The MURALES survey

Capetti, A.; Balmaverde, B.; Tadhunter, C. N.; Marconi, A.; Venturi, G.; Chiaberge, M.; Baldi, Ranieri D.; Baum, Stefi A.; Gilli, R.; Grandi, P.; Meyer, Eileen T.; Miley, G. K.; O’Dea, C. P.; Sparks, W. B.; Torresi, E.; Tremblay, G. R.

doi:10.1051/0004-6361/202141965

Cited by 10 publications

(10 citation statements)

References 70 publications

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“…The employed models adopt a unimodal standard Salpeter IMF with slope 1.3 (Salpeter 1955) as described in Vazdekis et al (1996) and scaled-solar Padova+00 isochrones (Girardi et al 2000), which have M/H metallicities spanning from -1.71 to +0.22 (in log, with respect to the solar value) and ages between 0.063 and 17.8 Gyr. The continuum modelling was done using the penalized pixel-fitting code (PPXF; Cappellari & Emsellem 2004;Cappellari 2017), which convolves the linearly combined stellar templates with a Gaussian function to reproduce the velocity and velocity dispersion of the absorption features. The main gas emission lines, as well as the residuals of not optimally subtracted sky lines, were masked during the stellar fitting, and underlying absorption features were extrapolated over in order to model the full spectral range.…”

Section: Discussionmentioning

confidence: 99%

“…To do so, we made use of a python-based graphical user interface (GUI) which allows us to extract spectra from single spaxels or multi-spaxel regions (details in D' Ago et al 2021). The interface allowed us to interactively probe a variety of regions and to test different fitting parameters to model the spectra with the software ppxf (Cappellari & Emsellem 2004;Cappellari 2017). As done for the stellar continuum fitting of the cube, we employed the E-MILES single-stellar population (SSP) model spectra (details in Sect.…”

Section: Stars In the Teacup Handlementioning

confidence: 99%

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Complex AGN feedback in the Teacup galaxy

Venturi,

Treister,

Finlez

et al. 2023

A&A

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Context. The z ∼ 0.1 type-2 QSO J1430+1339, known as the “Teacup”, is a complex galaxy showing a loop of ionised gas ∼10 kpc in diameter, co-spatial radio bubbles, a compact (∼1 kpc) jet, and outflow activity. Its closeness offers the opportunity to study in detail the intricate interplay between the central supermassive black hole (SMBH) and the material in and around the galaxy, both the interstellar medium (ISM) and circumgalactic medium (CGM). Aims. We characterise the spatially resolved properties and effects of the galactic ionised gas outflow and compare them with those of the radio jet and with theoretical predictions to infer its acceleration mechanism. Methods. We used VLT/MUSE optical integral field spectroscopic observations to obtain flux, kinematic, and excitation maps of the extended (up to ∼100 kpc) ionised gas and to characterise the properties of stellar populations. We built radial profiles of the outflow properties as a function of distance from the active nucleus, from kiloparsec up to tens of kiloparsec scales, at ∼1 kpc resolution. Results. We detect a velocity dispersion enhancement (≳300 km s−1) elongated over several kiloparsecs perpendicular to the radio jet, the active galactic nucleus (AGN) ionisation lobes, and the fast outflow, similar to what is found in other galaxies hosting compact, low-power jets, indicating that the jet strongly perturbs the host ISM during its passage. We observe a decreasing trend with distance from the nucleus for the outflow properties (mass outflow rate, kinetic rate, momentum rate). The mass outflow rate drops from around 100 M⊙ yr−1 in the inner 1–2 kpc to ≲0.1 M⊙ yr−1 at 30 kpc. The mass outflow rate of the ionised outflow is significantly higher (∼1–8 times) than the molecular one, in contrast with what is often quoted in AGN. Based on energetic and morphological arguments, the driver of the multi-phase outflow is likely a combination of AGN radiation and the jet, or AGN radiation pressure on dust alone. The outflow mass-loading factor is ∼5–10 and the molecular gas depletion time due to the multi-phase outflow is ≲108 yr, indicating that the outflow can significantly affect the star formation and the gas reservoir in the galaxy. However, the fraction of the ionised outflow that is able to escape the dark matter halo potential is likely negligible. We detect blue-coloured continuum emission co-spatial with the ionised gas loop. Here, stellar populations are younger (≲100–150 Myr) than in the rest of the galaxy (∼0.5–1 Gyr). This constitutes possible evidence for star formation triggered at the edge of the bubble due to the compressing action of the jet and outflow (“positive feedback”), as predicted by theory. All in all, the Teacup constitutes a rich system in which AGN feedback from outflows and jets, in both its negative and positive flavours, co-exist.

