068
[17]

The Astronomical Journal , author =

The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

work page doi:10.3847/1538-3881/aabc4f
[18]

The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package

The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package. , keywords =. doi:10.3847/1538-4357/ac7c74 , archivePrefix =. 2206.14220 , primaryClass =

work page Pith review doi:10.3847/1538-4357/ac7c74
[19]

The Astronomer's Telegram , keywords =

ASAS-SN Discovery of a Large Outburst From NGC5273 and SCAT Classification as a Likely Optical Changing-Look AGN. The Astronomer's Telegram , keywords =
[20]

, keywords =

The Small Sizes and High Implied Densities of ``Little Red Dots'' with Balmer Breaks Could Explain Their Broad Emission Lines without an Active Galactic Nucleus. , keywords =. doi:10.3847/2041-8213/ad90b8 , archivePrefix =. 2408.07745 , primaryClass =

work page doi:10.3847/2041-8213/ad90b8 2041
[21]

, year = 1977, month = jun, volume = 214, pages =

Luminosity Indicators in the Spectra of Quasi-Stellar Objects. , year = 1977, month = jun, volume =. doi:10.1086/155294 , adsurl =

work page doi:10.1086/155294 1977
[22]

A., Phillips, M

Classification parameters for the emission-line spectra of extragalactic objects. , keywords =. doi:10.1086/130766 , adsurl =

work page doi:10.1086/130766
[23]

, keywords =

Strong Gravitational Lensing as a Tool to Investigate the Structure of Jets at High Energies. , keywords =. doi:10.1088/0004-637X/788/2/139 , archivePrefix =. 1403.5316 , primaryClass =

work page doi:10.1088/0004-637x/788/2/139
[24]

R., Nelemans, G., & Steeghs, D

Shock-induced star formation in a model of the Mice. , keywords =. doi:10.1111/j.1365-2966.2004.07725.x , archivePrefix =. astro-ph/0402248 , primaryClass =

work page doi:10.1111/j.1365-2966.2004.07725.x 2004
[25]

, keywords =

Dynamics of interacting galaxies. , keywords =. doi:10.1146/annurev.aa.30.090192.003421 , adsurl =

work page doi:10.1146/annurev.aa.30.090192.003421
[26]

, keywords =

The Lick AGN Monitoring Project 2011: Spectroscopic Campaign and Emission-line Light Curves. , keywords =. doi:10.1088/0067-0049/217/2/2610.48550/arXiv.1503.01146 , archivePrefix =. 1503.01146 , primaryClass =

work page doi:10.1088/0067-0049/217/2/2610.48550/arxiv.1503.01146 2011
[27]

Gallazzi, S

What controls the [OIII] 5007 line strength in active galactic nuclei?. , keywords =. doi:10.1111/j.1365-2966.2005.08841.x , archivePrefix =. astro-ph/0501436 , primaryClass =

work page doi:10.1111/j.1365-2966.2005.08841.x 2005
[28]

H., White, R

The FIRST Survey: Faint Images of the Radio Sky at Twenty Centimeters. , keywords =. doi:10.1086/176166 , adsurl =

work page doi:10.1086/176166
[29]

C., Blandford, R

, year =. doi:10.1038/287307a0 , file =

work page doi:10.1038/287307a0
[30]

, author Blandford, R.D

Theory of extragalactic radio sources. Reviews of Modern Physics , year = 1984, month = apr, volume =. doi:10.1103/RevModPhys.56.255 , adsurl =

work page doi:10.1103/revmodphys.56.255 1984
[31]

, eprint =

Estimating Star Formation Rates from Infrared and Radio Luminosities: The Origin of the Radio-Infrared Correlation. , keywords =. doi:10.1086/367829 , archivePrefix =. astro-ph/0212121 , primaryClass =

work page doi:10.1086/367829
[32]

A Local Baseline of the Black Hole Mass Scaling Relations for Active Galaxies. I. Methodology and Results of Pilot Study. , keywords =. doi:10.1088/0004-637X/726/2/59 , archivePrefix =. 1008.4602 , primaryClass =

work page doi:10.1088/0004-637x/726/2/59
[33]

A Local Baseline of the Black Hole Mass Scaling Relations for Active Galaxies. IV. Correlations Between M _ BH and Host Galaxy , Stellar Mass, and Luminosity. , keywords =. doi:10.3847/1538-4357/ac151a , archivePrefix =. 2101.10355 , primaryClass =

work page doi:10.3847/1538-4357/ac151a
[34]

