<i>AKARI</i>NEAR- AND MID-INFRARED SPECTROSCOPY OF APM 08279+5255 AT<i>z</i>= 3.91

Oyabu, Shinki; Kawara, Kimiaki; Tsuzuki, Y.; Matsuoka, Yoshiki; Sameshima, Hiroaki; Asami, Naoko; Ohyama, Youichi

doi:10.1088/0004-637x/697/1/452

Cited by 15 publications

(17 citation statements)

References 48 publications

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“…The dust mass M dust is related to the flux density f ν as M dust / f ν = D 2 /[κ ν B ν ( T dust )] in the rest frame, where D is the distance to the source and κ ν is the absorption cross‐section per unit dust mass (e.g. Oyabu et al 2009). When a modified blackbody spectrum ν β B ν ( T dust ) is applied, β and T dust should be used together as a set, because M dust depends on κ ν B ν ( T dust ), but not on B ν ( T dust ) alone.…”

Section: Dust Emission and Energeticsmentioning

confidence: 99%

Stellar population and dust extinction in an ultraluminous infrared galaxy at z= 1.135

Kawara

Oyabu

Matsuoka

et al. 2009

Monthly Notices of the Royal Astronomical Society

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We present the detailed optical to far-infrared observations of SST J1604+4304, an ULIRG at z = 1.135. Analyzing the stellar absorption lines, namely, the CaII H & K and Balmer H lines in the optical spectrum, we derive the upper limits of an age for the stellar population. Given this constraint, the minimum χ 2 method is used to fit the stellar population models to the observed SED from 0.44 to 5.8µm. We find the following properties. The stellar population has an age 40 -200 Myr with a metallicity 2.5 Z ⊙ . The starlight is reddened by E(B − V ) = 0.8. The reddening is caused by the foreground dust screen, indicating that dust is depleted in the starburst site and the starburst site is surrounded by a dust shell. The infrared (8-1000µm) luminosity is L ir = 1.78 ± 0.63 × 10 12 L ⊙ . This is two times greater than that expected from the observed starlight, suggesting either that 1/2 of the starburst site is completely obscured at UV-optical wavelengths, or that 1/2 of L ir comes from AGN emission. The inferred dust mass is 2.0±1.0×10 8 M ⊙ . This is sufficient to form a shell surrounding the galaxy with an optical depth E(B −V ) = 0.8. From our best stellar population modelan instantaneous starburst with an age 40 Myr, we infer the rate of 19 supernovae(SNe) per year. Simply analytical models imply that 2.5 Z ⊙ in stars was reached when the gas mass reduced to 30% of the galaxy mass. The gas metallcity is 4.8Z ⊙ at this point. The gas-to-dust mass ratio is then 120 ± 73. The inferred dust production rate is 0.24 ± 0.12M ⊙ per SN. If 1/2 of L ir comes from AGN emission, the rate is 0.48 ± 0.24M ⊙ per SN. We discuss the evolutionary link of SST J1604+4304 to other galaxy populations in terms of the stellar masses and the galactic winds, including optically selected low-luminosity Lyman α-emitters and submillimeter selected highluminosity galaxies.

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Section: Dust Emission and Energeticsmentioning

confidence: 99%

Stellar population and dust extinction in an ultraluminous infrared galaxy at z= 1.135

Kawara

Oyabu

Matsuoka

et al. 2009

Monthly Notices of the Royal Astronomical Society

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“…Hence an SED which is UV bright and X-ray weak is clearly consistent with UV line driving, while one which has strong X-ray flux is less favourable. We plot the broadband SED from Spitzer (Soifer et al 2004), AKARI (Oyabu et al 2009), 2.5 m Isaac Newton Telescope (INT, Benn et al 2002) and Chandra (Epoch1) data. The optical continuum underneath the Hα line shows a clear disc spectrum, so we use this to constrain the mass accretion rate through the outer accretion disc via the OPTXAGNF model ).…”

Section: Broadband Sed and Quasar Parametersmentioning

confidence: 99%

Revisiting the extremely fast disc wind in a gravitationally lensed quasar APM 08279+5255

Hagino

Done

Odaka

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The gravitationally lensed quasar APM 08279+5255 has the fastest claimed wind from any AGN, with velocities of 0.6-0.7c, requiring magnetic acceleration as special relativisitic effects limit all radiatively driven winds to v<0.3-0.5c. However, this extreme velocity derives from interpreting both the narrow and broad absorption features in the X-ray spectrum as iron absorption lines. The classic ultrafast outflow source PDS 456 also shows similar absorption systems, but here the higher energy, broader feature is generally interpreted as an absorption edge. We reanalyse all the spectra from APM 08279+5255 using a full 3-dimensional Monte Carlo radiative transfer disc wind model for the ionised wind at 0.1-0.2c, together with complex absorption from lower ionisation material, and find that this is a better description of the data. Thus there is no strong requirement for outflow velocities beyond 0.2c, which can be powered by radiation driving. We show that UV line driving is especially likely given the spectral energy distribution of this source which is intrinsically UV bright and X-ray weak. While the peak of this emission is unobservable, it must be luminous enough to power the observed hot dust, favouring at least moderate black hole spin.

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“…In this view, the spectral capabilities at 2.5–5 μm of the Akari satellite look very promising (e.g. Oyabu et al 2009).…”

Section: The Agn/sb Spectral Decomposition At 5–8 μMmentioning

confidence: 99%

Exploring the active galactic nucleus and starburst content of local ultraluminous infrared galaxies through 5-8 μm spectroscopy

Nardini¹,

Risaliti²,

Salvati³

et al. 2009

Monthly Notices of the Royal Astronomical Society

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We present a 5–8 μm analysis of the Spitzer spectra of 71 ultraluminous infrared galaxies (ULIRGs) with redshift z < 0.15, devoted to the study of the role of active galactic nuclei (AGN) and starbursts (SBs) as the power source of the extreme infrared emission. Around ∼5 μm, an AGN is much brighter (by a factor of ≈30) than an SB of equal bolometric luminosity. This allows us to detect the presence of even faint accretion‐driven cores inside ULIRGs: signatures of AGN activity are found in ∼70 per cent of our sample (50/71 sources). Through a simple analytical model, we are also able to obtain a quantitative estimate of the AGN/SB contribution to the overall energy output of each source. Although the main fraction of ULIRG luminosity is confirmed to arise from star formation events, the AGN contribution is non‐negligible (∼23 per cent) and is shown to increase with luminosity. The existence of a rather heterogeneous pattern in the composition and geometrical structure of the dust among ULIRGs is newly supported by the comparison between individual absorption features and continuum extinction.

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AKARINEAR- AND MID-INFRARED SPECTROSCOPY OF APM 08279+5255 ATz= 3.91

Cited by 15 publications

References 48 publications

Stellar population and dust extinction in an ultraluminous infrared galaxy at z= 1.135

Stellar population and dust extinction in an ultraluminous infrared galaxy at z= 1.135

Revisiting the extremely fast disc wind in a gravitationally lensed quasar APM 08279+5255

Exploring the active galactic nucleus and starburst content of local ultraluminous infrared galaxies through 5-8 μm spectroscopy

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