The resolved size and structure of hot dust in the immediate vicinity of AGN

Gravity Collaboration; Dexter, J.; Shangguan, J.; Hönig, S.; Kishimoto, M.; Lutz, D.; Netzer, H.; Davies, R.; Sturm, E.; Pfuhl, O.; Amorim, A.; Bauböck, M.; Brandner, W.; Clénet, Y.; de Zeeuw, P. T.; Eckart, A.; Eisenhauer, F.; Förster Schreiber, N. M.; Gao, F.; Garcia, P. J. V.; Genzel, R.; Gillessen, S.; Gratadour, D.; Jiménez-Rosales, A.; Lacour, S.; Millour, F.; Ott, T.; Paumard, T.; Perraut, K.; Perrin, G.; Peterson, B. M.; Petrucci, P. O.; Prieto, M. A.; Rouan, D.; Schartmann, M.; Shimizu, T.; Sternberg, A.; Straub, O.; Straubmeier, C.; Tacconi, L. J.; Tristram, K.; Vermot, P.; Waisberg, I.; Widmann, F.; Woillez, J.
Referencia bibliográfica

Astronomy and Astrophysics

Fecha de publicación:
Número de autores
Número de autores del IAC
Número de citas
Número de citas referidas
We use VLTI/GRAVITY near-infrared interferometry measurements of eight bright type 1 AGN to study the size and structure of hot dust that is heated by the central engine. We partially resolve each source, and report Gaussian full width at half-maximum sizes in the range 0.3-0.8 mas. In all but one object, we find no evidence for significant elongation or asymmetry (closure phases ≲1°). The narrow range of measured angular sizes is expected given the similar optical flux of our targets, and implies an increasing effective physical radius with bolometric luminosity, as found from previous reverberation and interferometry measurements. The measured sizes for Seyfert galaxies are systematically larger than for the two quasars in our sample when measured relative to the previously reported R ∼ L1/2 relationship, which is explained by emission at the sublimation radius. This could be evidence of an evolving near-infrared emission region structure as a function of central luminosity.
Proyectos relacionados
Project Image
Centros de Galaxias a Escalas de Parsecs y Técnicas de Alta Resolución Espacial

Proyecto enfocado al estudio en el IR del núcleo de las galaxias más cercanas con resoluciones espaciales en el rango de 1 a 10 pc. Estas resoluciones espaciales, accesibles con los grandes telescopios de tierra usando técnicas frontera de observación, son por primera vez comparables a las que se obtienen rutinariamente con HST en el óptico y VLBI

Prieto Escudero