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-Hα+[NII] image of M86 region superposed on a color SDSS gri image. The Hα image is stretched to highlight the faint emission. The "low-velocity" (<500 km/s) Hα+[NII] emission is colored red, and the "high-velocity" (>2000 km/s) Hα+[NII] emission is colored green. The low-velocity emission is attributed to gas stripped from NGC 4438 in a collision with M86 and subsequently heated. High-velocity emission is observed near NGC 4388 in the lower right, although it does not extend all the way to M86, so it is unclear whether it is related.

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Deep wide-field H$\alpha$+[NII] imaging around the Virgo cluster giant elliptical galaxy M86 reveals a highly complex and disturbed ISM/ICM. The most striking feature is a set of H$\alpha$ filaments which clearly connect M86 with the nearby disturbed spiral NGC 4438 (23$'$=120 kpc projected away), providing strong evidence for a previously unrecogn...

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... were pro- cessed and mosaiced together in a standard way, except for ad- ditional flat fielding corrections using masked image frames, and a pupil correction for the Hα images. The Hα image superposed on an SDSS gri image (Adelman-McCarthy et al 2007) is shown in Figure 1, the R-band image is shown in We obtained spectroscopy at 24 selected positions near M86 with the SparsePak integral field unit (IFU) on the WIYN telescope. SparsePak ( Bershady et al. 2004) is a 90-fiber array which loosely covers an 80 ′′ ×80 ′′ field of view, with 5" diameter fibers. ...

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... These features are tidal tails formed after the gravitational interaction of the galaxy with M86 and NGC 4435 (e.g. Combes et al. 1988;Boselli et al. 2005;Kenney et al. 2008). Although the gas can be partly removed by ram pressure (Vollmer et al. 2009), the dominant perturbing mechanism is gravitational since able to act on the stellar component. ...
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... Observational measurements and upper limits are shown as discrete symbols. Bright Hα features include the M82 Cap (Lehnert et al. 1999), the Virgo filaments (Kenney et al. 2008), edge-on galaxies (Christlein et al. 2010), NGC 7793 (Dicaire et al. 2008), UGC 7321 (Adams et al. 2011), NGC 247 (Hlavacek-Larrondo et al. 2011, the outer disk of M31 (Madsen et al. 2001), the Leo Ring (Donahue et al. 1995), and the Virgo HI cloud (Weymann et al. 2001). The dashed and solid light grey lines around 100 mR represent Hα emission observations and surface brightness predictions for the Magellanic stream/bridge (Bland-Hawthorn et al. 2007;Barger et al. 2013). ...
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... SOFIA FIFI-LS observations were obtained for the nearest 6 out of the 12 proposed galaxies. The six galaxies included here should be regarded as an ex- Note-(1) : Galaxy name ; (2) : velocity from NED ; (3) : distance from Tonry et al. (2001); (4) : linear size conversion; (5) : Galaxy Type; Type T parameter in brackets from hyperleda a (6) : absolute K band magnitude MK (2MASS keyword k m ext) from Cappellari et al. (2011); (7) : effective radius Re from Cappellari et al. (2011);(8,9,10) : ellipticity, specific stellar angular momentum, Fast or Slow rotator (Slow if 0.31 √ e/λRe > 1) at Re; (11,12) : Hα+ [NII] fluxes and references (1 : Gavazzi et al. (2018); 2 : Trinchieri & di Serego Alighieri (1991); 3 : Kenney et al. (2008); 4 : Macchetto et al. (1996); 5 : Ho et al. (1997); 6 : Boselli et al. (2021)) (13) : gas mass estimated using a gas-to-dust ratio of 100 and the dust masses calculated by Amblard et al. (2014) using Spitzer and Herschel fluxes of these galaxies (Temi et al. 2009;Amblard et al. 2014); a :added to the sample to present new ALMA CO(3-2) data. a http://leda.univ-lyon1.fr/ ...
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... SOFIA FIFI-LS observations were obtained for the nearest 6 out of the 12 proposed galaxies. The six galaxies included here should be regarded as an ex- Note-(1) : Galaxy name ; (2) : velocity from NED ; (3) : distance from Tonry et al. (2001); (4) : linear size conversion; (5) : Galaxy Type; Type T parameter in brackets from hyperleda a (6) : absolute K band magnitude MK (2MASS keyword k m ext) from Cappellari et al. (2011); (7) : effective radius Re from Cappellari et al. (2011);(8,9,10) : ellipticity, specific stellar angular momentum, Fast or Slow rotator (Slow if 0.31 √ e/λRe > 1) at Re; (11,12) : Hα+ [NII] fluxes and references (1 : Gavazzi et al. (2018); 2 : Trinchieri & di Serego Alighieri (1991); 3 : Kenney et al. (2008); 4 : Macchetto et al. (1996); 5 : Ho et al. (1997); 6 : Boselli et al. (2021)) (13) : gas mass estimated using a gas-to-dust ratio of 100 and the dust masses calculated by Amblard et al. (2014) using Spitzer and Herschel fluxes of these galaxies (Temi et al. 2009;Amblard et al. 2014); a :added to the sample to present new ALMA CO(3-2) data. a http://leda.univ-lyon1.fr/ ...
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... Sabater et al. 2013). Indeed lines of support include: i) recent observations of Hα emission in NGC 4406 (Kenney et al. 2008), some of which is colocated in the region of its X-ray plume, suggest a collision with NGC 4438 as its origin; ii) NGC 4261 has a well defined disk of dust, 240 pc in diameter, that is aligned with its radio axis and perpendicular to the stellar component of the galaxy; iii) in NGC 4374 the dust lane major axis is strongly misaligned with the major axis of the stars and the kinematic of molecular gas is inconsistent with a stellar mass loss origin; iv) the giant elliptical NGC 4552 which is falling into the Virgo cluster, has central X-ray emission features (Machacek et al. 2006a) characteristic of a supersonic ram-pressure stripping of the gas, produced by its motion in the Virgo ICM. Overall, albeit suggestive, these remain qualitative features that require to be further tested with future targeted and deeper observations. ...
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... The stripping tails of cluster late-type galaxies have been observed from radio, mm, IR, and optical to X-ray (e.g. Gavazzi & Jaffe 1987;Gavazzi et al. 2001;Yoshida et al. 2002Yoshida et al. , 2004Oosterloo & van Gorkom 2005;Sun et al. 2007b;Yagi et al. 2007;Chung et al. 2007;Yoshida et al. 2008;Kenney et al. 2008;Sun et al. 2010;Yagi et al. 2010;Smith et al. 2010;Hester et al. 2010;Sivanandam et al. 2010;Fossati et al. 2012;Merluzzi et al. 2013;Jáchym et al. 2014;Kenney et al. 2014;Boselli et al. 2016;Poggianti et al. 2017;Gavazzi et al. 2018;Chen et al. 2020). In contrast to the early general wisdom that the stripped cold gas will simply mix with the hot ICM and be heated, now it is known that some fraction of the stripped ISM can collapse and form stars in the galactic halo and the intracluster space, especially in high-ICM-pressure environments (e.g. ...
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