Isolated galaxies are the ideal reference sample to study the galaxy structure minimizing potential environmental effects. We selected a complete sample of 14 nearby, late-type, highly inclined (i > 80 degrees), isolated galaxies from the Catalogue of Isolated Galaxies (CIG) which offers a vertical view of their disc structure. We aim to study extraplanar Diffuse Ionized Gas (eDIG) by comparing the old and young disc components traced by near-infrared (NIR) and ultraviolet (UV) imaging with the H alpha emission structure. We obtained H alpha monochromatic maps from the Fabry-Perot (FP) interferometry, while the old and young discs structures are obtained from the photometric analysis of the 2MASS Ks band, and GALEX NUV and FUV images, thereby identifying the stellar disc and whether the eDIG is present. The H alpha morphology is peculiar in CIG 71, CIG 183, and CIG 593 showing clear asymmetries. In general, geometric parameters (isophotal position angle, peak light distribution, and inclination) measured from H alpha, UV, and NIR show minimal differences (e.g. Ai < +/- 10 degrees), suggesting that interaction does not play a significant role in shaping the morphology, as expected in isolated galaxies. From H alpha maps, the eDIG was detected vertically in 11 out of 14 galaxies. Although the fraction of eDIG is high, the comparison between our sample and a generic sample of inclined spirals suggests that the phenomenon is uncorrelated to the galaxy environment. As suggested by the extraplanar UV emission found in 13 out of 14 galaxies the star formation extends well beyond the disc defined by the H alpha map.

ABSTRACT We present Fabry-Pérot observations in the H α and [S ii] lines to study the kinematics of the Magellanic-type dwarf irregular galaxy NGC 1569, these observations allowed us to compute the H α velocity field of this galaxy. Doing a detailed analysis of the velocity along the line of sight and H α 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 ionized gas around 31 supernova remnants previously detected in NGC 1569 by other authors, in optical and radio emission. We found that the H α 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.

We present an analysis of the optical properties of three Ultra Luminous X-ray (ULX) sources identified in NGC 925. We use Integral field unit data from the George Mitchel spectrograph in the context of the Metal-THINGS survey. The optical properties for ULX-1 and ULX-3 are presented, while the spaxel associated with ULX-2 had a low S/N, which prevented its analysis. We also report the kinematics and dimensions of the optical nebula associated with each ULX using ancillary data from the PUMA Fabry–Perot spectrograph. A BPT analysis demonstrates that most spaxels in NGC 925 are dominated by star-forming regions, including those associated with ULX-1 and ULX-3. Using the resolved gas-phase metallicities, a negative metallicity gradient is found, consistent with previous results for spiral galaxies, while the ionization parameter tends to increase radially throughout the galaxy. Interestingly, ULX-1 shows a very low gas metallicity for its galactocentric distance, identified by two independent methods, while exhibiting a typical ionization. We find that such low gas metallicity is best explained in the context of the high-mass X-ray binary population, where the low-metallicity environment favors active Roche lobe overflows that can drive much higher accretion rates. An alternative scenario invoking accretion of a low-mass galaxy is not supported by the data in this region. Finally, ULX-3 shows both a high metallicity and ionization parameter, which is consistent with the progenitor being a highly accreting neutron star within an evolved stellar population region.

AbstractWe present scanning Fabry-Perot observations of different types of star-forming galaxies from apparently isolated LIRGs to equal mass interacting galaxies. We analyze the ionized gas kinematics, its relation with the morphology of each system and the location of SF regions for different systems.

We present direct images in the H alpha and [S II] lambda lambda 6717,6731 angstrom lines of the Galactic supernova remnant (SNR) G109.1-1.0 (CTB 109). We confirm that the filaments detected are the optical counterpart of the X-ray and radio SNR due to their high [S II]/H alpha line ratios. We study for the first time the kinematics of the optical counterpart of SNR CTB 109 using the Universidad Nacional Autonoma de Mexico scanning Fabry-Perot interferometer PUMA. We estimate a systemic velocity of V-LSR = - 50 +/- 6 km s(-1) for this remnant and an expansion velocity of V-exp = 230 +/- 5 km s(-1). From this velocity and taking into account previous studies of the kinematics of objects at that Galactic longitude, we derive a distance to SNR CTB 109 of 3.1 +/- 0.2 kpc, locating it in the Perseus arm. Using the [S II] lambda 6717/[S II] lambda 6731 line ratio, we find an electronic density value around n(e) = 580 cm(-3). Considering that this remnant is evolving in a low-density medium with higher-density cloudlets responsible for the optical emission, we determine the age and energy deposited in the ISM by the supernova explosion (E-0) in both the Sedov-Taylor phase and the radiative phase. For both cases, the age is thousands of years and E-0 is rather typical of SNRs containing simple pulsars, so that the energy released to the ISM cannot be used to distinguish between SNRs hosting typical pulsars from those hosting powerful magnetars, like CTB 109.

