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arxiv: 2604.25219 · v1 · submitted 2026-04-28 · 🌌 astro-ph.GA

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Spectral Evolution and Transient Broad-Line Features in the Isolated AGN UNAM-KIAS 613

Castalia Alenka Negrete, Edgar Cortes-Su\'arez, H\'ector Manuel Hern\'andez-Toledo, Miguel \'Angel Arag\'on-Calvo, Paola Marziani

Authors on Pith no claims yet

Pith reviewed 2026-05-07 15:54 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords AGNbroad emission linesspectral evolutionoutflowsisolated galaxieslow-luminosity AGNH-alpha profile
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The pith

The double-peaked broad Hα profile in the low-luminosity AGN UNAM-KIAS 613 is a transient feature from a one-time bipolar outflow.

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

Multi-epoch spectra of the AGN in the isolated elliptical galaxy UNAM-KIAS 613 show a double-peaked broad Hα line in 2006 that had disappeared by 2018 and 2023, leaving a single central peak. The authors interpret this as evidence that the double peaks came from a bipolar outflow event rather than a stable relativistic disk or a tidal disruption. No continuum variability was seen over more than a decade, supporting a one-time event in this sub-Eddington system with a black hole mass around 10 to the 7.2 solar masses. The findings point to quick changes in line-emitting gas even when the overall accretion rate stays low. This case illustrates how disk, outflow, and host-galaxy processes interact in low-mass, low-accretion AGNs that are common but hard to study in detail.

Core claim

The paper reports that the distinctive double-peaked structure in the broad Hα emission line, seen in 2006 SDSS data and initially modeled as a relativistic accretion disk, was no longer present in 2018 and 2023 observations, which showed only a single-peaked central broad component. With no significant continuum variability detected in light curves from 2012 to 2025 and supporting multi-wavelength data indicating a radio-quiet, sub-Eddington AGN, the authors propose the double-peak structure arose from a transient bipolar outflow event. They suggest the system may be experiencing a turn-off of the accretion disk emitting region or a transition between accretion modes, highlighting the role

What carries the argument

The transient double-peaked broad-line profile interpreted as emission from a one-time bipolar outflow rather than a persistent disk.

Load-bearing premise

The interpretation assumes that the lack of detected continuum variability over the 2012-2025 period rules out a tidal disruption event and indicates the outflow was a single past event without needing quantitative modeling of the kinematics.

What would settle it

Detection of kinematic evidence for an outflow, such as blueshifted absorption lines or velocity-resolved maps, in new high-resolution spectra would support the bipolar outflow model; reappearance of the double peaks would challenge the transient one-time event idea.

Figures

Figures reproduced from arXiv: 2604.25219 by Castalia Alenka Negrete, Edgar Cortes-Su\'arez, H\'ector Manuel Hern\'andez-Toledo, Miguel \'Angel Arag\'on-Calvo, Paola Marziani.

Figure 1
Figure 1. Figure 1: Top panel: UNAM Kias 613 spectrum from SDSS Data Release 7 (black line). A stellar population synthesis was performed with STARLIGHT obtaining the best model (red line), the host galaxy spectrum (green line), the AGN power law (orange line) and the emission spectrum obtained by subtracting the best model to the observed spectrum (blue line). Bottom panel: Flux errors of the model. UNAM-KIAS sample (< 4%) u… view at source ↗
Figure 2
Figure 2. Figure 2: Asiago spectrum (top panel) and OAN-SPM spectrum (bottom panel) for UNAM-KIAS 613. In both cases, the stellar population model derived from the SDSS spectrum (red line) was subtracted to isolate the AGN emission-line spectrum (blue line). The observed spectra are shown in black. lower spectral resolution, which prevented reliable deblending of the narrow [N ii] 𝜆𝜆6548,6584 doublet from the H𝛼 line. Data re… view at source ↗
Figure 3
Figure 3. Figure 3: Left figure: Comparison between the H𝛼 region after normalizing by the [Nii]+H𝛼 flux. The SDSS spectrum is shown in all spectra. Right figures: The emission lines fitting procedure of each observation. In black, the observed spectrum, blue is the best model, gray is the narrow emission lines, and red is the broad emission lines. Spectrum Normalizations Scaled Continuum [Oi] H𝛼NC + [Nii] [Sii] 𝑓6200−6250 𝜆 … view at source ↗
Figure 5
Figure 5. Figure 5: The emission line profile produced by a bipolar outflow constrained between a cone of semiaperture Θ0 = 20 degrees, with the cone axis inclined by 𝑖 = 5 with respect to the line of sight (blue line). The bipolar outflow produces the satellite components that are observed at ≈ ±7500 km s−1 . A central Gaussian component with the same parameters (FWHM, shift) of the empirical model shown in view at source ↗
Figure 4
Figure 4. Figure 4: The disk model of UNAM-Kias 613 following Chen & Halpern (1989) (red line). The black line traces the continuum substract H𝛼 profile of the SDSS spectrum; the green line the residual after the subtraction of the disk model. 𝑡surv ∼ 𝑡𝜈 (𝑅out) ∼ 𝑅out/|𝑣r,drift|, and in an 𝛼-disk the inward drift speed is of order |𝑣r,drift| ∼ 𝛼 (𝐻/𝑅) 2 𝑣Kepl, implying that 𝑡𝜈 (𝑅) ∼ 1/𝛼 (𝑅/𝐻) 2 1/Ω𝐾 , with Ω𝐾 = √︁ 𝐺𝑀/𝑅3 . Sca… view at source ↗
Figure 6
Figure 6. Figure 6: Left panel: Optical light curve of UNAM-KIAS 613 from 2005 to 2025 in the 𝑉 and 𝑔 bands, with fluxes normalized for comparison. Purple symbols correspond to Catalina data (Drake et al. 2014), while blue and green symbols correspond to ASAS-SN observations (Kochanek et al. 2017). Vertical dashed lines mark the epochs of spectroscopic observations: SDSS (purple), Asiago (blue), and OAN-SPM (green). No signif… view at source ↗
Figure 7
Figure 7. Figure 7: The classification of radio sources. Left plot shows the limit between radio loud and star forming sources (Best & Heckman 2012) while right plot the best fit of star forming sources from Mingo et al. (2016). UK 613 is shown as red star and the gray markers are from the type 1 AGN sample from Cortes-Suárez et al. (2022). AGN AGN AGN LINER LINER LINER Star Forming Star Forming Star Forming Composite view at source ↗
Figure 8
Figure 8. Figure 8: The narrow line diagnostic diagrams from Baldwin et al. (1981). UK 613 is shown as a red star. Further constraints come from optical emission-line diagnostics. Based on the BPT diagrams (Baldwin et al. 1981, view at source ↗
Figure 9
Figure 9. Figure 9: Spectral Energy Distributions (SED) of three elliptical galaxies. From left to right: SED of small aperture (∼2–5”), SED of medium aperture (∼4–8”), and SED of big aperture (>10”), respectively. In all panels there are the SED of a massive classic elliptical galaxy (red stars), a blue-like less massive elliptical galaxy (blue stars) and UNAM-Kias 613 (purple stars). Range Frequency (Hz) Specific flux (Jy) … view at source ↗
Figure 10
Figure 10. Figure 10: The Large Scale Structure around UK 613. Left: three orthogonal cuts (distance-RA, RA-DEC and RA-distance clockwise) in the density field centered on UK 613 (marked by a red cross) showing the surrounding network of filaments, walls, and voids. The color palette is such that white and intense yellow roughly represents dense regions in clusters and groups, green walls and filaments and dark blue underdense… view at source ↗
Figure 11
Figure 11. Figure 11: Distribution of galaxies centered on UK 613. Black circles cor￾respond to neighboring galaxies. The horizontal rings show distances of 1,3 and 5 Mpc and the vertical lines indicate the distance from the horizontal plane to each galaxy (solid/dashed lines correspond to galaxies above//below the plane respectively). For visualization purposes the galaxies were oriented with the local geometry (see text for … view at source ↗
read the original abstract

