Broad Wings Research Articles

Defining dysmorphic facial features in congenital Zika syndrome.

Congenital Zika syndrome (CZS) constitutes a recently identified malformation caused by Zika virus infection during pregnancy. Limited data is available to date on the facial dysmorphic features of these patients. This study evaluated the facial dysmorphisms of children with CZS, compared with clinically healthy children, using clinical examination and standardized photographic images. Sixty-three children with CZS (9.70 ± 3.2 months-age), and 31 Controls (8.67 ± 6.2 months-age) joined the study. Seven out of 15 indices differed between groups: midfacial height (MFH)/horizontal facial reference (HFR) (p = .0003), interalar distance/HFR (p = .0027), nasal root depth/MFH (p = .0030), posterior nasal length/MFH (p = .0002), vertical position of the ear/MFH (p <.0001), ear length/MFH (p = .0005), chin height/total facial height (CH/TFH) (p <.0001). A CH/TFH of 0.229 showed 93.9% sensitivity and 80.6% specificity in diagnosing CZS. Children with CZS had broad, short faces, decreased intercanthal distance, short posterior nasal length, prominent nasal root, broad nasal wings, and high-set and long ears. Increased chin height index provided the most accurate diagnostic potential.

New luminous blue variable candidates in the NGC 247 galaxy

ABSTRACT We search for luminous blue variable (LBV) stars in galaxies outside the Local Group. Here we present a study of two bright Hα sources in the NGC 247 galaxy. Object j004703.27–204708.4 (MV = −9.08 ± 0.15 mag) shows the spectral lines typical for well-studied LBV stars: broad and bright emission lines of hydrogen and helium He i with P Cyg profiles, emission lines of iron Fe ii, silicon Si ii, nitrogen N ii and carbon C ii, forbidden iron [Fe ii] and nitrogen [N ii] lines. The variability of the object is ΔB = 0.74 ± 0.09 mag and ΔV = 0.88 ± 0.09 mag, which makes it a reliable LBV candidate. The star j004702.18–204739.93 (MV = −9.66 ± 0.23 mag) shows many emission lines of iron Fe ii, forbidden iron lines [Fe ii], bright hydrogen lines with broad wings, and also forbidden lines of oxygen [O i] and calcium [Ca ii] formed in the circumstellar matter. The study of the light curve of this star did not reveal significant variations in brightness (ΔV = 0.29 ± 0.09 mag). We obtained estimates of interstellar absorption, the photosphere temperature, as well as bolometric magnitudes $M_\text{bol}=-10.5^{+0.5}_{-0.4}$ and $M_\text{bol}=-10.8^{+0.5}_{-0.6}$, which correspond to bolometric luminosities $\log (L_\text{bol}/{\rm L}_{\odot })=6.11^{+0.20}_{-0.16}$ and $6.24^{+0.20}_{-0.25}$ for j004703.27–204708.4 and j004702.18–204739.93, respectively. Thus, the object j004703.27–204708.4 remains a reliable LBV candidate, while the object j004702.18–204739.93 can be classified as a B[e]-supergiant.

Intrinsic Properties of the Engine and Jet that Powered the Short Gamma-Ray Burst Associated with GW170817

Abstract GRB 170817A was a subluminous short gamma-ray burst detected about 1.74 s after the gravitational wave signal GW170817 from a binary neutron star (BNS) merger. It is now understood as an off-axis event powered by the cocoon of a relativistic jet pointing 15°–30° away from the direction of observation. The cocoon was energized by the interaction of the incipient jet with the non-relativistic baryon wind from the merger remnant, resulting in a structured outflow with a narrow core and broad wings. In this paper, we couple the observational constraints on the structured outflow with a model for the jet–wind interaction to constrain the intrinsic properties with which the jet was launched by the central engine, including its time delay from the merger event. Using wind prescriptions inspired by magnetized BNS merger simulations, we find that the jet was launched within about 0.4 s from the merger, implying that the 1.74 s observed delay was dominated by the fireball propagation up to the photospheric radius. We also constrain, for the first time for any gamma-ray burst, the jet opening angle at injection and set a lower limit to its asymptotic Lorentz factor. These findings suggest an initially Poynting-flux dominated jet, launched via electromagnetic processes. If the jet was powered by an accreting black hole, they also provide a significant constraint on the survival time of the metastable neutron star remnant.

