Towards an Understanding of the Globular Cluster Over-Abundance Around the Central -Giant Elliptical NGC 1399 I
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VEGAS: a VST Early-Type Galaxy Survey. the Faint Substructures of NGC 4472 Stellar Halo
VEGAS: A VST Early-type GAlaxy Survey. The faint substructures of NGC 4472 stellar halo. MARILENA SPAVONE ON THE BEHALF OF THE VEGAS TEAM: M. CAPACCIOLI, M. CANTIELLO, A. GRADO, E. IODICE, F. LA BARBERA, N.R. NAPOLITANO, C. TORTORA, L. LIMATOLA, M. PAOLILLO, T. PUZIA, R. PELETIER, A.J. ROMANOWSKY, D. FORBES, G. RAIMONDO OUTLINE The VST VEGAS survey Science aims Results on NGC 4472 field Conclusions Future plans MARILENA SPAVONE STELLAR HALOS 2015 ESO-GARCHING, 23-27 FEBRUARY THE VEGAS SURVEY Multiband u, g, r, i survey of ~ 110 galaxies with vrad < 4000 km/s in all environments (field to clusters). An example Obj. name Morph. type u g r i IC 1459 E3 5630 1850 1700 NGC 1399 E1 8100 5320 2700 NGC 3115 S0 14800 8675 6030 Observations to date (to P94) g-BAND ~ 16% i-BAND ~ 19% r-BAND ~ 3% + FORNAX u-BAND ~ 1% MARILENA SPAVONE STELLAR HALOS 2015 ESO-GARCHING, 23-27 FEBRUARY THE VEGAS SURVEY Multiband u, g, r, i survey of ~ 110 galaxies with vrad < 4000 km/s in all environments (field to clusters). OT ~ 350 h @ vst over 5 years Expected SB limits: 27.5 g, 2 27.0 r and 26.2 i mag/arcsec . g band expected SB limit MARILENA SPAVONE STELLAR HALOS 2015 ESO-GARCHING, 23-27 FEBRUARY THE VEGAS SURVEY Multiband u, g, r, i survey of ~ 110 galaxies with vrad < 4000 km/s in all environments (field to clusters). ~ 350 h @ vst over 5 years Expected SB limits: 27.5 g, 27.0 r and 26.2 i mag/arcsec2. -
Large-Scale Study of the NGC 1399 Globular Cluster System in Fornax
A&A 451, 789–796 (2006) Astronomy DOI: 10.1051/0004-6361:20054563 & c ESO 2006 Astrophysics Large-scale study of the NGC 1399 globular cluster system in Fornax L. P. Bassino1,2, F. R. Faifer1,2,J.C.Forte1,B.Dirsch3, T. Richtler3, D. Geisler3, and Y. Schuberth4 1 CONICET and Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, 1900 La Plata, Argentina e-mail: [lbassino;favio;forte]@fcaglp.unlp.edu.ar 2 IALP - CONICET, Argentina 3 Universidad de Concepción, Departamento de Física, Casilla 160, Concepción, Chile e-mail: [email protected];[email protected];[email protected] 4 Sternwarte der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany e-mail: [email protected] Received 21 November 2005 / Accepted 6 January 2006 ABSTRACT We present a Washington C and Kron-Cousins R photometric study of the globular cluster system of NGC 1399, the central galaxy of the Fornax cluster. A large areal coverage of 1 square degree around NGC 1399 is achieved with three adjoining fields of the MOSAIC II Imager at the CTIO 4-m telescope. Working on such a large field, we can perform the first indicative determination of the total size of the NGC 1399 globular cluster system. The estimated angular extent, measured from the NGC 1399 centre and up to a limiting radius where the areal density of blue globular clusters falls to 30 per cent of the background level, is 45 ± 5arcmin,which corresponds to 220−275 kpc at the Fornax distance. -
The Globular Cluster System of NGC 1399
Astronomy & Astrophysics manuscript no. sch1399 c ESO 2018 August 28, 2018 The globular cluster system of NGC 1399 ⋆,⋆⋆ V. dynamics of the cluster system out to 80 kpc Y. Schuberth1,2, T. Richtler2, M. Hilker3, B. Dirsch2, L. P. Bassino4, A. J. Romanowsky5,2, and L. Infante6 1 Argelander-Institut f¨ur Astronomie, Universit¨at Bonn, Auf dem H¨ugel 71, D-53121 Bonn, Germany 2 Universidad de Concepci´on, Departamento de Astronomia, Casilla 160-C, Concepci´on, Chile 3 European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany 4 Facultad de Ciencias Astron´omicas y Geof´ısicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, 1900–La Plata, Argentina; and Instituto de Astrof´ısica de La Plata (CCT La Plata – CONICET – UNLP) 5 UCO/Lick Observatory, University of California, Santa Cruz, CA 95064, USA 6 