arXiv subjects

B. Palit

Publications and source records attributed to B. Palit.

3 recordsLinked to original sources

arXiv2026

A break in the X-ray loudness of Markarian 590: evidence for an AGN spectral state transition?

Using decade-long multi-band {\it Swift} observations of the changing-look AGN Markarian 590, we identify a clear break in the dependence of the X-ray loudness parameter $\alpha_{\rm ox}$ on the source accretion rate. This break could be potential evidence for an accretion state transition, analogous to that observed for X-ray binaries. The $\alpha_{\rm ox}$ follows a pronounced 'V'-shaped dependence on Eddington ratio $\lambda_{\rm Edd}$, with a statistically significant break at $\lambda_{\rm Edd} =0.021\pm0.008$, consistent with the Eddington-ratio threshold associated with changing-look events in quasars. This behavior is indicative of a change in the inner accretion flow, from a truncated disk with a dominant hot corona at low accretion rates to an inward extending disk with enhanced UV emission and a prominent warm Comptonizing layer at higher rates. The UV and X-ray Eddington ratio tracers also show consistent breaks at $\lambda_{\rm Edd}\sim0.004$. Mkn~590 evolves through distinct phenomenological accretion phases, from a faint, hard X-ray dominated state, through a flaring phase, to a bright, UV/soft X-ray dominated phase and exhibiting variability on month-, year-, and decade-long timescales. This overall evolution is shorter than classical viscous timescales but broadly consistent with propagating thermal fronts in the accretion disk. We also found a declining radio-to-X-ray luminosity ratio with increasing $\lambda_{\rm Edd}$, indicating a relative suppression of radio emission as the disk becomes more dominant with respect to the X-ray corona. Taken together, these results provide evidence that Mkn~590 is undergoing a state transition, supporting a broad analogy between changing-look AGNs and X-ray binaries.

astro-ph.HE↗

arXiv2024

X-ray view of dissipative warm corona in active galactic nuclei

In the X-ray spectra of AGNs, a noticeable excess of soft X-rays is typically detected beyond the extrapolation of the power-law trend observed between 2-10 keV. In the scenario of warm Comptonization, observations propose a warm corona temperature ranging from 0.1-1 keV and an optical depth of approximately 10-20. Furthermore, according to radiative constraints derived from spectral analyses employing Comptonization models, it is suggested that the majority of the accretion power is released within the warm corona, while the disk beneath it is largely non-dissipative, emitting mainly the reprocessed radiation from the corona. We test the dissipative warm corona model using the radiative transfer code-TITAN/NOAR on a sample of 82 XMM-Newton observations of AGNs. Through spectral modeling of the X-ray data, we aim to estimate the total amount of internal heating inside the warm corona situated on top of the accretion disk. By modeling the 0.3-10 keV EPIC-pn spectra, we estimate the internal heating and optical depth of the warm corona and check their correlations with global parameters blackhole parameters. From model normalization, we compute the radial extent of warm corona on top of cold accretion disk. Our model infers the presence of dissipative warm corona, with optical depths distributed in the range 6-30 and total internal heating in the range 1-29 x 1e-23 erg/s-cm3. The extent of warm corona is spread across a large range from 7-408 gravitational radii, and we find that warm corona is more extended for larger accretion rates. Soft excess emission is ubiquitous in AGNs across wide mass range and accretion rate. We confirm that warm corona responsible for producing the soft-excess is highly dissipative in nature with larger optical depths being associated with lower internal heating and vice versa. The cold standard accretion disk regulates the extent of warm corona.

astro-ph.HE↗

arXiv2024

Unveiling Energy Pathways in AGN Accretion Flows with the Warm Corona Model for the Soft Excess

The soft excess in active galactic nuclei (AGNs) may arise through a combination of relativistic reflection and the effects of a warm corona at the surface of the accretion disc. Detailed examination of the soft excess can therefore constrain models of the transport and dissipation of accretion energy. Here, we analyze 34 XMM-Newton observations from 14 Type I AGNs with the reXcor spectral model which self-consistently combines emission from a warm corona with relativistic reflection assuming a lamppost corona. The model divides accretion energy between the disc, the warm corona, and the lamppost. The XMM-Newton observations span a factor of 188 in Eddington ratio ($\lambda_{\mathrm{obs}}$) and 350 in black hole mass, and we find that a warm corona is a significant contributor to the soft excess for 13 of the 14 AGNs with a mean warm corona heating fraction of $0.51$. The reXcor fits reveal that the fraction of accretion energy dissipated in the lamppost is anti-correlated with $\lambda_{\mathrm{obs}}$. In contrast, the relationship between $\lambda_{\mathrm{obs}}$ and both the optical depth and heating fraction of the warm corona appears to transition from an anti-correlation to a correlation at $\lambda_{\mathrm{obs,t}} \approx 0.15$. Therefore, at least one other physical process in addition to the accretion rate is needed to explain the evolution of the warm corona. Overall, we find that a warm corona appears to be a crucial depository of accretion energy in AGNs across a broad range of $\lambda_{\mathrm{obs}}$ and black hole mass.

astro-ph.HE↗