Hα KINEMATICS OF THE ISOLATED INTERACTING GALAXY PAIR KPG 486 (NGC 6090)

Sardaneta, M. M.; Rosado, M.; Sánchez-Cruces, M.

doi:10.22201/ia.01851101p.2020.56.01.09

Cited by 3 publications

(7 citation statements)

References 52 publications

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“…where r and θ are the radial and angular coordinates in the plane of the galaxy (Mihalas & Binney 1981) and V LoS (r, θ) is the LoS velocity extracted from each pixel of the FP velocity field (e.g. Fuentes-Carrera et al 2004;Epinat et al 2008a;Cárdenas-Martínez & Fuentes-Carrera 2018;Sardaneta et al 2020). This method has been used for the PUMA and GHASP datasets; the results are shown by the black filled and open squares in Fig.…”

Section: B2 the Intensity-peak Methodsmentioning

confidence: 99%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Sardaneta

Amram

Boselli

et al. 2022

A&A

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Using the VESTIGE survey, a deep narrow-band Hα imaging survey of the Virgo cluster carried out at the CFHT with MegaCam, we discovered a long and diffuse tail of ionised gas in the edge-on late-type galaxy NGC 4330. This peculiar feature indicates an ongoing ram pressure stripping event able to remove the gas in the outer region of the disc. Tuned hydrodynamic simulations suggest that the ram pressure stripping event is occurring almost face-on, making NGC 4330 the ideal candidate for studying the effects of the perturbation in the direction perpendicular to the disc plane. We present here two new independent sets of Fabry-Perot observations (R ≃ 10 000) with the purpose of understanding the effects of the ram pressure stripping process on the kinematics of the ionised gas. Despite their limited sensitivity to the diffuse gas emission, the data allowed us to measure the velocity and the velocity dispersion fields over the galaxy disc and in several features at the edges or outside the stellar disc formed after the ram pressure stripping event. We constructed the position-velocity diagrams and the rotation curves of the galaxy using three different techniques. The data show, consistent with the hydrodynamic simulations, that the galaxy has an inner solid-body rotation up to ∼2.4 kpc, with non-circular streaming motions outside this radius and in the several external features formed during the interaction of the galaxy with the surrounding intracluster medium. The data also indicate a decrease in the rotational velocity of the gas with increasing distance from the galaxy disc along the tails, suggesting a gradual but not linear loss of angular momentum in the stripped gas. Consistent with a ram pressure stripping scenario, the i-band image shows a boxy shape at the south-west edge of the disc, where the stellar orbits might have been perturbed by the modification of the gravitational potential well of the galaxy due to the displacement of the gas in the z direction.

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Section: B2 the Intensity-peak Methodsmentioning

confidence: 99%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Sardaneta

Amram

Boselli

et al. 2022

A&A

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“…Measuring the FWHM of the calibration arc lamp lines, we obtain R ≈ 5300 as the final resolving power (or v FWHM = 57 km s −1 ) of the PMAS data at the observed wavelength of Hα. Other Hα kinematics observations of eLARS01 can be found in Sardaneta et al (2020).…”

Section: Pmas Datamentioning

confidence: 99%

LARS XIII: High Angular Resolution 21 cm H i Observations of Lyα Emitting Galaxies

Reste

Hayes

Cannon

et al. 2022

ApJ

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The Lyα emission line is one of the main observables of galaxies at high redshift, but its output depends strongly on the neutral gas distribution and kinematics around the star-forming regions where UV photons are produced. We present observations of Lyα and 21 cm H i emission at comparable scales with the goal to qualitatively investigate how the neutral interstellar medium (ISM) properties impact Lyα transfer in galaxies. We have observed 21 cm H i at the highest possible angular resolution (≈3″ beam) with the Very Large Array in two local galaxies from the Lyman Alpha Reference Sample. We compare these data with Hubble Space Telescope Lyα imaging and spectroscopy, and Multi Unit Spectroscopic Explorer and Potsdam MultiAperture Spectrophotometer ionized gas observations. In LARS08, high-intensity Lyα emission is cospatial with high column density H i where the dust content is the lowest. The Lyα line is strongly redshifted, consistent with a velocity redistribution that allows Lyα escape from a high column density neutral medium with a low dust content. In eLARS01, high-intensity Lyα emission is located in regions of low column density H i, below the H i data sensitivity limit ( < 2 × 1020 cm−2). The perturbed ISM distribution with low column density gas in front of the Lyα emission region plays an important role in the escape. In both galaxies, the faint Lyα emission (∼1×10−16 erg s−1cm−2 arcsec−2) traces intermediate Hα emission regions where H i is found, regardless of the dust content. Dust seems to modulate, but not prevent, the formation of a faint Lyα halo. This study suggests the existence of scaling relations between dust, Hα, H i, and Lyα emission in galaxies.

