An Isolated Stellar-Mass Black Hole Detected Through Astrometric Microlensing

We report the first unambiguous detection and mass measurement of an isolated stellar-mass black hole (BH). We used the Hubble Space Telescope (HST) to carry out precise astrometry of the source star of the long-duration (t_E ~ 270 days), high-magnification microlensing event MOA-2011-BLG-191/OGLE-2011-BLG-0462, in the direction of the Galactic bulge. HST imaging, conducted at eight epochs over an interval of six years, reveals a clear relativistic astrometric deflection of the background star's apparent position. Ground-based photometry shows a parallactic signature of the effect of the Earth's motion on the microlensing light curve. Combining the HST astrometry with the ground-based light curve and the derived parallax, we obtain a lens mass of 7.1 +/- 1.3 M_Sun and a distance of 1.58 +/- 0.18 kpc. We show that the lens emits no detectable light, which, along with having a mass higher than is possible for a white dwarf or neutron star, confirms its BH nature. Our analysis also provides an absolute proper motion for the BH. The proper motion is offset from the mean motion of Galactic-disk stars at similar distances by an amount corresponding to a transverse space velocity of ~45 km/s, suggesting that the BH received a modest natal 'kick' from its supernova explosion. Previous mass determinations for stellar-mass BHs have come from radial-velocity measurements of Galactic X-ray binaries, and from gravitational radiation emitted by merging BHs in binary systems in external galaxies. Our mass measurement is the first ever for an isolated stellar-mass BH using any technique

LUME (LUnar Mission for Exploration): A new ASI proposal for lunar exploration and in situ resource utilization

A novel ASI Lunar mission is here proposed by a task force of Ph.D. students. After 14 th January 2004 president G.W Bush's speech, a new input to space human exploration has been given. The Moon, thanks to nearness to Earth, is identified as an important test bed for all future human missions. The task force LUME mission has been designed to fit with Italian technological capabilities leaving it open anyway for international cooperation. Three main module are foreseen: a lunar low altitude polar orbiter, a lander near the "peak of the eternal light" and a rover. The polar orbiter is equipped with a complete suite of experiments for remote sensing observation (high resolution color camera, VIS-NIR imaging spectrometer, neutron and X spectrometers and SAR radar). This will provide a lunar surface map in high spatial resolution at different wavelengths: the orbiter payload will be used both to refine the selection of the landing site and to support the rover navigation. The lander will reach the region of "peak of the eternal light", located in the South Pole-Aitken Basin. This landing site has been selected for two main reasons: a) sun-light is always available to deliver the power useful to perform lander experiments and b) some easy-reachable and interesting craters are close to this region. The lander embark a sun powered ISRU plant to demonstrate O 2 extraction from lunar (ilmenite) soil and a robotic arm that can pick up lunar samples both from the soil and the rover. The nuclear powered rover is equipped with a drill system that, in the first phase of its mission, will deliver samples to be processed by the ISRU plant. In a second phase the rover will move to "de Gerlache" crater, identified as an attractive region to search for water ice. The rover drill includes an imaging VIS-NIR spectrometer dedicated to analyze the mineral composition and the water ice presence along the walls of the excavated hole. Both the orbiter and the lander will carry as payload two aquatic enclosed ecosystems (biospheres): these systems have been chosen as the best trade off between reduced requirements and easy data comprehension to evaluate space environment effects on life

The Pan-STARRS1 Surveys

Pan-STARRS1 has carried out a set of distinct synoptic imaging sky surveys including the $3\pi$ Steradian Survey and the Medium Deep Survey in 5 bands ($grizy_{P1}$). The mean 5$\sigma$ point source limiting sensitivities in the stacked 3$\pi$ Steradian Survey in $grizy_{P1}$ are (23.3, 23.2, 23.1, 22.3, 21.4) respectively. The upper bound on the systematic uncertainty in the photometric calibration across the sky is 7-12 millimag depending on the bandpass. The systematic uncertainty of the astrometric calibration using the Gaia frame comes from a comparison of the results with Gaia: the standard deviation of the mean and median residuals ($\Delta ra, \Delta dec$) are (2.3, 1.7) milliarcsec, and (3.1, 4.8) milliarcsec respectively. The Pan-STARRS system and the design of the PS1 surveys are described and an overview of the resulting image and catalog data products and their basic characteristics are described together with a summary of important results. The images, reduced data products, and derived data products from the Pan-STARRS1 surveys are available to the community from the Mikulski Archive for Space Telescopes (MAST) at STScI

The Pan-STARRS1 Surveys

Pan-STARRS1 has carried out a set of distinct synoptic imaging sky surveys including the $3\pi$ Steradian Survey and the Medium Deep Survey in 5 bands ($grizy_{P1}$). The mean 5$\sigma$ point source limiting sensitivities in the stacked 3$\pi$ Steradian Survey in $grizy_{P1}$ are (23.3, 23.2, 23.1, 22.3, 21.4) respectively. The upper bound on the systematic uncertainty in the photometric calibration across the sky is 7-12 millimag depending on the bandpass. The systematic uncertainty of the astrometric calibration using the Gaia frame comes from a comparison of the results with Gaia: the standard deviation of the mean and median residuals ($\Delta ra, \Delta dec$) are (2.3, 1.7) milliarcsec, and (3.1, 4.8) milliarcsec respectively. The Pan-STARRS system and the design of the PS1 surveys are described and an overview of the resulting image and catalog data products and their basic characteristics are described together with a summary of important results. The images, reduced data products, and derived data products from the Pan-STARRS1 surveys are available to the community from the Mikulski Archive for Space Telescopes (MAST) at STScI