Submillimetre observations of z &gt; 6 quasars

Robson, Ian; Priddey, R.; Isaak, K. G.; McMahon, R. G.

doi:10.1111/j.1365-2966.2004.07923.x

Cited by 104 publications

(115 citation statements)

References 25 publications

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“…It has been detected previously at several sub-mm (Beelen et al 2006;Robson et al 2004) and mm (Bertoldi et al 2003;Riechers et al 2009) wavelengths. Under the assumption that the heating of the cold dust is dominated by young stars, the high FIR luminosity (L FIR ∼ 2 × 10 13 L , Beelen et al 2006) translates into a star-formation rate of ∼3000 M yr −1 .…”

Section: J1148+5251mentioning

confidence: 99%

Herschel-PACS far-infrared photometry of twoz > 4 quasars

Leipski¹,

Meisenheimer²,

Klaas³

et al. 2010

A&A

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We present Herschel far-infrared (FIR) observations of two sub-mm bright quasars at high redshift: SDSS J1148+5251 (z = 6.42) and BR 1202−0725 (z = 4.69) obtained with the PACS instrument. Both objects are detected in the PACS photometric bands. The Herschel measurements provide additional data points that constrain the FIR spectral energy distributions (SEDs) of both sources, and they emphasise a broad range of dust temperatures in these objects. For λ rest 20 μm, the two SEDs are very similar to the average SEDs of quasars at low redshift. In the FIR, however, both quasars show excess emission compared to low-z QSO templates, most likely from cold dust powered by vigorous star formation in the QSO host galaxies. For SDSS J1148+5251 we detect another object at 160 μm with a distance of ∼10 from the QSO. Although no physical connection between the quasar and this object can be shown with the available data, it could potentially confuse low-resolution measurements, thus resulting in an overestimate of the FIR luminosity of the z = 6.42 quasar.

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Section: J1148+5251mentioning

confidence: 99%

Herschel-PACS far-infrared photometry of twoz > 4 quasars

Leipski¹,

Meisenheimer²,

Klaas³

et al. 2010

A&A

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“…The sample includes QSOs detected in their dust continuum and CO line emission (Carilli et al 2000(Carilli et al , 2001Bertoldi et al 2003a,b;Petric et al 2003;Priddey et al 2003Priddey et al , 2008Walter et al 2003Walter et al , 2004Robson et al 2004;Beelen et al 2006;Maiolino et al 2007;Riechers et al 2007;Wang et al 2007Wang et al , 2008aWang et al ,b, 2010Wu et al 2009). We calculated dust masses from the detection of 1200 μm emission using Eq.…”

Section: Notesmentioning

confidence: 99%

Dust grain growth in the interstellar medium of 5 < z < 6.5 quasars

Michałowski

Murphy

Hjorth

et al. 2010

A&A

107

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Aims. We investigate whether stellar dust sources i.e. asymptotic giant branch (AGB) stars and supernovae (SNe) can account for dust detected in 5 < z < 6.5 quasars (QSOs). Methods. We calculate the required dust yields per AGB star and per SN using the dust masses of QSOs inferred from their millimeter emission and stellar masses approximated as the difference between the dynamical and the H 2 gas masses of these objects. Results. We find that AGB stars are not efficient enough to form dust in the majority of the z > 5 QSOs, whereas SNe may be able to account for dust in some QSOs. However, they require very high dust yields even for a top-heavy initial mass function.Conclusions. This suggests additional non-stellar dust formation mechanism e.g. significant dust grain growth in the interstellar medium of at least three out of nine z > 5 QSOs. SNe (but not AGB stars) may deliver enough heavy elements to fuel this growth.

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“…Over the last few years we have pursued a highly successful program aimed at elucidating the star formation history of optically-bright radio-quiet QSO host galaxies Priddey et al 2007Priddey et al , 2003aRobson et al 2004;Omont et al 2003Omont et al , 2001Omont et al , 1996aIsaak et al 2002Isaak et al , 1994McMahon et al 1999McMahon et al , 1994 via the detection of thermal emission from cool (∼50 K) dust with SCUBA, MAMBO and their single-pixel/few-pixel A&A 531, A128 (2011) predecessors. Optically-bright QSOs were targeted as likely signposts to massive underlying host galaxies in an era before large blind sub-mm surveys were possible.…”

Section: Introductionmentioning

confidence: 99%

Sub-millimeter detectedz ~ 2 radio-quiet QSOs

Orellana

Nagar

et al. 2011

A&A

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Context. We present near-IR spectroscopy of a sample of luminous (M B − 27.5; L bol > 10 14 L ), sub-millimeter-detected, dusty (M d ∼ 10 9 M ), radio-quiet quasi-stellar objects (QSOs) at z ∼ 2. Aims. A primary aim is to provide a more accurate QSO redshift determination in order to trace kinematics and inflows/outflows in these sub-mm bright QSOs. Additionally, the Hα and continuum properties allow an estimation of the black hole mass and accretion rate, offering insights into the starburst-AGN connection in sub-mm bright QSOs. Methods. We measure the redshift, width, and luminosity of the Hα line, and the continuum luminosity near Hα. Relative velocity differences between Hα and rest-frame UV emission lines are used to study the presence and strength of outflows/inflows. Luminosities and line widths are used to estimate the black hole masses, bolometric luminosities, Eddington fractions, and accretion rates; these are compared to the star-formation-rate (SFR), estimated from the sub-mm derived far-infrared (FIR) luminosity. Finally our sub-mmbright QSO sample is compared with other QSO samples at similar redshifts. Results. The Hα emission line was strongly detected in all sources. Two components -a very broad ( > ∼ 5000 km s −1 ) Gaussian and an intermediate-width ( > ∼ 1500 km s −1 ) Gaussian, were required to fit the Hα profile of all observed QSOs. Narrow ( < ∼ 1000 km s −1 ) lines were not detected in the sample QSOs. The rest-frame UV emission lines in these sub-mm bright QSOs show larger than average blue-shifted velocities, potentially tracing strong -up to 3000 km s −1 -outflows in the broad line region. With the exception of the one QSO which shows exceptionally broad Hα lines, the black hole masses of the QSO sample are in the range log M BH = 9.0−9.7 and the Eddington fractions are between 0.5 and ∼1. In black hole mass and accretion rate, this sub-mm bright QSO sample is indistinguishable from the Shemmer et al. (2004, ApJ, 614, 547) optically-bright QSO sample at z ∼ 2; the latter is likely dominated by sub-mm dim QSOs. Previous authors have demonstrated a correlation, over six orders of magnitude, between SFR and accretion rate in active galaxies: the sub-mm bright QSOs lie at the upper extremes of both quantities and their SFR is an order of magnitude higher than that predicted from the correlation.

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Submillimetre observations of z > 6 quasars

Cited by 104 publications

References 25 publications

Herschel-PACS far-infrared photometry of twoz > 4 quasars

Herschel-PACS far-infrared photometry of twoz > 4 quasars

Dust grain growth in the interstellar medium of 5 < z < 6.5 quasars

Sub-millimeter detectedz ~ 2 radio-quiet QSOs

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