BIBECHANA Vol. 21, No. 2, August 2024, 95-102 ISSN 2091-0762 (Print), 2382-5340 (Online) Journal homepage: http://nepjol.info/index.php/BIBECHANA Publisher:Dept. of Phys., Mahendra Morang A. M. Campus (Tribhuvan University)Biratnagar Dwarf galaxy merger-induced star formation rate: A case study of Mrk 1481 Daya Nidhi Chhatkuli1,∗, Sanjaya Paudel2, Amrit Sedain3 Binil Aryal4 1Tri-Chandra Multiple Campus, Tribhuvan University, Kathmandu, Nepal 2Department of Astronomy, Yonsei University, Seoul 03722, Republic of Korea 3Institut für Physik und Astronomie, Universität, Potsdam, Karl-Liebknecht-Str. 24/25, 14476 Golm, Germany 4 Office of Institute of Science and Technology, Tribhuvan University Kathmandu, Nepal ∗Corresponding author. Email: chhatkulidn@gmail.com Abstract The merger of the galaxies serves as a trigger for the increase in the galaxy’s star formation rate (SFR), which can be quantified by observing the column density of the Hα line. Our findings report the presence of various gas and metal emission lines, strongly indicating that the galaxy hosts very young stars and is currently undergoing active star formation processes. Notably, we report a relatively high SFR of ∼ 0.0055 M⊙ yr-1 for a dwarf galaxy, alongside a metallicity level of 12 + log(O/H) ∼ 8.88 dex. Our photometric analysis reinforces the notion that the galaxy is in the midst of a merger phase. Additionally, the analysis indicates that the galaxy has a relatively flat shape (Sérsic index ∼ 0.8), with stars distributed more broadly and less concentrated toward its center. This provides further evidence of the ongoing merger and its impact on the galaxy’s structure. The half-light radius of the galaxy is estimated to be 2.73 arcsec by using the Petrosian method. Keywords Dwarf Galaxy, Galaxy Merger, Star Formation Rate, Galaxy Morphology. Article information Manuscript received: November 30, 2023; Revised: January 16, 2024; Accepted: January 24, 2024 DOI https://doi.org/10.3126/bibechana.v21i2.60334 This work is licensed under the Creative Commons CC BY-NC License. https://creativecommons. org/licenses/by-nc/4.0/ 1 Introduction Galaxies are captivating celestial entities, offering a window into the cosmos. Their study provides valu- able insights into the origins and dispersion of ele- ments and energy, shedding light on the enigmatic forces of dark matter and dark energy shaping the universe [1–3]. Galaxy mergers represent a crucial aspect of galactic evolution, wherein two or more galaxies combine, resulting in a single, larger entity. These mergers engender interactions among stars, 95 http://nepjol.info/index.php/BIBECHANA chhatkulidn@gmail.com https://doi.org/10.3126/bibechana.v21i2.60334 https://creativecommons.org/licenses/by-nc/4.0/ https://creativecommons.org/licenses/by-nc/4.0/ Daya Nidhi Chhatkuli et al./ BIBECHANA 21 (2024) 95-102 96 gas, dust, and dark matter, leading to the redis- tribution and reconfiguration of the newly formed galaxy’s components. Spanning millions to billions of years, these processes exert a profound influence on the structure, star formation history, and evo- lution of the resultant galaxy. Additionally, galaxy mergers can trigger intense starbursts and are as- sociated with the formation of some of the uni- verse’s most massive galaxies. These mergers pri- marily occur due to gravitational forces, giving rise to major mergers between comparably sized large galaxies, minor mergers where smaller galaxies are absorbed by larger ones, cannibal mergers where a smaller galaxy is absorbed by a larger one, and tidal mergers where galactic tidal forces pull stars together. Dry galaxy mergers, specifically involv- ing galaxies with limited gas and dust, often lead to the creation of elliptical or spiral galaxies, de- pending on the galaxies involved, playing a piv- otal role in reshaping galactic structures and fea- tures, even when their gas and dust reservoirs are depleted [4–6]. Studying dwarf-dwarf galaxy merg- ers is important because dwarf galaxies were com- mon in the early universe and drove galaxy merg- ers. Yet, these mergers are often too far away to see directly, and finding low-redshift ones with dual active galactic nuclei (DAGN) is tough. In a recent study, scientists found the first two DAGN candi- dates in these mergers, known for their telltale tidal signs and dual, bright