Chandra Observation of a Group of Galaxies HCG 80: Does the Spiral-Only Group Have Hot Intragroup Gas?

Ota, Naomi; Morita, U.; Kitayama, Tetsu; Ohashi, T.

doi:10.1093/pasj/56.5.753

Cited by 7 publications

(6 citation statements)

References 44 publications

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“…If we use the spectral results and attribute the emission modelled with a plasma spectrum to a hot ISM, we can derive an average gas density of n e ∼ 7.5×10 −3 cm −3 and a total mass of M gas ∼ 3×10 8 M in the hot phase, under a simple assumption of a spherical distribution within r ∼ 7.5 kpc. This is ∼10× lower than what is detected in the neutral cold phase (H i Pompei et al 2007), but relatively high with respect to the hot ISM detected in the disk and halos of star-forming late type galaxies (Tüllmann et al 2006) and comparable to the amount of hot gas detected in HCG80a (Ota et al 2004).…”

Section: Individual Galaxiesmentioning

confidence: 55%

“…The X-ray properties appear also very similar: all 4 galaxies are detected as individual sources (both due to the AGN and starburst activity) already by the ROSAT satellite (Saracco & Ciliegi, 1995;Ponman et al, 1996;Dos Santos & Mamon, 1999), while the diffuse emission recently characterised with XMM-Newton has a comparable luminosity but slightly higher best fit temperature (∼ 0.5 keV, although within the uncertainties; note that the ROSAT data suggested a cooler temperature of 0.27 keV Dos Santos & Mamon, 1999) than SCG0018-4854. Only two other systems, with a spiral fraction of ∼ 1, have been studied with Chandra or XMM-Newton: HCG 80 (Ota et al, 2004) was not detected by Chandra, with an estimated limit to the luminosity of the diffuse component at L x ∼ 6 × 10 40 h −2 70 erg s −1 , in spite of the larger velocity dispersion (σ v ∼ 300 km s −1 ) of the system; low level diffuse emission is measured in recent XMM-Newton images of the Cartwheel, again at similar luminosities and gas temperatures (Crivellari et al, in preparation).…”

Section: Scg0018-4854 In Contextmentioning

confidence: 99%

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Detection of a hot intergalactic medium in the spiral-only compact group SCG0018-4854

Trinchieri

Iovino

Pompei³

et al. 2008

A&A

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Aims. Compact groups of galaxies are excellent laboratories for studying galaxy interactions and their effects on the evolution of galaxies. In particular, dynamically young systems, with a large fraction of interacting, late type galaxies, have so far escaped proper studies in the X-ray band and their hot intergalactic medium properties are virtually unknown. Motivated by this lack of knowledge, we present a detailed investigation here of the X-ray properties of such a dynamically young system. Methods. We obtained XMM-Newton observations of one spiral-only system in the new southern compact group catalogue: SCG0018-4854. We present here the results of the data analysis and discuss them in comparison with the few other similar systems also studied in the X-ray band. Results. The 4 members of SCG0018-4854 emit at a level comparable to what is expected based on their optical properties. We detect the low level diffuse emission between galaxies, which is most likely due to the presence of the intergalactic medium. Compared to other spiral-only groups, SCG0018-4854 could be the coolest system detected so far, although the measurements have large uncertainties. These results indicate that high quality deep X-ray observations are needed to allow a proper study of the properties of the potential well of dynamically young systems, before more general conclusions can be drawn on their average characteristics.

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Section: Individual Galaxiesmentioning

confidence: 55%

Section: Scg0018-4854 In Contextmentioning

confidence: 99%

Detection of a hot intergalactic medium in the spiral-only compact group SCG0018-4854

Trinchieri

Iovino

Pompei³

et al. 2008

A&A

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“…It is known that galaxy groups exhibit rather large scatter in their gas richness (Osmond & Ponman 2004), with spiral-rich ones tending to be particularly gas poor (Ota et al 2004). From equation (15), we may then speculate that a galaxy group borne as a relatively gas-rich system is subject to a fast merger process, while it remains otherwise an ordinary group.…”

Section: Discussionmentioning

confidence: 97%

A Galaxy Merger Scenario for the NGC 1550 Galaxy From Metal Distributions in the X-Ray Emitting Plasma

