A high sensitivity Hi survey of the sky at δ ≤ -25°

Arnal, E. M.; Bajaja, E.; Larrarte, J. J.; Morras, R.; Pöppel, W. G. L.

doi:10.1051/aas:2000134

Cited by 92 publications

(90 citation statements)

References 5 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The spectra were fitted with the XSPEC software using the combined mekal * wabs model, in which the former describes the ICM emission, and the latter describes the Galactic absorption with a Galactic hydrogen column density of n H . We freeze the cluster redshift to 0.2153 and n H to the value of 6.08 × 10 20 cm −2 given by the LAB survey (Hartmann & Burton 1997;Arnal et al 2000;Bajaja et al 2005;Kalberla et al 2005) at the X-ray flux-weighted centroid.…”

Section: Temperature and Surface Brightness Distributionsmentioning

confidence: 99%

Probing cluster dynamics in RXC J1504.1-0248 via radial and two-dimensional gas and galaxy properties

Zhang

Verdugo

Klein

et al. 2012

A&A

View full text Add to dashboard Cite

We study one of the most X-ray luminous cluster of galaxies in the REFLEX survey, RXC J1504.1-0248 (hereafter R1504; z cl = 0.2153), using XMM-Newton X-ray imaging spectroscopy, VLT/VIMOS optical spectroscopy, and WFI optical imaging. The mass distributions were determined using both the so-called hydrostatic method with X-ray imaging spectroscopy and the dynamical method with optical spectroscopy, respectively, which yield M H.E. 500 = (5.81 ± 0.49) × 10 14 M and M caustic 500 = (4.17 ± 0.42) × 10 14 M . According to recent calibrations, the richness-derived mass estimates closely agree with the hydrostatic and dynamical mass estimates. The line-of-sight velocities of spectroscopic members reveal a group of galaxies with high velocities (>1000 km s −1 ) at a projected distance of about r H.E. 500 = (1.18 ± 0.03) Mpc south-east of the cluster centroid, which is also indicated in the X-ray two-dimensional (2D) temperature, density, entropy, and pressure maps. The dynamical mass estimate is 80% of the hydrostatic mass estimate at r H.E. 500 . It can be partially explained by the ∼20% scatter in the 2D pressure map that can be propagated into the hydrostatic mass estimate. The uncertainty in the dynamical mass estimate caused by the substructure of the high velocity group is ∼14%. The dynamical mass estimate using blue members is 1.23 times that obtained using red members. The global properties of R1504 obey the observed scaling relations of nearby clusters, although its stellar-mass fraction is rather low.

show abstract

Section: Temperature and Surface Brightness Distributionsmentioning

confidence: 99%

Probing cluster dynamics in RXC J1504.1-0248 via radial and two-dimensional gas and galaxy properties

Zhang

Verdugo

Klein

et al. 2012

A&A

View full text Add to dashboard Cite

show abstract

“…In this paper we are using our new high-sensitivity southern 21-cm line survey (see Arnal et al 2000), combined with the Leiden/Dwingeloo Survey of Galactic Neutral Hydrogen (Hartmann & Burton 1997). The resulting grid has a spacing (Δl, Δb) = (0.50 • , 0.50 • ).…”

