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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. Non-circular gas motions are found in nine galaxies, with various causes including bars, nuclear outflows, or gravitational disturbances. Several galaxies have signatures of kinematically distinct stellar components, which are likely signatures of accretion or mergers. For all of our galaxies, we compute the angular momentum parameter λR. An evaluation of the galaxies in the λR ellipticity plane shows that all but two of the galaxies have significant support from random stellar motions, and have likely experienced gravitational interactions. This includes some galaxies with very small bulges and truncated/compact Hα morphologies, indicating that such galaxies cannot be fully explained by simple ram pressure stripping, but must have had significant gravitational encounters. Most of the sample galaxies show evidence for ICM-ISM stripping as well as gravitational interactions, indicating that the evolution of a significant fraction of cluster galaxies is likely strongly impacted by both effects. Key words: galaxies: evolution – galaxies: interactions – galaxies: ISM – galaxies: kinematics and dynamics – galaxies: nuclei – galaxies: peculiar 1. INTRODUCTION thus preventing their accretion onto the galaxy (Larson et al. 1980). While all of these processes probably do actually oc- It is well known that the environment affects the morpho- cur, it remains unclear which ones are dominant in driving the logical types of galaxies in clusters. Many studies have shown morphological evolution of cluster galaxies. that galaxies in clusters evolve morphologically with spirals Detailed studies of stellar and ionized gas kinematics can becoming redder and in some cases lenticular as the result help to discriminate between the different interaction processes. of environmental effects (Dressler 1980; Butcher & Oemler For example, gravitational interactions produce disturbed kine- 1978, 1984; Dressler et al. 1997; Poggianti et al. 1999, 2009; matics in both the stellar and gas components, whereas inter- Kormendy & Bender 2012) Several mechanisms have been pro- actions of a hydrodynamic nature will directly affect only the posed for driving galaxy evolution, including processes that gas. Recently, with the advent of Integral Field Units (IFUs) affect the stars, gas, and dark matter, and processes that affect such as DensePak, SAURON, GMOS, SINFONI, and MUSE, only the gas. In the first category, we include the following: these detailed studies have become possible. The observed ve- (1) low-velocity tidal interactions and mergers (e.g., Toomre & locity fields can be compared with those from simulations (e.g., Toomre 1972; Hernquist 1992), (2) high-velocity tidal interac- Bendo & Barnes 2000; Jesseit et al. 2007; Kronberger et al. tions and collisions (e.g., Moore et al. 1996), and (3) tidal inter- 2007, 2008), providing important clues about the physical pro- action between galaxies and the cluster as a whole or between cesses that drive galaxy evolution. galaxies and substructures within the cluster (Bekki 1999). In The Virgo cluster is the nearest moderately rich cluster with the second category, we include the following: (1) intraclus- a galaxy population spanning a large range of morphological ter medium–interstellar medium (ICM-ISM) stripping (Gunn types. The cluster has a moderately dense ICM and is dynam- &Gott1972;Nulsen1982; Schulz & Struck 2001; Vollmer ically young with on-going