High‐Resolution Observations of the Elliptical Galaxy NGC 4636 with the Reflection Grating Spectrometer on Board<i>XMM‐Newton</i>

Xu, Haiguang; Kahn, S. M.; Peterson, J. R.; Behar, E.; Paerels, F.; Mushotzky, R. F.; Jernigan, J. G.; Brinkman, A. C.; Makishima, Kazuo

doi:10.1086/342828

Cited by 196 publications

(216 citation statements)

References 38 publications

Supporting

Mentioning

185

Contrasting

Order By: Relevance

“…In contrast, galaxies with ISM luminosities much larger than L σ show largely extended emission with a radius of a few tens of r e with positive temperature gradients. XMM-Newton RGS observations provided evidence of a weak positive temperature gradient in the inner region of the ISM in NGC 4636, which has a much higher ISM luminosity than L σ (Xu et al 2002). The correlation between the temperature gradient and spatial distribution was confirmed with Chandra observations (Fukazawa et al 2006).…”

Section: Introductionmentioning

confidence: 64%

Gravitational potential and X-ray luminosities of early-type galaxies observed with XMM-Newton and Chandra

Nagino¹,

Matsushita²

2009

A&A

View full text Add to dashboard Cite

Aims. We study the dark matter content in early-type galaxies and investigate whether X-ray luminosities of early-type galaxies are determined by the surrounding gravitational potential. Methods. We derived gravitational mass profiles of 22 early-type galaxies observed with XMM-Newton and Chandra. Results. Sixteen galaxies show constant or decreasing radial temperature profiles, and their X-ray luminosities are consistent with kinematical energy input from stellar mass loss. The temperature profiles of the other 6 galaxies increase with radius, and their X-ray luminosities are significantly higher. The integrated mass-to-light ratio of each galaxy is constant at that of stars within 0.5-1 r e , and increases with radius, where r e is the effective radius of a galaxy. The scatter of the central mass-to-light ratio of galaxies was less in K-band light. At 3 r e , the integrated mass-to-light ratios of galaxies with flat or decreasing temperature profiles are twice the value at 0.5 r e , where the stellar mass dominates, and at 6 r e , these increase to three times the value at 0.5 r e . Conclusions. This feature should reflect common dark and stellar mass distributions in early-type galaxies: within 3 r e , the mass of dark matter is similar to the stellar mass, while within 6 r e , the former is larger than the latter by a factor of two. In contrast, X-ray luminous galaxies have higher gravitational mass in the outer regions than X-ray faint galaxies. We describe these X-ray luminous galaxies as the central objects of large potential structures; the presence or absence of this potential is the main source of the large scatter in the X-ray luminosity.

show abstract

Section: Introductionmentioning

confidence: 64%

Gravitational potential and X-ray luminosities of early-type galaxies observed with XMM-Newton and Chandra

Nagino¹,

Matsushita²

2009

A&A

View full text Add to dashboard Cite

show abstract

“…XMM-Newton RGS observations of the hot gas in clusters of galaxies and in elliptical galaxies reveal Ne/O ratios which are higher than Solar (Xu et al 2002;Peterson et al 2003;Werner et al 2006aWerner et al , 2006b. SN Ia produce very little O and Ne, and their ratio can be used to put constraints on the progenitors of SN CC .…”

Section: Summary Of the Efforts Of Using Icm Abundances To Constrain mentioning

confidence: 94%

Observations of Metals in the Intra-Cluster Medium

et al. 2008

View full text Add to dashboard Cite

Because of their deep gravitational potential wells, clusters of galaxies retain all the metals produced by the stellar populations of the member galaxies. Most of these metals reside in the hot plasma which dominates the baryon content of clusters. This makes them excellent laboratories for the study of the nucleosynthesis and chemical enrichment history of the Universe. Here we review the history, current possibilities and limitations of the abundance studies, and the present observational status of X-ray measurements of the chemical composition of the intra-cluster medium. We summarise the latest progress in using the abundance patterns in clusters to put constraints on theoretical models of supernovae and we show how cluster abundances provide new insights into the star-formation history of the Universe.

show abstract

“…The problem with the cooling scenario is that the observed lines at ∼10 6 K strongly constrain the amount of metals that can cool (e.g. Peterson et al 2003;Xu et al 2002). However, warm ISM is observed in ellipticals and its metallicity is nearly solar (e.g.…”

Section: Introductionmentioning

confidence: 99%

Abundance ratios in the hot ISM of elliptical galaxies

Pipino

Matteuccí

2011

A&A

View full text Add to dashboard Cite

Aims. We constrain possible explanations of the theoretical Fe discrepancy in the hot interstellar medium of elliptical galaxies and simultaneously explain the [α/Fe] ratios. Methods. We use the latest theoretical nucleosynthetic yields, incorporate dust, and explore different SNIa progenitor scenarios by means of a self-consistent chemical evolution model that reproduces the stellar populations properties of elliptical galaxies. Results. Models with Fe-only dust and/or a lower effective SNIa rate achieve a closer agreement with the observed Fe abundance. However, a suitable modification of the SNIa yields relative to the standard W7 model is needed to fully describe the abundance ratio pattern. The 2D explosion model C-DDT by Maeda and collaborator may be capable of reproducing the [Fe/H] and the [α/Fe] ratios.

show abstract

High‐Resolution Observations of the Elliptical Galaxy NGC 4636 with the Reflection Grating Spectrometer on BoardXMM‐Newton

Cited by 196 publications

References 38 publications

Gravitational potential and X-ray luminosities of early-type galaxies observed with XMM-Newton and Chandra

Gravitational potential and X-ray luminosities of early-type galaxies observed with XMM-Newton and Chandra

Observations of Metals in the Intra-Cluster Medium

Abundance ratios in the hot ISM of elliptical galaxies

Contact Info

Product

Resources

About