The SkyMapper Telescope and The Southern Sky Survey

Keller, Stefan; Schmidt, B. P.; Bessell, M. S.; Conroy, P.; Francis, Paul; Granlund, Alexander; Kowald, E.; Oates, A. P.; Martin-Jones, Tony; Preston, T.; Tisserand, Patrick; Vaccarella, Annino; Waterson, M.

doi:10.1071/as07001

Cited by 476 publications

(298 citation statements)

References 30 publications

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“…Larger statistically complete samples are required for a thorough comparison with theoretical predictions. Fortunately, such samples will be obtained from much larger and deeper surveys in the near future, such as from SEGUE-2 and the Apache POint Galactic Evolution Experiment (APOGEE), the Large Sky Area MultiObject Fiber Spectroscopic Telescope (LAMOST, Zhao et al 2006), and the Southern Sky Survey (SSS, Keller et al 2007). …”

Section: Summary and Discussionmentioning

confidence: 99%

The stellar content of the Hamburg/ESO survey

Christlieb²,

Schörck³

et al. 2010

A&A

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We determine the metallicity distribution function (MDF) of the Galactic halo based on metal-poor main-sequence turnoff-stars (MSTO) which were selected from the Hamburg/ESO objective-prism survey (HES) database. Corresponding follow-up moderateresolution observations (R 2000) of 682 stars (among which 617 were accepted program stars) were carried out with the 2.3 m telescope at the Siding Spring Observatory (SSO). Corrections for the survey volume covered by the sample stars were quantitatively estimated and applied to the observed MDF. The corrections are quite small, when compared with those for a previously studied sample of metal-poor giants. The corrected observational MDF of the turnoff sample was then compared with that of the giants, as well as with a number of theoretical predictions of Galactic chemical evolution, including the mass-loss modified simple model. Although the survey-volume corrected MDFs of the metal-poor turnoff and the halo giants notably differ in the region of [Fe/H] > −2.0, below [Fe/H] ∼ −2.0, (the region we scientifically focus on most) both MDFs show a sharp drop at [Fe/H] ∼ −3.6 and present rather similar distributions in the low-metallicity tail. Theoretical models can fit some parts of the observed MDF, but none is found to simultaneously reproduce the peak as well as the features in the metal-poor region with [Fe/H] between −2.0 to −3.6. Among the tested models only the GAMETE model, when normalized to the tail of the observed MDF below [Fe/H] ∼ −3.0, and with Z cr = 10 −3.4 Z , is able to predict the sharp drop at [Fe/H] ∼ −3.6.

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Section: Summary and Discussionmentioning

confidence: 99%

The stellar content of the Hamburg/ESO survey

Christlieb²,

Schörck³

et al. 2010

A&A

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“…As these primary uncertainties will be much reduced in the next generation of supernova surveys, e.g. the SkyMapper Supernova Survey (Keller et al 2007), our understanding of Milky Way dust extinction is the next-most important factor in the line. For this reason alone, and for several others, we would like to improve our understanding of dust extinction.…”

Section: Introductionmentioning

confidence: 99%

Milky Way dust extinction measured with QSOs

Wolf

2014

Monthly Notices of the Royal Astronomical Society

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We investigate reddening by Milky Way dust in the low-extinction regime of E B−V < 0.15. Using over 50,000 QSOs at 0.5 < z < 2.5 from the SDSS DR7 QSO Catalogue we probe the residual SDSS colours after dereddening and correcting for the known spectroscopic redshifts. We find that the extinction vector of Schlafly & Finkbeiner (2011, SF11) is a better fit to the data than that used by Schlegel et al. (1998, SFD). There is evidence for a non-linearity in the SFD reddening map, which is similarly present in the V1.2 map of the Planck Collaboration. This non-linearity is similarly seen when galaxies or stars are used as probes of the SFD map.

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“…Since most of the new discoveries were made using deep CCD sky surveys such as the Sloan Digital Sky Survey, which cover primarily the northern hemisphere, it seems highly likely that additional objects will be added once the southern sky is scanned in a similar manner (e.g. Keller et al 2007;Walsh et al 2009). …”

Section: Introductionmentioning

confidence: 99%

A photometric and spectroscopic study of the new dwarf spheroidal galaxy in Hercules

Adén¹,

Feltzing²,

Koch

et al. 2009

A&A

150

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Context. Dwarf spheroidal (dSph) galaxies are the least luminous, least massive galaxies known. Recently, the number of observed galaxies in this class has greatly increased thanks to large surveys. Determining their properties, such as mass, luminosity and metallicity, provides key information in our understanding of galaxy formation and evolution. Aims. Our aim is to provide as clean and as complete a sample as possible of red giant branch stars that are members of the Hercules dSph galaxy. With this sample we explore the velocity dispersion and the metallicity of the system. Methods. Strömgren photometry and multi-fibre spectroscopy are combined to provide information about the evolutionary state of the stars (via the Strömgren c 1 index) and their radial velocities. Based on this information we have selected a clean sample of red giant branch stars, and show that foreground contamination by Milky Way dwarf stars can greatly distort the results. Results. Our final sample consists of 28 red giant branch stars in the Hercules dSph galaxy. Based on these stars we find a mean photometric metallicity of −2.35 ± 0.31 dex which is consistent with previous studies. We find evidence for an abundance spread. Using those stars for which we have determined radial velocities we find a systemic velocity of 45.20 ± 1.09 km s −1 with a dispersion of 3.72 km s −1 , this is lower than values found in the literature. Furthermore we identify the horizontal branch and estimate the mean magnitude of the horizontal branch of the Hercules dSph galaxy to be V 0 = 21.17 ± 0.05, which corresponds to a distance of 147 +8 −7 kpc. Conclusions. When studying sparsely populated and/or heavily foreground contaminated dSph galaxies it is necessary to include knowledge about the evolutionary stage of the stars. This can be done in several ways. Here we have explored the power of the c 1 index in Strömgren photometry. This index is able to clearly identify red giant branch stars redder than the horizontal branch, enabling a separation of red giant branch dSph stars and foreground dwarf stars. Additionally, this index is also capable of correctly identifying both red and blue horizontal branch stars. We have shown that a proper cleaning of the sample results in a smaller value for the velocity dispersion of the system. This has implications for galaxy properties derived from such velocity dispersions.

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The SkyMapper Telescope and The Southern Sky Survey

Cited by 476 publications

References 30 publications

The stellar content of the Hamburg/ESO survey

The stellar content of the Hamburg/ESO survey

Milky Way dust extinction measured with QSOs

A photometric and spectroscopic study of the new dwarf spheroidal galaxy in Hercules

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