Multiwavelength Investigations of Hickson Compact Groups of Galaxies: Evolution of Star Formation with UV, IR and X-ray Diagnostics

Details Multiwavelength Investigations of Hickson Compact Groups of Galaxies: Evolution of Star Formation with UV, IR and X-ray Diagnostics Multiwavelength Investigations of Hickson Compact Groups of Galaxies: Evolution of Star Formation with UV, IR and X-ray Diagnostics

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21538606t&link_type=abstract

American Astronomical Society, AAS Meeting #215, #386.06; Bulletin of the American Astronomical Society, Vol. 42, p.601

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Nearby ( Mpc) compact groups of galaxies represent a special high-density environment, which, thanks to their relative proximity, can be studied in detail. The similarity of compact groups to dense environments at high redshift makes them an ideal laboratory for gaining insight on galaxy evolution and transformation in the distant Universe, where merging and interactions are prevalent. We have selected a diverse sample of 12 Hickson Compact Groups (HCGs), and performed observations in the X-ray (Chandra), the UV (Swift/UVOT), the optical (CTIO imaging/spectroscopy), and the IR (2MASS, Spitzer IRAC and MIPS). Until recently, large HCG samples were relatively unexplored in the UV, IR and X-ray wavelength regions. We aim to fully characterize star formation in galaxies of different morphological types and groups of different evolutionary stages. I will present Swift/UVOT 3-color UV data, which we combine with Spitzer and 2MASS IR data, to obtain, for the first time, dust maps and specific star-formation rate (SSFR) estimates for HCGs. I will discuss the interpretation of the 'gap' in mid-IR and SSFR space and how it relates to the proposed evolutionary schemes for compact groups. The X-ray regime also provides valuable information on the evolutionary stage of HCGs. I will discuss results on 5 HCGs from our sample and discuss the relative importance of the diffuse emission and X-ray binary contribution, as a function of stellar mass.

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