An H<scp>i</scp>Aperture Synthesis Mosaic of the Large Magellanic Cloud

Kim, Sungeun; Staveley‐Smith, L.; Dopita, Michael A.; Freeman, K. C.; Sault, R. J.; Kesteven, M. J.; McConnell, D.

doi:10.1086/306030

Cited by 398 publications

(637 citation statements)

References 28 publications

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“…For the two weaker sources, the uncertainty in the LMC absorbing column was larger than the derived value; for those objects, we list the 3 j upper limits in Table 2. For comparison, in Table 2 we list the hydrogen column density from the Australia Telescope Compact Array (ATCA) 21 cm observations by Kim et al (1998). The values derived from the X-ray spectral fits are in reasonable agreement with the measurements of the hydrogen content in the LMC.…”

Section: New Quasarsmentioning

confidence: 57%

“…First, the assumed value for the Galactic absorption may be overestimated, resulting in underestimating the LMC component of the absorbing column. Second, it is well established (e.g., Kim et al 1998) that the distribution of hydrogen in the LMC is far from homogeneous. The measurements from Kim et al (1998) are effectively averaged over a spatial resolution element of ∼1Ј (15 pc at the LMC), while the X-ray absorption is probing a specific line of sight.…”

Section: New Quasarsmentioning

confidence: 99%

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Discovery of Four X-Ray Quasars behind the Large Magellanic Cloud

Dobrzycki

Groot

Macri

et al. 2002

The Astrophysical Journal

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We present the discovery of four X-ray quasars ( , 0.53, 0.61, and 1.63) located behind the Large z p 0.26 em Magellanic Cloud; three of them are located behind the bar of the LMC. The quasars were identified via spectroscopy of optical counterparts to X-ray sources found serendipitously by the Chandra X-Ray Observatory satellite. All four quasars have archival VI photometry from the second phase of the Optical Gravitational Lensing Experiment (OGLE-II); one of them was found by OGLE to be variable. We present the properties of the quasars and discuss their possible applications.

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Section: New Quasarsmentioning

confidence: 57%

Section: New Quasarsmentioning

confidence: 99%

Discovery of Four X-Ray Quasars behind the Large Magellanic Cloud

Dobrzycki

Groot

Macri

et al. 2002

The Astrophysical Journal

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“…It is located at D ≈ 48.5 kpc from the center of MW. Up to 8.9 kpc its stellar disk mass is ∼2.7 × 10 9 M (de Vaucouleurs & Freeman 1972;Bothum & Thompson 1988;Zaritsky 1999;Bell & de Jong 2001) and the neutral gas mass is ∼0.5 × 10 9 M (Kim et al 1998); these masses contribute to the circular velocity of 39.3 km s −1 . The circular velocity derived by Van der Marel et al (2002) at 8.9 kpc is 64.8 ± 15.9 km s −1 ; consequently, a dark halo must exist in this galaxy.…”

Section: Numerical Results and Discussionmentioning

confidence: 99%

Mass limits for dark clusters of degenerate fermions

Membrado

Pacheco

2013

A&A

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We calculate the range of possible masses for dark spheres of bound fully degenerate fermions as a function of the fermion mass. The cosmological constant is included in our calculations. We deduce that the minimum fermion mass that is able to give rise to degenerate fermion clusters is ∼0.02 g −1/4 eV, where g is the spin degeneracy parameter. We show that degenerate fermions of mc 2 ≈ (15−30) g −1/4 eV can build bound degenerate dark haloes that could reproduce the values of the rotation velocities of galaxies. The masses and radii derived for these degenerate dark haloes of typical galaxies, without considering any cosmological information, agree with the Jeans masses and radii of a cosmological background of ∼(20−30) g −1/4 eV degenerate fermions at redshift z ≈ 50. However, degenerate fermion objects of 10 15 M composed of these particles are too small to constitute the dark halo of galaxy clusters. We also derive degeneracy conditions for hot and cold dark matter fermions.

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“…A new H I mosaic survey with the ATCA (Kim et al 1998) shows the overall rotation pattern clearly. A tilted ring analysis of the H I velocity field shows a strong radial change in the position angle of the kinematic line of nodes.…”

Section: The Rotation Of the Lmcmentioning

confidence: 94%