Samira Rahimli
Current Organizations / Institutes
The organizations/institutes from the scholar's latest article
Research Subjects
Samira Rahimli has a total of 10 co-authors. Here are the top co-authors by number of shared publications:
- Alexander Serebryanskiy
Fesenkov Astrophysical Institute, Observatory 23, Medeu District, Almaty 050020, Kazakhstan
3 shared publications - Luydmila Kondratyeva
Fesenkov Astrophysical Institute, Observatory 23, Medeu District, Almaty 050020, Kazakhstan
3 shared publications - Nazim Huseynov
Shamakhy Astrophysical Observatory Named After N. Tusi, Shamakhy District, Y. Mammadaliyev Settlement AZ-5626, Azerbaijan
3 shared publications - Saule Shomshekova
Fesenkov Astrophysical Institute, Observatory 23, Medeu District, Almaty 050020, Kazakhstan
3 shared publications - Laura Aktay
Fesenkov Astrophysical Institute, Observatory 23, Medeu District, Almaty 050020, Kazakhstan
2 shared publications - Vitaliy Kim
Fesenkov Astrophysical Institute, Observatory 23, Medeu District, Almaty 050020, Kazakhstan
2 shared publications
Latest Publications
- Open Access
Spectral and Photometric Studies of NGC 4151 in the Optical Range: Current Results
We present the results of long-term photometric and spectroscopic monitoring of the Seyfert galaxy NGC 4151 based on new observational data complemented by archival material spanning several decades. NGC 4151 is one of the most extensively studied active galactic nuclei, exhibiting pronounced variability in both optical continuum and emission-line fluxes, which makes it a key object for investigating physical processes in the central engine and the broad-line region. Our study covers the optical and near-infrared wavelength ranges, including the Ic band and the standard BVRc photometric filters. Using multi-band optical photometry and optical spectroscopy, we construct light curves of the continuum and emission lines and perform a comparative analysis of their temporal behavior during different activity states of the galaxy. The analysis focuses on variability amplitudes, long-term trends, and correlations between photometric and spectral characteristics, allowing us to examine the relationship between continuum variations and the line-emitting regions.
Open AccessSpectral and Photometric Studies of NGC 4151 in the Optical Range: Current Results
We present the results of long-term photometric and spectroscopic monitoring of the Seyfert galaxy NGC 4151 based on new observational data complemented by archival material spanning several decades. NGC 4151 is one of the most extensively studied active galactic nuclei, exhibiting pronounced variability in both optical continuum and emission-line fluxes, which makes it a key object for investigating physical processes in the central engine and the broad-line region. Our study covers the optical and near-infrared wavelength ranges, including the Ic band and the standard BVRc photometric filters. Using multi-band optical photometry and optical spectroscopy, we construct light curves of the continuum and emission lines and perform a comparative analysis of their temporal behavior during different activity states of the galaxy. The analysis focuses on variability amplitudes, long-term trends, and correlations between photometric and spectral characteristics, allowing us to examine the relationship between continuum variations and the line-emitting regions.
- Open Access
Spectral and Photometric Studies of NGC 3516 in the Optical Range
This paper presents the results of the photometric and spectral monitoring of the galaxy NGC 3516, which is an active galactic nucleus (AGN) of type Sy with a changing look. Observations were carried out at the Fesenkov Astrophysical Institute (FAI, Almaty, Kazakhstan) and the Shamakhy Astrophysical Observatory (ShAO, Shamakhy, Azerbaijan). Spectral monitoring of this galaxy in the wavelength range 4000–7000 Å began in 2020, while photometric observations have been conducted since 2014. During the observation period, estimates of the galaxy’s brightness in the B, V and filters were obtained, as well as measurements of the emission line and continuum fluxes. The light curve shows increased brightness of NGC 3516 in 2016 and 2019. The increase of emission line fluxes of H and H and continuum began in 2019 and continued until spring 2020, when these characteristics reached their maximal values. A powerful X-ray flare took place on 1 April 2020. A new phase of brightening began in 2021 and has continued until 2025. After reaching their maxima in 2020, the emission fluxes of H and H decreased by a factor of 1.5–2 and remained at a low level until 2022–2023, when they began to increase again. Medium-resolution spectra obtained on 20 April 2020, with the 1-meter “West” telescope (TSHAO) were used to study the broad components of the H and H emission line profiles. Model calculations showed that the broad profile of the H line consists of a central unshifted component and two (blue and red) components shifted symmetrically relative to the central component by a velocity of km . The H emission line was relatively weak, so the radial velocity of its components was determined with a large uncertainty: km .Open AccessSpectral and Photometric Studies of NGC 3516 in the Optical Range
This paper presents the results of the photometric and spectral monitoring of the galaxy NGC 3516, which is an active galactic nucleus (AGN) of type Sy with a changing look. Observations were carried out at the Fesenkov Astrophysical Institute (FAI, Almaty, Kazakhstan) and the Shamakhy Astrophysical Observatory (ShAO, Shamakhy, Azerbaijan). Spectral monitoring of this galaxy in the wavelength range 4000–7000 Å began in 2020, while photometric observations have been conducted since 2014. During the observation period, estimates of the galaxy’s brightness in the B, V and filters were obtained, as well as measurements of the emission line and continuum fluxes. The light curve shows increased brightness of NGC 3516 in 2016 and 2019. The increase of emission line fluxes of H and H and continuum began in 2019 and continued until spring 2020, when these characteristics reached their maximal values. A powerful X-ray flare took place on 1 April 2020. A new phase of brightening began in 2021 and has continued until 2025. After reaching their maxima in 2020, the emission fluxes of H and H decreased by a factor of 1.5–2 and remained at a low level until 2022–2023, when they began to increase again. Medium-resolution spectra obtained on 20 April 2020, with the 1-meter “West” telescope (TSHAO) were used to study the broad components of the H and H emission line profiles. Model calculations showed that the broad profile of the H line consists of a central unshifted component and two (blue and red) components shifted symmetrically relative to the central component by a velocity of km . The H emission line was relatively weak, so the radial velocity of its components was determined with a large uncertainty: km . - Open Access
