pith. machine review for the scientific record. sign in

arxiv: 2605.13514 · v1 · submitted 2026-05-13 · 🌌 astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

COOL-LAMPS IX: A Rare Duo of Quasars Each Lensed by a Single Massive Galaxy Cluster

Erik Solhaug , Michael D. Gladders , Andi M. Kisare , Simon D. Mork , Matthew B. Bayliss , Aidan P. Cloonan , H{\aa}kon Dahle , Isaiah R. Escapa
show 15 more authors
Michael K. Florian Gourav Khullar Guillaume Mahler Natalie Malagon Kate Napier Allison Noble Jane R. Rigby Riley Rosener T. Emil Rivera-Thorsen Keren Sharon Antony A. Stark Kabelo Tsiane Grace C. Wagner Brian Welch Yifan "Megan" Zhao
Authors on Pith no claims yet

Pith reviewed 2026-05-14 18:08 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords gravitational lensingquasarsgalaxy clusterswide-separation lensed quasarstime-delay cosmographyCOOL-LAMPS
0
0 comments X

The pith

One galaxy cluster lenses two background quasars, each into four images.

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

The paper reports the discovery of COOLJ1153+0755, a system in which a single galaxy cluster at redshift 0.43 gravitationally lenses two separate quasars at redshifts 1.52 and 1.94. Each quasar appears as four distinct images with maximum separations near 26 arcseconds. A lens model yields a projected cluster mass of roughly 3.3 times 10^14 solar masses within 500 kiloparsecs and predicts time delays of order 800 to 1200 days between the brightest images. This find increases the known wide-separation lensed quasar sample from seven to eight systems containing nine quasars total. The configuration supplies laboratories for measuring the Hubble constant via time-delay cosmography and for examining black-hole and galaxy co-evolution near the peak of cosmic star formation.

Core claim

COOLJ1153+0755 features two multiply-imaged quasars, a broad-line Type I at z=1.524 and a dust-obscured Type II at z=1.939, each split into four images by the same z=0.4301 cluster, with a simple lens model recovering a projected mass M(<500 kpc) ~ 3.3 x 10^14 solar masses and relative time delays of hundreds to over one thousand days.

What carries the argument

A simple lens model that recovers the cluster's projected mass and the relative time delays between images of each quasar from the observed image positions and redshifts.

If this is right

  • The known wide-separation lensed quasar sample grows from seven to eight systems containing nine quasars.
  • The system supplies two new laboratories for probing black hole-galaxy co-evolution at Cosmic Noon.
  • Relative time delays of hundreds to over a thousand days enable time-delay cosmography constraints on the Hubble constant.
  • The system was found without a morphological cut, showing that point-source selections miss such configurations.

Where Pith is reading between the lines

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

  • Future wide-field surveys may uncover additional dual-quasar systems by relaxing point-source morphology requirements.
  • The dense galaxy environment around the Type I quasar, including two other strongly lensed galaxies, offers a test bed for environmental influences on quasar activity.
  • Repeated imaging of the predicted time delays could independently verify the lens model and the cluster mass estimate.

Load-bearing premise

The images identified in imaging and confirmed by spectroscopy all belong to single background quasars at the quoted redshifts, and the lens model accurately recovers the cluster mass and time delays without major contamination or misidentification.

What would settle it

New spectroscopy or monitoring that shows the candidate images of either quasar have inconsistent redshifts or measured time delays that differ substantially from the model's predictions of 800 to 1200 days.

Figures

Figures reproduced from arXiv: 2605.13514 by Aidan P. Cloonan, Allison Noble, Andi M. Kisare, Antony A. Stark, Brian Welch, Erik Solhaug, Gourav Khullar, Grace C. Wagner, Guillaume Mahler, H{\aa}kon Dahle, Isaiah R. Escapa, Jane R. Rigby, Kabelo Tsiane, Kate Napier, Keren Sharon, Matthew B. Bayliss, Michael D. Gladders, Michael K. Florian, Natalie Malagon, Riley Rosener, Simon D. Mork, T. Emil Rivera-Thorsen, Yifan "Megan" Zhao.

