Cosmic Alignment toward the Radio Einstein Ring PKS 1830−211?

Courbin, F.; Meylan, G.; Kneib, Jean-Paul; Lidman, C.

doi:10.1086/341261

Cited by 47 publications

(105 citation statements)

References 24 publications

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“…PKS 1830-211 is composed of a background continuum source at redshift z = 2.507, possibly a blazar, and a lensing face-on spiral galaxy at z = 0.88582 along its line-of-sight (Wiklind & Combes 1996b;Lidman et al 1999;Courbin et al 2002; Winn et al 2002;de Rosa et al 2005). The lens splits the background continuum into three main components, two compact hotspots, a north-western and a south-eastern one separated by ∼1 , and an Einstein ring, which is prominent at low ( 10 GHz) frequencies.…”

Section: Resultsmentioning

confidence: 99%

The density, the cosmic microwave background, and the proton-to-electron mass ratio in a cloud at redshift 0.9

Henkel¹,

Menten²,

Murphy

et al. 2009

A&A

151

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Based on measurements with the Effelsberg 100-m telescope, a multi-line study of molecular species is presented toward the gravitational lens system PKS 1830-211, which is by far the best known target to study dense cool gas in absorption at intermediate redshift.Determining average radial velocities and performing Large Velocity Gradient radiative transfer calculations, the aims of this study are (1) to determine the density of the gas, (2) to constrain the temperature of the cosmic microwave background (CMB), and (3) to evaluate the proton-to-electron mass ratio at redshift z ∼ 0.89. Analyzing data from six rotational HC 3 N transitions (this includes the J = 7 ← 6 line, which is likely detected for the first time in the interstellar medium) we obtain n(H 2 ) ∼ 2600 cm −3 for the gas density of the south-western absorption component, assuming a background source covering factor, which is independent of frequency. With a possibly more realistic frequency dependence proportional to ν 0.5 (the maximal exponent permitted by observational boundary conditions), n(H 2 ) ∼ 1700 cm −3 . Again toward the south-western source, excitation temperatures of molecular species with optically thin lines and higher rotational constants are, on average, consistent with the expected temperature of the cosmic microwave background, T CMB = 5.14 K. However, individually, there is a surprisingly large scatter which far surpasses expected uncertainties. A comparison of CS J = 1 ← 0 and 4 ← 3 optical depths toward the weaker north-western absorption component results in T ex = 11 K and a 1-σ error of 3 K. For the main component, a comparison of velocities determined from ten optically thin NH 3 inversion lines with those from five optically thin rotational transitions of HC 3 N, observed at similar frequencies, constrains potential variations of the proton-to-electron mass ratio μ to Δμ/μ < 1.4 × 10 −6 with 3-σ confidence. Also including optically thin rotational lines from other molecular species, it is emphasized that systematic errors are ΔV < 1 km s −1 , corresponding to Δμ/μ < 1.0 × 10 −6 .

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Section: Resultsmentioning

confidence: 99%

The density, the cosmic microwave background, and the proton-to-electron mass ratio in a cloud at redshift 0.9

Henkel¹,

Menten²,

Murphy

et al. 2009

A&A

151

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“…The ratio of amplification factors at energies below and above 4.3 keV is estimated to be about 0.8. This value appears to be too low, as it is expected that the amplification factor should increase with energy and, so far, the available modeling of the magnification factor from radio/ optical observations has yielded values in the range 2-4 ( Nair et al 1993;Swift et al 2001;Courbin et al 2002).…”

Section: Discussion and Summarymentioning

confidence: 97%

High‐Energy Properties of PKS 1830−211

Zhang¹,

Chen²,

Collmar³

et al. 2008

Astrophysical Journal

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We report an analysis of X-ray and -ray observations of PKS 1830À211, based on long-term campaigns carried out by INTEGRAL and COMPTEL. The INTEGRAL data currently available provide a 33 significance detection in the 20-100 keV band, while the COMPTEL 6 yr data provide a 5.2 significance detection in the 1-3 MeVenergy band. In hard X-rays, INTEGRAL and supplementary Swift observations show flux variability on timescales of months. In -rays, the source shows persistent emission over years. The hard X-ray spectrum is well represented by a power-law model, with À $ 1.3 in the 20-250 keV band. This photon index is consistent with a previous report of À $ 1.3 obtained at E > 3.5 keV from XMM-Newton data fitted with a broken power law model. The joint XMM-Newton and INTEGRAL spectrum presented here is thus fitted with a broken power law model; the parameters are refined as compared with the previous fit. The results show that the photon index changes from $1.0 to $1.3 at a break energy of $4 keV. At MeV energies, the spectrum softens to À $ 2.2. These results, together with an EGRET measurement at E ! 100 MeV, constitute a broadband spectrum containing the peak of the power output at MeV energies, similar to most high-luminosity -ray blazars. The measured spectral characteristics are discussed in the framework of gravitational lensing effects.

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“…Ledoux et al (1998), Auger et al (2008) and Sluse et al (2008) used AO to study galaxy scale two-image lensed quasars (doubles). Rusin et al (2000); Courbin et al (2002); Meylan et al (2005) discovered additional lensing galaxies in known lensed quasars, using AO. Faure et al (2011) observed a quad in order to look for substructure, which McKean et al (2007) was successful in detecting for another quad.…”

Section: Introductionmentioning

confidence: 99%

Subaru Telescope adaptive optics observations of gravitationally lensed quasars in the Sloan Digital Sky Survey

Rusu

Oguri

Minowa

et al. 2016

Mon. Not. R. Astron. Soc.

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We present the results of an imaging observation campaign conducted with the Subaru Telescope adaptive optics system (IRCS+AO188) on 28 gravitationally lensed quasars and candidates (23 doubles, 1 quad, 1 possible triple and 3 candidates) from the SDSS Quasar Lens Search. We develop a novel modelling technique that fits analytical and hybrid point spread functions (PSFs), while simultaneously measuring the relative astrometry, photometry, as well as the lens galaxy morphology. We account for systematics by simulating the observed systems using separately observed PSF stars. The measured relative astrometry is comparable with that typically achieved with the Hubble Space Telescope, even after marginalizing over the PSF uncertainty. We model for the first time the quasar host galaxies in 5 systems, without a-priory knowledge of the PSF, and show that their luminosities follow the known correlation with the mass of the supermassive black hole. For each system, we obtain mass models far more accurate than those previously published from low-resolution data, and we show that in our sample of lensing galaxies the observed light profile is more elliptical than the mass, for ellipticity 0.25. We also identify eight doubles for which the sources of external and internal shear are more reliably separated, and should therefore be prioritized in monitoring campaigns aimed at measuring time-delays in order to infer the Hubble constant.

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Cosmic Alignment toward the Radio Einstein Ring PKS 1830−211?

Cited by 47 publications

References 24 publications

The density, the cosmic microwave background, and the proton-to-electron mass ratio in a cloud at redshift 0.9

The density, the cosmic microwave background, and the proton-to-electron mass ratio in a cloud at redshift 0.9

High‐Energy Properties of PKS 1830−211

Subaru Telescope adaptive optics observations of gravitationally lensed quasars in the Sloan Digital Sky Survey

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