sub-cluster mergers and infalling et al. 2001; van Gorkom 2004;Cen2014), (2) gas accretion, galaxies, making it an ideal place for detailed studies of various which may occur in the outskirt of clusters, and (3) starvation or environmental processes. Moreover, the Virgo cluster has a sig- strangulation, where the galaxies could lose their gas reservoir, nificant population of galaxies characterized by truncated star formation morphologies with no Hα in the outer disk but strong Hα in the inner region (Koopmann & Kenney, 2004), consis- 5 The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated tent with ICM-ISM stripping. However, some of them also have Universities, Inc. other peculiarities that are not presently well understood, pre- 6 Adjoint Professor. sumably reflecting different types of interactions. These peculiar 1 The Astrophysical Journal Supplement Series, 216:9 (34pp), 2015 January Cortes,´ Kenney, & Hardy Table 1 Galaxy Sample Properties R25 Inc. PA Vhelio DM87 D −1 Name R.A. (J2000) Decl. (J200) RSA/BST RC3 C30 SFC Hc MH (arcsec) (deg) (deg) (km s ) (deg) (Mpc) (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14) (15) a − ± 0.1 ± ± 1.3 NGC 4064 12 04 11.2 18 26 36 SBc(s): SB(s)a:pec 0.43 T/C8.7822.5 0.2 138 70 148 931 12 8.8 18.0 0.8 − ± 0.3 ± ± 1.0 NGC 4293 12 21 12.8 18 22 57 Sa pec (R)SB(s)0/a0.40T/A7.35 23.4 0.2 216 67 62 930 14 6.4 14.1 1.5 − ± ± ± 0.8 NGC 4351 12 24 01.6 12 12 18 Sc(s) II.3 SB(rs)ab: pec 0.37 T/N[s] 10.44 21.1 0.1 92 47 65 2317 16 1.7 20.3 1.2 NGC 4424 12 27 11.5 09 25 15 Sa pec SB(s)a: 0.42 T/C9.17a −21.7 ± 0.3 125 60 88 440 ± 6 3.1 15.2 ± 1.9 + NGC 4429 12 27 26.4 11 06 29 S03(6)/Sa pec SA(r)0 0.54 T/A6.76−24.3 ± 0.1 220 60 89 1127 ± 31 1.5 16.3 ± 0.9 − ± 0.1 ± ± 1.0 NGC 4450 12 28 29.3 17 05 07 Sab pec SA(s)ab 0.49 T/A6.90 23.6 0.2 205 46 179 1958 6 4.7 12.6 0.6 NGC 4457 12 28 59.3 03 34 16 RSb(rs) II (R)SAB(s)0/A0.66T/N[s] 7.96 −23.1 160b 34 c 79d 881 ± 14 8.8 16e NGC 4569 12 36 49.8 13 09 46 Sab(s) I-II SAB(rs)ab 0.43 T/N[s] 6.77 −23.80 ± 0.01 266 64 26 −232 ± 22 1.7 13.0 ± 0.1f NGC 4580 12 37 48.6 05 22 06 Sc/Sa SAB(rs)a pec 0.41 T/N[s] 8.77 −22.95 ± 0.05 87 45 154 1036 ± 7 7.2 22.1 ± 0.5 − ± 0.05 ± ± 1.0 NGC 4606 12 40 57.6 11 54 44 Sa pec SB(s)a: 0.42 T/C9.3022.20 0.11 103 67 44 1655 16 2.5 19.9 0.5 − ± 0.10 ± ± 0.5 NGC 4651 12 43 42.6 16 23 36 Sc(r) I-II SA(rs)c 0.55 N 8.25 23.90 0.04 157 51 72 804 10 5.1 26.9 1.2 − ± ± ± 1.3 NGC 4694 12 48 15.1 10 59 00 Amorph SB0 pec 0.62 T/C9.0321.6 0.2 120 42 146 1177 11 4.5 13.4 1.0 − ± 0.83 ± ± 5.1g NGC 4698 12 48 23.0 08 29 14 Sa SA(s)ab 0.51 A 7.43 24.50 0.41 187 62 169 1005 15 5.8 24.3 4.2 Notes. (1) Galaxy name; (2) right ascension in hours, minutes, and seconds; (3) declination in degrees, minutes, and seconds; (4) Hubble Types from Bingelli et al. (1987, hereafter BST), Sandage & Tammann (1987), or Sandage & Bedke (1994); (5) Hubble type from de Vaucouleurs et al. (1991, hereafter RC3); (6) central R light concentration parameter (Koopmann et al. 2001); (7) star formation class from Koopmann & Kenney (2004); (8) apparent magnitude in H band (Gavazzi et al. 1999); (9) absolute magnitude in H band (Cortes´ et al. 2008); (10) radius in units of arcseconds at the 25 R mag arcsec−2 isophote (Koopmann et al. 2001); (11) inclination from Koopmann et al. (2001); (12) optical PA at R25 (J. R. Cortes´ et al., in preparation); (13) heliocentric radial velocity from HyperLEDA; (14) the projected angular distance in degrees of the galaxy from M87; (15) line-of-sight distance (Cortes´ et al.
