<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="">Astro Journal Club next Wednesday starts at 3 p.m. (sharp) in the seminar room F-201 of the Physics Department.</div><div class=""><br class=""></div><div class=""><b class="">Presenter</b>: Ivan Delvecchio, dr.sc.</div><div class=""><br class=""></div><div class=""><b class="">Title</b>: Cospatial Star Formation and Supermassive Black Hole Growth in z∼3 Galaxies: Evidence for In-situ Co-evolution</div><div class=""><br class=""></div><div class=""><b class="">Authors</b>: Rujopakarn et al. (2018)</div><div class=""><br class=""></div><div class=""><b class="">Abstract</b>: </div><div class="">We present a sub-kpc localization of the sites of supermassive black hole (SMBH) growth in three active galactic nuclei (AGN) at z∼3 in relation to the regions of intense star formation in their hosts. These AGNs are selected from Karl G. Jansky Very Large Array (VLA) and Atacama Large Millimeter/submillimeter Array (ALMA) observations in the HUDF and COSMOS, with the centimetric radio emission tracing both star formation and AGN, and the sub/millimeter emission by dust tracing nearly pure star formation. We require radio emission to be ⩾5× more luminous than the level associated with the sub/millimeter star formation to ensure that the radio emission is AGN-dominated, thereby allowing localization of the AGN and star formation independently. In all three galaxies, the AGN are located within the compact regions of gas-rich, heavily obscured, intense nuclear star formation, with Re=0.4−1.1 kpc and average star formation rates of ≃100−1200 M⊙yr−1. If the current episode of star formation continues at such a rate over the stellar mass doubling time of their hosts, ≃0.2 Gyr, the newly formed stellar mass will be of the order of 1011 M⊙ within the central kpc region, concurrently and cospatially with significant growth of the SMBH. This is consistent with a picture of in-situ galactic bulge and SMBH formation. This work demonstrates the unique complementarity of VLA and ALMA observations to unambiguously pinpoint the locations of AGN and star formation down to ≃30 mas, corresponding to ≃230 pc at z=3. </div><div class=""><br class=""></div><div class=""><b class="">Link</b>: <a href="https://arxiv.org/abs/1801.07072" class="">https://arxiv.org/abs/1801.07072</a></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 (<a href="mailto:lceraj@phy.hr" class="">lceraj@phy.hr</a>).</div><div class=""><br class=""></div><div class="">You can find information about the upcoming AJC seminars and links to previous AJC presentations @ <a href="https://lanaceraj.wixsite.com/ajc-main" class="">https://lanaceraj.wixsite.com/ajc-main</a> </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></body></html>