2D kinematic study of the central region of NGC 4501

Abstract

GMOS-IFU observational data were used to study the detailed two dimensional gas kinematics and morphological structures within the ∼ 500 × 421 pc 2 of the active Seyfert 2 galaxy NGC 4501. We provide empirical evidences of possible outflowing material from the central zones of NGC 4501 to the observer. In addition, we performed a spectral synthesis and diagnostic diagram analysis to determine respectively the dominant stellar population in the inner disc of this galaxy and to unveil the actual nature of the central engine of NGC 4501. The principal finding of this work is that the central regions of NGC 4501 are dominated by non circular motions connected to probable outflows of matter from the nuclear regions of this galaxy. A predominant old stellar population inhabits the internal zones of NGC 4501 excluding the possibility of ongoing starburst activity in the central parsecs of this galaxy. The latter result is confirmed by the diagnostic diagram analysis that establishes a preponderant active galactic nucleus character for NGC 4501. These outcomes together provide a general description of the gas motion and the corresponding nuclear activity in the internal disc of NGC 4501 in an attempt to elucidate the possible relation among the central activity and the induced kinematic properties of this nearby galaxy.

VPLanet: The Virtual Planet Simulator

“…STELLAR computes the XUV luminosity according to the product of the luminosity and Eq. (J1) for stars that drive atmospheric escape and water loss (see § 3; Luger & Barnes 2015) Furthermore, STELLAR allows the user to model the long-term angular momentum evolution of low-mass stars using one of three magnetic braking models (Reiners & Mohanty 2012;Repetto & Nelemans 2014;Matt et al 2015Matt et al , 2019. Here, we demonstrate the modeling capabilities of STELLAR, while in the App.…”

“…In addition to tracking the evolution of fundamental stellar properties, STELLAR models the angular momentum evolution of stars undergoing stellar evolution, e.g., radius contrac-tion, and angular momentum loss due to magnetic braking. We allow the user to model magnetic braking using three different prescriptions from Reiners & Mohanty (2012), Repetto & Nelemans (2014), and Matt et al (2015), with the latter including the corrections of Matt et al (2019).…”

“…In this model, the dichotomy between unsaturated (ω < ω crit ) and saturated (ω ≥ ω crit ) assumes that for fast enough rotation rates, i.e., the stars in the "saturated" regime, the stellar magnetic field strength is constant, whereas in the unsaturated regime, the stellar magnetic field strength depends on the rotation rate. The Repetto & Nelemans (2014) model is simply based off of the observed spin-down of Sun-like stars by Skumanich (1972) and is given by…”

“…Crustal heat sources have been excluded because they do not contribute to the mantle heat budget. Note that heat can be released from the mantle in two Repetto & Nelemans (2014) magnetic braking models. Initially as the stars contract along the pre-main sequence, the rotation periods decrease via conservation of angular momentum.…”

Neutrino Emission as Diagnostics of Core-Collapse Supernovae

“…The astrophysical implications of a timed observation of black-hole formation might be even broader. Simulations (121) as well as observational evidence from the composition of metal-poor stars (148) and of companions in HMXBs HMXB: High-mass X-ray binary (149), and from the kinematics of some HMXBs (149,150) suggest that black hole formation can sometimes occur after shock revival due to fallback. A cut-off in the neutrino flux together with an explosion of sufficient energy would be a direct proof for this scenario.…”