Figure 1
Figure 1. Figure 1: Discovery imaging of COOL J1153+0755 from DECaLS (top) and unWISE (bottom). The 1′ × 1 ′ cutouts show DECaLS DR9 g, r, and z imaging (top) and unWISE W1 and W2 imaging (bottom), revealing infrared emission consistent with two candidate multiply-imaged quasars in COOL J1153+0755 (A and B), which motivated the deeper follow-up imaging shown in [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Deeper Magellan follow-up imaging and archival infrared Spitzer imaging reveal two lensed quasars, each with three images: COOL J1153A and COOL J1153B. Shown is a 1′ × 1 ′ multi-wavelength composite image using Magel￾lan LDSS3 and IMACS grz imaging (blue), FourStar JHKs imaging (green), and archival Spitzer/IRAC channels I1 and I2 (red). January 2023 and collected spectroscopic observations during April 20… view at source ↗
Figure 3
Figure 3. Figure 3: Surface brightness profile modeling of COOL J1153A (image A1) and COOL J1153B (image B3). For each system, we show the observed image, the best-fitting model, and the residual image in both the grz and JHKs bands. The RGB composites are constructed using g/J as blue, r/H as green, and z/Ks as red. White crosshairs in the leftmost panels mark the positions of COOL J1153A and COOL J1153B. The nearby objects,… view at source ↗
Figure 4
Figure 4. Figure 4: LDSS3 spectra of the three quasar images of COOL J1153A confirm identical redshifts and spectral features. The A1 and A3 spectra have been vertically offset for visual clarity. Major telluric line residuals are marked with ⊕. Mg ii], a line from the quasar broad-line region, experiences significant foreground absorption. We present a fit of the broad Mg ii] emission and foreground absorption in Appendix B,… view at source ↗
Figure 5
Figure 5. Figure 5: BPT diagram showing the positions of COOL J1153B (image B1) from (a) one Gaussian component for each line, and (b) one broad and narrow component for Hα with the other lines tied to the narrow component. We measure the line fluxes of [O iii] λ5007 and [N ii] λ6584 and relative to the Balmer emission lines Hα and Hβ. The multi￾colored distribution are galaxies from SDSS DR16 (Ahumada et al. 2020) with 0.02 … view at source ↗
Figure 6
Figure 6. Figure 6: The best-fit SEDs of COOL J1153A (left panel) and COOL J1153B (right panel) are consistent with Type I and Type II quasars, respectively. The SED components (stellar, dust, and AGN) are shown in different colored lines. For COOL J1153B the ALMA Band 6 detection is excluded from the primary fit, as it would require a steeper dust emission curve than the Rayleigh-Jeans law allows, possibly calling for a more… view at source ↗
Figure 8
Figure 8. Figure 8: Projected mass density, Σ, of our best-fit lens model in a 80′′ × 80′′ box centered on the BCG. We re￾port the integrated mass density of the lens within 200 kpc, M(< 200 kpc), and show the image locations with crosses for COOL J1153A and COOL J1153B to guide the eye. The lens model magnifications of the COOL J1153A quasar images are µA1 = 5.5 +1.5 −1.0 , µA2 = 5.4 +2.5 −1.6 , and µA3 = 8.4 +4.2 −2.2 . For… view at source ↗
Figure 10
Figure 10. Figure 10: Time delay surfaces relative to the leading im￾ages of the two quasars, ∆trel, A and ∆trel, B (see Eqns. 3 and 4), in COOL J1153+0755 from our best-fit lens model in units of days. Each set of contours corresponds to ∆trel for a source at source redshift zsource = 1.524 (COOL J1153A, ∆trel, A) and zsource = 1.939 (COOL J1153B, ∆trel, B). Ob￾served images of the quasars, appearing at critical points on the… view at source ↗
Figure 11
Figure 11. Figure 11: 1 ′×1 ′ images from HST/ACS (top left) and JWST/NIRCam (top right) centered on the BCG in COOL J1153+0755. Top left: The blue, green, and red channels correspond to the F475W, F606W, and F814W bands, respectively. Top right: The blue, green, and red channels correspond to the F115W, F150W, and F444W bands, respectively. Enlarged panels highlight selected regions of COOL J1153+0755: (1) northeastern image … view at source ↗
Figure 12
Figure 12. Figure 12: Progression of lens model by adding space-based model constraints, like improved centroid measurements of quasar images and nearby halo potentials. Here, we show an updated lens model based on improved constraints from the space-based data (blue and red) compared to the criti￾cal curves from [PITH_FULL_IMAGE:figures/full_fig_p019_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Nordic Optical Telescope/ALFOSC monitoring of the three brightest images of COOL J1153A (blue circles: A1; green: A2, offset by -0.7 mag for clarity; red: A3). As the monitoring continues, the time delay of the quasar images will become measurable. COOL J1153B lacks sufficient blue flux for monitoring in the g-band. So far, the COOL J1153A g-band light curves ( [PITH_FULL_IMAGE:figures/full_fig_p021_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: We report that COOL J1153+0755 is detected in archival ALMA data. Left: ALMA Band 7 shows > 4σ detections of COOL J1153A and COOL J1153B. Right: ALMA Band 6 shows a detection of COOL J1153B and a non-detection of COOL J1153A. An enlarged inset panel is provided to show the Band 6 flux near the brightest two images, B1 and B2. We perform a spatial coaddition of images B1, B2 and B3 and show this in the low… view at source ↗
Figure 15
Figure 15. Figure 15: Enlarged panels of [PITH_FULL_IMAGE:figures/full_fig_p027_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: LDSS3 spectrum of COOL J1153A centered on the Mg ii] λλ 2796, 2803 doublet. Multiple absorbers are seen along the line of sight. We fit a broad doublet Voigt profile at the redshift of the quasar and the line-of-sight absorbers as Gaussian profiles. Each component of Mg ii] doublets is shown in colored lines, making up the total model (dashed black line). The second absorber system seen in A1 and A3 is no… view at source ↗
Figure 17
Figure 17. Figure 17: FIRE spectrum of COOL J1153B at z = 1.939 (image B1) showing the Hα and [N ii] emission lines. We simulta￾neously fit Hα, [N ii] λλ6548,6583, and [O iii] λ5007 using two approaches: (a) single Gaussian profiles for each line with tied velocity widths, and (b) Hα modeled with one narrow and one broad component while other lines’ widths are tied to the narrow component. See [PITH_FULL_IMAGE:figures/full_fi… view at source ↗
Figure 18
Figure 18. Figure 18: FIRE spectrum (same as in [PITH_FULL_IMAGE:figures/full_fig_p031_18.png] view at source ↗
Figure 19
Figure 19. Figure 19: Corner plot of the ground-based lens model showing posterior distributions of nine of the parameters for the 2000 model samples derived from 10 Markov chains and 200 iterations. We indicate the best-fit model values (red) and median values (yellow) of the posterior distributions and the 1σ confidence interval thereof. The ground-based lens model includes 30 constraints and 29 free parameters and yields a … view at source ↗
read the original abstract