We present multi-epoch optical spectroscopy of the isolated elliptical galaxy UNAM-KIAS 613, hosting a low-luminosity Type 1 AGN. Analysis of archival Sloan Digital Sky Survey (SDSS) data from 2006 reveals a distinctive double-peaked broad H$\alpha$ profile, tentatively modeled by a relativistic accretion disk. Follow-up observations in 2018 and 2023 show the disappearance of the red and blue wings, leaving only a single-peaked, central broad component. No significant continuum variability is detected in ASAS-SN and Catalina light curves over 2012-2025, and multi-wavelength data (radio, mid-IR, X-ray) confirm a sub-Eddington, radio-quiet AGN (Eddington ratio $\approx$0.03-0.04, black hole mass $\approx$10$^{7.2}$ M$\odot$). We propose that the double-peak structure is in reality transient, and arose from a one-time bipolar outflow event rather than a stable disk or from a Tidal Disruption Event. The mid-IR SED and radio luminosity place UK 613 on the boundary between AGN and star formation dominance, suggesting residual star formation, while we have found that the isolated environment seems to be prone to the rejuvenation of ellipticals by recent ($\lesssim$ 1 Gyr) cold gas. We also examined its location within the cosmic web with the aim of identifying possible distinctive effects imprinted on its spectroscopic properties. Ultimately, our results are consistent that UNAM-KIAS 613 might have under gone a ''turn-off'' of the accretion disk emitting region or a transition between a radiatively-inefficient and radiatively-efficient accretion mode, and highlight the complex interplay of disk, outflow, host processes and environment in low-accretion, low-black hole mass AGNs, an AGN population still largely unexplored to-date.

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

2 major / 3 minor

Summary. The manuscript reports multi-epoch optical spectroscopy of the isolated elliptical galaxy UNAM-KIAS 613 hosting a low-luminosity Type 1 AGN. Archival 2006 SDSS spectra show a double-peaked broad Hα profile tentatively fit as a relativistic accretion disk; 2018 and 2023 follow-up spectra show the red and blue wings have disappeared, leaving a single-peaked central component. Public ASAS-SN and Catalina light curves exhibit no significant continuum variability from 2012–2025, and multi-wavelength data indicate sub-Eddington accretion (Eddington ratio ≈0.03–0.04, M_BH ≈10^{7.2} M_⊙). The authors interpret the transient double-peaked feature as arising from a one-time bipolar outflow rather than a stable disk or tidal disruption event, and discuss possible accretion-mode transitions, residual star formation, and the galaxy’s isolated environment.

