NGVS). XVIII. Measurement and Calibration of Surface Brightness Fluctuation Distances for Bright Galaxies in Virgo (And Beyond
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A Multivariate Statistical Analysis of Spiral Galaxy Luminosities. I. Data and Results
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server A Multivariate Statistical Analysis of Spiral Galaxy Luminosities. I. Data and Results Alice Shapley California Institute of Technology, Pasadena CA, 91125, USA G. Fabbiano Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 P. B. Eskridge Ohio State University, Dept. of Astronomy, 140 W 18th Ave, Columbus, OH 43210 ABSTRACT We have performed a multiparametric analysis of luminosity data for a sample of 234 normal spiral and irregular galaxies observed in X-rays with the Einstein Observatory. This sample is representative of S and Irr galaxies, with a good coverage of morphological types and absolute magnitudes. In addition to X-ray and optical data, we have compiled H-band magnitudes, IRAS near- and far-infrared, and 6cm radio continuum observations for the sample from the literature. We have also performed a careful compilation of distance estimates. We have explored the effect of morphology by dividing the sample into early (S0/a-Sab), intermediate (Sb-Sbc), and late-type (Sc-Irr) subsamples. The data were analysed with bivariate and multivariate survival analysis techniques that make full use of all the information available in both detections and limits. We find that most pairs of luminosities are correlated when considered individually, and this is not due to a distance bias. Different luminosity-luminosity correlations follow different power-law relations. Contrary to previous reports, the LX LB correlation follows a power-law with exponent − larger than 1. Both the significances of some correlations and their power-law relations are morphology dependent. -
Science Goals and Selection Criteria
University of Groningen The ATLAS(3D) project Cappellari, Michele; Emsellem, Eric; Krajnovic, Davor; McDermid, Richard M.; Scott, Nicholas; Kleijn, G. A. Verdoes; Young, Lisa M.; Alatalo, Katherine; Bacon, R.; Blitz, Leo Published in: Monthly Notices of the Royal Astronomical Society DOI: 10.1111/j.1365-2966.2010.18174.x IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2011 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Cappellari, M., Emsellem, E., Krajnovic, D., McDermid, R. M., Scott, N., Kleijn, G. A. V., Young, L. M., Alatalo, K., Bacon, R., Blitz, L., Bois, M., Bournaud, F., Bureau, M., Davies, R. L., Davis, T. A., de Zeeuw, P. T., Duc, P-A., Khochfar, S., Kuntschner, H., ... Weijmans, A-M. (2011). The ATLAS(3D) project: I. A volume-limited sample of 260 nearby early-type galaxies: science goals and selection criteria. Monthly Notices of the Royal Astronomical Society, 413(2), 813-836. https://doi.org/10.1111/j.1365- 2966.2010.18174.x Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. -
Pdf, Integral-Field Stellar and Ionized Gas Kinematics of Peculiar Virgo
The Astrophysical Journal Supplement Series, 216:9 (34pp), 2015 January doi:10.1088/0067-0049/216/1/9 C 2015. The American Astronomical Society. All rights reserved. INTEGRAL-FIELD STELLAR AND IONIZED GAS KINEMATICS OF PECULIAR VIRGO CLUSTER SPIRAL GALAXIES Juan R. Cortes´ 1,2,3,5, Jeffrey D. P. Kenney4, and Eduardo Hardy1,3,5,6 1 National Radio Astronomy Observatory Avenida Nueva Costanera 4091, Vitacura, Santiago, Chile; [email protected], [email protected] 2 Joint ALMA Observatory Alonso de Cordova´ 3107, Vitacura, Santiago, Chile 3 Departamento de Astronom´ıa, Universidad de Chile Casilla 36-D, Santiago, Chile 4 Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520-8101, USA; [email protected] Received 2014 March 10; accepted 2014 November 7; published 2014 December 24 ABSTRACT We present the stellar and ionized gas kinematics of 13 bright peculiar Virgo cluster galaxies observed with the DensePak Integral Field Unit at the WIYN 3.5 m telescope in order to look for kinematic evidence