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“…However, we attempted nonetheless to derive a RC from the Hα line VF of the galaxy following the methodology in Amram et al (1996); Fuentes-Carrera et al ( 2004); Sardaneta et al (2020) taking into consideration the detection of multiple velocity components in the inner parts of the galaxy; in particular, those found in the 'O' region and discussed in Section 3.1.1.…”

Section: Rc Computationmentioning

confidence: 99%

“…The procedure to compute the RC with ADHOCw is done manually in an iterative manner where the initial parameters are manually modified in order to obtain a RC with low dispersion values and as symmetric as possible when the approaching and receding sides are superposed (e.g. Amram et al 1992Amram et al , 1996Fuentes-Carrera et al 2004;Repetto et al 2010b;Sardaneta et al 2020). Usually in the case of isolated spiral galaxies, one of the requirements to derive the RC is for the inner parts on each side of the RC (receding and approaching velocities) to superpose, since the velocity fields are smooth and symmetrical resulting in symmetric and low-scattered rotation curves (Amram et al 1996).…”

Section: Rc Computationmentioning

confidence: 99%

“…With high resolution FP interferometry data it is possible to study the kinematics of Galactic and extragalactic SNRs obtaining the SNR expansion velocity, the energy deposited in the ISM by the SN explosion and the age of the SNR considering its evolutionary stage (see, Rosado 1981Rosado , 1982Rosado et al 1996;Ambrocio-Cruz et al 2014;Sánchez-Cruces et al 2018). In addition, FP data allows us to study the global kinematics of galaxies (Fuentes-Carrera et al 2019;Gómez-López et al 2019;Sardaneta et al 2020) and their regions with particular physical features such as perturbations induced by interactions (Fuentes-Carrera et al 2004;Repetto et al 2010b) or regions with a high star formation rate (SFR, see Cárdenas-Martínez & Fuentes-Carrera 2018). Thus, the kinematical method complements the classic optical method of SNR detection, as well as radio and X-ray observations by helping identify SNRs inside bright HII regions.…”

Section: Introductionmentioning

confidence: 99%

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A kinematical study of the dwarf irregular galaxy NGC 1569 and its supernova remnants

Sánchez-Cruces

Sardaneta

Fuentes-Carrera

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present Fabry-Pérot observations in the Hα and [S ii] lines to study the kinematics of the Magellanic-type dwarf irregular galaxy NGC 1569, these observations allowed us to computed the Hα velocity field of this galaxy. Doing a detailed analysis of the velocity along the line-of-sight and Hα velocity profiles, we identified the origin of most of the motions in the innermost parts of the galaxy and discarded the possibility of deriving a rotation curve that traces the gravitational well of the galaxy. We analysed the kinematics of the ionised gas around 31 supernova remnants previously detected in NGC 1569 by other authors, in optical and radio emission. We found that the Hα velocity profiles of the supernova remnants are complex indicating the presence of shocks. Fitting these profiles with several Gaussian functions, we computed their expansion velocities which rank from 87 to 188 km s−1 confirming they are supernova remnants. Also, we determined the physical properties such as electron density, mechanical energy, and kinematic age for 30 of the 31 supernova remnants and found they are in the radiative phase with an energy range from 1 to 39 × 1050 erg s−1 and an age from 2.3 to 8.9 × 104 yr. Finally, we estimated the Surface Brightness - Diameter (Σ-D) Relation for NGC 1569 and obtained a slope β = 1.26 ± 0.2, comparable with the β value obtained for supernova remnants in galaxies M31 and M33.

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Hα KINEMATICS OF THE ISOLATED INTERACTING GALAXY PAIR KPG 486 (NGC 6090)

Cited by 3 publications

References 52 publications

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

LARS XIII: High Angular Resolution 21 cm H i Observations of Lyα Emitting Galaxies

A kinematical study of the dwarf irregular galaxy NGC 1569 and its supernova remnants

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