2016A&A...587A..68B


Query : 2016A&A...587A..68B

2016A&A...587A..68B - Astronomy and Astrophysics, volume 587A, 68-68 (2016/3-1)

Spectacular tails of ionized gas in the Virgo cluster galaxy NGC 4569.

BOSELLI A., CUILLANDRE J.C., FOSSATI M., BOISSIER S., BOMANS D., CONSOLANDI G., ANSELMI G., CORTESE L., COTE P., DURRELL P., FERRARESE L., FUMAGALLI M., GAVAZZI G., GWYN S., HENSLER G., SUN M. and TOLOBA E.

Abstract (from CDS):

Using MegaCam at the CFHT, we obtained a deep narrow band Hα+[NII] wide-field image of NGC 4569 (M90), the brightest late-type galaxy in the Virgo cluster. The image reveals the presence of long tails of diffuse ionized gas, without any associated stellar component extending from the disc of the galaxy up to ≃80kpc (projected distance) and with a typical surface brightness of a few 10–18erg/s/cm2/arcsec2. These features provide direct evidence that NGC 4569 is undergoing a ram-presure stripping event. The image also shows a prominent 8kpc spur of ionized gas that is associated with the nucleus that spectroscopic data identify as an outflow. With some assumptions on the 3D distribution of the gas, we use the Hα surface brightness of these extended low-surface brightness features to derive the density and the mass of the gas that has been stripped during the interaction of the galaxy with the intracluster medium. The comparison with ad hoc chemo-spectrophotometric models of galaxy evolution indicates that the mass of the Hα emitting gas in the tail is a large fraction of that of the cold phase that has been stripped from the disc, suggesting that the gas is ionized within the tail during the stripping process. The lack of star-forming regions suggests that mechanisms other than photoionization are responsible for the excitation of the gas (shocks, heat conduction, magneto hydrodynamic waves). This analysis indicates that ram pressure stripping is efficient in massive (Mstar≃1010.5M) galaxies located in intermediate-mass (≃1014M) clusters under formation. It also shows that the mass of gas expelled by the nuclear outflow is only ∼1% than that removed during the ram pressure stripping event. Together these results indicate that ram pressure stripping, rather than starvation through nuclear feedback, can be the dominant mechanism that is responsible for the quenching of the star formation activity of galaxies in high density environments.

Abstract Copyright:

Journal keyword(s): galaxies: individual: NGC 4569 - galaxies: clusters: general - galaxies: clusters: individual: Virgo - galaxies: evolution - galaxies: interactions - galaxies: ISM

VizieR on-line data: <Available at CDS (J/A+A/587/A68): list.dat fits/*>

CDS comments: Table 2 regions not in SIMBAD.

Simbad objects: 21

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Number of rows : 21
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 Feige 34 HS* 10 39 36.7358839104 +43 06 09.212615280 9.613 10.91 11.14 11.319 11.464 sdOp 637 0
2 ACO 1367 ClG 11 44 44.6 +19 41 59           ~ 1036 1
3 NGC 4388 Sy2 12 25 46.820 +12 39 43.45 11.91 11.76 11.02     ~ 1260 2
4 M 86 GiG 12 26 11.814 +12 56 45.49 10.32 9.83 8.90   7.50 ~ 1044 1
5 NAME Virgo Cluster ClG 12 26 32.1 +12 43 24           ~ 6250 0
6 NGC 4438 LIN 12 27 45.6705493536 +13 00 31.708096380 11.37 11.02 10.17     ~ 608 2
7 SDSS J122942.96+104525.0 Sy2 12 29 42.9615849624 +10 45 24.913701540           ~ 88 0
8 IC 3418 LIN 12 29 43.919 +11 24 16.87   16.5       ~ 105 1
9 M 49 Sy2 12 29 46.798 +08 00 01.48   13.21 12.17     ~ 2022 2
10 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6649 3
11 IC 3540 GiG 12 35 27.2277280584 +12 45 00.945699012   14.8       ~ 60 0
12 M 89 LIN 12 35 39.8073444 +12 33 22.830809 11.29 10.73 9.75     ~ 958 2
13 IC 3583 GiG 12 36 43.558 +13 15 32.93   13.31       ~ 166 1
14 M 90 Sy2 12 36 49.8009839880 +13 09 46.523813040 10.56 10.26 9.54     ~ 846 1
15 M 58 SyG 12 37 43.597 +11 49 05.12 10.80 10.48 9.66     ~ 1017 2
16 NGC 4584 H2G 12 38 17.8738601928 +13 06 35.504341524   13.77       ~ 121 1
17 SDSS J123856.86+133305.7 G 12 38 56.862 +13 33 05.77           ~ 8 0
18 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4502 2
19 HZ 44 HS* 13 23 35.2629445608 +36 07 59.544140304 10.186 11.42 11.65 12.00 11.995 sdBN0VIIHe28 392 0
20 ESO 137-1 G 16 13 27.305 -60 45 50.59   14.84   13.87   ~ 102 0
21 ACO 3627 ClG 16 14 22.5 -60 52 07           ~ 271 2

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2022.05.28-23:24:34

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