CLASS B1152+199 and B1359+154: Two New Gravitational Lens Systems Discovered in the Cosmic Lens All-Sky Survey

Myers, S. T.; Rusin, D.; Fassnacht, C. D.; Blandford, R. D.; Pearson, T. J.; Readhead, A. C. S.; Jackson, N.; Browne, I. W. A.; Marlow,; Wilkinson, P. N.; Koopmans, L. V. E.; Bruyn, de Antonius

doi:10.1086/300875

Cited by 61 publications

(49 citation statements)

References 13 publications

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“…When computing ORM sample I, we used the numbers from ORM table A1 (calculating the critical radius, r , as half of the separation). List of references: 1, Wisotzki et al (2004); 2, Ofek et al (2006); 3, Rusin et al (2003); 4, Morgan et al (1999); 5, Wisotzki et al (2002); 6, Hagen and Reimers (2000); 7, Johnston et al (2003); 8, Kneib, Cohen and Hjorth (2000); 9, Kochanek et al (2000); 10, Lubin et al (2000); 11, Eigenbrod et al (2006a);12, Schechter et al (1998); 13, Lehár et al (2000); 14, Lacy et al (2002);15, Hewett et al (1994); 16, Surdej et al (1997); 17, Eisenhardt et al (1996); 18, Lidman et al (2000); 19, Weymann et al (1980);20, Tonry (1998); 21, Sluse et al (2003); 22, ; 23, Eigenbrod et al (2006b); 24, Burud et al (2002a); 25, Wisotzki et al (1996); 26, Burud et al (2002b); 27, Cohen, Lawrence and Blandford (2003); 28, Wiklind and Combes (1995); 29, Lawrence et al (1995); 30, Tonry and Kochanek (1999); 31, Fassnacht and Cohen (1998); 32, Myers et al (1999); 33, Patnaik et al (1992); 34, Lehár et al (1993);35, Treu and Koopmans (2003); 36, Winn et al (2002); 37, Langston et al (1989); 38, …”

Section: Conclusion and Discussionmentioning

confidence: 99%

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How robust are the constraints on cosmology and galaxy evolution from the lens-redshift test?

Capelo

Natarajan

2007

New J. Phys.

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The redshift distribution of galaxy lenses in known gravitational lens systems provides a powerful test that can potentially discriminate amongst cosmological models. However, applications of this elegant test have been curtailed by two factors: our ignorance of how galaxies evolve with redshift, and the absence of methods to deal with the effect of incomplete information in lensing systems. In this paper, we investigate both issues in detail. We explore how to extract the properties of evolving galaxies, assuming that the cosmology is well determined by other techniques. We propose a new nested Monte Carlo method to quantify the effects of incomplete data. We apply the lens-redshift test to an improved sample of seventy lens systems derived from recent observations, primarily from the SDSS, SLACS and the CLASS surveys. We find that the limiting factor in applying the lens-redshift test derives from poor statistics, including incomplete information samples, and biased sampling. Many lenses that uniformly sample the underlying true image separation distribution will be needed to use this test as a complementary method to measure the value of the cosmological constant or the properties of evolving galaxies. Planned future surveys by missions like the SNAP satellite or LSST are likely to usher in a new era for strong lensing studies that utilize this test. With expected catalogues of thousands of new strong lenses, the lens-redshift test could offer a powerful tool to probe cosmology as well as galaxy evolution.

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Section: Conclusion and Discussionmentioning

confidence: 99%

“…These include systems with multiple lensing galaxies of comparable luminosities (and therefore likely comparable halo masses) such as HE0230−2130 (Wisotzki et al 1998), B1359+154 (Myers et al 1999) and B2114+022 (Augusto et al 2001). We also exclude cluster-assisted systems such as Q0957+561 (Young et al 1980).…”

Section: Defining the New Lens Galaxy Samplementioning

confidence: 99%

How robust are the constraints on cosmology and galaxy evolution from the lens-redshift test?

Capelo

Natarajan

2007

New J. Phys.

