Physics of ULIRGs with MUSE and ALMA: The PUMA project

Perna, M.; Arribas, S.; Colina, L.; Pereira-Santaella, M.; Lamperti, Isabella; Teodoro, Enrico M. Di; Übler, Hannah; Costantin, Luca; Maiolino, R.; Cresci, G.; Bellocchi, E.; Catalán-Torrecilla, C.; Cazzoli, S.; López, Javier Piqueras

doi:10.1051/0004-6361/202142659

Cited by 11 publications

(11 citation statements)

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“…In general, the gas in these field starbursts is slightly more turbulent than in main-sequence galaxies, showing a higher σ 0 , especially at 2 < z < 4. A similar trend of increasing σ 0 as galaxies move above the MS at a fixed stellar mass is shown for star-forming galaxies at z = 0 − 3 (e.g., Perna et al 2022;Wisnioski et al 2015), suggesting that mergers or interactions would increase gas σ 0 as they enhance star formation.…”

Section: The Two Sbs Have Dynamically Cold Gas-rich Disks With Low Ve...supporting

confidence: 61%

Starbursts with suppressed velocity dispersion revealed in a forming cluster at z = 2.51

Xiao

Wang

Elbaz

et al. 2022

A&A

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One of the most prominent features of galaxy clusters is the presence of a dominant population of massive ellipticals in their cores. Stellar archaeology suggests that these gigantic beasts assembled most of their stars in the early Universe via starbursts. However, the role of dense environments and their detailed physical mechanisms in triggering starburst activities remain unknown. Here we report spatially resolved Atacama Large Millimeter/submillimeter Array (ALMA) observations of the CO J = 3−2 emission line, with a resolution of about 2.5 kpc, toward a forming galaxy cluster core with starburst galaxies at z = 2.51. In contrast to starburst galaxies in the field often associated with galaxy mergers or highly turbulent gaseous disks, our observations show that the two starbursts in the cluster exhibit dynamically cold (rotation-dominated) gas-rich disks. Their gas disks have extremely low velocity dispersion (σ0 ∼ 20−30 km s−1), which is three times lower than their field counterparts at similar redshifts. The high gas fraction and suppressed velocity dispersion yield gravitationally unstable gas disks, which enables highly efficient star formation. The suppressed velocity dispersion, likely induced by the accretion of corotating and coplanar cold gas, might serve as an essential avenue to trigger starbursts in massive halos at high redshifts.

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Section: The Two Sbs Have Dynamically Cold Gas-rich Disks With Low Ve...supporting

confidence: 61%

Starbursts with suppressed velocity dispersion revealed in a forming cluster at z = 2.51

Xiao

Wang

Elbaz

et al. 2022

A&A

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“…The grey contours on the moment 1 maps are every 50 km s −1 (every 25 km s −1 if the maximum value < 100 km s −1 ), and every 25 km s −1 (every 15 km s −1 if the maximum value < 150 km s −1 ) on the moment 2 map. In black are the CO(2-1) moment 0 contours ([3, 6, 25, 50, 75] tent with what observed in non-interacting galaxies (see Perna et al 2022). We identify only six outliers with PA differences 20 • (01572+0009, 07251-0248 E, 09022-3615,14348-1447 SW, 16090-0139, and 17208-0014).…”

Section: Comparison Of Position Angles Of the Molecular Gas Stellar A...mentioning

confidence: 55%

“…We obtain the PA of the major axis on the receding half of the galaxy, measured east of north (anticlockwise). We compare these PAs with the ones of the stellar and ionised gas (traced by Hα) disks presented in Perna et al (2022). Figure 5 shows the absolute differences between PA(CO) and the PA derived from the stellar and ionised gas kinematics.…”

Section: Comparison Of Position Angles Of the Molecular Gas Stellar A...mentioning

confidence: 99%

“…A detailed analysis of the MUSE data for Arp 220 has been presented in Perna et al (2020). Perna et al (2022) studied the properties and incidence of the ionised gas disks in the PUMA ULIRGs, the associated velocity dispersion and its relation with the offset from the main sequence. Pereira-Santaella et al (2021) analysed the ALMA 220 GHz continuum and provided evidence for the ubiquitous presence of deeply obscured AGN in ULIRGs, which could substantially contribute to their IR emission.…”

Section: Introductionmentioning

confidence: 99%

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Physics of ULIRGs with MUSE and ALMA: The PUMA project