X-ray sources, likely linked to actively feeding massive black holes. More research will give us valuable insights into how galaxies grew early on, how black holes formed in their centers, and how mergers triggered star formation [7–9]. The star formation rate (SFR) measures the rate at which new stars form, driven by the gravitational collapse of interstellar gas and dust into protostars and stars. Various factors influence SFR, including interstellar medium density, composition, tempera- ture, and nearby stars. Methods for SFR measure- ment include observations of star-forming regions, infrared surveys, and calculations based on region mass and star formation time. SFR plays a pivotal role in galaxy evolution, star distribution, and un- derstanding galaxy formation. In galaxy mergers, SFR can significantly rise due to increased gravita- tional potential, compressing gas and dust and re- distributing them, fostering higher star formation. Studying SFR during mergers offers insights into how these events influence star formation dynamics and galaxy evolution, with a notable connection to metallicity, as higher metallicity enhances gas cool- ing efficiency, promoting increased SFR, while lower metallicity can suppress it, as observed in galaxies such as the Milky Way [10–13]. Merging galaxies exhibit elevated metallicity levels compared to normal galaxies because the gas in mergers, which is abundant, gets transformed into stars, enriching the galaxy with metals. This heightened metal abundance results from the sub- stantial star and gas content in merging galax- ies. Moreover, metals in merging galaxies can re- distribute to other galaxies, further boosting their metallicity [8, 14–16]. Galaxy morphology is a fundamental field in as- tronomy that explores the shapes and structures of galaxies. It enables us to uncover the secrets of how galaxies form and evolve, providing valuable insights into the broader structure of the universe. One of the major advantages of galaxy morphology is the ability to understand the various life stages of the galaxy’s evolution and the influence of external factors such as mergers [17,18]. The surface bright- ness profile of a galaxy, essential for understanding its structure and components like the bulge, disk, and halo, is typically determined by analyzing the distribution of light from stars and gas. The Sér- sic profile, a mathematical model, is developed by Miguel A. Sérsic, quantifies this brightness distribu- tion, aiding in galaxy shape characterization via the Sérsic index (n) – low n values suggest diffuse galax- ies, while high n values indicate concentrated ones. The profile helps distinguish galaxy types, such as ellipticals and spirals, determine galaxy size (effec- tive radius), and estimate total luminosity for mass calculations. To understand the complex dynamics and morphology of interacting dwarf galaxy, we can employ a double Sérsic profile model [19]. Here, we present the study of the morphology of a merging dwarf galaxy, Mrk 1481, and calculate its SFR by using the flux of the emission line of the galaxy spectrum. Moreover, we estimate the size and Sérsic index of the galaxy. 2 Material and Methods 2.1 Sample Selection Interacting dwarf galaxies present fascinating op- portunities for the study of their photometric char- acteristics. In our investigation, we focused on a tidally interacting dwarf galaxy, Mrk 1481, of low redshift (z = 0.0059) with a radial velocity of 1803 km s-1 selected from the catalog by Paudel et. al, 2018 [20]. The apparent g and r-band magnitudes of the galaxy are 16.48 mag and 15.87 mag respec- tively. Its absolute B-band magnitude is -15.49 mag. It has a stellar mass of 2.2 × 108 M⊙. This specific galaxy, Mrk 1481, is situated at celestial coordinates R. A. (J2000): 13h 42m 59.4s and Dec. (J2000): 52° 41' 17.88". We determined its distance to be approximately 25.03 Mpc, calculated from its redshift, assuming a flat universe and adopting cos- mological parameters (H0 = 71 km s-1 Mpc-1, Ωm = 0.3, and Ω∧ = 0.7). The number of neighbors within the search criteria (sky-projected distance Daya Nidhi Chhatkuli et al./ BIBECHANA 21 (2024) 95-102 97 of fewer than 700 kpcs and a relative line-of-sight radial velocity of less than ± 700 km/s) is 9, and it has no satellite. Notably, the mass ratio between the