The Radial Velocity Experiment (Rave): Third Data Release

Siebert, A.; Williams, M.; Siviero, A.; Reid, Warren A.; Boeche, C.; Steinmetz, Matthias; Fulbright, Jon P.; Munari, U.; Zwitter, T.; Watson, Fred; Wyse, Rosemary F. Ġ.; Jong, Roelof S. de; Enke, H.; Anguiano, Borja; Burton, D.; Cass, C. J. P.; Fiegert, Kristin; Hartley, M.; Ritter, Andreas; Russel, K. S.; Stupar, M.; Bienaymé, O.; Freeman, K. C.; Gilmore, G.; Grebel, Eva K.; Helmi, Amina; Navarro, Julio F.; Binney, James; Bland-Hawthorn, Joss; Campbell, Randy; Famaey, Benoît; Gerhard, Ortwin; Gibson, Brad K.; Matijevič, G.; Parker, Quentin A.; Seabroke, G. M.; Sharma, Sanjib; Smith, M. C.; Boer, Elizabeth Wylie-de

doi:10.1088/0004-6256/141/6/187

Cited by 156 publications

(88 citation statements)

References 34 publications

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“…We study data from RAVE (Steinmetz et al 2006;Zwitter et al 2008;Siebert et al 2011;Kordopatis et al 2013), a magnitude-limited survey of stars randomly selected in the 9 < I < 12 magnitude range which is currently the largest spectroscopic sample of stars in the Milky Way for which individual elemental abundances are available (Boeche et al 2011).…”

Section: Chemo-kinematic Relation In Ravementioning

confidence: 99%

A New Stellar Chemo-Kinematic Relation Reveals the Merger History of the Milky Way Disk

Minchev

Chiappini

Martig

et al. 2014

ApJ

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The velocity dispersions of stars near the Sun are known to increase with stellar age, but age can be difficult to determine, so a proxy like the abundance of α elements (e.g., Mg) with respect to iron, [α/Fe], is used. Here we report an unexpected behavior found in the velocity dispersion of a sample of giant stars from the Radial Velocity Experiment survey with high-quality chemical and kinematic information, in that it decreases strongly for stars with [Mg/Fe] > 0.4 dex (i.e., those that formed in the first gigayear of the Galaxy's life). These findings can be explained by perturbations from massive mergers in the early universe, which have affected the outer parts of the disk more strongly, and the subsequent radial migration of stars with cooler kinematics from the inner disk. Similar reversed trends in velocity dispersion are also found for different metallicity subpopulations. Our results suggest that the Milky Way disk merger history can be recovered by relating the observed chemo-kinematic relations to the properties of past merger events.

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Section: Chemo-kinematic Relation In Ravementioning

confidence: 99%

A New Stellar Chemo-Kinematic Relation Reveals the Merger History of the Milky Way Disk

Minchev

Chiappini

Martig

et al. 2014

ApJ

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“…We use the SIM-BAD database to confirm 14 sources from Table 1 and 4 sources from Table 2 as previously known variable objects or AGN. These 14 sources from Table 1 include the three Mira types (KSP-V4, V223, V964) and one SR variable (KSP-V757), as we classify (Christiansen et al 2008), whereas the remaining 10 sources have either no classification (KSP-V385, V419, V729, V791, V951; Siebert et al 2011;Cutri et al 2003;Zacharias et al 2003) or are classified as just long period variables (KSP-V21, V118, V132, V687, V889; Christiansen et al 2008). Two of these 14 previously-known sources have known periods, KSP-V757 with a 59 day period and KSP-V889 with a 36 day period (Christiansen et al Column (1) lists the id.…”

Section: Classifications and Variable Typesmentioning

confidence: 99%

Kmtnet Supernova Program Variable Objects I. NGC 2784 Field

He¹,

Neilson²,

Lee³

et al. 2016

Journal of The Korean Astronomical Society

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We present analyses of ∼1250 variable sources identified in a 20 square degree field toward NGC 2784 by the KMTNet Supernova Program. We categorize the variable sources into three groups based on their B-band variability. The first group consists of 31 high variability sources with their Bband RMS variability greater than 0.3 magnitudes. The second group of medium variability contains 265 sources with RMS variability between 0.05 and 0.3 magnitudes. The remaining 951 sources belong to the third group of low variability with an RMS variability smaller than 0.05 magnitudes. Of the entire ∼1250 sources, 4 clearly show periods of variability greater than 100 days, while the rest have periods shorter than ∼51 days or no reliable periods. The majority of the sources show either rather irregular variability or short periods faster than 2 days. Most of the sources with reliable period determination between 2 and 51 days belong to the low-variability group, although a few belong to the medium-variability group. All the variable sources with periods longer than 35 days appear to be very red with B − V > 1.5 and V − I > 2.1 magnitudes. We classify candidates of 51 Cepheids, 17 semi-regular variables, 3 Mira types, 2 RV(B) Tauri stars, 26 eclipsing binary systems and 1 active galactic nucleus. The majority of long-term variables in our sample belong to either Mira or semi-regular types, indicating that long-term variability may be more prominent in post-main sequence phases of late-type stars. The depth of the eclipsing dips of the 26 candidates for eclipsing binaries is equivalent to ∼0.61 as the average relative size of the two stars in the binary system. Our results illustrate the power of the KMTNet Supernova Program for future studies of variable objects.

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“…Many more packages of general application have been employed in the literature, but they are not publicly available, e.g., MATISSE by Recio-Blanco et al (2006), TGMET 31 by Katz et al (1998), or MyGIsFOS by Sbordone et al (2013). Some packages have been developed for particular instruments or projects, such as various parts of the SEGUE Stellar Parameter Pipeline (Lee et al 2008a(Lee et al , b, 2011aAllende Prieto et al 2008), or the original RAVE analysis pipeline (e.g., Boeche et al 2011;Siebert et al 2011).…”

Section: Automated Toolsmentioning

confidence: 99%

Solar and stellar photospheric abundances

Prieto

2016

Living Rev. Sol. Phys.

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The determination of photospheric abundances in late-type stars from spectroscopic observations is a well-established field, built on solid theoretical foundations. Improving those foundations to refine the accuracy of the inferred abundances has proven challenging, but progress has been made. In parallel, developments on instrumentation, chiefly regarding multi-object spectroscopy, have been spectacular, and a number of projects are collecting large numbers of observations for stars across the Milky Way and nearby galaxies, promising important advances in our understanding of galaxy formation and evolution. After providing a brief description of the basic physics and input data involved in the analysis of stellar spectra, a review is made of the analysis steps, and the available tools to cope with large observational efforts. The paper closes with a quick overview of relevant ongoing and planned spectroscopic surveys, and highlights of recent research on photospheric abundances.

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The Radial Velocity Experiment (Rave): Third Data Release

Cited by 156 publications

References 34 publications

A New Stellar Chemo-Kinematic Relation Reveals the Merger History of the Milky Way Disk

A New Stellar Chemo-Kinematic Relation Reveals the Merger History of the Milky Way Disk

Kmtnet Supernova Program Variable Objects I. NGC 2784 Field

Solar and stellar photospheric abundances

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