APM 08279+5255: Keck Near‐ and Mid‐Infrared High‐Resolution Imaging

Egami, Eiichi; Neugebauer, G.; Soifer, B. T.; Matthews, K.; Ressler, Michael E.; Becklin, E. E.; Murphy, Thomas W.; Dale, Daniel A.

doi:10.1086/308862

Cited by 67 publications

(132 citation statements)

References 30 publications

(66 reference statements)

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“…This low magnification favours the lens model by Riechers et al (2009) with respect to that by Egami et al (2000), although it is affected by large errors as a result of the uncertainty on the BLR-luminosity relation. The best estimate of the black hole mass (dot-dashed line) is indicated together with its confidence intervals at 68% probability (dotted lines).…”

Section: Estimate Of the Lens Magnificationmentioning

confidence: 77%

“…With our direct time lag measurement, we can invert the distance-luminosity relation for C IV of Kaspi et al (2007) to obtain an estimate of APM 08279+5255 lens magnification, which is so far uncertain between 100 (Egami et al 2000) and 4 (Riechers et al 2009), depending on the model of the lensing galaxy shape, size, and positioning. This provides an estimate of µ = 2.4 +5.8 −1.9 , which is consistent at 1σ level with the model of Riechers et al (2009) and disfavours the model of Egami et al (2000). 4.…”

Section: Discussionmentioning

confidence: 99%

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A multi-epoch spectroscopic study of the BAL quasar APM 08279+5255

Saturni

Trèvese

Vagnetti

et al. 2016

A&A

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Context. The study of high-redshift bright quasars is crucial to gather information about the history of galaxy assembly and evolution. Variability analyses can provide useful data on the physics of quasar processes and their relation with the host galaxy. Aims. In this study, we aim to measure the black hole mass of the bright lensed BAL QSO APM 08279+5255 at z = 3.911 through reverberation mapping, and to update and extend the monitoring of its C IV absorption line variability. Methods. We perform the first reverberation mapping of the Si IV and C IV emission lines for a high-luminosity quasar at high redshift with the use of 138 R-band photometric data and 30 spectra available over 16 years of observations. We also cross-correlate the C IV absorption equivalent width variations with the continuum light curve to estimate the recombination time lags of the various absorbers and infer the physical conditions of the ionised gas. Results. We find a reverberation-mapping time lag of ∼900 rest-frame days for both Si IV and C IV emission lines. This is consistent with an extension of the BLR size-to-luminosity relation for active galactic nuclei up to a luminosity of ∼10 48 erg s −1 , and implies a black hole mass of 10 10 M . Additionally, we measure a recombination time lag of ∼160 days in the rest frame for the C IV narrow absorption system, which implies an electron density of the absorbing gas of ∼2.5 × 10 4 cm −3 . Conclusions. The measured black hole mass of APM 08279+5255 indicates that the quasar resides in an under-massive host-galaxy bulge with M bulge ∼ 7.5M BH , and that the lens magnification is lower than ∼8. Finally, the inferred electron density of the narrow-line absorber implies a distance of the order of 10 kpc of the absorbing gas from the quasar, placing it within the host galaxy.

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Section: Estimate Of the Lens Magnificationmentioning

confidence: 77%

Section: Discussionmentioning

confidence: 99%

A multi-epoch spectroscopic study of the BAL quasar APM 08279+5255

Saturni

Trèvese

Vagnetti

et al. 2016

A&A

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“…Hubble Space Telescope (HST) and radio images have suggested that there is a long-sought "third component", which is expected in the case of axi-symmetric gravitational lensing fields . A lens model indicating a magnification of about 100 was derived by Egami et al (2000). Spectroscopic HST observations, at medium-high-resolution (λ/∆λ ∼ 4500) confirmed that the third component is in fact part of the lensed image (Lewis et al 2002).…”

Section: Spectroscopymentioning

confidence: 86%

A multi-epoch spectroscopic study of the BAL quasar APM 08279+5255

Trèvese

Saturni

Vagnetti

et al. 2013

A&A

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Context. Broad absorption lines indicate gas outflows with velocities from thousands of km s −1 to about 0.2 the speed of light, which may be present in all quasars and may play a major role in the evolution of the host galaxy. The variability of absorption patterns can provide information on changes in the density and velocity distributions of the absorbing gas and its ionisation status. Aims. We want to accurately follow the evolution in time of the luminosity and both the broad and narrow C IV absorption features of an individual object, the quasar APM 08279+5255, and analyse the correlations among these quantities. Methods. We have collected 23 photometrical and spectro-photometrical observations at the 1.82 m Telescope of the Asiago Observatory since 2003, plus 5 other spectra from the literature. We analysed the evolution in time of the equivalent width of the broad absorption feature and two narrow absorption systems, the correlation among them and with the R band magnitude. We performed a structure function analysis of the equivalent width variations. Results. We present an unprecedented monitoring of a broad absorption line quasar based on 28 epochs during 14 years. The shape of broad absorption feature shows relative stability, while its equivalent width slowly declines until it sharply increases during 2011. At the same time, the R magnitude stays almost constant until it sharply increases during 2011. The equivalent width of the narrow absorption redwards of the systemic redshift only shows a decline. Conclusions. The broad absorption behaviour suggests changes in the ionisation status as the main cause of variability. We show for the first time a correlation of this variability with the R band flux. The different behaviour of the narrow absorption system might be due to recombination time delay. The structure function of the absorption variability has a slope comparable with typical optical variability of quasars. This is consistent with variations of the 200 Å ionising flux originating in the inner part of the accretion disk.

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“…The high redshift of z = 3.9 would have made it the most luminous known object in the Universe were it not for the magnification of a gravitational lens (Egami et al 2000). The magnification at optical wavelengths can be as large as µ = 100; for CO emission it is much less, µ = 7 (Downes et al 1999, Lewis et al 2002.…”

Section: Apm 08279+5245mentioning

confidence: 99%

Molecular Gas at High Redshift

Solomon

Bout

2005

Annu. Rev. Astron. Astrophys.

854

1,013

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The Early Universe Molecular Emission Line Galaxies (EMGs) are a population of galaxies with only 36 examples that hold great promise for the study of galaxy formation and evolution at high redshift. The classification, luminosity of molecular line emission, molecular mass, far-infrared (FIR) luminosity, star formation efficiency, morphology, and dynamical mass of the currently known sample are presented and discussed. The star formation rates derived from the FIR luminosity range from about 300 to 5000 M⊙ year −1 and the molecular mass from 4 × 10 9 to 1 × 10 11 M⊙. At the lower end, these star formation rates, gas masses, and diameters are similar to those of local ultraluminous infrared galaxies, and represent starbursts in centrally concentrated disks, sometimes, but not always, associated with active galactic nuclei.

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APM 08279+5255: Keck Near‐ and Mid‐Infrared High‐Resolution Imaging

Cited by 67 publications

References 30 publications

A multi-epoch spectroscopic study of the BAL quasar APM 08279+5255

A multi-epoch spectroscopic study of the BAL quasar APM 08279+5255

A multi-epoch spectroscopic study of the BAL quasar APM 08279+5255

Molecular Gas at High Redshift

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