Evolution of galaxies in clusters

Poggianti, Bianca M.

doi:10.22323/1.014.0104

Cited by 7 publications

(5 citation statements)

References 70 publications

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“…An alternative explanation is that local processes (e.g., galaxy-scale interaction) affect star formation activities, rather than the global processes (like ram-pressure stripping within the cluster-scale environment). This result again proves the correctness of the morphology-density relation pointed out by Dressler (1980), which can be well explained in the context of the hierarchical cosmological scenario (Poggianti 2004).…”

Section: Star Formation Properties Of Cluster Galaxiessupporting

confidence: 82%

Multicolor photometry of the nearby galaxy cluster A119

Tian¹,

Yuan²,

Xu³

et al. 2012

Res. Astron. Astrophys.

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This paper presents multicolor optical photometry of the nearby galaxy cluster Abell 119 (z = 0.0442) with the Beijing-Arizona-Taiwan-Connecticut (BATC) system of 15 intermediate bands. Within the BATC viewing field of 58 ′ × 58 ′ , there are 368 galaxies with known spectroscopic redshifts, including 238 member galaxies (called sample I). Based on the spectral energy distributions (SEDs) of 1376 galaxies brighter than i BATC = 19.5, photometric redshift technique and the color-magnitude relation of earlytype galaxies are applied to select faint member galaxies. As a result, 117 faint galaxies were selected as new member galaxies. Combined with sample I, an enlarged sample (called sample II) of 355 member galaxies is obtained. Spatial distribution and localized velocity structure for two samples demonstrate that A119 is a dynamically complex cluster with at least three prominent substructures in the central region within 1 Mpc. A large velocity dispersion for the central clump indicates a merging along the line of sight. No significant evidences for morphology and luminosity segregations are found in both samples. With the evolutionary synthesis model PEGASE, environmental effect on the star formation properties is confirmed. Faint galaxies in low-density region tend to have longer time scales of star formation, smaller mean stellar ages, and lower metallicities of interstellar medium, which is in agreement with the context of hierarchical cosmological scenario.

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Section: Star Formation Properties Of Cluster Galaxiessupporting

confidence: 82%

Multicolor photometry of the nearby galaxy cluster A119

Tian¹,

Yuan²,

Xu³

et al. 2012

Res. Astron. Astrophys.

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“…Panel (a) shows that the galaxies in the outer region are likely to have longer SFR time scales than those in the core region. Considering that late-type galaxies tend to have longer time scales of star formation, our result is consistent with the morphology-density relation first pointed out by Dressler (1980), which can be explained well in the context of the hierarchical cosmological scenario (Poggianti 2004). As shown in the panels (c) and (d), the outlier member galaxies are likely to possess younger stellar populations, resulting in a smaller mean stellar age weighted by either mass or light.…”

Section: Star Formation Propertiessupporting

confidence: 91%

“…As all galaxies in A98 have the same distance modulus, the apparent magnitudes could reflect their intrinsic luminosities. For bright and massive cluster galaxies in the core region of A98, their star formation activities have been reduced by some physical processes via environmental effects, such as galaxy-galaxy interaction, harassment, gas stripping, or strangulation (Poggianti 2004;Yuan et al 2005), which leads to a short SFR time scale. From Figure 11(b) and Figure 12(b), no bright (m h < 16.5) and no central (Σ > 0.4 gal.…”

Section: Star Formation Propertiesmentioning

confidence: 99%

Multicolor photometry of the galaxy cluster A98: substructures and star formation properties

Zhang

Yuan

et al. 2010

Res. Astron. Astrophys.

