dataesr/scientific-paragraphs-categorization huggingface dataset:
1 and 0. 5, including the one at z ∼ 0. 36 that has been published in  Ghirardini et al. (2021). Another four high-z supercluster candidates are detected at redshifts higher than 0. 5, but need further spectroscopic confirmation as the errors on the photometric redshifts may bias the linking length calculations. The eFEDS cluster and group catalog at the final eRASS equatorial depth provides a benchmark proof-of-concept for the eROSITA All-Sky Survey extended source detection and characterization. We confirm the excellent performance of eROSITA for cluster science and expect no significant deviations from our pre-launch expectations for the final all-sky survey. Acknowledgement. This work is based on data from eROSITA, the soft X-ray instrument aboard SRG, a joint Russian-German science mission supported by the Russian Space Agency (Roskosmos), in the interests of the Russian Academy of Sciences represented by its Space Research Institute (IKI), and the Deutsches Zentrum für Luft-und Raumfahrt (DLR).
A time gate was used to selectively focus on the decay of short-lived isomer, as will be shown below. Radioactive ions of 183 Tl were implanted in a carbon foil with a 6 mm diameter and 20 µ g/cm 2 thickness  [29]. The implantation position was surrounded with two partially depleted silicon detectors for detection of α particles and conversion electrons. An annular detector with thickness of 300 µ m and area of 450 mm 2 was placed 7 mm upstream from the foil. The beam passed through the hole with 8 mm diameter. Another silicon detector with thickness of 500 µ m and area of 300 mm 2 was placed downstream from the foil. Both detectors with typical energy resolution of approximately 25 keV (for both α particles and conversion electrons) covered a solid angle of 24% of 4π. Calibration data for these silicon detectors were taken using the two 241 Am sources mounted inside of the WM system.
Two coaxial germanium detectors with relative efficiencies of approximately 70% and 90% were used to detect γ rays. They were placed outside of the vacuum chamber of the WM system at 0 • and 90 • , relative to the beam direction. Energy and efficiency calibrations were performed using standard radioactive sources of 133 Ba, 137 Cs, 60 Co, and 152 Eu. Signals from the preamplifiers of the detectors were processed with a digital data acquisition system, based on commercial Digital Gamma Finder (DGF) modules.
The three peaks seen in Fig. 3   (10)  was determined for the 356. 5 keV transition. Based on a good agreement with the theoretical value of 0. 61, calculated with the BrICC software  [31] , an E 3 multipolarity was established unambiguously for the 356. 5 keV transition. Theoretical values for other multipolarities are given in Table  I. Figure  3 (c) gives the CE spectrum detected in prompt coincidence with the 356. 5 keV γ rays. The ratio α K /α L+M+N. = 1. 94  (28)  was determined for the 272. 2 keV transition. This suggests a mixed M1 + E 2 character for the transition, since the theoretical values are 4. 53 for a pure M1 and 1. 19 for a pure E 2 multipolarities. The intensity balance of the 272. 2 keV and 356. 5 keV γ -rays singles was used to determine the total internal conversion coefficient for the 272.
2 keV transition. The internal conversion is interpreted as missing γ -ray intensity. The total conversion coefficient α T = 0. 24(2) was determined for the 272. 2 keV transition. This corroborates the above conclusion on the mixed M1 + E 2 character of the transition, since theoretically α T (M1) = 0. 51 and α T (E 2) = 0. 15. Other multipolarities are excluded, see Table  I. Using a combination of both approaches, the M1/E 2 mixing ratio δ = 1. 87 +0. 28 -0. 21 was determined with the BrIccMixing software  [31].
ACKNOWLEDGMENTS The authors express their gratitude to the ISOLDE collaboration, the ISOLDE machine operators, and the CERN radioprotection team for excellent support. This work was supported by the  Ministry of Education, Science, Research and Sport of the Slovak Republic , the  Slovak Research and Development Agency  under Contract No. APVV-20-0532 , by Slovak grant agency  VEGA  (Contract No. 2/0067/21 ), by  FWO-Vlaanderen (Belgium) , by  GOA/2010/010  ( BOF KU Leuven ), by the  Interuniversity Attraction Poles Programme  initiated by the  Belgian Science Policy Office (BriX network   P7/12 ), by the  European Commission  within the  Seventh Framework Programme through I3-ENSAR  (Contract No. RII3-CT-2010-262010 ), by a grant from the  European Research Council  ( ERC-2011-AdG-291561-HELIOS ), and by a grant from the  U.
