Study of Star Formation Rate and Metallicity of an Interacting Dwarf Galaxy NGC 2604

Authors

  • Daya Nidhi Chhatkuli Central Department of Physics, Tribhuvan University, Kirtipur, Kathmandu
  • Sanjaya Paudel Centre for Galaxy Evolution Research, Department of Astronomy, Yonsei University, Seoul
  • Binil Aryal Central Department of Physics, Tribhuvan University, Kirtipur, Kathmandu

DOI:

https://doi.org/10.3126/jist.v25i2.33736

Keywords:

Dwarf galaxy, Characteristic peaks, Extinction, Hα line, Metallicity, Star formation rate

Abstract

We present a study of the Sloan Digital all Sky Survey Data Release 12 (SDSS DR12) optical spectra of an interacting dwarf galaxy NGC 2604 that has redshift 0.0069. Thirteen characteristic emission lines were identified in the wavelength range of 3885 Å to 6742 Å, the strongest line was due to Hα emission with a value of emission-line flux 1538.8 erg/s/cm2/Å. The other twelve emission lines were observed because of OI doublet, Hβ, Hγ, Hδ, OIII doublet, HeI, SII doublet and NII doublet transitions. Eleven characteristic lines agreed perfectly with the Gaussian distribution with greater than 99.9 % coefficient of regression. However, full-width half maximum (FWHM) was found to be less than 5 Å. No absorption metallic lines were observed in the spectra which indicates that the galaxy was either newly formed. The line metallicity of the galaxy was found to be 8.4 dex and the extinction coefficient was 0.2134. The star formation rate due to Hα emission after extinction correction was found to be 0.0927 Mʘ year -1 which is almost double of the value (0.057 Mʘ year -1) before correction.

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Published

2020-12-25

How to Cite

Chhatkuli, D. N., Paudel, S., & Aryal, B. (2020). Study of Star Formation Rate and Metallicity of an Interacting Dwarf Galaxy NGC 2604. Journal of Institute of Science and Technology, 25(2), 55–60. https://doi.org/10.3126/jist.v25i2.33736

Issue

Vol. 25 No. 2 (2020)

Section

Research Articles

License

The views and interpretations in this journal are those of the author(s). They are not attributable to the Institute of Science and Technology, T.U. and do not imply the expression of any opinion concerning the legal status of any country, territory, city, area of its authorities, or concerning the delimitation of its frontiers of boundaries.

The copyright of the articles is held by the Institute of Science and Technology, T.U.