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An optical photometric observation with the Beijing-Arizona-Taiwan-Connecticut (BATC) multicolor system is carried out for A98 (z = 0.104), a galaxy cluster with two large enhancements in X-ray surface brightness. The spectral energy distributions (SEDs) covering 15 intermediate bands are obtained for all sources detected down to V ∼ 20 mag in a field of 58 ′ × 58 ′ . After the star-galaxy separation by the color-color diagrams, a photometric redshift technique is applied to the galaxy sample for further membership determination. The color-magnitude relation is taken as a further restriction of the early-type cluster galaxies. As a result, a list of 198 faint member galaxies is achieved. Based on newly generated sample of member galaxies, the dynamical substructures, A98N, A98S, and A98W, are investigated in detail. A separate galaxy group, A98X, is also found to the south of main concentration of A98, which is gravitationally unbound to A98. For 74 spectroscopically confirmed member galaxies, the environmental effect on the star formation histories is found. The bright galaxies in the core region are found to have shorter time scales of star formation, longer mean stellar ages, and higher metallicities of interstellar medium, which can be interpreted in the context of hierarchical cosmological scenario.

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“…These mechanisms effect the gas either by stimulating star formation (which rapidly consumes the gas, locking it up in stars) or by removing the gas from the galaxy (and ionising it) or by preventing further accretion. Unlike the other mechanisms listed which quench star formation relatively quickly (∼10 7 years), strangulation causes a slow decline in star formation over longer timescales (>1 Gyr) (Poggianti 2004).…”

Section: Introductionmentioning

confidence: 92%

“…The amount of star formation in galaxies in general increases with redshift, with there being an order of magnitude increase in the cosmic star formation rate density between the present time and z ∼ 1 (Lilly et al 1996;Madau et al 1996;Hopkins 2004). The trend that with higher galaxy density there are fewer galaxies with ongoing star formation continues to at least z ∼ 0.8 (Poggianti et al 2008).…”

Section: Introductionmentioning

confidence: 98%

The H i gas content of galaxies around Abell 370, a galaxy cluster atz= 0.37

Lah¹,

Pracy²,

Chengalur³

et al. 2009

Monthly Notices of the Royal Astronomical Society

101

116

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We used observations from the Giant Metrewave Radio Telescope to measure the atomic hydrogen gas content of 324 galaxies around the galaxy cluster Abell 370 at a redshift of z= 0.37 (a look‐back time of ∼4 billion years). The H i 21 cm emission from these galaxies was measured by co‐adding their signals using precise optical redshifts obtained with the Anglo‐Australian Telescope. The average H i mass measured for all 324 galaxies is (6.6 ± 3.5) × 109 M⊙, while the average H i mass measured for the 105 optically blue galaxies is (19.0 ± 6.5) × 109 M⊙. The significant quantities of gas found around Abell 370 suggest that there has been substantial evolution in the gas content of galaxy clusters since redshift z= 0.37. The total amount of atomic hydrogen gas found around Abell 370 is up to approximately eight times more than that seen around the Coma cluster, a nearby galaxy cluster of similar size. Despite this higher gas content, Abell 370 shows the same trend as nearby clusters that galaxies close to the cluster core have lower H i gas content than galaxies further away where the galaxy density is lower. The optically blue galaxies contain the majority of the H i gas surrounding the cluster. However, there is evidence that the optically red galaxies contain appreciable quantities of H i gas within their central regions. The Abell 370 galaxies have H i mass‐to‐optical‐light ratios similar to local galaxy samples and have the same correlation between their star formation rate and H i mass as found in the nearby galaxies. The average star formation rate derived from [O ii] emission and from deredshifted 1.4 GHz radio continuum for the Abell 370 galaxies also follows the correlation found in the local Universe. The large amounts of H i gas found around the cluster can easily be consumed entirely by the observed star formation rate in the galaxies over ∼4 billion years (from z= 0.37) to the present day. Abell 370 appears set to evolve into a gas‐poor system similar to galaxy clusters observed in the local Universe.

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Evolution of galaxies in clusters

Cited by 7 publications

References 70 publications

Multicolor photometry of the nearby galaxy cluster A119

Multicolor photometry of the nearby galaxy cluster A119

Multicolor photometry of the galaxy cluster A98: substructures and star formation properties

The H i gas content of galaxies around Abell 370, a galaxy cluster atz= 0.37

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