Wide-separation lensed quasars (WSLQs) are rare systems that arise from the chance alignment of two objects: a galaxy cluster and a background quasar. After two decades, only seven WSLQs have been found. Here, we report the discovery of COOLJ1153+0755 by the COOL-LAMPS collaboration in DECaLS imaging and its confirmation with follow-up observations with the Magellan Telescopes and the Nordic Optical Telescope. This system features two multiply-imaged quasars each lensed into four images by the same $z=0.4301$ cluster: a classic broad-line Type I quasar at $z=1.524$ (COOLJ1153A) and a dust-obscured Type II quasar at $z=1.939$ (COOLJ1153B), with maximum image separations of $25.''6$ and $26.''0$, respectively. We construct a lens model to estimate a projected cluster mass of $M(<500\,{\rm kpc})\sim3.3\times10^{14}{\rm M}_{\odot}$ and relative time delays between the three brightest images of each quasar of $\Delta t_{\rm \,A3,A1}\sim800$, $\Delta t_{\rm \,A2,A1}\sim1200$, $\Delta t_{\rm \,B1,B3}\sim800$, and $\Delta t_{\rm \,B2,B3}\sim1000$ days. COOLJ1153A resides in a dense environment with three nearby galaxies, two of which are also strongly lensed. We identify COOLJ1153+0755 without making a morphological cut in the DECaLS catalog; none of its multiple images are classified as point sources in those data, implying that morphology-based selection would miss such systems. COOLJ1153+0755 expands the WSLQ sample from 7 to 8 systems (9 individual quasars), adding two powerful laboratories for probing black hole-galaxy co-evolution at Cosmic Noon and for time-delay cosmography constraints on the Hubble constant, $H_0$.

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

1 major / 2 minor

Summary. The manuscript reports the discovery of COOLJ1153+0755, a wide-separation lensed quasar system in which a single z=0.4301 galaxy cluster lenses two background quasars into four images each: a broad-line Type I quasar (COOLJ1153A) at z=1.524 with maximum image separation 25.6 arcsec and a dust-obscured Type II quasar (COOLJ1153B) at z=1.939 with 26.0 arcsec separation. DECaLS imaging plus Magellan and NOT spectroscopy confirm the redshifts and image identifications; a simple lens model then yields a projected cluster mass M(<500 kpc) ~ 3.3e14 Msun and relative time delays of order 800-1200 days among the brightest images of each quasar. The system is presented as the eighth known WSLQ, notable for containing both Type I and Type II quasars and for residing in a dense environment with additional strongly lensed galaxies.

Significance. If the image identifications and lens model hold, the discovery expands the rare sample of wide-separation lensed quasars from seven to eight systems and supplies two new laboratories for black-hole/galaxy co-evolution studies at Cosmic Noon plus time-delay cosmography. The spectroscopic confirmation of both redshifts and the morphological independence of the selection (no point-source cut required) are clear strengths that strengthen the observational foundation.

major comments (1)
  1. [Lens modeling section] Lens modeling section (description of mass and time-delay estimates): the simple lens model used to derive M(<500 kpc) ~ 3.3e14 Msun and the quoted time delays (Δt_A3,A1 ~800 d, Δt_A2,A1 ~1200 d, Δt_B1,B3 ~800 d, Δt_B2,B3 ~1000 d) does not include the three nearby galaxies around COOLJ1153A (two of which are themselves strongly lensed) as perturbers. For 25-arcsec image splittings, these local mass components can change the potential and predicted delays by tens of percent; an explicit test of their inclusion or a quantified uncertainty budget on the time delays is required before the cosmography utility can be claimed.
minor comments (2)
  1. [Abstract] Abstract: the phrase 'none of its multiple images are classified as point sources' is slightly ambiguous; clarify whether this refers to the DECaLS catalog classification of the individual images or to the system as a whole.
  2. [System description] The text states that COOLJ1153A 'resides in a dense environment with three nearby galaxies, two of which are also strongly lensed,' but does not specify whether these galaxies were used in the lens model or only noted for context; a short sentence linking the two would improve clarity.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their positive summary and constructive comment. We address the major comment below and will revise the manuscript to strengthen the lens modeling discussion.