that these galaxies have experienced gravitational interactions or gas stripping. Two-dimensional maps of the stellar velocity V, stellar velocity dispersion σ, and the ionized gas velocity (Hβ and/or [O iii]) are presented for the galaxies in the sample. The stellar rotation curves and velocity dispersion profiles are determined for 13 galaxies, and the ionized gas rotation curves are determined for 6 galaxies. Misalignments between the optical and kinematical major axes are found in several galaxies. While in some cases this is due to a bar, in other cases it seems to be associated with gravitational interaction or ongoing ram pressure stripping. -
The Young Nuclear Stellar Disc in the SB0 Galaxy NGC 1023
MNRAS 457, 1198–1207 (2016) doi:10.1093/mnras/stv2864 The young nuclear stellar disc in the SB0 galaxy NGC 1023 E. M. Corsini,1,2‹ L. Morelli,1,2 N. Pastorello,3 E. Dalla Bonta,` 1,2 A. Pizzella1,2 and E. Portaluri2 1Dipartimento di Fisica e Astronomia ‘G. Galilei’, Universita` di Padova, vicolo dell’Osservatorio 3, I-35122 Padova, Italy 2INAF–Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, I-35122 Padova, Italy 3Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia Accepted 2015 December 3. Received 2015 November 5; in original form 2015 September 11 Downloaded from ABSTRACT Small kinematically decoupled stellar discs with scalelengths of a few tens of parsec are known to reside in the centre of galaxies. Different mechanisms have been proposed to explain how they form, including gas dissipation and merging of globular clusters. Using archival Hubble Space Telescope imaging and ground-based integral-field spectroscopy, we investigated the http://mnras.oxfordjournals.org/ structure and stellar populations of the nuclear stellar disc hosted in the interacting SB0 galaxy NGC 1023. The stars of the nuclear disc are remarkably younger and more metal rich with respect to the host bulge. These findings support a scenario in which the nuclear disc is the end result of star formation in metal enriched gas piled up in the galaxy centre. The gas can be of either internal or external origin, i.e. from either the main disc of NGC 1023 or the nearby satellite galaxy NGC 1023A. The dissipationless formation of the nuclear disc from already formed stars, through the migration and accretion of star clusters into the galactic centre, is rejected. -
Thesis University of Western Australia
Kinematic and Environmental Regulation of Atomic Gas in Galaxies Jie Li March 2019 Master Thesis University of Western Australia Supervisors: Dr. Danail Obreschkow Dr. Claudia Lagos Dr. Charlotte Welker 20/05/2019 Acknowledgments I would like to thank my supervisors Danail Obreschkow, Claudia Lagos and Charlotte Welker for their guidance and support during this project, Luca Cortese, Robert Dˇzudˇzar and Garima Chauhan for their useful suggestions, my parents for giving me financial support and love, and ICRAR for o↵ering an open and friendly environments. Abstract Recent studies of neutral atomic hydrogen (H i) in nearby galaxies find that all isolated star-forming disk-dominated galaxies, from low-mass dwarfs to massive spirals systems, are H i saturated, in that they carry roughly (within a factor 1.5) as much H i fraction as permitted before this gas becomes gravitationally unstable. By taking this H i saturation for granted, the atomic gas fraction fatm of galactic disks can be predicted as a function of a stability parameter q j/M,whereM and j are the baryonic mass and specific / angular momentum of the disk (Obreschkow et al., 2016). The (logarithmic) di↵erence ∆fq between this predictor and the observed atomic fraction can thus be seen as a physically motivated way of defining a ‘H i deficiency’. While isolated disk galaxies have ∆f 0, q ⇡ objects subject to environmental removal/suppression of H i are expected to have ∆fq > 0. Within this framework, we revisit the H i deficiencies of satellite galaxies in the Virgo cluster (from the VIVA sample), as well as in clusters of the EAGLE simulation. -