Departamento de Astronom´ıa y Astrof´ısica, Pontificia Universidad Cat´olica de Chile, Casilla 306, Santiago 22, Chile Received 14 May, 2009; accepted 16 October, 2009 ABSTRACT Globular clusters (GCs) are tracers of the gravitational potential of their host galaxies. Moreover, their kinematic properties may provide clues for understanding the formation of GC systems and their host galaxies. We use the largest set of GC velocities obtained so far of any elliptical galaxy to revise and extend the previous investigations (Richtler et al. 2004) of the dynamics of NGC 1399, the central dominant galaxy of the nearby Fornax cluster of galaxies. The GC velocities are used to study the kinematics, their relation with population properties, and the dark matter halo of NGC 1399. -
Tidal Origin of NGC 1427A in the Fornax Cluster
MNRAS 000,1{9 (2017) Preprint 30 October 2017 Compiled using MNRAS LATEX style file v3.0 Tidal origin of NGC 1427A in the Fornax cluster K. Lee-Waddell1?, P. Serra2;1, B. Koribalski1, A. Venhola3;4, E. Iodice5, B. Catinella6, L. Cortese6, R. Peletier3, A. Popping6;7, O. Keenan8, M. Capaccioli9 1CSIRO Astronomy and Space Sciences, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia 2INAF { Osservatorio Astronomico di Cagliari, Via della Scienza 5, I-09047 Selargius (CA), Italy 3Kapteyn Astronomical Institute, University of Groningen, PO Box 800, NL-9700 AV Groningen, the Netherlands 4Astronomy Research Unit, University of Oulu, FI-90014, Finland 5INAF { Astronomical Observatory of Capodimonte, via Moiariello 16, Naples, I-80131, Italy 6International Centre for Radio Astronomy Research, The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia 7CAASTRO: ARC Centre of Excellence for All-sky Astrophysics, Australia 8School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, United Kingsdom 9Dip.di Fisica Ettore Pancini, University of Naples \Federico II," C.U. Monte SantAngelo, Via Cinthia, I-80126, Naples, Italy Accepted 2017 October 26. Received 2017 October 15; in original form 2017 March 31 ABSTRACT We present new Hi observations from the Australia Telescope Compact Array and deep optical imaging from OmegaCam on the VLT Survey Telescope of NGC 1427A, an arrow-shaped dwarf irregular galaxy located in the Fornax cluster. The data reveal a star-less Hi tail that contains ∼10% of the atomic gas of NGC 1427A as well as extended stellar emission that shed new light on the recent history of this galaxy. -
New Insights from HST Studies of Globular Cluster Systems I: Colors, Distancesprovided by CERN and Document Server Specific Frequencies of 28 Elliptical Galaxies 1
View metadata, citation and similar papers at core.ac.uk brought to you by CORE New Insights from HST Studies of Globular Cluster Systems I: Colors, Distancesprovided by CERN and Document Server Specific Frequencies of 28 Elliptical Galaxies 1 Arunav Kundu 2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 Electronic Mail: [email protected] and Dept of Astronomy, University of Maryland, College Park, MD 20742-2421 Bradley C. Whitmore Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 Electronic Mail: [email protected] Received ; accepted 1Based on observations with the NASA/ESA Hubble Space Telescope, obtained from the data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Re- search in Astronomy, Inc., under NASA contract NAS5-26555 1Present address: Astronomy Department, Yale University, 260 Whitney Av., New Haven, CT 06511 ABSTRACT We present an analysis of the globular cluster systems of 28 elliptical galaxies using archival WFPC2 images in the V and I-bands. The V-I color distributions of at least 50% of the galaxies appear to be bimodal at the present level of photometric accuracy.Weargue that this is indicative of multiple epochs of cluster formation early in the history of these galaxies, possibly due to mergers. We also present the first evidence of bimodality in low luminosity galaxies and discuss its implication on formation scenarios. The mean color of the 28 cluster systems studied by us is V-I = 1.04 0.04 (0.01) mag corresponding to a mean metallicity of Fe/H = -1.0 0.19 (0.04). -
