Interventions in Parkinson rsquo s disease  Role of executive function

Mahajan, Abhimanyu; Deal, Jennifer A.

doi:10.2741/4492

Cited by 26 publications

(39 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…An important caveat in this analysis is that when we set a given galaxy to a specific position in the PPS, due to the statistical nature of this association, we introduce a certain variance in the SFH. The fraction of virialized, infall and backsplash galaxies in cells of PPS, as listed by Mahajan et al (2011), represent the probability of recovering a galaxy properly associated to the corresponding cells, namely virial (89%), backsplash (35%) and infall (97%).…”

Section: Star Formation Historymentioning

confidence: 99%

The mass density profile and star formation history of Gaussian and non-Gaussian clusters

Carvalho

Costa

Moura³

et al. 2019

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

This paper is the third of a series in which we investigate the discrimination between Gaussian (G) and Non-Gaussian (NG) clusters, based on the velocity distribution of the member galaxies. We study a sample of 177 groups from the Yang catalog in the redshift interval of 0.03 ≤ z ≤ 0.1 and masses ≥ 10 14 M . Examining the projected stellar mass density distributions of G and NG groups we find strong evidence of a higher infall rate in the outskirts of NG groups over the G ones. There is a 61% excess of faint galaxies in NGs when contrasted with G groups, when integrating from 0.8 to 2.0R/R 200 . The study of the Star Formation History (SFH) of ellipticals and spirals in the three main regions of the Projected Phase Space (PPS) reveals also that the star formation in faint spirals of NG groups is significantly different from their counterpart in the G groups. The assembled mass for Faint spirals varies from 59% at 12.7 Gyr to 75% at 8.0 Gyr, while in G systems this variation is from 82% to 91%. This finding may also be interpreted as a higher infall rate of gas rich systems in NG groups. This accretion process through the filaments, disturbing the velocity distribution and modifying not only the stellar population of the incoming galaxies but also their SFH, should be seriously considered in modelling galaxy evolution.

show abstract

Section: Star Formation Historymentioning

confidence: 99%

The mass density profile and star formation history of Gaussian and non-Gaussian clusters

Carvalho

Costa

Moura³

et al. 2019

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

show abstract

“…The galaxies that fell into the cluster several gigayears ago are located in the regions of lower relative velocities. The PPS diagram turned out to be an efficient tool to map the galaxy evolution inside a cluster and, in particular, to study the star formation history (Mahajan et al 2011;Muzzin et al 2014) and the effect of the ram-pressure stripping (e.g. Hernández-Fernández et al 2014;Jaffé et al 2015;Yoon et al 2017;Jaffé et al 2018).…”

Section: Introductionmentioning

confidence: 99%

The Fornax3D project: Tracing the assembly history of the cluster from the kinematic and line-strength maps

Iodice

Sarzi

Bittner

et al. 2019

A&A

186

View full text Add to dashboard Cite

The 31 brightest galaxies (m B ≤ 15 mag) inside the virial radius of the Fornax cluster were observed from the centres to the outskirts with the Multi Unit Spectroscopic Explorer on the Very Large Telescope. These observations provide detailed high-resolution maps of the line-of-sight kinematics and line strengths of the stars and ionised gas reaching 2-3 R e for 21 early-type galaxies and 1-2 R e for 10 late-type galaxies. The majority of the galaxies are regular rotators, with eight hosting a kinematically distinct core. Only two galaxies are slow rotators. The mean age, total metallicity, and [Mg/Fe] abundance ratio in the bright central region inside 0.5R e and in the galaxy outskirts are presented. Extended emission-line gas is detected in 13 galaxies, most of them are late-type objects with wide-spread star formation. The measured structural properties are analysed in relation to the galaxies' position in the projected phase space of the cluster. This shows that the Fornax cluster appears to consist of three main groups of galaxies inside the virial radius: the old core; a clump of galaxies, which is aligned with the local large-scale structure and was accreted soon after the formation of the core; and a group of galaxies that fell in more recently.

show abstract

“…To infer the physical processes occurring during the infall, the distribution often associated with galaxies' properties is used to connect the properties with galaxies' orbital states. Examples include quenching of galaxies (Mahajan et al 2011;Oman & Hudson 2016), gas stripping because of ram pressure (Hernández-Fernández et al 2014;Jaffé et al 2015Jaffé et al , 2018Yoon et al 2017), and the assembly history of infalling satellites/groups (Oman et al 2013;Lisker et al 2018;Einasto et al 2018a,b;Adhikari et al 2019). In particular, calculated the mean values of the time since infall (TSI) of the populations of observed galaxies in different zones in a projected phase space, and then studied how their observed mean properties (such as sSFR, age, and metallicity) correlate with their mean TSI (see also Smith et al 2019) We instead divide a projected phase-space diagram into a grid of pixels.…”

Section: Introductionmentioning

confidence: 99%

YZiCS: Unveiling the Quenching History of Cluster Galaxies Using Phase-space Analysis

Rhee

Smith

Choi

et al. 2020

ApJS

View full text Add to dashboard Cite

We used the time since infall (TSI) of galaxies, obtained from the Yonsei Zoom-in Cluster Simulation, and the star formation rate (SFR) from the Sloan Digital Sky Survey (SDSS) Data Release 10 to study how quickly star formation of disk galaxies is quenched in cluster environments. We first confirm that both simulated and observed galaxies are consistently distributed in phase space. We then hypothesize that the TSI and SFR are causally connected; thus, both the TSI and SFR of galaxies at each position of phase space can be associated through abundance matching. Using a flexible model, we derive the star formation history (SFH) of cluster galaxies that best reproduces the relationship between the TSI and SFR at z ∼ 0.08. According to this SFH, we find that the galaxies with M * > 10 9.5 M generally follow the so-called "delayed-then-rapid" quenching pattern. Our main results are as following: (i) Part of the quenching takes place outside clusters through mass quenching and pre-processing. The e-folding timescale of this "ex-situ quenching phase" is roughly 3 Gyr with a strong inverse mass dependence. (ii) The pace of quenching is maintained roughly for 2 Gyr ("delay time") during the first crossing time into the cluster. During the delay time, quenching remains gentle probably because gas loss happens primarily on hot and neutral gases. (iii) Quenching becomes more dramatic (e-folding timescale of roughly 1 Gyr) after delay time, probably because ram pressure stripping is strongest near the cluster center. Counter-intuitively, more massive galaxies show shorter quenching timescales mainly because they enter their clusters with lower gas fractions due to ex-situ quenching.

show abstract

Interventions in Parkinson rsquo s disease Role of executive function

Cited by 26 publications

References 40 publications

The mass density profile and star formation history of Gaussian and non-Gaussian clusters

The mass density profile and star formation history of Gaussian and non-Gaussian clusters

The Fornax3D project: Tracing the assembly history of the cluster from the kinematic and line-strength maps

YZiCS: Unveiling the Quenching History of Cluster Galaxies Using Phase-space Analysis

Contact Info

Product

Resources

About