Resolved Molecular Gas in a Quasar Host Galaxy at Redshift [FORMULA][F]z=6.42[/F][/FORMULA]

Walter, Fabian; Carilli, C. L.; Bertoldi, F.; Menten, K. M.; Cox, P.; Lo, K. Y.; Fan, Xiaohui; Strauss, Michael A.

doi:10.1086/426017

Cited by 349 publications

(536 citation statements)

References 21 publications

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“…In the few cases where the gas emission has been resolved in high redshift quasar host galaxies, it is distributed in compact regions of < few kpc in size (e.g. Carilli et al 2002;Walter et al 2004;Riechers et al 2011a;Wang et al 2013;Willott et al 2013). The conventional interpretation is that the molecular gas in quasar hosts resides in a nuclear region close to the accreting black hole, and its excitation properties can therefore be explained by a single temperature and density gas component.…”

Section: Co(3-2) Sizesmentioning

confidence: 99%

“…Many of the recent efforts have focussed on z > 4 quasars (e.g. Carilli et al 2002;Walter et al 2004;Wang et al 2010) and, as a consequence, the numbers of quasars with CO detections at the peak epoch of galaxy formation (1.5< z < 3.0) is considerably smaller -<20 quasars. Many of the quasars that have been observed in molecular gas at these epochs are gravitationally lensed systems (e.g.…”

Section: Introductionmentioning

confidence: 99%

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The discovery of gas-rich, dusty starbursts in luminous reddened quasars atz∼ 2.5 with ALMA

Banerji

Carilli

Jones

et al. 2016

Mon. Not. R. Astron. Soc.

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We present ALMA observations of cold dust and molecular gas in four high-luminosity, heavily reddened (A V ∼ 2.5 − 6 mag) Type 1 quasars at z ∼ 2.5 with virial M BH ∼ 10 10 M , to test whether dusty, massive quasars represent the evolutionary link between submillimetre bright galaxies (SMGs) and unobscured quasars. All four quasars are detected in both the dust continuum and in the 12 CO(3-2) line. The mean dust mass is 6×10 8 M assuming a typical high redshift quasar spectral energy distribution (T=41K, β=1.95 or T=47K, β=1.6). The implied star formation rates are very high -1000 M yr −1 in all cases. Gas masses estimated from the CO line luminosities cover ∼1-5×10 10 (α CO /0.8)M and the gas depletion timescales are very short -∼ 5 − 20Myr. A range of gas-to-dust ratios is observed in the sample. We resolve the molecular gas in one quasar -ULASJ2315+0143 (z = 2.561) -which shows a strong velocity gradient over ∼20 kpc. The velocity field is consistent with a rotationally supported gas disk but other scenarios, e.g. mergers, cannot be ruled out at the current resolution of these data. In another quasar -ULASJ1234+0907 (z = 2.503) -we detected molecular line emission from two millimetre bright galaxies within 200 kpc of the quasar, suggesting that this quasar resides in a significant over-density. The high detection rate of both cold dust and molecular gas in these sources, suggests that reddened quasars could correspond to an early phase in massive galaxy formation associated with large gas reservoirs and significant star formation.

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Section: Co(3-2) Sizesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The discovery of gas-rich, dusty starbursts in luminous reddened quasars atz∼ 2.5 with ALMA

Banerji

Carilli

Jones

et al. 2016

Mon. Not. R. Astron. Soc.

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“…This galaxy been detected in thermal dust, non-thermal radio continuum, and CO line emission (Walter et al 2003;Bertoldi et (Walter et al 2004). The total flux is 0.15 Jy km s −1 , and the source is clearly resolved, with a full extend of about 1 .…”

Section: Introduction: Cosmic Reionization and The First Galaxiesmentioning

confidence: 84%

“…2). High resolution VLA imaging of the molecular gas distribution in J1148+5251 provides the only direct measure of the host galaxy dynamical mass, resulting in a value of ∼4×10 10 M within 3 kpc of the galaxy center (Walter et al 2004;Walter and Carilli, this volume). This mass is comparable to the gas mass, suggesting a baryon-dominated potential for the inner few kpc of the galaxy (Lintott et al 2006), as is true in nearby spheroidal galaxies, and for ULIRGs (Downes and Solomon 1998).…”

Section: Introduction: Cosmic Reionization and The First Galaxiesmentioning

confidence: 99%

“…A final interesting aspect of the molecular line studies of the most distant QSO host galaxies is the derivation of the sizes of the cosmic Stromgren spheres (Walter et al 2003;Fan et al 2006a). The size of the ionized region around the QSO, presumably formed by the radiation from the QSO, can be derived from the difference between the redshift of the host galaxy and the redshift of the on-set of the GunnPeterson trough.…”

Section: Introduction: Cosmic Reionization and The First Galaxiesmentioning

confidence: 99%

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Studying the first galaxies with ALMA

Carilli

Walter

Wang

et al. 2007

Astrophys Space Sci

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We discuss observations of the first galaxies, within cosmic reionization, at centimeter and millimeter wavelengths. We present a summary of current observations of the host galaxies of the most distant QSOs (z ∼ 6). These observations reveal the gas, dust, and star formation in the host galaxies on kpc-scales. These data imply an enriched ISM in the QSO host galaxies within 1 Gyr of the big bang, and are consistent with models of coeval supermassive black hole and spheroidal galaxy formation in major mergers at high redshift. Current instruments are limited to studying truly pathologic objects at these redshifts, meaning hyperluminous infrared galaxies (L FIR ∼ 10 13 L ). ALMA will provide the one to two orders of magnitude improvement in millimeter astronomy required to study normal star forming galaxies (i.e. Ly-α emitters) at z ∼ 6. ALMA will reveal, at sub-kpc spatial resolution, the thermal gas and dust-the fundamental fuel for star formation-in galaxies into cosmic reionization.

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