The extended Planetary Nebula Spectrograph (ePN.S) early-type galaxy - - PowerPoint PPT Presentation

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Aug 17, 2022 24 likes •80 views

The extended Planetary Nebula Spectrograph (ePN.S) early-type galaxy survey The kinematic diversity of stellar halos and the relation between halo transition scale and stellar mass Claudia Pulsoni, Ortwin Gerhard, Magda Arnaboldi, and the

SLIDE 1

The extended Planetary Nebula Spectrograph (ePN.S) early-type galaxy survey

The kinematic diversity of stellar halos and the relation between halo transition scale and stellar mass

Claudia Pulsoni, Ortwin Gerhard, Magda Arnaboldi, and the PN.S. Team

SLIDE 2

The extended Planetary Nebula Spectrograph (ePN.S) early-type galaxy survey  

33 early type galaxies with a wide range of

structural parameters (luminosity, central velocity dispersion, ellipticity, boxy/diskyness)

24 fast and 9 slow rotators
nearby, distance < 25 Mpc
Magnitude limited sample,
80-700 PNs per galaxy
Kinematics out to [3 - 13 Re], median 5.6 Re

The PN.S at the William Herschel Telescope, La

Arnaboldi+2018, in prep.

1010.4 < M*/M⊙ < 1011.7

P.I. M. Arnaboldi

M. Capaccioli - A. Chies-Santos - L. Coccato -
A. Cortesi - K. Freeman - O. Gerhard - J. Hartke -
K. Kuijken - A. Longobardi - M. Merrifield - N. R. Napolitano -
C. Pulsoni - A. Romanowsky - C. Tortora - E. Moylan - C. Narayan

Pulsoni et al. 2017arXiv171205833P

SLIDE 3

<V> [km/s]

FAST ROTATOR SLOW ROTATOR

ETGs Kinematics

Pulsoni et al. 2017, 2017arXiv171205833P

Emsellem+2004

Foster+2016 Statler+1999 Weijmans+2009

R / Re

Foster+2016

R / Re

Foster+2016

PAkin − PAphot[deg] Vrot[km/s] σ[km/s] PAkin − PAphot[deg] Vrot[km/s] σ[km/s]

<V> [km/s]

SLIDE 4

Halo Vs Central Kinematics

SLOW ROTATORS
nset of rotation in the halo
FAST ROTATORS
70% with slowly rotating outer

spheroid

30% rapidly rotating at large radii

(extended disk component or rapidly rotating outer spheroid)

40% triaxial fast rotators

consistent with presence of photometric twist

Pulsoni et al. 2017arXiv171205833P

SLIDE 5

Kinematic Transition Radius

The kinematic transition from central regions to halos of ETGs correlates

inversely with mass

RT marks the transition between the inner regions, dominated by the in-

situ stellar component, and the halo, which is mostly accreted

Pulsoni et al. 2017arXiv171205833P