read point-by-point responses

  1. Referee: [Lens modeling section] Lens modeling section (description of mass and time-delay estimates): the simple lens model used to derive M(<500 kpc) ~ 3.3e14 Msun and the quoted time delays (Δt_A3,A1 ~800 d, Δt_A2,A1 ~1200 d, Δt_B1,B3 ~800 d, Δt_B2,B3 ~1000 d) does not include the three nearby galaxies around COOLJ1153A (two of which are themselves strongly lensed) as perturbers. For 25-arcsec image splittings, these local mass components can change the potential and predicted delays by tens of percent; an explicit test of their inclusion or a quantified uncertainty budget on the time delays is required before the cosmography utility can be claimed.

    Authors: We agree that the three nearby galaxies represent local perturbers whose inclusion could affect the predicted time delays at the tens-of-percent level, particularly given the large image separations. Our current model is a deliberately simple cluster-scale representation intended to provide initial mass and delay estimates, as stated in the manuscript. In the revised version we will add an explicit test that incorporates these galaxies (using their observed positions and photometric mass estimates) as additional components in the lens model. We will report the resulting shifts in the time delays and include a quantified uncertainty budget on the delays to better support the potential cosmography applications. revision: yes

Circularity Check

0 steps flagged

No significant circularity: purely observational discovery with standard lens modeling

full rationale

The paper reports an observational discovery of two lensed quasars via DECaLS imaging and spectroscopic confirmation, followed by a standard lens model that fits observed image positions to estimate cluster mass and time delays. No derivation step reduces to self-definition, fitted inputs renamed as predictions, or load-bearing self-citations. The lens model is a conventional parametric fit to data and does not claim to derive new results from prior self-citations in a circular manner. The central claims rest on direct observations and standard modeling techniques that remain independent of the fitted outputs.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The discovery rests on standard gravitational lensing assumptions and spectroscopic redshift confirmation; no new free parameters or invented entities are introduced beyond the lens-model fit itself.

free parameters (1)
  • projected cluster mass within 500 kpc
    Derived from the lens model fit to image positions and separations.
axioms (1)
  • domain assumption Standard thin-lens gravitational lensing formalism applies to the observed image configurations.
    Invoked when constructing the lens model to estimate mass and time delays.

pith-pipeline@v0.9.0 · 5828 in / 1341 out tokens · 46326 ms · 2026-05-14T18:08:20.840650+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

138 extracted references · 125 canonical work pages · 61 internal anchors

  1. [1]

    The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

    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 internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aabc4f

  2. [4]

    Quantifying the Observational Effort Required for the Radial Velocity Characterization of TESS Planets

    Quantifying the Observational Effort Required for the Radial Velocity Characterization of TESS Planets. , keywords =. 2018. doi:10.3847/1538-3881/aacea9 , archivePrefix =. 1807.01263 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aacea9 2018

  3. [5]

    X-ray Scattering Echoes and Ghost Halos from the Intergalactic Medium: Relation to the nature of AGN variability

    X-Ray Scattering Echoes and Ghost Halos from the Intergalactic Medium: Relation to the Nature of AGN Variability. , keywords =. 2015. doi:10.1088/0004-637X/805/1/23 , archivePrefix =. 1503.01475 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/805/1/23 2015

  4. [6]

    , keywords =

    The 2013 Release of Cloudy. , keywords =. 2013

    2013

  5. [7]

    1989", month =

    T _ E X and LAT _ E X Macro Definition Files for Astronomical Publications. , year = "1989", month = "Mar", pages =

    1989

  6. [8]

    LaTeX: A Document Preparation System. 1994

    1994

  7. [9]

    Quasi-periodic Fast Propagating Magnetoacoustic Waves during the Magnetic Reconnection Between Solar Coronal Loops

    Quasi-periodic Fast Propagating Magnetoacoustic Waves during the Magnetic Reconnection Between Solar Coronal Loops. , keywords =. 2018. doi:10.3847/2041-8213/aaf167 , archivePrefix =. 1811.08553 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aaf167 2018

  8. [10]

    Nominal values for selected solar and planetary quantities: IAU 2015 Resolution B3

    Nominal Values for Selected Solar and Planetary Quantities: IAU 2015 Resolution B3. , keywords =. 2016. doi:10.3847/0004-6256/152/2/41 , archivePrefix =. 1605.09788 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-6256/152/2/41 2015

  9. [11]

    Swift X-Ray Observations of Classical Novae. II. The Super Soft Source Sample. , keywords =. 2011. doi:10.1088/0067-0049/197/2/31 , archivePrefix =. 1110.6224 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/197/2/31 2011

