The Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [C II] at Early times (ALPINE) targets the [C II] 158 μm line and the far-infrared continuum in 118 spectroscopically confirmed star-forming galaxies between z = 44 and z = 59 It represents the first large [C II] statistical sample built in this redshift range We present details regarding the data processing and the construction of the catalogs We detected 23 of our targets in the continuum To derive accurate infrared luminosities and obscured star formation rates (SFRs), we measured the conversion factor from the ALMA 158 μm rest-frame dust continuum luminosity to the total infrared luminosity (L_(IR)) after constraining the dust spectral energy distribution by stacking a photometric sample similar to ALPINE in ancillary single-dish far-infrared data We found that our continuum detections have a median L_(IR) of 44 × 10¹¹ L_⊙ We also detected 57 additional continuum sources in our ALMA pointings They are at a lower redshift than the ALPINE targets, with a mean photometric redshift of 25 ± 02 We measured the 850 μm number counts between 035 and 35 mJy, thus improving the current interferometric constraints in this flux density range We found a slope break in the number counts around 3 mJy with a shallower slope below this value More than 40% of the cosmic infrared background is emitted by sources brighter than 035 mJy Finally, we detected the [C II] line in 75 of our targets Their median [C II] luminosity is 48 × 10⁸ L_⊙ and their median full width at half maximum is 252 km s⁻¹ After measuring the mean obscured SFR in various [C II] luminosity bins by stacking ALPINE continuum data, we find a good agreement between our data and the local and predicted SFR–L_([C II]) relations

/pdf/the-alpine-alma-cii-survey-data-processing-catalogs-and-4cetc2skf0.pdf

The ALPINE-ALMA [CII] survey: data processing, catalogs, and statistical source properties

We study the global dust and (molecular) gas content in the Lyman Alpha Reference Sample (LARS), i.e. 14 local star-forming galaxies. We characterize their interstellar medium and relate newly derived properties to quantities relevant for Ly$\alpha$ escape. We observed LARS galaxies with Herschel/PACS, SOFIA/FIFI-LS, the IRAM 30m telescope and APEX, targeting far-infrared (FIR) continuum and emission lines of [C II]158$\mu$m, [O I]63$\mu$m, [O III]88$\mu$m and low-J CO lines. Using Bayesian methods we derive dust model parameters and estimate total gas masses for all LARS galaxies, taking into account a metallicity-dependent gas-to-dust ratio. Star formation rates were estimated from FIR, [C II]158$\mu$m and [O I]63$\mu$m luminosities. LARS covers a wide dynamic range in the derived properties, with FIR-based star formation rates from $\sim$0.5-100 $M_{\odot}\ yr^{-1}$, gas fractions between $\sim$15-80% and gas depletion times ranging from a few hundred Myr up to more than 10 Gyr. The distribution of LARS galaxies in the $\Sigma_{gas}$ vs. $\Sigma_{SFR}$ (Kennicutt-Schmidt plane) is thus quite heterogeneous. However, we find that LARS galaxies with the longest gas depletion times, i.e. relatively high gas surface densities ($\Sigma_{gas}$) and low star formation rate densities ($\Sigma_{SFR}$), have by far the highest Ly$\alpha$ escape fraction. A strong $\sim$linear relation is found between Ly$\alpha$ escape fraction and the total gas (HI+H$_2$) depletion time. We argue that the Ly$\alpha$ escape in those galaxies is driven by turbulence in the star-forming gas that shifts the Ly$\alpha$ photons out of resonance close to the places where they originate. We further report on an extreme [C II]158$\mu$m excess in LARS 5, corresponding to $\sim$14$\pm$3% of the FIR luminosity, i.e. the most extreme [C II]-to-FIR ratio observed in a non-AGN galaxy to date.

The Lyman Alpha Reference Sample XI: Efficient Turbulence Driven Ly{\alpha} Escape and the Analysis of IR, CO and [C II]158 {\mu}m

Hot, dust-obscured galaxies (Hot DOGs) are a population of hyper-luminous obscured quasars identified by WISE. We present ALMA observations of the [CII] fine-structure line and underlying dust continuum emission in a sample of seven of the most extremely luminous (EL; L_bol >= 10^14 L_sun) Hot DOGs, at redshifts z ~ 3.0-4.6. The [CII] line is robustly detected in four objects, tentatively in one, and likely red-shifted out of the spectral window in the remaining two based on additional data. On average, [CII] is red-shifted by ~ 780 km/s from rest-frame ultraviolet emission lines. EL Hot DOGs exhibit consistently very high ionized gas surface densities, with Sigma_[CII] ~ 1-2 x 10^9 L_sun/kpc^2; as high as the most extreme cases seen in other high-redshift quasars. As a population, EL Hot DOG hosts seem to be roughly centered on the main-sequence of star forming galaxies, but the uncertainties are substantial and individual sources can fall above and below. The average, intrinsic [CII] and dust continuum sizes (FWHMs) are ~ 2.1 kpc and ~ 1.6 kpc, respectively, with a very narrow range of line-to-continuum size ratios, 1.61 +/- 0.10, suggesting they could be linearly proportional. The [CII] velocity fields of EL Hot DOGs are diverse: from barely rotating structures, to resolved hosts with ordered, circular motions, to complex, disturbed systems that are likely the result of ongoing mergers. In contrast, all sources display large line-velocity dispersions, FWHM >~ 500 km/s, which on average are larger than optically and IR-selected quasars at similar or higher redshifts. We argue that a possible hypothesis for the lack of a common velocity structure, the systematically large dispersion of the ionized gas, and the presence of nearby companion galaxies may be that, rather than a continuous single event, the EL Hot DOG phase could be recurrent.