Section: H I Observations: High-sensitivity All-sky Surveymentioning

confidence: 99%

The interstellar medium surrounding the Scorpius-Centaurus association revisited

Pöppel¹,

Bajaja²,

Arnal

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We want to make a large-scale study of the morphology, kinematics, and origin of the H I, which surrounds the Sco-Cen association. Methods. We combine our high-sensitivity southern H I survey with the Leiden/Dwingeloo Survey, considering l = 240 • −400 • , b = −60 • to +60 • , and radial velocities of V = −41.8 to +40.8 km s −1 . We point out the main H I branches surrounding the association and derive their kinematics. Kinematical H I-maps were compared with spatial maps of interstellar (IS) Na I from the literature. Upper limits for distances d were derived from optical IS absorption components from the literature. Models of expanding spherical H I shells were fitted around each stellar subgroup. Results. The expanding ring of H I associated with the Gould Belt (GB) is very prominent. At each l, its radial velocity shifts ∼−7 km s −1 within an interval Δb ∼ 10 • −25 • . On the sky, the shifts occur within a narrow stripe extending between l, b ∼ 250 • , −18 • and 400 • , +50 • . The ranges of distances and radial thicknesses of most H I branches are nearly 70−160 pc and 40−90 pc, respectively. The shell-models fit the main branches. Interactions between the shells built a large expanding bubble with a transverse diameter of nearly 250 pc around the association. The near face is approaching with a mean velocityV ∼ −6.6 km s −1 at d ≤ 76 pc from the Sun, covering about 102 • × 65 • (l, b), forming an "H I-wall". There are streamers atV ∼ −15 to −35 km s −1 , as well as gas presumably overshot into Galactic Quadrant II. The receding gas is more tenuous. Conclusions. The association is traversing the ring since a time comparable to its age producing a significant disturbance on the expanding GB-ring of gas. The latter was almost totally shocked by the association, northerly of the stripe of velocity shifts. Southerly there are large amounts of preshocked gas, as well as smaller more localized shocked regions. Hot gas within the bubble produces most of the 1/4 keV radiation detected toward it by ROSAT. The total mass of the GB gas embedding the Sco-Cen association is estimated at M t ∼ 368 000 M ± 60%, including ∼34 000 M of associated H 2 and 30% of He. About 39% of the embedding gas was shocked by the association. At | b |≥ 35 • , a comparison of the observations with test points moving on ballistic orbits is consistent with the formation of the Sco-Cen association within the gas ring of the GB and the presumable explosive origin of the latter. The rotation of the ring is assumed.

show abstract

“…• , and the Instituto Argentino de Radioastronomía Survey (IAR: Arnal et al 2000;Bajaja et al 2005) at more southern declinations. The combined material has a velocity resolution of 1.3 km s −1 , a spatial resolution of 36 on a grid spacing of 0.…”

Section: Brief Description Of Leiden-argentine-bonn (Lab) Datamentioning

confidence: 99%

The Origin of the Magellanic Stream and its Leading Arm

Nidever

Majewski

Burton

2008

Astrophysics and Space Science Proceedings

View full text Add to dashboard Cite

We explore the Magellanic Stream (MS) using a Gaussian decomposition of the H I velocity profiles in the Leiden-Argentine-Bonn (LAB) all-sky H I survey. This decomposition exposes the MS to be composed of two filaments distinct both spatially (as first pointed out by Putman et al.) and in velocity. Using the velocity coherence of the filaments, one can be traced back to its origin in what we identify as the SouthEast H I Overdensity (SEHO) of the Large Magellanic Cloud (LMC), which includes 30 Doradus. Parts of the Leading Arm (LA) can also be traced back to the SEHO in velocity and position. Therefore, at least one-half of the trailing Stream and most of the LA originates in the LMC, contrary to previous assertions that both the MS and the LA originate in the Small Magellanic Cloud (SMC) and/or in the Magellanic Bridge. The two MS filaments show strong periodic, undulating spatial and velocity patterns that we speculate are an imprint of the LMC rotation curve. If true, then the drift rate of the Stream gas away from the Magellanic Clouds is ∼49 km s −1 and the age of the MS is ∼1.74 Gyr. The Staveley-Smith et al. high-resolution H I data of the LMC show gas outflows from supergiant shells in the SEHO that seem to be creating the LA and LMC filament of the MS. Blowout of LMC gas is an effect not previously accounted for but one that probably plays an important role in creating the MS and LA.

show abstract

A high sensitivity Hi survey of the sky at δ ≤ -25°

Cited by 92 publications

References 5 publications

Probing cluster dynamics in RXC J1504.1-0248 via radial and two-dimensional gas and galaxy properties

Probing cluster dynamics in RXC J1504.1-0248 via radial and two-dimensional gas and galaxy properties

The interstellar medium surrounding the Scorpius-Centaurus association revisited

The Origin of the Magellanic Stream and its Leading Arm

Contact Info

Product

Resources

About