Interacting Galaxies in the A901/902 Supercluster With Stages

Heiderman, Amanda; Jogee, Shardha; Marinova, Irina; Kampen, E. van; Barden, M.; Peng, Chien Y.; Heymans, Catherine; Gray, Meghan E.; Bell, Eric F.; Bacon, David; Balogh, Michael L.; Barazza, Fabio D.; Boehm, A.; Caldwell, J. A. R.; Häußler, Boris; Jahnke, K.; Lane, Kyle; McIntosh, Daniel H.; Meisenheimer, K.; Sanchez, Sebastian Francisco Sanchez; Somerville, Rachel S.; Taylor, Andy; Wisotzki, L.; Wolf, Christian; Zheng, Xianzhong

doi:10.1088/0004-637x/705/2/1433

Cited by 37 publications

(44 citation statements)

References 96 publications

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“…In Figure 2, we show the position in the sky plane of ET (bullets), LT (open squares), and major mergers (gray triangles) for M 10 10 M galaxies in the LSS: ET galaxies are concentrated in more populated regions, while LT galaxies are located in the outskirts of the structure, as expected by the morphology-density relation (Dressler 1980). In addition, the three gas-rich major mergers in the LSS are also located in the outskirts, a natural consequence of the external location of their progenitors, i.e., LT galaxies (see also Heiderman et al 2009). …”

Section: Large-scale Structure Effectmentioning

confidence: 56%

THE MINOR ROLE OF GAS-RICH MAJOR MERGERS IN THE RISE OF INTERMEDIATE-MASS EARLY TYPES ATz⩽ 1

López-Sanjuan

Balcells

Pérez‐González

et al. 2010

ApJ

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We study the evolution of galaxy structure since z ∼ 1 to the present. From a Great Observatories Origins Deep Survey South (GOODS-S) multi-band catalog, we define (blue) luminosity-and mass-weighted samples, limited by M B −20 and M 10 10 M , comprising 1122 and 987 galaxies, respectively. We extract early-type (ET; E/S0/ Sa) and late-type (LT; Sb-Irr) subsamples by their position in the concentration-asymmetry plane, in which galaxies exhibit a clear bimodality. We find that the ET fraction, f ET , rises with cosmic time, with a corresponding decrease in the LT fraction, f LT , in both luminosity-and mass-selected samples. However, the evolution of the comoving number density is very different: the decrease in the total number density of M B −20 galaxies since z = 1 is due to the decrease in the LT population, which accounts for ∼75% of the total star formation rate in the range under study, while the increase in the total number density of M 10 10 M galaxies in the same redshift range is due to the evolution of ETs. This suggests that we need a structural transformation between LT galaxies that form stars actively and ET galaxies in which the stellar mass is located. Comparing the observed evolution with the gas-rich major merger rate in GOODS-S, we infer that only ∼20% of the new ET galaxies with M 10 10 M appeared since z ∼ 1 can be explained by this kind of mergers, suggesting that minor mergers and secular processes may be the driving mechanisms of the structural evolution of intermediate-mass (M ∼ 4 × 10 10 M ) galaxies since z ∼ 1.

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Section: Large-scale Structure Effectmentioning

confidence: 56%

THE MINOR ROLE OF GAS-RICH MAJOR MERGERS IN THE RISE OF INTERMEDIATE-MASS EARLY TYPES ATz⩽ 1

López-Sanjuan

Balcells

Pérez‐González

et al. 2010

ApJ

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“…Le Fèvre et al 2000;Conselice et al 2003;Lotz et al 2008;Heiderman et al 2009;Jogee et al 2009;Bluck et al 2012). As the morphological selection is sensitive to the imaging quality, merger fraction measurements may be subject to large systematic uncertainties beyond z ∼ 1.…”