We present scanning Fabry–Perot interferometric observations of CIG 993, which is an apparently isolated luminous infrared galaxy that also exhibits luminous blue compact and Wolf–Rayet galaxy features, and which also has a high star formation rate. Our high-resolution observations of the Hα emission line allowed us to derive the radial velocity field (VF), the velocity dispersion σ, and the residual VFs of the galaxy. This galaxy exhibits several kinematical components. On the one hand, the velocity gradients detected on the VF can be associated with a rotating disk, which is in contrast to previous results with less spectral resolution. However, the VF, the σ and residual VF show significant deviations from circular motions in the central part of the galaxy that matches a region with high number of Wolf–Rayet and O stars, which is coincident with the blue luminous component of the galaxy. We find narrow and broad velocity components for the ionized gas in the central part of the galaxy. The broad component is evidence of a central outflow related with the ongoing burst of stellar formation. The morpho-kinematical analysis of the galaxy indicates we are only seeing the brightest parts of the galaxy, which correspond to the bulge, a central bar and the beginning of the disk. We believe that CIG 993 is a disk galaxy that harbors important star-forming processes, which are most likely caused by a relatively recent interaction. This could imply that small encounters can change the global characteristics of a galaxy without disturbing the main rotation disk motion or the morphology of the galaxy.

Context. Encounters between galaxies modify their morphology, kinematics, and star formation history. The relation between these changes and external perturbations is not straightforward. The great number of parameters involved requires both the study of large samples and individual encounters where particular features, motions, and perturbations can be traced and analysed in detail. Aims. We analysed the morphology, kinematics, and dynamics of two luminous infrared spiral galaxies of almost equal mass, NGC 5257 and NGC 5258, in which star formation is mostly confined to the spiral arms, in order to understand interactions between galaxies of equivalent masses and star-forming processes during the encounter. Methods. Using scanning Fabry–Perot interferometry, we studied the contribution of circular and non-circular motions and the response of the ionized gas to external perturbations. We compared the kinematics with direct images and traced the star-forming processes and gravitational effects due to the presence of the other galaxy. The spectral energy distribution of each member of the pair was fitted. A mass model was fitted to the rotation curve of each galaxy. Results. Large, non-circular motions detected in both galaxies are associated with a bar, spiral arms, and HII regions for the inner parts of the galaxies, and with the tidal interaction for the outer parts of the discs. Bifurcations in the rotation curves indicate that the galaxies have recently undergone pericentric passage. The pattern speed of a perturbation of one of the galaxies is computed. Location of a possible corotation seems to indicate that the gravitational response of the ionized gas in the outer parts of the disc is related to the regions where ongoing star formation is confined. The spectral energy distribution fit indicates slightly different star formation history for each member of the pair. For both galaxies, a pseudo-isothermal halo better fits the global mass distribution.

We present 3D observations of three interacting galaxies in order derive their extended kinematics and to trace events such as violent star-formation (SF), mass-transfer, structure perturbation and the presence of energetic sources induced by the interacting processes.

Luminous infrared galaxies (LIRG) have between 10(11) and 10(12) solar luminosities. The infrared luminosity is the product of the thermal heating of dust in regions of intense star formation or active galactic nuclei. The dust absorbs the ultraviolet and optical radiation, and re-emits in the IR. In order to produce such luminosities the star formation rate (SFR) must be very high, around 17 solar masses per year. In the local Universe, these SFRs are usually produced by interactions between galaxies or mergers.In this paper, we present the study of the galaxy CIG 302 which is part of a sample of nearby isolated LIRGs galaxies, CIG 302 does not exhibit obvious signs of interaction. Using direct imaging observations in the optical, infrared scanning Fabry-Perot interferometry, as well as images of astronomical archives, we identify the mechanisms at the origin of this excess emission in the IR, in particular the possible presence of a satellite galaxy that fell into the main galaxy disk.

We present observations scanning Fabry-Perot observations of the nearby galaxy NGC 5402 hosting one bright ultra-luminous X-ray source as part of a project to study the kinematics of the extended counterpart of this ULX and nature of the ionization of the gas.

Based on integral field spectroscopy data from the CALIFA survey, we investigate the possible dependence of spiral arm pitch angle with optical wavelength. For three of the five studied objects, the pitch angle gradually increases at longer wavelengths. This is not the case for two objects where the pitch angle remains constant. This result is confirmed by the analysis of SDSS data. We discuss the possible physical mechanisms to explain this phenomenon, as well as the implications of the results.

Star formation efficiency seems to increase as separation between interacting galaxy pairs decreases, suggesting that the starburst phase of interacting galaxies occurs at a late stage in the interaction. However, luminous infrared galaxies (LIRGs) are seen in early interacting systems for which the separation is still relatively large. We present a preliminary kinematical and dynamical study of the interacting LIRG galaxy pair Arp 240. The enhanced SF does not come from the central parts but from the outskirts, and it seems to be related to the perturbation due to the encounter.