, keywords =

The Mass of the Central Black Hole in the Nearby Seyfert Galaxy NGC 5273. , keywords =. doi:10.1088/0004-637X/796/1/8 , archivePrefix =. 1409.5794 , primaryClass =

work page doi:10.1088/0004-637x/796/1/8
[35]

, keywords =

Modeling the X-Ray-Ultraviolet Correlations in NGC 7469. , keywords =. doi:10.1086/308880 , archivePrefix =. astro-ph/0001239 , primaryClass =

work page doi:10.1086/308880
[36]

, keywords =

JWST ERS Program Q3D: The pitfalls of virial black hole mass constraints shown for a z 3 quasar with an ultramassive host. , keywords =. doi:10.1051/0004-6361/202450451 , archivePrefix =. 2404.14475 , primaryClass =

work page doi:10.1051/0004-6361/202450451
[37]

, keywords =

The Eddington Ratios in Seyfert 2 Galaxies with and without Hidden Broad-Line Regions. , keywords =. doi:10.1086/510708 , archivePrefix =. astro-ph/0611199 , primaryClass =

work page doi:10.1086/510708
[38]

J., Leggett, S

Chandra unveils a binary active galactic nucleus in Mrk 463. , keywords =. doi:10.1111/j.1365-2966.2008.13078.x , archivePrefix =. 0802.0825 , primaryClass =

work page doi:10.1111/j.1365-2966.2008.13078.x 2008
[39]

, keywords =

How Complex is the Obscuration in Active Galactic Nuclei? New Clues from the Suzaku Monitoring of the X-Ray Absorbers in NGC 7582. , keywords =. doi:10.1088/0004-637X/695/1/781 , archivePrefix =. 0901.1973 , primaryClass =

work page doi:10.1088/0004-637x/695/1/781 1973
[40]

CAIXA: a catalogue of AGN in the XMM-Newton archive. I. Spectral analysis. , keywords =. doi:10.1051/0004-6361:200810620 , archivePrefix =. 0811.1126 , primaryClass =

work page doi:10.1051/0004-6361:200810620
[41]

L., Pinfield, D

Simultaneous X-ray and optical observations of true type 2 Seyfert galaxies. , keywords =. doi:10.1111/j.1365-2966.2012.21959.x , archivePrefix =. 1209.0274 , primaryClass =

work page doi:10.1111/j.1365-2966.2012.21959.x 2012
[42]

, keywords =

The Kozai Mechanism and the Evolution of Binary Supermassive Black Holes. , keywords =. doi:10.1086/34265510.48550/arXiv.astro-ph/0203370 , archivePrefix =. astro-ph/0203370 , primaryClass =

work page doi:10.1086/34265510.48550/arxiv.astro-ph/0203370
[43]

, keywords =

PS16dtm: A Tidal Disruption Event in a Narrow-line Seyfert 1 Galaxy. , keywords =. doi:10.3847/1538-4357/aa77f7 , archivePrefix =. 1703.07816 , primaryClass =

work page doi:10.3847/1538-4357/aa77f7
[44]

D., & McKee, C

Reverberation mapping of the emission line regions of Seyfert galaxies and quasars. , keywords =. doi:10.1086/159843 , adsurl =

work page doi:10.1086/159843
[45]

J., Leggett, S

Effects of gravitational-wave recoil on the dynamics and growth of supermassive black holes. , keywords =. doi:10.1111/j.1365-2966.2008.13790.x , archivePrefix =. 0805.1420 , primaryClass =

work page doi:10.1111/j.1365-2966.2008.13790.x 2008
[46]

Living Rev

Electromagnetic counterparts to massive black-hole mergers. Living Rev. Relativ. , keywords =. doi:10.1007/s41114-022-00037-8 , archivePrefix =. , primaryClass =

work page doi:10.1007/s41114-022-00037-8
[47]

The Near-Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope. III. Integral-field spectroscopy. , keywords =. doi:10.1051/0004-6361/202142589 , archivePrefix =. 2202.03308 , primaryClass =

work page doi:10.1051/0004-6361/202142589
[48]

and Wolfire, Mark and Leroy, Adam K

The CO-to-H _ 2 Conversion Factor. , keywords =. doi:10.1146/annurev-astro-082812-140944 , archivePrefix =. 1301.3498 , primaryClass =

work page Pith review doi:10.1146/annurev-astro-082812-140944
[49]

