Data are given for 548 new proper-motion stars with {mu}>0.15arcsec/year found on 23 areas covering 25 square degrees each. These are located south of declination -40deg and between 16h and 24h in right ascension. Photographic magnitudes range from 10.0 to 20.0. Twenty stars have proper motions larger than 0.5arcsec/year a magnitude range between 14.0 and 19.5
Data are given for 494 new stars with proper motion larger than 0.15arcsec/year found on 21 areas covering 25 square degrees each. These are located between -5deg and -30deg in declination and between 0h and 9h in right ascension. Photographic magnitudes range from 9.5 to 19.0. Eight stars have proper motions larger than 0.5arcsec/year, in a magnitude range between 15.5 and 19.0.
This table presents relative proper motions and positions for 293 stars with proper motions larger than 0.15 arcsec/year, discovered as a result of a program to identify fast moving stars in the southern hemisphere, being carried out with the Maksutov Astrograph at the Estacion astronomica de Cerro el Roble
Data are given for 492 new stars with proper motion larger than 0.15arcsec/year found on 21 areas covering 25 square degrees each. These are located between -5deg and -30deg in declination and between 9h and 13h30m in right ascension. Photographic magnitudes range from 9.5 to 18.5. Four stars have proper motions larger than 0.5arcsec/year, in a magnitude range between 15.5 and 17.5.
Here we present 1584 new southern proper motion systems with {mu}>=0.18"/yr and 16.5>R_59F_>=18.0. This search complements the six previous SuperCOSMOS-RECONS (SCR) proper motion searches of the southern sky for stars within the same proper motion range, but with R_59F_<=16.5. As in previous papers, we present distance estimates for these systems and find that three systems are estimated to be within 25pc, including one, SCR 1546-5534, possibly within the RECONS 10pc horizon at 6.7pc, making it the second nearest discovery of the searches. We find 97 white dwarf candidates with distance estimates between 10 and 120pc, as well as 557 cool subdwarf candidates.
We present 2817 new southern proper motion systems with 0.40"/yr>{mu}>=0.18"/yr and declination between -47{deg} and 00{deg}. This is a continuation of the SuperCOSMOS-RECONS (SCR) proper motion searches of the southern sky. We use the same photometric relations as previous searches to provide distance estimates based on the assumption that the objects are single main-sequence stars. We find 79 new red dwarf systems predicted to be within 25pc, including a few new components of previously known systems.
A wealth of tiny galactic systems populates the surroundings of the Milky Way. However, some of these objects might have originated as former satellites of the Magellanic Clouds, in particular of the Large Magellanic Cloud (LMC). Examples of the importance of understanding how many systems are genuine satellites of the Milky Way or the LMC are the implications that the number and luminosity-mass function of satellites around hosts of different mass have for dark matter theories and the treatment of baryonic physics in simulations of structure formation. Here we aim at deriving the bulk motions and estimates of the internal velocity dispersion and metallicity properties in four recently discovered distant southern dwarf galaxy candidates, Columba I, Reticulum III, Phoenix II, and Horologium II. We combined Gaia DR2 astrometric measurements, photometry, and new FLAMES/GIRAFFE intermediate-resolution spectroscopic data in the region of the near-IR CaII triplet lines; this combination is essential for finding potential member stars in these low-luminosity systems. We find very likely member stars in all four satellites and are able to determine (or place limits on) the bulk motions and average internal properties of the systems. The systems are found to be very metal poor, in agreement with dwarf galaxies and dwarf galaxy candidates of similar luminosity. Of these four objects, we can only firmly place Phoenix II in the category of dwarf galaxies because of its resolved high velocity dispersion (9.5^+6.8^_-4.4_km/s) and intrinsic metallicity spread (0.33dex). For Columba I we also measure a clear metallicity spread. The orbital pole of Phoenix II is well constrained and close to that of the LMC, suggesting a prior association. The uncertainty on the orbital poles of the other systems is currently very large, so that an association cannot be excluded, except for Columba I. Using the numbers of potential former satellites of the LMC identified here and in the literature, we obtain for the LMC a dark matter mass of M_200_=1.9^+1.3^_-0.9_x10^11^M_{sun}_
We present the results of a survey of the Coma Berenices open star cluster (Melotte 111), undertaken using proper motions from the USNO-B1.0 (United States Naval Observatory, <I/284>) and photometry from the Two-Micron All-Sky Survey (2MASS, <II/246>) Point Source catalogues. We have identified 60 new candidate members with masses in the range 1.007<M<0.269M_{sun}_. For each we have estimated a membership probability by extracting control clusters from the proper motion vector diagram. All 60 are found to have greater than 60 per cent probability of being members, more than doubling the number of known cluster members. The new luminosity function for the cluster peaks at bright magnitudes, but is rising at K>>12, indicating that it is likely that lower mass members may exist. The mass function also supports this hypothesis.