We present a study of the host bulge properties and their relations with the black hole mass on a sample of 10 intermediate-type active galactic nuclei (AGN). Our sample consists mainly of early type spirals, four of them hosting a bar. For 70$^{+10}_{-17}%$ of the galaxies we have been able to determine the type of the bulge, and find that these objects probably harbor a pseudobulge or a combination of classical bulge/ pseudobulge, suggesting that pseudobulges might be frequent in intermediate-type AGN. In our sample, 50\pm14% of the objects show double-peaked emission lines. Therefore, narrow double-peaked emission lines seem to be frequent in galaxies harboring a pseudobulge or a combination of classical bulge/ pseudobulge. Depending on the bulge type, we estimated the black hole mass using the corresponding $M_{BH} - {\sigma*}$ relation and found them with a range of: 5.69$\pm$0.21 $<$ $\log M_{BH}^{\sigma*}$ $<$ 8.09$\pm$0.24. Comparing these $M_{BH}^{\sigma*}$ values with masses derived from the FWHM of H$\beta$ and the continuum luminosity at 5100 \AA from their SDSS-DR7 spectra ($M_{BH}$) we find that eight out of ten (80$^{+7}_{-17}$%) galaxies have black hole masses that are compatible within a factor of 3. This result would support that $M_{BH}$ and $M_{BH}^{\sigma*}$ are the same for intermediate-type AGN as has been found for type 1 AGN. However, when the type of the bulge is taken into account only 3 out of the 7 (43$^{+18}_{-15}%$) objects of the sample have their $M_{BH}^{\sigma*}$ and $M_{BH}$ compatible within 3-$\sigma$ errors. We also find that estimations based on the $M_{BH}-\sigma*$ relation for pseudobulges are not compatible in 50$\pm20%$ of the objects.

We present a kinematical study of the nearly edge-on galaxy ESO 379-G006 that shows the existence of extraplanar ionized gas. With Fabry-Perot spectroscopy at H-alpha, we study the kinematics of ESO 379-G006 using velocity maps and position-velocity diagrams parallel to the major and to the minor axis of the galaxy. We build the rotation curve of the disk and discuss the role of projection effects due to the fact of viewing this galaxy nearly edge-on. The twisting of the isovelocities in the radial velocity field of the disk of ESO 379-G006 as well as the kinematic asymmetries found in some position-velocity diagrams parallel to the minor axis of the galaxy suggest the existence of deviations to circular motions in the disk that can be modeled and explained with the inclusion of a radial inflow probably generated by a bar or by spiral arms. We succeeded in detecting extraplanar Diffuse Ionized Gas in this galaxy. At the same time, from the analysis of position-velocity diagrams, we found some evidence that the extraplanar gas could lag in rotation velocity with respect to the midplane rotation.

A sample of 10 nearby intermediate-type active galactic nuclei (AGNs) drawn from the Sloan Digital Sky Survey is presented. The aim of this work is to provide estimations of the black hole (BH) mass for the sample galaxies from the dynamics of the broad-line region. For this purpose, a detailed spectroscopic analysis of the objects was done. Using Baldwin–Phillips–Terlevich diagnostic diagrams, we have carefully classified the objects as true intermediate-type AGNs and found that 80%+7.2%−17.3% are composite AGNs. The BH mass estimated for the sample is within 6.54 ± 0.16 < log MBH < 7.81 ± 0.14. Profile analysis shows that five objects (J120655.63+501737.1, J121607.08+504930.0, J141238.14+391836.5, J143031.18+524225.8, and J162952.88+242638.3) have narrow double-peaked emission lines in both the red (Hα, [N ii] λλ6548,6583 and [S ii] λλ6716, 6731) and the blue (Hβ and [O iii] λλ4959, 5007) regions of the spectra, with velocity differences (ΔV) between the double peaks within 114 km s−1 < ΔV < 256 km s−1. Two of them, J121607.08+504930.0 and J141238.14+391836.5, are candidates for dual AGNs since their double-peaked emission lines are dominated by AGN activity. In searches of dual AGNs, type 1, type II, and intermediate-type AGNs should be carefully separated, due to the high serendipitous number of narrow double-peaked sources (50% ± 14.4%) found in our sample.

We use OSIRIS in its long-slit mode to look for mass transfer and induced star formation in the interacting galaxy pair KPG 468.

AbstractWe present a kinematical study of the marginally edge-on galaxy ESO 379-006. With Fabry-Perot spectroscopy at Hα we obtain velocity maps, the radial velocity field, and position-velocity diagrams parallel to the major and to the minor axis of the galaxy. We build the rotation curve of the galaxy and discuss the role of projection effects. The twisting of isovelocities in the radial velocity field of the disk of ESO 379-006 as well as a kinematical asymmetry found in the position-velocity diagrams parallel to the minor axis suggest the existence of non-circular motions that can be modeled by including a radial inflow besides the rotation motion. Extraplanar Diffuse Ionized gas was detected in this galaxy both from the images and from its kinematics. It is possible that the diffuse gas is lagging in rotation.