Double Nuclei in NGC 908 and NGC 1187

Menezes, R. B.; Steiner, J. E.

doi:10.3847/1538-4357/aae843

Cited by 8 publications

(4 citation statements)

References 49 publications

(53 reference statements)

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“…Beside the mergers, the presence of a nuclear eccentric stellar disk and central supermassive black hole (SMBH) can result in a double nucleus in galaxies (Tremaine 1995). The double nuclei in M31, NGC 4486B and NGC1187 are likely formed through this process along with only parsec-scale separations with their double nuclei (Lauer et al , 2012Menezes, & Steiner 2018).…”

Section: Introductionmentioning

confidence: 99%

“…Especially, the peculiar nuclear morphologies such as double or multiple nuclei deserve closer scrutiny. Galaxies with double nuclei usually reach the stage of galaxy interacting or starburst (Bridge et al 2010;Mezcua et al 2014), along with certain normal field galaxies (e.g., Menezes, & Steiner 2018). Based on spectroscopic investigations, many sources with double nuclei have been identified as AGNs, starburst nuclei, or giant HII regions (e.g., Mazzarella, & Boroson 1993;Moiseev et al 2010;Koss et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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The Nature of the Double Nuclei in the Barred S0 Galaxy IC 676

Zhang

et al. 2020

ApJ

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The lenticular galaxy IC 676 is a barred galaxy with double nuclei and active star formation in the central region. In this work we present the long-slit spectroscopy and archival multi-wavelength images to investigate the nature and origin of the double nuclei in IC 676. Through photometric 1D brightness profiles and 2D image decomposition, we show that this galaxy consists of a stellar bar with the length of ∼ 2.5 kpc and two Sérsic disks both of which with Sérsic index n ∼ 1.3. There is probably little or no bulge component assembled in IC 676. The luminosities of the double nuclei are primarily dominated by young stellar populations within the ages of 1-10 Myr. The northern nucleus has stronger star formation activity than the southern one. The surface densities of the star formation rate in the double nuclei are similar to those in starburst galaxies or the circumnuclear star forming regions in spiral galaxies. Each of the double nuclei in IC 676 likely consists of young massive star clusters, which can be resolved as bright knots in the HST high resolution image. Our results suggest that IC 676 likely has a complex formation and evolutionary history. The secular processes driven by the stellar bar and external accretion may dominate the formation and evolution of its double nuclei. This indicates that the secular evolution involving the internal and external drivers may have an important contribution for the evolution of lenticular galaxies.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Nature of the Double Nuclei in the Barred S0 Galaxy IC 676

Zhang

et al. 2020

ApJ

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“…As explained in Menezes et al ( 2019 ), the use of the Richardson-Lucy deconvolution is only advisable when a reliable estimate of the PSF is available, which is the case of NGC 7314. When such care is taken, the Richardson-Lucy deconvolution impro v es the visualisation of the spatial morphology of the structures, without compromising the data, as pro v en in man y articles such as da Silva, Menezes & Steiner ( 2020 ), Menezes & Steiner ( 2018 ), and Menezes, Steiner & Ricci ( 2013 ).…”

Section: Gmos Datamentioning

confidence: 99%

A closer look at NGC 7314 nuclear region: a multiwavelength analysis of the Seyfert nucleus and its surroundings

Silva

Menezes

Diaz

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The central regions of galaxies harboring Active Galactic Nuclei (AGNs) can be quite complex, especially at high activity, presenting, besides variability, a variety of phenomena related, for example, to ionization/excitation mechanisms. A detailed study is necessary in order to understand better those objects. For that reason, we performed a multiwavelength analysis of the nuclear region of the nearby Seyfert galaxy NGC 7314, using an optical data cube obtained with the Integral Field Unit from the Gemini Multi-Object Spectrograph, together with Hubble Space Telescope images, X-ray data from the XMM–Newton and the Nuclear Spectroscopic Telescope Array and radio data from Atacama Large Millimeter/Submillimeter Array. The goals were to study the nuclear and circumnuclear emission, the emission of the AGN and the gas kinematics. The optical spectrum shows the emission of a Seyfert nucleus, with broad components in the Hα and Hβ emission lines, characterizing a type 1 AGN, with a spectrum rich in coronal emission lines. The spatial morphology of the [O iii] λ5007 suggests the presence of an ionization cone, west of the nucleus, meanwhile the east cone seems to be obscured by dust. An extended [Fe vii] λ6087 emission was also detected, which could be possibly explained by a scenario involving photoionization+shocks mechanisms. X-rays analyses showed that there are variations in the flux, however we did not detect any variations in the column density along the line of sight. Its variability may be a consequence of changes in the AGN accretion rate.

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“…We named these parameters as the median age (T med ) and the median metallicity (Z med ). We used these same parameters in the analysis of the spectral synthesis in Menezes & Steiner (2018). The values obtained for regions 1, 2, and 3 were T med (1) = 1.27 × 10 10 yr, Z med (1) = 0.0066, T med (2) = 1.3×10 10 yr, Z med (2) = 0.0061, and T med (3) = 1.21 × 10 10 yr, Z med (3) = 0.0070.…”

Section: Stellar Archaeologyunclassified

The highly obscured Seyfert 2 nucleus in NGC 1448 observed with MUSE

Menezes,

da Silva,

Steiner

2021

Preprint

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We present the analysis of an optical data cube of the central region of NGC 1448, obtained with the Multi Unit Spectroscopic Explorer (MUSE). Chandra X-ray data indicate that the active galactic nucleus (AGN) is not located at the apparent stellar nucleus of the galaxy, but at a projected distance of 1.75 ± 0.22 arcsec (139 ± 17 pc). This is probably caused by the high interstellar extinction in the surroundings of the AGN, which corresponds to the true nucleus of the galaxy, as also proposed by previous studies. The morphology and classification of the optical line-emitting regions indicate two ionization cones, around an axis with a position angle of P A cones = −50 • ± 7 • , with emission-line spectra characteristic of Seyfert galaxies. The stellar and gas kinematics are consistent with a stellar and gas rotating disc around the nucleus, with a velocity amplitude of 125 km s −1 . Two probable outflows from the AGN were detected along the region of the two ionization cones. The AGN position does not coincide with the brightest line-emitting region at the centre of NGC 1448. That may be a consequence of the high obscuration from the AGN towards the observer (the AGN is actually Compton thick), mostly caused by a nearly edge-on torus. An additional hypothesis is that the AGN reduced its luminosity, during the last 440 yr, to nearly half of the value in the past. In this case, the brightest line-emitting region corresponds to a "light echo" or a "fossil" of the AGN in the past.

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Double Nuclei in NGC 908 and NGC 1187

Cited by 8 publications

References 49 publications

The Nature of the Double Nuclei in the Barred S0 Galaxy IC 676

The Nature of the Double Nuclei in the Barred S0 Galaxy IC 676

A closer look at NGC 7314 nuclear region: a multiwavelength analysis of the Seyfert nucleus and its surroundings

The highly obscured Seyfert 2 nucleus in NGC 1448 observed with MUSE

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