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A Triple AGN in the NGC 7733-7734 Merging Group
No full textInternational audienceContext. Galaxy interactions and mergers can lead to supermassive black hole (SMBH) binaries which become active galactic nuclei (AGN) pairs when the SMBHs start accreting mass. If there is a third galaxy involved in the interaction, then a triple AGN system can form. Aims. Our goal is to investigate the nature of the nuclear emission from the galaxies in the interacting pair NGC 7733-NGC 7734 using archival VLT/MUSE Integral field spectrograph data and study its relation to the stellar mass distribution traced by near-infrared (NIR) observations from the South African Astronomical Observatory (SAAO). Methods. We conducted near-infrared observations using the SAAO and identified the morphological properties of bulges in each galaxy. We used MUSE data to obtain a set of ionized emission lines from each galaxy and studied the ionization mechanism. We also examined the relation of the galaxy pair with any nearby companions with Far-UV observations using the UVIT. Results. The emission line analysis from the central regions of NGC 7733 and NGC 7734 show Seyfert and LINER type AGN activity. The galaxy pair NGC 7733-34 also shows evidence of a third component, which has Seyfert-like emission. Hence, the galaxy pair NGC 7733-34 forms a triple AGN system. We also detected an Extended Narrow-line region (ENLR) associated with the nucleus of NGC 7733
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Photograph of ER 7733 Hillsboro Sub. #2 transformer on blocks ready to attach skids
No full textPhotograph of ER 7733 Hillsboro Sub. #2 transformer on blocks ready to attach skid
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Photograph of ER 7733 Hillsboro Sub. #2 and #3 transformers on the temporary track
No full textPhotograph of ER 7733 Hillsboro Sub. #2 and #3 transformers on the temporary trac
Constraining the fundamental parameters of the O-type binary CPD-41 7733
Get PDFpeer reviewedUsing a set of high-resolution spectra, we studied the physical and orbital properties of the O-type binary CPD -41 7733, located in the core of NGC 6231. We report the unambiguous detection of a secondary spectral signature and we derive the first SB2 orbital solution of the system. The period is 5.6815 + 0.0015 days, and the orbit has no significant eccentricity. CPD -41 7733 probably consists of stars of spectral types O8.5 and B3. As for other objects in the cluster, we observe discrepant luminosity classifications while using spectroscopic or brightness criteria. Still, the present analysis suggests that both components display physical parameters close to those of typical O8.5 and B3 dwarfs. We also analyze the X-ray light curves and spectra obtained during six 30 ks XMM-Newton pointings spread over the 5.7 day period. We find no significant variability between the different pointings, nor within the individual observations. The CPD - 41 7733 X- ray spectrum is well reproduced by a three-temperature thermal mekal model with temperatures of 0.3, 0.8, and 2.4 keV. No X-ray overluminosity, resulting, e. g., from a possible wind interaction, is observed. The emission of CPD -41 7733 is thus very representative of typical O-type star X- ray emission
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Photograph of ER 7733 Hillsboro Sub. rolling #3 transformer to Sub. on 3x12 oak planks
No full textPhotograph of ER 7733 Hillsboro Sub. rolling #3 transformer to Sub. on 3x12 oak plank
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Photograph of ER 7733 Hillsboro Sub. #3 transformer being skidded to sub.
No full textPhotograph of ER 7733 Hillsboro Sub. #3 transformer being skidded to sub
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Photograph of ER 7733 Hillsboro Sub. skidding #3 transformer to substation
No full textPhotograph of ER 7733 Hillsboro Sub. skidding #3 transformer to substatio
Unveiling the kinematics of a central region in the triple-AGN host NGC 7733-7734 interacting group
No full textInternational audienceWe present a detailed study of the interacting triple active galactic nuclear system, NGC 7733-34, focusing on stellar kinematics, ionised gas characteristics, and star formation within the central region and stellar bars of both galaxies. We performed a comprehensive analysis using archival data from MUSE, HST/ACS, and DECaLS, complemented with observations from UVIT and IRSF. We identified a disc-like bulge in both NGC 7733 and NGC 7734 through a 2D decomposition. A central nuclear structure, with a semi-major axis of ∼1.113 kpc, was detected in NGC 7733 via a photometric and kinematic analysis, confirmed by the strong anti-correlation between V / σ and h 3 , indicative of circular orbits in the centre. NGC 7734 lacks a distinct nuclear structure. The presence of a disc-like bulge results in an anti-correlation between V / σ and h 3 , along with diffuse light. However, it does show higher central velocity dispersion, possibly attributed to an interaction with a smaller clump, which is likely a fourth galaxy within the system. Both galaxies demonstrate ongoing star formation, evidenced by FUV and H α observations. NGC 7734 shows recent star formation along its bar, while NGC 7733 experiences bar quenching. The star formation rate (SFR) analysis of NGC 7734 reveals that the bar region’s SFR dominates the galaxy’s overall SFR. Conversely, in NGC 7733, the lack of star formation along the bar and the presence of a Seyfert 2 active galactic nucleus (AGN) at the galaxy centre suggest the possibility of link among both. However, this would not affect the galaxy’s overall star formation. Our findings provide valuable insights into the stellar and gas kinematics, star formation processes, and AGN feedback mechanisms in interacting galaxies hosting stellar bars
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Photograph of ER 7733 Hillsboro Sub. Walter's truck and BJ Mack truck pulling #2 transformer
No full textPhotograph of ER 7733 Hillsboro Sub. Walter's truck and BJ Mack truck pulling #2 transforme
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