Inquiring into the nature of the Abell 2667 brightest cluster galaxy: physical properties from MUSE

Iani, Edoardo; Rodighiero, G.; Fritz, J.; Cresci, G.; Mancini, C.; Tozzi, P.; Rodríguez-Muñoz, L.; Rosati, P.; Caminha, G. B.; Zanella, Anita; Berta, S.; Cassata, P.; Concas, A.; Enia, A.; Fadda, D.; Franceschini, A.; Liu, Ang; Mercurio, A.; Morselli, L.; Pérez‐González, Pablo G.; Popesso, P.; Sabatini, Giovanni; Vernet, J.; Weeren, R. J. van

doi:10.1093/mnras/stz1631

Cited by 5 publications

(3 citation statements)

References 138 publications

(177 reference statements)

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“…For instance, Hamer & Edge (2016) and Iani et al (2019) determined the electron density for their sample of BCGs based on the [Sii] 6731/6716 emission line ratio and their inferred values, on the order of a few hundred cm −3 , are in very good agreement with the value of n e = 361 cm −3 that we determine for the M1931 BCG.…”

Section: Discussionsupporting

confidence: 83%

“…The occurrence of such 'composite' emission is typical for cool-core BCG. For example, Tremblay et al (2018), Iani et al (2019), Hamer & Edge (2016) also studied (cool-core) BCGs based on IFU data and infer composite emission for their systems in the BPT diagram and concluded that the systems are ionised by a superposition of many physical processes.…”

Section: Discussionmentioning

confidence: 99%

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The VLT-MUSE and ALMA view of the MACS 1931.8-2635 brightest cluster galaxy

Ciocan

Ziegler

Verdugo

et al. 2021

A&A

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We reveal the importance of ongoing in situ star formation in the brightest cluster galaxy (BCG) in the massive cool-core CLASH cluster MACS 1931.8-2635 at a redshift of z = 0.35 by analysing archival VLT-MUSE optical integral field spectroscopy. Using a multi-wavelength approach, we assessed the stellar and warm ionised medium components, which were spatially resolved by the VLT-MUSE spectroscopy, and linked them to the molecular gas by incorporating sub-mm ALMA observations. We measured the fluxes of strong emission lines such as: [O II] λ3727, Hβ, [O III] λ5007, Hα, [N II] λ 6584, and [S II] λ6718, 6732, which allowed us to determine the physical conditions of the warm ionised gas, such as electron temperature, electron density, extinction, ionisation parameter, (O/H) gas metallicities, star formation rates, and gas kinematics, as well as the star formation history of the system. Our analysis reveals the ionising sources in different regions of the galaxy. The ionised gas flux brightness peak corresponds to the location of the supermassive black hole in the BCG and the system shows a diffuse warm ionised gas tail extending 30 kpc in the north-east direction. The ionised and molecular gas are co-spatial and co-moving, with the gaseous component in the tail likely falling inward, providing fuel for star formation and accretion-powered nuclear activity. The gas is ionised by a mix of star formation and other energetic processes which give rise to LINER-like emission, with active galactic nuclei emission dominant only in the BCG core. We measured a star formation rate of ∼97 M⊙ yr−1, with its peak at the BCG core. However, star formation accounts for only 50–60% of the energetics needed to ionise the warm gas. The stellar mass growth of the BCG at z < 0.5 is dominated either by in situ star formation generated by thermally unstable intracluster medium cooling or by dry mergers, with these mechanisms accounting for the build-up of 20% of the stellar mass of the system. Our measurements reveal that the most central regions of the BCG contain the lowest gas-phase oxygen abundance, whereas the Hα arm exhibits slightly more elevated values, suggesting the transport of gas out to large distances from the centre as a result of active galactic nuclei outbursts. The galaxy is a dispersion-dominated system that is typical for massive, elliptical galaxies. The gas and stellar kinematics are decoupled, with the gaseous velocity fields being more closely related to the bulk motions of the intracluster medium.