  10. [12]

    Galaxy emission line classification using 3D line ratio diagrams

    Galaxy Emission Line Classification Using Three-dimensional Line Ratio Diagrams. , keywords =. 2014. doi:10.1088/0004-637X/793/2/127 , archivePrefix =. 1406.5186 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/793/2/127 2014

  11. [13]

    A Bayesian approach to strong lensing modelling of galaxy clusters

    A Bayesian approach to strong lensing modelling of galaxy clusters. New Journal of Physics , keywords =. doi:10.1088/1367-2630/9/12/447 , archivePrefix =. 0706.0048 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1367-2630/9/12/447

  12. [14]

    , keywords =

    Absorption by Highly Ionized Interstellar Gas Along Extragalactic and Galactic Sight Lines. , keywords =. doi:10.1086/118427 , adsurl =

    work page doi:10.1086/118427

  13. [15]

    A New Method For Galaxy Cluster Detection. I. The Algorithm. , keywords =. doi:10.1086/301557 , archivePrefix =. astro-ph/0004092 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/301557

  14. [16]

    CIGALE: a python Code Investigating GALaxy Emission

    CIGALE: a python Code Investigating GALaxy Emission. , keywords =. doi:10.1051/0004-6361/201834156 , archivePrefix =. 1811.03094 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201834156

  15. [17]

    Instrumentation in astronomy VI , year = 1986, editor =

    The IRAF Data Reduction and Analysis System. Instrumentation in astronomy VI , year = 1986, editor =. doi:10.1117/12.968154 , adsurl =

    work page doi:10.1117/12.968154 1986

  16. [18]

    Astronomical Data Analysis Software and Systems II , year = 1993, editor =

    IRAF in the Nineties. Astronomical Data Analysis Software and Systems II , year = 1993, editor =

    1993

  17. [19]

    and Kinney, Anne L

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/308692

  18. [20]

    A Two-Parameter Model for the Infrared/Submillimeter/Radio Spectral Energy Distributions of Galaxies and AGN

    A Two-parameter Model for the Infrared/Submillimeter/Radio Spectral Energy Distributions of Galaxies and Active Galactic Nuclei. , keywords =. doi:10.1088/0004-637X/784/1/83 , archivePrefix =. 1402.1495 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/784/1/83

  19. [21]

    , archivePrefix = "arXiv", eprint =

    3D radiative transfer modelling of the dusty tori around active galactic nuclei as a clumpy two-phase medium. , keywords =. doi:10.1111/j.1365-2966.2011.19775.x , archivePrefix =. 1109.1286 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.19775.x 2011

  20. [22]

    The dust covering factor in active galactic nuclei

    The dust covering factor in active galactic nuclei. , keywords =. doi:10.1093/mnras/stw444 , archivePrefix =. 1602.06954 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw444

  21. [23]

    Physics of the Interstellar and Intergalactic Medium

  22. [24]

    Merloni, S

    The host galaxies of active galactic nuclei. , keywords =. doi:10.1111/j.1365-2966.2003.07154.x , archivePrefix =. astro-ph/0304239 , primaryClass =

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

  23. [25]

    1981 , month = feb, journal =

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

    work page doi:10.1086/130766

  24. [26]

    Discovery of COOL J0335-1927, a Gravitationally Lensed Quasar at z = 3.27 with an Image Separation of 23.″3

    COOL-LAMPS. Discovery of COOL J0335-1927, a Gravitationally Lensed Quasar at z = 3.27 with an Image Separation of 23.″3. , keywords =. 2023a , month = sep, volume =. doi:10.3847/2041-8213/acf132 , archivePrefix =. 2305.14317 , primaryClass =

    work page doi:10.3847/2041-8213/acf132 1927

  25. [27]

    SDSS J1029+2623: A Gravitationally Lensed Quasar with an Image Separation of 22.5 Arcseconds

    SDSS J1029+2623: A Gravitationally Lensed Quasar with an Image Separation of 22.5''. , keywords =. doi:10.1086/510671 , archivePrefix =. astro-ph/0611275 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/510671

  26. [28]

    SDSSJ2222+2745 A Gravitationally Lensed Sextuple Quasar with Maximum Image Separation of 15.1" Discovered in the Sloan Giant Arcs Survey

    SDSS J2222+2745: A Gravitationally Lensed Sextuple Quasar with a Maximum Image Separation of 15.''1 Discovered in the Sloan Giant Arcs Survey. , keywords =. doi:10.1088/0004-637X/773/2/146 , archivePrefix =. 1211.1091 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/773/2/146

  27. [29]

    A Gravitationally Lensed Quasar with Quadruple Images Separated by 14.62 Arcseconds

    A gravitationally lensed quasar with quadruple images separated by 14.62arcseconds. , keywords =. doi:10.1038/nature02153 , archivePrefix =. astro-ph/0312427 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature02153

