Identifying the subtle signatures of feedback from distant AGN using ALMA observations and the EAGLE hydrodynamical simulations. Scholtz, J., Alexander, D. M., Harrison, C. M., Rosario, D. J., McAlpine, S., Mullaney, J. R, Stanley, F., Simpson, J., Theuns, T., Bower, R. G., Hickox, R. C., Santini, P., & Swinbank, A. M. ArXiv e-prints, 1712:arXiv:1712.02708, December, 2017. ![Identifying the subtle signatures of feedback from distant AGN using ALMA observations and the EAGLE hydrodynamical simulations [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex We present sensitive 870\${\textbackslash}mu\$m continuum measurements from our ALMA programmes of 114 X-ray selected AGN in the CDF-S and COSMOS fields. We use these observations in combination with data from Spitzer and Herschel to construct a sample of 86 X-ray selected AGN, 63 with ALMA constraints at \$z=1.5-3.2\$ with stellar mass \${\textgreater}2{\textbackslash}times10{\textasciicircum}\{10\}M_\{{\textbackslash}odot\}\$. We constructed broad-band spectral energy distributions in the infrared band (8 - 1000\${\textbackslash}mu\$m) and constrain star-formation rates (SFRs) uncontaminated by the AGN. Using a hierarchical Bayesian method that takes into account the information from upper limits, we fit SFR and specific SFR (sSFR) distributions. We explore these distributions as a function of both X-ray luminosity and stellar mass. We compare our measurements to two versions of the EAGLE hydrodynamical simulations: the reference model with AGN feedback and the model without AGN. We find good agreement between the observations and that predicted by the EAGLE reference model for the modes and widths of the sSFR distributions as a function of both X-ray luminosity and stellar mass; however, we found that the EAGLE model without AGN feedback predicts a significantly narrower width when compared to the data. Overall, from the combination of the observations with the model predictions, we conclude that (1) even with AGN feedback, we expect no strong relationship between the sSFR distribution parameters and instantaneous AGN luminosity and (2) a signature of AGN feedback is a broad distribution of sSFRs for all galaxies (not just those hosting an AGN) with stellar masses above \${\textbackslash}approx 10{\textasciicircum}\{10\}\$M\$_\{{\textbackslash}odot\}\$.
@article{scholtz_identifying_2017,
title = {Identifying the subtle signatures of feedback from distant {AGN} using {ALMA} observations and the {EAGLE} hydrodynamical simulations},
volume = {1712},
url = {http://adsabs.harvard.edu/abs/2017arXiv171202708S},
abstract = {We present sensitive 870\${\textbackslash}mu\$m continuum measurements from our ALMA
programmes of 114 X-ray selected AGN in the CDF-S and COSMOS fields. We
use these observations in combination with data from Spitzer and
Herschel to construct a sample of 86 X-ray selected AGN, 63 with ALMA
constraints at \$z=1.5-3.2\$ with stellar mass
\${\textgreater}2{\textbackslash}times10{\textasciicircum}\{10\}M\_\{{\textbackslash}odot\}\$. We constructed broad-band spectral energy
distributions in the infrared band (8 - 1000\${\textbackslash}mu\$m) and constrain
star-formation rates (SFRs) uncontaminated by the AGN. Using a
hierarchical Bayesian method that takes into account the information
from upper limits, we fit SFR and specific SFR (sSFR) distributions. We
explore these distributions as a function of both X-ray luminosity and
stellar mass. We compare our measurements to two versions of the EAGLE
hydrodynamical simulations: the reference model with AGN feedback and
the model without AGN. We find good agreement between the observations
and that predicted by the EAGLE reference model for the modes and widths
of the sSFR distributions as a function of both X-ray luminosity and
stellar mass; however, we found that the EAGLE model without AGN
feedback predicts a significantly narrower width when compared to the
data. Overall, from the combination of the observations with the model
predictions, we conclude that (1) even with AGN feedback, we expect no
strong relationship between the sSFR distribution parameters and
instantaneous AGN luminosity and (2) a signature of AGN feedback is a
broad distribution of sSFRs for all galaxies (not just those hosting an
AGN) with stellar masses above \${\textbackslash}approx 10{\textasciicircum}\{10\}\$M\$\_\{{\textbackslash}odot\}\$.},
urldate = {2018-01-08},
journal = {ArXiv e-prints},
author = {Scholtz, J. and Alexander, D. M. and Harrison, C. M. and Rosario, D. J. and McAlpine, S. and Mullaney, J. R and Stanley, F. and Simpson, J. and Theuns, T. and Bower, R. G. and Hickox, R. C. and Santini, P. and Swinbank, A. M.},
month = dec,
year = {2017},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {arXiv:1712.02708},
}
