AGN host galaxies at redshift<i>z</i> ≈  0.7: peculiar or not?

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

doi:10.1051/0004-6361/201015444

Cited by 48 publications

(47 citation statements)

References 56 publications

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“…For a negligible central point source, we found a typical systematic error of 20 % on galaxy sizes (see Fig. 7d in Böhm et al 2013). This value hence represents the systematic size error for galaxies with the light profiles of pure disks or disks with only weak bulges; this is the case for the vast majority of galaxies in our sample.…”

Section: Structural Parametersmentioning

confidence: 74%

“…These are very small (<1 %) throughout our sample. To gain a more realistic estimate of the systematic errors on r d , we relied on our own previous analysis of HST/ACS images using GALFIT in Böhm et al (2013). In that work, we investigated the effect of an active galactic nucleus on the morphologies of host galaxies at redshifts 0.5 < z < 1.1 as quantified with GAL-FIT.…”

Section: Structural Parametersmentioning

confidence: 99%

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Disk galaxy scaling relations at intermediate redshifts

Boehm¹,

Ziegler²

2016

A&A

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Aims. Galaxy scaling relations such as the Tully-Fisher relation (between the maximum rotation velocity V max and luminosity) and the velocity-size relation (between V max and the disk scale length) are powerful tools to quantify the evolution of disk galaxies with cosmic time. Methods. We took spatially resolved slit spectra of 261 field disk galaxies at redshifts up to z ≈ 1 using the FORS instruments of the ESO Very Large Telescope. The targets were selected from the FORS Deep Field and William Herschel Deep Field. Our spectroscopy was complemented with HST/ACS imaging in the F814W filter. We analyzed the ionized gas kinematics by extracting rotation curves from the two-dimensional spectra. Taking into account all geometrical, observational, and instrumental effects, these rotation curves were used to derive the intrinsic V max .Results. Neglecting galaxies with disturbed kinematics or insufficient spatial rotation curve extent, V max was reliably determined for 124 galaxies covering redshifts 0.05 < z < 0.97. This is one of the largest kinematic samples of distant disk galaxies to date. We compared this data set to the local B-band Tully-Fisher relation and the local velocity-size relation. The scatter in both scaling relations is a factor of ∼2 larger at z ≈ 0.5 than at z ≈ 0. The deviations of individual distant galaxies from the local Tully-Fisher relation are systematic in the sense that the galaxies are increasingly overluminous toward higher redshifts, corresponding to an overluminosity ∆M B = −(1.2 ± 0.5) mag at z = 1. This luminosity evolution at given V max is probably driven by younger stellar populations of distant galaxies with respect to their local counterparts, potentially combined with modest changes in dark matter mass fractions. The analysis of the velocity-size relation reveals that disk galaxies of a given V max have grown in size by a factor of ∼1.5 over the past ∼8 Gyr, most likely through accretion of cold gas and/or small satellites. From scrutinizing the combined evolution in luminosity and size, we find that the galaxies that show the strongest evolution toward smaller sizes at z ≈ 1 are not those that feature the strongest evolution in luminosity, and vice versa.

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Section: Structural Parametersmentioning

confidence: 74%

Section: Structural Parametersmentioning

confidence: 99%

Disk galaxy scaling relations at intermediate redshifts

Boehm¹,

Ziegler²

2016

A&A

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“…06−0. 09) (Böhm et al 2013). Figure 13 (left panel) shows the rotation-curve asymmetry A vs. the morphological asymmetry A morph for cluster and field galaxies.…”

Section: Influence Of Environmentmentioning

confidence: 99%

Ram pressure and dusty red galaxies – key factors in the evolution of the multiple cluster system Abell 901/902

