Kinematics of the outer halo of M 87 as mapped by planetary nebulae

Longobardi, A.; Arnaboldi, M.; Gerhard, Ortwin; Pulsoni, C.; Söldner-Rembold, Isabella

doi:10.1051/0004-6361/201832729

Cited by 51 publications

(70 citation statements)

References 97 publications

(232 reference statements)

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“…On the other hand, the substructure explanation seems more aligned with GCs on possible tangential orbits in M87, since the Virgo cluster is known to be not fully relaxed. Moreover, substructure in the kinematics of planetary nebulae in the Virgo cluster have already been identified (Longobardi et al 2018). Although differentiating between these two mechanisms may probe difficult, our results indicate that localized tangentially biased orbits are not inconsistent with the accretion build up of the ICGC component.…”

Section: Intracluster Gcs As Kinematic Tracers Of the Dark Mattersupporting

confidence: 49%

Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris

Ramos

Sales

Abadi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the assembly of globular clusters (GCs) in 9 galaxy clusters using the cosmological simulation Illustris. GCs are tagged to individual galaxies at infall time and their tidal removal and distribution within the cluster is followed later self-consistently by the simulation. The method relies on the simple assumption of a single power-law relation between halo mass (M vir ) and mass in GCs (M GC ) as found in observations. We find that the GCs specific frequency S N as a function of V-band magnitude naturally reproduces the observed "U"-shape, due to the combination of a power law M GC -M vir relation and the non-linear M * -M vir relation from the simulation. Additional scatter in the S N values are traced back to galaxies with early infall times due to the evolution in the M * -M vir relation with redshift. GCs that have been tidally removed from their galaxies form today the intra-cluster component from which about ∼ 60% were brought in by galaxies that orbit today within the cluster potential. The remaining "orphan" GCs are contributed by satellite galaxies with a wide range of stellar masses that are fully tidally disrupted at z = 0. This intra-cluster component is a good dynamical tracer of the dark matter potential providing an estimate of the velocity dispersion of the dark matter with 25% accuracy. As a consequence of the accreted nature of most intra-cluster GCs, their orbits are fairly radial with a predicted orbital anisotropy β ≥ 0.5. However, local tangential motions may appear as a consequence of localized substructure, providing a possible interpretation to the β < 0 values suggested in observations of M87 or NGC 1407. † Hellman Fellow cause of their inferred old ages (Vandenberg et al. 1996) clustered distribution around galaxies, they are believed to be surviving probes of the early star formation in the universe.GCs are, however, more metal poor than the bulk of the stars in their host galaxy. In fact, GCs display a wide range of colors and metallicities suggestive of a separation where the youngest and more metal rich GCs are formed insitu -and perhaps associated to major mergers-while the metal poor component is likely acquired hierarchically via the accretion of smaller galaxies (e.g.

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Section: Intracluster Gcs As Kinematic Tracers Of the Dark Mattersupporting

confidence: 49%

Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris

Ramos

Sales

Abadi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…M87 is (in projection) near the X-ray gas emission peak (e.g., Kellogg et al 1971) which is a good tracer for the potential minimum of the cluster. Moreover, the rising velocity dispersion profile of the surrounding planetary nebulae is steeper for M87 (Longobardi et al 2018) than for M49 (Hartke et al 2018), showing that intracluster planetary nebulae are more centered on M87 than on M49. The velocity dispersion profile of the globular clusters rises towards the outskirts of M87 (Côté et al 2001) but it falls towards the outskirts of M49 (Sharples et al 1998), showing that also the intracluster globular clusters are more centered on M87.…”