  28. [30]

    SDSS J0909$+$4449: A Large-separation Strongly Lensed Quasar at $z \sim 2.8$ with Three Images

    SDSS J0909+4449: A large-separation strongly lensed quasar at z 2.8 with three images. , keywords =. doi:10.1093/mnrasl/sly174 , archivePrefix =. 1809.07337 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/sly174

  29. [31]

    , keywords =

    Catalogues of active galactic nuclei from Gaia and unWISE data. , keywords =. doi:10.1093/mnras/stz2487 , archivePrefix =. 1909.02010 , primaryClass =

    work page doi:10.1093/mnras/stz2487 1909

  30. [32]

    COOL-LAMPS. III. Discovery of a 25.″9 Separation Quasar Lensed by a Merging Galaxy Cluster. , keywords =. doi:10.3847/1538-4357/acbe39 , archivePrefix =. 2209.03972 , primaryClass =

    work page doi:10.3847/1538-4357/acbe39

  31. [33]

    Overview of the DESI Legacy Imaging Surveys

    Overview of the DESI Legacy Imaging Surveys. , keywords =. doi:10.3847/1538-3881/ab089d , archivePrefix =. 1804.08657 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/ab089d

  32. [34]

    The Sloan Digital Sky Survey Quasar Lens Search. I. Candidate Selection Algorithm. , keywords =. doi:10.1086/506019 , archivePrefix =. astro-ph/0605571 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/506019

  33. [35]

    The Open Journal of Astrophysics , keywords =

    The Million Quasars (Milliquas) Catalogue, v8. The Open Journal of Astrophysics , keywords =. doi:10.21105/astro.2308.01505 , archivePrefix =. 2308.01505 , primaryClass =

    work page doi:10.21105/astro.2308.01505

  34. [36]

    , keywords =

    Nine lensed quasars and quasar pairs discovered through spatially extended variability in Pan-STARRS. , keywords =. doi:10.1051/0004-6361/202347598 , archivePrefix =. 2307.13729 , primaryClass =

    work page doi:10.1051/0004-6361/202347598

  35. [37]

    The STRong lensing Insights into the Dark Energy Survey (STRIDES) 2016 follow-up campaign. II. 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 internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2172 2016

  36. [38]

    150 new lenses, quasar pairs, and projected quasars

    Gravitationally lensed quasars in Gaia - IV. 150 new lenses, quasar pairs, and projected quasars. , keywords =. doi:10.1093/mnras/stac3721 , archivePrefix =. 2206.07714 , primaryClass =

    work page doi:10.1093/mnras/stac3721

  37. [39]

    Gravitationally lensed quasars in Gaia: III. 22 new lensed quasars from Gaia Data Release 2

    Gravitationally lensed quasars in Gaia - III. 22 new lensed quasars from Gaia data release 2. , keywords =. doi:10.1093/mnras/sty3366 , archivePrefix =. 1810.04480 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty3366

  38. [40]

    Euclid preparation. I. The Euclid Wide Survey. , keywords =. doi:10.1051/0004-6361/202141938 , archivePrefix =. 2108.01201 , primaryClass =

    work page doi:10.1051/0004-6361/202141938

  39. [41]

    , keywords =

    What does strong gravitational lensing? The mass and redshift distribution of high-magnification lenses. , keywords =. doi:10.1093/mnras/staa1429 , archivePrefix =. 2002.01479 , primaryClass =

    work page doi:10.1093/mnras/staa1429 2002

  40. [42]

    The Open Journal of Astrophysics , keywords =

    A halo model approach for mock catalogs of time-variable strong gravitational lenses. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.128482 , archivePrefix =. 2411.07509 , primaryClass =

    work page doi:10.33232/001c.128482

  41. [43]

    , keywords =

    Probing coherence in metal absorption towards multiple images of strong gravitationally lensed quasars. , keywords =. doi:10.1093/mnras/stae048 , archivePrefix =. 2401.03024 , primaryClass =

    work page doi:10.1093/mnras/stae048

  42. [44]

    , keywords =

    Absorption-based circumgalactic medium line emission estimates. , keywords =. doi:10.1093/mnras/stac2390 , archivePrefix =. 2202.11121 , primaryClass =

    work page doi:10.1093/mnras/stac2390

  43. [45]

    , year = 1964, month = jan, volume =

    On the possibility of determining Hubble's parameter and the masses of galaxies from the gravitational lens effect. , year = 1964, month = jan, volume =. doi:10.1093/mnras/128.4.307 , adsurl =

    work page doi:10.1093/mnras/128.4.307 1964

  44. [46]

    , keywords =

    Hubble Constant Measurement from Three Large-separation Quasars Strongly Lensed by Galaxy Clusters. , keywords =. 2023b , month = dec, volume =. doi:10.3847/1538-4357/ad045a , archivePrefix =. 2301.11240 , primaryClass =

    work page doi:10.3847/1538-4357/ad045a

  45. [47]

