RECORD
Fabry-Perot Observations of Globular Clusters III: M15
Astrophysics · Submitted 11 Dec 1996
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim This profile and the previously-published surface brightness profile can be equally well represented either by a stellar population whose M/L varies with radius from 1.7 in solar units at large radii to 3 in the central region, or by a population with a constant M/L of 1.7 and a central black hole of 1000 M_sol.
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
We have used an Imaging Fabry-Perot Spectrophotometer with the Sub-arcsecond Imaging Spectrograph on the CFHT to measure velocities for 1534 stars in the globular cluster M15. Combined with previous velocity samples, the total number of stars with measured velocities in M15 is 1597. The velocity dispersion profile for M15 remains flat at a value of 11 km/s from a radius of 0.4' into our innermost reliable point at 0.02' (0.06 pc). This profile and the previously-published surface brightness profile can be equally well represented either by a stellar population whose M/L varies with radius from 1.7 in solar units at large radii to 3 in the central region, or by a population with a constant M/L of 1.7 and a central black hole of 1000 M_sol. A non-parametric mass model that assumes no black hole, no rotation, and isotropy constrains the mass density of M15 to better than 30% at a radius of 0.07 parsecs. Using the assumption of local thermodynamic equilibrium, we estimate the present-day mass function and infer a significant number of 0.6-0.7 M_sol objects in the central few parsecs, 85% of which may be in the form of stellar remnants. Not only do we detect rotation; we find that the position angle of the projected rotation axis in the central 10" is 100 degrees different from that of the whole sample. We also detect an increase in the amplitude of the rotation at small radii. Although this increase needs to be confirmed with better-seeing data, it may be the result of a central mass concentration.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We have used an Imaging Fabry-Perot Spectrophotometer with the Sub-arcsecond Imaging Spectrograph on the CFHT to measure velocities for 1534 stars in the globular cluster M15. | method 0.71 | 0.98 | 0.05 | asserted 1.00 |
| s1 | Combined with previous velocity samples, the total number of stars with measured velocities in M15 is 1597. | contribution 0.40 | 0.47 | 0.04 | asserted 1.00 |
| s2 | The velocity dispersion profile for M15 remains flat at a value of 11 km/s from a radius of 0.4' into our innermost reliable point at 0.02' (0.06 pc). | result 1.00 | 0.91 | 0.24 | asserted 1.00 |
| s3 | This profile and the previously-published surface brightness profile can be equally well represented either by a stellar population whose M/L varies with radius from 1.7 in solar units at large radii to 3 in the central region, or by a population with a constant M/L of 1.7 and a central black hole of 1000 M_sol. | interpretation 0.81 | 0.76 | 0.36 | asserted 0.57 |
| s4 | A non-parametric mass model that assumes no black hole, no rotation, and isotropy constrains the mass density of M15 to better than 30% at a radius of 0.07 parsecs. | result 0.89 | 0.92 | 0.15 | asserted 1.00 |
| s5 | Using the assumption of local thermodynamic equilibrium, we estimate the present-day mass function and infer a significant number of 0.6-0.7 M_sol objects in the central few parsecs, 85% of which may be in the form of stellar remnants. | result 0.97 | 0.95 | 0.09 | asserted 0.51 |
| s6 | Not only do we detect rotation; we find that the position angle of the projected rotation axis in the central 10" is 100 degrees different from that of the whole sample. | result 1.00 | 0.97 | 0.14 | asserted 1.00 |
| s7 | We also detect an increase in the amplitude of the rotation at small radii. | result 1.00 | 0.95 | 0.08 | asserted 1.00 |
| s8 | Although this increase needs to be confirmed with better-seeing data, it may be the result of a central mass concentration. | interpretation 0.85 | 0.58 | 0.08 | hedged possibility 0.99 |
What was examined, and what was not
- arXiv listing abstract v1
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
We have used an Imaging Fabry-Perot Spectrophotometer with the Sub-arcsecond Imaging Spectrograph on the CFHT to measure velocities for 1534 stars in the globular cluster M15. Combined with previous velocity samples, the total number of stars with measured velocities in M15 is 1597. The velocity dispersion profile for M15 remains flat at a value of 11 km/s from a radius of 0.4' into our innermost reliable point at 0.02' (0.06 pc). This profile and the previously-published surface brightness profile can be equally well represented either by a stellar population whose M/L varies with radius from 1.7 in solar units at large radii to 3 in the central region, or by a population with a constant M/L of 1.7 and a central black hole of 1000 M_sol. A non-parametric mass model that assumes no black hole, no rotation, and isotropy constrains the mass density of M15 to better than 30% at a radius of 0.07 parsecs. Using the assumption of local thermodynamic equilibrium, we estimate the present-day mass function and infer a significant number of 0.6-0.7 M_sol objects in the central few parsecs, 85% of which may be in the form of stellar remnants. Not only do we detect rotation; we find that the position angle of the projected rotation axis in the central 10" is 100 degrees different from that of the whole sample. We also detect an increase in the amplitude of the rotation at small radii. Although this increase needs to be confirmed with better-seeing data, it may be the result of a central mass concentration.
Human review
References
How the literature uses it
2 arXiv papers cite this in 2 sentences
Papers citing it · 1 sentence without a confident label
Uses its data or values 1 paper
-
For M 15 the final baryon density is taken from [ref] .
Search for dark matter signals with Fermi-LAT observation of globular clusters NGC 6388 and M 15 · DM density distribution · 1.00
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.