SPECTRAL AND PHOTOMETRIC STUDY OF TWO OBJECTS IRAS 22023+5249 AND IRAS 06053+1837

The objects IRAS 06053+1837 and IRAS 22023+5249, are considered as planetary nebulacandidates. They have far infrared colors, which are typical to planetary nebulae. Their rather cool stars aresurronded by envelopes, in which some low-excitation emission lines are formed.BV photometry of the object IRAS 22023+5249, carried out in 2017-2020, resulted the scatter of B and Vvalues within 0m.25 and 0 m.10 respectively. Moreover a tendency of the gradual increasing of brightness is revealed.Absolute fluxes and equivalent widths of the Hβ, Hα, [NII], 6548, 6583A and HeI, 6678A emission lines in thespectrum of IRAS 22023+5249 are determined. The strengthening of the emission lines is confirmed. Most likelyincreasing of an effective temperrature of the star is responsible for observable variations. As a whole spectral andphotometric characteristics of the object IRAS 22023+5249 correspond to its status as a low-excitation planetarynebula.For the object IRAS 06053+1837observable data are obtained in 2014 -2019. Much larger the scatter of B V Rvalues is observed: 0m.50, 0m.15 and 0 m.30 respectively. The only HI emission lines are presented in its spectrum.Asymmetrical profiles of lines have broad wings on the short wavelength side. The evolutionary status of the objectis not defined; its characteristics, are more similar to those of the young AeBe Herbig stars.

Cockroach Stavba jarzembowskii sp. nov. (Blattaria: Liberiblattindae) from mid-Cretaceous Burmese amber

The family Liberiblattinidae is a small but phylogenetically most important group of Blattaria (cockroaches), comprising 17 Mesozoic genera and 20 species. The genus Stavba Vršanská et Vršanský in Vršanský et al. (2019c) of this family consists of two known species. Stavba jarzembowskii sp. nov. is described and figured based on an exceptionally preserved male individual in mid-Cretaceous amber from Myanmar. It is distinguished from the other two species by having more round eyes, a narrower body, broader wings with broader costal area and less crossveins in the radial sector and medial field, and relatively uncurved A veins. Our new find further adds the diversity within this genus and of the cockroaches in 99 Ma tropical forests of Burmese amber.

Fast ejecta resulted from jet–wind interaction in the Great Eruption of Eta Carinae

ABSTRACT The accretion model for the 19th century Great Eruption (GE) of η Carinae suggests that mass outflowing from the primary was accreted on to the secondary, and the gravitational energy of that mass accounts for the increase in luminosity and most of the kinetic energy of the ejecta. It further argues that the accretion was accompanied by the ejection of two jets that shaped the bipolar Homunculus nebula. Observations of echos from the GE found emission lines with broad wings suggesting some of the mass in equatorial directions reached more than $10\, 000 \, \rm {km\, s^{-1}}$. We run hydrodynamic simulations following periastron passage during the GE, launching jets from the secondary as it accreted gas erupted from the primary. We then follow the interaction of the polar jets with the surrounding primary wind, as they accelerate part of the flow to velocities ${\gt}10\, 000 \, \rm {km\, s^{-1}}$ and deflect it towards lower latitudes. We find that the amount of mass that reached these high velocities during the GE is $M_h \approx 0.02 \, \rm {M_{\odot }}$. This value reaches maximum and then decreases with time. Our simulations agree with previous results of the accretion model from which we estimate Mh taking into account the energy budget of the GE. The accretion model can explain the observations of high velocity gas in light echos with the known two stars, and a triple star system is not required.

Electron spin polarization in an Al(III) porphyrin complex with an axially bound nitroxide radical.

The generation and transfer of electron spin polarization and coherence plays an important role in quantum information technologies and spintronics. In this context, the excited state spin dynamics of molecular systems in which a stable free radical is attached to a chromophore are of particular interest. In such complexes, the coupling between the electron spin on the free radical with those on the chromophore generates excited states referred to as sing-doublet, trip-doublet, and trip-quartet. Here, we study the light-induced electron spin polarization in an aluminum(iii) porphyrin (AlPor) complex in which the nitroxide (2,2,6,6-tetramethylpiperidin-1-yl)oxyl (TEMPO) is covalently bound to the Al center via an ester linkage. In addition to the covalent bond to the TEMPO moiety, the Al center in AlPor also acts as a Lewis acid and can coordinate Lewis bases such as pyridine. Without pyridine bound, the spin polarized transient electron paramagnetic resonance spectrum of the complex at 80 K is unusual and displays a strong absorptive pattern with a Lorentzian lineshape. Coordination of pyridine to AlPor-TEMPO results in a dramatic change in the spin polarization pattern and a spectrum typical of the quartet state with broad wings from the ms = ±1/2 ↔ ±3/2 transitions with emissive/absorptive polarization and a narrow absorptive peak from the ms = ±1/2 ↔ ±1/2 transitions. At later times, the pattern evolves to a purely absorptive spectrum similar to that observed without pyridine. These changes are discussed in terms of a model in which back and forth transitions between the nearly degenerate lowest trip-doublet and trip-quartet states occur. It is argued that these transitions lead to the observed net polarization in AlPor-TEMPO and are fast enough that the outer lines are broadened. Density functional theory computations and the UV/Vis spectra suggest that the exchange interaction between TEMPO and the triplet state of AlPor increases when pyridine is bound, and the near degeneracy of the lowest excited states is lifted. It is argued that this slows the back and forth transitions which results in the strong change in the polarization pattern.

