The X-ray luminosity-velocity dispersion relation in the REFLEX cluster survey

Ortiz-Gil, A.; Guzzo, L.; Schuecker, P.; Böhringer, H.; Collins, C. A.

doi:10.1111/j.1365-2966.2004.07371.x

Cited by 44 publications

(58 citation statements)

References 38 publications

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“…Assuming that the gas entrained in the gravitational potential is virialized, self-similarity predicts s µ L X,gas 4 . This has previously been observed in galaxy clusters (e.g., Mushotzky & Scharf 1997;Mulchaey & Zabludoff 1998;Wu et al 1999;Helsdon & Ponman 2000;Xue & Wu 2000;Mahdavi & Geller 2001;Ortiz-Gil et al 2004). However, several relations between total L X,gas and σ have been reported for elliptical galaxies, with exponents ranging from~8 to 14 (including uncertainties; e.g., Eskridge et al 1995;Mahdavi & Geller 2001;Diehl & Statler 2007).…”

Section: The L Xgas -σ E Relationmentioning

confidence: 82%

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

Goulding

Greene

et al. 2016

ApJ

112

156

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Studies of the physical properties of local elliptical galaxies are shedding new light on galaxy formation. Here we present the hot-gas properties of 33 early-type systems within the MASSIVE galaxy survey that have archival Chandra X-ray observations, and we use these data to derive X-ray luminosities (L X,gas ) and plasma temperatures (T gas ) for the diffuse gas components. We combine this with the ATLAS 3D survey to investigate the X-ray-optical properties of a statistically significant sample of early-type galaxies across a wide range of environments. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, we deduce that all early types (independent of galaxy mass, environment, and rotational support) follow a universal scaling law such that µL T X,gas gas 4.5 . We further demonstrate that the scatter in L X,gas around both K-band luminosity (L K ) and the galaxy stellar velocity dispersion (s e ) is primarily driven by T gas , with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the gas origin directly to either stellar mass or galaxy potential. Indeed, our data require a steeper relation between L L , K X,gas , and s e than predicted by standard mass-loss models. Finally, we find that T gas is set by the galaxy potential inside the optical effective radius. We conclude that within the innermost 10-30 kpc region, early types maintain pressure-supported hot gas, with a minimum T gas set by the virial temperature, but the majority show evidence for additional heating.

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Section: The L Xgas -σ E Relationmentioning

confidence: 82%

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

Goulding

Greene

et al. 2016

ApJ

112

156

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“…This has been done, complementing the data described here with literature redshifts, for a sub-sample of 170 REFLEX clusters, allowing us to study the scaling relation between cluster velocity dispersion and X-ray luminosity (Ortiz-Gil et al 2004).…”

Section: Reflex Identification Strategy: Overviewmentioning

confidence: 99%

“…The new redshifts for galaxies in REFLEX clusters presented here have been used, together with a large bulk of existing data from the literature, to assign a systemic redshift to each cluster, as described in Paper II and to compute a velocity dispersion for a sub-set of 170 objects, as reported in Ortiz-Gil et al (2004). In Paper II, we already presented a first discussion of the sample resulting from the redshift survey, mostly concentrating on the unambiguous identification of the redshift system related to the X-ray source.…”

Section: Luminosity and Spatial Distributionmentioning

confidence: 99%

“…• the cluster X-ray luminosity function , and from this the mean abundance of clusters; • the two-point correlation function of the cluster distribution (Collins et al 2000); • the power spectrum of the cluster distribution ; • the values of the cosmic mean density of matter Ω M and the power spectrum normalization σ 8 , via the combination of the above observables (Schuecker et al 2003a); • the Gaussianity of the cluster distribution, as described by Minkowski functionals (Kersher et al 2001); • the value of the equation of state parameter of dark energy w (Schuecker et al 2003b); • the relation between cluster velocity dispersions (measurable for a sub-sample of 170 clusters) and X-ray luminosity (Ortiz-Gil et al 2004); • the cluster-galaxy correlation function (Sanchez et al 2005);…”

Section: Introductionmentioning

confidence: 99%

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The REFLEX galaxy cluster survey