, keywords =

Evidence for Periodicity in 43 year-long Monitoring of NGC 5548. , keywords =. doi:10.3847/0067-0049/225/2/29 , archivePrefix =. 1606.04606 , primaryClass =

work page doi:10.3847/0067-0049/225/2/29
[50]

, keywords =

The Emission-Line Properties of Low-Redshift Quasi-stellar Objects. , keywords =. doi:10.1086/191661 , adsurl =

work page doi:10.1086/191661
[51]

, keywords =

The Wasilewski Sample of Emission-Line Galaxies: Follow-up CCD Imaging and Spectroscopic and IRAS Observations. , keywords =. doi:10.1086/191341 , adsurl =

work page doi:10.1086/191341
[52]

MNRAS , author =

The cosmological evolution of the QSO luminosity density and of the star formation rate. , keywords =. doi:10.1046/j.1365-8711.1998.01264.x , archivePrefix =. astro-ph/9710134 , primaryClass =

work page doi:10.1046/j.1365-8711.1998.01264.x 1998
[53]

J., Lucas, P

Further calibration of the Swift ultraviolet/optical telescope. , archivePrefix = "arXiv", eprint =. doi:10.1111/j.1365-2966.2010.16832.x , adsurl =

work page doi:10.1111/j.1365-2966.2010.16832.x 2010
[54]

, keywords =

The Intermediate Line Region of QSOs. , keywords =. doi:10.1086/174425 , adsurl =

work page doi:10.1086/174425
[55]

, keywords =

Discovery of a Radio-loud/Radio-quiet Binary Quasar. , keywords =. doi:10.1086/311956 , archivePrefix =. astro-ph/9901387 , primaryClass =

work page doi:10.1086/311956
[56]

, keywords =

An Atlas of Galaxy Spectral Energy Distributions from the Ultraviolet to the Mid-infrared. , keywords =. doi:10.1088/0067-0049/212/2/18 , archivePrefix =. 1312.3029 , primaryClass =

work page doi:10.1088/0067-0049/212/2/18
[57]

, keywords =

Molecular outflow and feedback in the obscured quasar XID2028 revealed by ALMA. , keywords =. doi:10.1051/0004-6361/201731641 , archivePrefix =. 1712.04505 , primaryClass =

work page doi:10.1051/0004-6361/201731641
[58]

2003, MNRAS, 340, 1214, doi: 10.1046/j.1365-8711.2003.06380.x

Stellar population synthesis at the resolution of 2003. , keywords =. doi:10.1046/j.1365-8711.2003.06897.x , archivePrefix =. astro-ph/0309134 , primaryClass =

work page doi:10.1046/j.1365-8711.2003.06897.x 2003
[59]

2011 , month = feb, pages =

, title =. 2011 , month = feb, pages =. arXiv , doi =:1008.4382 , file =

work page arXiv 2011
[60]

J., Shen, Y., Blaes, O., et al

A characteristic optical variability time scale in astrophysical accretion disks. Science , keywords =. doi:10.1126/science.abg9933 , archivePrefix =. 2108.05389 , primaryClass =

work page doi:10.1126/science.abg9933
[61]

J., Stone, Z., Shen, Y ., & Jiang, Y .-F

Too Quiet for Comfort: Local Little Red Dots Lack Variability over Decades. arXiv e-prints , keywords =. doi:10.48550/arXiv.2511.16082 , archivePrefix =. 2511.16082 , primaryClass =

work page doi:10.48550/arxiv.2511.16082
[62]

The Swift X-ray Telescope

The Swift X-Ray Telescope. , keywords =. doi:10.1007/s11214-005-5097-2 , archivePrefix =. astro-ph/0508071 , primaryClass =

work page Pith review doi:10.1007/s11214-005-5097-2
[63]

doi:10.5281/zenodo.6984365 , version =

JWST Calibration Pipeline. doi:10.5281/zenodo.6984365 , version =

work page doi:10.5281/zenodo.6984365
[64]

J., Almaini, O., et al

Testing thermal reprocessing in active galactic nuclei accretion discs. , keywords =. doi:10.1111/j.1365-2966.2007.12098.x , archivePrefix =. 0706.1464 , primaryClass =

work page doi:10.1111/j.1365-2966.2007.12098.x 2007
[65]

