ORCID Profile
0000-0003-2901-6842
Current Organisation
EUMETSAT
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Astronomical and Space Sciences | Cosmology and Extragalactic Astronomy
Publisher: EDP Sciences
Date: 09-2016
Publisher: American Astronomical Society
Date: 18-08-2016
Publisher: Oxford University Press (OUP)
Date: 24-10-2017
Publisher: American Astronomical Society
Date: 04-10-2018
Publisher: American Astronomical Society
Date: 09-10-2017
Publisher: EDP Sciences
Date: 07-2019
DOI: 10.1051/0004-6361/201935283
Abstract: Context . Galaxy-wide outflows driven by star formation and/or an active galactic nucleus (AGN) are thought to play a crucial rule in the evolution of galaxies and the metal enrichment of the inter-galactic medium. Direct measurements of these processes are still scarce and new observations are needed to reveal the nature of outflows in the majority of the galaxy population. Aims . We combine extensive, spatially-resolved, multi-wavelength observations, taken as part of the Close AGN Reference Survey (CARS), for the edge-on disc galaxy HE 1353−1917 in order to characterise the impact of the AGN on its host galaxy via outflows and radiation. Methods . Multi-color broad-band photometry was combined with spatially-resolved optical, near-infrared (NIR) and sub-mm and radio observations taken with the Multi-Unit Spectroscopy Explorer (MUSE), the Near-infrared Integral Field Spectrometer (NIFS), the Atacama Large Millimeter Array (ALMA), and the Karl G. Jansky Very Large Array (VLA) to map the physical properties and kinematics of the multi-phase interstellar medium. Results . We detect a biconical extended narrow-line region ionised by the luminous AGN orientated nearly parallel to the galaxy disc, extending out to at least 25 kpc. The extra-planar gas originates from galactic fountains initiated by star formation processes in the disc, rather than an AGN outflow, as shown by the kinematics and the metallicity of the gas. Nevertheless, a fast, multi-phase, AGN-driven outflow with speeds up to 1000 km s −1 is detected close to the nucleus at 1 kpc distance. A radio jet, in connection with the AGN radiation field, is likely responsible for driving the outflow as confirmed by the energetics and the spatial alignment of the jet and multi-phase outflow. Evidence for negative AGN feedback suppressing the star formation rate (SFR) is mild and restricted to the central kpc. But while any SFR suppression must have happened recently, the outflow has the potential to greatly impact the future evolution of the galaxy disc due to its geometrical orientation. Conclusions. . Our observations reveal that low-power radio jets can play a major role in driving fast, multi-phase, galaxy-scale outflows even in radio-quiet AGN. Since the outflow energetics for HE 1353−1917 are consistent with literature, scaling relation of AGN-driven outflows the contribution of radio jets as the driving mechanisms still needs to be systematically explored.
Publisher: EDP Sciences
Date: 26-06-2019
DOI: 10.1051/0004-6361/201834441
Abstract: The absence of star formation in the bar region that has been reported for some galaxies can theoretically be explained by shear. However, it is not clear how star-forming (SF) bars fit into this picture and how the dynamical state of the bar is related to other properties of the host galaxy. We used integral-field spectroscopy from VLT/MUSE to investigate how star formation within bars is connected to structural properties of the bar and the host galaxy. We derived spatially resolved H α fluxes from MUSE observations from the CARS survey to estimate star formation rates in the bars of 16 nearby (0.01 z 0.06) disc galaxies with stellar masses between 10 10 M ⊙ and 10 11 M ⊙ . We further performed a detailed multicomponent photometric decomposition on images derived from the data cubes. We find that bars clearly ide into SF and non-SF types, of which eight are SF and eight are non-SF. Whatever the responsible quenching mechanism is, it is a quick process compared to the lifetime of the bar. The star formation of the bar appears to be linked to the flatness of the surface brightness profile in the sense that only the flattest bars ( n bar ≤0.4) are actively SF (SFR b 0.5 M ⊙ yr −1 ). Both parameters are uncorrelated with Hubble type. We find that star formation is 1.75 times stronger on the leading than on the trailing edge and is radially decreasing. The conditions to host non-SF bars might be connected to the presence of inner rings. Additionally, from testing an AGN feeding scenario, we report that the star formation rate of the bar is uncorrelated with AGN bolometric luminosity. The results of this study may only apply to type-1 AGN hosts and need to be confirmed for the full population of barred galaxies.
Publisher: EDP Sciences
Date: 28-07-2017
Publisher: American Astronomical Society
Date: 11-2020
Publisher: American Astronomical Society
Date: 17-10-2019
Publisher: American Astronomical Society
Date: 22-07-2016
Publisher: EDP Sciences
Date: 03-2022
DOI: 10.1051/0004-6361/202040122
Abstract: Context. The strong asymmetry in the optical [O III ] λ 5007 emission line is one of the best signatures of active galactic nuclei (AGN) driven warm (∼10 4 K) ionized gas outflows on host galaxy scales. While large spectroscopic surveys such as the sloan digital sky survey (SDSS) have characterized the kinematics of [O III ] for large s les of AGN, estimating the associated energetics requires spatially resolving these outflows with, for ex le, integral field unit (IFU) studies. Aims. As part of the Close AGN Reference Survey, we obtained spatially resolved IFU spectroscopy for a representative s le of 39 luminous type 1 AGN at 0.01 z 0.06 with the multi unit spectroscopic explorer and the visible multi object spectrograph IFUs at the very large telescope to infer the spatial location of the ionized gas outflows. Methods. We compared the 2D light distributions of the [O III ] wing to that of the H β broad emission line region, a classical point source (PSF). We then used the PSF to distinguish between the unresolved and resolved [O III ] wing emission. We further determined its location using spectro-astrometry for the point-like sources. Results. The [O III ] wing is spatially unresolved in 23 out of the 36 AGN with 80% of the flux associated with a point-like source. We measured 100 pc offsets in the spatial location of the outflow from the AGN nucleus using the spectro-astrometry technique for these sources. For the other 13 AGN, the [O III ] wing emission is resolved and possibly extended on several kiloparsec scales. Conclusions. We conclude that [O III ] wing emission can be compact or extended in an unbiased luminous AGN s le, where both cases are likely to appear. Electron density in the compact [O III ] wing regions (median n e ∼ 1900 cm −3 ) is nearly a magnitude higher than in the extended ones (median n e ∼ 500 cm −3 ). The presence of spatially extended and compact [O III ] wing emission is unrelated to the AGN bolometric luminosity and to inclination effects, which means other features such as time delays, or mechanical feedback (radio jets) may shape the ionized gas outflow properties.
Publisher: American Astronomical Society
Date: 08-07-2019
Start Date: 06-2019
End Date: 06-2024
Amount: $360,000.00
Funder: Australian Research Council
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