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The Sgr A* Stellar Cluster: New NIR Imaging and Spectroscopy
Astrophysics · Submitted 2 Nov 1999
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These data demonstrate clearly that there is no strong CO bandhead absorption originating in the northern part (S1/S2 area) of the central stellar cluster at the position of Sgr A*.
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The abstract, sentence by sentence
We report preliminary results based on new near-infrared observations of the central stellar cluster of our Galaxy conducted with the infrared spectrometer ISAAC at the ESO VLT UT1 and the MPE speckle camera SHARP at the ESO NTT. We obtained lambda / dlambda >= 3000 K-band spectroscopy of the 2.058 um He I, 2.165 um Br gamma emission lines, and 2.29 um CO bandhead absorption line. These data demonstrate clearly that there is no strong CO bandhead absorption originating in the northern part (S1/S2 area) of the central stellar cluster at the position of Sgr A*. This makes it likely that these K~14.5 stars are O9 - B0.5 stars with masses of 15 to 20 M(sun). Weaker CO bandhead absorption in the southern part of the cluster (S10/S11 area) could be due to contributions from neighbouring stars. We also report the detection of Br gamma line emission at the position of the central stellar cluster which could be associated with the 'mini-spiral' rather than with the Sgr A* cluster itself. At the NTT we obtained another epoch epoch of proper motion measurments. The changes of source positions are consistent with the proper motion velocities derived from earlier epochs.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We report preliminary results based on new near-infrared observations of the central stellar cluster of our Galaxy conducted with the infrared spectrometer ISAAC at the ESO VLT UT1 and the MPE speckle camera SHARP at the ESO NTT. | contribution 0.56 | 0.96 | 0.03 | asserted 0.98 |
| s1 | We obtained lambda / dlambda >= 3000 K-band spectroscopy of the 2.058 um He I, 2.165 um Br gamma emission lines, and 2.29 um CO bandhead absorption line. | method 0.88 | 0.97 | 0.04 | asserted 1.00 |
| s2 | These data demonstrate clearly that there is no strong CO bandhead absorption originating in the northern part (S1/S2 area) of the central stellar cluster at the position of Sgr A*. | result 1.00 | 0.94 | 0.56 | asserted 1.00 |
| s3 | This makes it likely that these K~14.5 stars are O9 - B0.5 stars with masses of 15 to 20 M(sun). | interpretation 1.00 | 0.72 | 0.13 | hedged possibility 1.00 |
| s4 | Weaker CO bandhead absorption in the southern part of the cluster (S10/S11 area) could be due to contributions from neighbouring stars. | interpretation 0.76 | 0.81 | 0.05 | hedged possibility 1.00 |
| s5 | We also report the detection of Br gamma line emission at the position of the central stellar cluster which could be associated with the 'mini-spiral' rather than with the Sgr A* cluster itself. | result 0.93 | 0.95 | 0.07 | hedged possibility 0.99 |
| s6 | At the NTT we obtained another epoch epoch of proper motion measurments. | method 0.48 | 0.96 | 0.02 | asserted 1.00 |
| s7 | The changes of source positions are consistent with the proper motion velocities derived from earlier epochs. | result 0.89 | 0.88 | 0.05 | hedged possibility 0.87 |
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Original abstract
We report preliminary results based on new near-infrared observations of the central stellar cluster of our Galaxy conducted with the infrared spectrometer ISAAC at the ESO VLT UT1 and the MPE speckle camera SHARP at the ESO NTT. We obtained lambda / dlambda >= 3000 K-band spectroscopy of the 2.058 um He I, 2.165 um Br gamma emission lines, and 2.29 um CO bandhead absorption line. These data demonstrate clearly that there is no strong CO bandhead absorption originating in the northern part (S1/S2 area) of the central stellar cluster at the position of Sgr A*. This makes it likely that these K~14.5 stars are O9 - B0.5 stars with masses of 15 to 20 M(sun). Weaker CO bandhead absorption in the southern part of the cluster (S10/S11 area) could be due to contributions from neighbouring stars. We also report the detection of Br gamma line emission at the position of the central stellar cluster which could be associated with the 'mini-spiral' rather than with the Sgr A* cluster itself. At the NTT we obtained another epoch epoch of proper motion measurments. The changes of source positions are consistent with the proper motion velocities derived from earlier epochs.
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