    A 2.4 per cent measurement of H _ 0 from lensed quasars: 5.3 tension between early- and late-Universe probes

    H0LiCOW - XIII. A 2.4 per cent measurement of H _ 0 from lensed quasars: 5.3 tension between early- and late-Universe probes. , keywords =. doi:10.1093/mnras/stz3094 , archivePrefix =. 1907.04869 , primaryClass =

    work page doi:10.1093/mnras/stz3094 1907

  46. [48]

    COOL-LAMPS. VIII. Known Wide-separation Lensed Quasars and Their Host Galaxies Reveal a Lack of Evolution in M _ BH /M _ Since z 3. , keywords =. doi:10.3847/1538-4357/addabf , archivePrefix =. 2408.03379 , primaryClass =

    work page doi:10.3847/1538-4357/addabf

  47. [49]

    The UV--mid-IR Spectral Energy Distribution of a z=1.7 Quasar Host Galaxy

    The UV-Mid-IR Spectral Energy Distribution of a z = 1.7 Quasar Host Galaxy. , keywords =. doi:10.1088/0004-637X/702/1/472 , archivePrefix =. 0904.1708 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/702/1/472

  48. [50]

    , keywords =

    The Black Hole Mass of the z = 2.805 Multiply Imaged Quasar SDSS J2222+2745 from Velocity-resolved Time Lags of the C IV Emission Line. , keywords =. doi:10.3847/1538-4357/abe943 , archivePrefix =. 2011.02007 , primaryClass =

    work page doi:10.3847/1538-4357/abe943 2011

  49. [51]

    , keywords =

    Dynamical Modeling of the C IV Broad Line Region of the z = 2.805 Multiply Imaged Quasar SDSS J2222+2745. , keywords =. doi:10.3847/2041-8213/ac081b , archivePrefix =. 2103.10961 , primaryClass =

    work page doi:10.3847/2041-8213/ac081b 2041

  50. [52]

    Spatially Resolved Patchy Lyman-$\alpha$ Emission Within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8

    Spatially Resolved Patchy Ly Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8. , keywords =. doi:10.3847/2041-8213/aa831a , archivePrefix =. 1708.00453 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aa831a 2041

  51. [53]

    , keywords =

    SExtractor: Software for source extraction. , keywords =. doi:10.1051/aas:1996164 , adsurl =

    work page doi:10.1051/aas:1996164

  52. [54]

    R., Millman, K

    Harris, Charles R. and Millman, K. Jarrod and van der Walt, St. Array programming with NumPy , url =. Nature , number =. 2020 , bdsk-url-1 =. doi:10.1038/s41586-020-2649-2 , id =

    work page doi:10.1038/s41586-020-2649-2 2020

  53. [55]

    Matplotlib: A 2D graphics environment

    Matplotlib: A 2D Graphics Environment. Computing in Science and Engineering , keywords =. doi:10.1109/MCSE.2007.55 , adsurl =

    work page doi:10.1109/mcse.2007.55 2007

  54. [56]

    E., et al

    SciPy 1.0: fundamental algorithms for scientific computing in Python. Nature Methods , keywords =. doi:10.1038/s41592-019-0686-2 , archivePrefix =. 1907.10121 , primaryClass =

    work page doi:10.1038/s41592-019-0686-2 1907

  55. [57]

    Astropy: A Community Python Package for Astronomy

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322068

  56. [58]

    SAOImage DS9: A utility for displaying astronomical images in the X11 window environment

  57. [59]

    The Sloan Digital Sky Survey: Technical Summary

    The Sloan Digital Sky Survey: Technical Summary. , keywords =. doi:10.1086/301513 , archivePrefix =. astro-ph/0006396 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/301513

  58. [60]

    Sloan Digital Sky Survey IV: Mapping the Milky Way, Nearby Galaxies, and the Distant Universe

    Sloan Digital Sky Survey IV: Mapping the Milky Way, Nearby Galaxies, and the Distant Universe. , keywords =. doi:10.3847/1538-3881/aa7567 , archivePrefix =. 1703.00052 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aa7567

  59. [61]

    The MOSDEF Survey: Electron Density and Ionization Parameter at $z\sim2.3$

    The MOSDEF Survey: Electron Density and Ionization Parameter at z -0.5ex 2.3. , keywords =. doi:10.3847/0004-637X/816/1/23 , archivePrefix =. 1509.03636 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/816/1/23

  60. [62]

    Lectures on Gravitational Lensing

    Lectures on Gravitational Lensing. arXiv e-prints , keywords =. doi:10.48550/arXiv.astro-ph/9606001 , archivePrefix =. astro-ph/9606001 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9606001

  61. [63]

    , keywords =

    A new formulation of gravitational lens theory, time-delay, and Fermat's principle. , keywords =

  62. [64]

