Interacting galaxies in deep fields of the Hubble Space Telescope

Mohamed, Y. H.; Решетников, В. П.

doi:10.1007/s10511-011-9168-7

Cited by 6 publications

(4 citation statements)

References 12 publications

(9 reference statements)

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“…The gravitational interaction among galaxies, most of which are supposed to host a supermassive black hole (BH), with M ≥ 10 6 M (Shankar et al 2004;Lou & Jiang 2008), is a well-established observational fact (Gopal-Krishna et al 2003;Ellison et al 2011;Mohamed & Reshetnikov 2011;Lambas et al 2012). Moreover, in a few documented astrophysical cases, strong indications exist to believe that a binary merger among supermassive BHs has occurred or is ongoing (Rodriguez et al 2006;Komossa et al 2003;Dotti et al 2009).…”

Section: Introductionmentioning

confidence: 99%

Accurate Simulations of Binary Black Hole Mergers in Force-Free Electrodynamics

Alic

Moesta

Rezzolla

et al. 2012

ApJ

100

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We provide additional information on our recent study of the electromagnetic emission produced during the inspiral and merger of supermassive black holes when these are immersed in a force-free plasma threaded by a uniform magnetic field. As anticipated in a recent letter, our results show that although a dual-jet structure is present, the associated luminosity is ∼ 100 times smaller than the total one, which is predominantly quadrupolar. We here discuss the details of our implementation of the equations in which the force-free condition is not implemented at a discrete level, but rather obtained via a damping scheme which drives the solution to satisfy the correct condition. We show that this is important for a correct and accurate description of the current sheets that can develop in the course of the simulation. We also study in greater detail the three-dimensional charge distribution produced as a consequence of the inspiral and show that during the inspiral it possesses a complex but ordered structure which traces the motion of the two black holes. Finally, we provide quantitative estimates of the scaling of the electromagnetic emission with frequency, with the diffused part having a dependence that is the same as the gravitational-wave one and that scales as L non−coll EM ≈ Ω 10/3−8/3 , while the collimated one scales as L coll EM ≈ Ω 5/3−6/3 , thus with a steeper dependence than previously estimated. We discuss the impact of these results on the potential detectability of dual jets from supermassive black holes and the steps necessary for more accurate estimates.

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Section: Introductionmentioning

confidence: 99%

Accurate Simulations of Binary Black Hole Mergers in Force-Free Electrodynamics

Alic

Moesta

Rezzolla

et al. 2012

ApJ

100

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“…When studying distant galaxies, we used the catalog of interacting galaxies found in deep fields of the Hubble Space Telescope (Mohamed and Reshetnikov 2011). This catalog includes data for about seven hundred candidates for galaxies with tidal structures (z ≤ 1.5) in several Hubble deep fields (HDF-N, HDF-S, HUDF, GOODS, GEMS).…”

Section: Nearby and Distant Galaxies With Tidal Structuresmentioning

confidence: 99%

On the characteristics of tidal structures of interacting galaxies

Mohamed,

Reshetnikov,

Sotnikova

2011

Preprint

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We present the results of our analysis of the geometrical tidal tail characteristics for nearby and distant interacting galaxies. The sample includes more than two hundred nearby galaxies and about seven hundred distant ones. The distant galaxies have been selected in several deep fields of the Hubble Space Telescope (HDF-N, HDF-S, HUDF, GOODS, GEMS) and they are at mean redshift z = 0.65. We analyze the distributions of lengths and thicknesses for the tidal structures and show that the tails in distant galaxies are shorter than those in nearby ones. This effect can be partly attributed to observational selection effects, but, on the other hand, it may result from the general evolution of the sizes of spiral galaxies wih z. The location of interacting galaxies on the galaxy luminosity (L) -tidal tail length (l) plane are shown to be explained by a simple geometrical model, with the upper envelope of the observed distribution being l ∝ √ L. We have solved the problem on the relationship between the observed distribution of tail flattening and the tail length in angular measure by assuming the tidal tails to be arcs of circumferences visible at arbitrary angles to the line of sight. We conclude that the angular length of the tidal tails visually distinguished in nearby and distant galaxies, on average, exceeds 180 o .

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“…These observations have shown that as redshift increases, galaxies appear more irregular, have closer neighbors, exhibit features of recent interactions, or appear to be in the process of merging (Burkey et al 1994;Duncan et al 2019, and references therein). Various studies have visually identified and classified these merging systems based upon appearance (Darg et al 2010) and features such as tidal tails, streams, and other diffuse/extended flux regions (Elmegreen et al 2007;Mohamed & Reshetnikov 2011;Elmegreen et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Deep Large Binocular Camera r-band Observations of the GOODS-N Field

Ashcraft

McCabe

Redshaw

et al. 2023

PASP

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We obtained 838 Sloan r-band images (∼28 hr) of the GOODS-North field with the Large Binocular Camera (LBC) on the Large Binocular Telescope in order to study the presence of extended, low surface brightness features in galaxies and investigate the trade-off between image depth and resolution. The individual images were sorted by effective seeing, which allowed for optimal resolution and optimal depth mosaics to be created with all images with seeing FWHM < 0.″9 and FWHM < 2.″0, respectively. Examining bright galaxies and their substructure as well as accurately deblending overlapping objects requires the optimal resolution mosaic, while detecting the faintest objects possible (to a limiting magnitude of m AB ∼ 29.2 mag) requires the optimal depth mosaic. The better surface brightness sensitivity resulting from the larger LBC pixels, compared to those of extant WFC3/UVIS and ACS/WFC cameras aboard the Hubble Space Telescope allows for unambiguous detection of both diffuse flux and very faint tidal tails. Azimuthally-averaged radial surface brightness profiles were created for the 360 brightest galaxies in each of the two mosaics. On average, these profiles showed minimal difference between the optimal resolution and optimal depth surface brightness profiles. However, ≲15% of the profiles show excess flux in the galaxy outskirts down to surface brightness levels of μ r AB ≃ 31 mag arcsec−2. This is relevant to Extragalactic Background Light (EBL) studies as diffuse light in the outer regions of galaxies are thought to be a major contribution to the EBL. While some additional diffuse light exists in the optimal depth profiles compared to the shallower, optimal resolution profiles, we find that diffuse light in galaxy outskirts is a minor contribution to the EBL overall in the r-band.

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Interacting galaxies in deep fields of the Hubble Space Telescope

Cited by 6 publications

References 12 publications

Accurate Simulations of Binary Black Hole Mergers in Force-Free Electrodynamics

Accurate Simulations of Binary Black Hole Mergers in Force-Free Electrodynamics

On the characteristics of tidal structures of interacting galaxies

Deep Large Binocular Camera r-band Observations of the GOODS-N Field

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