Kawaharada

Makishima

Kitaguchi

et al. 2009

ApJ

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The elliptical galaxy NGC 1550 at a redshift of z = 0.01239, identified with an extended X-ray source RX J0419+0225, was observed with XMM-Newton for 31 ks. From the X-ray data and archival near infra-red data of Two Micron All Sky survay, we derive the profiles of components constituting the NGC 1550 system; the gas mass, total mass, metal mass, and galaxy luminosity. The metals (oxygen, silicon, and iron) are extended to ∼ 200 kpc from the center, wherein ∼ 70% of the K-band luminosity is carried by NGC 1550 itself. As first revealed with ASCA, the data reconfirms the presence of a dark halo, of which the mass (1.6×10 13 M ⊙ ) is typical of a galaxy group rather than of a single galaxy. Within 210 kpc, the K-band mass-to-light ratio reaches 75 M ⊙ /L ⊙ , which is comparable to those of clusters of galaxies. The iron-mass-to-light ratio profile (silicon-and oxygen-mass-to-light ratio profiles as well) exhibits about two orders of magnitude decrease toward the center. Further studies comparing mass densities of metals with those of the other cluster components reveal that the iron (as well as silicon) in the ICM traces very well the total gravitating mass, whereas the stellar component is significantly more concentrated to within several tens kpc of the NGC 1550 nucleus. Thus, in the central region, the amount of metals is significantly depleted for the luminous galaxy light. Among a few possible explanations of this effect, the most likely scenario is that galaxies in this system were initially much more extended than today, and gradually fell to the center and merged into NGC 1550.

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“…The pioneering work of Zabludoff (1999) suggested that groups might fall into different classes defined by their X-ray properties: from groups with a luminous, extended, hot IGM centred on a giant E to groups with little or no diffuse emission. Several examples of these classes can now be found in the literature (see e.g., Mulchaey et al 2003;Trinchieri et al 2003;Belsole et al 2003;Ota et al 2004). In a hierarchical evolutionary scenario, the final product of a merged group would be a luminous isolated E with an extended X-ray halo, and a few have indeed been identified (see e.g., Mulchaey & Zabludoff 1999;Vikhlinin et al 1999;Jones et al 2003;Khosroshahi et al 2004).…”

Section: Introductionmentioning

confidence: 95%

Small-scale systems of galaxies

Grützbauch

Zeilinger

Rampazzo

et al. 2009

A&A

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Context. In hierarchical evolutionary scenarios, isolated, physical pairs may represent an intermediate phase, or "way station", between collapsing groups and isolated elliptical (E) galaxies (or fossil groups). Aims. We started a comprehensive study of a sample of galaxy pairs composed of a giant E and a spiral (S) with the aim of investigating their formation/evolutionary history from observed optical and X-ray properties. Methods. We present VLT-VIMOS observations designed to identify faint galaxies associated with the E+S systems from candidate lists generated using photometric criteria on WFI images covering an area of ∼0.2 h −1 100 Mpc radius around the pairs. Results. We found two and ten new members likely to be associated with the X-ray bright systems RR 143 and RR 242, respectively. The X-ray faint RR 210 and RR 216, which were only partially covered by the VIMOS observations, have two and three new faint members, respectively. The new members increase the number of associated galaxies to 4, 7, 6, and 16 for RR 143, RR 210, RR 216, and RR 242, respectively, down to M R ∼ −12 + 5 log h 100 . We derive structural properties of the faint members from surface photometry. The faint galaxy population of all the systems is dominated by disk galaxies, 40% being S0s with generally low bulge to total light ratios. A small fraction of the faint companions show signatures of interaction. A remarkable shell system is detected in the early-type galaxy RR 242_24532. We also derive dynamical properties and optical luminosity functions for the 4 groups. Conclusions. The above results are discussed in the context of the evolution of poor galaxy group associations. A comparison between the optical luminosity functions (OLFs) of our E+S systems and a sample of X-ray bright poor groups suggest that the OLF of X-ray detected poor galaxy systems is not universal. The OLF of our X-ray bright systems suggests that they are more dynamically evolved than our X-ray faint sample and some X-ray bright groups in the literature. However, we suggest that the X-ray faint E+S pairs represent a phase in the dynamical evolution of some X-ray bright poor galaxy groups. The recent or ongoing interaction in which the E member of the X-ray faint pairs is involved could have decreased the luminosity of any surrounding X-ray emitting gas.

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Chandra Observation of a Group of Galaxies HCG 80: Does the Spiral-Only Group Have Hot Intragroup Gas?

Cited by 7 publications

References 44 publications

Detection of a hot intergalactic medium in the spiral-only compact group SCG0018-4854

Detection of a hot intergalactic medium in the spiral-only compact group SCG0018-4854

A Galaxy Merger Scenario for the NGC 1550 Galaxy From Metal Distributions in the X-Ray Emitting Plasma

Small-scale systems of galaxies

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