The Radial Velocity Experiment (Rave): Fourth Data Release

Kordopatis, G.; Gilmore, G.; Steinmetz, Matthias; Boeche, C.; Seabroke, G. M.; Siebert, A.; Zwitter, T.; Binney, James; Laverny, P. de; Recio–Blanco, A.; Williams, M.; Piffl, Tilmann; Enke, H.; Roêser, S.; Bijaoui, A.; Wyse, Rosemary F. Ġ.; Freeman, K. C.; Munari, U.; Carrillo, I.; Anguiano, Borja; Burton, D.; Campbell, Randy; Cass, C. J. P.; Fiegert, Kristin; Hartley, M.; Parker, Quentin A.; Reid, Warren A.; Ritter, Andreas; Russell, K. S.; Stupar, M.; Watson, Fred; Bienaymé, O.; Bland‐Hawthorn, J.; Gerhard, Ortwin; Gibson, B. K.; Grebel, Eva K.; Helmi, Amina; Navarro, Julio F.; Conrad, C.; Famaey, Benoît; Faure, Carole; Just, A.; Kos, Janez; Matijevič, G.; McMillan, Paul J.; Minchev, Ivan; Scholz, R.‐D.; Sharma, Sanjib; Siviero, A.; Boer, Elizabeth Wylie de; Žerjal, M.

doi:10.1088/0004-6256/146/5/134

Cited by 300 publications

(330 citation statements)

References 91 publications

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“…It is important to note that the low end of the 90 per cent confidence interval, 2.5 × 10 11 M , is likely ruled out by observations of the inner part of the Galactic halo. Using the fourth data release of the Radial Velocity Experiment (Kordopatis et al 2013), Piffl et al (2014) found that the MW halo mass within 180 kpc is ≥9 × 10 11 M at 90 per cent confidence (Smith et al 2007;Xue et al 2008;Gnedin et al 2010;Deason et al 2012, found similar lower bounds, albeit with larger uncertainties). This result could, in principle, be used as a prior for the kind of analysis we have carried out in this paper, along with other constraints coming from the orbital properties of the massive satellites (e.g.…”

Section: Discussionmentioning

confidence: 94%

Milky Way mass constraints from the Galactic satellite gap

Cautun

Frenk

Weygaert

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We use the distribution of maximum circular velocities, V max , of satellites in the Milky Way (MW) to constrain the virial mass, M 200 , of the Galactic halo under an assumed prior of a ΛCDM universe. This is done by analysing the subhalo populations of a large sample of halos found in the Millennium II cosmological simulation. The observation that the MW has at most three subhalos with V max 30 km/s requires a halo mass M 200 1.4 × 10 12 M , while the existence of the Magellanic Clouds (assumed to have V max 60 km/s) requires M 200 1.0 × 10 12 M . The first of these conditions is necessary to avoid the "too-big-to-fail" problem highlighted by Boylan-Kolchin et al., while the second stems from the observation that massive satellites like the Magellanic Clouds are rare. When combining both requirements, we find that the MW halo mass must lie in the range 0.25 M 200 /(10 12 M ) 1.4 at 90% confidence. The gap in the abundance of Galactic satellites between 30 km/s V max 60 km/s places our galaxy in the tail of the expected satellite distribution.

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Section: Discussionmentioning

confidence: 94%

Milky Way mass constraints from the Galactic satellite gap

Cautun

Frenk

Weygaert

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…Gaia has already produced billions of RVS spectra and by the end of the mission, each star will be observed on average 40 times. This can be compared with the extremely successful RAVE survey (Radial VElocity Experiment, Kordopatis et al 2013), which measured RVs for half a million stars with V<12 mag. The Gaia end-of-mission errors will vary with the star's colour and will be of the order of 1 km s −1 for the bright red stars (G<12.5 mag and cooler than F types) and will be about 15-20 km s −1 or more for fainter and bluer stars.…”

Section: Radial Velocitiesmentioning

confidence: 99%

Globular clusters with Gaia

Pancino

Bellazzini

Giuffrida

et al. 2017

Mon. Not. R. Astron. Soc.

