Searching for environmental effects on galaxy kinematics in groups and clusters at<i>z</i>∼ 1 from the ORELSE survey

Pelliccia, Debora; Lemaux, B. C.; Tomczak, Adam; Lubin, Lori M.; Shen, Lu; Épinat, B.; Wu, Po-Feng; Gal, R. R.; Rumbaugh, N.; Kocevski, Dale D.; Tresse, L.; Squires, G.

doi:10.1093/mnras/sty2876

Cited by 23 publications

(70 citation statements)

References 120 publications

(224 reference statements)

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“…We adopt the correlation of M BH with bulge mass M bulge following equation 10 in Kormendy & Ho (2013) to estimate M BH and assume a bulge-to-total stellar mass ratio of 0.3 for galaxies log(M * )< 11 and 0.4 for log(M * )≥ 11 found in Lang et al (2014), which were derived from a star forming galaxy population selected in UVJ colour-colour diagram at 0.5 < z < 2.5. We confirm this ratio on average (mean) equal to 0.3 with a standard deviation of 0.3 using 142 galaxies in the ORELSE survey that occupy the star-forming region of the NUVrJ colour-colour diagram and have stellar mass in a range of 8.3<log(M * )<11 and median at 9.7 (Pelliccia et al 2019) 2 . We estimated the median L Edd for each bin in the low-and high-f AGN sub-samples binning by log(sSFR) as shown in the left panel of Figure 5.…”

Section: Estimating the States Of The Agnsupporting

confidence: 68%

The properties of radio and mid-infrared detected galaxies and the effect of environment on the co-evolution of AGN and star formation at z ∼ 1

Shen

Lemaux

Lubin

et al. 2020

Monthly Notices of the Royal Astronomical Society

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In this study we investigate 179 radio-IR galaxies drawn from a sample of spectroscopically-confirmed galaxies that are detected in radio and mid-infrared (MIR) in the redshift range of 0.55 ≤ z ≤ 1.30 in the Observations of Redshift Evolution in Large Scale Environments (ORELSE) survey. We constrain the Active Galactic Nuclei (AGN) contribution in the total IR luminosity (f AGN ), and estimate the AGN luminosity (L AGN ) and the star formation rate (SFR) using the CIGALE Spectral Energy Distribution (SED) fitting routine. Based on the f AGN and radio luminosity, radio-IR galaxies are split into: galaxies that host either high or low f AGN AGN (high-/lowf AGN ), and star forming galaxies with little to no AGN activity (SFGs). We study the colour, stellar mass, radio luminosity, L AGN and SFR properties of the three radio-IR sub-samples, comparing to a spec-IR sample drawn from spectroscopically-confirmed galaxies that are also detected in MIR. No significant difference between radio luminosity of these sub-samples was found, which could be due to the combined contribution of radio emission from AGN and star formation. We find a positive relationship between L AGN and specific SFR (sSFR) for both AGN sub-samples, strongly suggesting a co-evolution scenario of AGN and SF in these galaxies. A toy model is designed to demonstrate this co-evolution scenario, where we find that, in almost all cases, a rapid quenching timescale is required, which we argue is a signature of AGN quenching. The environmental preference for intermediate/infall regions of clusters/groups remains across the co-evolution scenario, which suggests that galaxies might be in an orbital motion around the cluster/group during the scenario.

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Section: Estimating the States Of The Agnsupporting

confidence: 68%

The properties of radio and mid-infrared detected galaxies and the effect of environment on the co-evolution of AGN and star formation at z ∼ 1

Shen

Lemaux

Lubin

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Our aim is to study the impact of environment on the TFR by comparing this relation obtained for the MAGIC group sample to the one derived for other samples of either field (KMOS3D, Übler et al 2017;KROSS, Tiley et al 2019) or cluster (ORELSE, Pelliccia et al 2019) galaxies over a similar redshift range. The whole KMOS3D sample covers a wider redshift range.…”

Section: Stellar and Baryonic Mass Tully-fisher Relationsmentioning

confidence: 97%

“…Some studies have, however, targeted a few dozen galaxies in groups and (proto-)clusters at intermediate redshift with KMOS and FORS2 (e.g., Sobral et al 2013;Pérez-Martínez et al 2017;Böhm et al 2020). So far, the most complete study of the TFR as a function of environment has been performed from long-slit spectroscopy observations by Pelliccia et al (2019), using a sample of 94 galaxies at z ∼ 1, a fraction of which were members of clusters. They do not report significant modification of the TFR with environment.…”