9/2 proton with the excited 0 + state in 178 Pt. A more precise dataset needs to (9/2 -) 299. 0 927. 7 0 + 355. 0 (9/2 -) 628. 7 0 + 0 183 Tl m 182 Hg (9/2 -) 279. 8 407(17) E α = 6058 keV 0 + 421. 0 HF = 5(2) (9/2 -) 127(17) 0 + 0 179 Au 178 Pt.
Using the VESTIGE survey, a deep narrow-band Hα imaging survey of the Virgo cluster carried on at the CFHT with MegaCam, we have discovered a long and diffuse tail of ionised gas in the edge-on late-type galaxy NGC 4330. This peculiar feature witnesses 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 to study 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 10000) with the purpose of understanding the effects of 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.
Such resolution unreached in the more distant UGC 6697 and JO204 despite their extraordinary MUSE data. The paper is structured as follows: in Sect. 2 we describe the MegaCam CFHT narrow-band imaging and the FP highresolution spectroscopic observations along with the multifrequency data used in the analysis. In Sect. 3 and 4 we analyse the imaging data and construct the rotation curve of the galaxy, while in Sect. 5 we study the 2-D kinematics of the gas and the specific kinematics of the gas out of the plane in Sect. 6. The results of the analysis are compared to the hydrodynamic simulations of  Vollmer et al. (2021)  in Sect. 7. The discussion and conclusions are given in Sect. 8. (1)  HRS 124 a α (J2000) (2)  12 h 23 m 17. 10 s b δ (J2000) (3).
VESTIGE narrow-band imaging Deep Hα narrow-band imaging of NGC 4330 has been gathered with MegaCam at the CFHT by the VESTIGE survey  (Boselli et al. 2018c) , and the first imaging results have been presented in  Fossati et al. (2018). Briefly, the galaxy has been observed using the narrow-band filter MP9603 (λ c = 6591 Å; ∆λ = 106 Å), which includes the Hα line and the two [NII] lines at λ 6548 Å and λ 6584 Å 1. The galaxy has been observed during the main VESTIGE survey but also during a pilot run. The data used in this work are the combination of these two datasets, and are thus deeper than those analysed in  Fossati et al. (2018) , which were limited to the pilot observations. To secure the subtraction of the stellar continuum, the galaxy was also observed in the broad r-band filter with shorter exposures to avoid saturation within the nucleus.
Tuned simulations suggest that this particular shape could be produced after a ram pressure stripping event. The gas removed out from the disc plane in the z-direction can alter the shape of the gravitational potential well, modifying the stellar orbits, thus producing a thicker disc  (Farouki & Shapiro 1980; Clarke et al. 2017; Safarzadeh & Scannapieco 2017; Steyrleithner et al. 2020). This phenomenon might explain the peculiar morphology of NGC 4330, with a boxy shape particularly evident in the southwest direction, where the stripping is more efficient. Unfortunately, we lack of stellar kinematical data necessary to further probe this scenario.
Associated to the diffuse emission, the VESTIGE Hα image shows a few weak compact regions with a surface brightness over Σ(Hα) ∼ 10 -17 erg s -1 cm -2 arcsec -2 , which corresponds to the GHASP detection limit where star formation is probably taking place. Not all the features located out of the plane of the galaxy and above this threshold limit are clearly detected in the monochromatic FP image of NGC 4330, neither in the PUMA data nor in the deeper GHASP data. The bent region at the northeast edge of the disc (labelled A in Fig. 2 f ) is clearly detected as well as a few regions on the southwest extension of the disc (labelled K, L and M). A few ionised regions have also been detected at the limit of the stellar disc (labelled E, G and F).
