2018A&A...616A.123H


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.07CET13:21:42

2018A&A...616A.123H - Astronomy and Astrophysics, volume 616A, 123-123 (2018/8-1)

Three dynamically distinct stellar populations in the halo of M49.

HARTKE J., ARNABOLDI M., GERHARD O., AGNELLO A., LONGOBARDI A., COCCATO L., PULSONI C., FREEMAN K.C. and MERRIFIELD M.

Abstract (from CDS):


Context. M49 (NGC 4472) is the dominant galaxy in subcluster B of the Virgo Cluster, and a benchmark for studying the build-up of the extended halos of brightest group galaxies in the outskirts of galaxy clusters.
Aims. We investigate the kinematics in the outer halo of M49, look for substructures, and describe the transition to the surrounding intra-group light.
Methods. As kinematic tracers, we use planetary nebulae (PNe), combining kinematics from the extended Planetary Nebula Spectrograph (PN.S) early-type galaxy survey with our recent deep photometric sample. We study the position-velocity-plane for bright and faint PN populations out to 95kpc radius, and employ a multi-Gaussian model for the velocity distribution to identify stellar populations with distinct kinematics and histories.
Results. We report the detection of stellar-kinematic substructure associated with the interaction of M49 with the dwarf irregular galaxy VCC 1249. We find two kinematically distinct PN populations associated with the main M49 halo and the extended intra-group light (IGL). These have velocity dispersions σhalo~=170km/s and σIGL~=400km/s at 10-80kpc radii. The overall luminosity profile and velocity dispersion at ∼80kpc are consistent with a flat circular velocity curve extrapolated from X-ray observations. The dispersion of the PNe associated with the IGL joins onto that of the satellite galaxies in subcluster B at ∼100kpc radius. This is the first time that the transition from halo to IGL is observed based on the velocities of individual stars.
Conclusions. Therefore the halo of M49, consisting of at least three distinct components, has undergone an extended accretion history within its parent group potential. The blue colours of the IGL component are consistent with a population of stars formed in low-mass galaxies at redshift ∼0.5 that has since evolved passively, as suggested by other data.

Abstract Copyright: © ESO 2018

Journal keyword(s): galaxies: individual: M49 - galaxies: elliptical and lenticular, cD - galaxies: clusters: individual: Virgo - galaxies: halos - planetary nebulae: general

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10605 1
2 M 74 G 01 36 41.772 +15 47 00.46 10.52 10.00 9.46 9.16   ~ 1342 1
3 NAME Hydra I Cluster ClG 10 36 36.0 -27 31 04           ~ 765 1
4 M 84 Sy2 12 25 03.74333 +12 53 13.1393 12.67 12.09 10.49     ~ 1610 2
5 M 86 GiG 12 26 11.814 +12 56 45.49 10.32 9.83 8.90   7.50 ~ 997 1
6 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5667 0
7 M 49 Sy2 12 29 46.798 +08 00 01.48   13.21 12.17     ~ 1925 2
8 UGC 7636 LSB 12 30 00.350 +07 55 47.44   15.4       ~ 114 0
9 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6045 3
10 NGC 4697 GiG 12 48 35.8992791100 -05 48 02.497675635   10.97   9.83   ~ 784 0
11 ACO 2199 ClG 16 28 37.0 +39 31 28           ~ 1086 1
12 3C 338.0 QSO 16 28 38.2443686587 +39 33 04.231770853   12.78 11.78     ~ 690 5
13 NAME Virgo Extension GrG ~ ~           ~ 42 0

    Equat.    Gal    SGal    Ecl

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2019.12.07-13:21:42

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