Lamperti

Pereira-Santaella

Perna

et al. 2022

A&A

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We study molecular outflows in a sample of 25 nearby (z < 0.17, d < 750 Mpc) ultra-luminous infrared galaxy (ULIRG) systems (38 individual nuclei) as part of the Physics of ULIRGs with MUSE and ALMA (PUMA) survey, using ∼ 400 pc (0.1-1.0" beam FWHM) resolution ALMA CO(2-1) observations. We used a spectro-astrometry analysis to identify high-velocity (> 300 km s −1 ) molecular gas disconnected from the galaxy rotation, which we attribute to outflows. In 77% of the 26 nuclei with log L IR /L > 11.8, we identified molecular outflows with an average v out = 490 km s −1 , outflow masses 1 − 35 × 10 7 M , mass outflow rates Ṁout = 6 − 300 M yr −1 , mass-loading factors η = Ṁout /S FR = 0.1−1, and an average outflow mass escape fraction of 45±6%. The majority of these outflows (18/20) are spatially resolved with radii of 0.2 − 0.9 kpc and have short dynamical times (t dyn = R out /v out ) in the range 0.5 − 2.8 Myr. The outflow detection rate is higher in nuclei dominated by starbursts (SBs, 14/15 = 93%) than in active galactic nuclei (AGN, 6/11 = 55%). Outflows perpendicular to the kinematic major axis are mainly found in interacting SBs. We also find that our sample does not follow the Ṁout versus AGN luminosity relation reported in previous works. In our analysis, we include a sample of nearby main-sequence galaxies (SFR = 0.3 − 17 M yr −1 ) with detected molecular outflows from the PHANGS-ALMA survey to increase the L IR dynamic range. Using these two samples, we find a correlation between the outflow velocity and the star-formation rate (SFR), as traced by L IR (v out ∝ S FR 0.25±0.01 ), which is consistent with what was found for the atomic ionised and neutral phases. Using this correlation, and the relation between M out /R out and v out , we conclude that these outflows are likely momentum-driven. Finally, we compare the CO outflow velocities with the ones derived from the OH 119µm doublet. In 76% of the targets, the outflow is detected in both CO and OH, while in three targets (18%) the outflow is only detected in CO, and in one target the outflow is detected in OH but not in CO. The difference between the OH and CO outflow velocities could be due to the far-IR background source required by the OH absorption which makes these observations more dependent on the specific outflow geometry.

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“…Some authors (e.g Perna et al 2022. and references therein) use the inclination-corrected velocity to calculate the dynamical ratio.…”

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confidence: 99%

Unexplored outflows in nearby low luminosity AGNs

Cazzoli

Hermosa-Muñoz

Márquez

et al. 2022

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Context. Multi-phase outflows play a central role in galaxy evolution shaping the properties of galaxies. Understanding outflows and their effects in low luminosity active galactic nuclei (AGNs), such as low ionisation nuclear emission line regions (LINERs), is essential. LINERs bridge the gap between normal and active galaxies, being the most numerous AGN population in the local Universe. Aims. Our goal is to analyse the kinematics and ionisation mechanisms of the multi-phase gas of NGC 1052, the prototypical LINER, in order to detect and map the ionised and neutral phases of the putative outflow. Methods. We obtained Very Large Telescope MUSE and Gran Telescopio Canarias MEGARA optical integral field spectroscopy data for NGC 1052. In addition to stellar kinematics maps, by modelling spectral lines with multiple Gaussian components, we obtained flux, kinematic, and excitation maps of both ionised and neutral gas. Results. The stars are distributed in a dynamically hot disc (V/σ ∼ 1.2), with a centrally peaked velocity dispersion map (σc = 201 ± 10 km s−1) and large observed velocity amplitudes (ΔV = 167 ± 19 km s−1). The ionised gas, probed by the primary component is detected up to ∼30″ (∼3.3 kpc) mostly in the polar direction with blue and red velocities (∣V∣ < 250 km s−1). The velocity dispersion map shows a notable enhancement (σ > 90 km s−1) crossing the galaxy along the major axis of rotation in the central 10″. The secondary component has a bipolar morphology, velocity dispersion larger than 150 km s−1, and velocities up to 660 km s−1. A third component is detected with MUSE (and barely with MEGARA), but it is not spatially resolved. The broad-line region (BLR) component (used to model the broad Hα emission only) has a full width at half maximum of 2427 ± 332 and 2350 ± 470 km s−1 for MUSE and MEGARA data, respectively. The maps of the NaD absorption indicate optically thick neutral gas with complex kinematics. The velocity field is consistent with a slow rotating disc (ΔV = 77 ± 12 km s−1), but the velocity dispersion map is off-centred without any counterpart in the (centrally peaked) flux map. Conclusions. We found evidence of an ionised gas outflow (secondary component) with a mass of 1.6 ± 0.6 × 105 M⊙, and mass rate of 0.4 ± 0.2 M⊙ yr−1. The outflow is propagating in a cocoon of gas with enhanced turbulence and might be triggering the onset of kiloparsec-scale buoyant bubbles (polar emission), both probed by the primary component. Taking into account the energy and kinetic power of the outflow (1.3 ± 0.9 × 1053 erg and 8.8 ± 3.5 × 1040 erg s−1, respectively) as well as its alignment with both the jet and the cocoon, and that the gas is collisionally ionised (due to gas compression), we consider that the most likely power source of the outflow is the jet, although some contribution from the AGN is possible. The hints of the presence of a neutral gas outflow are weak.

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Physics of ULIRGs with MUSE and ALMA: The PUMA project

Cited by 11 publications

References 91 publications

Starbursts with suppressed velocity dispersion revealed in a forming cluster at z = 2.51

Starbursts with suppressed velocity dispersion revealed in a forming cluster at z = 2.51

Physics of ULIRGs with MUSE and ALMA: The PUMA project

Unexplored outflows in nearby low luminosity AGNs

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