Comparison of the three methods Figure  3  shows the RCs derived using three different methods: (1) the intensity-peak method (IPM), (2) the envelope-tracing method (ETM), and (3) the iteration-method (ITM). The RCs obtained with the IPM using both GHASP and PUMA datasets show that NGC 4330 is rotating as a solid-body inside a radius of ∼30 arcsec. The output of the fit of Eq. B. 4 (ETM) provides similar terminal velocities reached around ∼ 30 arcsec (∼2. 4 kpc) as well as similar transition radii between the rising and the flat part of the RCs compared to the IPM method. After this transition, the RCs computed with the ETM method are flat up to the photometric radius R 23. 5 ∼ 140 arcsec (∼11. 6 kpc), which is represented by the red line in panels (a) and (c) of Fig. 3. The approaching and receding sides of the RCs measured with the IPM method start to differ at a radius of ∼ 30 arcsec (∼ 2.
5 kpc) and do not have a single point of matching where the two sides overlap until the photometric radius. The rotation velocity obtained for each dataset with the ETM differs by 8 km s -1. This number is within the uncertainties due to the differences in resolution between the two instruments and could be partly due to a different threshold for the PVD extraction. Both datasets show that the RCs derived using the ETM are steeper than those derived using the IPM in the inner regions. This difference is due to the fact that here the contribution of regions along the same LoS but located at different radial distances from the galaxy centre is large, while this is not the case at the edges of the disc where the ETM measures the rotation. Close to the galaxy centre, the width of the PVD is supposed to narrow because along the minor axis, the rotation velocity vector lies in the sky plane, thus its projected component along the LoS is null.
Since we do not observe a large decrease of the PVD width in the centre, we conclude that it is mainly due to radial velocity dispersion. For the GHASP dataset, the RCs derived from the ETM and the ITM have a similar inflexion shape along the transition radius (r t ) between the rising and the flat part of the RC (see Fig. 3 ). Nevertheless, the fit shows that the parameter r t differs by ∼5 arcsec (∼0. 4 kpc) using the two methods. For the PUMA dataset, r t occurs at a radius ∼9 arcsec (∼0. 7 kpc) larger with the ETM than with the ITM, which makes the RC steeper with this last method (see Fig. 3 ). Despite the difference between r t computed using the ETM and ITM, an acceptable discrepancy between the maximal rotational velocities of ∼ 8 km s -1 is observed at the photometric radius in the RCs of each dataset.
These peculiar motions are not modelled with the other methods. Nevertheless, the ETM and ITM withdraw the effects of LoS to the rotational velocity on the inner disc, and allow us to obtain a reliable measure of the maximal rotational velocity of the galaxy, we fix it to the average value of the four velocities given in table B. 1 for the two datasets: V max rot = 158 ± 12 km s -1 , the uncertainty being estimated from their standard deviation.
Velocity fields Figure  5  shows the velocity field of the ionised gas of NGC 4330 derived from the PUMA and GHASP FP datasets. The velocity fields of both datasets are consistent, they display a rigid body shape inside of a diameter of ∼60 arcsec (∼4. 8 kpc) where the isovelocity contours are parallel to the minor axis of the galaxy. We have traced on these maps two parallel dashed lines at at r 0 ± 30 arcsec (±2. 4 kpc) enclosing this region. Outside this diameter the isovelocity contours become almost parallel to the major axis in the NW hook (region A) and on its counterpart, between regions I and J. However, these maps differ in the southern tail, i. e. in regions K and L (see point 5 hereafter). These last features are the signature of non-circular motions that indicate strong perturbations in the kinematics of the regions affected by the stripping process.
The two-dimensional velocity field obtained with highresolution FP interferometry allows us also to measure the kinematic of the gas in very low surface brightness regions. These regions, labelled from A to M, were previously identified in the monochromatic image and they are now identified on the velocity fields of both datasets in Fig. 5. Our data allowed us to measure the LoS velocities of the stripped gas in the southern re- gions, in region F located on the compression front on the northeaster side of the disc and in region I on the disc plane. The LoS velocities of all these regions are given in Table  5. 4 and will be further discussed in Sect. 5. 4. We notice that: 1. The detection and estimation of the LoS velocity of the gas over the galaxy disc, and more specifically inside of regions A, E, F, G, H, I, J (westernmost part) are robust since derived from independent sets of data with consistent results.
