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

Pulsoni, C.; Gerhard, Ortwin; Arnaboldi, M.; Coccato, L.; Longobardi, A.; Napolitano, N. R.; Moylan, Emily; Narayan, Chaitra A.; Gupta, Vidit; Burkert, Andreas; Capaccioli, M.; Chies-Santos, Ana L.; Cortesi, A.; Freeman, K. C.; Kuijken, Konrad; Merrifield, M. R.; Romanowsky, Aaron J.; Tortora, C.

doi:10.1051/0004-6361/201732473

Cited by 55 publications

(32 citation statements)

References 229 publications

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“…This seems in contradiction with the total density power law ρ tot ∝ r −2.1±0.1 usually found in other determinations. Pulsoni et al (2017) used planetary nebulae (PNe) as tracers of the gravitational field around ellipticals. They obtained two-dimensional velocity and velocity dispersion for 33 ETGs.…”

Section: The Dark Matter Distribution In Ellipticalsmentioning

confidence: 99%

The distribution of dark matter in galaxies

Salucci

2019

Astron Astrophys Rev

239

177

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The distribution of the non-luminous matter in galaxies of different luminosity and Hubble type is much more than a proof of the existence of dark particles governing the structures of the Universe. Here, we will review the complex but well-ordered scenario of the properties of the dark halos also in relation with those of the baryonic components they host. Moreover, we will present a number of tight and unexpected correlations between selected properties of the dark and the luminous matter. Such entanglement evolves across the varying properties of the luminous component and it seems to unequivocally lead to a dark particle able to interact with the Standard Model particles over cosmological times. This review will also focus on whether we need a paradigm shift, from pure collisionless dark particles emerging from "first principles", to particles that we can discover only by looking to how they have designed the structure of the galaxies.

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Section: The Dark Matter Distribution In Ellipticalsmentioning

confidence: 99%

The distribution of dark matter in galaxies

Salucci

2019

Astron Astrophys Rev

239

177

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“…Bellstedt et al (2017) utilises the SKiMS technique which uses DEIMOS slit observations to capture the underlying stellar velocity field and apply a novel interpolation method to obtain a continuous velocity map with a radial coverage out to ∼ 2-3R e . A similar approach is used by Pulsoni et al (2018), however using planetary nebulae as discrete tracers, which allow for a significantly larger radial coverage out to typically ∼ 6R e . Fig.…”

Section: Profile Gradients At Fixed Radii and Maximum Amplitudementioning

confidence: 99%

“…Very recently, the boundaries of observing stellar halo kinematics has been further pushed by Pulsoni et al (2018). Using planetary nebulae as tracers for the underlying stellar velocity field, they observed stellar kinematics out to typically ∼ 6R e , with a range of [3R e − 13R e ].…”

Section: Introductionmentioning

confidence: 99%

Kinematics of simulated galaxies II: Probing the stellar kinematics of galaxies out to large radii

Schulze

Remus

Dolag

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We investigate the stellar kinematics of a sample of galaxies extracted from the hydrodynamic cosmological Magneticum Pathfinder simulations out to 5 half-mass radii. We construct differential radial stellar spin profiles quantified by the observationally widely used λ R and the closely related (V/σ) parameters. We find three characteristic profile shapes: profiles exhibiting a (i) peak within 2.5 half-mass radii and a subsequent decrease (ii) continuous increase that plateaus at larger radii typically with a high amplitude (iii) completely flat behaviour typically with low amplitude, in agreement with observations. This shows that the kinematic state of the stellar component can vary significantly with radius, suggesting a distinct interplay between in-situ star formation and ex-situ accretion of stars. Following the evolution of our sample through time, we provide evidence that the accretion history of galaxies with decreasing profiles is dominated by the anisotropic accretion of low mass satellites that get disrupted beyond ∼ 2.0 half-mass radii, building up a stellar halo with non-ordered motion while maintaining the central rotation already present at z = 2. In fact, at z = 2 decreasing profiles are the predominant profile class. Hence, we can predict a distinct formation pathway for galaxies with a decreasing profile and show that the centre resembles an old embedded disk. Furthermore, we show that the radius of the kinematic transition provides a good estimation for the transition radius from in-situ stars in the centre to accreted stars in the halo. formation on cosmological time-scales, the mechanisms determining the detailed inner baryonic structure of galaxies are still not completely understood (Naab & Ostriker 2017).The broad morphological distinction into late-type galaxies (LTGs) and early-type galaxies (ETGs) is mainly driven by the low-redshift evolution of galaxies. While latetype galaxies are expected to experience a quiet formation pathway, mostly driven by internal secular processes that leave the disc structure in the centre intact, early-type galaxies are subject to a complex interplay between environmental processes like mergers, tidal striping, ram-pressure stripping, harassment and strangulation.Early observations based on photometry perceived ETGs as fairly simple objects without significant internal structure. In contrast to the accepted picture at that time,