- 22 November 2024
- Published by MDPI AG in Preprints.org
Spectral and Photometric Studies of NGC 3516 in the Optical RangeSpectral and Photometric Studies of NGC 3516 in the Optical Range
(1) Background: NGC 3516 is an active Seyfert galaxy, which has become a focal point of astronomical studies due to its variable luminosity and emission lines, linked to the activity of its central supermassive black hole (SMBH). This paper presents an analysis of long-term observations from 2014 to 2024, including photometric and spectroscopic data collected at the Fesenkov Astrophysical Institute (FAI, Kazakhstan) and the Shamakhy Astrophysical Observatory (SHAO, Azerbaijan). The primary aim of this study was to investigate the changes in luminosity and spectral characteristics of NGC 3516, providing insights into the dynamics of the galaxy’s activity and its evolving chemical composition. (2) Methods: The research utilized photometric data in the B, V, R filters, along with spectroscopic observations in the wavelength range of λ4000 Å–λ7000 ÅThe spectroscopic data were normalized to analyze the profiles of emission lines and their variations over time. Broad emission line profiles (Hα and Hβ) were also analyzed to estimate radial velocities. A three-component model was applied, demonstrating a better statistical fit to the observed data, indicating a complex structure and dynamics within the galaxy’s Broad Line Region (BLR).; (3) Results: The main results of the study show that from 2018 to 2024, the brightness of NGC 3516 varied with amplitudes of ΔB=0.35 mag, ΔV=0.18 mag, ΔR=0.20 mag. An increase in brightness was observed in April 2020, likely associated with an X-ray flare detected simultaneously. Spectroscopic observations revealed a gradual weakening of the Hγλ4340 Å emission line starting from mid-2023. Narrow emission lines of [FeII] λ4814.53 Å and [FeVII] λ6087 Å were detected, indicating an active phase of the galaxy in May 2020. Photometric observations also revealed an increase in the object’s brightness in 2020. These observations suggest intriguing changes in the object’s activity, potentially indicating luminosity and chemical composition dynamics over the observed period. For the broad Hα line profile in the spectrum of NGC 3516, obtained with the AZT-8 on April 20, 2020, the radial velocity v=981−20+19 km/s. The radial velocity for the Hβ profile was 937−576+584 km/s; (4) Conclusions: Long-term observations of NGC 3516 have revealed significant changes in its luminosity and spectral characteristics, suggesting dynamic processes within the active nucleus of the galaxy. The observed variability in the broad emission line profiles could be linked to processes within the Broad Line Region (BLR) interacting with the SMBH and surrounding matter. These results may help in a more accurate estimation of the SMBH mass and provide deeper insights into the dynamics and evolution of active Seyfert galaxies.
- 22 November 2024
- Published by MDPI AG in Preprints.org
Open AccessSpectral and Photometric Studies of NGC 3516 in the Optical RangeSpectral and Photometric Studies of NGC 3516 in the Optical Range
(1) Background: NGC 3516 is an active Seyfert galaxy, which has become a focal point of astronomical studies due to its variable luminosity and emission lines, linked to the activity of its central supermassive black hole (SMBH). This paper presents an analysis of long-term observations from 2014 to 2024, including photometric and spectroscopic data collected at the Fesenkov Astrophysical Institute (FAI, Kazakhstan) and the Shamakhy Astrophysical Observatory (SHAO, Azerbaijan). The primary aim of this study was to investigate the changes in luminosity and spectral characteristics of NGC 3516, providing insights into the dynamics of the galaxy’s activity and its evolving chemical composition. (2) Methods: The research utilized photometric data in the B, V, R filters, along with spectroscopic observations in the wavelength range of λ4000 Å–λ7000 ÅThe spectroscopic data were normalized to analyze the profiles of emission lines and their variations over time. Broad emission line profiles (Hα and Hβ) were also analyzed to estimate radial velocities. A three-component model was applied, demonstrating a better statistical fit to the observed data, indicating a complex structure and dynamics within the galaxy’s Broad Line Region (BLR).; (3) Results: The main results of the study show that from 2018 to 2024, the brightness of NGC 3516 varied with amplitudes of ΔB=0.35 mag, ΔV=0.18 mag, ΔR=0.20 mag. An increase in brightness was observed in April 2020, likely associated with an X-ray flare detected simultaneously. Spectroscopic observations revealed a gradual weakening of the Hγλ4340 Å emission line starting from mid-2023. Narrow emission lines of [FeII] λ4814.53 Å and [FeVII] λ6087 Å were detected, indicating an active phase of the galaxy in May 2020. Photometric observations also revealed an increase in the object’s brightness in 2020. These observations suggest intriguing changes in the object’s activity, potentially indicating luminosity and chemical composition dynamics over the observed period. For the broad Hα line profile in the spectrum of NGC 3516, obtained with the AZT-8 on April 20, 2020, the radial velocity v=981−20+19 km/s. The radial velocity for the Hβ profile was 937−576+584 km/s; (4) Conclusions: Long-term observations of NGC 3516 have revealed significant changes in its luminosity and spectral characteristics, suggesting dynamic processes within the active nucleus of the galaxy. The observed variability in the broad emission line profiles could be linked to processes within the Broad Line Region (BLR) interacting with the SMBH and surrounding matter. These results may help in a more accurate estimation of the SMBH mass and provide deeper insights into the dynamics and evolution of active Seyfert galaxies.