S. Carniani

The multi-phase winds of Markarian 231: from the hot, nuclear, ultra-fast wind to the galaxy-scale, molecular outflow

Mrk 231 is a nearby ultra-luminous IR galaxy exhibiting a kpc-scale, multi-phase AGN-driven outflow. This galaxy represents the best target to investigate in detail the morphology and energetics of powerful outflows, as well as their still poorly-understood expansion mechanism and impact on the host galaxy. In this work, we present the best sensitivity and angular resolution maps of the molecular disk and outflow of Mrk 231, as traced by CO(2−1) and (3−2) observations obtained with the IRAM/PdBI. In addition, we analyze archival deep Chandra and NuSTAR X-ray observations. We use this unprecedented combination of multi-wavelength data sets to constrain the physical properties of both the molecular disk and outflow, the presence of a highly-ionized ultra-fast nuclear wind, and their connection. The molecular CO(2−1) outflow has a size of ~1 kpc, and extends in all directions around the nucleus, being more prominent along the south-west to north-east direction, suggesting a wide-angle biconical geometry. The maximum projected velocity of the outflow is nearly constant out to ~1 kpc, thus implying that the density of the outflowing material must decrease from the nucleus outwards as ~r-2. This suggests that either a large part of the gas leaves the flow during its expansion or that the bulk of the outflow has not yet reached out to ~1 kpc, thus implying a limit on its age of ~1 Myr. Mapping the mass and energy rates of the molecular outflow yields OF = [500−1000] M⊙ yr-1 and Ėkin,OF = [7−10] × 10^(43) erg s^(-1). The total kinetic energy of the outflow is Ekin,OF is of the same order of the total energy of the molecular disk, Edisk. Remarkably, our analysis of the X-ray data reveals a nuclear ultra-fast outflow (UFO) with velocity −20 000 km s^(-1), UFO = [0.3−2.1] M_⊙ yr^(-1), and momentum load UFO/ rad = [0.2−1.6]. We find Ėkin,UFO ~ Ėkin,OF as predicted for outflows undergoing an energy conserving expansion. This suggests that most of the UFO kinetic energy is transferred to mechanical energy of the kpc-scale outflow, strongly supporting that the energy released during accretion of matter onto super-massive black holes is the ultimate driver of giant massive outflows. The momentum flux OF derived for the large scale outflows in Mrk 231 enables us to estimate a momentum boost OF/ UFO ≈ [30−60]. The ratios Ėkin,UFO/Lbol,AGN = [1−5] % and Ėkin,OF/Lbol,AGN = [1−3] % agree with the requirements of the most popular models of AGN feedback.

The assembly of ‘normal’ galaxies at z ∼ 7 probed by ALMA

We report new deep observations obtained with the Atacama Large Millimetre Array (ALMA) aimed at investigating the (C II)158µm line and continuum emission in three spectroscopically confirmedLymanbreakgalaxiesat6.8 <z ≤7.1,i.e.wellwithinthere-ionizationepoch.With star formation rates of SFR ∼ 5-15Myr −1 these systems are much more representative of thehigh-zgalaxypopulationthanothersystemstargetedinthepastbymillimetreobservations. For the galaxy with the deepest observation we detect (C II) emission at redshift z = 7.107, fully consistent with the Ly α redshift, but spatially offset by 0.7arcsec (4 kpc) from the optical emission. At the location of the optical emission, tracing both the Ly α line and the far-UV continuum, no (C II) emission is detected in any of the three galaxies, with 3σ upper limits significantly lower than the (C II) emission observed in lower redshift galaxies. These results suggest that molecular clouds in the central parts of primordial galaxies are rapidly disrupted by stellar feedback. As a result, (C II) emission mostly arises from more external accreting/satelliteclumpsofneutralgas.Thesefindingsareinagreementwithrecentmodelsof galaxy formation. Thermal far-infrared continuum is not detected in any of the three galaxies. However, the upper limits on the infrared-to-UV emission ratio do not exceed those derived in metal- and dust-poor galaxies.

Ionised outflows in z ~ 2.4 quasar host galaxies

AGN-driven outflows are invoked by galaxy evolutionary models to quench star formation and to explain the origin of the relations observed locally between super massive black holes and their host galaxies. This work aims to detect the presence of extended ionised outflows in luminous quasars where we expect the maximum activity both in star formation and in black hole accretion. Currently, there are only a few studies based on spatially resolved observations of outflows at high redshift,

ALMA constraints on the faint millimetre source number counts and their contribution to the cosmic infrared background

z>2

AGN wind scaling relations and the co-evolution of black holes and galaxies

. We analyse a sample of six luminous (

Star formation inside a galactic outflow

{\rm L>10^{47} \ erg/s}

Tracing the reionization epoch with ALMA: [CII] emission in z~7 galaxies

) quasars at

Tracing outflows in the AGN forbidden region with SINFONI

z\sim2.4

Quasar outflows at z ≥ 6: the impact on the host galaxies

, observed in H-band using the near-IR integral field spectrometer SINFONI at VLT. We perform a kinematic analysis of the [OIII] emission line at

Molecular gas on large circumgalactic scales at z=3.47

\lambda = 5007\AA