HST Imaging of the Globular Clusters in the Fornax Cluster: NGC 1379
HST Imaging of the Globular Clusters in the Fornax Cluster: NGC 1379 Rebecca A. W. Elson Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK Electronic mail: [email protected] Carl J. Grillmair Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109 USA Electronic mail: [email protected] Duncan A. Forbes School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK Electronic mail: [email protected] Mike Rabban Lick Observatory, University of California, Santa Cruz, CA 95064 USA Electronic mail: [email protected] Gerard. M. Williger Goddard Space Flight Center, Greenbelt, MD 20771 USA Electronic mail: [email protected] arXiv:astro-ph/9710041v1 3 Oct 1997 Jean P. Brodie Lick Observatory, University of California, Santa Cruz, CA 95064 USA Electronic mail: [email protected] Received ; accepted –2– ABSTRACT We present B and I photometry for ∼ 300 globular cluster candidates in NGC 1379, an E0 galaxy in the Fornax Cluster. Our data are from both Hubble Space Telescope (HST) and ground-based observations. The HST photometry (B only) is essentially complete and free of foreground/background contamination to ∼ 2 mag fainter than the peak of the globular cluster luminosity function. Fitting a Gaussian to the luminosity function we find hBi = 24.95 ± 0.30 and σB =1.55 ± 0.21. We estimate the total number of globular clusters to be 436 ± 30. To a radius of 70 arcsec we derive a moderate specific frequency, SN =3.5 ± 0.4. At radii r ∼ 3 − 6 kpc the surface density profile of the globular cluster system is indistinguishable from that of the underlying galaxy light. -
The Globular Cluster System of NGC 1316 (Fornax A) During a Merger Event
Astronomy & Astrophysics manuscript no. (will be inserted by hand later) The Globular Cluster System of NGC 1316 (Fornax A) M. G´omez1,2, T. Richtler3, L. Infante1, and G. Drenkhahn4 1 Departamento de Astronom´ıa y Astrof´ısica, P. Universidad Cat´olica de Chile. Casilla 306, Santiago, Chile e-mail: [email protected],[email protected] 2 Sternwarte der Universit¨at Bonn, Auf dem H¨ugel 71, D-53121 Bonn, Germany 3 Departamento de F´ısica, Universidad de Concepci´on. Casilla 4009, Concepci´on, Chile e-mail: [email protected] 4 Max-Planck-Institut f¨ur Astrophysik, Postfach 1317, D-85741 Garching bei M¨unchen, Germany e-mail: [email protected] Received ... / Accepted ... Abstract. We have studied the Globular Cluster System of the merger galaxy NGC 1316 in Fornax, using CCD BVI photometry. A clear bimodality is not detected from the broadband colours. However, dividing the sample into red (presumably metal-rich) and blue (metal-poor) subpopulations at B − I = 1.75, we find that they follow strikingly different angular distributions. The red clusters show a strong correlation with the galaxy elongation, but the blue ones are circularly distributed. No systematic difference is seen in their radial profile and both are equally concentrated. We derive an astonishingly low Specific Frequency for NGC 1316 of only SN = 0.9, which confirms with a larger field a previous finding by Grillmair et al. (1999). Assuming a “normal” SN of ∼ 4 for early-type galaxies, we use stellar population synthesis models to estimate in 2 Gyr the age of this galaxy, if an intermediate-age population were to explain the low SN we observe. -
115 Abell Galaxy Cluster # 373