Guzzo

Schuecker

Böehringer

et al. 2009

A&A

Self Cite

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We present the final data from the spectroscopic survey of the ROSAT-ESO Flux-Limited X-ray (REFLEX) catalog of galaxy clusters. The REFLEX survey covers 4.24 steradians (34% of the entire sky) below a declination of δ = +2.5 0 and at high Galactic latitude (|b| > 20 • ). The REFLEX catalog includes 447 entries with a median redshift of 0.08 and is better than 90% complete to a limiting flux f X = 3 × 10 −12 erg s −1 cm −2 (0.1 to 2.4 keV), representing the largest statistically homogeneous sample of clusters drawn from the ROSAT All-Sky Survey (RASS) to date. Here we describe the details of the spectroscopic observations carried out at the ESO 1.5 m, 2.2 m, and 3.6 m telescopes, as well as the data reduction and redshift measurement techniques. The spectra typically cover the wavelength range 3600-7500 Å at a two-pixel resolution of ∼14 Å, and the measured redshifts have a total rms error of ∼100 km s −1 . In total we present 1406 new galaxy redshifts in 192 clusters, most of which previously did not have any redshift measured. Finally, the luminosity/redshift distributions of the cluster sample and a comparison to the no-evolution expectations from the cluster X-ray luminosity function are presented.

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“…In fact, theoretical predictions based on purely gravitational collapse lead to L X ∝ σ 4 v . There are several observational studies of this relation, the majority of them finding values between 4 and 5.3 for the slope (Quintana & Melnick 1982;Edge & Stewart 1991;Mulchaey & Zabludoff 1998;Borgani et al 1999;Xue & Wu 2000;Mahdavi & Geller 2001;Girardi & Mezzetti 2001;Ortiz-Gil et al 2004;Hilton et al 2005). In Fig.…”

Section: X −σ V Relationmentioning

confidence: 99%

Fossil group origins

Zarattini¹,

Barrena²,

Girardi³

et al. 2014

A&A

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Context. Virialized halos grow by the accretion of smaller ones in the cold dark matter scenario. The rate of accretion depends on the different properties of the host halo. Those halos for which this accretion rate was very fast and efficient resulted in systems dominated by a central galaxy surrounded by smaller galaxies that were at least two magnitudes fainter. These galaxy systems are called fossil systems, and they can be the fossil relics of ancient galaxy structures. Aims. We started an extensive observational program to characterize a sample of 34 fossil group candidates spanning a broad range of physical properties. Methods. Deep r-band images were obtained with the 2.5-m Isaac Newton Telescope and Nordic Optic Telescope. Optical spectroscopic observations were performed at the 3.5-m Telescopio Nazionale Galileo for ∼1200 galaxies. This new dataset was completed with Sloan Digital Sky Survey Data Release 7 archival data to obtain robust cluster membership and global properties of each fossil group candidate. For each system, we recomputed the magnitude gaps between the two brightest galaxies (Δm 12 ) and the first and fourth ranked galaxies (Δm 14 ) within 0.5 R 200 . We consider fossil systems to be those with Δm 12 ≥ 2 mag or Δm 14 ≥ 2.5 mag within the errors. Results. We find that 15 candidates turned out to be fossil systems. Their observational properties agree with those of non-fossil systems. Both follow the same correlations, but the fossil systems are always extreme cases. In particular, they host the brightest central galaxies, and the fraction of total galaxy light enclosed in the brightest group galaxy is larger in fossil than in non-fossil systems. Finally, we confirm the existence of genuine fossil clusters. Conclusions. Combining our results with others in the literature, we favor the merging scenario in which fossil systems formed from mergers of L * galaxies. The large magnitude gap is a consequence of the extreme merger ratio within fossil systems and therefore it is an evolutionary effect. Moreover, we suggest that at least one fossil group candidate in our sample could represent a transitional fossil stage. This system could have been a fossil in the past, but not now owing to the recent accretion of another group of galaxies.

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The X-ray luminosity-velocity dispersion relation in the REFLEX cluster survey

Cited by 44 publications

References 38 publications

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

The REFLEX galaxy cluster survey

Fossil group origins

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