Deep optical observations of the massive galaxy cluster Abell 1413

Castagne, D.; Soucail, G.; Pointecouteau, É.; Cappi, A.; Maurogordato, S.; Benoist, Christophe; Ferrari, C.

doi:10.1051/0004-6361/201116837

Cited by 5 publications

(7 citation statements)

References 57 publications

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“…Schombert 1987Schombert , 1988. Early classification efforts assigned the term "cD" to those galaxies (Matthews et al 1964;Morgan & Lesh 1965) whose haloes can in extreme cases embrace the entire host galaxy cluster as in the case of Abell 1413 (Oemler 1976;Castagné et al 2012) frequently also presenting double or multiple nuclei of central galaxies (see Kormendy & Djorgovski 1989, for a discussion of the early literature). In the following, we use the term "cD" in this simple sense, irrespective of whether the halo can photometrically identified as a separate entity or not, see Bender et al (2015) for a more profound discussion.…”

Section: Introductionmentioning

confidence: 99%

The Hydra I cluster core

Hilker

Richtler

Barbosa

et al. 2018

A&A

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Context. NGC 3311, the central galaxy of the Hydra I cluster, shows signatures of recent infall of satellite galaxies from the cluster environment. Previous work has shown that the line-of-sight velocity dispersion of the stars and globular clusters in the extended halo of NGC 3311 rises up to the value of the cluster velocity dispersion. In the context of Jeans models, a massive dark halo with a large core is needed to explain this finding. However, position dependent long-slit measurements show that the kinematics are still not understood. Aims. We aim to find kinematic signatures of sub-structures in the extended halo of NGC 3311. Methods. We performed multi-object spectroscopic observations of the diffuse stellar halo of NGC 3311 using VLT/FORS2 in MXU mode to mimic a coarse “IFU”. The slits of the outermost masks reach out to about 35 kpc of galactocentric distance. We use PPXF to extract the kinematic information of velocities, velocity dispersions and the high-order moments h3 and h4. Results. We find a homogeneous velocity field and velocity dispersion field within a radius of about 10 kpc. Beyond this radius, both the velocities and the velocity dispersion start to depend on azimuth angle and show a significant intrinsic scatter. The inner spheroid of NGC 3311 can be described as a slow rotator. Outside 10 kpc the cumulative angular momentum is rising, however, without showing an ordered rotation signal. If the radial dependence alone is considered, the velocity dispersion does not simply rise but fills an increasingly large range of dispersion values with two well defined envelopes. The lower envelope is about constant at 200 km s−1. The upper envelope rises smoothly, joining the velocity dispersion of the outer globular clusters and the cluster galaxies. We interpret this behaviour as the superposition of tracer populations with increasingly shallower radial distributions between the extremes of the inner stellar populations and the cluster galaxies. Simple Jeans models illustrate that a range of mass profiles can account for all observed velocity dispersions, including radial MOND models. Conclusions. The rising velocity dispersion of NGC 3311 apparently is a result of averaging over a range of velocity dispersions related to different tracer populations in the sense of different density profiles and anisotropies. Jeans models using one tracer population with a unique density profile are not able to explain the large range of the observed kinematics. Previous claims about the cored dark halo of NGC 3311 are therefore probably not valid. This may in general apply to central cluster galaxies with rising velocity dispersion profiles, where infall processes are important.

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Section: Introductionmentioning

confidence: 99%

The Hydra I cluster core

Hilker

Richtler

Barbosa

et al. 2018

A&A

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“…These previous studies at different wavelengths showed that the properties of A1413 are intermediate between classical relaxed and merging clusters. From the morphological point of view, it shows a high ellip-ticity confirmed by both optical (Castagné et al 2012) and X-ray (Pratt & Arnaud 2002) studies. The cluster is elongated approximately in the North-South direction (Fig.…”

Section: Introductionmentioning

confidence: 71%

“…The cluster is elongated approximately in the North-South direction (Fig. 7 of Castagné et al 2012). Studying the galaxy number density distribution, Castagné et al (2012) estimated the value of the cluster ellipticity ∼ 0.35 at large radii, increasing up to ∼0.8 at the cluster center r < 1 .…”

Section: Introductionmentioning

confidence: 99%

“…In this work, we present the galaxy cluster Abell 1413 (hereafter A1413; Planck name: PSZ2 G226.18+76.79), which is a nearby (z = 0.143) massive (M 500 = 5.95 +0.24 −0.25 × 10 14 M , Planck Collaboration XXVII 2016) system. It is well studied in the optical (Castagné et al 2012), X-ray (Pratt & Arnaud 2002), and radio (Govoni et al 2001;Giacintucci et al 2017;Savini et al 2019) bands. These previous studies at different wavelengths showed that the properties of A1413 are intermediate between classical relaxed and merging clusters.…”

Section: Introductionmentioning

confidence: 99%

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LOFAR detection of extended emission around a mini halo in the galaxy cluster Abell 1413