WINTER Medium-scope challenges 271 # # 115 Abell Galaxy Cluster # 373 Target Type RA Dec. Constellation Magnitude Size Chart AGCS 373 Galaxy cluster 03 38.5 –35 27.0 Fornax – 180 ′ 5.22 Chart 5.22 Abell Galaxy Cluster (South) 373 272 Cosmic Challenge WINTER Nestled in the southeast corner of the dim early winter western suburbs. Deep photographs reveal that NGC constellation Fornax, adjacent to the distinctive triangle 1316 contains many dust clouds and is surrounded by a formed by 6th-magnitude Chi-1 ( 1), Chi-2 ( 2), and complex envelope of faint material, several loops of Chi-3 ( 3) Fornacis, is an attractive cluster of galaxies which appear to engulf a smaller galaxy, NGC 1317, 6 ′ known as Abell Galaxy Cluster – Southern Supplement to the north. Astronomers consider this to be a case of (AGCS) 373. In addition to his research that led to the galactic cannibalism, with the larger NGC 1316 discovery of more than 80 new planetary nebulae in the devouring its smaller companion. The merger is further 1950s, George Abell also examined the overall structure signaled by strong radio emissions being telegraphed of the universe. He did so by studying and cataloging from the scene. 2,712 galaxy clusters that had been captured on the In my 8-inch reflector, NGC 1316 appears as a then-new National Geographic Society–Palomar bright, slightly oval disk with a distinctly brighter Observatory Sky Survey taken with the 48-inch Samuel nucleus. NGC 1317, about 12th magnitude and 2 ′ Oschin Schmidt camera at Palomar Observatory. In across, is visible in a 6-inch scope, although averted 1958, he published the results of his study as a paper vision may be needed to pick it out. -
Globular Clusters and Galactic Nuclei
Scuola di Dottorato “Vito Volterra” Dottorato di Ricerca in Astronomia– XXIV ciclo Globular Clusters and Galactic Nuclei Thesis submitted to obtain the degree of Doctor of Philosophy (“Dottore di Ricerca”) in Astronomy by Alessandra Mastrobuono Battisti Program Coordinator Thesis Advisor Prof. Roberto Capuzzo Dolcetta Prof. Roberto Capuzzo Dolcetta Anno Accademico 2010-2011 ii Abstract Dynamical evolution plays a key role in shaping the current properties of star clus- ters and star cluster systems. We present the study of stellar dynamics both from a theoretical and numerical point of view. In particular we investigate this topic on different astrophysical scales, from the study of the orbital evolution and the mutual interaction of GCs in the Galactic central region to the evolution of GCs in the larger scale galactic potential. Globular Clusters (GCs), very old and massive star clusters, are ideal objects to explore many aspects of stellar dynamics and to investigate the dynamical and evolutionary mechanisms of their host galaxy. Almost every surveyed galaxy of sufficiently large mass has an associated group of GCs, i.e. a Globular Cluster System (GCS). The first part of this Thesis is devoted to the study of the evolution of GCSs in elliptical galaxies. Basing on the hypothesis that the GCS and stellar halo in a galaxy were born at the same time and, so, with the same density distribution, a logical consequence is that the presently observed difference may be due to evolution of the GCS. Actually, in this scenario, GCSs evolve due to various mechanisms, among which dynamical friction and tidal interaction with the galactic field are the most important. -
Revealing Hidden Substructures in the $ M {BH} $-$\Sigma $ Diagram
Draft version November 14, 2019 A Typeset using L TEX twocolumn style in AASTeX63 Revealing Hidden Substructures in the MBH –σ Diagram, and Refining the Bend in the L–σ Relation Nandini Sahu,1,2 Alister W. Graham2 And Benjamin L. Davis2 — 1OzGrav-Swinburne, Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia 2Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia (Accepted 2019 October 22, by The Astrophysical Journal) ABSTRACT Using 145 early- and late-type galaxies (ETGs and LTGs) with directly-measured super-massive black hole masses, MBH , we build upon our previous discoveries that: (i) LTGs, most of which have been 2.16±0.32 alleged to contain a pseudobulge, follow the relation MBH ∝ M∗,sph ; and (ii) the ETG relation 1.27±0.07 1.9±0.2 MBH ∝ M∗,sph is an artifact of ETGs with/without disks following parallel MBH ∝ M∗,sph relations which are offset by an order of magnitude in the MBH -direction. Here, we searched for substructure in the MBH –(central velocity dispersion, σ) diagram using our recently published, multi- component, galaxy decompositions; investigating divisions based on the presence of a depleted stellar core (major dry-merger), a disk (minor wet/dry-merger, gas accretion), or a bar (evolved unstable 5.75±0.34 disk). The S´ersic and core-S´ersic galaxies define two distinct relations: MBH ∝ σ and MBH ∝ 8.64±1.10 σ , with ∆rms|BH = 0.55 and 0.46 dex, respectively. We also report on the consistency with the slopes and bends in the galaxy luminosity (L)–σ relation due to S´ersic and core-S´ersic ETGs, and LTGs which all have S´ersic light-profiles. -
