Implications of Einstein-Maxwell dilaton-axion gravity from the black hole continuum spectrum

TL;DR

This study investigates how Einstein-Maxwell dilaton-axion gravity influences black hole spectra, using quasar observations to constrain the dilaton parameter and assess the theory's astrophysical viability.

Contribution

It provides the first detailed analysis of quasar spectra in Kerr-Sen black hole backgrounds within EMDA gravity, constraining the dilaton parameter using observational data.

Findings

Dilaton parameter r_2~0.2 is favored by quasar data.

Strong dilaton charges r_2>1.6 are disfavored.

Estimated black hole spins from quasar spectra.

Abstract

String inspired models can serve as potential candidates to replace GR in the high energy regime where quantum gravity is expected to play a vital role. Such models not only subsume the ultraviolet nature of gravity but also exhibit promising prospects in resolving issues like dark matter and dark energy, which cannot be adequately addressed within the framework of GR. The Einstein-Maxwell dilaton-axion (EMDA) theory, which is central to this work is one such string inspired model arising in the low energy effective action of the heterotic string theory with interesting implications in inflationary cosmology and in the late time acceleration of the universe. It is therefore important to survey the role of such a theory in explaining astrophysical observations, e.g. the continuum spectrum of black holes which is expected to hold a wealth of information regarding the background metric. The Kerr-Sen spacetime corresponds to the exact, stationary, and axisymmetric black hole solution in EMDA gravity, possessing dilatonic charge and angular momentum originating from the axionic field. In this work, we compute the theoretical spectrum from the accretion disk around quasars in the Kerr-Sen background assuming the thin accretion disk model due to Novikov \& Thorne. This is then used to evaluate the theoretical estimates of optical luminosity for a sample of eighty Palomar-Green quasars which are subsequently compared with the available observations. Our results based on $\chi^2$ analysis indicate that the dilaton parameter $r_2\sim 0.2$ is favored by optical observations of quasars which is further corroborated by other error estimators e.g., the Nash-Sutcliffe efficiency, the index of agreement, and their modified versions. We further report that strong dilaton charges ($r_2>1.6$) are disfavored by quasar optical data and the spins associated with the quasars are also estimated.