Star Formation Activity in Clash Brightest Cluster Galaxies

Fogarty, Kevin; Postman, Marc; Connor, Thomas; Donahue, M.; Moustakas, John

doi:10.1088/0004-637x/813/2/117

Cited by 49 publications

(113 citation statements)

References 85 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In Fogarty et al (2015), we attempted to estimate the cooling rate of the ICM by measuringṀ g for gas that was at a radius < 35 kpc or for gas that had an average t cool /t f f ratio below 70 5 . We found that while reddening-corrected UV photometric SFRs scale withṀ g in both cases, star formation appears to be increasingly 'inefficient' as the SFR decreases.…”

Section: Discussionmentioning

confidence: 99%

“…In Fogarty et al (2015), we identified 11 BCGs in the CLASH X-ray selected sample with evidence of ongoing star formation. In each of these BCGs, we detected extended UV emission in WFC3/UVIS photometry and extended Hα + [N II] emission by differencing ACS images.…”

Section: Methodsmentioning

confidence: 99%

“…AGN jet feedback is thought to inject energy into the ICM, thus offsetting cooling while also triggering condensation of thermodynamically unstable volumes of ICM plasma, which then precipitate onto the BCG and fuel star formation and further AGN activity Li & Bryan 2014;Li et al 2015;Gaspari et al 2012Gaspari et al , 2013Gaspari et al , 2015Fogarty et al 2015;Gaspari et al 2016;Prasad et al 2015;Yang & Reynolds 2016;Meece et al 2016). Recently, the precipitation aspect of this model was shown to be consistent with observations of molecular gas accretion onto the AGN in the Abell 2597 BCG (Tremblay et al 2016).…”

Section: Introductionmentioning

confidence: 99%

“…The cooling times quoted in Fogarty et al (2015) were taken from the ACCEPT website (http://www.pa.msu.edu/astro/MC2/accept/). ACCEPT website cooling times are incorrect and need to be multiplied by a factor of 6.9/2.…”

mentioning

confidence: 99%

See 3 more Smart Citations

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

Fogarty

Postman

Larson

et al. 2017

ApJ

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

See 2 more Smart Citations

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

Fogarty

Postman

Larson

et al. 2017

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…The process of feeding the AGN with cold clumps in the feedback mechanism cycle is termed the cold feedback mechanism, and was suggested by Pizzolato & Soker (2005). The cold feedback mechanism has been later strengthened by observations of cold gas and by more detailed studies (e.g., Revaz et al 2008;Pope 2009;Pizzolato & Soker 2010;Edge et al 2010;Wilman et al 2011;Nesvadba et al 2011;Cavagnolo et al 2011;Gaspari et al 2012a,b;McCourt et al 2012;Sharma et al 2012;Farage et al 2012;Wagh et al 2014;Banerjee & Sharma 2014;McNamara et al 2014;Li et al 2015;Prasad et al 2015;Russell et al 2015;Tremblay et al 2015;Fogarty et al 2015). Gilkis & Soker (2012) and Hillel & Soker (2014) have shown that the mixing of the hot bubble gas with the ICM is a much more efficient heating process than heating by repeated shocks; hereafter termed shocksheating.…”

Section: Introductionmentioning

confidence: 99%

Heating the intracluster medium by jet-inflated bubbles

Hillel

Soker

2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We examine the heating of the intra-cluster medium (ICM) of cooling flow clusters of galaxies by jet-inflated bubbles and conclude that mixing of hot bubble gas with the ICM is more important than turbulent heating and shock heating. We use the pluto hydrodynamical code in full 3D to properly account for the inflation of the bubbles and to the multiple vortices induced by the jets and bubbles. The vortices mix some hot shocked jet gas with the ICM. For the parameters used by us the mixing process accounts for about four times as much heating as that by the kinetic energy in the ICM, namely, turbulence and sound waves. We conclude that turbulent heating plays a smaller role than mixing. Heating by shocks is even less efficient.

show abstract

Molecular gas in distant brightest cluster galaxies

Castignani

Combes

Salomé

et al. 2020

A&A

View full text Add to dashboard Cite

Brightest cluster galaxies (BCGs) are excellent laboratories to study galaxy evolution in dense Mpc-scale environments. We have observed in CO(1→0), CO(2→1), CO(3→2), or CO(4→3), with the IRAM-30m, 18 BCGs at z ∼ 0.2 − 0.9 that are drawn from the Cluster Lensing And Supernova survey with Hubble (CLASH) survey. Our sample includes RX1532, which is our primary target, being among the BCGs with the highest star formation rate (SFR 100 M /yr) in the CLASH sample. We unambiguously detected both CO(1→0) and CO(3→2) in RX1532, yielding a large reservoir of molecular gas, M H 2 = (8.7 ± 1.1) × 10 10 M , and a high level of excitation r 31 = 0.75 ± 0.12. A morphological analysis of the Hubble Space Telescope I-band image of RX1532 reveals the presence of clumpy substructures both within and outside the half-light radius r e = (11.6 ± 0.3) kpc, similarly to those found independently both in ultraviolet and in H α in previous work. We tentatively detected CO(1→0) or CO(2→1) in four other BCGs, with molecular gas reservoirs in the range M H 2 = 2 × 10 10−11 M . For the remaining 13 BCGs we set robust upper limits of M H 2 /M 0.1, which are among the lowest molecular gas to stellar mass ratios found for distant ellipticals and BCGs. By comparison with distant cluster galaxies observed in CO our study shows that RX1532 (M H 2 /M = 0.40 ± 0.05) belongs to the rare population of star forming and gas-rich BCGs in the distant universe. By using available X-ray based estimates of the central intra-cluster medium entropy, we show that the detection of large reservoirs of molecular gas M H 2 10 10 M in distant BCGs is possible when the two conditions are met: i) high SFR and ii) low central entropy, which favors the condensation and the inflow of gas onto the BCGs themselves, similarly to what has been previously found for some local BCGs.

show abstract

Star Formation Activity in Clash Brightest Cluster Galaxies

Cited by 49 publications

References 85 publications

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

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

Heating the intracluster medium by jet-inflated bubbles

Molecular gas in distant brightest cluster galaxies

Contact Info

Product

Resources

About