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Using the multi-object adaptive optics demonstrator RAVEN to observe metal-poor stars in and towards the Galactic Centre

Lamb, M. and Venn, K. and Andersen, D. and Oya, S. and Shetrone, M. and Fattahi, A. and Howes, L. and Asplund, M. and Lardière, O. and Akiyama, M. and Ono, Y. and Terada, H. and Hayano, Y. and Suzuki, G. and Blain, C. and Jackson, K. and Correia, C. and Youakim, K. and Bradley, C. (2017) Using the multi-object adaptive optics demonstrator RAVEN to observe metal-poor stars in and towards the Galactic Centre. Monthly Notices of the Royal Astronomical Society, 465 (3). pp. 3536-3557. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20170418-083220534

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Abstract

The chemical abundances for five metal-poor stars in and towards the Galactic bulge have been determined from the H-band infrared spectroscopy taken with the RAVEN multi-object adaptive optics science demonstrator and the Infrared Camera and Spectrograph at the Subaru 8.2-m telescope. Three of these stars are in the Galactic bulge and have metallicities between −2.1 < [Fe/H] < −1.5, and high [α/Fe] ∼ +0.3, typical of Galactic disc and bulge stars in this metallicity range; [Al/Fe] and [N/Fe] are also high, whereas [C/Fe] < +0.3. An examination of their orbits suggests that two of these stars may be confined to the Galactic bulge and one is a halo trespasser, though proper motion values used to calculate orbits are quite uncertain. An additional two stars in the globular cluster M22 show [Fe/H] values consistent to within 1σ, although one of these two stars has [Fe/H] = −2.01 ± 0.09, which is on the low end for this cluster. The [α/Fe] and [Ni/Fe] values differ by 2σ, with the most metal-poor star showing significantly higher values for these elements. M22 is known to show element abundance variations, consistent with a multipopulation scenario though our results cannot discriminate this clearly given our abundance uncertainties. This is the first science demonstration of multi-object adaptive optics with high-resolution infrared spectroscopy, and we also discuss the feasibility of this technique for use in the upcoming era of 30-m class telescope facilities.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stw2865DOIArticle
https://academic.oup.com/mnras/article/465/3/3536/2420718/Using-the-multi-object-adaptive-opticsPublisherArticle
https://arxiv.org/abs/1611.02712arXivDiscussion Paper
ORCID:
AuthorORCID
Fattahi, A.0000-0002-6831-5215
Howes, L.0000-0003-0117-0231
Asplund, M.0000-0002-5804-3682
Correia, C.0000-0002-6996-0734
Additional Information:© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Received: 20 September 2016. Revision Received: 02 November 2016. Accepted: 03 November 2016. Published: 05 November 2016. This paper is based (in part) on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We are sincerely grateful to the RAVEN team, and the support of the Subaru staff during our engineering runs. MPL and KAV also acknowledge funding from an NSERC Discovery Grant to help fund this research.
Funders:
Funding AgencyGrant Number
Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery GrantUNSPECIFIED
Subject Keywords:instrumentation: adaptive optics, techniques: spectroscopic, stars: abundances, Galaxy: centre, globular clusters: individual: M22
Issue or Number:3
Record Number:CaltechAUTHORS:20170418-083220534
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170418-083220534
Official Citation:M. Lamb, K. Venn, D. Andersen, S. Oya, M. Shetrone, A. Fattahi, L. Howes, M. Asplund, O. Lardière, M. Akiyama, Y. Ono, H. Terada, Y. Hayano, G. Suzuki, C. Blain, K. Jackson, C. Correia, K. Youakim, C. Bradley; Using the multi-object adaptive optics demonstrator RAVEN to observe metal-poor stars in and towards the Galactic Centre. Mon Not R Astron Soc 2017; 465 (3): 3536-3557. doi: 10.1093/mnras/stw2865
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:76628
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:18 Apr 2017 17:49
Last Modified:03 Oct 2019 17:03

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