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black holes

Page history last edited by chris.power@uwa.edu.au 9 years ago

Results:

 

Spatial distribution:

OWLS additionally has black holes sent to the origin in the same way as nIFTy Madrid.

 

SMBH mass function:

 

Radial plot about [499,498,499] excluding OWLS outliers:

 

Accretion Rates:

 

 

Aims:

 

RJT: My main interest is looking at SFR-BHAR correlations and the phenomenology of AGN feedback in the BCG and cluster core. A lot of the things I want to do need very detailed tracking, so I've tried to adjust to ensemble based comparisons. But even so, can construct z=0,0.5,1 SFR-BHAR correlations from the galaxy catalogues. Of course heavily biased region, but nonetheless still interesting to see how the two compare.

 

Individual BH details: beyond the scaling relations which Stuart has looked at, I'm interested in precisely how well the BH population tracks halos in a physical sense, as obviously the local density is an important determinant of BH growth and some thought and effort has gone into creating algorithms (e.g. potential tracking) to do this. High res tests have shown a few of these approaches may be sensitive to sudden changes following feedback events - may or may not be such an issue at lower res.

 

Classifying AGN heating: Curious to examine mass flux rates through spheres, and also the level of heating anisotropy across algorithms. I've been looking at this in spiral galaxy fueling and a grad student has developed a simple approach to predict flux rates that allows a bit of the noise to be taken out. 

 

Differences between early (group) vs later (cluster) heating: Not sure about this part as Chris mentioned he might have a student interested in this.

 

Lastly, I might look at Eddington ratio distributions although without a lot of snapshots this is probably going to be quite noisy and again I'm not sure if Stuart wanted to look at this.

 

Student Projects:

 

Maitrayee Gupta and Qin Fei to look at how black hole growth and feedback and stellar mass growth and feedback vary between full physics runs, and correlate with change in central entropy profile between non-radiative runs and full physics runs.

 

 

 

 

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