Significance. The multi-epoch spectroscopic documentation of the broad-line profile change, combined with the absence of detectable continuum variability over more than a decade, provides a valuable observational constraint on spectral evolution in low-luminosity AGNs. If the outflow interpretation can be placed on a quantitative footing, the work would help illuminate the interplay between disk, outflow, and host-galaxy processes in the still-underexplored regime of sub-Eddington, low-mass black holes. The use of public photometric archives and the environmental context add useful context, though the interpretive step remains qualitative.

major comments (2)
  1. [Abstract and Discussion] Abstract and Discussion: The central claim that the 2006 double-peaked Hα profile is better explained by a one-time bipolar outflow than by a stable relativistic disk or a TDE rests entirely on the negative observation of no continuum variability and the later disappearance of the wings. No kinematic decomposition (e.g., two-component velocity offsets, P-Cygni profile fits, or wing-velocity modeling), no χ² or residual comparison to the tentative relativistic-disk model, and no light-curve or timing simulations to test whether a TDE could have faded before 2012 monitoring are presented. This absence of positive dynamical or temporal evidence is load-bearing for the preferred interpretation.
  2. [Results (multi-wavelength properties)] Results section (multi-wavelength properties): The Eddington ratio (≈0.03–0.04) and black-hole mass (≈10^{7.2} M_⊙) are invoked to argue for a sub-Eddington state inconsistent with ongoing TDE activity, yet no derivation details, uncertainty estimates, or sensitivity tests on these parameters are supplied. Without quantified errors or alternative accretion-rate histories, the exclusion of a TDE scenario remains qualitative.
minor comments (3)
  1. [Abstract] The phrasing “our results are consistent that UNAM-KIAS 613 might have under gone a ‘turn-off’” contains a grammatical error (“under gone” → “undergone”) and an awkward construction; rephrase for clarity.
  2. [Discussion] The statement that “the isolated environment seems to be prone to the rejuvenation of ellipticals by recent (≲ 1 Gyr) cold gas” is vague; specify what observational or simulation evidence supports this claim for UK 613 or the sample.
  3. [Discussion] The sentence “We also examined its location within the cosmic web with the aim of identifying possible distinctive effects imprinted on its spectroscopic properties” does not report what, if any, distinctive effects were actually found; either quantify the result or remove the clause.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript on the spectral evolution of UNAM-KIAS 613. We have considered each major comment in detail and outline below how we will revise the paper to address the concerns while preserving the observational focus of the work.

read point-by-point responses

  1. Referee: [Abstract and Discussion] Abstract and Discussion: The central claim that the 2006 double-peaked Hα profile is better explained by a one-time bipolar outflow than by a stable relativistic disk or a TDE rests entirely on the negative observation of no continuum variability and the later disappearance of the wings. No kinematic decomposition (e.g., two-component velocity offsets, P-Cygni profile fits, or wing-velocity modeling), no χ² or residual comparison to the tentative relativistic-disk model, and no light-curve or timing simulations to test whether a TDE could have faded before 2012 monitoring are presented. This absence of positive dynamical or temporal evidence is load-bearing for the preferred interpretation.

    Authors: We acknowledge that the preferred outflow interpretation would be strengthened by additional quantitative tests. In the revised manuscript we will add, in the Results section, a direct χ² comparison of the 2006 Hα profile against the relativistic disk model, a single broad Gaussian, and a two-Gaussian decomposition, together with residual plots. We will also report the velocity offsets obtained from the two-Gaussian fit and discuss their implications for a bipolar outflow while noting the moderate S/N of the archival spectrum as a limitation. For the TDE scenario we will expand the Discussion to include a comparison with published TDE light-curve decay timescales and argue that the absence of detectable variability from 2012 onward, combined with the 12-year gap before monitoring began, makes a TDE origin less likely; we will not add new hydrodynamic simulations, as these lie outside the scope of this observational study. These additions will provide a more balanced presentation without altering the core observational results. revision: yes

  2. Referee: [Results (multi-wavelength properties)] Results section (multi-wavelength properties): The Eddington ratio (≈0.03–0.04) and black-hole mass (≈10^{7.2} M_⊙) are invoked to argue for a sub-Eddington state inconsistent with ongoing TDE activity, yet no derivation details, uncertainty estimates, or sensitivity tests on these parameters are supplied. Without quantified errors or alternative accretion-rate histories, the exclusion of a TDE scenario remains qualitative.

    Authors: We agree that greater transparency is needed. The black-hole mass was obtained via the single-epoch virial estimator using the broad Hα FWHM and luminosity, and the bolometric luminosity was derived from the 5100 Å continuum with a standard correction factor, cross-checked against X-ray and WISE mid-IR luminosities. In the revised Results section we will insert an explicit subsection presenting the adopted formulas, the measured line parameters with their fitting uncertainties, and the propagated statistical plus systematic errors (including the typical 0.3–0.5 dex uncertainty on virial masses). We will also report sensitivity tests varying the bolometric correction by ±20 % and the assumed Eddington ratio range. While a complete time-dependent accretion-rate reconstruction is not possible with the existing sparse data, we will note that the decade-long low-luminosity state is inconsistent with the rapid decline expected for a TDE, thereby making the sub-Eddington argument more quantitative. revision: yes

Circularity Check

0 steps flagged

No significant circularity; observational claims rest on direct data comparison without self-referential reductions.

full rationale

The manuscript reports multi-epoch spectra (SDSS 2006 showing double-peaked Hα, later epochs showing single peak), public light curves (ASAS-SN/Catalina 2012-2025 with no variability), and multi-wavelength properties (sub-Eddington ratio ~0.03-0.04). The central proposal—that the 2006 profile arose from a one-time bipolar outflow rather than stable disk or TDE—is an interpretive inference from the negative observation of wing disappearance plus absent continuum variability. No equations, fitted parameters renamed as predictions, or self-citation chains appear in the provided text or abstract. The argument does not reduce by construction to its inputs; it is an external comparison against archival and survey data. This is the most common honest finding for purely observational papers.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 1 invented entities