, keywords =

Pairing of Supermassive Black Holes in Unequal-Mass Galaxy Mergers. , keywords =. doi:10.1088/0004-637X/696/1/L89 , archivePrefix =. 0811.0615 , primaryClass =

work page doi:10.1088/0004-637x/696/1/l89
[66]

C., et al

The Dust Content and Opacity of Actively Star-forming Galaxies. , keywords =. doi:10.1086/308692 , archivePrefix =. astro-ph/9911459 , primaryClass =

work page Pith review doi:10.1086/308692
[67]

, keywords =

Observational evidence of quasar feedback quenching star formation at high redshift. , keywords =. doi:10.1051/0004-6361/201118358 , archivePrefix =. 1112.3071 , primaryClass =

work page doi:10.1051/0004-6361/201118358
[68]

2004, PASP, 116, 138, doi: 10.1086/381875

Parametric Recovery of Line-of-Sight Velocity Distributions from Absorption-Line Spectra of Galaxies via Penalized Likelihood. , keywords =. doi:10.1086/381875 , archivePrefix =. astro-ph/0312201 , primaryClass =

work page doi:10.1086/381875
[69]

, keywords =

Dynamical Masses of Early-Type Galaxies at z -0.5ex 2: Are they Truly Superdense?. , keywords =. doi:10.1088/0004-637X/704/1/L34 , archivePrefix =. 0906.3648 , primaryClass =

work page doi:10.1088/0004-637x/704/1/l34
[70]

2017, MNRAS, 466, 798, doi: 10.1093/mnras/stw3020

Improving the full spectrum fitting method: accurate convolution with Gauss-Hermite functions. , keywords =. doi:10.1093/mnras/stw3020 , archivePrefix =. 1607.08538 , primaryClass =

work page internal anchor Pith review doi:10.1093/mnras/stw3020
[71]

MNRAS , eprint =

Full spectrum fitting with photometry in PPXF: stellar population versus dynamical masses, non-parametric star formation history and metallicity for 3200 LEGA-C galaxies at redshift z 0.8. MNRAS , eprint =
[72]

A., Clayton, G

The Relationship between Infrared, Optical, and Ultraviolet Extinction. , keywords =. doi:10.1086/167900 , adsurl =

work page doi:10.1086/167900
[73]

, keywords =

Cool Gas in High-Redshift Galaxies. , keywords =. doi:10.1146/annurev-astro-082812-140953 , archivePrefix =. 1301.0371 , primaryClass =

work page doi:10.1146/annurev-astro-082812-140953
[74]

2022, , 134, 114501, 10.1088/1538-3873/ac9642

CASA, the Common Astronomy Software Applications for Radio Astronomy. , keywords =. doi:10.1088/1538-3873/ac9642 , archivePrefix =. 2210.02276 , primaryClass =

work page doi:10.1088/1538-3873/ac9642
[75]

, keywords =

A Quasar-based Supermassive Black Hole Binary Population Model: Implications for the Gravitational Wave Background. , keywords =. doi:10.3847/1538-4357/ac32de , archivePrefix =. 2107.11390 , primaryClass =

work page doi:10.3847/1538-4357/ac32de
[76]

Centrella, J

Reviews of Modern Physics , year =. arXiv , doi =:1010.5260 , file =

work page arXiv
[77]

arXiv e-prints , keywords =

The Pan-STARRS1 Surveys. arXiv e-prints , keywords =
[78]

2016, MNRAS, 463, 2145, doi:10.1093/mnras/stw1838

A population of short-period variable quasars from PTF as supermassive black hole binary candidates. , keywords =. doi:10.1093/mnras/stw1838 , archivePrefix =. 1604.01020 , primaryClass =

work page doi:10.1093/mnras/stw1838
[79]

, keywords =

Candidate periodically variable quasars from the Dark Energy Survey and the Sloan Digital Sky Survey. , keywords =. doi:10.1093/mnras/staa2957 , archivePrefix =. 2008.12329 , primaryClass =

work page doi:10.1093/mnras/staa2957 2008
[80]

arXiv e-prints , keywords =

Small-scale double quasars discovered in the DECam Legacy Survey. arXiv e-prints , keywords =

Showing first 80 references.