2019, Smirnova-Pinchukova, I., Husemann, B., Busch, G., Appleton, P., Bethermin, M., Combes, F., Croom, S., Davis, T.A., Fischer, C., Gaspari, M., Groves, B., Klein, R., O’Dea, C.P., Pérez-Torres, M., Scharwächter, J., Singha, M., Tremblay, G.R., Urrutia, T.

The [C ii]λ158 µm line is one of the strongest far-infrared (FIR) lines and an important coolant in the interstellar medium of galaxies that is accessible out to high redshifts. The excitation of [C ii] is complex and can best be studied in detail at low redshifts. Here we report the discovery of the highest global [C ii] excess with respect to the FIR luminosity in the nearby AGN host galaxy HE 1353−1917. This galaxy is exceptional among a sample of five targets because the AGN ionization cone and radio jet directly intercept the cold galactic disk. As a consequence, a massive multiphase gas outflow on kiloparsec scales is embedded in an extended narrow-line region. Because HE 1353−1917 is distinguished by these special properties from our four bright AGN, we propose that a global [C ii] excess in AGN host galaxies could be a direct signature of a multiphase AGN-driven outflow with a high mass-loading factor.

2023, Herenz, E.C., Inoue, J., Salas, H., Koenigs, B., Moya-Sierralta, C., Cannon, J.M., Hayes, M., Papaderos, P., Östlin, G., Bik, A., Le Reste, A., Kusakabe, H., Monreal-Ibero, A., Puschnig, J.

Context. Outflows from low-mass star-forming galaxies are a fundamental ingredient for models of galaxy evolution and cosmology. Despite seemingly favourable conditions for outflow formation in compact starbursting galaxies, convincing observational evidence for kiloparsec-scale outflows in such systems is scarce. Aims. The onset of kiloparsec-scale ionised filaments in the halo of the metal-poor compact dwarf SBS 0335-052E was previously not linked to an outflow. In this paper we investigate whether these filaments provide evidence for an outflow. Methods. We obtained new VLT/MUSE WFM and deep NRAO/VLA B-configuration 21 cm data of the galaxy. The MUSE data provide morphology, kinematics, and emission line ratios of Hβ/Hα and [O ¯III]λ5007/Hα of the low surface-brightness filaments, while the VLA data deliver morphology and kinematics of the neutral gas in and around the system. Both datasets are used in concert for comparisons between the ionised and the neutral phase. Results. We report the prolongation of a lacy filamentary ionised structure up to a projected distance of 16 kpc at SBHα = 1.5 - 10-18 erg s cm-2 arcsec-2. The filaments exhibit unusual low Hα/Hβ 2.4 and low [Oa ¯III]/Hα ∼ 0.4 - 0.6 typical of diffuse ionised gas. They are spectrally narrow (∼20 km s-1) and exhibit no velocity sub-structure. The filaments extend outwards from the elongated Ha ¯I halo. On small scales, the NHI peak is offset from the main star-forming sites. The morphology and kinematics of Ha ¯I and Ha ¯II reveal how star-formation-driven feedback interacts differently with the ionised and the neutral phase. Conclusions. We reason that the filaments are a large-scale manifestation of star-formation- driven feedback, namely limb-brightened edges of a giant outflow cone that protrudes through the halo of this gas-rich system. A simple toy model of such a conical structure is found to be commensurable with the observations.

2022, Yang, A.Y., Urquhart, J.S., Wyrowski, F., Thompson, M.A., König, C., Colombo, D., Menten, K.M., Duarte-Cabral, A., Schuller, F., Csengeri, T., Eden, D., Barnes, P., Traficante, A., Bronfman, L., Sanchez-Monge, A., Ginsburg, A., Cesaroni, R., Lee, M.-Y., Beuther, H., Medina, S.-N.X., Mazumdar, P., Henning, T.

Context. The formation processes of massive stars are still unclear, but a picture is emerging involving accretion disks and molecular outflows in what appears to be a scaled-up version of low-mass star formation. A census of outflow activity toward high-mass star-forming clumps in various evolutionary stages has the potential to shed light on high-mass star formation. Aims. We conducted an outflow survey toward ATLASGAL (APEX Telescope Large Area Survey of the Galaxy) clumps using SEDIGISM (structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium) data and aimed to obtain a large sample of clumps exhibiting outflow activity in different evolutionary stages. Methods. We identify the high-velocity wings of the 13CO lines, which indicate outflow activity, toward ATLASGAL clumps by (1) extracting the simultaneously observed 13CO (2-1) and C18O (2-1) spectra from SEDIGISM, and (2) subtracting Gaussian fits to the scaled C18O (core emission) from the 13CO line after considering opacity broadening. Results. We detected high-velocity gas toward 1192 clumps out of a total sample of 2052, corresponding to an overall detection rate of 58%. Outflow activity has been detected in the earliest (apparently) quiescent clumps (i.e., 70 μm weak) to the most evolved H » II region stages (i.e., 8 μm bright with tracers of massive star formation). The detection rate increases as a function of evolution (quiescent = 51%, protostellar = 47%, YSO = 57%, UC H » II regions = 76%). Conclusions. Our sample is the largest outflow sample identified so far. The high detection rate from this large sample is consistent with the results of similar studies reported in the literature and supports the scenario that outflows are a ubiquitous feature of high-mass star formation. The lower detection rate in early evolutionary stages may be due to the fact that outflows in the early stages are weak and difficult to detect. We obtain a statistically significant sample of outflow clumps for every evolutionary stage, especially for outflow clumps in the earliest stage (i.e., 70 μm dark). The detections of outflows in the 70 μm dark clumps suggest that the absence of 70 μm emission is not a robust indicator of starless and/or pre-stellar cores.