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We use these observations in combination with data from Spitzer and Herschel to construct a sample of 86 X-ray selected AGN, 63 with ALMA constraints at \\$z=1.5-3.2\\$ with stellar mass \\${\\textgreater}2{\\textbackslash}times10{\\textasciicircum}\\{10\\}M_\\{{\\textbackslash}odot\\}\\$. We constructed broad-band spectral energy distributions in the infrared band (8 - 1000\\${\\textbackslash}mu\\$m) and constrain star-formation rates (SFRs) uncontaminated by the AGN. Using a hierarchical Bayesian method that takes into account the information from upper limits, we fit SFR and specific SFR (sSFR) distributions. We explore these distributions as a function of both X-ray luminosity and stellar mass. We compare our measurements to two versions of the EAGLE hydrodynamical simulations: the reference model with AGN feedback and the model without AGN. We find good agreement between the observations and that predicted by the EAGLE reference model for the modes and widths of the sSFR distributions as a function of both X-ray luminosity and stellar mass; however, we found that the EAGLE model without AGN feedback predicts a significantly narrower width when compared to the data. Overall, from the combination of the observations with the model predictions, we conclude that (1) even with AGN feedback, we expect no strong relationship between the sSFR distribution parameters and instantaneous AGN luminosity and (2) a signature of AGN feedback is a broad distribution of sSFRs for all galaxies (not just those hosting an AGN) with stellar masses above \\${\\textbackslash}approx 10{\\textasciicircum}\\{10\\}\\$M\\$_\\{{\\textbackslash}odot\\}\\$.","urldate":"2018-01-08","journal":"ArXiv e-prints","author":[{"propositions":[],"lastnames":["Scholtz"],"firstnames":["J."],"suffixes":[]},{"propositions":[],"lastnames":["Alexander"],"firstnames":["D.","M."],"suffixes":[]},{"propositions":[],"lastnames":["Harrison"],"firstnames":["C.","M."],"suffixes":[]},{"propositions":[],"lastnames":["Rosario"],"firstnames":["D.","J."],"suffixes":[]},{"propositions":[],"lastnames":["McAlpine"],"firstnames":["S."],"suffixes":[]},{"propositions":[],"lastnames":["Mullaney"],"firstnames":["J.","R"],"suffixes":[]},{"propositions":[],"lastnames":["Stanley"],"firstnames":["F."],"suffixes":[]},{"propositions":[],"lastnames":["Simpson"],"firstnames":["J."],"suffixes":[]},{"propositions":[],"lastnames":["Theuns"],"firstnames":["T."],"suffixes":[]},{"propositions":[],"lastnames":["Bower"],"firstnames":["R.","G."],"suffixes":[]},{"propositions":[],"lastnames":["Hickox"],"firstnames":["R.","C."],"suffixes":[]},{"propositions":[],"lastnames":["Santini"],"firstnames":["P."],"suffixes":[]},{"propositions":[],"lastnames":["Swinbank"],"firstnames":["A.","M."],"suffixes":[]}],"month":"December","year":"2017","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:1712.02708","bibtex":"@article{scholtz_identifying_2017,\n\ttitle = {Identifying the subtle signatures of feedback from distant {AGN} using {ALMA} observations and the {EAGLE} hydrodynamical simulations},\n\tvolume = {1712},\n\turl = {http://adsabs.harvard.edu/abs/2017arXiv171202708S},\n\tabstract = {We present sensitive 870\\${\\textbackslash}mu\\$m continuum measurements from our ALMA \nprogrammes of 114 X-ray selected AGN in the CDF-S and COSMOS fields. We\nuse these observations in combination with data from Spitzer and\nHerschel to construct a sample of 86 X-ray selected AGN, 63 with ALMA\nconstraints at \\$z=1.5-3.2\\$ with stellar mass\n\\${\\textgreater}2{\\textbackslash}times10{\\textasciicircum}\\{10\\}M\\_\\{{\\textbackslash}odot\\}\\$. We constructed broad-band spectral energy\ndistributions in the infrared band (8 - 1000\\${\\textbackslash}mu\\$m) and constrain\nstar-formation rates (SFRs) uncontaminated by the AGN. Using a\nhierarchical Bayesian method that takes into account the information\nfrom upper limits, we fit SFR and specific SFR (sSFR) distributions. We\nexplore these distributions as a function of both X-ray luminosity and\nstellar mass. We compare our measurements to two versions of the EAGLE\nhydrodynamical simulations: the reference model with AGN feedback and\nthe model without AGN. We find good agreement between the observations\nand that predicted by the EAGLE reference model for the modes and widths\nof the sSFR distributions as a function of both X-ray luminosity and\nstellar mass; however, we found that the EAGLE model without AGN\nfeedback predicts a significantly narrower width when compared to the\ndata. Overall, from the combination of the observations with the model\npredictions, we conclude that (1) even with AGN feedback, we expect no\nstrong relationship between the sSFR distribution parameters and\ninstantaneous AGN luminosity and (2) a signature of AGN feedback is a\nbroad distribution of sSFRs for all galaxies (not just those hosting an\nAGN) with stellar masses above \\${\\textbackslash}approx 10{\\textasciicircum}\\{10\\}\\$M\\$\\_\\{{\\textbackslash}odot\\}\\$.},\n\turldate = {2018-01-08},\n\tjournal = {ArXiv e-prints},\n\tauthor = {Scholtz, J. and Alexander, D. M. and Harrison, C. M. and Rosario, D. J. and McAlpine, S. and Mullaney, J. 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