The central claims depend on standard AGN parameter estimation methods and the post-hoc interpretation of line-profile changes as a transient outflow; no new physical constants are introduced but several fitted quantities and domain assumptions underpin the narrative.

free parameters (2)
  • Black hole mass = 10^{7.2} M_sun
    Estimated from broad-line width and continuum luminosity using standard virial methods
  • Eddington ratio = 0.03-0.04
    Derived from bolometric luminosity and black-hole mass
axioms (2)
  • domain assumption Double-peaked broad Hα can be tentatively modeled as emission from a relativistic accretion disk
    Invoked for the 2006 SDSS spectrum in the abstract
  • domain assumption Absence of significant continuum variability rules out a tidal disruption event
    Based on ASAS-SN and Catalina light curves spanning 2012-2025
invented entities (1)
  • One-time bipolar outflow event no independent evidence
    purpose: To explain the transient appearance and disappearance of the double-peaked Hα wings
    Postulated to account for the observed spectral evolution without invoking a stable disk or TDE

pith-pipeline@v0.9.0 · 5675 in / 1570 out tokens · 51506 ms · 2026-05-07T15:54:22.073873+00:00 · methodology

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Reference graph

Works this paper leans on

147 extracted references · 139 canonical work pages · 1 internal anchor

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

  2. [2]

    Antonucci R., Hurt T., Agol E., 1996, @doi [ ] 10.1086/309858 , https://ui.adsabs.harvard.edu/abs/1996ApJ...456L..25A 456, L25

    work page doi:10.1086/309858 1996

  3. [3]

    A., 2021, @doi [ ] 10.1093/mnras/stab403 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.503..557A 503, 557

    Aragon-Calvo M. A., 2021, @doi [ ] 10.1093/mnras/stab403 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.503..557A 503, 557

    work page doi:10.1093/mnras/stab403 2021

  4. [4]

    A., 2024, @doi [ ] 10.1093/mnras/stae468 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.529...74A 529, 74

    Aragon-Calvo M. A., 2024, @doi [ ] 10.1093/mnras/stae468 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.529...74A 529, 74

    work page doi:10.1093/mnras/stae468 2024

  5. [5]

    A., Szalay A

    Aragon-Calvo M. A., Szalay A. S., 2013, @doi [ ] 10.1093/mnras/sts281 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.428.3409A 428, 3409

    work page doi:10.1093/mnras/sts281 2013

  6. [6]

    A., Jones B

    Arag \'o n-Calvo M. A., Jones B. J. T., van de Weygaert R., van der Hulst J. M., 2007, @doi [ ] 10.1051/0004-6361:20077880 , https://ui.adsabs.harvard.edu/abs/2007A&A...474..315A 474, 315

    work page doi:10.1051/0004-6361:20077880 2007

  7. [7]

    Astrophysical Journal723(1), 364–382 (2010) https://doi

    Arag \'o n-Calvo M. A., Platen E., van de Weygaert R., Szalay A. S., 2010, @doi [ ] 10.1088/0004-637X/723/1/364 , https://ui.adsabs.harvard.edu/abs/2010ApJ...723..364A 723, 364

    work page doi:10.1088/0004-637x/723/1/364 2010

  8. [8]

    A., Neyrinck M

    Aragon Calvo M. A., Neyrinck M. C., Silk J., 2019, @doi [The Open Journal of Astrophysics] 10.21105/astro.1697.07881 , https://ui.adsabs.harvard.edu/abs/2019OJAp....2E...7A 2, 7

    work page doi:10.21105/astro.1697.07881 2019

  9. [9]

    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

    Assef R. J., et al., 2013, @doi [ ] 10.1088/0004-637X/772/1/26 , https://ui.adsabs.harvard.edu/abs/2013ApJ...772...26A 772, 26

    work page doi:10.1088/0004-637x/772/1/26 2013

  10. [10]

    A., Phillips, M

    Baldwin J. A., Phillips M. M., Terlevich R., 1981, @doi [ ] 10.1086/130766 , http://adsabs.harvard.edu/abs/1981PASP...93....5B 93, 5

    work page doi:10.1086/130766 1981

  11. [11]

    Ballo L., Heras F. J. H., Barcons X., Carrera F. J., 2012, @doi [ ] 10.1051/0004-6361/201117464 , https://ui.adsabs.harvard.edu/abs/2012A&A...545A..66B 545, A66

    work page doi:10.1051/0004-6361/201117464 2012

  12. [12]

    R., 2012, Active Galactic Nuclei

    Beckmann V., Shrader C. R., 2012, Active Galactic Nuclei

    2012

  13. [13]

    The Astrophysical Journal , volume =

    Ben \' tez-Llambay A., Navarro J. F., Abadi M. G., Gottl \"o ber S., Yepes G., Hoffman Y., Steinmetz M., 2013, @doi [ ] 10.1088/2041-8205/763/2/L41 , https://ui.adsabs.harvard.edu/abs/2013ApJ...763L..41B 763, L41

    work page doi:10.1088/2041-8205/763/2/l41 2013

  14. [14]

    The Low-Luminosity End of the Radius-Luminosity Relationship for Active Galactic Nuclei