Kinematics and star formation of high-redshift hot dust-obscured quasars as seen by ALMA

There are only ﬁve radio-loud quasars currently known within 1 Gyr from the Big Bang ( z > 6 ) and the properties of their host galaxies have not been explored in detail. We present a NOrthern Extended Millimeter Array (NOEMA) survey of [CII] (158 µ m) and underlying continuum emission of four z > 6 radio-loud quasars, revealing their diverse properties. J0309+2717 ( z = 6 . 10 ) has a bright [CII] line and underlying continuum, implying a starburst with a star-formation rate SFR=340–1200 M (cid:12) yr − 1 . J1429+5447 ( z = 6 . 18 ) has a SFR= 520 − 870 M (cid:12) yr − 1 and its [CII] proﬁle is consistent with two Gaussians, which could be interpreted as a galaxy merger. J1427+3312 ( z = 6 . 12 ) has a moderate SFR = 30–90 M (cid:12) yr − 1 . Notably, this is a broad absorption line quasar and we searched for the presence of high-velocity outﬂows in the host galaxy. Although the NOEMA data reveal a tentative broad component of the [CII] line as wide as ∼ 1400 km s − 1 , the sensitivity of our current data is not suﬃcient to conﬁrm it. Finally, P172+18 ( z = 6 . 82 ) is undetected in both [CII] and continuum, implying a SFR < 22 − 40 M (cid:12) yr − 1 . The broad range of SFRs is similar to what is observed in radio-quiet quasars at similar redshifts. If radio jets do not signiﬁcantly contribute to both [CII] and IR luminosities, this suggest no feedback from the jet on the star formation in the host galaxy.

/pdf/the-cii-and-fir-properties-of-z-6-radio-loud-quasars-1cpkpb6l.pdf

The [CII] and FIR properties of z>6 radio-loud quasars

We present a spatially-resolved study of the ionised gas in the central 2 kpc of the Seyfert 2 galaxy NGC 2110 and investigate the role of its moderate luminosity radio jet (kinetic radio power of $P_\mathrm{jet} = 2.3 \times 10^{43}\mathrm{erg\ s^{-1}}$). We use new optical integral-field observations taken with the MEGARA spectrograph at GTC. We fit the emission lines with a maximum of two Gaussian components, except at the AGN position where we used three. Aided by existing stellar kinematics, we use the observed velocity and velocity dispersion of the emission lines to classify the different kinematic components. The disc component is characterised by lines with $\sigma \sim 60-200\ \mathrm{km\ s^{-1}}$. The outflow component has typical values of $\sigma \sim 700\ \mathrm{km\ s^{-1}}$ and is confined to the central 400 pc, which is coincident with linear part of the radio jet detected in NGC 2110. At the AGN position, the [O III]$\lambda$5007 line shows high velocity components reaching at least $1000\ \mathrm{km\ s^{-1}}$. This and the high velocity dispersions indicate the presence of outflowing gas outside the galaxy plane. Spatially-resolved diagnostic diagrams reveal mostly LI(N)ER-like excitation in the outflow and some regions in the disc, which could be due to the presence of shocks. However, there is also Seyfert-like excitation beyond the bending of the radio jet, probably tracing the edge of the ionisation cone that intercepts with the disc of the galaxy. NGC 2110 follows well the observational trends between the outflow properties and the jet radio power found for a few nearby Seyfert galaxies. All these pieces of information suggest that part of observed ionised outflow in NGC 2110 might be driven by the radio jet. However, the radio jet was bent at radial distances of 200 pc (in projection) from the AGN, and beyond there, most of the gas in the galaxy disc is rotating.

A radio-jet-driven outflow in the Seyfert 2 galaxy NGC 2110?

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.

/pdf/the-close-agn-reference-survey-cars-discovery-of-a-global-c-zttob1k3xp.pdf

The Close AGN Reference Survey (CARS). Discovery of a global [C II] 158 μm line excess in AGN HE 1353-1917

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The Close AGN Reference Survey (CARS). Discovery of a global [C II] 158 μm line excess in AGN HE 1353-1917