A coronagraphic absorbing cloud reveals the narrow-line region and extended Lyman α emission of QSO J0823+0529

Fathivavsari, H.; Petitjean, P.; Noterdaeme, P.; Pâris, Isabelle; Finley, Hayley; López, Sebastián; Srianand, R.; Sánchez, Paula

doi:10.1093/mnras/stv1984

Cited by 20 publications

(21 citation statements)

References 63 publications

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“…To start with, we note that the size and surface brightness of the Lyα emission seen are both less than what is typically seen in the case of radio-loud QSOs at similar redshifts (see for example, Roche et al 2014).This suggests that the origin of Lyα emission in the present case may be very different from the extended Lyα seen around radio galaxies. We also note that, based on the surface brightness of the Lyα emission, lack of N V absorption and fine-structure lines of Si II, this DLA is not similar to the one studied by Fathivavsari et al (2015), where the DLA is thought to be dense, compact and close to the QSO covering the broad as well as narrow emission line region only partially (see also , Finley et al 2013). Therefore, it is most likely that we are not seeing the extended NLR of the host galaxy.…”

Section: Fluorescent Lyα Emission Induced By the Quasarcontrasting

confidence: 75%

Detection of emission lines fromz∼ 3 DLAs towards the QSO J2358+0149

Srianand

Hussain

Noterdaeme

et al. 2016

Mon. Not. R. Astron. Soc.

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Using VLT/X-shooter we searched for emission line galaxies associated to four damped Lyman-α systems (DLAs) and one sub-DLA at 2.73 z 3.25 towards QSO J2358+0149. We detect [O III] emission from a "low-cool" DLA at z abs = 2.9791 (having log N(H I) = 21.69 ± 0.10, [Zn/H] = −1.83 ± 0.18) at an impact parameter of, ρ ∼ 12 kpc. The associated galaxy is compact with a dynamical mass of (1 − 6) × 10 9 M ⊙ , very high excitation Hβ] both greater than 10), 12+[O/H] 8.5 and moderate star formation rate (SFR 2 M ⊙ yr −1 ). Such properties are typically seen in the low-z extreme blue compact dwarf galaxies. The kinematics of the gas is inconsistent with that of an extended disk and the gas is part of either a large scale wind or cold accretion. We detect Lyα emission from the z abs = 3.2477 DLA (having log N(H I)=21.12±0.10 and [Zn/H]=−0.97 ± 0.13). The Lyα emission is redshifted with respect to the metal absorption lines by 320 km s −1 , consistent with the location of the red hump expected in radiative transport models. We derive SFR∼0.2-1.7 M ⊙ yr −1 and Lyα escape fraction of 10 per cent. No other emission line is detected from this system. Because the DLA has a small velocity separation from the quasar (∼500 km s −1 ) and the DLA emission is located within a small projected distance (ρ < 5 kpc), we also explore the possibility that the Lyα emission is being induced by the QSO itself. QSO induced Lyα fluorescence is possible if the DLA is within a physical separation of 340 kpc to the QSO. Detection of stellar continuum light and/or the oxygen emission lines would disfavor this possibility. We do not detect any emission line from the remaining three systems.

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Section: Fluorescent Lyα Emission Induced By the Quasarcontrasting

confidence: 75%

Detection of emission lines fromz∼ 3 DLAs towards the QSO J2358+0149

Srianand

Hussain

Noterdaeme

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Interestingly, this ghostly DLA has characteristics similar to those of the 'eclipsing' DLA found along the line of sight to the quasar J0823+0529 (Fathivavsari et al 2015). Both DLAs have very small sizes and are located close to the central AGN.…”

Section: Discussionsupporting

confidence: 56%

A ghostly damped Ly α system revealed by metal absorption lines

Fathivavsari

Petitjean

Zou

et al. 2016

Monthly Notices of the Royal Astronomical Society: Letters

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We report the discovery of the first 'ghostly' damped Lyα absorption system (DLA), which is identified by the presence of absorption from strong low-ion species at z abs = 1.70465 along the line of sight to the quasar SDSSJ113341.29−005740.0 with z em = 1.70441. No Lyα absorption trough is seen associated with these absorptions because the DLA trough is filled with the leaked emission from the broad emission line region of the quasar. By modeling the quasar spectrum and analyzing the metal lines, we derive logN (H i)(cm −2 )∼21.0 ± 0.3. The DLA cloud is small (≤ 0.32 pc) thus not covering entirely the broad line region and is located at ≥ 39 pc from the central active galactic nucleus (AGN). Although the DLA is slightly redshifted relative to the quasar, its metallicity ([S/H]=−0.41±0.30) is intermediate between what is expected from infalling and outflowing gas. It could be possible that the DLA is part of some infalling material accreting onto the quasar host galaxy through filaments, and that its metallicity is raised by mixing with the enriched outflowing gas emanating from the central AGN. Current DLA surveys miss these 'ghostly' DLAs, and it would be important to quantify the statistics of this population by searching the SDSS database using metal absorption templates.

