Projects
NGC5972 jet feedback
August 2021 - February 2025
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Ali et al. 2025
Cartoon schematic diagram showing various mechanisms at play in NGC5972. The green helix represents the [O III] emission as observed from the HST image. The jet axis is indicated by the red line, and the radio emission is depicted by the dotted red lobes. The black clouds denote the shock regions perpendicular to the jet, as determined by BPT analysis. The red and blue structures represent the outflow region in the galaxy. The shocked cocoon is shown in yellow.
It is widely accepted that active galactic nuclei (AGN) feedback in the form of radio jets, radiation, and/or winds has a significant impact on the surrounding interstellar medium. However, the role of photoionization (by the accretion disk) vs that of shock ionization (by jets/winds) has not yet been unambiguously disentangled. Previous studies have shown that the spatial coincidence between optical and radio emission could indicate AGN jet/wind induced shock. However, there is a still lack of comprehensive understanding of the effects of highly energetic jets on the host and its immediate surroundings.
We intend to study the relationship between radio jets and the distribution and kinematics of the ionized gas in NGC5972, a "Voorwerp" galaxy. Our primary objective is to quantify the contribution of the jet to the feedback mechanism by analyzing the correlations between radio emission and optical [OIII] emission in extended emission line regions spanning several kiloparsecs. To achieve this, we are utilizing EVLA, GMRT polarization data and MUSE IFU spectroscopic data.
Probing Cosmology: Gravitational Lensing and Precision with GW+EM Lensed Signal
September 2023 - June 2024
Detecting gravitational waves (GW) in combination with electromagnetic (EM) counterpart signals holds the potential to serve as an excellent cosmological probe (Liao et al. 2017). Thus, this project is focused on stimulating systems having compact binary coalescence (CBC) to study the GW+EM signals. We aim to use the gravitational lensing method to constrain the value of cosmological parameters to contribute a deeper understanding of the fundamental properties of the universe.
Our research methodology involves the creation of realistic Hubble Space Telescope (HST) image simulations tailored to various lens system configurations using the software "Glafic (Oguri 2010)." These simulations employ various mass and light profile for data generation. A central aspect of our project is to test the accuracy of lens modeling in terms of uncertainties in the Fermat potential δ(Δψ) from lensed GW+EM system. We created mock datasets for multiple lensing configurations, optimized best-fit lens models using chi-square analysis, and calculated differences in the lensing potential that could arise if model assumptions deviate from the true system. In particular, we investigated how uncertainties in the inferred Fermat potential could stem from mismatches between the mock and model configurations — specifically by varying the noise profiles, as well as the underlying mass density and light distribution models. This allowed us to quantify the sensitivity of lens modeling accuracy to different systematic factors.