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The treatment of crowded fields in Gaia data will only be a reality in a few years from now. In particular, for globular clusters, only the end-of-mission data (public in 2022-2023) will have the necessary full crowding treatment and will reach sufficient quality for the faintest stars. As a consequence, the work on the deblending and decontamination pipelines is still ongoing. We describe the present status of the pipelines for different Gaia instruments, and we model the end-of-mission crowding errors on the basis of available information. We then apply the nominal post-launch Gaia performances, appropriately worsened by the estimated crowding errors, to a set of 18 simulated globular clusters with different concentration, distance, and field contamination. We conclude that there will be 10 3 -10 4 stars with astrometric performances virtually untouched by crowding (contaminated by <1 mmag) in the majoritiy of clusters. The most limiting factor will be field crowding, not cluster crowding: the most contaminated clusters will only contain 10-100 clean stars. We also conclude that: (i) the systemic proper motions and parallaxes will be determined to 1% or better up to 15 kpc, and the nearby clusters will have radial velocities to a few km s −1 ; (ii) internal kinematics will be of unprecendented quality, cluster masses will be determined to 10% up to 15 kpc and beyond, and it will be possible to identify differences of a few km s −1 or less in the kinematics (if any) of cluster sub-populations up to 10 kpc and beyond; (iii) the brightest stars (V 17 mag) will have space-quality, wide-field photometry (mmag errors), and all Gaia photometry will have 1-3% errors on the absolute photometric calibration.

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“…Despite the saturation, we were able to measure a parallax from the multiepoch VVV data: 40.35±7.19 mas and 49.07±7.06 mas (24.78 +5.4 −3.7 pc and 20.4 +3.4 −2.6 pc) respectively. 2MASS J20044356-7123334 (or LTT 7914) was observed by the RAdial Velocity Experiment (RAVE) in its fourth data release Kordopatis et al (2013) and described there. They derived a T ef f =4817 and log g=4 and metallicity [Fe/H]=0.05, based on this we could assume the dwarf nature and apply the relations described before, deriving a distance of 108 pc.…”

Section: Probable Multiple Systemsmentioning

confidence: 99%

Spectrophotometric characterization of high proper motion sources fromWISE

Beamín

Ivanov

Minniti

et al. 2015

Mon. Not. R. Astron. Soc.

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The census of the solar neighborhood is almost complete for stars and becoming more complete in the brown dwarf regime. Spectroscopic, photometric and kinematic characterization of nearby objects helps us to understand the local mass function, the binary fraction, and provides new targets for sensitive planet searches. We aim to derive spectral types and spectro-photometric distances of a sample of new high proper motion sources found with the WISE satellite, and obtain parallaxes for those objects that fall within the area observed by the Vista Variables in the Vía Láctea survey (VVV). We used low resolution spectroscopy and template fitting to derive spectral types, multiwavelength photometry to characterize the companion candidates and obtain photometric distances. Multi-epoch imaging from the VVV survey was used to measure the parallaxes and proper motions for three sources. We confirm a new T2 brown dwarf within ∼15 pc. We derived optical spectral types for twenty four sources, mostly M dwarfs within 50 pc. We addressed the wide binary nature of sixteen objects found by the WISE mission and previously known high proper motion sources. Six of these are probably members of wide binaries, two of those are new, and present evidence against the physical binary nature of two candidate binary stars found in the literature, and eight that we selected as possible binary systems. We discuss a likely microlensing event produced by a nearby low mass star and a galaxy, that is to occur in the following five years.

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The Radial Velocity Experiment (Rave): Fourth Data Release

Cited by 300 publications

References 91 publications

Milky Way mass constraints from the Galactic satellite gap

Milky Way mass constraints from the Galactic satellite gap

Globular clusters with Gaia

Spectrophotometric characterization of high proper motion sources fromWISE

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