Search for X-ray emission from the Shapley supercluster and the WHIM with Suzaku

Ikuyuki Mitsuishi, Anjali Gupta, Noriko Y. Yamasaki, Yoh Takei, Takaya Ohashi, Kosuke Sato, Massimiliano Galeazzi, J. Patrick Henry, Richard L. Kelley

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Abstract

Suzaku performed observations of 3 regions in and around the Shapley supercluster: a region located between A3558 and A3556, at ∼0.9 times the virial radii of both clusters, and two other regions at 1° and 4°away from the first pointing. The 4°-offset observation was used to evaluate the Galactic foreground emission. We did not detect significant redshifted Oxygen emission lines (O VII and OV III) in the spectra of all three pointings, after subtracting the contribution of foreground and background emission. An upper limit for the redshifted OV III Kα line intensity of the warm-hot intergalactic medium (WHIM) is 1.5×10 -7 photons s -1 cm -2 arcmin -2, which corresponds to an overdensity of ∼380 (Z/0.1Z ) -1/2(L/3Mpc) -1/2, assuming T=3×10 6 K. We found excess continuum emission in the 1°-offset and on-filament regions, represented by thermal models with kT ∼1 keV and ∼2 keV, respectively. The redshifts of both 0 and that of the supercluster (0.048) are consistent with the observed spectra. The ∼1 keV emission can be also fitted with Ne-rich Galactic (zero redshift) thin thermal emission. Radial intensity profile of 2 keV component suggests contribution from nearby clusters A3558 and A3556, but with significant steepening of the intensity slope in the outer region of A3558.

Original languageEnglish (US)
Title of host publicationAIP Conference Proceedings
Pages344-345
Number of pages2
Volume1427
DOIs
StatePublished - 2012
EventSuzaku 2011: Exploring the X-Ray Universe: Suzaku and Beyond - Palo Alto, CA, United States
Duration: Jul 20 2011Jul 22 2011

Other

OtherSuzaku 2011: Exploring the X-Ray Universe: Suzaku and Beyond
CountryUnited States
CityPalo Alto, CA
Period7/20/117/22/11

Fingerprint

intergalactic media
x rays
K lines
thermal emission
filaments
slopes
continuums
radii
photons
oxygen
profiles

Keywords

  • cluster
  • supercluster
  • WHIM
  • X-ray

ASJC Scopus subject areas

  • Physics and Astronomy(all)

Cite this

Mitsuishi, I., Gupta, A., Yamasaki, N. Y., Takei, Y., Ohashi, T., Sato, K., ... Kelley, R. L. (2012). Search for X-ray emission from the Shapley supercluster and the WHIM with Suzaku. In AIP Conference Proceedings (Vol. 1427, pp. 344-345) https://doi.org/10.1063/1.3696235

Search for X-ray emission from the Shapley supercluster and the WHIM with Suzaku. / Mitsuishi, Ikuyuki; Gupta, Anjali; Yamasaki, Noriko Y.; Takei, Yoh; Ohashi, Takaya; Sato, Kosuke; Galeazzi, Massimiliano; Henry, J. Patrick; Kelley, Richard L.

AIP Conference Proceedings. Vol. 1427 2012. p. 344-345.

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Mitsuishi, I, Gupta, A, Yamasaki, NY, Takei, Y, Ohashi, T, Sato, K, Galeazzi, M, Henry, JP & Kelley, RL 2012, Search for X-ray emission from the Shapley supercluster and the WHIM with Suzaku. in AIP Conference Proceedings. vol. 1427, pp. 344-345, Suzaku 2011: Exploring the X-Ray Universe: Suzaku and Beyond, Palo Alto, CA, United States, 7/20/11. https://doi.org/10.1063/1.3696235
Mitsuishi I, Gupta A, Yamasaki NY, Takei Y, Ohashi T, Sato K et al. Search for X-ray emission from the Shapley supercluster and the WHIM with Suzaku. In AIP Conference Proceedings. Vol. 1427. 2012. p. 344-345 https://doi.org/10.1063/1.3696235
Mitsuishi, Ikuyuki ; Gupta, Anjali ; Yamasaki, Noriko Y. ; Takei, Yoh ; Ohashi, Takaya ; Sato, Kosuke ; Galeazzi, Massimiliano ; Henry, J. Patrick ; Kelley, Richard L. / Search for X-ray emission from the Shapley supercluster and the WHIM with Suzaku. AIP Conference Proceedings. Vol. 1427 2012. pp. 344-345
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AU - Takei, Yoh

AU - Ohashi, Takaya

AU - Sato, Kosuke

AU - Galeazzi, Massimiliano

AU - Henry, J. Patrick

AU - Kelley, Richard L.

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N2 - Suzaku performed observations of 3 regions in and around the Shapley supercluster: a region located between A3558 and A3556, at ∼0.9 times the virial radii of both clusters, and two other regions at 1° and 4°away from the first pointing. The 4°-offset observation was used to evaluate the Galactic foreground emission. We did not detect significant redshifted Oxygen emission lines (O VII and OV III) in the spectra of all three pointings, after subtracting the contribution of foreground and background emission. An upper limit for the redshifted OV III Kα line intensity of the warm-hot intergalactic medium (WHIM) is 1.5×10 -7 photons s -1 cm -2 arcmin -2, which corresponds to an overdensity of ∼380 (Z/0.1Z ⊙) -1/2(L/3Mpc) -1/2, assuming T=3×10 6 K. We found excess continuum emission in the 1°-offset and on-filament regions, represented by thermal models with kT ∼1 keV and ∼2 keV, respectively. The redshifts of both 0 and that of the supercluster (0.048) are consistent with the observed spectra. The ∼1 keV emission can be also fitted with Ne-rich Galactic (zero redshift) thin thermal emission. Radial intensity profile of 2 keV component suggests contribution from nearby clusters A3558 and A3556, but with significant steepening of the intensity slope in the outer region of A3558.

AB - Suzaku performed observations of 3 regions in and around the Shapley supercluster: a region located between A3558 and A3556, at ∼0.9 times the virial radii of both clusters, and two other regions at 1° and 4°away from the first pointing. The 4°-offset observation was used to evaluate the Galactic foreground emission. We did not detect significant redshifted Oxygen emission lines (O VII and OV III) in the spectra of all three pointings, after subtracting the contribution of foreground and background emission. An upper limit for the redshifted OV III Kα line intensity of the warm-hot intergalactic medium (WHIM) is 1.5×10 -7 photons s -1 cm -2 arcmin -2, which corresponds to an overdensity of ∼380 (Z/0.1Z ⊙) -1/2(L/3Mpc) -1/2, assuming T=3×10 6 K. We found excess continuum emission in the 1°-offset and on-filament regions, represented by thermal models with kT ∼1 keV and ∼2 keV, respectively. The redshifts of both 0 and that of the supercluster (0.048) are consistent with the observed spectra. The ∼1 keV emission can be also fitted with Ne-rich Galactic (zero redshift) thin thermal emission. Radial intensity profile of 2 keV component suggests contribution from nearby clusters A3558 and A3556, but with significant steepening of the intensity slope in the outer region of A3558.

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