ALMA captures feeding and feedback from the active galactic nucleus in NGC 613

We report ALMA observations of CO(3–2) emission in the Seyfert/nuclear starburst galaxy NGC 613, at a spatial resolution of 17 pc, as part of our NUclei of GAlaxies (NUGA) sample. Our aim is to investigate the morphology and dynamics of the gas inside the central kiloparsec, and to probe nuclear fueling and feedback phenomena. The morphology of CO(3–2) line emission reveals a two-arm trailing nuclear spiral at r ≲ 100 pc and a circumnuclear ring at a radius of ∼350 pc that is coincident with the star-forming ring seen in the optical images. Also, we find evidence for a filamentary structure connecting the ring and the nuclear spiral. The ring reveals two breaks into two winding spiral arms corresponding to the dust lanes in the optical images. The molecular gas in the galaxy disk is in a remarkably regular rotation, however the kinematics in the nuclear region are very skewed. The nuclear spectrum of CO and dense gas tracers HCN(4–3), HCO+(4–3), and CS(7–6) show broad wings up to ±300 km s−1, associated with a molecular outflow emanating from the nucleus (r ∼ 25 pc). We derive a molecular outflow mass Mout = 2 × 106 M⊙ and a mass outflow rate of Ṁout = 27 M⊙ yr−1. The molecular outflow energetics exceed the values predicted by AGN feedback models: the kinetic power of the outflow corresponds to PK, out = 20%LAGN and the momentum rate is Ṁoutv ∼ 400LAGN/c. The outflow is mainly boosted by the AGN through entrainment by the radio jet, but given the weak nuclear activity of NGC 613, we might be witnessing a fossil outflow resulting from a previously strong AGN that has now faded. Furthermore, the nuclear trailing spiral observed in CO emission is inside the inner Lindblad resonance ring of the bar. We compute the gravitational torques exerted in the gas to estimate the efficiency of the angular momentum exchange. The gravity torques are negative from 25 to 100 pc and the gas loses its angular momentum in a rotation period, providing evidence for a highly efficient inflow towards the center. This phenomenon shows that the massive central black hole has significant dynamical influence on the gas, triggering the inflowing of molecular gas to feed the black hole.

Diffusion in agitated frictional granular matter near the jamming transition.

We study agitated frictional disks in two dimensions with the aim of developing a scaling theory for their diffusion over time. As a function of the area fraction ϕ and mean-square velocity fluctuations 〈v^{2}〉 the mean-square displacement of the disks 〈d^{2}〉 spans four to five orders of magnitude. The motion evolves from a subdiffusive form to a complex diffusive behavior at long times. The statistics of 〈d^{n}〉 at all times are multiscaling, since the probability distribution function (PDF) of displacements has very broad wings. Even where a diffusion constant can be identified it is a complex function of ϕ and 〈v^{2}〉. By identifying the relevant length and time scales and their interdependence one can rescale the data for the mean-square displacement and the PDF of displacements into collapsed scaling functions for all ϕ and 〈v^{2}〉. These scaling functions provide a predictive tool, allowing one to infer from one set of measurements (at a given ϕ and 〈v^{2}〉) what are the expected results at any value of ϕ and 〈v^{2}〉 within the scaling range.

