Intracluster Planetary Nebulae in Clusters and Groups

We present the results from multiple surveys for intracluster planetary nebulae (IPNe) in nearby galaxy clusters and groups. We find that in the case of clusters, our observations imply: 1) the amount of intracluster starlight is significant, up to 20% of the total starlight, 2) in Virgo, is elongated along our line of sight, and 3) is clustered on the sky, implying ongoing tidal stripping. In contrast, searches for IPNe in groups have found little or no intra-group population, implying there may be something in the cluster environment that significantly enhances intracluster star production. from high-resolution N-body simulations, we find that the IPNe should create observable features in position-velocity space, and that these features may eventually allow us to place limits on the dynamics of galaxy clusters.

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Intracluster Planetary Nebulae

Symposium - International Astronomical Union ◽

10.1017/s0074180900209832 ◽

2003 ◽

Vol 209 ◽

pp. 597-604 ◽

Cited By ~ 4

Author(s):

John J. Feldmeier

Keyword(s):

Velocity Field ◽

Stellar Population ◽

Planetary Nebulae ◽

Line Of Sight ◽

Galaxy Groups ◽

The Past ◽

Star Production ◽

Intracluster Light ◽

Lower Luminosity

We review the progress of research on intracluster planetary nebulae (IPN). In the past five years, hundreds of IPN candidates have been detected in the Virgo and Fornax galaxy clusters and searches are also underway in poorer galaxy groups. From the observations to date, and applying the known properties of extragalactic planetary nebulae, the intracluster light in Virgo and Fornax: 1) is significant, at least 20% of the total cluster stellar luminosity, 2) is elongated in Virgo along our line of sight, and 3) may derive from lower-luminosity galaxies, consistent with some models of intracluster star production. A fraction of IPN candidates are not true IPN, but emission-line sources of very large observed equivalent width (≥ 200 Å). The most likely source for these contaminating objects are Lyman-α galaxies at z ≈ 3.1. Follow-up spectroscopy of the IPN candidates will be crucial to discriminate against high red-shift galaxies and to derive the velocity field of the intracluster stellar population.

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High-resolution VLA low radio frequency observations of the Perseus cluster: radio lobes, mini-halo, and bent-jet radio galaxies

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2003 ◽

2020 ◽

Vol 499 (4) ◽

pp. 5791-5805

Author(s):

M Gendron-Marsolais ◽

J Hlavacek-Larrondo ◽

R J van Weeren ◽

L Rudnick ◽

T E Clarke ◽

...

Keyword(s):

High Resolution ◽

Dynamic Range ◽

Galaxy Cluster ◽

High Dynamic Range ◽

Radio Galaxies ◽

Radio Sources ◽

Nearby Galaxy ◽

Cluster Galaxy ◽

Ngc 1275 ◽

Perseus Cluster

ABSTRACT We present the first high-resolution 230–470 MHz map of the Perseus cluster obtained with the Karl G. Jansky Very Large Array. The high dynamic range and resolution achieved have allowed the identification of previously unknown structures in this nearby galaxy cluster. New hints of sub-structures appear in the inner radio lobes of the brightest cluster galaxy NGC 1275. The spurs of radio emission extending into the outer X-ray cavities, inflated by past nuclear outbursts, are seen for the first time at these frequencies, consistent with spectral aging. Beyond NGC 1275, we also analyse complex radio sources harboured in the cluster. Two new distinct, narrowly collimated jets are visible in IC 310, consistent with a highly projected narrow-angle tail radio galaxy infalling into the cluster. We show how this is in agreement with its blazar-like behaviour, implying that blazars and bent-jet radio galaxies are not mutually exclusive. We report the presence of filamentary structures across the entire tail of NGC 1265, including two new pairs of long filaments in the faintest bent extension of the tail. Such filaments have been seen in other cluster radio sources such as relics and radio lobes, indicating that there may be a fundamental connection between all these radio structures. We resolve the very narrow and straight tail of CR 15 without indication of double jets, so that the interpretation of such head–tail sources is yet unclear. Finally, we note that only the brightest western parts of the mini-halo remain, near NGC 1272 and its bent double jets.

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Deep spectroscopy of nearby galaxy clusters – II. The Hercules cluster

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stx371 ◽

2017 ◽

Vol 467 (4) ◽

pp. 4410-4423 ◽

Cited By ~ 9

Author(s):

I. Agulli ◽

J. A. L. Aguerri ◽

A. Diaferio ◽

L. Dominguez Palmero ◽

R. Sánchez-Janssen

Keyword(s):

Galaxy Clusters ◽

Nearby Galaxy

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Studying the dynamical properties of 20 nearby galaxy clusters

Monthly Notices of the Royal Astronomical Society ◽

10.1111/j.1365-2966.2011.19178.x ◽

2011 ◽

Vol 416 (3) ◽

pp. 2027-2040 ◽

Cited By ~ 13

Author(s):

Mohamed H. Abdullah ◽

Gamal B. Ali ◽

H. A. Ismail ◽

Mohamed A. Rassem

Keyword(s):

