A Mass Model for the Lensing Cluster SDSS J1004+4112: Constraints from the Third Time Delay

Forés-Toribio, Raquel; Muñoz, J. A.; Kochanek, C. S.; Mediavilla, E.

doi:10.3847/1538-4357/ac8c40

Cited by 14 publications

(6 citation statements)

References 40 publications

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“…The fraction of matter in compact objects is arbitrarily taken to be lower than usual because the system is lensed by a cluster: κ /κ = 3%. These values are from Guerras et al (2017) based on the model of Oguri (2010) and they are in agreement with more recent modeling by Forés-Toribio et al (2022). Since κ /κ is poorly known, we tested the robustness of the results using κ /κ = 1% and κ /κ = 7%, the latter value being more typical of the fraction of compact objects in lens galaxies (Mediavilla et al 2009).…”

Section: Methodology and Model Parameterssupporting

confidence: 81%

Microlensing of the broad emission line region in the lensed quasar J1004+4112

Hutsemékers

Sluse

Savić

et al. 2023

A&A

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J1004+4112 is a lensed quasar for which the first broad emission line profile deformations due to microlensing were identified. Detailed interpretations of these features have nevertheless remained controversial. Based on 15 spectra obtained from 2003 to 2018, in this work, we revisit the microlensing effect that distorts the C IV broad emission line profile in J1004+4112. We take advantage of recent measurements of the image macro-magnification ratios, along with the fact that at one epoch, image B was not microlensed, thus constituting a reference spectrum to unambiguously characterize the microlensing effect observed in image A. After disentangling the microlensing in images A and B, we show that the microlensing-induced line profile distortions in image A, although variable, are remarkably similar over a period of 15 years. We find they are characterized by a strong magnification of the blue part of the line profile, a strong demagnification of the red part of the line profile, and a small-to-negligible demagnification of the line core. We used the microlensing effect, characterized by either the full magnification profile of the C IV emission line or a set of four integrated indices, to constrain the broad emission-line region (BLR) size, geometry, and kinematics. For this purpose, we modeled the deformation of the emission lines considering three simple, representative BLR models: a Keplerian disk, an equatorial wind, and a biconical polar wind, with various inclinations with respect to the line of sight. We find that the observed magnification profile of the C IV emission line in J1004+4112 can be reproduced with the simple BLR models we considered, without the need for more complex BLR features. The magnification appears dominated by the position of the BLR with respect to the caustic network – and not by the velocity-dependent size of the BLR. The favored models for the C IV BLR are either the Keplerian disk or the equatorial wind, depending on the orientation of the BLR axis with respect to the caustic network. We also find that the polar wind model can be discarded. We measured the C IV BLR half-light radius as r1/2=2.8−1.7+2.0 light-days. This value is smaller than the BLR radius expected from the radius-luminosity relation derived from reverberation mapping, but it is still in reasonable agreement given the large uncertainties.

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Section: Methodology and Model Parameterssupporting

confidence: 81%

Microlensing of the broad emission line region in the lensed quasar J1004+4112

Hutsemékers

Sluse

Savić

et al. 2023

A&A

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“…The HST data and the lens model for SDSS J1004+4112 are shown in Figure 1. The redshifts of the arcs in our lens model are the same as those used by Forés-Toribio et al (2022). The strong lensing mass model parameters are reported in Table 3.…”

Section: Sdss J1004+4112mentioning

confidence: 99%

Hubble Constant Measurement from Three Large-separation Quasars Strongly Lensed by Galaxy Clusters

Napier,

Sharon,

Dahle

et al. 2023

ApJ

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Tension between cosmic microwave background–based and distance ladder–based determinations of the Hubble constant H 0 motivates the pursuit of independent methods that are not subject to the same systematic effects. A promising alternative, proposed by Refsdal in 1964, relies on the inverse scaling of H 0 with the delay between the arrival times of at least two images of a strongly lensed variable source such as a quasar. To date, Refsdal’s method has mostly been applied to quasars lensed by individual galaxies rather than by galaxy clusters. Using the three quasars strongly lensed by galaxy clusters (SDSS J1004+4112, SDSS J1029+2623, and SDSS J2222+2745) that have both multiband Hubble Space Telescope data and published time delay measurements, we derive H 0, accounting for the systematic and statistical sources of uncertainty. While a single time delay measurement does not yield a well-constrained H 0 value, analyzing the systems together tightens the constraint. Combining the six time delays measured in the three cluster-lensed quasars gives H 0 = 74.1 ± 8.0 km s−1 Mpc−1. To reach 1% uncertainty in H 0, we estimate that a sample size of order of 620 time delay measurements of similar quality as those from SDSS J1004+4112, SDSS J1029+2623, and SDSS J2222+2745 would be needed. Improving the lens modeling uncertainties by a factor of two and a half may reduce the needed sample size to 100 time delays, potentially reachable in the next decade.

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“…In the case of sources at different redshifts, different models tend to find similar mass profiles that are not biased, demonstrating that the degeneracy does not exist for multiple lensed sources (Meneghetti et al 2017). With regard to the measured time delays, as in the work of Forés-Toribio et al (2022), their formal errors (see Muñoz et al 2022) are enlarged by a factor of 5. We also remark that quasar image flux ratios at near-infrared and radio wavelengths (which are less sensitive to microlensing effects) are used to weight mass models.…”

Section: Introductionmentioning

confidence: 96%

“…Additionally, most lens mass models of SDSS J1004+4112 were performed using parametric techniques: Inada et al (2003), Oguri et al (2004), Fohlmeister et al (2007Fohlmeister et al ( , 2008, Oguri (2010), Forés-Toribio et al (2022), Napier et al (2023), Liu et al (2023). Some non-parametric models are also available (e.g., Williams & Saha 2004;Saha et al 2006;Liesenborgs et al 2009;Mohammed et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Parameter-free Hubble constant from the quadruply lensed quasar SDSS J1004+4112

Martínez-Arrizabalaga,

Diego,

Goicoechea

2024

A&A

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We present a free-form lens model for the multiply lensed quasar in the galaxy cluster SDSS J$1004+4112$. Our lens model draws minimal assumptions on the distribution of mass in the lens plane. We have paid particular attention to the model uncertainties on the predicted time delay originating from the particular configuration of model variables. Taking into account this uncertainty, we obtained a value of the Hubble constant of $H_0= 74^ parsec $, which is consistent with recent independent estimates. The predicted time delay between the central image E and image C (the first to arrive) is $ E-C 200$ days for the estimated Hubble constant. Future measurements of $ E-C $ will allow for a tighter constraint to be imposed on $H_0$ in this cluster-QSO system.

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A Mass Model for the Lensing Cluster SDSS J1004+4112: Constraints from the Third Time Delay

Cited by 14 publications

References 40 publications

Microlensing of the broad emission line region in the lensed quasar J1004+4112

Microlensing of the broad emission line region in the lensed quasar J1004+4112

Hubble Constant Measurement from Three Large-separation Quasars Strongly Lensed by Galaxy Clusters

Parameter-free Hubble constant from the quadruply lensed quasar SDSS J1004+4112

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