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Monitoring the Dusty S-cluster Object (DSO/G2) on its Orbit toward the Galactic Center Black Hole
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SYSNO ASEP 0441745 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Monitoring the Dusty S-cluster Object (DSO/G2) on its Orbit toward the Galactic Center Black Hole Author(s) Valencia-S, M. (DE)
Eckart, A. (DE)
Zajaček, Michal (ASU-R) ORCID
Peissker, F. (DE)
Parsa, M. (DE)
Grosso, N. (FR)
Mossoux, E. (FR)
Porquet, D. (FR)
Jalali, B. (DE)
Karas, Vladimír (ASU-R) RID, ORCID
Yazici, S. (DE)
Shahzamanian, B. (DE)
Sabha, N. (DE)
Saalfeld, R. (DE)
Smajic, S. (DE)
Grellmann, R. (DE)
Moser, L. (DE)
Horrobin, M. (DE)
Borkar, A. (DE)
García-Marín, M. (DE)
Dovčiak, Michal (ASU-R) RID, ORCID
Kunneriath, Devaky (ASU-R) RID
Karssen, G. (DE)
Bursa, Michal (ASU-R) RID, ORCID
Straubmeier, C. (DE)
Bushouse, H. (US)Number of authors 26 Source Title Astrophysical Journal - ISSN 0004-637X
Roč. 800, č. 2 (2015), 125/1-125/21Number of pages 21 s. Publication form Print - P Language eng - English Country US - United States Keywords black holes ; galactic center ; Milky way Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics R&D Projects GC13-00070J GA ČR - Czech Science Foundation (CSF) Institutional support ASU-R - RVO:67985815 UT WOS 000349782500048 DOI 10.1088/0004-637X/800/2/125 Annotation We analyze and report in detail new near-infrared (1.45-2.45 μm) observations of the Dusty S-cluster Object (DSO/G2) during its approach to the black hole at the center of the Galaxy that were carried out with the ESO Very Large Telescope/SINFONI between 2014 February and September. Before 2014 May we detect spatially compact Brγ and Paα line emission from the DSO at about 40 mas east of Sgr A*. The velocity of the source, measured from the redshifted emission, is 2700 ± 60 km s–1. No blueshifted emission above the noise level is detected at the position of Sgr A* or upstream of the presumed orbit. We do not detect any significant extension of the velocity gradient across the source. We find a Brγ line FWHM of 50 ± 10 Å before and 15 ± 10 Å after the peribothron transit, i.e., no significant line broadening with respect to last year is observed. Brγ line maps show that the bulk of the line emission originates from a region of less than 20 mas diameter. This is consistent with a very compact source on an elliptical orbit with a peribothron time passage in 2014.39 ± 0.14. Increased accretion activity of Sgr A* may still be upcoming. We discuss details of a source model according to which the DSO is a young accreting star rather than a coreless gas and dust cloud. Workplace Astronomical Institute Contact Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2016
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