We computed absolute stellar PMs from multi-epoch observations in the $K_s$ filter over time baselines between $\sim$12 and 47 months. This work encompasses 18 VMC tiles covering a total sky area of $\sim$28~deg$^2$. We present proper motion (PM) measurements within the central region of the Large Magellanic Cloud (LMC) using near-infrared data from the VISTA survey of the Magellanic Cloud system (VMC). Our publicly available model populations may be used in future studies of the LMC, including its structure and contribution to LISA confusion noise. Our results suggest that the total number, periods, and chirp masses of LISA sources may provide independent constraints on both LMC stellar mass and recent star formation. The range in the number of detections is primarily due to differences in the LMC total stellar mass and recent star formation in our models. Importantly, amongst these we forecast a few tens to a hundred double degenerate supernovae type Ia progenitors, a class of binaries which have never been unambiguously observed. Our models yield a hundred to several hundred detectable DWDs: indeed, the LMC will be a resolved galaxy in the LISA sky. We assemble three LMC models base on: (1) the density distribution and star formation history from optical wavelength observation, (2) a detailed hydrodynamic simulation, and (3) combining the two. Here we present the first dedicated study of the LMC with gravitational wave sources. The Large Magellanic Cloud (LMC) is expected to be prominent on the LISA sky due to its proximity and its large population of double white dwarfs (DWD).
Mosaic pro 1.0.10 full#
The Laser Interferometer Space Antenna (LISA) will unveil the non-transient gravitational wave sky full of inspiralling stellar-mass compact binaries within the Local Universe. The mass of the disk component of the LMC is 2.5 × 109 M☉, and the upper limit to all mass within a radius of 4 kpc is ~3.5 × 109 M☉. The bulk of the H I resides in a disk 7.3 kpc in diameter. On the large scale, the H I disk appears to be remarkably symmetric and to have a well-organized and orderly, if somewhat complex, rotational field. The structure of the neutral atomic ISM in the LMC is dominated by H I filaments combined with numerous shells and holes. This mosaic, with a spatial resolution 15 times higher than that which had been previously obtained, emphasizes the turbulent and fractal structure of the ISM on the small scale, resulting from the dynamical feedback of the star formation processes with the ISM. The resolution of the mosaicked images is 10 (15 pc, using a distance to the LMC of 50 kpc). We present the results of an H I aperture synthesis mosaic of the Large Magellanic Cloud (LMC), made by combining data from 1344 separate pointing centers using the Australia Telescope Compact Array (ATCA).
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