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Monitoring dusty sources in the vicinity of Sagittarius A*

Authors :
Peissker, F.
Hosseini, S. E.
Zajacek, M.
Eckart, A.
Saalfeld, R.
Valencia-S, M.
Parsa, M.
Karas, V.
Peissker, F.
Hosseini, S. E.
Zajacek, M.
Eckart, A.
Saalfeld, R.
Valencia-S, M.
Parsa, M.
Karas, V.
Publication Year :
2020

Abstract

Context. Several dusty infrared sources traced on their orbits around Sgr A* with SINFONI and NACO mounted at the VLT/Chile show near-infrared (NIR) excess and Doppler-shifted line emission. We investigate these sources in order to clarify their nature and compare their relationship to other observed NIR objects close to Sgr A*. Aims. Using SINFONI, we are able to determine the spectroscopic properties of the dusty infrared sources. Furthermore, we can extract spatial and velocity information of these objects. We are able to identify X7, X7.1, X8, G1, DSO/G2, D2, D23, D3, D3.1, D5, and D9 in the Doppler-shifted line maps of the SINFONI H + K data. From our K- and L '-band NACO data, we derive the related magnitudes of the brightest sources located west of Sgr A*. Methods. For determining the line of sight velocity information and to investigate single emission lines, we used the near-infrared integral field spectrograph SINFONI datasets between 2005 and 2015. For the kinematic analysis, we used NACO datasets from the years between 2002 and 2018. This study was done in the H, K-s, and L ' band. From the 3D SINFONI data-cubes, we extracted line maps in order to derive positional information for the sources. In the NACO images, we identified the dusty counterpart of the objects. When possible, we determined the Keplerian orbits and applied a photometric analysis. Results. The spectrum of the investigated objects show a Doppler-shifted Br gamma and HeI line emission. For some objects west of Sgr A*, we additionally find [FeIII] line emission that can be clearly distinguished from the background. A one-component blackbody model fits the extracted near-infrared flux for the majority of the investigated objects, with the characteristic dust temperature of 500K. The photometric derived H- and K-S -band magnitudes are between mag(II) > 22:5 and mag(K) = 18:1(-0:8)(+0:3) for the dusty sources. For the H-band magnitudes we can provide an upper limit. For the bright dusty sourc

Details

Database :
OAIster
Notes :
English
Publication Type :
Electronic Resource
Accession number :
edsoai.on1238107346
Document Type :
Electronic Resource