A spectroscopic study of the low redshift dwarf galaxy SDSS J134326.99+431118.7 to calculate star formation rate

  • Daya Nidhi Chhatkuli Central Department of Physics, Tribhuvan University https://orcid.org/0000-0002-8040-6902
  • Sanjaya Paudel Research Professor, Younsei University, Seoul, South Korea
  • Binil Aryal Central Department of Physics, T. U.
Keywords: Dwarf galaxy, Star formation rate, Characteristic peaks, H_α line

Abstract

We present a spectroscopic study of an interacting emission-line dwarf galaxy SDSS J134326.99+431118.7. We analyzed eight-strong emission lines of wavelength in a range of 3902.1Å to 6619.1Å. Among them, the strongest emission line is OIII, with an intensity of 1043.6 x 10-17 erg/s/cm2/Å. These characteristic lines show a perfect Gaussian fit with a coefficient of regression greater than 98%, where the derived full width half maximum (FWHM) is less than 3.8 Å. The line ratio between Ha  and Hb, (Ha/ Hb), is  2.73. This suggests that the galaxy is a starburst galaxy. Star Formation Rate (SFR) of the galaxy derived from Ha  emission line flux is 0.019  and emission line metallicity derived from flux ratio between NII and Ha is 7.85 dex. These morphological and physical properties of SDSSJ134326.99+431118.7 are very similar to those of a typical Blue Compact Dwarf (BCD) galaxy. We conclude that we have presented another evidence of forming a BCD-type galaxy through a merger.

BIBECHANA 18 (1) (2021) 100-107

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Author Biographies

Sanjaya Paudel, Research Professor, Younsei University, Seoul, South Korea

Research Professor, Department of Physics, Younsei University.

Binil Aryal, Central Department of Physics, T. U.

Professor of Physics, CDP

Published
2021-01-01
How to Cite
Chhatkuli, D., Paudel, S., & Aryal, B. (2021). A spectroscopic study of the low redshift dwarf galaxy SDSS J134326.99+431118.7 to calculate star formation rate. BIBECHANA, 18(1), 100-107. https://doi.org/10.3126/bibechana.v18i1.29466
Section
Research Article