Section: B Comparison With Other Merger Fraction Studiesmentioning

confidence: 99%

RESOLVING THE DISCREPANCY OF GALAXY MERGER FRACTION MEASUREMENTS AT z ∼ 0–3

Man

Zirm

Toft

2016

ApJ

137

191

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We measure the merger fraction of massive galaxies using the UltraVISTA/COSMOS Ks-band selected catalog, complemented with the deeper, higher resolution 3DHST+CANDELS catalog selected in the HST /WFC3 H -band, presenting the largest mass-complete photometric merger sample up to z ∼ 3. We find that selecting mergers using the H 160 -band flux ratio leads to an increasing merger fraction with redshift, while selecting mergers using the stellar mass ratio causes a diminishing redshift dependence. Defining major and minor mergers as having stellar mass ratios of 1:1 -4:1 and 4:1 -10:1 respectively, the results imply ∼1 major and 1 minor merger for an average massive (log(M ⋆ /M ⊙ ) 10.8) galaxy during z = 0.1 − 2.5. There may be an additional ∼ 0.5(0.3) major (minor) merger if we use the H-band flux ratio selection. The observed amount of major merging alone is sufficient to explain the observed number density evolution for the very massive (log(M ⋆ /M ⊙ ) 11.1) galaxies. We argue that these very massive galaxies can put on a maximum of 6% of stellar mass in addition to major and minor merging, so that their number density evolution remains consistent with observations. The observed number of major and minor mergers can increase the size of a massive quiescent galaxy by a factor of two at most. This amount of merging is enough to bring the compact quiescent galaxies formed at z > 2 to lie at 1σ below the mean of the stellar mass-size relation as measured in some works (e.g. Newman et al. 2012), but additional mechanisms are needed to fully explain the evolution, and to be consistent with works suggesting stronger evolution (e.g. van der Wel et al. 2014).

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“…For a comparison to intermediate-density cluster environments, we use the study of M09 for the A901/902 cluster system (z ∼ 0.165; n ∼ 1000 galaxies Mpc −3 , see Table 5 in Heiderman et al 2009). To match our sample, we pick S0 galaxies from the M09 study with M V −18, using classifications performed by the members of the STAGES collaboration for the A901/902 cluster system (Gray et al 2009;see Wolf et al 2009 for more .…”

Section: S0 Bar Fraction Across Different Environmentsmentioning

confidence: 99%

THEHST/ACS COMA CLUSTER SURVEY. VIII. BARRED DISK GALAXIES IN THE CORE OF THE COMA CLUSTER

Marinova

Jogee

Weinzirl

et al. 2012

ApJ

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We use high-resolution (∼0. 1) F814W Advanced Camera for Surveys (ACS) images from the Hubble Space Telescope ACS Treasury survey of the Coma cluster at z ∼ 0.02 to study bars in massive disk galaxies (S0s), as well as low-mass dwarf galaxies in the core of the Coma cluster, the densest environment in the nearby universe. Our study helps to constrain the evolution of bars and disks in dense environments and provides a comparison point for studies in lower density environments and at higher redshifts. Our results are: (1) we characterize the fraction and properties of bars in a sample of 32 bright (M V −18, M * > 10 9.5 M ) S0 galaxies, which dominate the population of massive disk galaxies in the Coma core. We find that the measurement of a bar fraction among S0 galaxies must be handled with special care due to the difficulty in separating unbarred S0s from ellipticals, and the potential dilution of the bar signature by light from a relatively large, bright bulge. The results depend sensitively on the method used: the bar fraction for bright S0s in the Coma core is 50% ± 11%, 65% ± 11%, and 60% ± 11% based on three methods of bar detection, namely, strict ellipse fit criteria, relaxed ellipse fit criteria, and visual classification. (2) We compare the S0 bar fraction across different environments (the Coma core, A901/902, and Virgo) adopting the critical step of using matched samples and matched methods in order to ensure robust comparisons. We find that the bar fraction among bright S0 galaxies does not show a statistically significant variation (within the error bars of ±11%) across environments which span two orders of magnitude in galaxy number density (n ∼ 300-10,000 galaxies Mpc −3 ) and include rich and poor clusters, such as the core of Coma, the A901/902 cluster, and Virgo. We speculate that the bar fraction among S0s is not significantly enhanced in rich clusters compared to low-density environments for two reasons. First, S0s in rich clusters are less prone to bar instabilities as they are dynamically heated by harassment and are gas poor as a result of ram pressure stripping and accelerated star formation. Second, high-speed encounters in rich clusters may be less effective than slow, strong encounters in inducing bars. (3) We also take advantage of the high resolution of the ACS (∼50 pc) to analyze a sample of 333 faint (M V > −18) dwarf galaxies in the Coma core. Using visual inspection of unsharp-masked images, we find only 13 galaxies with bar and/or spiral structure. An additional eight galaxies show evidence for an inclined disk. The paucity of disk structures in Coma dwarfs suggests that either disks are not common in these galaxies or that any disks present are too hot to develop instabilities.

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Interacting Galaxies in the A901/902 Supercluster With Stages

Cited by 37 publications

References 96 publications

THE MINOR ROLE OF GAS-RICH MAJOR MERGERS IN THE RISE OF INTERMEDIATE-MASS EARLY TYPES ATz⩽ 1

THE MINOR ROLE OF GAS-RICH MAJOR MERGERS IN THE RISE OF INTERMEDIATE-MASS EARLY TYPES ATz⩽ 1

RESOLVING THE DISCREPANCY OF GALAXY MERGER FRACTION MEASUREMENTS AT z ∼ 0–3

THEHST/ACS COMA CLUSTER SURVEY. VIII. BARRED DISK GALAXIES IN THE CORE OF THE COMA CLUSTER

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