Bösch

Böhm

Wolf

et al. 2013

A&A

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Aims. We present spectroscopic observations of 182 disk galaxies (96 in the cluster and 86 in the field environment) in the region of the Abell 901/902 multiple cluster system, which is located at a redshift of z ∼ 0.165. We estimate dynamical parameters of the four subclusters and analyse the kinematics of spiral galaxies, searching for indications of ram-pressure stripping. Furthermore, we focus on dusty red galaxies as a possible intermediate stage in the transformation of field galaxies to lenticulars when falling into the cluster. Methods. We obtained multi-object slit spectroscopy using the VLT instrument VIMOS. We carried out a redshift analysis, determined velocity dispersions using biweight statistics, and detected possible substructures with the Dressler-Shectman test. We exploited rotation curves from emission lines to analyse distortions in the gaseous disk of a galaxy, as well as HST/ACS images to quantify the morphological distortions of the stellar disk. Results. The presence of substructures and non-Gaussian redshift distributions indicate that the cluster system is dynamically young and not in a virialised state. We find evidence of two important galaxy populations. Morphologically distorted galaxies are probably subject to increased tidal interactions. They show pronounced rotation-curve asymmetries at intermediate cluster-centric radii and low rest-frame peculiar velocities. Morphologically undistorted galaxies show the strongest rotation-curve asymmetries at high rest-frame velocities and low cluster-centric radii. Supposedly, this group is strongly affected by ram-pressure stripping due to interaction with the intra-cluster medium. Among the morphologically undistorted galaxies, dusty red galaxies have particularly strong rotation-curve asymmetries, suggesting that ram pressure is an important factor in these galaxies. Furthermore, dusty red galaxies have on average a bulge-to-total ratio that is higher by a factor of two than cluster blue-cloud and field galaxies. The fraction of kinematically distorted galaxies is 75% higher in the cluster than in the field environment. This difference mainly stems from morphologically undistorted galaxies, indicating a cluster-specific interaction process that only affects the gas kinematics but not the stellar morphology. Also the ratio between gas and stellar scale length is reduced for cluster galaxies compared to the field sample. Both findings could be explained best by ram-pressure effects. Conclusions. Ram-pressure stripping seems to be an important interaction process in the multiple cluster system A901/902. Dusty red galaxies might be a crucial element in understanding the transformation of field disk galaxies into cluster lenticular galaxies.

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“…However, several studies claimed to find no significant excess of mergers in AGN hosts (Dunlop et al 2003;Sanchez et al 2004b;Grogin et al 2005;Li et al 2008;Gabor et al 2009;Tal et al 2009;Cisternas et al 2011;Kocevski et al 2012;Schawinski et al 2012;Bohm et al 2013). These studies report that a significant fraction of AGNs appear to reside in isolated disk-dominated galaxies for which internal processes are likely responsible for fueling their active nuclei.…”

Section: Introductionmentioning

confidence: 98%

Galaxy And Mass Assembly (GAMA): A “No Smoking” Zone for Giant Elliptical Galaxies?

Khosroshahi

Raouf

Miraghaei

et al. 2017

ApJ

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We study the radio emission of the most massive galaxies in a sample of dynamically relaxed and unrelaxed galaxy groups from the Galaxy and Mass Assembly survey. The dynamical state of the group is defined by the stellar dominance of the brightest group galaxy (BGG), e.g., the luminosity gap between the two most luminous members, and the offset between the position of the BGG and the luminosity centroid of the group. We find that the radio luminosity of the largest galaxy in the group strongly depends on its environment, such that the BGGs in dynamically young (evolving) groups are an order of magnitude more luminous in the radio than those with a similar stellar mass but residing in dynamically old (relaxed) groups. This observation has been successfully reproduced by a newly developed semi-analytic model that allows us to explore the various causes of these findings. We find that the fraction of radio-loud BGGs in the observed dynamically young groups is ∼2 times that of the dynamically old groups. We discuss the implications of this observational constraint on the central galaxy properties in the context of galaxy mergers and the super massive black hole accretion rate.

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AGN host galaxies at redshiftz ≈ 0.7: peculiar or not?

Cited by 48 publications

References 56 publications

Disk galaxy scaling relations at intermediate redshifts

Disk galaxy scaling relations at intermediate redshifts

Ram pressure and dusty red galaxies – key factors in the evolution of the multiple cluster system Abell 901/902

Galaxy And Mass Assembly (GAMA): A “No Smoking” Zone for Giant Elliptical Galaxies?

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