A LOW-REDSHIFT GALAXY CLUSTER X-RAY TEMPERATURE FUNCTION INCORPORATING<i>SUZAKU</i>DATA

Shang, Cien; Scharf, Caleb

doi:10.1088/0004-637x/690/1/879

Cited by 16 publications

(10 citation statements)

References 51 publications

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“…The uncorrected observed L X -T relation behaves quite similarly to that of the uncorrected L X -M. The observed slope of our group sample is consistent within the errors with that of the clusters and in general with the results from other papers investigating galaxy groups (e.g., Osmond & Ponman 2004;Shang & Scharf 2009;Eckmiller et al 2011). Because the emissivity at low temperatures scales with T −0.6 (McKee & Cowie 1977), the relation predicted by the self-similar scenario for galaxy groups is L X ∝ T 1.1 , which is flatter than the observed relation.…”

Section: Selection Biassupporting

confidence: 90%

Scaling properties of a complete X-ray selected galaxy group sample

Lovisari

Reiprich

Schellenberger

2015

A&A

246

326

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Context. Upcoming X-ray surveys like eROSITA require precise calibration between X-ray observables and mass down to the lowmass regime to set tight constraints on the fundamental cosmological parameters. Since an individual mass measurement is only possible for relatively few objects, it is crucial to have reliable and clearly understood scaling relations that relate the total mass to easily observable quantities. Aims. The main goal of this work is to constrain the galaxy group scaling relations corrected for selection effects, and to quantify the influence of non-gravitational physics at the low-mass regime. Methods. We analyzed XMM-Newton observations for a complete sample of galaxy groups selected from the ROSAT All-Sky Survey and compared the derived scaling properties with a galaxy cluster sample. To investigate the role played by the different non-gravitational processes we then compared the observational data with the predictions of hydrodynamical simulations. Results. After applying the correction for selection effects (e.g., Malmquist bias), the L X -M relation is steeper than the observed one. Its slope (1.66 ± 0.22) is also steeper than the value obtained by using the more massive systems of the HIFLUGCS sample. This behavior can be explained by a gradual change of the true L X -M relation, which should be taken into account when converting the observational parameters into masses. The other observed scaling relations (not corrected for selection biases) do not show any break, although the comparison with the simulations suggests that feedback processes play an important role in the formation and evolution of galaxy groups. Thanks to our master sample of 82 objects spanning two order of magnitude in mass, we tightly constrain the dependence of the gas mass fraction on the total mass, finding a difference of almost a factor of two between groups and clusters. We also found that the use of different AtomDB versions in the calculation of the group properties (e.g., temperature and density) yields a gas fraction of up to 20% lower than an older version.

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Section: Selection Biassupporting

confidence: 90%

Scaling properties of a complete X-ray selected galaxy group sample

Lovisari

Reiprich

Schellenberger

2015

A&A

246

326

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“…It is possible there is a gradual, continuous shift which may be harder to detect due to the increase in scatter, and which leads to different results depending on which objects are compared. For example, we found that the L x − T slope of our group sample selected by luminosity is consistent with that of the HIFLUGCS clusters, as well as the samples of Osmond & Ponman (2004) and Shang & Scharf (2009), but the relation for systems below 3 keV is steeper than the slope for hotter objects. Using a broken powerlaw function however does not significantly improve the fit.…”

Section: Discussionsupporting

confidence: 78%

Testing the low-mass end of X-ray scaling relations with a sample ofChandragalaxy groups

Eckmiller

Hudson

Reiprich

2011

A&A

130

183

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Context. Well-determined scaling relations between X-ray observables and cluster mass are essential for using large cluster samples to constrain fundamental cosmological parameters. Scaling relations between cluster masses and observables, such as the luminositytemperature, mass-temperature, luminosity-mass relations, have been investigated extensively, however the question of whether these relations hold true also for poor clusters and groups remains unsettled. Some evidence supports a "break" at the low end of the group/cluster mass range, possibly caused by the stronger influence of non-gravitational physics on low-mass systems. Aims. The main goal of this work is to test local scaling relations for the low-mass range in order to check whether or not there is a systematic difference between clusters and groups, and to thereby extend this method of reliable and convenient cluster mass determination for future large samples down to the group regime. Methods. We compiled a statistically complete sample of 112 X-ray galaxy groups, 26 of which have usable Chandra data. Temperature, metallicity, and surface brightness profiles were created for these 26 groups, and used to determine the main physical quantities and scaling relations. We then compared the group properties to those of the HIFLUGCS clusters, as well as several other group and cluster samples. Results. We present radial profiles for the individual objects and scaling relations of the whole sample (. Temperature and metallicity profiles behave universally, except for the core regions.and L x − Y x relations of the group sample are generally in good agreement with clusters. The L x − T relation steepens for T < 3 keV, which could point to a larger impact of heating mechanisms on cooler systems. We found a significant drop in the gas mass fraction below < ∼ 1 keV, as well as a correlation with radius, which indicates the ICM is less dominant in groups compared to clusters and the galaxies have a stronger influence on the global properties of the system. In all relations the intrinsic scatter for groups is larger than for clusters, which appears not to be correlated with merger activity but could be due to scatter caused by baryonic physics in the group cores. We also demonstrate the importance of selection effects. Conclusions. We have found some evidence for a similarity break between groups and clusters. However this does not have a strong effect on the scaling relations.

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“…The presence of an X-ray point source at the location of JO206 is also hinted by the map presented in Shang & Scharf (2009). Moreover, there is a 1.4 GHz NVSS detection within 8 arcsec from the position of JO206 (Condon et al 1998).…”

Section: Gas Ionization Mechanismmentioning

confidence: 53%

GASP. I. Gas Stripping Phenomena in Galaxies with MUSE

Poggianti

Moretti

Gullieuszik

et al. 2017

ApJ

346

406

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GASP (GAs Stripping Phenomena in galaxies with MUSE) is a new integral-field spectroscopic survey with MUSE at the VLT aiming at studying gas removal processes in galaxies. We present an overview of the survey and show a first example of a galaxy undergoing strong gas stripping. GASP is obtaining deep MUSE data for 114 galaxies at z=0.04-0.07 with stellar masses in the range 10 9.2 -10 11.5 M in different environments (galaxy clusters and groups, over more than four orders of magnitude in halo mass). GASP targets galaxies with optical signatures of unilateral debris or tails reminiscent of gas stripping processes ("jellyfish galaxies"), as well as a control sample of disk galaxies with no morphological anomalies. GASP is the only existing Integral Field Unit (IFU) survey covering both the main galaxy body and the outskirts and surroundings, where the IFU data can reveal the presence and the origin of the outer gas. To demonstrate GASP's ability to probe the physics of gas and stars, we show the complete analysis of a textbook case of a "jellyfish" galaxy, JO206. This is a massive galaxy (9 × 10 10 M ) in a low-mass cluster (σ ∼ 500 km s −1 ), at a small projected clustercentric radius and a high relative velocity, with ≥90kpc-long tentacles of ionized gas stripped away by ram pressure. We present the spatially resolved kinematics and physical properties of gas and stars, and depict the evolutionary history of this galaxy.

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A LOW-REDSHIFT GALAXY CLUSTER X-RAY TEMPERATURE FUNCTION INCORPORATINGSUZAKUDATA

Cited by 16 publications

References 51 publications

Scaling properties of a complete X-ray selected galaxy group sample

Scaling properties of a complete X-ray selected galaxy group sample

Testing the low-mass end of X-ray scaling relations with a sample ofChandragalaxy groups

GASP. I. Gas Stripping Phenomena in Galaxies with MUSE

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