Galaxy formation and evolution

Abstract:

Context. The spatial distribution of giant molecular clouds (GMCs) at sub-kiloparsec scales encodes information about cloud formation and evolution. However, we still lack a general quantitative characterisation of molecular gas structure at this scale. Aims. We aim to provide a quantitative description of molecular gas structure at 150–1000 pc for a typical star-forming main sequence galaxy. We analyse how GMCs cluster together and how CO emission is spatially correlated with bright GMCs using a sample of 8984 GMCs from 40 galaxies observed by PHANGS-ALMA. Methods. We homogenized our data to a common spatial resolution of 150 pc and a mass sensitivity of 2.5 M ⊙ pc −2 to remove observational bias. We then calculated the nearest neighbour distances, neighbour number density, and two-point correlation functions (2PCFs) for the catalogued GMCs in each galaxy. When analysing the 2PCFs, we generated several control samples that reflect different null hypotheses on large spatial scales. We stacked integrated intensity CO emission profiles around the position of catalogued GMCs to probe the gas distribution on scales between the observational resolution and the typical GMC-GMC spacing. Results. Our measurements of cloud spacing and the number of neighbours show that GMC clustering follows the large-scale gas distribution. Once we accounted for this contribution, the peak excess clustering relative to the null hypothesis in the 2PCF dropped from 1 + ω ∼ 2.3 to 1.3, with the power-law slope flattened from −0.25 to 0. Stacks of CO intensity around local maxima show a strong clustering signal on scales smaller than the typical GMC-GMC separation. We show that this is largely the same signal captured by the ‘GMC size’ measured by CPROPS , with an additional ∼20% of the flux in an extended component beyond 500 pc. We find that our stacked profiles can be fit with a double Gaussian function plus a constant offset. The broad Gaussian component accounts for 70% of the over-density power above the constant background and is stronger around massive and gravitationally bound GMCs. Conclusions. Our measurements yield a general statistical description of the structure of CO emission from ≈150 pc to galactic scales that can serve as a benchmark for simulations of molecular cloud formation and destruction in galaxy disks. Our results indicate that galactic structure exerts a strong influence on the GMC distribution in galaxy disks and that the formation of massive gravitationally bound GMCs is related to strong local gas clustering.

Abstract:

Abstract Blue asymmetries (“Blueshifts”) in the C iv 1550Å emission line are common in luminous quasars. If they are formed in winds, how much energy, momentum and mass do those winds transport? We address this question by considering how much mass must be supplied through the line-forming region to maintain a given density and ionization state. Using a combination of 1D analytic and 2D numerical models, we find that for blueshifted C iv lines to form in a wind, the wind must have mass outflow rates of ~50fV times the accretion rate, where fV ≤ 1 is the volume filling factor accounting for clumping. Our results therefore disfavour line formation in a smooth disc wind and point towards one of two scenarios: either the wind is clumpy, with required clumping factors suggestively close to those in hot star winds; alternatively, if the mass is instead swept up from the ambient medium, the wind need not be clumpy and MHD and radiative winds can provide the original source of momentum and energy. The power of the outflow depends on the square of the terminal velocity of the flow, v∞. If the wind is also the BAL outflow, with v∞ ~ 10, 000 km s−1, the wind power is significant and important for feedback. There are various caveats which moderate our conclusions, motivating i) a better theoretical understanding of wind driving and clump formation physics and ii) improved observational constraints on the physical conditions where the lines are formed.

Abstract:

Abstract Radio continuum surveys provide samples of active galactic nuclei (AGN) and star forming galaxies (SFGs) to high redshifts, free of biases due to dust obscuration. However, radio detected sources require multi-wavelength counterparts to understand their intrinsic properties (e.g. redshift, stellar mass) and to study the evolution of star formation and AGN activity. In this work we present host galaxy counterparts for the MeerKAT International GHz Tiered Extragalactic Exploration (MIGHTEE) survey continuum Data Release 1 in regions with the best ancillary data (totalling 7.5 sq. deg). We combine statistical cross-matching and visual inspection to identify Ks-band selected host galaxies, and additionally combine multiple radio components into single physical objects, where needed. This results in a combined radio catalogue of ~66 000 sources, with host counterparts and redshifts identified for ~95 per cent of sources in the COSMOS field, ~91 per cent in XMM-LSS and ~90 per cent in CDFS-DEEP. This includes a significant fraction of sources with spectroscopic redshifts within the COSMOS field (~50 per cent), with ~30 and ~20 per cent in the XMM-LSS and CDFS-DEEP fields respectively. Using the cross-matched catalogue, we make an initial identification of radio-excess and star forming galaxies based on comparisons of the radio luminosities to host star formation rates. Using this split as a proxy for radio loud AGN or SFGs, we present expectations for the redshift distributions of these sources, finding broad agreement with those from deep radio luminosity functions and simulated catalogues.