Galaxy Clusters ◽

Nearby Galaxy ◽

Dynamical Properties

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A comparison between observed and analytical velocity dispersion profiles of 20 nearby galaxy clusters

Astrophysics and Space Science ◽

10.1007/s10509-014-1824-z ◽

2014 ◽

Vol 351 (1) ◽

pp. 289-297

Author(s):

Mohammad S. Khan ◽

Mohamed H. Abdullah ◽

Gamal B. Ali

Keyword(s):

Galaxy Clusters ◽

Velocity Dispersion ◽

Nearby Galaxy

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Massive and refined: A sample of large galaxy clusters simulated at high resolution. I: Thermal gas and properties of shock waves

New Astronomy ◽

10.1016/j.newast.2010.05.003 ◽

2010 ◽

Vol 15 (8) ◽

pp. 695-711 ◽

Cited By ~ 55

Author(s):

F. Vazza ◽

G. Brunetti ◽

C. Gheller ◽

R. Brunino

Keyword(s):

High Resolution ◽

Shock Waves ◽

Galaxy Clusters

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Line of Sight Analysis

10.5194/epsc2021-150 ◽

2021 ◽

Author(s):

Emily Law ◽

Natalie Gallegos ◽

Shan Malhotra

Keyword(s):

High Resolution ◽

Solar System ◽

High Gain ◽

Line Of Sight ◽

Time Intervals ◽

Ground Station ◽

Points Of Interest ◽

Digital Elevation ◽

Initial Release ◽

Elevation Model

The Line of Sight (LoS) is one of the latest tools to join the analytics suite of tools for the Solar System Treks (https://trek.nasa.gov) portals.&#160; The LoS tool provides a way to compute visibility between the entities in our solar system. More concretely, this utility searches for windows of communication or a &#8220;line of sight&#8221; between any two entities. Entities include orbiters, rovers, planetary bodies, ground stations, and other topographical locations. In addition to establishing communications between the two entities, the tool also takes into account local terrains of the entities in question. The software seeks to answer questions about establishing communications between a rover and an orbiter, or an orbiter to a ground station. In mission planning, LoS can be used to determine possible traverses for a rover that must maintain communications with a lander, or find time intervals of communication to an orbiter when a rover or lander are near an obstructing surface feature such as a crater rim or mound. Computations can be even more granular and lines of sight can be computed between mission instruments, thus allowing to ask questions such as &#8220;Is the High Gain Antenna on a rover visible from an orbiter?&#8221; The initial release of the software focuses on the lunar surface and the LRO spacecraft. Users can ask whether a topographical location on the moon is visible from the orbiter or a discrete set of ground stations on Earth. The tool uses NAIF SPICE and various mission kernels for computing planetary geometries. LoS also uses high resolution Digital Elevation Model (DEM) to model the terrain surrounding the points of interest. In-house software is used to convert high resolution DEMs into a format compatible with the tool. Users can provide their own DEMs to model the terrain on different topographical locations to use for their own computations.

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MACS J0416.1–2403: Impact of line-of-sight structures on strong gravitational lensing modelling of galaxy clusters

Astronomy and Astrophysics ◽

10.1051/0004-6361/201731433 ◽

2018 ◽

Vol 614 ◽

pp. A8 ◽

Cited By ~ 13

Author(s):

G. Chirivì ◽

S. H. Suyu ◽

C. Grillo ◽

A. Halkola ◽

I. Balestra ◽

...

Keyword(s):

Galaxy Clusters ◽

Gravitational Lensing ◽

Line Of Sight ◽

Mass Distributions ◽

Strong Gravitational Lensing ◽

Cluster Mass ◽

Critical Curves ◽

Single Lens ◽

Best Fitting ◽

Modelling Techniques

Exploiting the powerful tool of strong gravitational lensing by galaxy clusters to study the highest-redshift Universe and cluster mass distributions relies on precise lens mass modelling. In this work, we aim to present the first attempt at modelling line-of-sight (LOS) mass distribution in addition to that of the cluster, extending previous modelling techniques that assume mass distributions to be on a single lens plane. We have focussed on the Hubble Frontier Field cluster MACS J0416.1–2403, and our multi-plane model reproduces the observed image positions with a rms offset of ~0.′′53. Starting from this best-fitting model, we simulated a mock cluster that resembles MACS J0416.1–2403 in order to explore the effects of LOS structures on cluster mass modelling. By systematically analysing the mock cluster under different model assumptions, we find that neglecting the lensing environment has a significant impact on the reconstruction of image positions (rms ~0.′′3); accounting for LOS galaxies as if they were at the cluster redshift can partially reduce this offset. Moreover, foreground galaxies are more important to include into the model than the background ones. While the magnification factor of the lensed multiple images are recovered within ~10% for ~95% of them, those ~5% that lie near critical curves can be significantly affected by the exclusion of the lensing environment in the models. In addition, LOS galaxies cannot explain the apparent discrepancy in the properties of massive sub-halos between MACS J0416.1–2403 and N-body simulated clusters. Since our model of MACS J0416.1–2403 with LOS galaxies only reduced modestly the rms offset in the image positions, we conclude that additional complexities would be needed in future models of MACS J0416.1–2403.

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