The gravitationally lensed, luminous infrared galaxy IRAS F10214+4724 observed with XMM-Newton

Iwasawa, K.; Vignali, C.; Evans, A. S.; Sanders, D. B.; Trentham, Neil

doi:10.1016/j.newast.2009.05.009

Cited by 2 publications

(2 citation statements)

References 26 publications

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“…Spectro-polarimetry revealed the rest-frame ultraviolet to be ∼28 percent polarised, as well as the presence of broad ultraviolet lines (Goodrich et al 1996), providing strong evidence that this was the reflected light (presumably off dust clouds associated with the narrow-line region) from an obscured AGN. The source model of IRAS 10214 could now conclusively include an active nucleus, however X-ray observations with both the Chandra (Alexander et al 2005) and XMM-Newton (Iwasawa et al 2010) space telescopes made low S/N detections, seemingly inconsistent with the powerful AGN suggested by the luminous [O iii]λ5007Å line emission strength (L OIII ∼ 10 37 W, Serjeant et al 1998). This lead to the suggestion that this is a Compton thick object (i.e.…”

Section: Introductionmentioning

confidence: 99%

“…This function is as yet undetermined and hence included in the ordinate label. The flux densities used in this plot are sourced fromRowan-Robinson et al (1991);Downes et al (1992);Rowan-Robinson et al (1993);Lawrence et al (1993);Barvainis et al (1995);Benford et al (1999);Teplitz et al (2006);Alexander et al (2005);Solomon & Vanden Bout (2005);Ao et al (2008);Iwasawa et al (2010).…”

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confidence: 99%

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The preferentially magnified active nucleus in IRAS F10214+4724 – I. Lens model and spatially resolved radio emission

Deane

Rawlings

Marshall

et al. 2013

Monthly Notices of the Royal Astronomical Society

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This is the first paper in a series that present a multi-wavelength analysis of the archetype Ultra-Luminous InfraRed Galaxy (ULIRG) IRAS FSC10214+47, a gravitationally lensed, starburst/AGN at z = 2.3. Here we present a new lens model and spatially-resolved radio data, as well as a deep HST F160W map. The lens modelling employs a Bayesian Markov Chain Monte Carlo algorithm with extended-source, forward ray-tracing. Using these high resolution HST, MERLIN and VLA maps, the algorithm allows us to constrain the level of distortion to the continuum spectral energy distribution resulting from emission components with differing magnification factors, due to their size and proximity to the caustic. Our lens model finds the narrow line region (NLR), and by proxy the active nucleus, is preferentially magnified. This supports previous claims that preferential magnification could mask the expected polycyclic aromatic hydrocarbon spectral features in the Spitzer mid-infrared spectrum which roughly trace the star-forming regions. Furthermore, we show the arc-to-counter-image flux ratio is not a good estimate of the magnification in this system, despite its common use in the IRAS FSC10214+47 literature. Our lens modelling suggests magnifications of µ ∼ 15−20±2 for the HST F814W, MERLIN 1.7 GHz and VLA 8 GHz maps, significantly lower than the canonical values of µ = 50 − 100 often used for this system. Systematic errors such as the dark matter density slope and co-location of stellar and dark matter centroids dominate the uncertainties in the lens model at the 40 percent level.

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Section: Introductionmentioning

confidence: 99%

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confidence: 99%

The preferentially magnified active nucleus in IRAS F10214+4724 – I. Lens model and spatially resolved radio emission

Deane

Rawlings

Marshall

et al. 2013

Monthly Notices of the Royal Astronomical Society

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The preferentially magnified active nucleus in IRAS F10214+4724 – III. VLBI observations of the radio core

Deane¹,

Rawlings²,

Garrett³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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We report 1.7 GHz Very Long Baseline Interferometry (VLBI) observations of IRAS F10214+4724, a lensed z = 2.3 obscured quasar with prodigious star formation. We detect what we argue to be the obscured active nucleus with an effective angular resolution of < 50 pc at z = 2.3. The S 1.7 = 210 µJy (9-σ) detection of this unresolved source is located within the HST rest-frame ultraviolet/optical arc, however, 100 milli-arcseconds northward of the arc centre of curvature. This leads to a source plane inversion that places the European VLBI Network detection to within milli-arcseconds of the modelled cusp caustic, resulting in a very large magnification (µ ∼70), over an order of magnitude larger than the CO (1→0) derived magnification of a spatially resolved JVLA map, using the same lens model. We estimate the quasar bolometric luminosity from a number of independent techniques and with our X-ray modelling find evidence that the AGN may be close to Compton-thick, with an intrinsic bolometric luminosity log 10 ( L bol,QSO /L ) = 11.34 ± 0.27 dex. We make the first black hole mass estimate of IRAS F10214+4724 and find log 10 (M BH /M ) = 8.36 ± 0.56 which suggests a low black hole accretion rate (λ =Ṁ/Ṁ Edd ∼ 3± 7 2 percent). We find evidence for a M BH /M spheroid ratio that is 1-2 orders of magnitude larger than that of submillimetre galaxies (SMGs) at z ∼ 2. At face value, this suggests IRAS F10214+4724 has undergone a different evolutionary path compared to SMGs at the same epoch. A primary result of this work is the demonstration that emission regions of differing size and position can undergo significantly different magnification boosts (> 1 dex) and therefore distort our view of high-redshift, gravitationally lensed galaxies.

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The gravitationally lensed, luminous infrared galaxy IRAS F10214+4724 observed with XMM-Newton

Cited by 2 publications

References 26 publications

The preferentially magnified active nucleus in IRAS F10214+4724 – I. Lens model and spatially resolved radio emission

The preferentially magnified active nucleus in IRAS F10214+4724 – I. Lens model and spatially resolved radio emission

The preferentially magnified active nucleus in IRAS F10214+4724 – III. VLBI observations of the radio core

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