    Ivezi ´c, S

    LSST: From Science Drivers to Reference Design and Anticipated Data Products. , keywords =. doi:10.3847/1538-4357/ab042c , archivePrefix =. 0805.2366 , primaryClass =

    work page doi:10.3847/1538-4357/ab042c

  63. [65]

    arXiv e-prints , keywords =

    PypeIt: The Python Spectroscopic Data Reduction Pipeline. arXiv e-prints , keywords =. 2020a , month = may, eid =

  64. [66]

    2020, The Journal of Open Source Software, 5, 2308, doi: 10.21105/joss.02308

    J. Xavier Prochaska and Joseph F. Hennawi and Kyle B. Westfall and Ryan J. Cooke and Feige Wang and Tiffany Hsyu and Frederick B. Davies and Emanuele Paolo Farina and Debora Pelliccia , title =. 2020b , publisher =. doi:10.21105/joss.02308 , url =

    work page doi:10.21105/joss.02308

  65. [67]

    2020c , month = apr, eid =

    pypeit/PypeIt: Release 1.0.0. 2020c , month = apr, eid =. doi:10.5281/zenodo.3743493 , version =

    work page doi:10.5281/zenodo.3743493

  66. [68]

    , keywords =

    Spectral Classification of Emission-Line Galaxies. , keywords =. doi:10.1086/191166 , adsurl =

    work page doi:10.1086/191166

  67. [69]

    Pseudo Elliptical Lensing Mass Model: Application to the NFW Mass Distribution

    Pseudo elliptical lensing mass model: Application to the NFW mass distribution. , keywords =. doi:10.1051/0004-6361:20020639 , archivePrefix =. astro-ph/0112138 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20020639

  68. [70]

    PySpecKit: Python Spectroscopic Toolkit

  69. [71]

    , keywords =

    Pyspeckit: A Spectroscopic Analysis and Plotting Package. , keywords =. doi:10.3847/1538-3881/ac695a , archivePrefix =. 2205.04987 , primaryClass =

    work page doi:10.3847/1538-3881/ac695a

  70. [72]

    , keywords =

    ALMA 1.3 mm Survey of Lensed Submillimeter Galaxies Selected by Herschel: Discovery of Spatially Extended SMGs and Implications. , keywords =. doi:10.3847/1538-4357/abd6e4 , archivePrefix =. 2101.03677 , primaryClass =

    work page doi:10.3847/1538-4357/abd6e4

  71. [73]

    , year = 2011, month = mar, volume =

    IMACS: The Inamori-Magellan Areal Camera and Spectrograph on Magellan-Baade. , year = 2011, month = mar, volume =. doi:10.1086/658908 , adsurl =

    work page doi:10.1086/658908 2011

  72. [74]

    Computing in Science and Engineering , keywords =

    Jupyter-Enabled Astrophysical Analysis Using Data-Proximate Computing Platforms. Computing in Science and Engineering , keywords =. doi:10.1109/MCSE.2021.3057097 , archivePrefix =. 2104.06527 , primaryClass =

    work page doi:10.1109/mcse.2021.3057097 2021

  73. [75]

    Ram Pressure Stripping of Disc Galaxies: The Role of the Inclination Angle , shorttitle =

    The host galaxies and classification of active galactic nuclei. , keywords =. doi:10.1111/j.1365-2966.2006.10859.x , archivePrefix =. astro-ph/0605681 , primaryClass =

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

  74. [76]

    and Nicholls, David C

    Understanding Galaxy Evolution Through Emission Lines. , keywords =. doi:10.1146/annurev-astro-081817-051832 , archivePrefix =. 1910.09730 , primaryClass =

    work page doi:10.1146/annurev-astro-081817-051832 1910

  75. [77]

    R., Knigge, C., Drew, J

    Observational evidence for AGN feedback in early-type galaxies. , keywords =. doi:10.1111/j.1365-2966.2007.12487.x , archivePrefix =. 0709.3015 , primaryClass =

    work page doi:10.1111/j.1365-2966.2007.12487.x 2007

  76. [78]

    J., Dopita, M

    Theoretical Modeling of Starburst Galaxies. , keywords =. doi:10.1086/321545 , archivePrefix =. astro-ph/0106324 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/321545

  77. [79]

    The Gaia mission

    The Gaia mission. , keywords =. doi:10.1051/0004-6361/201629272 , archivePrefix =. 1609.04153 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629272

  78. [80]

    2023 , month = jun, journal =

    Gaia Data Release 3. Summary of the content and survey properties. , keywords =. doi:10.1051/0004-6361/202243940 , archivePrefix =. 2208.00211 , primaryClass =

    work page doi:10.1051/0004-6361/202243940

  79. [81]

    , keywords =

    The Two Micron All Sky Survey (2MASS). , keywords =. doi:10.1086/498708 , adsurl =

    work page doi:10.1086/498708

  80. [82]

    , year = 2013, month = jun, volume =

    FourStar: The Near-Infrared Imager for the 6.5 m Baade Telescope at Las Campanas Observatory. , year = 2013, month = jun, volume =. doi:10.1086/671164 , adsurl =

    work page doi:10.1086/671164 2013

Showing first 80 references.