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

Nagino, Ryo; Matsushita, Kyoko

doi:10.1051/0004-6361/200810978

Cited by 74 publications

(93 citation statements)

References 41 publications

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“…More specifically, we find that inside r e the stellar component accounts for < ∼ 70% of the gravitating mass. This result is not new (see, e.g., Kronawitter et al 2000;Nagino & Matsushita 2009, where 22 objects with XMM-Newton and Chandra X-ray luminosities are mass-modeled). However, our finding is at odds with the claim of substantial proportions of DM inside r e (Humphrey et al 2006) and with the idea that the well known tilt of the fundamental plane of ellipticals is due to systematic variations of the DM fraction inside r e with galaxy properties.…”

Section: Discussionmentioning

confidence: 91%

Dark matter halos around isolated ellipticals

Memola

Salucci

Babić

2011

A&A

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Aims. We investigate the distribution of the luminous and the dark matter components in the isolated ellipticals NGC 7052 and NGC 7785, which are embedded in an emitting hot gas halo, by means of relevant X-ray and photometric data. Methods. To calculate the dark matter distribution in these rare objects, we performed an improved X-ray analysis of the XMM-Newton data of NGC 7785, and we used former results based on Chandra data of NGC 7052. For each object we also derived the stellar spheroid length scale from the surface photometry and the spheroid stellar mass from an analysis of the galaxy spectral energy distribution. Results. We find that a dark matter component is present in these objects. It is subdominant and mixed with the luminous matter inside the optical region half-light radius wide, while it dominates the gravitational potential at outer radii. On the whole, the dark halo structure is very similar to that found around spirals of comparable luminosity and it is well reproduced by a Burkert halo, while a Sérsic spheroid accounts well for the baryonic component.

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Section: Discussionmentioning

confidence: 91%

Dark matter halos around isolated ellipticals

Memola

Salucci

Babić

2011

A&A

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“…This model has properties consistent with observed massive early-type (and even shell) galaxies (Auger et al 2010;Nagino & Matsushita 2009;Fukazawa et al 2006). The potential of the cannibalized galaxy is chosen to be a single Plummer sphere with the total mass M = 2 × 10 10 M and Plummer radius b * = 2 kpc.…”

Section: Parameters Of the Simulationmentioning

confidence: 92%

“…Several methods have been used to measure the gravitational potentials and their gradients of elliptical galaxies, including strong and weak gravitational lensing (e.g., Gavazzi et al 2007;Mandelbaum et al 2008;Auger et al 2010), X-ray observations of hot gas in the massive gas-rich galaxies (e.g., Fukazawa et al 2006;Nagino & Matsushita 2009;Churazov et al 2008;Das et al 2010), rotation curves of detected disks and rings of neutral hydrogen (e.g., Weijmans et al 2008), stellar-dynamical modeling from integrated light spectra (e.g., Weijmans et al 2009;de Lorenzi et al 2009;Churazov et al 2010;Thomas et al 2011), and the use of tracers such as planetary nebulae, globular clusters, and satellite galaxies (e.g., Coccato et al 2009;Nierenberg et al 2011;Deason et al 2012;Norris et al 2012). All these methods have their limits, such as the redshift of the observed object, the luminosity profile, and gas content.…”

Section: Introductionmentioning

confidence: 99%

Quadruple-peaked spectral line profiles as a tool to constrain gravitational potential of shell galaxies

