Physical Properties of H ii Regions in M51 from Spectroscopic Observations. (10th August 2020)

• Record Type: Journal Article
• Authors: Wei, Peng; Zou, Hu; Kong, Xu; Zhou, Xu; Hu, Ning; Lin, Zesen; Mao, Yewei; Lin, Lin; Zhou, Zhimin; Liu, Xiang; Ma, Shuguo; Ma, Lu; Zhong, Tuhong; Dang, Fei; Sun, Jiantao; Lin, Xinkui
• Is Part Of: Publications of the Astronomical Society of the Pacific. Volume 132:Number 1015(2020)
• Publication Date: 2020-08-10
• Subjects: Galaxy abundances -- Galaxy evolution -- H II regions -- Interstellar dust extinction -- Interstellar medium -- Star formation; Astronomy -- Periodicals; Astronomy; Periodicals; Periodicals; 520.5
• DOI: 10.1088/1538-3873/ab9d92
• Languages: English
• ISSNs: 0004-6280

Abstract

Abstract: M51 and NGC 5195 is an interacting system that can be explored in great details with ground-based telescopes. The H ii regions in M51 were observed using the 2.16 m telescope of the National Astronomical Observatories of the Chinese Academy of Sciences and the 6.5 m Multiple Mirror Telescope with spatial resolution of less than ∼100 pc. We obtain a total of 113 spectra across the galaxy and combine the literature data of Croxall et al. to derive a series of physical properties, including the gas-phase extinction, stellar population age, star formation rate (SFR) surface density, and oxygen abundance. The spatial distributions and radial profiles of these properties are investigated in order to study the characteristics of M51 and the clues to the formation and evolution of this galaxy. M51 presents a mild radial extinction gradient. The lower gas-phase extinction in the north spiral arms compared to the south arms are possibly caused by the past encounters with the companion galaxy of NGC 5195. A number of H ii regions have the stellar age between 50 and 500 Myr, consistent with the recent interaction history by simulations in the literatures. The SFR surface density presents a mild radial gradient, which is ubiquitous in spiral galaxies. There is a negative metallicity gradient of −0.08 dex R e − 1 in the disk region, which is also commonly found in many spiral galaxies. It is supported by the "inside-out" scenario of galaxy formation. We find a positive abundance gradient of 0.26 dex R e − 1 in the inner region. There are possible reasons causing the positive gradient, including the freezing of the chemical enrichment due to the star-forming quenching in the bulge and the gas infall and dilution due to the pseudobulge growth and/or galactic interaction.