Extreme gas kinematics in an off-nuclear HII region of SDSS J143245.98+404300.3

We present and discuss the properties of an ionized gas component with extreme kinematics in a recently reported off-nuclear HII region located at ∼0.8−1.0 kpc from the nucleus of SDSS J143245.98+404300.3. The high-velocity-gas component is identified by the detection of very broad emission wings in the Hα line, with full width at half maximum (FWHM) ≥ 850−1000 km s−1. Such gas kinematics are outstandingly high compared to other HII regions in local galaxies and are similar to those reported in some star-forming clumps of galaxies at z ∼ 2. The spatially resolved analysis indicates that the high-velocity gas extends at least ∼90 pc and it could be compatible with an ionized outflow entraining gas at a rate between approximately seven and nine times faster than the rate at which gas is being converted into stars. We do not detect broad emission wings in other emission lines such as Hβ, perhaps due to moderate dust extinction, nor in [N II]λλ6548, 6584 or [S II]λλ6717, 6731, which could be due to the presence of turbulent mixing layers originated by the impact of fast-flowing winds. The lack of spectral signatures associated to the presence of Wolf–Rayet stars points towards stellar winds from a large number of massive stars and/or supernovae as the likely mechanisms driving the high-velocity gas.

Widespread QSO-driven outflows in the early Universe

We present the stacking analysis of a sample of 48 quasi-stellar objects (QSOs) at 4.5 &lt; z &lt; 7.1 detected by the Atacama Large Millimetre Array (ALMA) in the [CII]λ158μm emission line to investigate the presence and the properties of massive, cold outflows associated with broad wings in the [CII] profile. The high sensitivity reached through this analysis allows us to reveal very broad [CII] wings tracing the presence of outflows with velocities in excess of 1000 km s−1. We find that the luminosity of the broad [CII] emission increases withLAGN, while it does not significantly depend on the star formation rate of the host galaxy, indicating that the central active galactic nucleus (AGN) is the main driving mechanism of the [CII] outflows in these powerful, distant QSOs. From the stack of the ALMA cubes, we derive an average outflow spatial extent of ∼3.5 kpc. The average atomic neutral mass outflow rate inferred from the stack of the whole sample isṀout∼ 100M⊙yr−1, while for the most luminous systems it increases to ∼200 M⊙yr−1. The associated outflow kinetic power is about 0.1% ofLAGN, while the outflow momentum rate is ∼LAGN/cor lower, suggesting that these outflows are either driven by radiation pressure onto dusty clouds or, alternatively, are driven by the nuclear wind and energy conserving but with low coupling with the interstellar medium. We discuss the implications of the resulting feedback effect on galaxy evolution in the early Universe.

A multiwavelength study of a massive, active galaxy at z ∼ 2: coupling the kinematics of the ionized and molecular gas

ABSTRACTWe report a multiwavelength study of the massive ($M_{\star } \gtrsim 10^{11} \rm {M}_{\odot }$), z ∼ 2 star-forming galaxy GMASS 0953, which hosts an obscured AGN. We combined near-infrared observations of the GNIRS, SINFONI and KMOS spectrographs to study the kinematics of the [O iii] λ5007 and H α emission lines. Our analysis shows that GMASS 0953 may host an ionized disc extending up to 13 kpc, which rotates at a velocity of $V_{\rm {ion}} = 203^{+17}_{-20}$ km s−1 at the outermost radius. Evidence of rotation on a smaller scale (R ∼ 1 kpc) arises from the CO(J = 6–5) line. The central velocity $V_{\rm {CO}} = 320^{+ 92}_{-53}$ km s−1 traced by the molecular gas is higher than Vion, suggesting that the galaxy harbours a multiphase disc with a rotation curve that peaks in the very central regions. The galaxy appears well located on the z = 0 baryonic Tully–Fisher relation. We also discuss the possibility that the [O iii] λ5007 and H α velocity gradients are due to a galactic-scale wind. Besides, we found evidence of an AGN-driven outflow traced by a broad blueshifted wing affecting the [O iii] λ5007 line, which presents a velocity offset Δv = −535 ± 152 km s−1 from the systemic velocity. Because of the short depletion time-scale (τdep ∼ 108 yr) due to gas ejection and gas consumption by star formation activity, GMASS 0953 may likely evolve into a passive galaxy. However, the role of the AGN in depleting the gas reservoir of the galaxy is quite unclear because of the uncertainties affecting the outflow rate.

