P. E.J. Nulsen
The narrow X-ray tail and double Hα tails of ESO 137-002 in A3627
Nulsen, P. E.J.; Zhang, B.; Sun, M.; Ji, L.; Sarazin, C.; Lin, X. B.; Nulsen, P. E. J.; Roediger, E.; Donahue, M.; Forman, W.; Jones, C.; Voit, G. M.; Kong, X.
X. B. Lin
P. E. J. Nulsen
Dr Elke Roediger E.Roediger@hull.ac.uk
Senior Lecturer/ Director of Studies for Physics
G. M. Voit
We present the analysis of a deep Chandra observation of a ~2 L * late-type galaxy, ESO 137-002, in the closest rich cluster A3627. The Chandra data reveal a long (gsim40 kpc) and narrow tail with a nearly constant width (~3 kpc) to the southeast of the galaxy, and a leading edge ~1.5 kpc from the galaxy center on the upstream side of the tail. The tail is most likely caused by the nearly edge-on stripping of ESO 137-002's interstellar medium (ISM) by ram pressure, compared to the nearly face-on stripping of ESO 137-001 discussed in our previous work. Spectral analysis of individual regions along the tail shows that the gas throughout it has a rather constant temperature, ~1 keV, very close to the temperature of the tails of ESO 137-001, if the same atomic database is used. The derived gas abundance is low (~0.2 solar with the single-kT model), an indication of the multiphase nature of the gas in the tail. The mass of the X-ray tail is only a small fraction (<5%) of the initial ISM mass of the galaxy, suggesting that the stripping is most likely at an early stage. However, with any of the single-kT, double-kT, and multi-kT models we tried, the tail is always "over-pressured" relative to the surrounding intracluster medium (ICM), which could be due to the uncertainties in the abundance, thermal versus non-thermal X-ray emission, or magnetic support in the ICM. The Hα data from the Southern Observatory for Astrophysical Research show a ~21 kpc tail spatially coincident with the X-ray tail, as well as a secondary tail (~12 kpc long) to the east of the main tail diverging at an angle of ~23° and starting at a distance of ~7.5 kpc from the nucleus. At the position of the secondary Hα tail, the X-ray emission is also enhanced at the ~2σ level. We compare the tails of ESO 137-001 and ESO 137-002, and also compare the tails to simulations. Both the similarities and differences of the tails pose challenges to the simulations. Several implications are briefly discussed.
|Journal Article Type||Article|
|Publication Date||Nov 10, 2013|
|Publisher||American Astronomical Society|
|Peer Reviewed||Peer Reviewed|
|APA6 Citation||Zhang, B., Sun, M., Ji, L., Sarazin, C., Lin, X. B., Nulsen, P. E. J., …Kong, X. (2013). The narrow X-ray tail and double Hα tails of ESO 137-002 in A3627. The Astrophysical journal, 777(2), doi:10.1088/0004-637x/777/2/122|
|Copyright Statement||© 2016. The American Astronomical Society. All rights reserved.|
|Additional Information||This is a copy of an article published in the Astrophysical journal, 2013, v.777 issue 2.|
© 2016. The American Astronomical Society. All rights reserved.
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