Leo II Group: decoupled cores of NGC 3607 and NGC3608

Afanasiev, V. L.; Сильченко, О. К.

doi:10.1080/10556790701553524

Cited by 12 publications

(12 citation statements)

References 49 publications

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“…The following things can be noticed: (1) in the near-IR, tracing the old stellar population of galaxies, the S0s in NIRS0S are not less luminous than the spirals in OSUBSGS (both samples are magnitude-limited, selected in a similar manner). A similar result in the near-IR was obtained also by Burnstein et al ([89]).…”

Section: Properties Of Bulges In the Hubble Sequencementioning

confidence: 96%

Overview of the Near-IR S0 Galaxy Survey (NIRS0S)

Laurikainen

Salo

Buta

et al. 2011

Advances in Astronomy

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An overview of the results of the Near-IR S0 galaxy Survey (NIRS0S) is presented. NIRS0S is a magnitude (m B 12.5 mag) and inclination (< 65 o ) limited sample of ∼ 200 nearby galaxies, mainly S0s, but include also Sa and E galaxies. It uses deep K s -band images, typically reaching a surface brightness of 23.5 mag arcsec −2 . Detailed visual and photometric classifications were made, for the first time coding also the lenses in a systematic manner. The main analysis methods include 2D multicomponent decomposition approach, and Fourier analysis of the non-axisymmetric structures. As a comparison sample, a similar sized spiral galaxy sample with similar image quality was used. The main emphasis were to study whether the S0s are former spirals in which star formation has been ceased, and also, how robust are bars in galaxies. Based on our analysis the Hubble sequence was revisited: following the early idea by van den Bergh we suggested that the S0s are spread throughout the Hubble sequence in parallel tuning forks as spirals (S0a, S0b, S0c etc.). This is evidenced by our improved bulge-to-total (B/T ) flux ratios in the S0s, covering the full B/T range, reaching small values typical to late-type spirals. The properties of bulges and disks in S0s were found to be similar to those in spirals and also, the masses and scale parameters of the bulges and disks to be coupled. It was estimated that the spiral bulges brighter than -20 mag in K-band are massive enough to be converted into the bulges of S0s merely by star formation. Bars were found to be fairly robust both in S0s and spirals, but inspite of that bars might evolve significantly within the Hubble sequence.We review the main results of the Near-IR S0 galaxy Survey (NIRS0S) obtained so far 1 . NIRS0S is a magnitude (mB 12.5 mag) and inclination (less than 65 o ) limited sample of ∼ 200 nearby galaxies, mainly S0s, but include also Sa spirals and 25 late-type ellipticals. Late-type ellipticals were included for not to miss any potentially misclassified S0s. The observations were done in the Ks-band, carried out using 3-4 meter sized ground-based telescopes with sub-arcsecond pixel resolution. The images are deep, typically reaching a surface brightnesses of 23.5 mag arcsec −2 in azimuthally averaged profiles (∼ 2 mag deeper than the 2MASS images), thus allowing the detection of the faint outer disks in S0s. Our main emphasis was to address possible secular evolutionary processes in galaxies by comparing the photometric properties of S0s and spirals, based on similarly selected samples, with similar image quality. ⋆

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Section: Properties Of Bulges In the Hubble Sequencementioning

confidence: 96%

Overview of the Near-IR S0 Galaxy Survey (NIRS0S)

Laurikainen

Salo

Buta

et al. 2011

Advances in Astronomy

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“…Dist. (2010); b: 1-ellipticals, 2-S0s with classical bulges, 3-S0s with pseudo bulges, 4-spirals with classical bulges, 5-spirals with pseudo bulges and 6-ongoing mergers; c: classification is given by Davis et al (2017); d: classification is from Afanasiev & Silchenko (2007). Figure 1.…”

Section: Galaxymentioning

confidence: 99%

Study of central light concentration in nearby galaxies

Sreedevi

Ravikumar

2018

Monthly Notices of the Royal Astronomical Society

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We propose a novel technique to estimate the masses of super massive black holes (SMBHs) residing at the centres of massive galaxies in the nearby Universe using simple photometry. Aperture photometry using SEXTRACTOR is employed to determine the central intensity ratio (CIR) at the optical centre of the galaxy image for a sample of 49 nearby galaxies with SMBH mass estimations. We find that the CIR of ellipticals and classical bulges is strongly correlated with SMBH masses whereas pseudo bulges and ongoing mergers show significant scatter. Also, the CIR of low luminosity AGNs in the sample shows significant connection with the 5 GHz nuclear radio emission suggesting a stronger link between the former and the SMBH evolution in these galaxies. In addition, it is seen that various structural and dynamical properties of the SMBH host galaxies are correlated with the CIR making the latter an important parameter in galaxy evolution studies. Finally, we propose the CIR to be an efficient and simple tool not only to distinguish classical bulges from pseudo bulges but also to estimate the mass of the central SMBH.

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“…NGC 3607) with such features may have undergone a gas-rich merger event. The central region of NGC 3607 hosts a stellar-gaseous polar disc with hints of ongoing star formation (Afanasiev & Silchenko 2007).…”

Section: This Workmentioning

confidence: 99%

The SLUGGS survey: exploring the metallicity gradients of nearby early-type galaxies to large radii

Pastorello

Forbes

Foster

et al. 2014

Monthly Notices of the Royal Astronomical Society

118

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Stellar metallicity gradients in the outer regions of galaxies are a critical tool for disentangling the contributions of in-situ and ex-situ formed stars. In the two-phase galaxy formation scenario, the initial gas collapse creates steep metallicity gradients, while the accretion of stars formed in satellites tends to flatten these gradients in the outskirts, particularly for massive galaxies. This work presents the first compilation of extended metallicity profiles over a wide range of galaxy mass. We use the DEIMOS spectrograph on the Keck telescope in multi-slit mode to obtain radial stellar metallicity profiles for 22 nearby early-type galaxies. From the calcium triplet lines in the near-infrared we measure the metallicity of the starlight up to 3 effective radii. We find a relation between the outer metallicity gradient and galaxy mass, in the sense that lower mass systems show steeper metallicity gradients than more massive galaxies. This result is consistent with a picture in which the ratio of ex-situ to in-situ formed stars is lower in less massive galaxies as a consequence of the smaller contribution by accretion. In addition, we infer a correlation between the strength of the calcium triplet feature in the near-infrared and the stellar initial mass function slope that is consistent with recent models in the literature.

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Leo II Group: decoupled cores of NGC 3607 and NGC3608

Cited by 12 publications

References 49 publications

Overview of the Near-IR S0 Galaxy Survey (NIRS0S)

Overview of the Near-IR S0 Galaxy Survey (NIRS0S)

Study of central light concentration in nearby galaxies

The SLUGGS survey: exploring the metallicity gradients of nearby early-type galaxies to large radii

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