Ebrová

Jílková

Jungwiert

et al. 2012

A&A

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Context. Stellar shells observed in many giant elliptical and lenticular as well as a few spiral and dwarf galaxies presumably result from galaxy mergers. Line-of-sight velocity distributions of the shells could, in principle, if measured with a sufficiently high signalto-noise ratio, constitute a method to constrain the gravitational potential of the host galaxy. Aims. Merrifield & Kuijken (1998, MNRAS, 297, 1292) predicted a double-peaked line profile for stationary shells resulting from a nearly radial minor merger. In this paper, we aim at extending their analysis to a more realistic case of expanding shells, inherent to the merging process, whereas we assume the same type of merger and the same orbital geometry. Methods. We used an analytical approach as well as test particle simulations to predict the line-of-sight velocity profile across the shell structure. Simulated line profiles were convolved with spectral PSFs to estimate peak detectability. Results. The resulting line-of-sight velocity distributions are more complex than previously predicted due to nonzero phase velocity of the shells. In principle, each of the Merrifield & Kuijken (1998) peaks splits into two, giving a quadruple-peaked line profile, which allows more precise determination of the potential of the host galaxy and contains additional information. We find simple analytical expressions that connect the positions of the four peaks of the line profile and the mass distribution of the galaxy, namely, the circular velocity at the given shell radius and the propagation velocity of the shell. The analytical expressions were applied to a test-particle simulation of a radial minor merger, and the potential of the simulated host galaxy was successfully recovered. Shell kinematics can thus become an independent tool to determine the content and distribution of the dark matter in shell galaxies up to ∼100 kpc from the center of the host galaxy.

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“…For galaxies with extended gas beyond the ACIS chips, we compared our measurements with results in the literature. For example, Nagino & Matsushita (2009) recently analyzed Chandra and XMM-Newton observations for a sample of gas rich elliptical galaxies and reported their gas luminosities and temperatures in concentric annuli. We estimated the emission-weighted average temperature and confirmed that our results are consistent with those of Nagino & Matsushita within the uncertainties.…”

Section: X-ray Data Analysismentioning

confidence: 99%

X-Ray Scaling Relations of “Core” and “Coreless” E and S0 Galaxies

Kim

Fabbiano

2015

ApJ

100

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We have re-examined the two X-ray scaling relations of early-type galaxies (ETGs), L X,GAS -L K and L X,GAS -T GAS , using 61 ATLAS 3D E and S0 galaxies observed with Chandra (including ROSAT results for a few X-ray bright galaxies with extended hot gas). With this sample, which doubles the number of ETGs available for study, we confirm the strong, steep correlations reported by Boroson et al (2011). Moreover, the larger sample allows us to investigate the effect of structural and dynamical properties of ETGs in these relations. Using the sub-sample of 11 'genuine' E galaxies with central surface brightness cores, slow stellar rotations and old stellar populations, we find that the scatter of the correlations is strongly reduced, yielding an extremely tight relation, of the form L X,GAS ~ T GAS 4.5±0.3 . The rms deviation is only 0.13 dex. For the gas-rich galaxies in this sample (L X, GAS > 10 40 erg s -1 ), this relation is consistent with recent simulations for velocity dispersion supported E galaxies. However, the tight L X,GAS -T GAS relation of genuine E galaxies extends down into the L X ~ 10 38 erg s -1 range, where simulations predict the gas to be in outflow/wind state, with resulting L X much lower than observed in our sample. The observed correlation may suggest the presence of small bound hot halos even in this low luminosity range. At the high luminosity end, the L X,GAS -T GAS correlation of core elliptical galaxies is similar to that found in samples of cD galaxies and groups, but shifted down toward relatively lower L X,GAS for a given T GAS . In particular cDs, central dominant galaxies sitting at the bottom of the potential well imposed by the group dark matter, have an order of magnitude higher L X,GAS than our sample core galaxies for the same L K and T GAS . We suggest that enhanced cooling in cDs, which have higher hot gas densities and lower entropies, could lower T GAS to the range observed in giant Es; this conclusion is supported by the presence of extended cold gas in several cDs. Instead, in the sub-sample of coreless ETGs -these galaxies also tend to show stellar rotation, a flattened galaxy figure and rejuvenation of the stellar population -L X,GAS and T GAS are not correlated. The L X -T GAS distribution of coreless ETGs is a scatter diagram clustered at L X, GAS < 10 40 erg s -1 , similar to that reported for the hot interstellar medium (ISM) of spiral galaxies, suggesting that both the energy input from star formation and the effect of galactic rotation and flattening may disrupt the hot ISM.

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

Cited by 74 publications

References 41 publications

Dark matter halos around isolated ellipticals

Dark matter halos around isolated ellipticals

Quadruple-peaked spectral line profiles as a tool to constrain gravitational potential of shell galaxies

X-Ray Scaling Relations of “Core” and “Coreless” E and S0 Galaxies

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