Tidal interaction, star formation and chemical evolution in blue compact dwarf galaxy Mrk 22

Paswan, Abhishek; Omar, Amitesh; Jaiswal, Sumit

doi:10.1093/mnras/stx2614

Cited by 10 publications

(7 citation statements)

References 172 publications

(225 reference statements)

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“…The higher electron density, particularly in the density-bounded HII region, is consistent with typical electron density obtained in prior low-redshift LyC/Lyα leakers such as GPs (e.g., Izotov et al 2020a;Guseva et al 2020). In the ionization-bounded HII region (i.e., extended disk outside the circle), it is typical ( 100 cm −3 ), comparable to that observed in normal starforming galaxies (e.g., Guseva et al 2011;Izotov & Thuan 2011;Paswan et al 2018Paswan et al , 2019.…”

Section: Wolf-rayet Feature and Physical Conditions Of Ionized Gassupporting

confidence: 52%

“…For some spaxels, the line flux ratios of f Hα /f Hβ are found to be below the expected theoretical value of 2.86. A low value of f Hα /f Hβ is often associated with intrinsically low reddening, and hence we assumed an internal E(B − V ) values as zero for such cases (e.g., Paswan et al 2018Paswan et al , 2019. Throughout this work, we have used only those emission lines whose signal-to-noise ratio (SNR) is 3.…”

Section: Datamentioning

confidence: 99%

See 1 more Smart Citation

SDSS-IV MaNGA: an observational evidence of density bounded region in a Lyman-$α$ emitter

Paswan,

Saha,

Leitherer

et al. 2021

Preprint

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Using Integral Field Unit (IFU) spectroscopy, we present here the spatially resolved morphologies of [SII]λ6717,6731/Hα and [SII]λ6717,6731/[OIII]λ5007 emission line ratios for the first time in a Blueberry Lyman-α emitter (BBLAE) at z ∼ 0.047. Our derived morphologies show that the extreme starburst region of the BBLAE, populated by young ( 10 Myr), massive Wolf-Rayet stars, is [SII]-deficient, while the rest of the galaxy is [SII]-enhanced. We infer that the extreme starburst region is density-bounded (i.e., optically thin to ionizing photons), and the rest of the galaxy is ionization-bounded − indicating a Blister-type morphology. We find that the previously reported small escape fraction (10%) of Lyα photons is from our identified densitybounded HII region of the BBLAE. This escape fraction is likely constrained by a porous dust distribution.We further report a moderate correlation between [SII]-deficiency and inferred Lyman Continuum (LyC) escape fraction using a sample of confirmed LyC leakers studied in the literature, including the BBLAE studied here. The observed correlation also reveals its dependency on the stellar mass and gas-phase metallicity of the leaky galaxies. Finally, the future scope and implications of our work are discussed in detail.

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Section: Wolf-rayet Feature and Physical Conditions Of Ionized Gassupporting

confidence: 52%

Section: Datamentioning

confidence: 99%

SDSS-IV MaNGA: an observational evidence of density bounded region in a Lyman-$α$ emitter

Paswan,

Saha,

Leitherer

et al. 2021

Preprint

View full text Add to dashboard Cite

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“…A low value of f Hα /f Hβ is often associated with intrinsically low reddening and hence we assumed a E(B -V) internal as zero for such cases. Previously, lower than theoretical value of f Hα /f Hβ has been reported in several galaxies (López-Sánchez & Esteban 2009;Ramya et al 2009;Gunawardhana et al 2013;Paswan et al 2018). Such low value is usually believed as resulted from variations in physical conditions of ionized gas such as high electron temperature or low electron density in the emission region for which the theoretical ratio f Hα /f Hβ may be less than 2.86 (e.g., Grinin 1980;López-Sánchez & Esteban 2009).…”

Section: Results and Analysismentioning

confidence: 92%

Optical spectroscopy of star-forming regions in dwarf Wolf–Rayet galaxies

Paswan

Omar

Jaiswal

2018

Monthly Notices of the Royal Astronomical Society

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We present here spatially-resolved optical spectroscopic observations of four nearby dwarf Wolf-Rayet (WR) galaxies. The ages of the most recent starburst events in these galaxies are found between 3 and 10 Myr. The gas-phase metallicities [12+log(O/H)] for the spatially-resolved star-forming regions are derived using several indicators. The star-forming regions within the galaxies are found chemically homogeneous within the uncertainties in the estimates. Nitrogen-enrichment as expected in the WR regions is not detected. This implies that metal-enrichment due to supernovae explosions in the most recent star-forming episode is not being detected here. It is suggested that the newly synthesized metals still reside in hot gas-phase. The metals from the previous episodes, cooled by now and well mixed across the whole extent of galaxies, are making galaxies chemically homogeneous with normal N/O ratio. These galaxies are residing in dense environments with galaxy density in the range of 8 − 80 Mpc −3 .

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“…Alternatively, it could be a merger system as double nuclei is indicated (Mazzarella et al 1991). Paswan et al (2018) recently found a significant metallicity difference between the two nuclei, which also suggests that MRK 22 could be a merging system of two galaxies.…”

Section: Mrk 22mentioning

confidence: 96%

HI imaging of dwarf star-forming galaxies: Masses, morphologies and gas deficiencies

Jaiswal,

Omar

2020

Preprint

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The GMRT observations of the H i 21 cm-line emission from 13 nearby dwarf star-forming galaxies are presented. These galaxies are selected from the catalogues of Wolf-Rayet galaxies having very young (≤10 Myr) star formation.The ranges of star formation rates and stellar masses of the sample galaxies are 0.03 -1.7 M yr −1 and 0.04 -22.3 ×10 8 M , respectively. The H i line emission is detected from 12 galaxies with peak column density > 1 × 10 21 cm −2 .The 3σ H i column density sensitivities per channel width of 7 km s −1 for low (60 × 60 ) resolution images are in the range 0.8-1.9 × 10 19 cm −2 . The H i channel images, moment images, global profiles and mass surface density profiles are presented here. The average value of the peak H i mass surface density is estimated to be ∼2.5 M pc −2 , which is significantly less compared to that in massive spiral galaxies. The scaling relations of (M stars + M H I + M He ) vs M dyn , gas fraction vs M B , M H I vs M stars , H i-to-stellar mass ratio vs M stars , and M H I vs D H I for the sample galaxies are estimated. These scaling relations can be used to constraint the key parameters in the galaxy evolution models. These galaxies are residing in group environment with galaxy density up to 8 galaxy Mpc −3 . A H i mass deficiency (with DEF HI > 0.3) is noticed in majority of galaxies for their optical diameters as compared to galaxies in field environments. Clear signatures of tidal interactions in these galaxies could be inferred using the H i images. Isolated H i clouds without known optical counterparts are seen in the vicinity of several galaxies. H i emission envelope is found to be having an offset from the optical envelope in several galaxies. Consistent with the previous studies on galaxy evolution in group

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Tidal interaction, star formation and chemical evolution in blue compact dwarf galaxy Mrk 22

Cited by 10 publications

References 172 publications

SDSS-IV MaNGA: an observational evidence of density bounded region in a Lyman-$α$ emitter

SDSS-IV MaNGA: an observational evidence of density bounded region in a Lyman-$α$ emitter

Optical spectroscopy of star-forming regions in dwarf Wolf–Rayet galaxies

HI imaging of dwarf star-forming galaxies: Masses, morphologies and gas deficiencies

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