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Section: Discussionmentioning

confidence: 99%

Section: Stars In the Teacup Handlementioning

confidence: 99%

Complex AGN feedback in the Teacup galaxy

Venturi,

Treister,

Finlez

et al. 2023

A&A

Self Cite

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“…The possibility of outflows and more generally, jets, inducing star formation has been studied in both galactic (see Bicknell et al 2000;Miley & De Breuck 2008;Capetti et al 2022) and cosmological scales (Gilli et al 2019), as well as simulations (Gaibler et al 2012). As such, it is possible that the observed star formation from the RG is either induced or enhanced by the jet.…”

Section: Discussionmentioning

confidence: 99%

An Extended Lyα Outflow from a Radio Galaxy at z = 3.7?

Coloma Puga,

Balmaverde,

Capetti

et al. 2023

ApJL

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Spatially resolved observations of active galactic nuclei (AGN) host galaxies undergoing feedback processes are one of the most relevant avenues through which galactic evolution can be studied, given the long-lasting effects AGN feedback has on gas reservoirs, star formation, and AGN environments at all scales. Within this context, we report results from Very Large Telescope/MUSE integral field optical spectroscopy of TN J1049-1258, one of the most powerful radio sources known, at a redshift of 3.7. We detected extended (∼18 kpc) Lyα emission, spatially aligned with the radio axis, redshifted by 2250 ± 60 km s−1 with respect to the host galaxy systemic velocity, and cospatial with UV continuum emission. This Lyα emission could arise from a companion galaxy, although there are arguments against this interpretation. Alternatively, it might correspond to an outflow of ionized gas stemming from the radio galaxy. The outflow would be the highest redshift spatially resolved ionized outflow to date. The enormous amount of energy injected, however, appears to be unable to quench the host galaxy’s prodigious star formation, occurring at a rate of ∼4500 M ⊙yr−1, estimated using its far-infrared luminosity. Within the field, we also found two companion galaxies at projected distances of ∼25 and ∼60 kpc from the host, which suggests the host galaxy is harbored within a protocluster.

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“…On galactic scales (from a few kpc to a few tens of kpc) AGN jets have clearly shown to be able to compress, redistribute and even drive out of the host galaxy a considerable quantity of atomic, molecular and ionised gas (e.g. Miley et al 1981;Clark et al 1997;Wagner et al 2012;Morganti et al 2013;Santoro et al 2018;Mukherjee et al 2018;Zovaro et al 2019;Nesvadba et al 2021;Ruffa et al 2022;Murthy et al 2022;Capetti et al 2022). On larger, extragalactic scales (hundreds of kpc), jets have shown as well to be able to displace the surrounding thermal intragroup/intracluster medium (IGrM/ICM), creating cavities in its X-ray distribution, but also to induce turbulence, shocks and sound waves, and to uplift metal-rich gas from the system's most central regions (see McNamara & Nulsen 2007;Fabian 2012 for reviews).…”

Section: Introductionmentioning

confidence: 99%

AGN feedback in an infant galaxy cluster: the LOFAR-Chandra view of the giant FRII radio galaxy J103025+052430 at z=1.7

Brienza¹,

Prandoni²,

D'Amato³

et al. 2023

Preprint

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In the nearby universe jets from Active Galactic Nuclei (AGN) are observed to have a dramatic impact on their surrounding extragalactic environment. The effect of jets at high redshift (z>1.5) is instead much less constrained. However, studying their impact at the 'cosmic noon', the epoch when both star formation and AGN activity peak, is crucial to fully understand galaxy evolution.Here we present a study of the giant (∼750 kpc) radio galaxy 103025+052430 located at the centre of a protocluster at redshift z=1.7, with a focus on its interaction with the external medium. We present new LOFAR observations at 144 MHz, which we combine with VLA 1.4 GHz data and 0.5-7 keV Chandra archival data. The new radio map at 144 MHz confirms that the source has a complex morphology, which can possibly fit the 'hybrid morphology' radio galaxy classification. The large size of the source gave us the possibility to perform a resolved radio spectral index analysis, a very unique opportunity for a source at such high redshift. This reveals a tentative, unexpected, flattening of the radio spectral index at the edge of the backflow in the Western lobe, which might be indicating plasma compression. The spatial coincidence between this region and the thermal X-ray bubble C, suggests a causal connection between the two. Contrary to previous estimates for the bright X-ray component A, we find that inverse Compton scattering between the radio-emitting plasma of the Eastern lobe and the CMB photons can account for a large fraction (∼ 45%-80%) of its total 0.5-7 keV measured flux. Finally, the X-ray bubble C, which is consistent with a thermal origin, is found to be significantly overpressurised with respect to the ambient medium. This suggests that it will tend to expand and release its energy in the surroundings, contributing to the overall intracluster medium heating. Overall, 103025+052430 gives us the chance to investigate the interaction between AGN jets and the surrounding medium in a system that is likely the predecessor of the rich galaxy clusters we all well know at z=0.

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The MURALES survey

Cited by 10 publications

References 70 publications

Complex AGN feedback in the Teacup galaxy

Complex AGN feedback in the Teacup galaxy

An Extended Lyα Outflow from a Radio Galaxy at z = 3.7?

AGN feedback in an infant galaxy cluster: the LOFAR-Chandra view of the giant FRII radio galaxy J103025+052430 at z=1.7

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