interacting dwarf galaxies M1 and M2 is 20. The SDSS optical image and its spectrum are shown in Figure 1. In the image, the blue part repre- sents the area where stars are currently forming in the galaxy. This is mainly happening because of the gravitational pull between the two dwarf galax- ies, which causes them to interact. The spectrum shows strong emission lines, which indicates that the galaxy is an emission type. Figure 1: The SDSS optical image of the emission-type interacting dwarf galaxy Mrk 1481 is shown in the left panel and its optical spectrum is shown in the right panel. The X-axis is the rest-frame wavelength and Y-axis is flux. 2.2 Data Analysis We examine the gas content of the galaxy by ana- lyzing its optical spectrum obtained from the SDSS Data Archive Server (DAS). Our analysis aims to understand the galaxy’s composition. It is impor- tant to note that we relied on archival data and didn’t apply any additional data processing to the galaxy’s spectra. To reproduce the spectra from the SDSS data server, we utilize a tool called TOPCAT. The SDSS fiber, which collects this data, has a di- ameter of 3 arcsecs, covering only a small portion of the galaxy. The SDSS optical spectrum ranges from 4,000 Å to 7,000 Å, encompassing key emis- sion and absorption lines often used to study the chemical properties of stars and galaxies. We used a Gaussian fit analysis to examine the prominent emission lines in the spectra, revealing a combination of hydrogen and metal lines within the galaxy. To calculate the galaxy’s star-formation rate, we applied the Kennicutt initial mass function and used neutral hydrogen’s luminosity. This ap- proach is based on [21,22]. We took a closer look at the way the interacting galaxy appears in pictures to figure out where its tidal effects come from. The major axis light profile of the galaxy is extracted by using the Image Reduction and Analysis Facil- ity (IRAF) task ellipse, and the best-fitted elliptical isophotes are drawn on the image as described by Jedrzejewski [23]. To estimate the galaxy’s size, we applied the Sérsic profile [24], which helps us un- derstand how big the galaxy is. We also used Pho- tutils to see how the galaxy’s shape changes over time. This helped us getting a better idea of what the galaxy looks like by studying its brightness pat- terns in images. We obtained the g-band image of the galaxy from the SDSS data server and employed IRAF to generate the fitted image of the galaxy us- ing the Sérsic profile. In the following section, we will delve into the outcomes of our analysis. 3 Results and Discussion 3.1 Spectroscopic Analysis In our study, we focused on analyzing the galaxy’s key emission lines, including Hβ , OIII5008, Hα and NII6585, (see Figure 2). Black dots correspond to the observed flux, while the red solid lines depict the Gaussian fit applied to the galaxy’s data. These lines are significant for assessing the SFR and gain- ing insights into the galaxy’s metallicity. The major cause of the broadening of the characteristic lines is Doppler's broadening. The Balmer decrement is the ratio of the fluxes in the Hα and Hβ lines often used to estimate the amount of dust along the line of sight. The Balmer decrement is used in astronomy to measure the red- Daya Nidhi Chhatkuli et al./ BIBECHANA 21 (2024) 95-102 98 dening and attenuation of light from astronomical objects, particularly in the study of galaxies and nebulae. The Balmer decrement is also used to de- termine the dependence of the Balmer decrement with galaxy stellar mass and to study the evolu- tion of the Balmer decrement with redshift [25]. We calculated the value of Balmer increment to be 3.15. In the context of a merging dwarf galaxy, a Balmer decrement of 3.15 indicates a significant amount of dust, which affects the observed colors and spectra of the galaxy. This value suggests that the light from the galaxy is being heavily scattered and absorbed by dust, impacting the interpretation of its properties and the processes occurring within it [26–28]. The galaxy’s star formation rate determined from the neutral hydrogen line before extinction correction stands at 0.0046 M⊙yr−1. The SFR is significantly influenced by the presence of dust particles in the interstellar medium, particularly impacting the Hα emission, where a substantial amount is