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    Astronomy & Astrophysics manuscript no. planck c ESO 2018 October 26, 2018 The Herschel Virgo Cluster Survey? XV. Planck submillimetre sources in the Virgo Cluster M. Baes1, D. Herranz2, S. Bianchi3, L. Ciesla4, M. Clemens5, G. De Zotti5, F. Allaert1, R. Auld6, G. J. Bendo7, M. Boquien8, A. Boselli8, D. L. Clements9, L. Cortese10, J. I. Davies6, I. De Looze1, S. di Serego Alighieri3, J. Fritz1, G. Gentile1;11, J. Gonzalez-Nuevo´ 2, T. Hughes1, M. W. L. Smith6, J. Verstappen1, S. Viaene1, and C. Vlahakis12 1 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281, B-9000 Gent, Belgium 2 Instituto de F´ısica de Cantabria (CSIC-UC), Avda. los Castros s/n, 39005 Santander, Spain 3 INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125, Florence, Italy 4 University of Crete, Department of Physics, Heraklion 71003, Greece 5 INAF-Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 6 School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK 7 UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, United Kingdom 8 Aix Marseille Universite,´ CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France 9 Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK 10 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, 3122, Australia 11 Department of Physics and Astrophysics, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium 12 Joint ALMA Observatory / European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile October 26, 2018 ABSTRACT We cross-correlate the Planck Catalogue of Compact Sources (PCCS) with the fully sampled 84 deg2 Herschel Virgo Cluster Survey (HeViCS) fields.
  • 190 Index of Names

    190 Index of Names

    Index of names Ancora Leonis 389 NGC 3664, Arp 005 Andriscus Centauri 879 IC 3290 Anemodes Ceti 85 NGC 0864 Name CMG Identification Angelica Canum Venaticorum 659 NGC 5377 Accola Leonis 367 NGC 3489 Angulatus Ursae Majoris 247 NGC 2654 Acer Leonis 411 NGC 3832 Angulosus Virginis 450 NGC 4123, Mrk 1466 Acritobrachius Camelopardalis 833 IC 0356, Arp 213 Angusticlavia Ceti 102 NGC 1032 Actenista Apodis 891 IC 4633 Anomalus Piscis 804 NGC 7603, Arp 092, Mrk 0530 Actuosus Arietis 95 NGC 0972 Ansatus Antliae 303 NGC 3084 Aculeatus Canum Venaticorum 460 NGC 4183 Antarctica Mensae 865 IC 2051 Aculeus Piscium 9 NGC 0100 Antenna Australis Corvi 437 NGC 4039, Caldwell 61, Antennae, Arp 244 Acutifolium Canum Venaticorum 650 NGC 5297 Antenna Borealis Corvi 436 NGC 4038, Caldwell 60, Antennae, Arp 244 Adelus Ursae Majoris 668 NGC 5473 Anthemodes Cassiopeiae 34 NGC 0278 Adversus Comae Berenices 484 NGC 4298 Anticampe Centauri 550 NGC 4622 Aeluropus Lyncis 231 NGC 2445, Arp 143 Antirrhopus Virginis 532 NGC 4550 Aeola Canum Venaticorum 469 NGC 4220 Anulifera Carinae 226 NGC 2381 Aequanimus Draconis 705 NGC 5905 Anulus Grahamianus Volantis 955 ESO 034-IG011, AM0644-741, Graham's Ring Aequilibrata Eridani 122 NGC 1172 Aphenges Virginis 654 NGC 5334, IC 4338 Affinis Canum Venaticorum 449 NGC 4111 Apostrophus Fornac 159 NGC 1406 Agiton Aquarii 812 NGC 7721 Aquilops Gruis 911 IC 5267 Aglaea Comae Berenices 489 NGC 4314 Araneosus Camelopardalis 223 NGC 2336 Agrius Virginis 975 MCG -01-30-033, Arp 248, Wild's Triplet Aratrum Leonis 323 NGC 3239, Arp 263 Ahenea