Hard-state Accretion Disk Winds from Black Holes: The Revealing Case of MAXI J1820+070

Abstract We report on a detailed optical spectroscopic follow-up of the black hole (BH) transient MAXI J1820+070 (ASASSN-18ey). The observations cover the main part of the X-ray binary outburst, when the source alternated between hard and soft states following the classical pattern widely seen in other systems. We focus the analysis on the He i emission lines at 5876 and 6678 Å, as well as on Hα. We detect clear accretion disk wind features (P-Cyg profiles and broad emission line wings) in the hard state, both during outburst rise and decay. These are not witnessed during the several months long soft state. However, our data suggest that the visibility of the outflow might be significantly affected by the ionization state of the accretion disk. The terminal velocity of the wind is above ∼1200 km s−1, which is similar to outflow velocities derived from (hard-state) optical winds and (soft-state) X-ray winds in other systems. The wind signatures, in particular the P-Cyg profiles, are very shallow, and their detection has only been possible thanks to a combination of source brightness and intense monitoring at very high signal-to-noise. This study indicates that cold, optical winds are most likely a common feature of BH accretion, and therefore, that wind-like outflows are a general mechanism of mass and angular momentum removal operating throughout the entire X-ray binary outburst.

Uncovering QSO-driven outflows and galaxy assembly at cosmic Dawn with ALMA

AbstractI will present evidence of QSO-driven outflows in the early Universe, resulting from the stacking analysis of ALMA observations of the [CII] emission line for a sample of 50 QSOs at z ∼ 5 – 7. The high sensitivity reached by our analysis allowed us to assess that very broad wings are on average present in the [CII] profile, and extend beyond velocities of 1000 km/s in systems with low and high SFR. Such wings are therefore tracing QSO-driven [CII] outflows, with associated mass outflow rates of 100 – 200Mȯ / yr. I will discuss how these outflows relate to those observed in lower-z AGNs and give an estimate of their spatial extent. Furthermore, I will focus on the high-resolution ALMA observation of a hyper luminous QSO at z ∼ 4.5, revealing an exceptional overdensity with multiple companions as close as 2 kpc. These crowded surroundings, and the QSO host galaxy itself, are forming stars at a very high rate (hundreds of Mȯ / yr), suggesting that a significant fraction of the stellar mass assembly at early epochs might have taken place in the companions. I will discuss how the BH and host-galaxy masses are growing in this multi- source system, which likely represents the cradle of what would be a giant galaxy at z = 0.

O iii] Emission line properties in a new sample of heavily reddened quasars at z &gt; 2

We present VLT-SINFONI near infra-red spectra of 26 new heavily reddened quasar candidates selected from the UKIDSS-LAS, VISTA VHS and VIKING imaging surveys. This new sample extends our reddened quasar search to both brighter and fainter luminosities. 25 of the 26 candidates are confirmed to be broad line quasars with redshifts $0.7<z<2.6$ and dust extinctions $0.5<E(B-V)<3.0$. Combining with previously identified samples, we study the H$\alpha$, H$\beta$ and [OIII] emission line properties in 22 heavily reddened quasars with $L_{bol}\approx 10^{47}$ erg/s and $z>2$. We present the first comparison of the [OIII] line properties in high luminosity obscured quasars to a large sample of 111 unobscured quasars in the same luminosity and redshift range. Broad wings extending to velocities of 2500 km/s are seen in the [OIII] emission line profiles of our reddened quasars, suggesting that strong outflows are affecting the ionised gas kinematics. However, we find no significant difference between the kinematics of the [OIII] emission in reddened and unobscured quasars when the two samples are matched in luminosity and redshift. Our results are consistent with a model where quasar-driven outflows persist for some time after the obscuring dust has been cleared from along the line of sight. Assuming the amount of ionised gas in obscured and unobscured quasars is similar, we use the equivalent width distribution of the [OIII] emission to constrain the location of the obscuring dust in our reddened quasars. We find that the dust is most likely to be located on galactic scales, outside the [OIII] emitting region.

Transition-region explosive events produced by plasmoid instability

Magnetic reconnection is thought to be a key process in most solar eruptions. Thanks to highresolution observations and simulations, the studied scale of the reconnection process has become smaller and smaller. Spectroscopic observations show that the reconnection site can be very small, which always exhibits a bright core and two extended wings with fast speeds, i.e., transition-region explosive events. In this paper, using the PLUTO code, we perform a 2-D magnetohydrodynamic simulation to investigate small-scale reconnection in double current sheets. Based on our simulation results, such as the line-of-sight velocity, number density and plasma temperature, we can synthesize the line profile of Si IV 1402.77 Å which is a well known emission line used to study transition-region explosive events on the Sun. The synthetic line profile of Si IV 1402.77 Å is complex with a bright core and two broad wings which can extend to nearly 200 km s−1. Our simulation results suggest that the transition-region explosive events on the Sun are produced by plasmoid instability during small-scale magnetic reconnection.