absorbed. To address this, we calcu- lated the galaxy’s extinction coefficient, which is measured to be 0.1997. It’s worth noting that the Hβ line is less affected by dust particle interaction. Consequently, after correcting for extinction, the SFR of the galaxy is 0.0055 M⊙yr−1 which is al- most similar to the Zhao et al. [29], where they calculated star formation as 0.0058 M⊙yr−1 and af- ter the extinction correction, 0.0339 M⊙yr−1. This high value of SFR of this galaxy indicates that the galaxy is actively forming stars at a significant rate. The high SFR can lead to the formation of mas- sive stars, which can then die in supernova explo- sions and enrich the surrounding environment with heavy elements [30]. For the full calculation of the star formation rate and the extinction correction, see [7]. We also determined the metallicity ratios for some of the prominent lines, providing insights into the galaxy’s evolution and characteristics. Gas- phase metallicity is commonly assessed by calcu- lating the oxygen abundance relative to hydrogen, defined as 12 + log(O/H). This is due to oxygen’s significance in both the mass of the universe and the electron temperature of the gas. In our analysis, we found that the metallicity of our interacting dwarf galaxy stands at 8.86 dex [31] calculated as 8.69 dex). This suggests that the galaxy’s outer regions have become hotter because the ionizing photons have been absorbed by the metals, impacting their properties. A high value of metallicity means that the galaxy contains a significant number of heavy elements, such as iron, in its stellar population [32]. 3.2 Photometric Analysis In our study, we employed Photutils to analyze the galaxy’s isophotes and their orientation, as depicted in the upper left panel of Figure 3. The evident twisting in these isophotes strongly indicates that the galaxy is undergoing a merger phase, leading to continual alterations in their appearance. We have also examined how the galaxy’s ellipticity and posi- tion angle change with its radius, as depicted in the upper-right panel of Figure 3. Notably, the galaxy appears nearly spherical towards its center, but as we move outward, it becomes more elliptical. This suggests that the outer regions of the galaxy are be- coming more elongated, indicating a potential tidal connection and influence. We used the Sérsic profile to model the galaxy’s surface brightness profile, as shown in the lower left panel of Figure 3. The Sérsic index for the fit, represented by “n”, is 0.8, and we measured an ef- fective radius of 6.62 arcseconds. These values in- dicate that the galaxy has a relatively flat bright- ness distribution, resembling an exponential profile. This suggests that the distribution of stars is more spread out and less concentrated toward the center. The Petrosian radius is a measure of the size of a galaxy, and it is derived from the Petrosian function, which helps in characterizing the overall extent of a galaxy’s light profile. It takes into ac- count variations in a galaxy’s brightness, making it particularly useful for galaxies with diverse struc- tures. The Petrosian index is a dimensionless profile that represents the rate of change of surface bright- ness with radius in a galaxy's light profile. The Petrosian index is useful in determining radial con- centrations of galaxy light profiles and performing accurate measurements of galaxy radii [33]. In our analysis, we calculated the Petrosian radius, specif- ically with a Sérsic index (n) of 0.2, which indicates how much light is distributed at different distances from the galaxy’s center. At a distance of 2ap (twice the Petrosian ra- dius), we assume that the Petrosian profile encom- passes the entirety of the galaxy’s brightness. This assumption allows us to effectively capture the over- all extent of the galaxy’s light distribution seen in the lower right panel of Figure 3. Moreover, the half-light radius of the galaxy is estimated to be 2.73 arcsec. Daya Nidhi Chhatkuli et al./ BIBECHANA 21 (2024) 95-102 99 Figure 2: The figure illustrates the Gaussian profile of the galaxy’s prominent emitted spectral lines Hβ , OIII5008, Hα, and NII6585. The error bars reflect the percentile error associated with the observations. We show a conservative estimate of the flux error in the plot, i.e., 10% of the observed flux