The Close AGN Reference Survey (CARS)

Smirnova-Pinchukova, I.; Busch, G.; Appleton, P. N.; Béthermin, M.; Combes, F.; Croom, S. M.; Davis, Timothy A.; Fischer, C.; Gaspari, M.; Groves, Brent; Klein, Randolf; O’Dea, C. P.; Pérez-Torres, M. Á.; Scharwächter, J.; Singha, M.; Tremblay, G. R.; Urrutia, T.

doi:10.1051/0004-6361/201935577

Cited by 14 publications

(11 citation statements)

References 41 publications

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“…However, for the case of [C II], the discrepancy is mainly driven by LARS 5, a galaxy that is known to have a large scale outflow (Duval et al 2016). Our finding is thus in agreement with other studies (Appleton et al 2013(Appleton et al , 2018Smirnova-Pinchukova et al 2019) that reported on excess [C II]158 µm emission due to shocks connected to out flowing gas. Excluding LARS 5, the [C II] prescription of De Looze et al (2014) leads to SFRs that are only ∼80% higher.…”

Section: Metallicity-dependent Co-to-h 2 Conversionsupporting

confidence: 94%

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The Lyman Alpha Reference Sample

Puschnig

Hayes

Östlin

et al. 2020

A&A

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Context. Lyman-α (Lyα) is the brightest emission line in star-forming galaxies. However, its interpretation in terms of physical properties is hampered by the resonant nature of Lyα photons. In order to remedy this complicated situation, the Lyman Alpha Reference Sample (LARS) was defined, enabling the study of Lyα production and escape mechanisms in 14 local star-forming galaxies. Aims. With this paper, we complement our efforts and study the global dust and (molecular) gas content as well as the properties of gas associated with photon-dominated regions. We aim to characterize the interstellar medium of LARS galaxies, allowing us to relate these newly derived properties to quantities relevant for Lyα escape. Methods. We observed LARS galaxies with Herschel, SOFIA, the IRAM 30m telescope, and APEX, targeting far-infrared (FIR) continuum and emission lines of [C II]158 μm, [O I]63 μm, [O III]88 μm, and low-J CO lines. Using Bayesian methods we derived dust model parameters and estimated the 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 μm, and [O I]63 μm luminosities. Results. LARS covers a wide dynamic range in the derived properties, with FIR-based star formation rates from ∼0.5−100 M⊙ yr−1, gas fractions between ∼15−80%, and gas depletion times ranging from a few hundred megayears up to more than ten gigayears. The distribution of LARS galaxies in the Σgas versus ΣSFR (Kennicutt–Schmidt plane) is thus quite heterogeneous. However, we find that LARS galaxies with the longest gas depletion times, that is, relatively high gas surface densities (Σgas) and low star formation rate densities (ΣSFR), have by far the highest Lyα escape fraction. A strong approximately linear relation is found between the Lyα escape fraction and the total gas (HI+H2) depletion time. We argue that the Lyα escape in those galaxies is driven by turbulence in the star-forming gas that shifts the Lyα photons out of resonance close to the places where they originate. We further report on an extreme [C II]158 μm excess in LARS 5, corresponding to ∼14 ± 3% of the FIR luminosity, which probably is the most extreme [C II]-to-FIR ratio observed in a galaxy (without active nucleus) to date.

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Section: Metallicity-dependent Co-to-h 2 Conversionsupporting

confidence: 94%

“…4 and 6. We note that shock-enhanced [C II]158 µm excess was previously observed in other galaxies with outflows (Appleton et al 2013(Appleton et al , 2018Smirnova-Pinchukova et al 2019).…”

Section: Extreme [C Ii]158 µM Line Strength In Lars 5 and Basic Pdr A...supporting

confidence: 73%

The Lyman Alpha Reference Sample

Puschnig

Hayes

Östlin

et al. 2020

A&A

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“…There is thus a mild average [CII] excess in the most luminous sources of our sample. Even if it is rare, [CII]-excesses have been observed in the local Universe (Smirnova-Pinchukova et al 2019), but we usually observe a deficit in bright sources (Díaz-Santos et al 2013). This apparent [CII] excess could also be an SED effect.…”

Section: Obscured Sfr As a Function Of [Cii] Luminositymentioning

confidence: 68%

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

Bethermin,

Fudamoto,

Ginolfi

et al. 2020

Preprint

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The ALPINE-ALMA large program targets the [CII] 158 µm line and the far-infrared continuum in 118 spectroscopically confirmed star-forming galaxies between z=4.4 and z=5.9. It represents the first large [CII] statistical sample built in this redshift range. We present details of 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, 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 4.4×10 11 L . We also detected 57 additional continuum sources in our ALMA pointings. They are at lower redshift than the ALPINE targets, with a mean photometric redshift of 2.5±0.2. We measured the 850 µm number counts between 0.35 and 3.5 mJy, 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 0.35 mJy. Finally, we detected the [CII] line in 75 of our targets. Their median [CII] luminosity is 4.8×10 8 L and their median full width at half maximum is 252 km/s. After measuring the mean obscured SFR in various [CII] luminosity bins by stacking ALPINE continuum data, we find a good agreement between our data and the local and predicted SFR-L [CII] relations of De Looze et al. (2014) and Lagache et al. (2018).

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“…Evidence of excess C + with respect to the maximum line cooling efficiency expected from pure photo-dissociation regions has been seen in purely star-forming galaxies at z 1-2 (Brisbin et al 2015). In the local Universe, Seyfert galaxies hosting powerful AGNdriven radio jets and winds inject turbulence into the surrounding ISM, contributing to the excitation of a larger mass of the C + reservoir (Guillard et al 2015;Appleton et al 2018;Smirnova-Pinchukova et al 2019) (in contrast with the depletion scenario based on ionization described above, from Langer & Pineda 2015). In addition, low velocity shocks driven by galaxy collisions can also turbulently heat the gas on large scales in dense environments (Appleton et al 2013(Appleton et al , 2017.…”

Section: What Emission Is the Smbh In Extremely Luminous Hotmentioning

confidence: 99%

Kinematics and Star Formation of High-Redshift Hot Dust-Obscured Quasars as Seen by ALMA

Diaz-Santos,

Assef,

Eisenhardt

et al. 2021

Preprint

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Hot, dust-obscured galaxies (Hot DOGs) are a population of hyper-luminous obscured quasars identified by WISE. We present ALMA observations of the [C ii] 158 µm fine-structure line and underlying dust continuum emission in a sample of seven of the most extremely luminous (EL; L bol ≥ 10 14 L ) Hot DOGs, at redshifts z 3.0-4.6. The [C ii] 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, [C ii] is red-shifted by 780 km s −1 from rest-frame ultraviolet emission lines. EL Hot DOGs exhibit consistently very high ionized gas surface densities, with Σ [CII] 1-2 × 10 9 L 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 [C ii] 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 [C ii] 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 [CII] 500 km s −1 , 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. The dynamical friction from the frequent in-fall of nearby galaxies and gas clumps, together with the subsequent quasar feedback, would contribute to the high turbulence of the gas within the host in a self-sustaining process that could potentially trigger not only a single, continuous EL event, but instead a number of recurrent shorter-lived episodes as long as external accretion continues.

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The Close AGN Reference Survey (CARS)

Cited by 14 publications

References 41 publications

The Lyman Alpha Reference Sample

The Lyman Alpha Reference Sample

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

Kinematics and Star Formation of High-Redshift Hot Dust-Obscured Quasars as Seen by ALMA

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