Mapping the Lyα Emission around a z ∼ 6.6 QSO with MUSE: Extended Emission and a Companion at a Close Separation

被引：40

作者：

Farina, Emanuele P. ^{[1
]}

Venemans, Bram P. ^{[1
]}

Decarli, Roberto ^{[1
]}

Hennawi, Joseph F. ^{[1
]}

Walter, Fabian ^{[1
,2
,3
]}

Banados, Eduardo ^{[4
]}

Mazzucchelli, Chiara ^{[1
]}

Cantalupo, Sebastiano ^{[5
]}

Arrigoni-Battaia, Fabrizio ^{[6
]}

McGreer, Ian D. ^{[7
]}

机构：

[1] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[2] CALTECH, Astron Dept, MC105-24, Pasadena, CA 91101 USA

[3] Pete V Domenici Array Sci Ctr, Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA

[4] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA

[5] Swiss Fed Inst Technol, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland

[6] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[7] Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA

来源：

ASTROPHYSICAL JOURNAL | 2017年 / 848卷 / 02期

基金：

瑞士国家科学基金会;

关键词：

cosmology: observations; galaxies: high-redshift; quasars: general; quasars:individual (J0305-3150); DIGITAL-SKY-SURVEY; PHOTOMETRICALLY CLASSIFIED QUASARS; INTERMEDIATE-REDSHIFT QUASARS; OPTICALLY THICK ABSORBERS; ALMA SPECTROSCOPIC SURVEY; SUPERMASSIVE BLACK-HOLES; STAR-FORMING GALAXIES; METAL-POOR GAS; CIRCUMGALACTIC MEDIUM; BINARY QUASARS;

D O I：

10.3847/1538-4357/aa8df4

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We utilize the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope to search for extended Ly alpha emission around the z similar to 6.6 QSO J0305-3150. After carefully subtracting the point spread function, we reach a nominal 5 sigma surface-brightness limit of SB5 sigma. = 1.9 x 10(-18) erg s(-1) cm(-2) arcsec(-2) over a 1 arcsec(2) aperture, collapsing five. wavelength slices centered at the expected location of the redshifted Ly alpha emission (i.e., at 9256 angstrom). Current data suggest the presence (5 sigma accounting for systematics) of a Ly alpha nebula that extends for 9 kpc around the QSO. This emission is displaced and redshifted by 155 km s(-1) with respect to the location of the QSO host galaxy traced by the [C II] 158 mu m emission line. The total luminosity is L(Ly alpha) = (3.0 +/- 0.4) x 10(42) erg s(-1). Our analysis suggests that this emission is unlikely to rise from optically thick clouds illuminated by the ionizing radiation of the QSO. It is more plausible that the Ly alpha emission is due to the fluorescence of the highly ionized optically thin gas. This scenario implies a high hydrogen volume density of n(H) similar to 6 cm(-3). In addition, we detect a Ly alpha emitter (LAE) in the immediate vicinity of the QSO, i.e., with a projected separation of similar to 12.5 kpc and a line-of-sight velocity difference of 560 km s(-1). The luminosity of the LAE is L(Ly alpha) = (2.1 +/- 0.2) x 10(42) erg s(-1) and its inferred star-formation rate is SFR similar to 1.3M(circle dot) yr(-1). The probability of finding such a close LAE is one order of magnitude above the expectations based on the QSO-galaxy cross-correlation function. This discovery is in agreement with a scenario where dissipative interactions favor the rapid build-up of supermassive black holes at early cosmic times.

引用

页数：16

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