<html><head><meta http-equiv="Content-Type" content="text/html charset=utf-8"></head><body style="word-wrap: break-word; -webkit-nbsp-mode: space; -webkit-line-break: after-white-space;" class=""><div class="">Dear all,</div><div class=""><br class=""></div><div class="">next <b class="">Wednesday (Oct 18th)</b> we are starting with a new season of Astro Journal Club at <b class="">3 p.m. </b>(sharp) in the seminar room <b class="">F-201</b> of the Physics Department. </div><div class=""><br class=""></div><div class=""><b class="">Presenter</b>: Lana Ceraj</div><div class=""><br class=""></div><div class=""><b class="">Title of paper</b>: Decoupled Black Hole Accretion and Quenching: The Relationship Between BHAR, SFR, and Quenching in Milky Way and Andromeda-mass Progenitors Since z = 2.5</div><div class=""><br class=""></div><div class=""><b class="">Authors</b>: M. J. Cowley et al. (2017)</div><div class=""><br class=""></div><div class=""><b class="">Abstract</b>: </div><div class="">We investigate the relationship between the black hole accretion rate (BHAR) and star-formation rate (SFR) for Milky Way (MW) and Andromeda (M31)-mass progenitors from z = 0.2 - 2.5. We source galaxies from the Ks-band selected ZFOURGE survey, which includes multi-wavelenth data spanning 0.3 - 160um. We use decomposition software to split the observed SEDs of our galaxies into their active galactic nuclei (AGN) and star-forming components, which allows us to estimate BHARs and SFRs from the infrared (IR). We perform tests to check the robustness of these estimates, including a comparison to BHARs and SFRs derived from X-ray stacking and far-IR analysis, respectively. We find as the progenit- ors evolve, their relative black hole-galaxy growth (i.e. their BHAR/SFR ratio) increases from low to high redshift. The MW-mass progenitors exhibit a log-log slope of 0.64 +/- 0.11, while the M31-mass progenitors are 0.39 +/- 0.08. This result contrasts with previous studies that find an almost flat slope when adopting X-ray/AGN-selected or mass-limited samples and is likely due to their use of a broad mixture of galaxies with different evolutionary histories. Our use of progenitor-matched samples highlights the potential importance of carefully selecting progenitors when searching for evolutionary relationships between BHAR/SFRs. Additionally, our finding that BHAR/SFR ratios do not track the rate at which progenitors quench casts doubts over the idea that the suppression of star-formation is predominantly driven by luminous AGN feedback (i.e. high BHARs).</div><div class=""><br class=""></div><div class=""><b class="">Link</b> to paper: <a href="https://arxiv.org/abs/1710.04225" class="">https://arxiv.org/abs/1710.04225</a></div><div class=""><br class=""></div><div class=""><b class="">Status</b>: Submitted on 11 Oct 2017</div><div class=""><br class=""></div><div class=""><br class=""></div><div class="">If you’d like to present a paper from the field of astrophysics, please contact me via this email (<b class=""><a href="mailto:lceraj@phy.hr" class="">lceraj@phy.hr</a></b>). All slots are currently free. </div><div class=""><br class=""></div><div class=""><br class=""></div><div class="">See you all on Wednesday.</div><div class=""><br class=""></div><div class="">Cheers,</div><div class="">Lana</div><div class=""><br class=""></div></body></html>