    Bentz M. C., et al., 2013, @doi [ ] 10.1088/0004-637X/767/2/149 , http://adsabs.harvard.edu/abs/2013 ...767..149B 767, 149

    work page Pith review doi:10.1088/0004-637x/767/2/149 2013

  15. [15]

    2012, MNRAS, 423, 600, doi: 10.1111/j.1365-2966.2012.20901.x

    Best P. N., Heckman T. M., 2012, @doi [ ] 10.1111/j.1365-2966.2012.20414.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.421.1569B 421, 1569

    work page doi:10.1111/j.1365-2966.2012.20414.x 2012

  16. [16]

    Bianchi L., Shiao B., Thilker D., 2017, @doi [ ] 10.3847/1538-4365/aa7053 , https://ui.adsabs.harvard.edu/abs/2017ApJS..230...24B 230, 24

    work page doi:10.3847/1538-4365/aa7053 2017

  17. [17]

    2025, arXiv e-prints, arXiv:2507.01355, doi: 10.48550/arXiv.2507.01355

    Birmingham S., Ward C., Nyland K., Dobie D., Graham M. J., Kaplan D. L., Murphy T., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2507.01355 , https://ui.adsabs.harvard.edu/abs/2025arXiv250701355B p. arXiv:2507.01355

    work page doi:10.48550/arxiv.2507.01355 2025

  18. [18]

    R., Schlegel, D

    Blanton M. R., et al., 2005, @doi [ ] 10.1086/429803 , https://ui.adsabs.harvard.edu/abs/2005AJ....129.2562B 129, 2562

    work page doi:10.1086/429803 2005

  19. [19]

    R., Bershady, M

    Blanton M. R., et al., 2017, @doi [ ] 10.3847/1538-3881/aa7567 , https://ui.adsabs.harvard.edu/abs/2017AJ....154...28B 154, 28

    work page doi:10.3847/1538-3881/aa7567 2017

  20. [20]

    Bon E., Jovanovi \'c P., Marziani P., Bon N., Ota s evi \'c A., 2018, @doi [Frontiers in Astronomy and Space Sciences] 10.3389/fspas.2018.00019 , https://ui.adsabs.harvard.edu/abs/2018FrASS...5...19B 5, 19

    work page doi:10.3389/fspas.2018.00019 2018

  21. [21]

    , keywords =

    Boroson T. A., Green R. F., 1992, @doi [ ] 10.1086/191661 , https://ui.adsabs.harvard.edu/abs/1992 ...80..109B 80, 109

    work page doi:10.1086/191661 1992

  22. [22]

    Bruzual G., Charlot S., 2003, @doi [ ] 10.1046/j.1365-8711.2003.06897.x , https://ui.adsabs.harvard.edu/abs/2003MNRAS.344.1000B 344, 1000

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

  23. [23]

    Bundy K., et al., 2015, @doi [ ] 10.1088/0004-637X/798/1/7 , https://ui.adsabs.harvard.edu/abs/2015ApJ...798....7B 798, 7

    work page Pith review doi:10.1088/0004-637x/798/1/7 2015

  24. [24]

    A., Clayton, G

    Cardelli J. A., Clayton G. C., Mathis J. S., 1989, @doi [ ] 10.1086/167900 , https://ui.adsabs.harvard.edu/abs/1989ApJ...345..245C 345, 245

    work page doi:10.1086/167900 1989

  25. [25]

    Ceccarelli L., Duplancic F., Garcia Lambas D., 2022, @doi [ ] 10.1093/mnras/stab2902 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.509.1805C 509, 1805

    work page doi:10.1093/mnras/stab2902 2022

  26. [26]

    Charalampopoulos P., et al., 2022, @doi [ ] 10.1051/0004-6361/202142122 , https://ui.adsabs.harvard.edu/abs/2022A&A...659A..34C 659, A34

    work page doi:10.1051/0004-6361/202142122 2022

  27. [27]

    P., 1989, @doi [ ] 10.1086/167782 , https://ui.adsabs.harvard.edu/abs/1989ApJ...344..115C 344, 115

    Chen K., Halpern J. P., 1989, @doi [ ] 10.1086/167782 , https://ui.adsabs.harvard.edu/abs/1989ApJ...344..115C 344, 115

    work page doi:10.1086/167782 1989

  28. [28]

    , keywords =

    Chen K., Halpern J. P., Filippenko A. V., 1989, @doi [ ] 10.1086/167332 , https://ui.adsabs.harvard.edu/abs/1989ApJ...339..742C 339, 742

    work page doi:10.1086/167332 1989

  29. [29]

    Choi Y.-Y., Woo J.-H., Park C., 2009, @doi [ ] 10.1088/0004-637X/699/2/1679 , https://ui.adsabs.harvard.edu/abs/2009ApJ...699.1679C 699, 1679

    work page doi:10.1088/0004-637x/699/2/1679 2009

  30. [30]

    D., Drew, J

    Cid Fernandes R., Mateus A., Sodr \'e L., Stasi \'n ska G., Gomes J. M., 2005, @doi [ ] 10.1111/j.1365-2966.2005.08752.x , https://ui.adsabs.harvard.edu/abs/2005MNRAS.358..363C 358, 363

    work page doi:10.1111/j.1365-2966.2005.08752.x 2005

  31. [31]

    V., Gurovich S., D \' az Tello J., S \"o chting I

    Coldwell G. V., Gurovich S., D \' az Tello J., S \"o chting I. K., Lambas D. G., 2014, @doi [ ] 10.1093/mnras/stt1920 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.437.1199C 437, 1199

    work page doi:10.1093/mnras/stt1920 2014

  32. [32]

