Herschel-PACS far-infrared photometry of twoz &gt; 4 quasars

Leipski, C.; Meisenheimer, K.; Klaas, U.; Walter, Fabian; Nielbock, M.; Krause, O.; Dannerbauer, H.; Bertoldi, F.; Besel, M.-A.; Rosa, Gisella De; Fan, Xiaohui; Haas, Martín; Hutsemékers, Damien; Jean, C.; Lemke, D.; Rix, H. W.; Stickel, M.

doi:10.1051/0004-6361/201014718

Cited by 31 publications

(37 citation statements)

References 38 publications

(52 reference statements)

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“…Changing T dust to a very high value of 80 K (compare with Fig. 2 of Michałowski et al 2008), i.e., an upper bound for other QSOs (Haas et al 1998;Benford et al 1999;Leech et al 2001;Priddey & McMahon 2001;Knudsen et al 2003;Beelen et al 2006;Aravena et al 2008;Leipski et al 2010), decreases the M dust by a factor of ∼2.3. Hence, we also assumed (T dust , β) = (80, 2.0).…”

Section: Notesmentioning

confidence: 90%

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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Section: Notesmentioning

confidence: 90%

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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“…Because the mm/submm dust continuum fluxes of the two galaxies are nearly the same, we plot the NW galaxy fluxes (lower curve) divided by five, for better readbility. Data points at 350, 160, 70, and 24 μm are from Benford et al (1999), Leipski et al (2010), and Hines et al (2006). The other curves show model dust components for the SE galaxy: a starburst-heated 50 K component and two quasar-heated warm (130 K) and hot (410 K) dust components.…”

Section: Dust Mass and Infrared Luminositymentioning

confidence: 99%

“…The 350 μm flux measured by Benford et al (1999; rest frame 60 μm), comprises not only the fluxes of the SE and NW "starburst" components, but also a substantial contribution (30 to 50 percent) from the quasar warm dust component. The Herschel/PACS fluxes at 160 and 70 μm (Leipski et al 2010; rest frame 28 and 12 μm) are entirely from the quasar-heated "warm" and "hot" dust components; the contributions from the SE and NW "starburst" components are negligible. The Spitzer/MIPS flux at 24 μm (Hines et al 2006; rest-frame 4.2 μm) is mainly from the quasar-heated "hot" dust component.…”

Section: Dust Mass and Infrared Luminositymentioning

confidence: 99%

BR1202–0725: an extreme multiple merger atz= 4.7

Salomé

Guèlin

Downes

et al. 2012

A&A

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The radio-quiet quasar BR1202-0725 (z = 4.695) is a remarkable source with a bright northwest (NW) companion detected at submillimeter and radio wavelengths but invisible in the optical. In the absence of amplification by gravitational lensing, BR1202−0725 would be the most luminous binary CO and far-infrared (far-IR) source in the Universe. In this paper, we report observations with the IRAM Plateau de Bure interferometer of BR1202-0725 in the redshifted emission of the CO(5-4) and (7-6) lines, the [C I]( 3 P 2 − 3 P 1 ) line, a high angular resolution (0.3 × 0.8 ) 1.3 mm map of the rest-frame, far-IR dust continuum, and a search for the CO(11−10) line. We compare these results with recent ALMA data in the [C II] line. Both the quasar host galaxy and its NW companion are spatially resolved in the molecular line emission and the dust continuum. The CO profile of the NW companion is very broad with a full width at half maximum of ∼1000 ± 130 km s −1 , compared to ∼360 ± 40 km s −1 for the quasar host galaxy to the southeast (SE). The difference in linewidths and center velocities, and the absence of any lens candidate or arc-like structure in the field, at any wavelength, show that the obscured NW galaxy and the SE quasar host galaxy cannot be lensed images of the same object. Instead, we find morphological and kinematic evidence for sub-structures in both the NW and SE sources. We interpret these results as strong indications that the BR1202-0725 complex is a group of young, interacting, and highly active starburst galaxies.

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“…The FIR luminosity of L FIR ∼ 10 12−13 L is attributed to cold dust (T ∼ 30-60 K) (e.g., Wang et al 2008) which is probably distributed over kilo-parsec scales throughout the host galaxy (Leipski et al 2010). The amount of cold dust inferred is about a few times 10 8 M (e.g., Bertoldi et al 2003a;Robson et al 2004;Beelen et al 2006;Michałowski et al 2010).…”

Section: Introductionmentioning

confidence: 97%

Genesis and evolution of dust in galaxies in the early Universe

Gall

Andersen

Hjorth

2011

A&A

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Aims. We intend to assess the most plausible scenarios for generating large amounts of dust in high-z quasars (QSOs) on the basis of observationally derived physical properties of QSOs at z 6. Methods. We use a chemical evolution model to compute the temporal progression of quantities such as the amount of dust and gas, stellar masses, star formation rates (SFRs) and the metallicity for various combinations of the initial mass function (IMF), the mass of the galaxy, dust production efficiencies, and the degree of dust destruction in the ISM. We investigate the influence of the SFR on the evolution of these quantities, and determine the earliest epochs at which agreement with observations can be achieved. We apply the obtained results to individual QSOs at z 6. Results. We find that large quantities of dust can be generated rapidly as early as 30 Myr after the onset of the starburst when the SFR of the starburst is 10 3 M yr −1 . The amount of dust and several other physical quantities of individual QSOs at z 6 are satisfactorily reproduced by models at epochs 30, 70, 100, and 170 Myr for galaxies with initial gas masses of 1-3 × 10 11 M . The best agreement with observations is obtained with top-heavy IMFs. A sizable dust contribution from supernovae (SNe) is however required, while at these epochs dust production by asymptotic giant branch (AGB) stars is negligible. Moderate dust destruction in the ISM can be accommodated.

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

Cited by 31 publications

References 38 publications

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

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

BR1202–0725: an extreme multiple merger atz= 4.7

Genesis and evolution of dust in galaxies in the early Universe

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