Ionised gas is detected in regions K and L with similar LoS velocities. A velocity difference of ∼50 km s -1 is observed between both datasets, which could also be due to parasitic night skylines. Thus, despite this difference in the two datasets, these velocities are consistent with streaming motions caused by the stripping process. 6. The gas detected in regions J, K, and H has a velocity similar to that measured at the edge of the rotating disc (1450 km s -1 ), suggesting a flat rotation curve. 7. Figure  5  also shows two dashed lines at ∼30 arcsec (∼2. 4 kpc) from the galactic centre. These dashed lines enclose the disc section where the ionised gas shows a rigidbody rotation as indicated by the velocity contours parallel to the minor axis. To the southwest, region I marks the limit where the velocity contours start to become parallel to the major axis.
Velocity dispersion Figure  6  shows the velocity dispersion of the galaxy as measured from the PUMA and GHASP datasets. Following  Boselli et al. (2021b)  we checked that the velocity profiles have a single peak, i. e. that the barycentric method applied to measure the velocity dispersions does not introduce any strong systematic bias in the results. At first order, the velocity dispersion of the gas is fairly constant over the disc of the galaxy, with σ ∼ 35±10 km s -1 and σ ∼ 21±7 km s -1 for the PUMA and the GHASP data, respectively. The PUMA velocity dispersion is higher than the one measured in the GHASP data because of its reduced spectral resolution. It is indeed difficult to measure velocities far below the instrumental resolution (σ LS F = 19. 5 and 13. 1 km s -1 , respectively) as it has been recently discussed in  Boselli et al.
(2021b)  in comparing VLT/MUSE data with FP data obtained with GHASP. At higher spatial frequencies, fluctuations in the velocity dispersion are observed on scales comparable to or larger than the one set by the seeing. These fluctuations are smoother in the GHASP data than in the PUMA ones. This is due to the difference in the method used to compute the map (Gaussian smoothing versus Voronoi tessellation, respectively). et al. 1996)  and also to investigate the dynamic of HII galaxies  (Moiseev & Lozinskaya 2012; Carvalho & Plana 2018). Moiseev & Lozinskaya (2012)  show a sketch where different features and regions in the plot can be interpreted in terms of (case 1) HII regions (constant velocity dispersion region with high Hα intensity), (case 2) shell (inclined bands in the plot), (case 3) low density turbulent ISM (triangular shape with a base spanning from low to high velocity dispersion and a triangle height ranging from low to moderate Hα intensity).
Once we identified the regions presenting a large scatter with the mean velocity dispersion of the residual velocity field, which are not supposed to be in rotation in the plane of the disc, they were masked from the observed velocity field and the axisymmetric model was recomputed. This is because the axisymmetric model is not supposed to be observationally constrained by non-axisymmetric motions. The residual velocity maps given in Fig. 7  do not show any systematic pattern in the galactic disc and have a velocity dispersion of σ res ∼ 19 km s -1 for the GHASP dataset and σ res ∼ 24 km s -1 for the PUMA dataset. The residual velocity is ∼ 0 km s -1 , suggesting that the adopted cylindrical model (described in section B. 4) reproduces well the axisymmetric rotation of the disc modelled by the rotation curve and its associated parameters.
An accurate examination of Fig. 7  indicates how the kinematical properties of the various extraplanar ionised gas features created after a ram pressure stripping event differ from those properties predicted by a purely axisymmetric cylindrical model. The most discrepant regions in terms of relative velocity of the gas are regions G, H, and L for the PUMA data and G, H, and from J to M on the southwest side of the galaxy, for the GHASP data. Here the mean gas velocity is ∼50 km s -1 higher than that observed in the model. A less pronounced difference in the same direction is observed in region E (∼ 20 km s -1 ), which is located in projection close to the kinematic centre of the disc. On the contrary, the gas inside the regions D (PUMA) and B, C, D (GHASP) has a mean velocity ∼ 40 km s -1 higher than that of the cylindrical model.
Peculiar motions Table  5. 4 gives the main kinematical properties of the gas in regions A to M. The GHASP data indicate that the gas inside most of these particular regions has a velocity dispersion near to the mean value measured over the galactic disc, and this is probably due to the Gaussian smoothing used to create the map of the velocity dispersion. The PUMA data rather indicate that the gas inside all the same regions has a velocity dispersion higher than the one measured within the galaxy disc, with the higher velocity dispersions measured in regions E, G, and K. On the other hand, the residual velocity field derived from both sets of data shows that the gas in regions A, E, F, and I follows the rigid-body rotation with a low residual velocity. This result is expected for the gas in regions E, F, and I because they are still associated to the galactic disc, but not for the region A which has been perturbed by the stripping process.
