Physics of ULIRGs with MUSE and ALMA: The PUMA project

Perna, M.; Arribas, S.; Pereira-Santaella, M.; Colina, L.; Bellocchi, E.; Catalán-Torrecilla, C.; Cazzoli, S.; Gómez, A.; Maiolino, R.; López, Javier Piqueras; Pino, Bruno Rodríguez Del

doi:10.1051/0004-6361/202039702

Cited by 24 publications

(34 citation statements)

References 134 publications

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“…We have analyzed new high-resolution ALMA ∼220 GHz and CO(2-1) observations of a representative sample of 22 local ULIRGs (32 individual nuclei) as part of the Physics of ULIRGs with MUSE and ALMA (PUMA) project (see also Perna et al 2021). The main results of this work are the following:…”

Section: Discussionmentioning

confidence: 99%

“…( † ) For the 4 nuclei undetected in the ALMA images and the 2 systems (F12072-0444 and F13451+1232) not observed by ALMA, we used near-IR and optical HST images, whose astrometry was tied to Gaia DR2, to measure the nuclear position (see Sect. 3.1 of Perna et al 2021).…”

Section: Alma Observationsmentioning

confidence: 96%

“…4). In addition to our VLT/MUSE-AO optical integral field spectroscopy (Perna et al 2020(Perna et al , 2021, the majority of the targets have extensive ancillary multi-wavelength data which include mid-and far-IR (e.g., Veilleux et al 2009;Spoon et al 2013;Pearson et al 2016;Chu et al 2017), radio (e.g., Condon et al 1998;Helfand et al 2015), and X-ray (e.g., Iwasawa et al 2011) observations.…”

Section: Sample Of Local Ulirgsmentioning

confidence: 99%

“…4.3). (f) Nuclear activity classification based on optical spectroscopy (see Perna et al 2021). (g) System morphology: I. Interacting system with nuclear separation >1 kpc; M. Advanced merger with nuclear separation <1 kpc (see Perna et al 2021).…”

Section: Alma Observationsmentioning

confidence: 99%

“…To do so, we combine sub-kpc resolution optical MUSE and Band 6 (∼220 GHz) ALMA data to trace the multi-phase structure of the massive outflows as well as to investigate basic properties of the ULIRGs like their main power source. The first MUSE results on the spatially resolved stellar kinematics and the ionized outflow phase were presented by Perna et al (2021) while the detailed analysis of the Arp 220 MUSE data was presented in Perna et al (2020). Likewise, Pereira-Santaella et al (2018) presented the first ALMA results on the spatially resolved cold molecular outflows detected in three of these local ULIRGs.…”

Section: Introductionmentioning

confidence: 99%

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Are local ULIRGs powered by AGN? The sub-kpc view of the 220 GHz continuum. PUMA II

Pereira-Santaella,

Colina,

García-Burillo

et al. 2021

Preprint

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We analyze new high-resolution (400 pc) ∼220 GHz continuum and CO(2-1) ALMA observations of a representative sample of 22 local (z<0.165) ULIRG systems (32 individual nuclei) as part of the "Physics of ULIRGs with MUSE and ALMA" (PUMA) project. The deconvolved half-light radii of the ∼220 GHz continuum sources, r cont , are between <60 pc and 350 pc (median 80-100 pc). We associate these regions with the regions emitting the bulk of the infrared luminosity (L IR ). The good agreement, within a factor of 2, between the observed ∼220 GHz fluxes and the extrapolation of the infrared gray-body, and the small contributions from synchrotron and free-free emission support this assumption. The cold molecular gas emission sizes are between 60 and 700 pc and are, on average, ∼2.6 times larger than the continuum. Using these measurements, we derive the nuclear L IR and cold molecular gas surface densities (Σ L IR = 10 11.5 − 10 14.3 L kpc −2 and Σ H 2 = 10 2.9 − 10 4.2 M pc −2 , respectively). Assuming that the L IR is produced by star-formation, the median Σ L IR corresponds to Σ SFR = 2500 M yr −1 kpc −2 . This Σ SFR implies extremely short depletion times, Σ H 2 /Σ SFR <1-15 Myr, and unphysical star-formation efficiencies >1 for 70% of the sample. Therefore, this favors the presence of an obscured AGN in these objects that could dominate the L IR . We also classify the ULIRG nuclei in two groups: (a) compact nuclei (r cont <130 pc) with high mid-IR excess emission (∆L 6−20µm /L IR ) found in optically classified AGN; and (b) nuclei following a relation with decreasing ∆L 6−20µm /L IR for decreasing r cont . The majority, 65%, of the nuclei in interacting systems lie in the low-r cont end (<130 pc) of this relation, while only 25% of the mergers do so. This suggests that in the early stages of the interaction, the activity occurs in a very compact and dust-obscured region while, in more advanced merger stages, the activity is more extended, unless an optically detected AGN is present. Approximately two thirds of the nuclei have nuclear radiation pressures above the Eddington limit. This is consistent with the ubiquitous detection of massive outflows in local ULIRGs and supports the importance of the radiation pressure in the outflow launching process.