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“…This result seems to be in stark contrast with previous narrow-band and spectroscopic surveys for bright radio-quiet quasars at highredshift. These studies have found detection rates of giant nebula less than 10% using NB imaging at < < z 2 3 (Cantalupo et al 2014;Martin et al 2014;Hennawi et al 2015;Arrigoni Battaia et al 2016), while spectroscopic surveys at any redshift have found exclusively smaller nebulae (<60 pkpc) and only in about 50% of the cases (North et al 2012;Fathivavsari et al 2015). Because all these surveys-including our MUSE observations-reached a similar depth, the origin of this discrepancy must be searched for somewhere else.…”

Section: Why Such a High Detection Ratementioning

confidence: 72%

“…There are only a few cases in which the nebulae are symmetric enough to expect a detection over scales extending to 100 pkpc (e.g., #5);however, the difficulty of estimating the exact PSF of the quasar through slit spectroscopy may result in a substantial reduction of the detection rate. This effect may also reduce the detectability of the inner parts of the nebulae to the level found by spectroscopic surveys (North et al 2012;Fathivavsari et al 2015). Moreover, the availability of more spatial positions and the large FoV provided by MUSE with respect to a single slit will clearly facilitate the extraction and detection of extended emission around the quasars.…”

Section: Why Such a High Detection Ratementioning

confidence: 99%

UBIQUITOUS GIANT Lyα NEBULAE AROUND THE BRIGHTEST QUASARS AT z ∼ 3.5 REVEALED WITH MUSE^∗

Borisova

Cantalupo

Lilly

et al. 2016

ApJ

279

536

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Direct Lyα imaging of intergalactic gas atz 2 has recently revealed giant cosmological structures around quasars, e.g., the Slug Nebula. Despite their high luminosity, the detection rate of such systems in narrow-band and spectroscopic surveys is less than 10%, possibly encoding crucial information on the distribution of gas around quasars and the quasar emission properties. In this study, we use the MUSE integral-field instrument to perform a blind survey for giant a Ly nebulae around 17 bright radio-quiet quasars at < < z 3 4 that does not suffer from most of the limitations of previous surveys. After data reduction and analysis performed with specifically developed tools, we found that each quasar is surrounded by giant a Ly nebulae with projected sizes larger than 100 physical kiloparsecs and, in some cases, extending up to 320 kpc. The circularly averaged surface brightness profiles of the nebulae appear to be very similar to each other despite their different morphologies and are consistent with power laws with slopes»-1.8. The similarity between the properties of all these nebulae and the Slug Nebula suggests a similar origin for all systems and that a large fraction of gas around bright quasars could be in a relatively "cold" (T ∼ 10 4 K) and dense phase. In addition, our results imply that such gas is ubiquitous within at least 50 kpc from bright quasars at < < z 3 4 independently of the quasar emission opening angle, or extending up to 200 kpc for quasar isotropic emission.

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A coronagraphic absorbing cloud reveals the narrow-line region and extended Lyman α emission of QSO J0823+0529

Cited by 20 publications

References 63 publications

Detection of emission lines fromz∼ 3 DLAs towards the QSO J2358+0149

Detection of emission lines fromz∼ 3 DLAs towards the QSO J2358+0149

A ghostly damped Ly α system revealed by metal absorption lines

UBIQUITOUS GIANT Lyα NEBULAE AROUND THE BRIGHTEST QUASARS AT z ∼ 3.5 REVEALED WITH MUSE^∗

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A coronagraphic absorbing cloud reveals the narrow-line region and extended Lyman α emission of QSO J0823+0529

Cited by 20 publications

References 63 publications

Detection of emission lines fromz∼ 3 DLAs towards the QSO J2358+0149

Detection of emission lines fromz∼ 3 DLAs towards the QSO J2358+0149

A ghostly damped Ly α system revealed by metal absorption lines

UBIQUITOUS GIANT Lyα NEBULAE AROUND THE BRIGHTEST QUASARS AT z ∼ 3.5 REVEALED WITH MUSE∗

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UBIQUITOUS GIANT Lyα NEBULAE AROUND THE BRIGHTEST QUASARS AT z ∼ 3.5 REVEALED WITH MUSE^∗