In region A, the velocity contours from both datasets indicate that the gas is rotating with a slight bending with respect to the minor axis. The PVD obtained with the PUMA dataset shows that the gas at the northeast, where the Hα monochromatic map has a hook feature, has higher radial velocities than those expected from the model. For this reason, we could expect that here the gas has a higher velocity dispersion due to non-circular  Notes.
2001; Boselli et al. 2006 Boselli et al. , 2021b;; Roediger & Hensler 2005; Tonnesen & Bryan 2009). To identify the main kinematic features resulting from the ram pressure stripping event, we compare the predicted values by theoretical fittings with the observed data. We have applied the ETM on each PVD measured along the major axis at different distances from the disc plane. In the left panels of Fig. 8  the best fit to the terminal velocity of each PVD is overlaid on its correspondent plot. In addition, in the context of the iteration method (ITM), we built a first order approximation data cube model to compute the rotation curve (RC) of NGC 4330 (see in Sect. 4). Here we compare the PVDs from the observational data with the PVDs at the same position obtained from that data cube model in the central panels of Fig.
PVDs along the minor axis The ram pressure stripping event, which is acting almost face-on in NGC 4330, has reduced the vertical height of the ionised gas disc in the northern direction (upwind). We thus study the PVDs along the kinematic minor axis to determine whether galactic fountains or inflows have been suppressed by the external pressure (e. g. Heald et al. 2006 Heald et al. , 2007;; Rosado et al. 2013). Figure  10  shows the PVDs perpendicular to the kinematic major axis obtained from the PUMA dataset. The pseudo-slits are located in specific places to highlight the main features of the disc and its asymmetries, and they cross the regions labelled from A to M identified in Sect. 2. We also compare the PVDs from the observational data with the PVDs at the same position obtained from that data cube model computed with the iteration method (ITM, see Sect.
For each figure we provide three panels, the top one corresponds to the data whereas the middle and bottom ones to the models. show the model at a depth comparable to the sensitivity of our observations. The plotted Hα emission map is the one extracted from the model for the snapshots of highest goodness for the diffuse gas. This corresponds to a peak of ram pressure occured 140 Myr ago. Similarly to the deep Hα observations presented in  Fossati et al. (2018) , the model shows extra-planar linear filaments in the downwind region of the galactic disc, which correspond to the low surface brightness filaments located in the southwest tail and close to the Fig. 10. Position-velocity diagrams parallel to the kinematic minor axis obtained from the PUMA dataset. The locations of the pseudo-slits are in the upper-left corner of each panel and they are traced on the Hα monochromatic map in the left panel with colour correspondence.
Simulations suggests that a thicker disc could results from the perturbation of the gravitational potential well due to the displacement of the gaseous component from the disc plane after a ram pressure stripping event  (Farouki & Shapiro 1980; Clarke et al. 2017; Safarzadeh & Scannapieco 2017; Steyrleithner et al. 2020 ). The boxy shape would thus result from the induced perturbation on the stellar orbits. The datasets used in this work, which are sensitive only to the kinematics of the ionised gas, do not allow us to test this hypothesis. However, in the central regions, the kinematic major axis matches with the dust lane position angles, indicating that the perturbation probably had only a moderate effect on the dynamics of the inner gas. It is thus conceivable that the dynamics of the stars are also moderately perturbed.
Figure6shows the velocity dispersion of the galaxy as measured from the PUMA and GHASP datasets. FollowingBoselli et al. (2021b)  we checked that the velocity profiles have a single peak, i. e. that the barycentric method applied to measure the velocity dispersions does not introduce any strong systematic bias in the results. At first order, the velocity dispersion of the gas is fairly constant over the disc of the galaxy, with σ ∼ 35±10 km s -1 and σ ∼ 21±7 km s -1 for the PUMA and the GHASP data, respectively. The PUMA velocity dispersion is higher than the one measured in the GHASP data because of its reduced spectral resolution. It is indeed difficult to measure velocities far below the instrumental resolution (σ LS F = 19. 5 and 13. 1 km s -1 , respectively) as it has been recently discussed inBoselli et al.