Structure, mass and distance of the Virgo cluster from a Tolman-Bondi model

Fouqué, P.; Solanes, J. M.; Sanchís, T.; Balkowski, C.

doi:10.1051/0004-6361:20010833

Cited by 101 publications

(102 citation statements)

References 25 publications

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“…Moreover, the error contours in the ðM VIC ; R VIC Þ plane drawn in Figure 3 show that our predictions are in reasonable agreement with previous estimates of the values of these parameters. Thus, while mass calculations of the central cluster region based on the X-ray emission or the virial theorem amount to about several times 10 14 M , our best estimate M VIC ¼ 2:8 Â 10 15 M approaches the values d2 Â 10 15 M inferred from modelings of the velocity field of the Local Supercluster (Tully & Shaya 1984;Fouqué et al 2001). The acceptable barycentric distances are also well within the very poorly constrained range ($16-24 Mpc) of VIC distances reported in the literature, although our most likely value R VIC ¼ 21:0 Mpc advocates a large distance scale, which, for a cosmological VIC velocity of 1200 km s À1 , brings the local value of the Hubble constant to about 60 km s À1 Mpc À1 .…”

Section: Model Predictions Versus Observationssupporting

confidence: 54%

“…Especially interesting is the case of the H i-deficient background group observed at R $ 28 Mpc and V $ 1000 km s À1 , whose near turnaround position in the Hubble diagram and the assumed standard harmonic oscillation movement of the galaxies around the cluster center, together with a cosmic age presumably close to 13.5 Gyr, indicate that it might have passed through the Virgo core about 4.5 Gyr ago. The fit to the observed velocity field also indicates that a significant number of galaxies in the VIC region might be currently falling toward the cluster from the frontside-perhaps not for the first time either-so it does not substantiate former claims of a paucity of objects of this sort (Fouqué et al 2001). …”

Section: Implications On the Origin Of The Gas Deficiencymentioning

confidence: 63%

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Are the Hi–deficient Galaxies on the Outskirts of Virgo Recent Arrivals?

Sanchís¹,

Solanes²,

Salvador-Solé³

et al. 2002

ApJ

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The presence on the Virgo Cluster outskirts of spiral galaxies with gas deficiencies as strong as those of the inner galaxies stripped by the intracluster medium has led us to explore the possibility that some of these peripheral objects are not newcomers. A dynamical model for the collapse and rebound of spherical shells under the point-mass and radial-flow approximations has been developed to account for the amplitude of the motions in the Virgo I Cluster (VIC) region. According to our analysis, it is not infeasible that galaxies far from the cluster, including those in a gas-deficient group well to its background, went through its core a few Gyr ago. The implications would be (1) that the majority of the H i-deficient spirals in the VIC region might have been deprived of their neutral hydrogen by interactions with the hot intracluster medium and (2) that objects spending a long time outside the cluster cores might keep the gas-deficient status without altering their morphology.

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Section: Model Predictions Versus Observationssupporting

confidence: 54%

Section: Implications On the Origin Of The Gas Deficiencymentioning

confidence: 63%

Are the Hi–deficient Galaxies on the Outskirts of Virgo Recent Arrivals?

Sanchís¹,

Solanes²,

Salvador-Solé³

et al. 2002

ApJ

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“…From formula (45), we can get the distance to M87 with an accuracy of 5% (the error in the angle measurement is negligible). This is already better than standard estimates by classical distance indicators [24], whose accuracy ranges from 10% to 25%.…”

Section: Time Delay In Supermassive Black Hole Lensingmentioning

confidence: 65%

Time Delay in Black Hole Gravitational Lensing as a Distance Estimator

Bozza

Mancini

2004

General Relativity and Gravitation

124

171

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We calculate the time delay between different relativistic images formed by black hole gravitational lensing in the strong field limit. For spherically symmetric black holes, it turns out that the time delay between the first two images is proportional to the minimum impact angle. Their ratio gives a very interesting and precise measure of the distance of the black hole. Moreover, using also the separation between the images and their luminosity ratio, it is possible to extract the mass of the black hole. The time delay for the black hole at the center of our Galaxy is just few minutes, but for supermassive black holes with M = 10 8 ÷ 10 9 M⊙ in the neighbourhood of the Local Group the time delay amounts to few days, thus being measurable with a good accuracy.

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“…The center of Virgo Cluster lies at a distance ≈ 16.5 Mpc [22] at the position of RA=186.8 • and Dec=12.7 • (J2000). Its mass is estimated to be 1.2 × 10 15 M ⊙ within 8 degrees (2.2 Mpc) from the center of the cluster [24]. The angle between the direction of PKS B1424-418 and the Virgo Cluster is ≈ 60 • , much greater than the radius of the Virgo Cluster, so the cluster can be treated as a point source when calculating the gravitational potential.…”

mentioning

confidence: 99%

Testing the Equivalence Principle and Lorentz Invariance with PeV Neutrinos from Blazar Flares

2016

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It was recently proposed that a giant flare of the blazar PKS B1424-418 at redshift z = 1.522 is in association with a PeV-energy neutrino event detected by IceCube. Based on this association we here suggest that the flight time difference between the PeV neutrino and gamma-ray photons from blazar flares can be used to constrain the violations of equivalence principle (EP) and the Lorentz invariance for neutrinos. From the calculated Shapiro delay due to clusters or superclusters in the nearby universe, we find that violation of the equivalence principle for neutrinos and photons is constrained to an accuracy of at least 10 −5 , which is two orders of magnitude tighter than the constraint placed by MeV neutrinos from supernova 1987A. Lorentz invariance violation (LIV) arises in various quantum-gravity theories, which predicts an energy-dependent velocity of propagation in vacuum for photons and neutrinos. We find that the association of the PeV neutrino with the gamma-ray outburst set limits on the energy scale of possible LIV to > 0.01E pl for linear LIV models and > 6 × 10 −8 E pl for quadratic order LIV models, where E pl is the Planck energy scale. These are the most stringent constraints on neutrino LIV for subluminal neutrinos. −262 TeV and a median positional uncertainty of R 50 = 15.9 • centered at the coordinate RA=208.4 • , Dec=−55.8 • (J2000). By searching this field for positional coincidences with gamma-ray-emitting active galactic nuclei (AGNs), a high-fluence outburst of the blazar PKS B1424-418 is found to be in temporal and positional coincidence with the neutrino event [3]. An association between the giant flare of PKS B1424-418 and the PeV neutrino is then suggested based on the unprecedented nature of the two events and a posteriori probability for chance coincidence of about 5% (i.e. a 2 σ confidence correlation) [3]. It is also argued that the flare provides an energy output high enough to explain the observed PeV event [3]. PKS B1424-418 is at redshift z = 1.522 and classified as a flat spectrum radio quasar [5].

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Structure, mass and distance of the Virgo cluster from a Tolman-Bondi model

Cited by 101 publications

References 25 publications

Are the Hi–deficient Galaxies on the Outskirts of Virgo Recent Arrivals?

Are the Hi–deficient Galaxies on the Outskirts of Virgo Recent Arrivals?

Time Delay in Black Hole Gravitational Lensing as a Distance Estimator

Testing the Equivalence Principle and Lorentz Invariance with PeV Neutrinos from Blazar Flares

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