    V., Pereyra L., Alonso S., Donoso E., Duplancic F., 2017, @doi [ ] 10.1093/mnras/stx294 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.467.3338C 467, 3338

    Coldwell G. V., Pereyra L., Alonso S., Donoso E., Duplancic F., 2017, @doi [ ] 10.1093/mnras/stx294 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.467.3338C 467, 3338

    work page doi:10.1093/mnras/stx294 2017

  33. [33]

    , keywords =

    Condon J. J., Cotton W. D., Greisen E. W., Yin Q. F., Perley R. A., Taylor G. B., Broderick J. J., 1998, @doi [ ] 10.1086/300337 , http://adsabs.harvard.edu/abs/1998AJ....115.1693C 115, 1693

    work page doi:10.1086/300337 1998

  34. [34]

    S., 2008, @doi [ ] 10.1086/524310 , https://ui.adsabs.harvard.edu/abs/2008ApJ...673..715C 673, 715

    Constantin A., Hoyle F., Vogeley M. S., 2008, @doi [ ] 10.1086/524310 , https://ui.adsabs.harvard.edu/abs/2008ApJ...673..715C 673, 715

    work page doi:10.1086/524310 2008

  35. [35]

    A., Hern \'a ndez-Toledo H

    Cortes-Su \'a rez E., Negrete C. A., Hern \'a ndez-Toledo H. M., Ibarra-Medel H., Lacerna I., 2022, @doi [ ] 10.1093/mnras/stac1505 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.514.3626C 514, 3626

    work page doi:10.1093/mnras/stac1505 2022

  36. [36]

    2012, MNRAS, 420, 1825, doi: 10.1111/j.1365-2966.2011.19805.x

    Croom S. M., et al., 2012, @doi [ ] 10.1111/j.1365-2966.2011.20365.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.421..872C 421, 872

    work page doi:10.1111/j.1365-2966.2011.20365.x 2012

  37. [37]

    Davenport J., 2021, PyKOSMOS: A Python-Based Spectral Reduction Suite for KOSMOS at APO, @doi 10.5281/zenodo.5120786 , https://doi.org/10.5281/zenodo.5120786

    work page doi:10.5281/zenodo.5120786 2021

  38. [38]

    Decarli R., Dotti M., Treves A., 2011, @doi [ ] 10.1111/j.1365-2966.2010.18102.x , http://adsabs.harvard.edu/abs/2011MNRAS.413...39D 413, 39

    work page doi:10.1111/j.1365-2966.2010.18102.x 2011

  39. [39]

    Dey A., et al., 2019, @doi [ ] 10.3847/1538-3881/ab089d , https://ui.adsabs.harvard.edu/abs/2019AJ....157..168D 157, 168

    work page doi:10.3847/1538-3881/ab089d 2019

  40. [40]

    C., Liu J., Mathes G., Flohic H

    Doan A., Eracleous M., Runnoe J. C., Liu J., Mathes G., Flohic H. M. L. G., 2020, @doi [ ] 10.1093/mnras/stz2705 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.491.1104D 491, 1104

    work page doi:10.1093/mnras/stz2705 2020

  41. [41]

    2012, MNRAS, 420, 1825, doi: 10.1111/j.1365-2966.2011.19805.x

    Done C., Davis S. W., Jin C., Blaes O., Ward M., 2012, @doi [ ] 10.1111/j.1365-2966.2011.19779.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.420.1848D 420, 1848

    work page doi:10.1111/j.1365-2966.2011.19779.x 2012

  42. [42]

    J., et al., 2014, @doi [ ] 10.1088/0067-0049/213/1/9 , https://ui.adsabs.harvard.edu/abs/2014ApJS..213....9D 213, 9

    Drake A. J., et al., 2014, @doi [ ] 10.1088/0067-0049/213/1/9 , https://ui.adsabs.harvard.edu/abs/2014ApJS..213....9D 213, 9

    work page doi:10.1088/0067-0049/213/1/9 2014

  43. [43]

    M., Collin-Souffrin S., 1990, A&Ap, http://adsabs.harvard.edu/abs/1990A\

    Dumont A. M., Collin-Souffrin S., 1990, A&Ap, http://adsabs.harvard.edu/abs/1990A\

    1990

  44. [44]

    , keywords =

    Elitzur M., Ho L. C., 2009, @doi [ ] 10.1088/0004-637X/701/2/L91 , https://ui.adsabs.harvard.edu/abs/2009ApJ...701L..91E 701, L91

    work page doi:10.1088/0004-637x/701/2/l91 2009

  45. [45]

    , keywords =

    Elitzur M., Ho L. C., Trump J. R., 2014, @doi [ ] 10.1093/mnras/stt2445 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.438.3340E 438, 3340

    work page doi:10.1093/mnras/stt2445 2014

  46. [46]

    Elvis M., 2000, @doi [ ] 10.1086/317778 , https://ui.adsabs.harvard.edu/abs/2000ApJ...545...63E 545, 63

    work page doi:10.1086/317778 2000

  47. [47]

    , keywords =

    Eracleous M., Halpern J. P., 1994, @doi [ ] 10.1086/191856 , https://ui.adsabs.harvard.edu/abs/1994ApJS...90....1E 90, 1

    work page doi:10.1086/191856 1994

  48. [48]

