Strong dusty bursts of star formation in galaxies falling into the cluster RXJ0152.7-1357

Details Strong dusty bursts of star formation in galaxies falling into the cluster RXJ0152.7-1357 Strong dusty bursts of star formation in galaxies falling into the cluster RXJ0152.7-1357

2006-10-19

arxiv.org/abs/astro-ph/0610578v1

Astrophys.J.654:825-834,2007

Astronomy and Astrophysics

Astrophysics

12 pages, 6 figures, accepted for publication in ApJ. A full resolution version and fig.2 are available at http://mips.as.ar

Scientific paper

10.1086/509107

We have observed the cluster RX J0152.7-1357 (z$\sim$0.83) at 24$\mu$m with the Multiband Imaging Photometer for Spitzer (MIPS). We detected twenty-two sources associated with spectroscopically confirmed cluster members, while ten more have photometric redshifts compatible with membership. Two of the 32 likely cluster members contain obvious active nuclei while the others are associated with dusty star formation. The median IR-determined star formation rate among the remaining galaxies is estimated at 22 M$_\odot$$ $yr$^{-1}$, significantly higher than in previous estimates from optical data. Most of the MIR-emitting galaxies also have optical emission lines, but a few do not and hence have completely hidden bursts of star formation or AGN activity. An excess of MIR-emitting galaxies is seen in the cluster in comparison to the field at the same redshift. The MIR cluster members are more associated with previously detected infalling late type galaxies rather than triggered by the ongoing merging of bigger X-ray clumps. Rough estimates also show that ram pressure may not be capable of stripping the gas away from cluster outskirt galaxies but it may disturb the gas enough to trigger the star formation activity. Harassment can also play a role if for example these galaxies belong to poor galaxy groups. Thus, bursts of star formation occur in the cluster environment and could also help consume the galaxy gas content in addition to ram pressure, harassment or galaxy-galaxy strong interactions.

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