Other numerical simu- of view. The emission morphology is Waller ; Scowen et al. Some of this FUV emission lution, an anomolous pattern of non-logarithmic arms can be attributed to scattering of starlight by dust can now be traced with unprecedented clarity. The along the spiral arms Stecher et al. We note that the physical in- FUV emission remains uncertain see next Section. Well-known from that of logarithmic spirals. These patterns are identi- Survey images cf. A wide range other wavelengths.
Arms and Knots at other Wavelengths the list, further highlighting the ubiquitous nature of the linear arm segments. The background-subtracted et al. These descrip- FUV surface brightnesses of the arm segments aver- tions invariably referred to the outermost arms to the age to 5. At smaller galactocentric Orion nebulae per square kpc Bohlin et al. Better correspondence outermost giant HII region, NGC , where it ap- is evident between the FUV-bright knots making up pears to loop around and ultimately connect with this the arm segments and the young star clusters revealed kpc-size starbursting region see Figure 2b [Plate in the blue print.
Previous UV imaging Stecher et al. The ident in an arc of shared emission 1—1. UV images of the Orion results in a pattern speed for the density-wave front nebula Bohlin et al. The inner- 4. The blue photograph of M in the Atlas tained from a recent mapping of 2. Figure to contain many blue star clusters at the limit of de- 3 Plate xxx shows a contour map of the CO emis- tection. These well-correlated which appear to be background galaxies. Combes ; Garcia-Burillo et al. Beginning 1.
The super- — yield the clearest spiral structure Howard et al. Characteristic interaction time scales are of HII region in M Spectroscopic studies indicate order — years.
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That Combes Such interactions can induce the for- NGC is just now undergoing a massive starburst mation of massive condensations at the ends of the appears to be fortuitous. Using this simple formu- to dynamicists concerned with the evolution of gi- lation, we obtain for the faint southern arm a mean ant spiral galaxies. Can a single model explain the interaction timescale of 4. Anticipating numerical simulations specific to yrs. Numerical simulations of the interaction between the M system Combes et al. Internal Perturbations 5.
Howard et al companion galaxies are able to produce lopsided dis- Godbole, RM and Pancheri, Giulia Eikonalised minijet model predictions for cross-sections of photon induced processes. Canonical Structure.
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Galaxy Interactions at Low and High Redshift
Kumara P, Kirana Codes for solving three dimensional linear elastostatic problems using constant boundary elements while ignoring body forces. Mukherjee, Arnab and Bagchi, Biman Rotational friction on small globular proteins: Combined dielectric and hydrodynamic effect. Minj, Suvarsha and Rajashekar, TB Mapping of two schemes of classification for software classification.
Narayan, Vijay and Menon, Narayanan and Ramaswamy, Sriram Nonequilibrium steady states in a vibrated-rod monolayer : tetratic, nematic, and smectic correlations. Padmanabhan, T and Patel, Apoorva Semiclassical quantization of gravity I: Entropy of horizons and the area spectrum. Patel, Apoorva Scalar and axial matrix elements of the nucleon: sea quark content. Rao, Sumathi and Sen, Diptiman An introduction to bosonization and some of its applications. The velocity fields of the two components are corotating around the same axis, approximately the north—south direction slit B in Figure 7 , and span a similar velocity range.
Uncertainties on the stellar motion are the formal errors of the fit calculated using the original noise spectrum data cube and have been normalized by the of the fit. These errors are systematically larger than those for the gas, reflecting the quality of the fit, but are still much smaller than the measured velocities, reassuring us about the robustness of our results.
In the gas, the locus of negative velocities shows a bending in the external regions, with the convexity pointing toward the east. The velocity dispersion maps highlight some differences between the two components. Nominal errors on the dispersions are similar to uncertainties on the velocities, both for the gas and the stars. To better contrast the gas and stellar kinematics, we extract the velocity profiles Figure 8 along the rotation axis and its perpendicular direction B and A in Figure 7 , respectively.
We compute the average value of the spaxels entering the slit at each distance, weighted for the corresponding errors. Along slit A, the gas presents a quite regular rotation. The stars follow the same trend, even though the curve is more noisy. In contrast, along slit B, for both components the curve is always quite flat, even though with many local variations. Figure 8. Velocity profiles along the two slits shown in Figure 7 A, B , as indicated in the labels, both for the gas and the stars. Distances are deprojected considering the galaxy inclination and position angle.
Values and vertical errors are weighted by the formal errors; for the stellar velocity, horizontal errors indicate the width of the Voronoi bins.
The extended optical_disk_of_m
The gas metallicity and ionization parameter for each star-forming spaxel were calculated using the pyqz Python module7 Dopita et al. We used a modified version of the code F. The ionization parameter is quantified as the ionizing photon flux through a unit area divided by the local number density of hydrogen atoms. The spatial distribution of the ionization parameter for P is presented in Figure 9. It is generally very low, in the range. This is in agreement with other galaxies in the GASP survey Paper I , Paper IV , even though in this case a clear clumpy pattern emerges, while in other galaxies a more smooth distribution is observed.
Figure 9. Ionization parameter q map.
Figure 10 shows that the spatially resolved metallicity is overall quite low, in the range , with an average value of 8. According to the Tremonti et al. However, the uncertainties in the absolute calibration of the metallicity scale F.
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Vogt , private communication prevent us from drawing solid conclusions regarding the low metallicity of P Figure Metallicity map. Left: contours represent the original body see Figure Slits A , B and conic apertures C — E used to extract metallicity gradients are also shown. The galaxy shows a sharp decrease in its metallicity from the center toward the outskirts. The metallicity distribution is inhomogeneous, and it is not characterized by spherical symmetry.
For example, two regions of very low metallicity stand out in the southwest and northeast sides of the galaxy, while the northwest side has systematically higher metallicity values. Trends between metallicity and distance from the galaxy center are more clear in Figure 11 , where metallicity gradients along different axes are shown. To start, we use the axis defined by the velocity maps slits A and B in Figures 7 and In order to get more signal in the galaxy outskirts, instead of extracting gradients along a slit, we select all of the spaxels within conic apertures wide around the slits and take the median of the metallicity as a function of distance.
This choice also allows us to compute errors as the standard deviation within the aperture. Along A, the gradients extracted on the two sides east negative and west positive of the galaxy are quite similar, except that on the west side at there is a steeper decline in the metallicity values with distance than on the other side.
Trends are inverted at , where the east side is more metal-poor than the west side. Along B, gradients are symmetric around the 0 position up to 5''; then the north side of the galaxy presents a systematically higher metallicity.
Metallicity gradients extracted along the directions A — E shown in Figure Red points correspond to the side of the slits north or west of the center positive arcsecs ; blue points correspond to the side of the slits south or east of the center negative arcsecs. Left: profiles in arcsec, not deprojected.
Right: profiles normalized by a scale radius; all distances are deprojected considering the galaxy inclination and position angle. Shaded areas represent the profiles normalized by adopting different scale lengths see text for details. Gray lines are from Pilyugin et al.