    , keywords =

    Eracleous M., Halpern J. P., 2003, @doi [ ] 10.1086/379540 , https://ui.adsabs.harvard.edu/abs/2003ApJ...599..886E 599, 886

    work page doi:10.1086/379540 2003

  49. [49]

    , keywords =

    Eracleous M., Livio M., Halpern J. P., Storchi-Bergmann T., 1995, @doi [ ] 10.1086/175104 , https://ui.adsabs.harvard.edu/abs/1995ApJ...438..610E 438, 610

    work page doi:10.1086/175104 1995

  50. [50]

    Flohic H. M. L. G., Eracleous M., 2008, @doi [ ] 10.1086/590547 , https://ui.adsabs.harvard.edu/abs/2008ApJ...686..138F 686, 138

    work page doi:10.1086/590547 2008

  51. [51]

    Flohic H. M. L. G., Eracleous M., Bogdanovi \'c T., 2012, @doi [ ] 10.1088/0004-637X/753/2/133 , https://ui.adsabs.harvard.edu/abs/2012ApJ...753..133F 753, 133

    work page doi:10.1088/0004-637x/753/2/133 2012

  52. [52]

    M., 1988, in Miller H

    Gaskell C. M., 1988, in Miller H. R., Wiita P. J., eds, , Vol. 307, Active Galactic Nuclei. Springer-Verlag, p. 61, @doi 10.1007/3-540-19492-4_168

    work page doi:10.1007/3-540-19492-4_168 1988

  53. [53]

    , keywords =

    Gaskell C. M., Harrington P. Z., 2018, @doi [ ] 10.1093/mnras/sty848 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.478.1660G 478, 1660

    work page doi:10.1093/mnras/sty848 2018

  54. [54]

    George K., 2023, @doi [ ] 10.1051/0004-6361/202345837 , https://ui.adsabs.harvard.edu/abs/2023A&A...671A.166G 671, A166

    work page doi:10.1051/0004-6361/202345837 2023

  55. [55]

    George K., Zingade K., 2015, @doi [ ] 10.1051/0004-6361/201424826 , https://ui.adsabs.harvard.edu/abs/2015A&A...583A.103G 583, A103

    work page doi:10.1051/0004-6361/201424826 2015

  56. [56]

    P., Eracleous M., 2007, @doi [ ] 10.1086/511032 , https://ui.adsabs.harvard.edu/abs/2007ApJS..169..167G 169, 167

    Gezari S., Halpern J. P., Eracleous M., 2007, @doi [ ] 10.1086/511032 , https://ui.adsabs.harvard.edu/abs/2007ApJS..169..167G 169, 167

    work page doi:10.1086/511032 2007

  57. [57]

    M., Maccacaro T., Schild R

    Gioia I. M., Maccacaro T., Schild R. E., Wolter A., Stocke J. T., Morris S. L., Henry J. P., 1990, @doi [ ] 10.1086/191426 , https://ui.adsabs.harvard.edu/abs/1990ApJS...72..567G 72, 567

    work page doi:10.1086/191426 1990

  58. [58]

    Estimating Black Hole Masses in Active Galaxies Using the Halpha Emission Line

    Greene J. E., Ho L. C., 2005, @doi [ ] 10.1086/431897 , https://ui.adsabs.harvard.edu/abs/2005ApJ...630..122G 630, 122

    work page Pith review doi:10.1086/431897 2005

  59. [59]

    P., Eracleous M., 1994, @doi [ ] 10.1086/187537 , https://ui.adsabs.harvard.edu/abs/1994ApJ...433L..17H 433, L17

    Halpern J. P., Eracleous M., 1994, @doi [ ] 10.1086/187537 , https://ui.adsabs.harvard.edu/abs/1994ApJ...433L..17H 433, L17

    work page doi:10.1086/187537 1994

  60. [60]

    P., Filippenko A

    Halpern J. P., Filippenko A. V., 1988, @doi [ ] 10.1038/331046a0 , https://ui.adsabs.harvard.edu/abs/1988Natur.331...46H 331, 46

    work page doi:10.1038/331046a0 1988

  61. [61]

    Hao L., et al., 2005, @doi [ ] 10.1086/428485 , https://ui.adsabs.harvard.edu/abs/2005AJ....129.1783H 129, 1783

    work page doi:10.1086/428485 2005

  62. [62]

    E., Krawczynski H., 2006, @doi [ ] 10.1146/annurev.astro.44.051905.092446 , https://ui.adsabs.harvard.edu/abs/2006ARA&A..44..463H 44, 463

    Harris D. E., Krawczynski H., 2006, @doi [ ] 10.1146/annurev.astro.44.051905.092446 , https://ui.adsabs.harvard.edu/abs/2006ARA&A..44..463H 44, 463

    work page doi:10.1146/annurev.astro.44.051905.092446 2006

  63. [63]

    Hayasaki K., Stone N., Loeb A., 2016, @doi [ ] 10.1093/mnras/stw1387 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.461.3760H 461, 3760

    work page doi:10.1093/mnras/stw1387 2016

  64. [64]

    M., V \'a zquez-Mata J

    Hern \'a ndez-Toledo H. M., V \'a zquez-Mata J. A., Mart \' nez-V \'a zquez L. A., Choi Y.-Y., Park C., 2010, @doi [ ] 10.1088/0004-6256/139/6/2525 , https://ui.adsabs.harvard.edu/abs/2010AJ....139.2525H 139, 2525

    work page doi:10.1088/0004-6256/139/6/2525 2010

  65. [65]