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Section: Discussionsupporting

confidence: 83%

Section: Discussionmentioning

confidence: 99%

The VLT-MUSE and ALMA view of the MACS 1931.8-2635 brightest cluster galaxy

Ciocan

Ziegler

Verdugo

et al. 2021

A&A

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“…The process by which cold clumps carry the accretion flow onto the central SMBH (rather than Bondi-type accretion of the hot gas) is the cold feedback mechanism (Pizzolato & Soker 2005, 2010Gaspari et al 2013;Gaspari, Brighenti, & Temi 2015;; note that some studies use other terms for this mechanism, like chaotic cold accretion, e.g., McKinley et al 2021). There are many papers in recent years that support the cold feedback mechanism (e.g., a small sample of recent papers, Babyk et al 2018;Gaspari et al 2018;Ji et al 2018;Prasad et al 2018;Pulido et al 2018;Voit 2018a;Yang et al 2018;Choudhury et al 2019;Iani et al 2019;Rose et al 2019;Russell et al 2019;Stern et al 2019;Storchi-Bergmann, & Schnorr-Müller 2019;Vantyghem et al 2019;Voit 2019;Hardcastle & Croston 2020;Martz et al 2020;Prasad et al 2020;Eckert et al 2021;Maccagni et al 2021;Pasini et al 2021;Qiu et al 2021;Singh, Voit, & Nath 2021).…”

Section: Introductionmentioning

confidence: 99%

Jittering jets by negative angular momentum feedback in cooling flows

Soker¹

2021

Preprint

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I apply the jittering jets in cooling flow scenario to explain the perpendicular to each other and almost coeval two pairs of bubbles in the cooling flow galaxy cluster RBS 797, and conclude that the interaction of the jets with the cold dense clumps that feed the supermassive black hole (SMBH) takes place in the zone where the gravitational influence of the SMBH and that of the cluster are about equal. According to the jittering jets in cooling flow scenario jets uplift and entrain cold and dense clumps, impart the clumps velocity perpendicular to the original jets' direction, and 'drop' them closer to the jets' axis. The angular momentum of these clumps is at a very high angle to the original jets' axis. When these clumps feed the SMBH in the next outburst the new jets' axis is at a high angle to the axis of the first pair of jets. I apply this scenario to recent observations that show the two perpendicular pairs of bubbles in RBS 797 to have a small age difference of < 10 Myr, and conclude that the jets-clumps interaction takes place in a distance of about ≈ 10 − 100 pc from the SMBH. Interestingly, in this zone the escape velocity from the SMBH is about equal to the sound speed of the intracluster medium (ICM). I discuss the implications of this finding.

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Euclid preparation

Gabarra¹,

Mancini²,

Muñoz³

et al. 2023

A&A

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This work focusses on the pilot run of a simulation campaign aimed at investigating the spectroscopic capabilities of the Euclid Near-Infrared Spectrometer and Photometer (NISP), in terms of continuum and emission line detection in the context of galaxy evolutionary studies. To this purpose, we constructed, emulated, and analysed the spectra of 4992 star-forming galaxies at 0.3 ≤ z ≤ 2.5 using the NISP pixel-level simulator. We built the spectral library starting from public multi-wavelength galaxy catalogues, with value-added information on spectral energy distribution (SED) fitting results, and stellar population templates from Bruzual & Charlot (2003, MNRAS, 344, 1000). Rest-frame optical and near-IR nebular emission lines were included using empirical and theoretical relations. Dust attenuation was treated using the Calzetti extinction law accounting for the differential attenuation in line-emitting regions with respect to the stellar continuum. The NISP simulator was configured including instrumental and astrophysical sources of noise such as the dark current, read-out noise, zodiacal background, and out-of-field stray light. In this preliminary study, we avoided contamination due to the overlap of the slitless spectra. For this purpose, we located the galaxies on a grid and simulated only the first order spectra. We inferred the 3.5σ NISP red grism spectroscopic detection limit of the continuum measured in the H band for star-forming galaxies with a median disk half-light radius of 0.″4 at magnitude H = 19.5 ± 0.2 AB mag for the Euclid Wide Survey and at H = 20.8 ± 0.6 AB mag for the Euclid Deep Survey. We found a very good agreement with the red grism emission line detection limit requirement for the Wide and Deep surveys. We characterised the effect of the galaxy shape on the detection capability of the red grism and highlighted the degradation of the quality of the extracted spectra as the disk size increased. In particular, we found that the extracted emission line signal-to-noise ratio (S/N) drops by ~45% when the disk size ranges from 0.″25 to 1″. These trends lead to a correlation between the emission line S/N and the stellar mass of the galaxy and we demonstrate the effect in a stacking analysis unveiling emission lines otherwise too faint to detect.

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Inquiring into the nature of the Abell 2667 brightest cluster galaxy: physical properties from MUSE

Cited by 5 publications

References 138 publications

The VLT-MUSE and ALMA view of the MACS 1931.8-2635 brightest cluster galaxy

The VLT-MUSE and ALMA view of the MACS 1931.8-2635 brightest cluster galaxy

Jittering jets by negative angular momentum feedback in cooling flows

Euclid preparation

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