Section: Introductionmentioning

confidence: 99%

The Tully-Fisher relation in dense groups at z ∼ 0.7 in the MAGIC survey

Abril-Melgarejo

Épinat

Mercier

et al. 2021

A&A

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Context. Galaxies in dense environments are subject to interactions and mechanisms that directly affect their evolution by lowering their gas fractions and consequently reducing their star-forming capacity earlier than their isolated counterparts. Aims. The aim of our project is to get new insights into the role of environment in the stellar and baryonic content of galaxies using a kinematic approach, through the study of the Tully-Fisher relation (TFR). Methods. We study a sample of galaxies in eight groups, over-dense by a factor larger than 25 with respect to the average projected density, spanning a redshift range of 0.5 < z < 0.8 and located in ten pointings of the MAGIC MUSE Guaranteed Time Observations program. We perform a morpho-kinematics analysis of this sample and set up a selection based on galaxy size, [O II]λλ3727,3729 emission line doublet signal-to-noise ratio, bulge-to-disk ratio, and nuclear activity to construct a robust kinematic sample of 67 star-forming galaxies. Results. We show that this selection considerably reduces the number of outliers in the TFR, which are predominantly dispersion-dominated galaxies. Similar to other studies, we find that including the velocity dispersion in the velocity budget mainly affects galaxies with low rotation velocities, reduces the scatter in the relation, increases its slope, and decreases its zero-point. Including gas masses is more significant for low-mass galaxies due to a larger gas fraction, and thus decreases the slope and increases the zero-point of the relation. Our results suggest a significant offset of the TFR zero-point between galaxies in low- and high-density environments, regardless of the kinematics estimator used. This can be interpreted as a decrease in either stellar mass by ∼0.05 − 0.3 dex or an increase in rotation velocity by ∼0.02 − 0.06 dex for galaxies in groups, depending on the samples used for comparison. We also studied the stellar and baryon mass fractions within stellar disks and found they both increase with stellar mass, the trend being more pronounced for the stellar component alone. These fractions do not exceed 50%. We show that this evolution of the TFR is consistent either with a decrease in star formation or with a contraction of the mass distribution due to the environment. These two effects probably act together, with their relative contribution depending on the mass regime.

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“…If for a given galaxy, no cluster/group within ±6000 km s −1 are found, the parent structure is the one with the smallest η. See Shen et al (2019) and Pelliccia et al (2019) for more details on this calculation. Here, we discuss all possible uncertainties on the global environment measurement.…”

Section: Appendix a The Uncertainty Of Global Environment Measurementmentioning

confidence: 99%

Extended Radio AGN at z ∼ 1 in the ORELSE Survey: The Confining Effect of Dense Environments

Shen

Liu

Zhang

et al. 2020

ApJ

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Recent hydrodynamic simulations and observations of radio jets have shown that the surrounding environment has a large effect on their resulting morphology. To investigate this, we use a sample of 50 Extended Radio Active Galactic Nuclei (ERAGN) detected in the Observations of Redshift Evolution in Large-Scale Environments survey. These sources are all successfully cross-identified to galaxies within a redshift range of 0.55z1.35, either through spectroscopic redshifts or accurate photometric redshifts. We find that ERAGN are more compact in high-density environments than those in low-density environments at a significance level of 4.5σ. Among a series of internal properties under our scrutiny, only the radio power demonstrates a positive correlation with their spatial extent. After removing the possible radio power effect, the difference of size in low-and high-density environments persists. In the global environment analyses, the majority (86%) of high-density ERAGN reside in the cluster/group environment. In addition, ERAGN in the cluster/group central regions are preferentially compact with a small scatter in size, compared to those in the cluster/group intermediate regions and fields. In conclusion, our data appear to support the interpretation that the dense intracluster gas in the central regions of galaxy clusters plays a major role in confining the spatial extent of radio jets. Unified Astronomy Thesaurus concepts: Radio active galactic nuclei (2134); Radio galaxies (1343); Galaxy clusters (584); Radio jets (1347)

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Searching for environmental effects on galaxy kinematics in groups and clusters atz∼ 1 from the ORELSE survey

Cited by 23 publications

References 120 publications

The properties of radio and mid-infrared detected galaxies and the effect of environment on the co-evolution of AGN and star formation at z ∼ 1

The properties of radio and mid-infrared detected galaxies and the effect of environment on the co-evolution of AGN and star formation at z ∼ 1

The Tully-Fisher relation in dense groups at z ∼ 0.7 in the MAGIC survey

Extended Radio AGN at z ∼ 1 in the ORELSE Survey: The Confining Effect of Dense Environments

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