    L., & Haiman, Z

    Hopkins P. F., Bundy K., Murray N., Quataert E., Lauer T. R., Ma C.-P., 2009, @doi [ ] 10.1111/j.1365-2966.2009.15062.x , https://ui.adsabs.harvard.edu/abs/2009MNRAS.398..898H 398, 898

    work page doi:10.1111/j.1365-2966.2009.15062.x 2009

  66. [66]

    , keywords =

    Huang S., Ho L. C., Peng C. Y., Li Z.-Y., Barth A. J., 2013, @doi [ ] 10.1088/2041-8205/768/2/L28 , https://ui.adsabs.harvard.edu/abs/2013ApJ...768L..28H 768, L28

    work page doi:10.1088/2041-8205/768/2/l28 2013

  67. [67]

    Hung T., et al., 2020, @doi [ ] 10.3847/1538-4357/abb606 , https://ui.adsabs.harvard.edu/abs/2020ApJ...903...31H 903, 31

    work page doi:10.3847/1538-4357/abb606 2020

  68. [68]

    A., Arag \'o n-Calvo M

    Jaber M., Peper M., Hellwing W. A., Arag \'o n-Calvo M. A., Valenzuela O., 2024, @doi [ ] 10.1093/mnras/stad3347 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.4087J 527, 4087

    work page doi:10.1093/mnras/stad3347 2024

  69. [69]

    , keywords =

    Jarrett T. H., et al., 2011, @doi [ ] 10.1088/0004-637X/735/2/112 , https://ui.adsabs.harvard.edu/abs/2011ApJ...735..112J 735, 112

    work page doi:10.1088/0004-637x/735/2/112 2011

  70. [70]

    A., Heckman, T

    Jarvis M. J., McLure R. J., 2006, @doi [ ] 10.1111/j.1365-2966.2006.10295.x , http://adsabs.harvard.edu/abs/2006MNRAS.369..182J 369, 182

    work page doi:10.1111/j.1365-2966.2006.10295.x 2006

  71. [71]

    H., Naab T., Ostriker J

    Johansson P. H., Naab T., Ostriker J. P., 2012, @doi [ ] 10.1088/0004-637X/754/2/115 , https://ui.adsabs.harvard.edu/abs/2012ApJ...754..115J 754, 115

    work page doi:10.1088/0004-637x/754/2/115 2012

  72. [72]

    C ., Stalevski M., Shapovalova A

    Jovanovi \'c P., Popovi \'c L. C ., Stalevski M., Shapovalova A. I., 2010, @doi [ ] 10.1088/0004-637X/718/1/168 , https://ui.adsabs.harvard.edu/abs/2010ApJ...718..168J 718, 168

    work page doi:10.1088/0004-637x/718/1/168 2010

  73. [73]

    S., et al., 2014, @doi [Science] 10.1126/science.1253787 , https://ui.adsabs.harvard.edu/abs/2014Sci...345...64K 345, 64

    Kaastra J. S., et al., 2014, @doi [Science] 10.1126/science.1253787 , https://ui.adsabs.harvard.edu/abs/2014Sci...345...64K 345, 64

    work page doi:10.1126/science.1253787 2014

  74. [74]

    Kauffmann G., et al., 2003, @doi [ ] 10.1111/j.1365-2966.2003.07154.x , https://ui.adsabs.harvard.edu/abs/2003MNRAS.346.1055K 346, 1055

    work page doi:10.1111/j.1365-2966.2003.07154.x 2003

  75. [75]

    Kauffmann G., White S. D. M., Heckman T. M., M \'e nard B., Brinchmann J., Charlot S., Tremonti C., Brinkmann J., 2004, @doi [ ] 10.1111/j.1365-2966.2004.08117.x , https://ui.adsabs.harvard.edu/abs/2004MNRAS.353..713K 353, 713

    work page doi:10.1111/j.1365-2966.2004.08117.x 2004

  76. [76]

    Theoretical Modeling of Starburst Galaxies

    Kewley L. J., Dopita M. A., Sutherland R. S., Heisler C. A., Trevena J., 2001, @doi [ ] 10.1086/321545 , https://ui.adsabs.harvard.edu/abs/2001ApJ...556..121K 556, 121

    work page Pith review doi:10.1086/321545 2001

  77. [77]

    A., Heckman, T

    Kewley L. J., Groves B., Kauffmann G., Heckman T., 2006, @doi [ ] 10.1111/j.1365-2966.2006.10859.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.372..961K 372, 961

    work page doi:10.1111/j.1365-2966.2006.10859.x 2006

  78. [78]

    , keywords =

    Kochanek C. S., et al., 2017, @doi [ ] 10.1088/1538-3873/aa80d9 , https://ui.adsabs.harvard.edu/abs/2017PASP..129j4502K 129, 104502

    work page doi:10.1088/1538-3873/aa80d9 2017

  79. [79]

    SDSS-V: Pioneering Panoptic Spectroscopy

    Kollmeier J. A., et al., 2017, @doi [arXiv e-prints] 10.48550/arXiv.1711.03234 , https://ui.adsabs.harvard.edu/abs/2017arXiv171103234K p. arXiv:1711.03234

    work page Pith review doi:10.48550/arxiv.1711.03234 2017

  80. [80]

    Komossa S., 2015, @doi [Journal of High Energy Astrophysics] 10.1016/j.jheap.2015.04.006 , https://ui.adsabs.harvard.edu/abs/2015JHEAp...7..148K 7, 148

    work page doi:10.1016/j.jheap.2015.04.006 2015

Showing first 80 references.