Soft X-ray band emission from solids

Fabian, D.J.

doi:10.1080/10408437108243430

Cited by 20 publications

(25 citation statements)

References 72 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For a number of years upper limits on the AGN contribution to the 2-10 keV XRB have been determined based on the different spectral shapes of AGN and the XRB (e.g. Fabian, Canizares & Barcons 1989). Almost all investigations have extrapolated AGN spectra measured at soft X-ray energies (<3.5 keV) to the 2-10 keV band.…”

Section: Discussionmentioning

confidence: 99%

“…Almost all investigations have extrapolated AGN spectra measured at soft X-ray energies (<3.5 keV) to the 2-10 keV band. Many AGN appear to have extremely soft X-ray spectra at low energy, possibly due to the presence of a separate soft excess component, and this has lead to very low estimates of the AGN contribution to the 2-10 keV XRB (e.g., <13 per cent for a ¼ 1:4; Fabian et al 1989).…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

The hard X-ray spectrum of soft X-ray-selected AGN

Page¹

1998

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

I use ASCA data to investigate the 2–10 keV X‐ray emission of active galactic nuclei (AGN) taken from the ROSAT International X‐ray Optical Survey (RIXOS). I find that the integrated spectrum of these faint, soft X‐ray‐selected AGN in the 2–10 keV band is harder (best‐fitting α = 0.8 ± 0.1) than the slope measured with ROSAT between 0.1 and 2 keV, but softer than the 2–10 keV X‐ray background, and consistent with the average 2–10 keV spectrum of bright, nearby Seyfert galaxies. With this spectral slope and using measurements of the AGN contribution to the 1–2 keV X‐ray background, I estimate that the AGN percentage contribution to the 2–10 keV background is 0.60 +0.19−0.14 times the AGN percentage contribution to the 1–2 keV background. Hence AGN produce between 12 and 32 per cent of the 2–10 keV X‐ray background. This is only the contribution from the types of AGN which are found in soft X‐ray surveys; a population of absorbed AGN could represent an additional component of the 2–10 keV X‐ray background.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

The hard X-ray spectrum of soft X-ray-selected AGN

Page¹

1998

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…In this case, the initial metallicity of the intracluster gas should be anti-correlated with L X (see also David et al 1990). Even though some subsequent contamination due to galactic winds from the surviving protogalaxies must certainly have occurred (e.g., Matteucci & Gibson 1995), such an anti-correlation does appear to exist (Fabian et al 1994). Thus, this scenario would allow IGCs to resolve at least some aspects of the high-S N problem if we allow S IGC N to increase with cluster mass.…”

Section: Intergalactic Globular Clustersmentioning

confidence: 99%

M87, Globular Clusters, and Galactic Winds: Issues in Giant Galaxy Formation

Harris¹,

Harris²,

McLaughlin³

1998

The Astronomical Journal

103

141

View full text Add to dashboard Cite

“…The existence of an intrinsic spread or dispersion in the galaxy cluster X-ray luminosity-temperature (L-T) relationship has been noted by several authors (Edge & Stewart 1991, Fabian et al 1994, Mushotzky & Scharf 1997. Fabian et al (1994) demonstrated a correlation between the amplitude of the L-T relationship and the cooling flow mass deposition rateṀ(M ⊙ yr −1 ) (L ∝ T 3.3Ṁ 0.4 ).…”

Section: Introductionmentioning

confidence: 93%

“…This variation also does not evolve with redshift (Mushotzky & Loewenstein 1997). As Fabian et al (1994) have pointed out, it is likely that temperatures, iron abundances and cooling flows are all linked consequences of cluster histories.…”

Section: Introductionmentioning

confidence: 99%

The Galaxy Cluster Luminosity-Temperature Relationship and Iron Abundances: A Measure of Formation History?

Scharf

Mushotzky

1997

The Astrophysical Journal

View full text Add to dashboard Cite

Both the X-ray luminosity-temperature (L-T) relationship and the iron abundance distribution of galaxy clusters show intrinsic dispersion. Using a large set of galaxy clusters with measured iron abundances, we find a correlation between abundance and the relative deviation of a cluster from the mean L-T relationship. We argue that these observations can be explained by taking into account the range of cluster formation epochs expected in a hierarchical universe. The known relationship of cooling flow mass deposition rate to luminosity and temperature is also consistent with this explanation. From the observed cluster population, we estimate that the oldest clusters formed at z ? 2.We propose that the iron abundance of a galaxy cluster can provide a parameterization of its age and dynamical history.

show abstract

Soft X-ray band emission from solids

Cited by 20 publications

References 72 publications

The hard X-ray spectrum of soft X-ray-selected AGN

The hard X-ray spectrum of soft X-ray-selected AGN

M87, Globular Clusters, and Galactic Winds: Issues in Giant Galaxy Formation

The Galaxy Cluster Luminosity-Temperature Relationship and Iron Abundances: A Measure of Formation History?

Contact Info

Product

Resources

About