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“…Because of their relatively strong [O iii] 5007 Å emission, PNe can be readily identified. They have been shown to be efficient tracers of stellar light in different galaxies like M 87 (Longobardi et al 2013), M 49 (Hartke et al 2017), and many other early-type galaxies (Coccato et al 2009;Cortesi et al 2013;Pulsoni et al 2018). The luminosity-specific PN number (α-parameter) varies slightly with B − V colour of galaxies with higher values for late-type galaxies and lower values for early-type galaxies (Buzzoni et al 2006).…”

Section: Introductionmentioning

confidence: 99%

The survey of planetary nebulae in Andromeda (M 31)

Bhattacharya

Arnaboldi

Hartke

et al. 2019

A&A

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Context. The Andromeda (M 31) galaxy subtends nearly 100 square degrees on the sky. Any study of its halo must therefore account for the severe contamination from the Milky Way halo stars whose surface density displays a steep gradient across the entire M 31 field of view. Aims. Our goal is to identify a population of stars firmly associated with the M 31 galaxy. Planetary nebulae (PNe) are one such population that are excellent tracers of light, chemistry, and motion in galaxies. We present a 16 square degree survey of the disc and inner halo of M 31 with the MegaCam wide-field imager at the CFHT to identify PNe, and characterise the luminosity-specific PN number and PN luminosity function (PNLF) in M 31. Methods. PNe were identified via automated detection techniques based on their bright [O iii] 5007 Å emission and absence of a continuum. Subsamples of the faint PNe were independently confirmed by matching with resolved Hubble Space Telescope sources from the Panchromatic Hubble Andromeda Treasury and spectroscopic follow-up observations with HectoSpec at the MMT. Results. The current survey reaches two magnitudes fainter than the previous most sensitive survey. We thus identify 4289 PNe, of which only 1099 were previously known. By comparing the PN number density with the surface brightness profile of M 31 out to ∼30 kpc along the minor axis, we find that the stellar population in the inner halo has a luminosity-specific PN number value that is seven times higher than that of the disc. We measure the luminosity function of the PN population and find a bright cut-off and a slope consistent with previous determinations. Interestingly, it shows a significant rise at the faint end, present in all radial bins covered by the survey. This rise in the M 31 PNLF is much steeper than that observed for the Magellanic clouds and Milky Way bulge. Conclusions. The significant radial variation of the PN specific frequency value indicates that the stellar population at deprojected minor-axis radii larger than ∼10 kpc is different from that in the disc of M 31. The rise at the faint end of the PNLF is a property of the late phases of the stellar population. M 31 shows two major episodes of star formation and the rise at the faint end of the PNLF is possibly associated with the older stellar population. It may also be a result of varying opacity of the PNe.

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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

Cited by 55 publications

References 229 publications

The distribution of dark matter in galaxies

The distribution of dark matter in galaxies

Kinematics of simulated galaxies II: Probing the stellar kinematics of galaxies out to large radii

The survey of planetary nebulae in Andromeda (M 31)

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