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In this work we present scanning Fabry-Perot H$alpha$ observations of the isolated interacting galaxy pair NGC 5278/79 obtained with the PUMA Fabry-Perot interferometer. We derived velocity fields, various kinematic parameters and rotation curves for both galaxies. Our kinematical results together with the fact that dust lanes have been detected in both galaxies, as well as the analysis of surface brightness profiles along the minor axis, allowed us to determine that both components of the interacting pair are trailing spirals.
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In this work we present scanning Fabry-Perot H$alpha$ observations of the isolated interacting galaxy pair NGC 5278/79 obtained with the PUMA Fabry-Perot interferometer. We derived velocity fields and rotation curves for both galaxies. For NGC 5278 we also obtained the residual velocity map to investigate the non-circular motions, and estimated its mass by fitting the rotation curve with a disk+halo components. We test three different types of halo (pseudo-isothermal, Hernquist and Navarro Frenk White) and obtain satisfactory fits to the rotation curve for all profiles. The amount of dark matter required by pseudo-isothermal profile is about ten times smaller than, that for the other two halo distributions. Finally, our kinematical results together with the analysis of dust lanes distribution and of surface brightness profiles along the minor axis allowed us to determine univocally that both components of the interacting pair are trailing spirals.
In optical images, the not amply studied isolated interacting galaxy pair KPG 486 (NGC 6090) displays similar features to the galaxy pair The Antennae (NGC 4038/39). To compare the distribution of ionized hydrogen gas, morphology and kinematic and dynamic behaviour between both galaxy pairs, we present observations in the H$alpha$ emission line of NGC 6090 acquired with the scanning Fabry-Perot interferometer, PUMA. For each galaxy in NGC 6090 we obtained several kinematic parameters, its velocity field and its rotation curve, we also analysed some of the perturbations induced by their encounter. We verified the consistency of our results by comparing them with kinematic results from the literature. The comparison of our results on NGC 6090 with those obtained in a previous similar kinematic analysis made for The Antennae highlighted great differences between these galaxy pairs.
The central regions of cool-core galaxy clusters harbour multiphase gas with temperatures ranging from $10 mathrm{K}$--$10^7 mathrm{K}$. Feedback from AGN jets prevents the gas from undergoing a catastrophic cooling flow. However, the exact mechanism of this feedback energy input is unknown, mainly due to the lack of velocity measurements of the hot phase gas, which has large thermal velocities. However, recent observations have measured the velocity structure functions ($mathrm{VSF}$s) of the cooler phases (at $10 mathrm{K}$ and $10^4 mathrm{K}$) and used them to indirectly estimate the motions of the hot phase. In the first part of this study, we conduct high-resolution ($384^3$--$1536^3$ resolution elements) simulations of homogeneous isotropic subsonic turbulence, without radiative cooling. We analyse the second-order velocity structure functions ($mathrm{VSF}_2$) in these simulations and study the effects of varying spatial resolution, the introduction of magnetic fields and the effect of line of sight (LOS) projection on the $mathrm{VSF}_2$. In the second part of the study, we analyse high-resolution ($768^3$ resolution elements) idealised simulations of multiphase turbulence in the intracluster medium (ICM) from Mohapatra et al 2021. We compare $mathrm{VSF}_2$ for both the hot ($Tsim10^7 mathrm{K}$) and cold ($Tsim10^4 mathrm{K}$) phases. We also look for the effect of LOS projection. For turbulence without radiative cooling, we observe a steepening in the slopes of the $mathrm{VSF}_2$ upon projection. In our runs with radiative cooling and multiphase gas, we find that the $mathrm{VSF}_2$ of the hot and cold phases have similar scaling, but introducing magnetic fields steepens the $mathrm{VSF}_2$ of the cold phase only. We also find that projection along the LOS steepens the $mathrm{VSF}_2$ for the hot phase and mostly flattens it for the cold phase.
This is the second part of an H-alpha kinematics follow-up survey of the Spitzer Infrared Nearby Galaxies Survey (SINGS) sample. The aim of this program is to shed new light on the role of baryons and their kinematics and on the dark/luminous matter relation in the star forming regions of galaxies, in relation with studies at other wavelengths. The data for 37 galaxies are presented. The observations were made using Fabry-Perot interferometry with the photon-counting camera FaNTOmM on 4 different telescopes, namely the Canada-France-Hawaii 3.6m, the ESO La Silla 3.6m, the William Herschel 4.2m, and the Observatoire du mont Megantic 1.6m telescopes. The velocity fields are computed using custom IDL routines designed for an optimal use of the data. The kinematical parameters and rotation curves are derived using the GIPSY software. It is shown that non-circular motions associated with galactic bars affect the kinematical parameters fitting and the velocity gradient of the rotation curves. This leads to incorrect determinations of the baryonic and dark matter distributions in the mass models derived from those rotation curves.
The impact of ram pressure stripping (RPS) on galaxy evolution has been studied for over forty years. Recent multi-wavelength data have revealed many examples of galaxies undergoing RPS, often accompanied with multi-phase tails. As energy transfer in the multi-phase medium is an outstanding question in astrophysics, RPS galaxies are great objects to study. Despite the recent burst of observational evidence, the relationship between gas in different phases in the RPS tails is poorly known. Here we report, for the first time, a strong linear correlation between the X-ray surface brightness (SB$_{rm X}$) and the H$alpha$ surface brightness (SB$_{rm Halpha}$) of the diffuse gas in the RPS tails at $sim$ 10 kpc scales, as SB$_{rm X}$/SB$_{rm Halpha} sim$ 3.6. This discovery supports the mixing of the stripped interstellar medium (ISM) with the hot intracluster medium (ICM) as the origin of the multi-phase RPS tails. The established relation in stripped tails, also in comparison with the likely similar correlation in similar environments like X-ray cool cores and galactic winds, provides an important test for models of energy transfer in the multi-phase gas. It also indicates the importance of the H$alpha$ data for our understanding of the ICM clumping and turbulence.
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