Section: Introductionmentioning

confidence: 94%

Structure of Brightest Cluster Galaxies and Intracluster Light

Kluge

Neureiter

Riffeser

et al. 2020

ApJS

120

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Observations of 170 local (z 0.08) galaxy clusters in the northern hemisphere have been obtained with the Wendelstein Telescope Wide Field Imager (WWFI). We correct for systematic effects such as PSF broadening, foreground stars contamination, relative bias offsets and charge persistence. Scattered light induced background inhomogeneities are reduced down to ∆SB > 31 g' mag arcsec −2 by large dithering and subtraction of night-sky flats. Residual background inhomogeneities brighter than SB σ < 27.6 g' mag arcsec −2 caused by galactic cirrus are detected in front of 23% of the clusters. However, the large field of view allows to discriminate between accretion signatures and galactic cirrus. We detect accretion signatures in form of tidal streams in 22%, shells in 9.4%, multiple nuclei in 47% and two Brightest Cluster Galaxies (BCGs) in 7% of the clusters / BCGs.We measure semi-major axis surface brightness profiles of the BCGs and their surrounding Intracluster Light (ICL) down to a limiting surface brightness of SB = 30 g' mag arcsec −2 . The spatial resolution in the inner regions is increased by combining the WWFI light profiles with those that we measured from archival Hubble Space Telescope images or deconvolved WWFI images. We find that 71% of the BCG+ICL systems have SB profiles that are well described by a single Sérsic (SS) function whereas 29% require a double Sérsic (DS) function to obtain a good fit. SS BCGs, having more symmetric isophotal shapes and fewer detected accretion signatures than DS BCGs, appear to have slightly more relaxed morphology than their DS counterparts. Members of the latter type encompass S2 = 52 ± 21% of their total light in the outer Sérsic component. There is a wide scatter in transition radii r × between the two Sérsic components and surface brightnesses at the transition radii SB(r × ). The integrated brightnesses of the BCG+ICL systems correlate only weakly with S2, r × and SB(r × ). That indicates that the outer Sérsic component is unlikely to trace the dynamically hot ICL since BCG+ICL systems grow at present epoch predominantly in their outskirts.We find that BCGs have scaling relations that differ markedly from those of normal ellipticals, likely due to their indistinguishable embedding in the ICL. The most extended BCG+ICL systems have luminosities and radii comparable to whole clusters. We use different plausible estimates for the ICL component (based on an integrated brightness threshold, SB thresholds and profile decompositions) and find that they do not affect our conclusions about the properties of the ICL. On average, the ICL seems to be better aligned than the BCG with the host cluster in terms of position angle and centering. That makes it a potential Dark Matter tracer. We find positive correlations between BCG+ICL brightness and cluster mass, cluster radius, cluster richness and integrated satellite brightness, confirming that BCG/ICL growth is indeed coupled with cluster growth.

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“…The kinematics of planetary nebulae in galaxies in the Virgo cluster have been studied by many authors (Longobardi et al 2013(Longobardi et al , 2015Hartke et al 2018;Longobardi et al 2018). These studies have found that in M87 and M49 the planetary nebulae of the ICL have different velocity and spatial distributions than those in the BCG halo.…”

Section: The Icl Is a Distinct Kinematic Component Separate From Thementioning

confidence: 99%

Clocking the formation of today’s largest galaxies: wide field integral spectroscopy of brightest cluster galaxies and their surroundings

Edwards

Salinas

Stanley

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The formation and evolution of local brightest cluster galaxies (BCGs) is investigated by determining the stellar populations and dynamics from the galaxy core, though the outskirts and into the intracluster light (ICL). Integral spectroscopy of 23 BCGs observed out to 4 r e is collected and high signal-to-noise regions are identified. Stellar population synthesis codes are used to determine the age, metallicity, velocity, and velocity dispersion of stars within each region. The intracluster light (ICL) spectra are best modeled with populations that are younger and less metal-rich than those of the BCG cores. The average BCG core age of the sample is 13.3 ± 2.8 Gyr and the average metallicity is [Fe/H] = 0.30 ± 0.09, whereas for the ICL the average age is 9.2 ± 3.5 Gyr and the average metallicity is [Fe/H] = 0.18 ± 0.16. The velocity dispersion profile is seen to be rising or flat in most of the sample (17/23), and those with rising values reach the value of the host cluster's velocity dispersion in several cases. The most extended BCGs are closest to the peak of the cluster's X-ray luminosity. The results are consistent with the idea that the BCG cores and inner regions formed quickly and long ago, with the outer regions and ICL forming more recently, and continuing to assemble through minor merging. Any recent star formation in the BCGs is a minor component, and is associated with the cluster cool core status.

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Kinematics of the outer halo of M 87 as mapped by planetary nebulae

Cited by 51 publications

References 97 publications

Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris

Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris

Structure of Brightest Cluster Galaxies and Intracluster Light

Clocking the formation of today’s largest galaxies: wide field integral spectroscopy of brightest cluster galaxies and their surroundings

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