deg) in any filter, with the redshift distribution of these sources peaking at z~1.
We provide an upper limit on the estimated number of quasars for which the AD time lag can be computed within 01000 sources in each Deep Drilling field (DDF, 10 sq. Running our metric on different LSST cadence strategies, we produce an atlas of the performance estimations for LSST photometric RM measurements. It accounts for redshift, cadence, the magnitude limit, and magnitude corrections for dust extinction. We examine the effect of LSST cadence strategies on AD RM using our metric AGNTimeLagMetric. This brings us to face challenges in the reverberation mapping (RM) measurement of AD sizes in active galactic nuclei (AGNs) using interband continuum delays. Rubin Observatory Legacy Survey of Space and Time (LSST) will detect an unprecedentedly large sample of actively accreting supermassive black holes with typical accretion disk (AD) sizes of a few light days. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovacevic-Dojcinovic, Masa Lakicevic, Djorđe Savic, Oliver Vince, Sasa Simic, Iva Cvorovic-Hajdinjak, Sladjana Marceta-MandicĪbstract : The Vera C. Assef, Paula Sanchez-Saez, Robert Nikutta, Claudia M. Kovacevic, Viktor Radovic, Dragana Ilic, Luka C. We anticipate that future high quality observational data of the S2 stellar orbit or other stellar orbits can help reveal the actual mass distribution near the SMBH and the nature of dark matter.ģ.The LSST era of supermassive black holes accretion-disk reverberation mapping (arXiv)Īuthor : Andjelka B. Here, we report an interesting phenomenon that if a significant amount of dark matter or stellar mass is distributed around the SMBH, the precession speed of the S2 stellar orbit could be `slow down’ by at most 27\% compared with that without dark matter surrounding the SMBH, assuming the optimal dark matter scenario. In particular, the star S2 has completed at least one period since our first detection of its position, which can provide rich information to examine the properties of the SMBH, and the astrophysical environment surrounding the SMBH. Their orbital nature can give stringent constraints for the mass of the SMBH. Therefore, some of our solutions could, in principle, replace the standard BH-picture of the galactic center and, at the same time, have the advantage that they have been composed of the main matter ingredient of the UniverseĢ.Investigating the nature of mass distribution surrounding the Galactic supermassive black hole (arXiv)Īuthor : Man Ho Chan, Chak Man Lee, Chi Wai YuĪbstract : In the past three decades, many stars orbiting about the supermassive black hole (SMBH) at the Galactic Centre (Sgr A*) were identified. Their effective potentials which govern the motion of a test body, can display a reasonable similarity to the effective potential of a Schwarzschild BH at the galactic center. We emphasize that all objects are solutions of Einstein equations. These astrophysical objects come out in three types: a fuzzy droplet without horizon and fuzzy Black Holes (BHs) with one or two horizons. Here we probe into this possibility by constructing stable objects with fuzzy mass distributions based on standard DM profiles. Indeed, given the fact that DM is the dominant matter species in the Universe, it is natural to assume a close connection between DM and SMBHs. However, the role of DM might be different in the galactic bulges and centers where Supermassive Black Holes (SMBHs) dominate the gravitational interaction. 1.Possible Connection between Dark Matter and Supermassive Black Holes (arXiv)Īuthor : Davide Batic, Joud Mojahed Faraji, Marek NowakowskiĪbstract : Dark Matter (DM) is usually studied in connection with rotational curves in the outskirts of the galaxies.
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