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تسجيل مستخدم جديدA panoramic view of the Milky Way analogue NGC 891
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Recent panoramic observations of the dominant spiral galaxies of the Local Group have revolutionized our view of how these galaxies assemble their mass. However, it remains completely unclear whether the properties of the outer regions of the Local Group large spirals are typical. Here, we present the first panoramic view of a spiral galaxy beyond the Local Group, based on the largest, contiguous, ground-based imaging survey to date resolving the stellar halo of the nearest prime analogue of the Milky Way, NGC 891 (D~10 Mpc). The low surface brightness outskirts of this galaxy are populated by multiple, coherent, and vast substructures over the 90kpc * 90kpc extent of the survey. These include a giant stream, the first to be resolved into stars beyond the Local Group using ground-based facilities, that loops around the parent galaxy up to distances of ~50kpc. The bulge and the disk of the galaxy are found to be surrounded by a previously undetected large, flat and thick cocoon-like stellar structure at vertical and radial distances of up to ~15kpc and ~40kpc respectively.
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We present deep ACS images of 3 fields in the edge-on disk galaxy NGC 891, which extend from the plane of the disk to 12 kpc, and out to 25 kpc along the major axis. The photometry of individual stars reaches 2.5 magnitudes below the tip of the RGB.
We use the astrophotometric catalogue to probe the stellar content and metallicity distribution across the thick disk and spheroid of NGC 891. The CMDs of thick disk and spheroid population are dominated by old RGB stars with a wide range of metallicities, from a metal-poor tail at [Fe/H] ~ -2.4 dex, up to about half-solar metallicity. The peak of the MDF of the thick disk is at -0.9 dex. The inner parts of the thick disk, within 14 kpc along the major axis show no vertical colour/metallicity gradient. In the outer parts, a mild vertical gradient of Delta(V-I)/Delta|Z| = 0.1 +/- 0.05 kpc^-1 is detected. This gradient is however accounted for by the mixing with the metal poor halo stars. No metallicity gradient along the major axis is present for thick disk stars, but strong variations of about 0.35 dex around the mean of [Fe/H] = -1.13 dex are found. The properties of the asymmetric MDFs of the thick disk stars show no significant changes in both the radial and the vertical directions. The stellar populations at solar cylinder-like distances show strikingly different properties from those of the Galaxy, suggesting that the accretion histories of both galaxies have been different. The spheroid population shows remarkably uniform stellar population properties. The median metallicity of the halo stellar population shows a shallow gradient from about -1.15 dex in the inner parts to -1.27 dex at 24 kpc distance from the centre. Similar to the thick disk stars, large variations around the mean relation are present.
We present a structural analysis of NGC891, an edge-on galaxy that has long been considered to be an analogue of the Milky Way. Using starcounts derived from deep HST/ACS images, we detect the presence of a thick disk component in this galaxy with ve
rtical scale height 1.44+/-0.03 kpc and radial scale length 4.8+/-0.1 kpc, only slightly longer than that of the thin disk. A stellar spheroid with a de Vaucouleurs-like profile is detected from a radial distance of 0.5 kpc to the edge of the survey at 25 kpc; the structure appears to become more flattened with distance, reaching q = 0.50 in the outermost halo region probed. The halo inside of 15 kpc is moderately metal-rich (median [Fe/H] ~ -1.1) and approximately uniform in median metallicity. Beyond that distance a modest chemical gradient is detected, with the median reaching [Fe/H] ~ -1.3 at 20 kpc. We find evidence for subtle, but very significant, small-scale variations in the median colour and density over the halo survey area. We argue that the colour variations are unlikely to be due to internal extinction or foreground extinction, and reflect instead variations in the stellar metallicity. Their presence suggests a startling conclusion: that the halo of this galaxy is composed of a large number of incompletely-mixed sub-populations, testifying to its origin in a deluge of small accretions.
The Milky Way disk consists of two prominent components - a thick, alpha-rich, low-metallicity component and a thin, metal-rich, low-alpha component. External galaxies have been shown to contain thin and thick disk components, but whether distinct co
mponents in the [$alpha$/Fe]-[Z/H] plane exist in other Milky Way-like galaxies is not yet known. We present VLT-MUSE observations of UGC 10738, a nearby, edge-on Milky Way-like galaxy. We demonstrate through stellar population synthesis model fitting that UGC 10738 contains alpha-rich and alpha-poor stellar populations with similar spatial distributions to the same components in the Milky Way. We discuss how the finding that external galaxies also contain chemically distinct disk components may act as a significant constraint on the formation of the Milky Ways own thin and thick disk.
The nature of our Milky Way Galaxy is reexamined from an eclectic point of view. Evidence for a central bar, for example, is not reflected in the distribution of RR Lyrae variables in the central bulge [4,5], and it is not clear if either a 2-armed o
r 4-armed spiral pattern is appropriate for the spiral arms. Radial velocity mapping of the Galaxy using radio H I, H II, or CO observations is compromised by the assumptions adopted for simple Galactic rotation. The Suns local standard of rest (LSR) velocity is $sim 14$ km s$^{-1}$ rather than 20 km s$^{-1}$, the local circular velocity is $251 pm 9$ km s$^{-1}$ rather than 220 km s$^{-1}$, and young groups of stars exhibit a 10--20 km s$^{-1}$ kick relative to what is expected from Galactic rotation. By implication, the same may be true for star-forming gas clouds affected by the Galaxys spiral density wave, raising concerns about their use for mapping spiral arms. Proper motion data in conjunction with the newly-estimated velocity components for the Suns motion imply a distance to the Galactic centre of $R_0=8.34pm0.27$ kpc, consistent with recent estimates which average $8.24pm0.09$ kpc. A cosinusoidal Galactic potential is not ruled out by observations of open star clusters. The planetary nebula cluster Bica 6, for example, has a near-escape orbit for a Newtonian potential, but a near-normal orbit in a cosinusoidal potential field. The nearby cluster Collinder 464 also displays unusually large tidal effects consistent with those expected for a cosinusoidal potential. A standard Newtonian version of the Virial Theorem for star clusters yields very reasonable masses ($sim 3 times 10^{11}M_{odot}$ and $sim 4 times 10^{11}M_{odot}$) for the Milky Way and M31 subgroups of the Local Group, respectively. A cosinusoidal relation should yield identical results.
Galaxies are surrounded by halos of hot gas whose mass and origin remain unknown. One of the most challenging properties to measure is the metallicity, which constrains both of these. We present a measurement of the metallicity around NGC 891, a near
by, edge-on, Milky Way analog. We find that the hot gas is dominated by low metallicity gas near the virial temperature at $kT=0.20pm0.01$ keV and $Z/Z_{odot} = 0.14pm0.03$(stat)$^{+0.08}_{-0.02}$(sys), and that this gas co-exists with hotter ($kT=0.71pm0.04$ keV) gas that is concentrated near the star-forming regions in the disk. Model choices lead to differences of $Delta Z/Z_{odot} sim 0.05$, and higher $S/N$ observations would be limited by systematic error and plasma emission model or abundance ratio choices. The low metallicity gas is consistent with the inner part of an extended halo accreted from the intergalactic medium, which has been modulated by star formation. However, there is much more cold gas than hot gas around NGC 891, which is difficult to explain in either the accretion or supernova-driven outflow scenarios. We also find a diffuse nonthermal excess centered on the galactic center and extending to 5 kpc above the disk with a 0.3-10 keV $L_X = 3.1times 10^{39}$ erg s$^{-1}$. This emission is inconsistent with inverse Compton scattering or single-population synchrotron emission, and its origin remains unclear.
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