Bimodality in Low-Luminosity E and S0 Galaxies
Mon. Not. R. Astron. Soc. 387, 331–343 (2008) doi:10.1111/j.1365-2966.2008.13235.x Bimodality in low-luminosity E and S0 galaxies A. E. Sansom⋆ and M. S. Northeast Centre for Astrophysics, University of Central Lancashire, Preston, Lancs PR1 HE Accepted 2008 March 17. Received 2008 February 14; in original form 2007 November 26 ABSTRACT Stellar population characteristics are presented for a sample of low-luminosity early-type galaxies (LLEs) in order to compare them with their more luminous counterparts. Long-slit spectra of a sample of 10 LLEs were taken with the ESO New Technology Telescope, selected for their low luminosities. Line strengths were measured on the Lick standard system. Lick indices for these LLEs were correlated with velocity dispersion (σ), alongside published data for a variety of Hubble types. The LLEs were found to fall below an extrapolation of the correlation for luminous ellipticals and were consistent with the locations of spiral bulges in plots of line strengths versus σ. Luminosity weighted average ages, metallicities and abundance ratios were estimated from χ 2 fitting of 19 Lick indices to predictions from simple stellar population models. The LLEs appear younger than luminous ellipticals and of comparable ages to spiral bulges. These LLEs show a bimodal metallicity distribution, consisting of a low- metallicity group (possibly misclassified dwarf spheroidal galaxies) and a high-metallicity group (similar to spiral bulges). Finally, they have low α-element to iron peak abundance ratios indicative of slow, extended star formation. Key words: galaxies: abundances – galaxies: elliptical and lenticular, cD – galaxies: evolution. -
High Resolution Imaging of the Early-Type Galaxy NGC 1380: an Insight Into the Nature of Extended Extragalactic Star Clusters
A&A 467, 1003–1009 (2007) Astronomy DOI: 10.1051/0004-6361:20066546 & c ESO 2007 Astrophysics High resolution imaging of the early-type galaxy NGC 1380: an insight into the nature of extended extragalactic star clusters A. L. Chies-Santos, B. X. Santiago, and M. G. Pastoriza Departamento de Astronomia, Instituto de Física, UFRGS. Av. Bento Gonçalves 9500, Porto Alegre, RS, Brazil e-mail: [email protected] Received 11 October 2006 / Accepted 27 February 2007 ABSTRACT Context. NGC 1380 is a lenticular galaxy located near the centre of the Fornax Cluster, northeast of NGC 1399. The globular cluster system of this galaxy has hitherto only been studied from the ground. Recent studies of similar early-type galaxies, specially lenticular ones, reveal the existence of star clusters that apparently break up the traditional open/globular cluster dichotomy. Aims. With higher quality photometry from HST/WFPC2 we study the star clusters in NGC 1380, measuring their magnitudes, colours, sizes and projected distances from the centre of the galaxy. Methods. We used deep archival HST/WFPC2 in the B and V bands. We built colour magnitude diagrams from which we selected a sample of cluster candidates. We also analysed their colour distribution and measured their sizes. Based on their location in the luminosity-size diagram we estimated probabilities of them being typical globular clusters as those found in the Galaxy. Results. A total of about 570 cluster candidates were found down to V = 26.5. We measured sizes for approximately 200 of them. The observed colour distribution has three apparent peaks.