Lenticular Galaxies at the Outskirts of the Leo Ii Group: NGC 3599 and NGC 3626

Сильченко, О. К.; Моисеев, А. В.; Shulga, A. P.

doi:10.1088/0004-6256/140/5/1462

Cited by 20 publications

(16 citation statements)

References 43 publications

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“…Ages weighted by B-band luminosity become younger, 3.4 and 4.8 Gyr (Table 3), respectively, in good agreement with the previous findings by Sil 'chenko et al (2010). At odds with us, Sil'chenko et al (2010) suggested that this ETG results from a minor merger. Simulated and observed maps in Figure 3 do not show any signature of interactions, in good agreement with the findings of Marino et al (2013).…”

Section: Ngc 3599mentioning

confidence: 86%

THENUV–rVERSUSM_rPLANE AS A TRACER OF EARLY-TYPE GALAXY EVOLUTION IN THE USGC U376 AND LGG 225 GROUPS

Mazzei

Marino

Rampazzo

2014

ApJ

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With the aim of tracing back the evolution of galaxies in nearby groups we use smooth particle hydrodynamical (SPH) simulations with chemo-photometric implementation. Here we focus on the evolution of the early-type members (Es and S0s, ETGs hereafter) in two groups, USGC U376 and LGG 225, both in the Leo cloud. We use the near-UV (NUV)-optical rest-frame (NUV − r) versus M r color magnitude diagram to follow their evolution, from the blue cloud (BC) to the red sequence (RS), through the green valley (GV). ETGs brighter than M r = −21 mag are older than 13 Gyr and spend up to 10 Gyr of their overall evolutionary time in the BC before they reach the RS migrating through the GV. Fainter ETGs are younger, of ≈ 2 Gyr on average, and evolve for about 7-8 Gyr along the BC. The turn-off occurs at z ≈ 0.3 − 0.4. Therefore these ETGs spend up to 3-5 Gyr crossing the GV; UGC 06324, the faintest ETG in the sample, still is in the GV. The mechanism driving their evolution is gravitational, due to merging and/or interaction. Our SPH simulations suggest that ETG members of these groups evolved toward the RS before and during the group collapse phase. This result is consistent with the dynamical analysis of both groups showing that they are not yet virialized.

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Section: Ngc 3599mentioning

confidence: 86%

THENUV–rVERSUSM_rPLANE AS A TRACER OF EARLY-TYPE GALAXY EVOLUTION IN THE USGC U376 AND LGG 225 GROUPS

Mazzei

Marino

Rampazzo

2014

ApJ

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“…The classical bulge formed their stars rapidly and explain the general trend in [α/Fe] as a function of height, as disk light (with its lower [α/Fe]) contributes less and less to the integrated spectrum. The boxy appearance is explained by the simultaneous presence of a bar (which appears boxy in projection), and the double hump of the rotation curve hints at the presence of a small disky pseudobulge (see also Sil'chenko et al, 2010).…”

Section: Bulges As Composite Systemsmentioning

confidence: 95%

Stellar Populations of Bulges at Low Redshift

Sánchez‐Blázquez

2016

Astrophysics and Space Science Library

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“…The classical bulge formed their stars rapidly and explain the general trend in OE˛=Fe as a function of height, as disc light (with its lower OE˛=Fe) contributes less and less to the integrated spectrum. The boxy appearance is explained by the simultaneous presence of a bar (which appears boxy in projection), and the double hump of the rotation curve hints at the presence of a small discy pseudobulge (see also Sil'chenko et al 2010). …”

Section: Bulges As Composite Systemsmentioning

confidence: 95%

Galactic Bulges

2016

Astrophysics and Space Science Library

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978-3-319-19377-9 ISBN 978-3-319-19378-6 (eBook) DOI 10.1007/978-3-319-19378-6 Library of Congress Control Number: 2015949217 Springer Cham Heidelberg New York Dordrecht London © Springer International Publishing Switzerland 2016 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. The use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specific statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. The publisher, the authors and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication. Neither the publisher nor the authors or the editors give a warranty, express or implied, with respect to the material contained herein or for any errors or omissions that may have been made.Cover Illustration: In the cover the 3.6 images of one nearby galaxy, NGC 4565, is shown. The images are from the Spitzer Survey of Stellar Structure in Galaxies (PI Kartik Sheth).Printed on acid-free paper Springer International Publishing AG Switzerland is part of Springer Science+Business Media (www.springer.com) PrefaceThe main motivation for this book was our impression that when observers talk about bulges in galaxies, they do not necessarily mean the same thing as people making theoretical models. Even among the observers, it is not always clear what they mean by classical and pseudobulges. According to most researchers, classical bulges are highly relaxed systems typically formed in galaxy mergers or by coalescence of massive gas clumps at high redshifts, whereas pseudobulges have more disc-like properties. Some people divide pseudobulges further into discy pseudobulges, defined as small central discs in the plane of the galactic disc, and boxy/peanut bulges which are actually dynamically heated, vertically thick inner parts of bars. Galaxies can also have central star clusters, usually called nuclear clusters, which structures are not called bulges in this book (see the review by Cole and Debattista). In recent years significant progress has been made both on the theoretical and observational sides, including galactic and extragalactic research. In this book we try to bring all these communities closer to each other.Most probably many of us share the Copernican approach trying to understand the universe with some simple beautiful theory. Such an attempt is the current paradigm of structure formation, i.e., the hierarchical growth of dark matter halos ( CDM), and the subsequent formatio...

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Lenticular Galaxies at the Outskirts of the Leo Ii Group: NGC 3599 and NGC 3626

Cited by 20 publications

References 43 publications

THENUV–rVERSUSM_rPLANE AS A TRACER OF EARLY-TYPE GALAXY EVOLUTION IN THE USGC U376 AND LGG 225 GROUPS

THENUV–rVERSUSM_rPLANE AS A TRACER OF EARLY-TYPE GALAXY EVOLUTION IN THE USGC U376 AND LGG 225 GROUPS

Stellar Populations of Bulges at Low Redshift

Galactic Bulges

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Lenticular Galaxies at the Outskirts of the Leo Ii Group: NGC 3599 and NGC 3626

Cited by 20 publications

References 43 publications

THENUV–rVERSUSMrPLANE AS A TRACER OF EARLY-TYPE GALAXY EVOLUTION IN THE USGC U376 AND LGG 225 GROUPS

THENUV–rVERSUSMrPLANE AS A TRACER OF EARLY-TYPE GALAXY EVOLUTION IN THE USGC U376 AND LGG 225 GROUPS

Stellar Populations of Bulges at Low Redshift

Galactic Bulges

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THENUV–rVERSUSM_rPLANE AS A TRACER OF EARLY-TYPE GALAXY EVOLUTION IN THE USGC U376 AND LGG 225 GROUPS

THENUV–rVERSUSM_rPLANE AS A TRACER OF EARLY-TYPE GALAXY EVOLUTION IN THE USGC U376 AND LGG 225 GROUPS