The galaxy UGC 5101 contains an active nucleus (AGN), a compact core that emits copious radiation and possible stimulates star formation. In this Hubble image, the tidal tail at the left suggests that the galaxy is actually a merging pair of galaxies. Astronomers studying how AGN influence their host galaxy's development have concluded that both grow together.
NASA, ESA, the Hubble Heritage Team; STScI/AURA)-ESA/Hubble Collaboration and A. Evans University of Virginia, Charlottesville/NRAO/Stony Brook University
Most galaxies host a supermassive black hole (SMBH) at their nucleus (a supermassive black hole is one whose mass exceeds a million solar-masses.) A key unresolved issue in galaxy formation and evolution is the role these SMBHs play in shaping their galaxies. Most astronomers agree that there must be a strong connection because of the observed correlations between a SMBH's mass and its galaxy's luminosity, stellar mass, and the stellar motions in the galaxy. These correlations apply both in local galaxies and those at earlier cosmic epochs. But despite progress in studying SMBHs, how they effect their hosts still not understood. In some suggested scenarios the SMBH suppresses star formation in the galaxy by expelling material. In others, like the merger scenario, the effect is the opposite: the SMBH boosts star formation by helping stir up the interstellar medium. Computer simulations have been undertaken to try to settle these differences, and they tend to show that cold gas flowing in from the intergalactic medium can feed both SMBH and galaxy growth.
Star formation is one of the principle markers of galaxy growth. Observations of galaxies have tried to measure the star formation by correlating the formation rate with the intrinsic luminosity (star formation heats the dust whose infrared emission can dominate the luminosity). However, the emission from the region around a supermassive black hole that is actively accreting, an active galactic nucleus (AGN), can easily be confused with the emission from star formation. X-rays or the emission of highly excited ions can be used to determine the AGN contributions independently, but these measures may be complicated by intervening dust extinction or other effects. Furthermore there is evidence that in small or less luminous galaxies, or in those at earlier cosmic epochs, other factors like element abundances strongly influenced the galaxy's development.
CfA astronomer Belinda Wilkes and Joanna Kuraszkiewicz and five colleagues examined 323 galaxies known to host AGN from their strong X-ray emission (as measured by the XMM-Newton telescope) and also to have active star formation underway as determined by their far infrared emission (as measured with the Herschel Space Telescope). The galaxies are all at distances such that their light has been traveling from between about two to eleven billion years. Their statistical analysis of the sample finds that on average the AGN contributes about 20% to the infrared luminosity although it can sometimes be as much as >90%. They reach the important conclusions that there is no evidence (at least in this set of objects) for a strong correlation between the two or that AGN quench the star formation. In fact, it appears that both grow together.
"Is There a Relationship Between Agn and Star Formation in Ir-Bright Agns?" Y. Sophia Dai, Belinda J. Wilkes, Jacqueline Bergeron, Joanna Kuraszkiewicz, Alain Omont, Adam Atanas, and Harry I. Teplitz, MNRAS 478, 4238, 2018.