Multi-Wavelength Statistics of Clumpy Galaxies

Authors' Affiliations

Isaiah Cox and Dr. Beverly Smith, Department of Physics and Astronomy, College of Arts and Sciences, East Tennessee State University, Johnson City TN.

Location

Ballroom

Start Date

4-5-2018 8:00 AM

End Date

4-5-2018 12:00 PM

Poster Number

14

Name of Project's Faculty Sponsor

Beverly Smith

Faculty Sponsor's Department

Physics and Astronomy

Classification of First Author

Undergraduate Student

Type

Poster: Competitive

Project's Category

Natural Sciences

Abstract or Artist's Statement

We calculated the fraction of ‘clumpy’ galaxies (fclumpy) for three samples of nearby galaxies. These samples include interacting galaxies with strong tidal features, collisional ring galaxies, and normal spiral galaxies. We define a ‘clumpy’ galaxy as a galaxy that has luminous star-forming regions contributing more than 8% of the total flux for the galaxy. We calculate fclumpy for 16 different wavelengths. We find that fclumpy is highest in the ultraviolet, Hα, and 24μm, while fclumpy is the lowest in optical and near-infrared wavelengths. We also see a significant increase in fclumpy for the interacting samples compared to the normal spirals.

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Apr 5th, 8:00 AM Apr 5th, 12:00 PM

Multi-Wavelength Statistics of Clumpy Galaxies

Ballroom

We calculated the fraction of ‘clumpy’ galaxies (fclumpy) for three samples of nearby galaxies. These samples include interacting galaxies with strong tidal features, collisional ring galaxies, and normal spiral galaxies. We define a ‘clumpy’ galaxy as a galaxy that has luminous star-forming regions contributing more than 8% of the total flux for the galaxy. We calculate fclumpy for 16 different wavelengths. We find that fclumpy is highest in the ultraviolet, Hα, and 24μm, while fclumpy is the lowest in optical and near-infrared wavelengths. We also see a significant increase in fclumpy for the interacting samples compared to the normal spirals.