Spatially Resolved Relationship Between Attenuation and Specific Star Formation Rate in MaNGA
Raisa Rahma Rizkia, Luki Aldila Ahmad, Cut Dafina Khalisha

Institut Teknologi Bandung

Abstract

Dust in galaxies affects the appearance of active star formation regions by absorbing and scattering starlight which can make the regions appear fainter and redder. This effect, dust attenuation, varies across different parts of the galaxy, leading to misinterpretations of star formation activities. We present the relation of dust attenuation (A_V) and specific star formation rate (sSFR) of star-forming spiral galaxies using spatially resolved measurements from the SDSS-IV MaNGA survey and see how this relationship affects the properties of the galaxies, such as galaxy mass, morphology, and inclination. We use two methods to trace dust attenuation: (1) the Balmer decrement (H&#945-/H&#946-) to measure dust attenuation in gas (A_V,gas), and (2) full-spectrum stellar population fitting to measure the dust attenuation for stellar light (A_V,stars). By analyzing these quantities pixel-by-pixel, we explore how dust attenuation correlates with sSFR. Our hypothesis is that A_V,stars will be lower than A_V,gas due to the existence of two dust components: thick dust in stellar birth clouds and diffuse dust in the ISM. This study is important for the understanding of spatially varying dust attenuation in star formation studies and supports a model where dust geometry changes with both local star-forming conditions and global galaxy properties.

Keywords: galaxies: ISM - galaxies: stellar content - galaxies: star formation - galaxies: spiral - ISM: dust - ISM: extinction

Topic: Galaxies and Cosmology

Plain Format | Corresponding Author (Raisa Rahma Rizkia)

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