Details

Autor(en) / Beteiligte

• Karouzos, Marios
• Im, Myungshin
• Trichas, Markos
• Goto, Tomogotsu
• Malkan, Matthew
• Ruiz, Angel
• Jeon, Yiseul
• Kim, Ji Hoon
• Lee, Hyung Mok
• Kim, Seong Jin
• Oi, Nagisa
• Matsuhara, Hideo
• Takagi, Toshinobu
• Murata, Kazumi
• Wada, Takehiko
• Wada, Kensuke
• Shim, Hyunjin
• Hanami, Hitoshi
• Serjeant, Stephen
• White, Glenn
• Pearson, Chris
• Ohyama, Youichi

Titel

GALAXIES ON DIET: FEEDBACK SIGNATURES IN RADIO-AGN HOST GALAXIES

Ist Teil von

• 천문학논총, 2017, Vol.32 (1), p.201-203

Erscheinungsjahr

2017

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• There exists strong evidence supporting the co-evolution of central supermassive black holes and their host galaxies; however it is still under debate how such a relation comes about and whether it is relevant for all or only a subset of galaxies. An important mechanism connecting AGN to their host galaxies is AGN feedback, potentially heating up or even expelling gas from galaxies. AGN feedback may hence be responsible for the eventual quenching of star formation and halting of galaxy growth. A rich multi-wavelength dataset ranging from the X-ray regime (Chandra), to far-IR (Herschel), and radio (WSRT) is available for the North Ecliptic Pole field, most notably surveyed by the AKARI infrared space telescope, covering a total area on the sky of 5.4 sq. degrees. We investigate the star formation properties and possible signatures of radio feedback mechanisms in the host galaxies of 237 radio sources below redshift z = 2 and at a radio 1.4 GHz flux density limit of 0.1 mJy. Using broadband SED modelling, the nuclear and host galaxy components of these sources are studied simultaneously as a function of their radio luminosity. Here we present results concerning the AGN content of the radio sources in this field, while also offering evidence showcasing a link between AGN activity and host galaxy star formation. In particular, we show results supporting a maintenance type of feedback from powerful radio-jets.