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

Open Access

Issue		A&A Volume 501, Number 1, July I 2009


Page(s)		157 - 169
Section		Extragalactic astronomy
DOI		https://doi.org/10.1051/0004-6361/200810978
Published online		29 April 2009

Online Material

Table 3: Spectral fitting results of the projected annular spectra.

Table 4: Spectral fitting results of the deprojected annular spectra.

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Figure 18:

( Left) The ISM temperature profiles of sample galaxies. The cross data points represent temperature profile derived from projected spectra, and the diamond data points are from deprojected spectra. The solid lines represent each best-fit function. ( Center) The ISM density profiles. The diamond data points represent XMM-Newton data, and the cross data points are Chandra data obtained from spatial analysis. The solid lines represent each best-fit function. The black data points are used to fit the function, but the gray data points are not. The dot-dashed lines show best-fit function of the ISM density profile obtained from the spectral fit. These ISM density profiles are normalized by the value at $1~r_{\rm e}$ . ( Right) The integrated mass profiles. The solid and dot-dashed lines are total mass obtained from ISM density profiles from the surface brightness and spectral fit, respectively. The dashed lines are upper and lower limit. We also plotted the stellar mass profiles assuming stellar M/L_B to be 3 and 8 (dotted lines).

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$\begin{figure}\par\includegraphics[width=18cm]{0978fA1k.eps}\\ \includegraphic... ...]{0978fA1n.eps}\\ \includegraphics[width=18cm]{0978fA1o.eps}\\ \end{figure}$	Figure 18: continued.
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$\begin{figure}\par\includegraphics[width=18cm]{0978fA1p.eps}\\ \includegraphic... ...]{0978fA1s.eps}\\ \includegraphics[width=18cm]{0978fA1t.eps}\\ \end{figure}$	Figure 18: continued.
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$\begin{figure}\par\includegraphics[width=18cm]{0978fA1u.eps}\\ \includegraphics[width=18cm]{0978fA1v.eps}\\ \end{figure}$	Figure 18: continued.
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