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.