Ram-pressure feeding of supermassive black holes

Poggianti, Bianca M.; Jaffé, Yara L.; Moretti, Alessia; Gullieuszik, Marco; Radovich, M.; Tonnesen, Stephanie; Fritz, J.; Bettoni, D.; Vulcani, Benedetta; Fasano, G.; Bellhouse, Callum; Hau, G. K. T.; Omizzolo, A.

doi:10.1038/nature23462

Cited by 141 publications

(174 citation statements)

References 49 publications

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“…We have classified it as a jellyfish galaxy, as its Hα emitting tail (extending out to at least ∼ 35 kpc) is longer than the stellar disk extension. Among the GASP targeted galaxies, most of those exhibiting such long tails also possess a central AGN (Poggianti et al 2017b), as does JW100 (see also Radovich et al 2019).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

GASP. XXII. The Molecular Gas Content of the JW100 Jellyfish Galaxy at z ∼ 0.05: Does Ram Pressure Promote Molecular Gas Formation?

Moretti

Paladino

Poggianti

et al. 2020

ApJ

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Within the GASP survey, aimed at studying the effect of the ram-pressure stripping on the star formation quenching in cluster galaxies, we analyze here ALMA observations of the jellyfish galaxy JW100. We find an unexpected large amount of molecular gas (∼ 2.5 × 10 10 M ), 30% of which is located in the stripped gas tail out to ∼35 kpc from the galaxy center. The overall kinematics of molecular gas is similar to the one shown by the ionized gas, but for clear signatures of double components along the stripping direction detected only out to 2 kpc from the disk. The line ratio r 21 has a clumpy distribution and in the tail can reach large values (≥ 1), while its average value is low (0.58 with a 0.15 dispersion). All these evidence strongly suggest that the molecular gas in the tail is newly born from stripped HI gas or newly condensed from stripped diffuse molecular gas. The analysis of interferometric data at different scales reveals that a significant fraction (∼ 40%) of the molecular gas is extended over large scales (≥ 8 kpc) in the disk, and this fraction becomes predominant in the tail (∼ 70%). By comparing the molecular gas surface density with the star formation rate surface density derived from the Hα emission from MUSE data, we find that the depletion time on 1 kpc scale is particularly large (5 − 10 Gyr) both within the ram-pressure disturbed region in the stellar disk, and in the complexes along the tail.

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Section: Observations and Data Reductionmentioning

confidence: 99%

GASP. XXII. The Molecular Gas Content of the JW100 Jellyfish Galaxy at z ∼ 0.05: Does Ram Pressure Promote Molecular Gas Formation?

Moretti

Paladino

Poggianti

et al. 2020

ApJ

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“…3 The stellar and ionized gas kinematics obtained with MUSE were presented in Poggianti et al (2017a) and a visual 3D representation can be seen at https://web.oapd.inaf.it/gasp/jw100.html. JW100 hosts a central AGN (Seyfert2), that is detectable both in X-ray (Wong et al 2008) and from MUSE emission-line ratios (Poggianti et al 2017a, see also ESO press release #1725 https://www.eso.org/public/news/eso1725/).…”

Section: Introductionmentioning

confidence: 99%

GASP XXIII: A Jellyfish Galaxy as an Astrophysical Laboratory of the Baryonic Cycle

