Extragalactic large-scale structures  behind the southern Milky Way

Woudt, P. A.; Kraan-Korteweg, R. C.; Cayatte, V.; Balkowski, C.; Felenbok, P.

doi:10.1051/0004-6361:20034600

Cited by 31 publications

(53 citation statements)

References 27 publications

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“…As the Norma cluster has also been proposed as the possible center of a "Great Attractor" region (Woudt et al 2003, Kolatt et al 1995, this large angular separation supports the idea that the SBF-GA and the ZOA-GA might be different substructures within a generally overdense region of the universe.…”

Section: The Great Attractor Acting Upon Hydra and Centaurussupporting

confidence: 63%

The distance to Hydra and Centaurus from surface brightness fluctuations: Consequences for the Great Attractor model

Mieske¹,

Hilker²,

Infante³

2005

A&A

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Abstract. We present I-band Surface Brightness Fluctuation (SBF) measurements for 16 early-type galaxies (3 giants, 13 dwarfs) in the central region of the Hydra cluster, based on deep photometric data in 7 fields obtained with VLT FORS1. From the SBF-distances to the galaxies in our sample we estimate the distance of the Hydra cluster to be 41. for the Cen30 component of Centaurus. Allowing for a thermal velocity dispersion of 200 km s −1 , this rules out a common peculiar flow velocity for both clusters at 98% confidence. We find that the 9× 10 15 M "Great Attractor" at a distance of 45 Mpc can explain the observed peculiar velocities if shifted about 15• towards the Hydra cluster position. Our results are inconsistent at 94% confidence with a scenario where the Centaurus cluster is identical to the GA. In order to better restrict partially degenerate Great Attractor parameters like its mass and distance, a recalculation of the local flow model with updated distance information over a larger area than covered by us would be needed.

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Section: The Great Attractor Acting Upon Hydra and Centaurussupporting

confidence: 63%

The distance to Hydra and Centaurus from surface brightness fluctuations: Consequences for the Great Attractor model

Mieske¹,

Hilker²,

Infante³

2005

A&A

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“…It is distinct from the much flatter distribution of the H i-survey undertaken under the same observing conditions for the Hydra/Antlia survey area (top panel of inset; as in Paper I). This is in agreement with the results by Woudt et al (2004) who have shown that the velocity distribution of all survey galaxies for which we obtained redshifts (about 15% on average for the deep ZOA surveys, mostly optical spectra from our dedicated follow-up surveys at the SAAO and ESO, plus some previously published redshifts), is fairly flat out to 20 000 km s −1 in the Hydra/Antlia region, while the Crux region and -much more pronounced -the GA region show a distinct broad peak of galaxies at ∼4000−5000 km s −1 (see their Fig. 5), while the histogram is otherwise similar for the three survey regions.…”

Section: Velocity Distribution and Detection Ratesupporting

confidence: 94%

“…The extent and shape of this wall was suspected in earlier papers (e.g., Kraan-Korteweg et al 1994) and strongly supported in more recent work (Woudt et al 2004;Kraan-Korteweg 2005;Ebeling et al 2005;Radburn-Smith et al 2006). A sketch of this Wall, as well as the Centaurus filament, is given with Fig.…”

Section: Sky Projectionssupporting

confidence: 68%

“…This emphasises that H i-observations, even when dependent on optical (or NIR) pre-identification, are tremendously powerful in mapping LSS of highly obscured galaxies in and across the ZOA. Note that optical redshifts for these survey regions have been obtained earlier with the SAAO 1.9 m telescope Woudt et al 1999), as well as with multi-object spectroscopy using the 3.6 m telescope of ESO in Chile (Woudt et al 2004). In the second panel (2000-4000) the Centaurus Wall (CenW) is the dominant feature (Fairall 1998;Fairall et al 1998).…”

Section: Large-scale Structure In the Crux And Ga Regionsmentioning

confidence: 58%

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Parkes H I observations of galaxies behind the southern Milky Way