provided by the SDSS webpage (https://www.sdss.org/dr15/spectro/caveats/). The wavelengths given in the X-axis are redshift corrected. Figure 3: Caption of Figure 3 is given in next page. Daya Nidhi Chhatkuli et al./ BIBECHANA 21 (2024) 95-102 100 Figure 3 (Caption): The upper left panel shows the isophotes of the interacting dwarf galaxy, Mrk 1481. The green ellipses represent the contour levels of the galaxy. The upper right panel shows the radial profile of position angle and ellipticity. The brightness profile of the galaxy is illustrated in the lower left panel, where the black dots represent the observed data and the blue solid line depicts the 1D Sérsic fitting of the galaxy. The lower right panel shows the radial profile of the Petrosian index and cumulative intensity at the g-band. The vertical dashed line represents the Petrosian radius at Sérsic index 0.2 (horizontal brown line). The vertical green-colored dashed line intersects the curve at a half-light radius. 4 Conclusion In our comprehensive analysis of the spectroscopic and photometric attributes of the interacting dwarf galaxy, Mrk 1481, we made a noteworthy discovery. Our observations revealed the presence of highly prominent gas emission lines, indicating that the galaxy is currently undergoing a starburst phase, with the formation of very young stars in progress. To quantify this star formation activity, we con- ducted Gaussian profile fits of the emission lines and calculated the total flux, a key parameter in determining the galaxy’s star formation rate. Our findings indicate a remarkably high star formation rate, measuring at 0.0046 M⊙yr−1 when using the Hα lines. However, after applying an extinction cor- rection, this rate increases to 0.0055 M⊙yr−1. This adjustment underscores the active nature of star formation within the galaxy, highlighting the inten- sity of this ongoing process. We also calculated the metallicity of the galaxy which comes out 8.88 dex, and it shows that the galaxy is very metal-rich and young stars are forming. Additionally, we delved into the photometric characteristics of the galaxy. We employed a Sérsic profile to model the galaxy, with a Sérsic index of 0.8 and a half-light radius of 2.73 arcseconds. The analysis of changing ellip- ticity and position angle of the galaxy has led us to the observation that the galaxy is undergoing a merger, particularly at its outer regions, indicating a potential tidal connection and influence. Acknowledgements Daya Nidhi Chhatkuli acknowledges the University Grants Commission of Nepal, for financial support (Award No.: PhD-75/76-S & T-13) to carry out this research. This study is based on the archival images and spectra from the Sloan Digital Sky Survey (http://www:sdss.org/collaboration/credits.html ). A Brief Statement on the Observational Data Sources The Sloan Digital Sky Survey (SDSS) is a com- prehensive astronomical survey that has played a pivotal role in mapping the night sky and gather- ing data on a vast number of celestial objects. Ob- servations of celestial objects, including Mrk 1481, often involve multiple telescopes and instruments across different wavelengths. We use SDSS data to study the spectra, photometry, and other charac- teristics of galaxies, quasars, and various celestial bodies. To understand Mrk 1481, we have used SDSS data to analyze its spectral features, measure its redshift, study its morphology, and derive in- formation about its physical properties. The SDSS data is publicly accessible and has become an in- valuable resource for astronomers worldwide. 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The Astronomical Jour- nal, 163(5):202, 2022. https://doi.org/10. 3847/1538-3881/ac5908 http://doi.org/10.1093/mnras/stv626 http://doi.org/10.1093/mnras/stv626 http://doi.org/10.3126/jnphyssoc.v7i4.42928 http://doi.org/10.3126/jnphyssoc.v7i4.42928 http://doi.org/10.1088/0004-6256/141/2/68 http://doi.org/10.1088/0004-6256/141/2/68 https://iopscience.iop.org/article/10.1086/316471/pdf https://iopscience.iop.org/article/10.1086/316471/pdf http://doi.org/10.1086/322874 http://doi.org/10.1086/322874 https://doi.org/10.3847/1538-3881/ac5908 https://doi.org/10.3847/1538-3881/ac5908 Introduction Material and Methods Sample Selection Data Analysis Results and Discussion Spectroscopic Analysis Photometric Analysis Conclusion