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Section: Discussionmentioning

confidence: 99%

Section: Alma Observationsmentioning

confidence: 96%

Section: Sample Of Local Ulirgsmentioning

confidence: 99%

Section: Alma Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Are local ULIRGs powered by AGN? The sub-kpc view of the 220 GHz continuum. PUMA II

Pereira-Santaella,

Colina,

García-Burillo

et al. 2021

Preprint

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show abstract

Physics of ULIRGs with MUSE and ALMA: The PUMA project

Pereira-Santaella

Colina

García‐Burillo

et al. 2021

A&A

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We analyze new high-resolution (400 pc) ∼220 GHz continuum and CO(2–1) Atacama Large Millimeter Array (ALMA) observations of a representative sample of 23 local (z < 0.165) ultra-luminous infrared systems (ULIRGs; 34 individual nuclei) as part of the “Physics of ULIRGs with MUSE and ALMA” (PUMA) project. The deconvolved half-light radii of the ∼220 GHz continuum sources, rcont, are between < 60 pc and 350 pc (median 80–100 pc). We associate these regions with the regions emitting the bulk of the infrared luminosity (LIR). The good agreement, within a factor of 2, between the observed ∼220 GHz fluxes and the extrapolation of the infrared gray-body as well as the small contributions from synchrotron and free–free emission support this assumption. The cold molecular gas emission sizes, rCO, are between 60 and 700 pc and are similar in advanced mergers and early interacting systems. On average, rCO are ∼2.5 times larger than rcont. Using these measurements, we derived the nuclear LIR and cold molecular gas surface densities (ΣLIR = 1011.5 − 1014.3 L⊙ kpc−2 and ΣH2 = 102.9 − 104.2 M⊙ pc−2, respectively). Assuming that the LIR is produced by star formation, the median ΣLIR corresponds to ΣSFR = 2500 M⊙ yr−1 kpc−2. This ΣSFR implies extremely short depletion times, ΣH2/ΣSFR < 1–15 Myr, and unphysical star formation efficiencies > 1 for 70% of the sample. Therefore, this favors the presence of an obscured active galactic nucleus (AGN) in these objects that could dominate the LIR. We also classify the ULIRG nuclei in two groups: (a) compact nuclei (rcont < 120 pc) with high mid-infrared excess emission (ΔL6−20 μm/LIR) found in optically classified AGN; and (b) nuclei following a relation with decreasing ΔL6−20 μm/LIR for decreasing rcont. The majority, 60%, of the nuclei in interacting systems lie in the low-rcont end (<120 pc) of this relation, while this is the case for only 30% of the mergers. This suggests that in the early stages of the interaction, the activity occurs in a very compact and dust-obscured region while, in more advanced merger stages, the activity is more extended, unless an optically detected AGN is present. Approximately two-thirds of the nuclei have nuclear radiation pressures above the Eddington limit. This is consistent with the ubiquitous detection of massive outflows in local ULIRGs and supports the importance of the radiation pressure in the outflow launching process.

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Capturing dual AGN activity and kiloparsec-scale outflows in IRAS 20210+1121

Saturni

Vietri

Piconcelli

et al. 2021

A&A

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The most standard scenario for the evolution of massive galaxies across cosmic time assumes a correspondence based on the interplay between active galactic nuclei (AGN) feedback, which injects large amounts of energy into the host environment, and galaxy mergers, with their ability to trigger massive star formation events and accretion onto supermassive black holes. Interacting systems hosting AGN are useful laboratories for obtaining key insights into both phenomena. In this context, we present an analysis of the optical spectral properties of IRAS 20210+1121 (I20210), a merging system at z = 0.056. According to X-ray data, this object comprises two interacting galaxies, each hosting an obscured AGN. The optical spectra confirm the presence of AGN features in both galaxies. In particular, we are able to provide a Seyfert classification for I20210 North. The spectrum of I20120 South shows broad blueshifted components associated with the most intense emission lines that indicate the presence of an ionized outflow, for which we derive a maximum velocity of ∼2000 km s−1, an extension of ∼2 kpc, and a mass rate of ∼0.6 M⊙ yr−1. We also report the existence of an ionized nebular component with v ∼ 1000 km s−1 at ∼6.5 kpc southwards of I20210 South, which can be interpreted as disrupted gas ejected from the host galaxy by the action of the outflow. I20120 therefore exhibits a double obscured AGN, with one of them showing evidence of ongoing events for AGN-powered outflows. Future spatially resolved spectroscopy will allow for an accurate mapping of the gas kinematics in this AGN pair and evaluate the impact of the outflow on both the interstellar medium and the galaxy environment.

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Physics of ULIRGs with MUSE and ALMA: The PUMA project

Cited by 24 publications

References 134 publications

Are local ULIRGs powered by AGN? The sub-kpc view of the 220 GHz continuum. PUMA II

Are local ULIRGs powered by AGN? The sub-kpc view of the 220 GHz continuum. PUMA II

Physics of ULIRGs with MUSE and ALMA: The PUMA project

Capturing dual AGN activity and kiloparsec-scale outflows in IRAS 20210+1121

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