Schroeder

Kraan-Korteweg

Henning

2009

A&A

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As part of our programme to map the large-scale distribution of galaxies behind the southern Milky Way, we observed 314 opticallyselected, partially-obscured galaxies in the Zone of Avoidance (ZOA) in the Crux and Great Attractor (GA) regions. An additional 29 galaxies were observed in the Vela ZOA survey region (because of the small numbers they are not discussed any further). The observations were conducted with the Parkes 64 m (210 ft) radio telescope, in a single-pixel pointed mode, reaching an rms noise level of typically 2−6 mJy over the velocity search range of 400 < v < 10 500 km s −1 . A total of 162 galaxies were detected (plus 14 galaxies in the Vela region). The detection rate is slightly higher than for the Hydra/Antlia region (52% versus 45%) observed in the same way. This can be explained by the prominence of the GA overdensity in the survey regions, which leads to a relatively higher fraction of nearby galaxies. It is also evident from the quite narrow velocity distribution (largely confined to 3000−6000 km s −1 ) and deviates significantly from the expectation of a uniform galaxy distribution for the given sensitivity and velocity range. No systematic differences were found between detections and non-detections, in terms of latitude, foreground extinction, or environment, except for the very central part of the rich Norma cluster, where hardly any galaxies were detected. A detailed investigation of the H i content of the galaxies reveals strong H i deficiency at the core of the Norma cluster (within about a 0.4 Abell radius), similar to what has been found in the Coma cluster. The redshifts obtained by this observing technique result in a substantial reduction of the so-called redshift ZOA. This is obvious when analysing the large-scale structure of the new H i data in combination with data from other (optical) ZOA redshift surveys. The lower latitude detections provide further evidence of the extension of the Norma Wall, across the ZOA, in particular its bending towards the Cen-Crux clusters above the Galactic plane at slightly higher redshift, rather than a straight continuation towards the Centaurus clusters.

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“…It is also the sixth brightest cluster in ROSAT All-Sky Survey and the second brightest non-cool-core cluster after Coma (Böhringer et al 1996). ESO 137-001 is a blue emission-line galaxy (Woudt et al 2004) that is only ∼180 kpc from the cluster's X-ray peak in projection. Its radial velocity (4680 ± 71 km s −1 ; Woudt et al 2004) is close to the average velocity in A3627 (4871 ± 54 km s −1 ; Woudt et al 2008), so most of its motion is probably in the plane of sky.…”

Section: No 2 2010 Spectacular X-ray Tails Intracluster Star Formamentioning

confidence: 99%

SPECTACULAR X-RAY TAILS, INTRACLUSTER STAR FORMATION, AND ULXs IN A3627

Sun

Donahue

Röediger

et al. 2009

ApJ

175

270

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We present the discovery of spectacular double X-ray tails associated with ESO 137-001 and a possibly heated X-ray tail associated with ESO 137-002, both late-type galaxies in the closest rich cluster Abell 3627. A deep Chandra observation of ESO 137-001 allows us for the first time to examine the spatial and spectral properties of such X-ray tails in detail. Besides the known bright tail that extends to ∼80 kpc from ESO 137-001, a fainter and narrower secondary tail with a similar length was surprisingly revealed, as well as some intriguing substructures in the main tail. There is little temperature variation along both tails. The widths of the secondary tail and the greater part of the main tail also remain nearly constant with the distance from the galaxy. All these results challenge the current simulations. The Chandra data also reveal 19 X-ray point sources around the X-ray tails. We identified six X-ray point sources as candidates of intracluster ultra-luminous X-ray sources with L 0.3-10 keV of up to 2.5 × 10 40 erg s −1 . Gemini spectra of intracluster H ii regions downstream of ESO 137-001 are also presented, as well as the velocity map of these H ii regions that shows the imprint of ESO 137-001's disk rotation. For the first time, we unambiguously know that active star formation can happen in the cold interstellar medium (ISM) stripped by intracluster medium (ICM) ram pressure, and it may contribute a significant amount of the intracluster light. We also report the discovery of a 40 kpc X-ray tail of another late-type galaxy in A3627, ESO 137-002. Its X-ray tail seems hot, ∼2 keV (compared to ∼0.8 keV for ESO 137-001's tails). The Hα data for ESO 137-002 are also presented. We conclude that the high-pressure environment around these two galaxies is important for their bright X-ray tails and the intracluster star formation. The soft X-ray tails can reveal a great deal of the thermal history of the stripped cold ISM in mixing with the hot ICM, which is discussed along with intracluster star formation.

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Extragalactic large-scale structures behind the southern Milky Way

Cited by 31 publications

References 27 publications

The distance to Hydra and Centaurus from surface brightness fluctuations: Consequences for the Great Attractor model

The distance to Hydra and Centaurus from surface brightness fluctuations: Consequences for the Great Attractor model

Parkes H I observations of galaxies behind the southern Milky Way

SPECTACULAR X-RAY TAILS, INTRACLUSTER STAR FORMATION, AND ULXs IN A3627

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