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“…The emission is partially resolved for both the CO and continuum maps; the continuum clearly shows three peaks of emission. Because ofthe complicated lensing configuration that creates six images of B1359+154 (e.g., Myers et al 1999), it is difficult to associate the 130 GHz peaks with individual images, but the three peaks roughly correspond to images A, B/C, and D/E/F and have the appropriate relative brightnesses.…”

Section: B1359+154mentioning

confidence: 99%

A Total Molecular Gas Mass Census in Z ∼ 2–3 Star-Forming Galaxies: Low-J Co Excitation Probes of Galaxies’ Evolutionary States

Sharon

Riechers

Hodge

et al. 2016

ApJ

133

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We present CO(1-0) observations obtained at the Karl G. Jansky Very Large Array for 14z 2 galaxies with existing CO(3-2) measurements, including 11 galaxies thatcontain active galactic nuclei (AGNs) and three submillimeter galaxies (SMGs). We combine this sample with an additional 15z 2 galaxies from the literature that have both CO(1-0) and CO(3-2) measurements in order to evaluate differences in CO excitation between SMGs and AGN host galaxies, tomeasure the effects of CO excitation on the derived molecular gas properties of these populations, and to look for correlations between the molecular gas excitation and other physical parameters. With our expanded sample of CO(3-2)/CO(1-0) line ratio measurements, we do not find a statistically significant difference in the mean line ratio between SMGs and AGN host galaxies as can be found in the literature; we instead find =  r 1.03 0. for both populations combined). We also do not measure a statistically significant difference between the distributions of the line ratios for these populations at the p=0.05 level, although this result is less robust. We find no excitation dependence on the index or offset of the integrated Schmidt-Kennicutt relation for the two CO lines, and weobtain indices consistent with N=1 for the various subpopulations. However, including low-z "normal" galaxies increases our best-fit Schmidt-Kennicutt index toÑ 1.2. While we do not reproduce correlations between the CO line width and luminosity, we do reproduce correlations between CO excitation and star-formation efficiency.

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“…The lensed quasar B 1359+154 was discovered as part of the CLASS survey and discussed by Myers et al (1999). The quasar is at redshift z = 3.24 and has a maximum image separation of 1.7 .…”

Section: The Multiple Quasar B 1359+154mentioning

confidence: 99%

Integral field spectroscopy of four lensed quasars: analysis of their neighborhood and evidence for microlensing

Anguita¹,

Fauré²,

Yonehara³

et al. 2008

A&A

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Context. Gravitationally lensed quasars constitute an independent tool to derive the Hubble constant through the time-delays of their different images; they offer as well the opportunity to study the mass distribution and interstellar medium of their lensing galaxies and, through microlensing due to stars in their lensing galaxy, they also allow one to study details of the emitting source. Aims. For such studies, one needs to have an excellent knowledge of the close environment of the lensed images in order to model the lensing potential: this means, ideally, observational data over a large field-of-view and spectroscopy at high spatial resolution. Methods. We present VIMOS integral field observations of 27 × 27 fields of view around four lensed quasars: HE 0230-2130, RX J0911.4 + 0551, H 1413 + 117 and B 1359 + 154. Using the low, medium and high resolution modes, we study the quasar images and the quasar environments. Because of the complexity of the reduction of integral field datasets, we provide a detailed report of the data reduction. Results. Comparison between the quasar spectra of the different images reveals differences for HE 0230-2130, RX J0911.4 + 0551 and H 1413+117: flux ratios between the images of the same quasar are different when measured in the emission lines and in the continuum. We have also measured the redshifts of galaxies in the neighborhood of HE 0230-2130 and RX J0911.4 + 0551 which possibly contribute to the total lensing potential, given their close proximity to the line-of-sight toward the quasars. Conclusions. A careful analysis reveals that microlensing is the most natural explanation for the (de)magnification of the continuum emitting region of the background sources. In HE 0230-2130, image D is likely to be affected by microlensing magnification; in RX J0911.4+0551, images A1 and A3 are likely to be modified by microlensing de-magnification and in H 1413+117 at least image D is affected by microlensing. We have not been able to recover any microlensing information or galaxies close to the line-of-sight in the neighborhood of B 1359+154.

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CLASS B1152+199 and B1359+154: Two New Gravitational Lens Systems Discovered in the Cosmic Lens All-Sky Survey

Cited by 61 publications

References 13 publications

How robust are the constraints on cosmology and galaxy evolution from the lens-redshift test?

How robust are the constraints on cosmology and galaxy evolution from the lens-redshift test?

A Total Molecular Gas Mass Census in Z ∼ 2–3 Star-Forming Galaxies: Low-J Co Excitation Probes of Galaxies’ Evolutionary States

Integral field spectroscopy of four lensed quasars: analysis of their neighborhood and evidence for microlensing

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