The active galaxy MCG--6-30-15 has a 400 pc diameter stellar kinematically distinct core, counter-rotating with respect to the main body of the galaxy. Our previous high spatial resolution (0".1) H-band observations of this galaxy mapped the stellar kinematics and [Fe II] 1.64 \mum gas dynamics though mainly restricted to the spatial region of the counter-rotating core. In this work we probe the stellar kinematics on a larger field-of-view and determine the ionised and molecular gas dynamics to study the formation of the counter-rotating core and the implications for AGN fuelling. We present integral field spectroscopy observations with SINFONI in the H and K-bands in the central 1.2 kpc and with VIMOS HR-blue in the central 4 kpc of the galaxy. Ionised gas outflows of v ~ 100 km/s are traced by the [Ca VIII] 2.32 \mum coronal line and extend out to at least a radius of r ~ 140 pc. The molecular gas, traced by the H2 2.12 \mum emission is also counter rotating with respect to the main body of the galaxy, indicating that the formation of the distinct core was associated with inflow of external gas into the centre of MCG--6-30-15. The molecular gas traces the available gas reservoir for AGN fuelling and is detected as close as r ~ 50 - 100 pc. External gas accretion is able to significantly replenish the fuelling reservoir suggesting that the event that formed the counter-rotating core was also the main mechanism providing gas for AGN fuelling.

Tracing the origin of the AGN fuelling reservoir in MCG–6-30-15 / De Jesus Raimundo, S. I.; Davies, R. I.; Canning, R. E. A.; Celotti, A.; Fabian, A. C.; Gandhi, P.. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. - ISSN 0035-8711. - 464:4(2017), pp. 4227-4246. [10.1093/mnras/stw2635]

Tracing the origin of the AGN fuelling reservoir in MCG–6-30-15

De Jesus Raimundo, S. I.;Celotti, A.;
2017

Abstract

The active galaxy MCG--6-30-15 has a 400 pc diameter stellar kinematically distinct core, counter-rotating with respect to the main body of the galaxy. Our previous high spatial resolution (0".1) H-band observations of this galaxy mapped the stellar kinematics and [Fe II] 1.64 \mum gas dynamics though mainly restricted to the spatial region of the counter-rotating core. In this work we probe the stellar kinematics on a larger field-of-view and determine the ionised and molecular gas dynamics to study the formation of the counter-rotating core and the implications for AGN fuelling. We present integral field spectroscopy observations with SINFONI in the H and K-bands in the central 1.2 kpc and with VIMOS HR-blue in the central 4 kpc of the galaxy. Ionised gas outflows of v ~ 100 km/s are traced by the [Ca VIII] 2.32 \mum coronal line and extend out to at least a radius of r ~ 140 pc. The molecular gas, traced by the H2 2.12 \mum emission is also counter rotating with respect to the main body of the galaxy, indicating that the formation of the distinct core was associated with inflow of external gas into the centre of MCG--6-30-15. The molecular gas traces the available gas reservoir for AGN fuelling and is detected as close as r ~ 50 - 100 pc. External gas accretion is able to significantly replenish the fuelling reservoir suggesting that the event that formed the counter-rotating core was also the main mechanism providing gas for AGN fuelling.
464
4
4227
4246
https://doi.org/10.1093/mnras/stw2635
http://arxiv.org/abs/1610.03529v1
De Jesus Raimundo, S. I.; Davies, R. I.; Canning, R. E. A.; Celotti, A.; Fabian, A. C.; Gandhi, P.
File in questo prodotto:
File Dimensione Formato  
Raimundoetal.pdf

accesso aperto

Tipologia: Documento in Post-print
Licenza: Non specificato
Dimensione 2.89 MB
Formato Adobe PDF
2.89 MB Adobe PDF Visualizza/Apri
stw2635.pdf

accesso aperto

Tipologia: Versione Editoriale (PDF)
Licenza: Non specificato
Dimensione 2.87 MB
Formato Adobe PDF
2.87 MB Adobe PDF Visualizza/Apri

I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.

Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/20.500.11767/47818
Citazioni
  • ???jsp.display-item.citation.pmc??? ND
  • Scopus 10
  • ???jsp.display-item.citation.isi??? 9
social impact