Lusetti,

Bonafede,

Lovisari

et al. 2024

A&A

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The relation between giant radio halos and mini halos in galaxy clusters is not understood. The former are usually associated with merging clusters, while the latter are found in relaxed systems. In recent years, the advent of low-frequency radio observations has challenged this dichotomy by finding intermediate objects with a hybrid radio morphology. We aim to investigate the presence of diffuse radio emission in the cluster Abell 1413 and determine its dynamical status to explore the relation between mini halos and giant radio halos. We used LOFAR observations centred at 144 MHz to study the diffuse radio emission. To investigate the dynamical state of the system, we used newly analysed archival data. Abell 1413 shows features that are typically present in both relaxed (e.g., peaked x-ray surface brightness distribution and some large-scale inhomogeneities) and disturbed (e.g., flatter temperature and metallicity profiles) clusters. This suggests that Abell 1413 is neither disturbed nor fully relaxed, and we argue that it is an intermediate-phase cluster. At 144 MHz, we discover a wider diffuse component surrounding the previously known mini halo at the cluster center. By fitting the radio surface-brightness profile with a double-exponential model, we can disentangle the two components. We find an inner mini halo with an $e$-folding radius, $r_ e,1 kpc,$ and an extended component with e,2 kpc$. We also evaluated the point-to-point correlation between the radio and X-ray surface brightness, finding a sublinear relation for the outer emission and a superlinear relation for the mini halo. The mini halo and the diffuse emission extend over different scales and show different features, confirming the double nature of the radio emission and suggesting that the mechanisms responsible for the re-acceleration of the radio-emitting particle might be different.

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“…Schombert 1987Schombert , 1988. Early classification efforts assigned the term 'cD' to those galaxies (Matthews et al 1964;Morgan & Lesh 1965) whose halos can in extreme cases embrace the entire host galaxy cluster as in the case of Abell 1413 (Oemler 1976;Castagné et al 2012) frequently also presenting double or multiple nuclei of central galaxies (see Kormendy & Djorgovski 1989, for a discussion of the early literature). In the following, we use the term 'cD' in this simple sense, irrespective of whether the halo can photometrically identified as a separate entity or not, see Bender et al (2015) for a more profound discussion.…”

Section: Introductionmentioning

confidence: 99%

The Hydra I cluster core - II. Kinematic complexity in a rising velocity dispersion profile around the cD galaxy NGC 3311

Hilker,

Richtler,

Barbosa

et al. 2018

Preprint

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Context. NGC 3311, the central galaxy of the Hydra I cluster, shows signatures of recent infall of satellite galaxies from the cluster environment. Previous work has shown that the line-of-sight velocity dispersion of the stars and globular clusters in the extended halo of NGC 3311 rises up to the value of the cluster velocity dispersion. In the context of Jeans models, a massive dark halo with a large core is needed to explain this finding. However, position dependent long-slit measurements show that the kinematics are still not understood. Aims. We aim to find kinematic signatures of sub-structures in the extended halo of NGC 3311. Methods. We performed multi-object spectroscopic observations of the diffuse stellar halo of NGC 3311 using VLT/FORS2 in MXU mode to mimic a coarse 'IFU'. The slits of the outermost masks reach out to about 35 kpc of galactocentric distance. We use pPXF to extract the kinematic information of velocities, velocity dispersions and the high-order moments h 3 and h 4 . Results. We find a homogeneous velocity field and velocity dispersion field within a radius of about 10 kpc. Beyond this radius, both the velocities and the velocity dispersion start to depend on azimuth angle and show a significant intrinsic scatter. The inner spheroid of NGC 3311 can be described as a slow rotator. Outside 10 kpc the cumulative angular momentum is rising, however, without showing an ordered rotation signal. If the radial dependence alone is considered, the velocity dispersion does not simply rise but fills an increasingly large range of dispersion values with two well defined envelopes. The lower envelope is about constant at 200 km s −1 . The upper envelope rises smoothly, joining the velocity dispersion of the outer globular clusters and the cluster galaxies. We interpret this behaviour as the superposition of tracer populations with increasingly shallower radial distributions between the extremes of the inner stellar populations and the cluster galaxies. Simple Jeans models illustrate that a range of of mass profiles can account for all observed velocity dispersions, including radial MOND models. Conclusions. The rising velocity dispersion of NGC 3311 apparently is a result of averaging over a range of velocity dispersions related to different tracer populations in the sense of different density profiles and anisotropies. Jeans models using one tracer population with a unique density profile are not able to explain the large range of the observed kinematics. Previous claims about the cored dark halo of NGC 3311 are therefore probably not valid. This may in general apply to central cluster galaxies with rising velocity dispersion profiles, where infall processes are important.

show abstract

Deep optical observations of the massive galaxy cluster Abell 1413

Cited by 5 publications

References 57 publications

The Hydra I cluster core

The Hydra I cluster core

LOFAR detection of extended emission around a mini halo in the galaxy cluster Abell 1413

The Hydra I cluster core - II. Kinematic complexity in a rising velocity dispersion profile around the cD galaxy NGC 3311

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