Poggianti

Ignesti

Gitti

et al. 2019

ApJ

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107

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With MUSE, Chandra, VLA, ALMA and UVIT data from the GASP programme we study the multiphase baryonic components in a jellyfish galaxy (JW100) with a stellar mass 3.2 × 10 11 M hosting an AGN. We present its spectacular extraplanar tails of ionized and molecular gas, UV stellar light, X-ray and radio continuum emission. This galaxy represents an excellent laboratory to study the interplay between different gas phases and star formation, and the influence of gas stripping, gas heating, and AGN. We analyze the physical origin of the emission at different wavelengths in the tail, in particular in-situ star formation (related to Hα, CO and UV emission), synchrotron emission from relativistic electrons (producing the radio continuum) and heating of the stripped interstellar medium (ISM) (responsible for the X-ray emission). We show the similarities and differences of the spatial distributions of ionized gas, molecular gas and UV light, and argue that the mismatch on small scales (1kpc) is due to different stages of the star formation process. We present the relation Hα-X-ray surface brightness, which is steeper for star-forming regions than for diffuse ionised gas regions with high [OI]/Hα ratio. We propose that ISM heating due to interaction with the intracluster medium (either for mixing, thermal conduction or shocks) is responsible for the X-ray tail, the observed [OI]excess and the lack of star formation in the northern part of the tail. We also report the tentative discovery in the tail of the most distant (and among the brightest) currently known ULX, a point-like ultraluminous X-ray source commonly originating in a binary stellar system powered either by an intermediate-mass black hole or a magnetized neutron star.

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“…We also examine the influence of galaxy kinematics on the AGN activity. Recent results by Poggianti et al 2017 suggest that some interactions such as RPS feed the central black hole of massive disk galaxies, triggering AGN activity. Due to the characteristics of our sample, we choose a more simplistic approach by studying the frequency of AGNs in galaxies that display regular and distorted gas kinematics in the cluster environment.…”

Section: Discussionmentioning

confidence: 99%

Galaxy kinematics across different environments in the RXJ1347−1145 cluster complex

Pérez-Martínez

Ziegler

Böhm

et al. 2020

A&A

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Aims. In order to understand the role of the different processes that drive galaxy evolution in clusters, we need comprehensive studies that simultaneously examine several of the most important physical properties of galaxies. In this work we study the interplay between the kinematic state and star formation activity of galaxies in the RXJ1347-1145 cluster complex at z∼0.45. Methods. We used VLT/VIMOS to obtain slit spectra for 95 galaxies across the 40 x40 area where the RXJ1347-1145 cluster complex resides. We determined the cluster membership of our targets by identifying one or more of the available emission lines within the wavelength range. Our spectroscopy is complemented with archival SUBARU/Suprime-Cam deep photometric observations in five optical bands (B, V, Rc, Ic, z'). We examined the kinematic properties of our sample attending to the degree of distortion of the extracted rotation curves. Regular rotating galaxies were included in our Tully-Fisher analysis while the distorted ones were used to study the role of cluster-specific interactions with respect to star formation and AGN activity. Results. Our analysis confirmed the cluster membership for approximately half of our targets. We report a higher fraction of galaxies with irregular gas kinematics in the cluster environment than in the field. Cluster galaxies with regular rotation display a moderate brightening in the B-band Tully-Fisher relation compatible with the gradual evolution of the stellar populations with lookback time, and no significant evolution in the stellar-mass Tully-Fisher relation, in line with previous studies at similar redshift. Average specific star formation rate (sSFR) values are slightly lower in our cluster sample (-0.15 dex) with respect to the main sequence of starforming galaxies, confirming the role of the environment in the early quenching of star formation in clusters. Finally, we carried out an exploratory observational study on the stellar-to-halo mass relation finding that cluster galaxies tend to have slightly lower stellar mass values for a fixed halo mass compared to their field counterparts.

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Ram-pressure feeding of supermassive black holes

Cited by 141 publications

References 49 publications

GASP. XXII. The Molecular Gas Content of the JW100 Jellyfish Galaxy at z ∼ 0.05: Does Ram Pressure Promote Molecular Gas Formation?

GASP. XXII. The Molecular Gas Content of the JW100 Jellyfish Galaxy at z ∼ 0.05: Does Ram Pressure Promote Molecular Gas Formation?

GASP XXIII: A Jellyfish Galaxy as an Astrophysical Laboratory of the Baryonic Cycle

Galaxy kinematics across different environments in the RXJ1347−1145 cluster complex

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