A New Species of the Mayfly Genus Teloganopsis Ulmer, 1939 (Ephemeroptera, Ephemerellidae) from the South of the Russian Far East

All the developmental stages of Teloganopsis orbicularissp. n. from the Far East of Russia are described. The male imago of the new species is characterized by the rounded lobes of the penis and by broad hind wings. T e larvae have a light medial longitudinal stripe and groups of short setae on the medial longitudinal stripe on tergites IV–IX. The hypopharynx is rounded; the superlinguae are broad, ovate. The maxillae are uniformly broad with a bevel-edged fang-like top; the palpus is missing. The glossae are rounded, broad, and closely approximate. The eggs are ellipsoidal with one polar roundish cap. The chorion surface is covered with a reticulation of broad, gently sloping spongy ridges and deep round tartareous meshes. The systematic position of the new species is discussed.

Eye and wing structure closely reflects the visual ecology of dung beetles.

An important resource partitioning strategy allowing dung beetles to coexist in the same habitat, while utilising the same food, is species' separation of activity times. After establishing the diel activity period of three closely related, co-occurring dung beetles, we examined their eye and wing morphology. Absolute and relative eye size, and facet size were greater in the nocturnal Escarabaeus satyrus, followed by the crepuscular Scarabaeus zambesianus and then the diurnal Kheper lamarcki. The diurnal K. lamarcki had the highest wing aspect ratio (long, narrow wings), followed by the crepuscular S. zambesianus and the nocturnal E. satyrus (short, broad wings), suggesting that dim-light active species fly slower than diurnal species. In addition, the two species active in dim light had a lower wing loading than the diurnal species, indicating the need for greater manoeuvrability in the dark. Analyses of wing shape revealed that the diurnal K. lamarcki wing had a proportionally larger jugal and anal region than both dim light species. Our results show that different species of dung beetles have a combination of optical and morphological wing adaptations to support their foraging activities in diverse light conditions.

ALMA Observations of the Massive Molecular Outflow G331.512-0.103. II. Physical Properties, Kinematics, and Geometry Modeling

We present observations and analysis of the massive molecular outflow G331.512-0.103, obtained with ALMA band 7, continuing the work from Merello et al. (2013). Several lines were identified in the observed bandwidth, consisting of two groups: lines with narrow profiles, tracing the emission from the core ambient medium; and lines with broad velocity wings, tracing the outflow and shocked gas emission. The physical and chemical conditions, such as density, temperature, and fractional abundances are calculated. The ambient medium, or core, has a mean density of $\sim 5\times 10^6$ cm$^{-3}$ and a temperature of $\sim 70$ K. The SiO and SO$_2$ emission trace the very dense and hot part of the shocked outflow, with values of $n_{\rm H_2}\sim10^9$ cm$^{-3}$ and $T \sim 160-200$ K. The interpretation of the molecular emission suggests an expanding cavity geometry powered by stellar winds from a new-born UCHII region, alongside a massive and high-velocity molecular outflow. This scenario, along with the estimated physical conditions, is modeled using the 3D geometry radiative transfer code MOLLIE for the SiO(J$=8-7$) molecular line. The main features of the outflow and the expanding shell are reproduced by the model.

The structure of the Mg ii broad line emitting region in Type 1 AGNs

We investigate the structure of the Mg II broad line emission region in a sample of 284 Type 1 active galactic nuclei (AGNs), through comparing the kinematical parameters of the broad Mg II and broad H$\beta$ lines. We found that the Mg II emitting region has more complex kinematics than the H$\beta$ one. It seems that the \ion{Mg}{ii} broad line originates from two subregions: one which contributes to the line core, which is probably virialized, and the other, 'fountain-like' emitting region, with outflows-inflows nearly orthogonal to the disc, which become suppressed with stronger gravitational influence. This subregion mostly contributes to the emission of the Mg II broad line wings. The kinematics of the Mg II core emitting region is similar to that of the H$\beta$ broad line region (seems to be virialized), and therefore the Full Width at Half Maximum (FWHM) of Mg II still can be used for the black hole (BH) mass estimation in the case where the Mg II core component is dominant. However, one should be careful with using the \ion{Mg}{ii} broad line for the BH mass estimation in the case of very large widths (FWHM$>$ 6000 km s$^{-1}$) and/or in the case of strong blue asymmetry.