Starbursting brightest cluster galaxy: a <i>Herschel</i> view of the massive cluster MACS J1931.8−2634

Santos, J. S.; Balestra, I.; Tozzi, P.; Altiéri, B.; Valtchanov, I.; Mercurio, A.; Nonino, M.; Yu, Heng; Rosati, P.; Grillo, C.; Medezinski, Elinor; Biviano, A.

doi:10.1093/mnrasl/slv179

Cited by 9 publications

(20 citation statements)

References 49 publications

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“…Abell 611 show a clear unresolved X-ray emission in the hard band, and the BCG of MACSJ0744 is also a candidate X-ray AGN. These are the only two detections of unresolved X-ray emission in our sample together with MACSJ1931, which hosts a bright obscured AGN (see Santos et al 2016). This may suggest different modes of accretion marked by the presence of nuclear X-ray emission, as discussed in a forthcoming paper by our team (Li-Lan Yang et al 2018, in preparation).…”

Section: Bcg Spectral Propertiesmentioning

confidence: 57%

JVLA 1.5 GHz Continuum Observation of CLASH Clusters. I. Radio Properties of the BCGs

Tozzi

Weeren

et al. 2018

ApJ

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We present high-resolution (∼ 1"), 1.5 GHz continuum observations of the brightest cluster galaxies (BCGs) of 13 CLASH (Cluster Lensing And Supernova survey with Hubble) clusters at 0.18 < z < 0.69 with the Karl G. Jansky Very Large Array (JVLA). Radio emission is clearly detected and characterized for 11 BCGs, while for two of them we obtain only upper limits to their radio flux (< 0.1 mJy at 5σ confidence level). We also consider five additional clusters whose BCG is detected in FIRST or NVSS. We find radio powers in the range from 2 × 10 23 to ∼ 10 26 W Hz −1 and radio spectral indices α 30 1.5 (defined as the slope between 1.5 and 30 GHz) distributed from ∼ −1 to −0.25 around the central value α = −0.68. The radio emission from the BCGs is resolved in three cases (Abell 383, MACS J1931, and RX J2129), and unresolved or marginally resolved in the remaining eight cases observed with JVLA. In all the cases the BCGs are consistent with being powered by active galactic nuclei (AGN). The radio power shows a positive correlation with the BCG star formation rate, and a negative correlation with the central entropy of the surrounding intracluster medium (ICM) except in two cases (MACS J1206 and CL J1226). Finally, over the restricted range in radio power sampled by the CLASH BCGs, we observe a significant scatter between the radio power and the average mechanical power stored in the ICM cavities.

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Section: Bcg Spectral Propertiesmentioning

confidence: 57%

JVLA 1.5 GHz Continuum Observation of CLASH Clusters. I. Radio Properties of the BCGs

Tozzi

Weeren

et al. 2018

ApJ

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“…The extended emission in this galaxy seen in the HST data was reported and characterised by Fogarty et al (2019). The M1931 BCG has been shown to have elevated SFR ranging from ∼90 M yr −1 from UV data (Donahue et al 2015) to ∼150 M yr −1 from IR data (Santos et al 2016) up to ∼250 M yr −1 from UV through far-IR (Fogarty et al 2017). Such high levels of star formation are not only atypical for 'red and dead' elliptical The cross shows the location of the AGN, as identified according to different diagnostic diagrams; see Sect.…”

Section: Data: Macs 19318-2635 Galaxy Cluster and Its Bcgmentioning

confidence: 72%

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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“…As Santos et al (2016) postulate a potentially large AGN contribution to the UV-IR SED of MACS1931.8-2653, we ran a separate SED fitting analysis for this BCG wherein we include the IR AGN model of Siebenmorgen et al (2015). We allowed iSEDfit to sample the full range of parameters that describe the Siebenmorgen et al (2015) AGN emission model library, which for our purposes are nuisance parameters.…”

Section: Testing Impact Of Agn Emission On Sed Resultsmentioning

confidence: 99%

The Relationship Between Brightest Cluster Galaxy Star Formation and the Intracluster Medium in CLASH

Fogarty

Postman

Larson

et al. 2017

ApJ

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We study the nature of feedback mechanisms in the 11 CLASH brightest cluster galaxies (BCGs) that exhibit extended ultraviolet and nebular line emission features. We estimate star formation rates (SFRs), dust masses, and starburst durations using a Bayesian photometry-fitting technique that accounts for both stellar and dust emission from the UV through far IR. By comparing these quantities to intracluster medium (ICM) cooling times and free-fall times derived from X-ray observations and lensing estimates of the cluster mass distribution, we discover a tight relationship between the BCG SFR and the ICM cooling time to free-fall time ratio, t cool /t f f , with an upper limit on the intrinsic scatter of 0.15 dex. Furthermore, starburst durations may correlate with ICM cooling times at a radius of 0.025R 500 , and the two quantities converge upon reaching the Gyr regime. Our results provide a direct observational link between the thermodynamical state of the ICM and the intensity and duration of BCG star formation activity, and appear consistent with a scenario where active galactic nuclei (AGN) induce condensation of thermally unstable ICM overdensities that fuel longduration (> 1 Gyr) BCG starbursts. This scenario can explain (a) how gas with a low cooling time is depleted without causing a cooling flow and (b) the scaling relationship between SFR and t cool /t f f . We also find that the scaling relation between SFR and dust mass in BCGs with SFRs < 100 M yr −1 is similar to star-forming field galaxies; BCGs with large (> 100 M yr −1 ) SFRs have dust masses comparable to extreme starbursts.

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Starbursting brightest cluster galaxy: a Herschel view of the massive cluster MACS J1931.8−2634

Cited by 9 publications

References 49 publications

JVLA 1.5 GHz Continuum Observation of CLASH Clusters. I. Radio Properties of the BCGs

JVLA 1.5 GHz Continuum Observation of CLASH Clusters. I. Radio Properties of the BCGs

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

The Relationship Between Brightest Cluster Galaxy Star Formation and the Intracluster Medium in CLASH

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